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@ARTICLE{warren_brown+2005, | |
author = {{Brown}, Warren R. and {Geller}, Margaret J. and {Kenyon}, Scott J. and | |
{Kurtz}, Michael J.}, | |
title = "{Discovery of an Unbound Hypervelocity Star in the Milky Way Halo}", | |
journal = {\apjl}, | |
keywords = {Galaxy: Center, Galaxy: Halo, Galaxy: Kinematics and Dynamics, Galaxy: Stellar Content, Stars: Early-Type, Astrophysics}, | |
year = 2005, | |
month = mar, | |
volume = {622}, | |
number = {1}, | |
pages = {L33-L36}, | |
doi = {10.1086/429378}, | |
archivePrefix = {arXiv}, | |
eprint = {astro-ph/0501177}, | |
primaryClass = {astro-ph}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2005ApJ...622L..33B}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@article{peissker+2020, | |
doi = {10.3847/1538-4357/ab9c1c}, | |
url = {https://doi.org/10.3847%2F1538-4357%2Fab9c1c}, | |
year = 2020, | |
month = {aug}, | |
publisher = {American Astronomical Society}, | |
volume = {899}, | |
number = {1}, | |
pages = {50}, | |
author = {Florian Pei{\ss}ker and Andreas Eckart and Michal Zaja{\v{c}}ek and Basel Ali and Marzieh Parsa}, | |
title = {S62 and S4711: Indications of a Population of Faint Fast-moving Stars inside the S2 Orbit{\textemdash}S4711 on a 7.6 yr Orbit around Sgr A{\ast}}, | |
journal = {The Astrophysical Journal}, | |
abstract = {We present high-pass filtered NACO and SINFONI images of the newly discovered stars S4711–S4715 between 2004 and 2016. Our deep H+K-band (SINFONI) and K-band (NACO) data show the S-cluster star S4711 on a highly eccentric trajectory around Sgr A* with an orbital period of 7.6 yr and a periapse distance of 144 au to the supermassive black hole (SMBH). S4711 is hereby the star with the shortest orbital period and the smallest mean distance to the SMBH during its orbit to date. The used high-pass filtered images are based on coadded data sets to improve the signal to noise. The spectroscopic SINFONI data let us determine detailed stellar properties of S4711 like the mass and the rotational velocity. The faint S-cluster star candidates, S4712–S4715, can be observed in a projected distance to Sgr A* of at least temporarily ≤120 mas. From these stars, S4714 is the most prominent, with an orbital period of 12 yr and an eccentricity of 0.985. The stars S4712–S4715 show similar properties, with magnitudes and stellar masses comparable to those of S4711. The MCMC simulations determine confidently precise uncertainties for the orbital elements of S62 and S4711–S4715. The presence of S4711 in addition to S55, S62, and the also newly found star S4714 implies a population of faint stars that can be found at distances to Sgr A* that are comparable to the size of our solar system. These short orbital time period stars in the dense cluster around the SMBH in the center of our Galaxy are perfect candidates to observe gravitational effects such as the periapse shift.} | |
} | |
@ARTICLE{cowling1941, | |
author = {{Cowling}, T.~G.}, | |
title = "{The non-radial oscillations of polytropic stars}", | |
journal = {\mnras}, | |
year = 1941, | |
month = jan, | |
volume = {101}, | |
pages = {367}, | |
doi = {10.1093/mnras/101.8.367}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/1941MNRAS.101..367C}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{madigan+2011, | |
author = {{Madigan}, Ann-Marie and {Hopman}, Clovis and {Levin}, Yuri}, | |
title = "{Secular Stellar Dynamics near a Massive Black Hole}", | |
journal = {\apj}, | |
keywords = {black hole physics, celestial mechanics, Galaxy: center, stars: kinematics and dynamics, Astrophysics - Astrophysics of Galaxies}, | |
year = 2011, | |
month = sep, | |
volume = {738}, | |
number = {1}, | |
eid = {99}, | |
pages = {99}, | |
doi = {10.1088/0004-637X/738/1/99}, | |
archivePrefix = {arXiv}, | |
eprint = {1010.1535}, | |
primaryClass = {astro-ph.GA}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2011ApJ...738...99M}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{stone+2008athena, | |
author = {{Stone}, James M. and {Gardiner}, Thomas A. and {Teuben}, Peter and | |
{Hawley}, John F. and {Simon}, Jacob B.}, | |
title = "{Athena: A New Code for Astrophysical MHD}", | |
journal = {\apjs}, | |
keywords = {hydrodynamics, MHD, methods: numerical, Astrophysics}, | |
year = 2008, | |
month = sep, | |
volume = {178}, | |
number = {1}, | |
pages = {137-177}, | |
doi = {10.1086/588755}, | |
archivePrefix = {arXiv}, | |
eprint = {0804.0402}, | |
primaryClass = {astro-ph}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2008ApJS..178..137S}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{ligo+2020unequal, | |
author = {{Abbott}, R. and {Abbott}, T.~D. and {Abraham}, S. and {Acernese}, F. and | |
{Ackley}, K. and {Adams}, C. and {Adhikari}, R.~X. and {Adya}, V.~B. and | |
{Affeldt}, C. and {Agathos}, M. and et al.}, | |
title = "{GW190412: Observation of a binary-black-hole coalescence with asymmetric masses}", | |
journal = {\prd}, | |
year = 2020, | |
month = aug, | |
volume = {102}, | |
number = {4}, | |
eid = {043015}, | |
pages = {043015}, | |
doi = {10.1103/PhysRevD.102.043015}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2020PhRvD.102d3015A}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{choi+2016, | |
author = {{Choi}, Jieun and {Dotter}, Aaron and {Conroy}, Charlie and | |
{Cantiello}, Matteo and {Paxton}, Bill and {Johnson}, Benjamin D.}, | |
title = "{Mesa Isochrones and Stellar Tracks (MIST). I. Solar-scaled Models}", | |
journal = {\apj}, | |
keywords = {stars: evolution, stars: general, stars: interiors, Astrophysics - Solar and Stellar Astrophysics}, | |
year = 2016, | |
month = jun, | |
volume = {823}, | |
number = {2}, | |
eid = {102}, | |
pages = {102}, | |
doi = {10.3847/0004-637X/823/2/102}, | |
archivePrefix = {arXiv}, | |
eprint = {1604.08592}, | |
primaryClass = {astro-ph.SR}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2016ApJ...823..102C}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{dotter2016, | |
author = {{Dotter}, Aaron}, | |
title = "{MESA Isochrones and Stellar Tracks (MIST) 0: Methods for the Construction of Stellar Isochrones}", | |
journal = {\apjs}, | |
keywords = {methods: numerical, stars: evolution, Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics}, | |
year = 2016, | |
month = jan, | |
volume = {222}, | |
number = {1}, | |
eid = {8}, | |
pages = {8}, | |
doi = {10.3847/0067-0049/222/1/8}, | |
archivePrefix = {arXiv}, | |
eprint = {1601.05144}, | |
primaryClass = {astro-ph.SR}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2016ApJS..222....8D}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{merritt+2011, | |
author = {{Merritt}, David and {Alexander}, Tal and {Mikkola}, Seppo and | |
{Will}, Clifford M.}, | |
title = "{Stellar dynamics of extreme-mass-ratio inspirals}", | |
journal = {\prd}, | |
keywords = {04.30.Db, 04.25.Nx, 04.80.Cc, Wave generation and sources, Post-Newtonian approximation, perturbation theory, related approximations, Experimental tests of gravitational theories, Astrophysics - Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology}, | |
year = 2011, | |
month = aug, | |
volume = {84}, | |
number = {4}, | |
eid = {044024}, | |
pages = {044024}, | |
doi = {10.1103/PhysRevD.84.044024}, | |
archivePrefix = {arXiv}, | |
eprint = {1102.3180}, | |
primaryClass = {astro-ph.CO}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2011PhRvD..84d4024M}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{ivanov+2013, | |
author = {{Ivanov}, P.~B. and {Papaloizou}, J.~C.~B. and {Chernov}, S.~V.}, | |
title = "{A unified normal mode approach to dynamic tides and its application to rotating Sun-like stars}", | |
journal = {\mnras}, | |
keywords = {hydrodynamics, celestial mechanics, planet-star interactions, binaries: close, stars: oscillations, Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies}, | |
year = 2013, | |
month = jul, | |
volume = {432}, | |
number = {3}, | |
pages = {2339-2365}, | |
doi = {10.1093/mnras/stt595}, | |
archivePrefix = {arXiv}, | |
eprint = {1304.2027}, | |
primaryClass = {astro-ph.SR}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2013MNRAS.432.2339I}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{burkart+2012, | |
author = {{Burkart}, Joshua and {Quataert}, Eliot and {Arras}, Phil and | |
{Weinberg}, Nevin N.}, | |
title = "{Tidal asteroseismology: Kepler's KOI-54}", | |
journal = {\mnras}, | |
keywords = {asteroseismology, hydrodynamics, waves, binaries: close, stars: oscillations, Astrophysics - Solar and Stellar Astrophysics}, | |
year = 2012, | |
month = apr, | |
volume = {421}, | |
number = {2}, | |
pages = {983-1006}, | |
doi = {10.1111/j.1365-2966.2011.20344.x}, | |
archivePrefix = {arXiv}, | |
eprint = {1108.3822}, | |
primaryClass = {astro-ph.SR}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2012MNRAS.421..983B}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{generozov2020, | |
author = {{Generozov}, Aleksey}, | |
title = "{A stream of hypervelocity stars from the Galactic Center}", | |
journal = {arXiv e-prints}, | |
keywords = {Astrophysics - Astrophysics of Galaxies}, | |
year = 2020, | |
month = may, | |
eid = {arXiv:2005.10267}, | |
pages = {arXiv:2005.10267}, | |
archivePrefix = {arXiv}, | |
eprint = {2005.10267}, | |
primaryClass = {astro-ph.GA}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2020arXiv200510267G}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{warren_brown+2006, | |
author = {{Brown}, Warren R. and {Geller}, Margaret J. and {Kenyon}, Scott J. and | |
{Kurtz}, Michael J.}, | |
title = "{Hypervelocity Stars. I. The Spectroscopic Survey}", | |
journal = {\apj}, | |
keywords = {Galaxies: Individual: Name: Leo A, Galaxies: Individual: Name: Draco, Galaxy: Halo, Galaxy: Stellar Content, Stars: Horizontal-Branch, Stars: White Dwarfs, Astrophysics}, | |
year = 2006, | |
month = aug, | |
volume = {647}, | |
number = {1}, | |
pages = {303-311}, | |
doi = {10.1086/505165}, | |
archivePrefix = {arXiv}, | |
eprint = {astro-ph/0604111}, | |
primaryClass = {astro-ph}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2006ApJ...647..303B}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{chen&amaro-seoane2014, | |
author = {{Chen}, Xian and {Amaro-Seoane}, Pau}, | |
title = "{A Rapidly Evolving Region in the Galactic Center: Why S-stars Thermalize and More Massive Stars are Missing}", | |
journal = {\apjl}, | |
keywords = {Galaxy: center, Galaxy: kinematics and dynamics, methods: analytical, stars: massive, stars: Wolf-Rayet, Astrophysics - Astrophysics of Galaxies}, | |
year = 2014, | |
month = may, | |
volume = {786}, | |
number = {2}, | |
eid = {L14}, | |
pages = {L14}, | |
doi = {10.1088/2041-8205/786/2/L14}, | |
archivePrefix = {arXiv}, | |
eprint = {1401.6456}, | |
primaryClass = {astro-ph.GA}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2014ApJ...786L..14C}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{wenbinlu+2020, | |
author = {{Lu}, Wenbin and {Fuller}, Jim and {Raveh}, Yael and {Perets}, Hagai B. and | |
{Li}, Ting S. and {Hosek}, Matthew W., Jr. and {Do}, Tuan}, | |
title = "{The former companion of the hyper-velocity star S5-HVS1}", | |
journal = {arXiv e-prints}, | |
keywords = {Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics}, | |
year = 2020, | |
month = may, | |
eid = {arXiv:2005.12300}, | |
pages = {arXiv:2005.12300}, | |
archivePrefix = {arXiv}, | |
eprint = {2005.12300}, | |
primaryClass = {astro-ph.HE}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2020arXiv200512300L}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{pfuhl+2014, | |
author = {{Pfuhl}, O. and {Alexander}, T. and {Gillessen}, S. and {Martins}, F. and | |
{Genzel}, R. and {Eisenhauer}, F. and {Fritz}, T.~K. and {Ott}, T.}, | |
title = "{Massive Binaries in the Vicinity of Sgr A*}", | |
journal = {\apj}, | |
keywords = {binaries: eclipsing, Galaxy: center, infrared: stars, stars: early-type, stars: massive, stars: Wolf-Rayet, Astrophysics - Astrophysics of Galaxies}, | |
year = 2014, | |
month = feb, | |
volume = {782}, | |
number = {2}, | |
eid = {101}, | |
pages = {101}, | |
doi = {10.1088/0004-637X/782/2/101}, | |
archivePrefix = {arXiv}, | |
eprint = {1307.7996}, | |
primaryClass = {astro-ph.GA}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2014ApJ...782..101P}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{martins+2006, | |
author = {{Martins}, F. and {Trippe}, S. and {Paumard}, T. and {Ott}, T. and | |
{Genzel}, R. and {Rauw}, G. and {Eisenhauer}, F. and {Gillessen}, S. and | |
{Maness}, H. and {Abuter}, R.}, | |
title = "{GCIRS 16SW: A Massive Eclipsing Binary in the Galactic Center}", | |
journal = {\apjl}, | |
keywords = {Stars: Binaries: Eclipsing, Galaxy: Center, Stars: Early-Type, Astrophysics}, | |
year = 2006, | |
month = oct, | |
volume = {649}, | |
number = {2}, | |
pages = {L103-L106}, | |
doi = {10.1086/508328}, | |
archivePrefix = {arXiv}, | |
eprint = {astro-ph/0608215}, | |
primaryClass = {astro-ph}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2006ApJ...649L.103M}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{krumholz&thompson2007, | |
author = {{Krumholz}, Mark R. and {Thompson}, Todd A.}, | |
title = "{Mass Transfer in Close, Rapidly Accreting Protobinaries: An Origin for Massive Twins?}", | |
journal = {\apj}, | |
keywords = {Accretion, Accretion Disks, Stars: Binaries: Close, Stars: Binaries: Spectroscopic, Stars: Evolution, Stars: Formation, Stars: Pre-Main-Sequence, Astrophysics}, | |
year = 2007, | |
month = jun, | |
volume = {661}, | |
number = {2}, | |
pages = {1034-1041}, | |
doi = {10.1086/515566}, | |
archivePrefix = {arXiv}, | |
eprint = {astro-ph/0611822}, | |
primaryClass = {astro-ph}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2007ApJ...661.1034K}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{sana+2013, | |
author = {{Sana}, H. and {de Koter}, A. and {de Mink}, S.~E. and | |
{Dunstall}, P.~R. and {Evans}, C.~J. and {H{\'e}nault-Brunet}, V. and | |
{Ma{\'\i}z Apell{\'a}niz}, J. and {Ram{\'\i}rez-Agudelo}, O.~H. and | |
{Taylor}, W.~D. and {Walborn}, N.~R. and {Clark}, J.~S. and | |
{Crowther}, P.~A. and {Herrero}, A. and {Gieles}, M. and {Langer}, N. and | |
{Lennon}, D.~J. and {Vink}, J.~S.}, | |
title = "{The VLT-FLAMES Tarantula Survey. VIII. Multiplicity properties of the O-type star population}", | |
journal = {\aap}, | |
keywords = {stars: early-type, stars: massive, binaries: spectroscopic, open clusters and associations: individual: 30 Dor, binaries: close, Magellanic Clouds, Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics}, | |
year = 2013, | |
month = feb, | |
volume = {550}, | |
eid = {A107}, | |
pages = {A107}, | |
doi = {10.1051/0004-6361/201219621}, | |
archivePrefix = {arXiv}, | |
eprint = {1209.4638}, | |
primaryClass = {astro-ph.SR}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2013A&A...550A.107S}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{kiminki&kobulnicky2012, | |
author = {{Kiminki}, Daniel C. and {Kobulnicky}, Henry A.}, | |
title = "{An Updated Look at Binary Characteristics of Massive Stars in the Cygnus OB2 Association}", | |
journal = {\apj}, | |
keywords = {binaries: close, binaries: general, binaries: spectroscopic, stars: early-type, stars: kinematics and dynamics, techniques: radial velocities, Astrophysics - Solar and Stellar Astrophysics}, | |
year = 2012, | |
month = may, | |
volume = {751}, | |
number = {1}, | |
eid = {4}, | |
pages = {4}, | |
doi = {10.1088/0004-637X/751/1/4}, | |
archivePrefix = {arXiv}, | |
eprint = {1203.2156}, | |
primaryClass = {astro-ph.SR}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2012ApJ...751....4K}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{ishida+2015, | |
author = {{Ishida}, E.~E.~O. and {Vitenti}, S.~D.~P. and {Penna-Lima}, M. and | |
{Cisewski}, J. and {de Souza}, R.~S. and {Trindade}, A.~M.~M. and | |
{Cameron}, E. and {Busti}, V.~C. and {COIN Collaboration}}, | |
title = "{COSMOABC: Likelihood-free inference via Population Monte Carlo Approximate Bayesian Computation}", | |
journal = {Astronomy and Computing}, | |
keywords = {Galaxies: statistics, (cosmology:) large-scale structure of universe, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics}, | |
year = 2015, | |
month = nov, | |
volume = {13}, | |
pages = {1-11}, | |
doi = {10.1016/j.ascom.2015.09.001}, | |
archivePrefix = {arXiv}, | |
eprint = {1504.06129}, | |
primaryClass = {astro-ph.CO}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2015A&C....13....1I}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@article{gala, | |
doi = {10.21105/joss.00388}, | |
url = {https://doi.org/10.21105\%2Fjoss.00388}, | |
year = 2017, | |
month = {oct}, | |
publisher = {The Open Journal}, | |
volume = {2}, | |
number = {18}, | |
author = {Adrian M. Price-Whelan}, | |
title = {Gala: A Python package for galactic dynamics}, | |
journal = {The Journal of Open Source Software} | |
} | |
@ARTICLE{dremova+2019, | |
author = {{Dremova}, G.~N. and {Dremov}, V.~V. and {Tutukov}, A.~V.}, | |
title = "{The Statistics of S Stars and Their Correlation with Hypervelocity Stars}", | |
journal = {Astronomy Reports}, | |
year = 2019, | |
month = oct, | |
volume = {63}, | |
number = {10}, | |
pages = {862-876}, | |
doi = {10.1134/S1063772919100032}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2019ARep...63..862D}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{fragione+2017, | |
author = {{Fragione}, G. and {Capuzzo-Dolcetta}, R. and {Kroupa}, P.}, | |
title = "{Hypervelocity stars from young stellar clusters in the Galactic Centre}", | |
journal = {\mnras}, | |
keywords = {Galaxy: centre, Galaxy: kinematics and dynamics, stars: kinematics and dynamics, galaxies: star clusters: general, Astrophysics - Astrophysics of Galaxies}, | |
year = 2017, | |
month = may, | |
volume = {467}, | |
number = {1}, | |
pages = {451-460}, | |
doi = {10.1093/mnras/stx106}, | |
archivePrefix = {arXiv}, | |
eprint = {1609.05305}, | |
primaryClass = {astro-ph.GA}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2017MNRAS.467..451F}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{kobayashi+2012, | |
author = {{Kobayashi}, Shiho and {Hainick}, Yanir and {Sari}, Re'em and | |
{Rossi}, Elena M.}, | |
title = "{Ejection and Capture Dynamics in Restricted Three-body Encounters}", | |
journal = {\apj}, | |
keywords = {binaries: general, Galaxy: center, Galaxy: halo, Galaxy: kinematics and dynamics, planets and satellites: formation, planets and satellites: individual: Triton, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies}, | |
year = 2012, | |
month = apr, | |
volume = {748}, | |
number = {2}, | |
eid = {105}, | |
pages = {105}, | |
doi = {10.1088/0004-637X/748/2/105}, | |
archivePrefix = {arXiv}, | |
eprint = {1201.4794}, | |
primaryClass = {astro-ph.HE}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2012ApJ...748..105K}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{cai+2018, | |
author = {{Cai}, Rong-Gen and {Liu}, Tong-Bo and {Wang}, Shao-Jiang}, | |
title = "{The GWs from the S-stars revolving around the SMBH at Sgr A*}", | |
journal = {arXiv e-prints}, | |
keywords = {General Relativity and Quantum Cosmology}, | |
year = 2018, | |
month = aug, | |
eid = {arXiv:1808.03164}, | |
pages = {arXiv:1808.03164}, | |
archivePrefix = {arXiv}, | |
eprint = {1808.03164}, | |
primaryClass = {gr-qc}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2018arXiv180803164C}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{launhardt+2002, | |
author = {{Launhardt}, R. and {Zylka}, R. and {Mezger}, P.~G.}, | |
title = "{The nuclear bulge of the Galaxy. III. Large-scale physical characteristics of stars and interstellar matter}", | |
journal = {\aap}, | |
keywords = {DUST, EXTINCTION, ISM: STRUCTURE, GALAXY: CENTRE, GALAXY: STRUCTURE, INFRARED: ISM, Astrophysics}, | |
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and V{\'a}zquez-Baeza, Yoshiki | |
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volume={17}, | |
number={3}, | |
pages={261-272}, | |
abstract={SciPy is an open-source scientific computing library for the Python programming language. Since its initial release in 2001, SciPy has become a de facto standard for leveraging scientific algorithms in Python, with over 600 unique code contributors, thousands of dependent packages, over 100,000 dependent repositories and millions of downloads per year. In this work, we provide an overview of the capabilities and development practices of SciPy 1.0 and highlight some recent technical developments.}, | |
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abstract = {Matplotlib is a 2D graphics package used for Python for | |
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primaryClass = {astro-ph}, | |
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} | |
@ARTICLE{antonini+2010, | |
author = {{Antonini}, Fabio and {Faber}, Joshua and {Gualandris}, Alessia and | |
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adsurl = {https://ui.adsabs.harvard.edu/abs/2019ApJ...880...42W}, | |
archiveprefix = {arXiv}, | |
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eid = {42}, | |
eprint = {1901.03339}, | |
file = {:Wernke/2019.pdf:PDF;:Wernke/2019.pdf:PDF}, | |
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primaryclass = {astro-ph.HE}, | |
} | |
@ARTICLE{mori+2019, | |
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eprint = {1910.03459}, | |
primaryClass = {astro-ph.HE}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2019ApJ...885..142M}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
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eprint = {1401.7354}, | |
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adsurl = {https://ui.adsabs.harvard.edu/abs/2014ApJ...783..131Y}, | |
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@ARTICLE{kocsis&tremaine2011, | |
author = {{Kocsis}, Bence and {Tremaine}, Scott}, | |
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eprint = {1006.0001}, | |
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adsurl = {https://ui.adsabs.harvard.edu/abs/2011MNRAS.412..187K}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{merritt+2009, | |
author = {{Merritt}, David and {Gualandris}, Alessia and {Mikkola}, Seppo}, | |
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adsurl = {https://ui.adsabs.harvard.edu/abs/2009ApJ...693L..35M}, | |
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@ARTICLE{tamayo+2019, | |
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primaryClass = {astro-ph.EP}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2020MNRAS.491.2885T}, | |
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eprint = {1409.4779}, | |
primaryClass = {astro-ph.EP}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2015MNRAS.446.1424R}, | |
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} | |
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eprint = {1110.4876}, | |
primaryClass = {astro-ph.EP}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2012A&A...537A.128R}, | |
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@ARTICLE{bradnick+2017, | |
author = {{Bradnick}, B. and {Mandel}, I. and {Levin}, Y.}, | |
title = "{Stellar binaries in galactic nuclei: tidally stimulated mergers followed by tidal disruptions}", | |
journal = {\mnras}, | |
keywords = {binaries: close, stars: kinematics and dynamics, galaxies: nuclei, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies}, | |
year = "2017", | |
month = "Aug", | |
volume = {469}, | |
number = {2}, | |
pages = {2042-2048}, | |
doi = {10.1093/mnras/stx1007}, | |
archivePrefix = {arXiv}, | |
eprint = {1703.05796}, | |
primaryClass = {astro-ph.HE}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2017MNRAS.469.2042B}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{naoz+2018, | |
author = {{Naoz}, Smadar and {Ghez}, Andrea M. and {Hees}, Aurelien and | |
{Do}, Tuan and {Witzel}, Gunther and {Lu}, Jessica R.}, | |
title = "{Confusing Binaries: The Role of Stellar Binaries in Biasing Disk Properties in the Galactic Center}", | |
journal = {\apjl}, | |
keywords = {binaries: close, quasars: supermassive black holes, stars: black holes, stars: kinematics and dynamics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics}, | |
year = "2018", | |
month = "Feb", | |
volume = {853}, | |
number = {2}, | |
eid = {L24}, | |
pages = {L24}, | |
doi = {10.3847/2041-8213/aaa6bf}, | |
archivePrefix = {arXiv}, | |
eprint = {1801.03934}, | |
primaryClass = {astro-ph.GA}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2018ApJ...853L..24N}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@INPROCEEDINGS{yelda+2013, | |
author = {{Yelda}, Sylvana and {Ghez}, A.~M. and {Lu}, J.~R. and {Do}, T. and | |
{Meyer}, L. and {Morris}, M.}, | |
title = "{The Kinematic Structure of the Young Stellar Disk in the Galactic Center}", | |
booktitle = {American Astronomical Society Meeting Abstracts \#221}, | |
year = "2013", | |
series = {American Astronomical Society Meeting Abstracts}, | |
volume = {221}, | |
month = "Jan", | |
eid = {254.03}, | |
pages = {254.03}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2013AAS...22125403Y}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{bartko+2010, | |
author = {{Bartko}, H. and {Martins}, F. and {Trippe}, S. and {Fritz}, T.~K. and {Genzel}, R. and {Ott}, T. and {Eisenhauer}, F. and {Gillessen}, S. and {Paumard}, T. and {Alexander}, T. and {Dodds-Eden}, K. and {Gerhard}, O. and {Levin}, Y. and {Mascetti}, L. and {Nayakshin}, S. and {Perets}, H.~B. and {Perrin}, G. and {Pfuhl}, O. and {Reid}, M.~J. and {Rouan}, D. and {Zilka}, M. and {Sternberg}, A.}, | |
title = "{An Extremely Top-Heavy Initial Mass Function in the Galactic Center Stellar Disks}", | |
journal = {\apj}, | |
keywords = {Galaxy: center, stars: early-type, stars: luminosity function, mass function, Astrophysics - Astrophysics of Galaxies}, | |
year = 2010, | |
month = jan, | |
volume = {708}, | |
number = {1}, | |
pages = {834-840}, | |
doi = {10.1088/0004-637X/708/1/834}, | |
archivePrefix = {arXiv}, | |
eprint = {0908.2177}, | |
primaryClass = {astro-ph.GA}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2010ApJ...708..834B}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{bartko+2009, | |
author = {{Bartko}, H. and {Martins}, F. and {Fritz}, T.~K. and {Genzel}, R. and | |
{Levin}, Y. and {Perets}, H.~B. and {Paumard}, T. and {Nayakshin}, S. and | |
{Gerhard}, O. and {Alexander}, T. and {Dodds-Eden}, K. and | |
{Eisenhauer}, F. and {Gillessen}, S. and {Mascetti}, L. and {Ott}, T. and | |
{Perrin}, G. and {Pfuhl}, O. and {Reid}, M.~J. and {Rouan}, D. and | |
{Sternberg}, A. and {Trippe}, S.}, | |
title = "{Evidence for Warped Disks of Young Stars in the Galactic Center}", | |
journal = {\apj}, | |
keywords = {Galaxy: center, stars: early-type, stars: formation, stars: luminosity function, mass function, stellar dynamics, Astrophysics}, | |
year = "2009", | |
month = "Jun", | |
volume = {697}, | |
number = {2}, | |
pages = {1741-1763}, | |
doi = {10.1088/0004-637X/697/2/1741}, | |
archivePrefix = {arXiv}, | |
eprint = {0811.3903}, | |
primaryClass = {astro-ph}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2009ApJ...697.1741B}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{antonini&merritt2013, | |
author = {{Antonini}, Fabio and {Merritt}, David}, | |
title = "{Relativity and the Evolution of the Galactic Center S-star orbits}", | |
journal = {\apjl}, | |
keywords = {Galaxy: center, relativistic processes, stars: kinematics and dynamics, Astrophysics - Astrophysics of Galaxies, General Relativity and Quantum Cosmology}, | |
year = "2013", | |
month = "Jan", | |
volume = {763}, | |
number = {1}, | |
eid = {L10}, | |
pages = {L10}, | |
doi = {10.1088/2041-8205/763/1/L10}, | |
archivePrefix = {arXiv}, | |
eprint = {1211.4594}, | |
primaryClass = {astro-ph.GA}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2013ApJ...763L..10A}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{koposov+2019, | |
author = {{Koposov}, Sergey E. and {Boubert}, Douglas and {Li}, Ting S. and | |
{Erkal}, Denis and {Da Costa}, Gary S. and {Zucker}, Daniel B. and | |
{Ji}, Alexander P. and {Kuehn}, Kyler and {Lewis}, Geraint F. and | |
{Mackey}, Dougal and {Simpson}, Jeffrey D. and {Shipp}, Nora and | |
{Wan}, Zhen and {Belokurov}, Vasily and {Bland-Hawthorn}, Joss and | |
{Martell}, Sarah L. and {Nordlander}, Thomas and {Pace}, Andrew B. and | |
{De Silva}, Gayandhi M. and {Wang}, Mei-Yu and {S5 collaboration}}, | |
title = "{Discovery of a nearby 1700 km s$^{-1}$ star ejected from the Milky Way by Sgr A*}", | |
journal = {\mnras}, | |
keywords = {stars: kinematics and dynamics, Galaxy: centre, Galaxy: fundamental parameters, Astrophysics - Astrophysics of Galaxies}, | |
year = "2020", | |
month = "Jan", | |
volume = {491}, | |
number = {2}, | |
pages = {2465-2480}, | |
doi = {10.1093/mnras/stz3081}, | |
archivePrefix = {arXiv}, | |
eprint = {1907.11725}, | |
primaryClass = {astro-ph.GA}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2020MNRAS.491.2465K}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@ARTICLE{cohn1979, | |
author = {{Cohn}, H.}, | |
title = "{Numerical integration of the Fokker-Planck equation and the evolution of star clusters}", | |
journal = {\apj}, | |
keywords = {Fokker-Planck Equation, Galactic Evolution, Galactic Structure, Measure And Integration, Star Clusters, Astronomical Models, Astrophysics}, | |
year = "1979", | |
month = "Dec", | |
volume = {234}, | |
pages = {1036-1053}, | |
doi = {10.1086/157587}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/1979ApJ...234.1036C}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@Article{subr&haas2016, | |
Title = {{The Properties of Hypervelocity Stars and S-stars Originating from an Eccentric Disk around a Supermassive Black Hole}}, | |
Author = {{{\v S}ubr}, L. and {Haas}, J.}, | |
Journal = {\apj}, | |
Year = {2016}, | |
Month = sep, | |
Pages = {1}, | |
Volume = {828}, | |
Abstract = {Hypervelocity stars (HVSs), which are observed in the Galactic halo, are believed to be accelerated to large velocities by a process of tidal disruption of binary stars passing close to the supermassive black hole (SMBH) which resides in the center of the Galaxy. It is, however, still unclear where these relatively young stars were born and what dynamical process pushed them to nearly radial orbits around the SMBH. In this paper we investigate the possibility that the young binaries originated from a thin eccentric disk, similar to the one currently observed in the Galactic center. By means of direct N-body simulations, we follow the dynamical evolution of an initially thin and eccentric disk of stars with a 100% binary fraction orbiting around the SMBH. Such a configuration leads to Kozai-Lidov oscillations of orbital elements, bringing a considerable number of binaries to the close vicinity of the black hole. Subsequent tidal disruption of these binaries accelerates one of their components to velocities well above the escape velocity from the SMBH, while the second component becomes tightly bound to the SMBH. We describe the main kinematic properties of the escaping and tightly bound stars within our model, and compare them qualitatively to the properties of the observed HVSs and S-stars, respectively. The most prominent feature is strong anisotropy in the directions of the escaping stars, which is observed for Galactic HVSs but has not yet been explained.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016ApJ...828....1S}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/0004-637X/828/1/1}, | |
Eid = {1}, | |
Eprint = {1606.09247}, | |
Keywords = {black hole physics, Galaxy: halo, Galaxy: nucleus, methods: numerical, stars: early-type, stars: kinematics and dynamics}, | |
Owner = {aleksey}, | |
Timestamp = {2019.02.04} | |
} | |
@Misc{aarseth2006, | |
Title = {{NBODY Codes: Numerical Simulations of Many-body (N-body) | |
Gravitational Interactions}}, | |
Author = {{Aarseth}, S.~J.}, | |
HowPublished = {Astrophysics Source Code Library}, | |
Month = feb, | |
Year = {2011}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011ascl.soft02006A}, | |
Archiveprefix = {ascl}, | |
Eprint = {1102.006}, | |
Keywords = {Software} | |
} | |
@Article{abbate+2018, | |
author = {{Abbate}, F. and {Mastrobuono-Battisti}, A. and {Colpi}, M. and {Possenti}, A. and {Sippel}, A.~C. and {Dotti}, M.}, | |
title = {{Probing the formation history of the nuclear star cluster at the Galactic Centre with millisecond pulsars}}, | |
journal = {\mnras}, | |
year = {2018}, | |
volume = {473}, | |
pages = {927-936}, | |
month = jan, | |
abstract = {The origin of the nuclear star cluster in the centre of our Galaxy is still unknown. One possibility is that it formed after the disruption of stellar clusters that spiralled into the Galactic Centre due to dynamical friction. We trace the formation of the nuclear star cluster around the central black hole, using state-of-the-art N-body simulations, and follow the dynamics of the neutron stars born in the clusters. We then estimate the number of millisecond pulsars (MSPs) that are released in the nuclear star cluster during its formation. The assembly and tidal dismemberment of globular clusters lead to a population of MSPs distributed over a radius of about 20 pc, with a peak near 3 pc. No clustering is found on the subparsec scale. We simulate the detectability of this population with future radio telescopes like the MeerKAT radio telescope and SKA1, and find that about an order of 10 MSPs can be observed over this large volume, with a paucity of MSPs within the central parsec. This helps discriminating this scenario from the in situ formation model for the nuclear star cluster that would predict an overabundance of MSPs closer to the black hole. We then discuss the potential contribution of our MSP population to the gamma-ray excess at the Galactic Centre.}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
adsurl = {http://adsabs.harvard.edu/abs/2018MNRAS.473..927A}, | |
archiveprefix = {arXiv}, | |
doi = {10.1093/mnras/stx2364}, | |
eprint = {1708.01627}, | |
file = {:/home/aleksey/Documents/Abbate/abbate+2018.pdf:PDF;:Abbate/abbate+2018.pdf:PDF;:abbate+2018.pdf:PDF;:abbate+2018.pdf:PDF}, | |
keywords = {pulsars: general, Galaxy: centre, Galaxy: formation, globular clusters: general}, | |
owner = {aleksey}, | |
timestamp = {2018.04.19}, | |
} | |
@Article{abbott+2016, | |
Title = {{The Rate of Binary Black Hole Mergers Inferred from | |
Advanced LIGO Observations Surrounding GW150914}}, | |
Author = {{Abbott}, B.~P. and {Abbott}, R. and {Abbott}, T.~D. and | |
{Abernathy}, M.~R. and {Acernese}, F. and {Ackley}, K. and | |
{Adams}, C. and {Adams}, T. and {Addesso}, P. and | |
{Adhikari}, R.~X. and et al.}, | |
Journal = {\apjl}, | |
Year = {2016}, | |
Month = dec, | |
Pages = {L1}, | |
Volume = {833}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016ApJ...833L...1A}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/2041-8205/833/1/L1}, | |
Eid = {L1}, | |
Eprint = {1602.03842}, | |
Keywords = {black holes, gravitational waves, stars: massive}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{aharon+2016, | |
author = {{Aharon}, D. and {Mastrobuono Battisti}, A. and {Perets}, H.~B.}, | |
title = {{The History of Tidal Disruption Events in Galactic Nuclei}}, | |
journal = {\apj}, | |
year = {2016}, | |
volume = {823}, | |
pages = {137}, | |
month = jun, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
adsurl = {http://adsabs.harvard.edu/abs/2016ApJ...823..137A}, | |
archiveprefix = {arXiv}, | |
doi = {10.3847/0004-637X/823/2/137}, | |
eid = {137}, | |
eprint = {1507.08287}, | |
file = {:Aharon/aharon+2016.pdf:PDF}, | |
keywords = {galaxies: nuclei, galaxies: star clusters: general, stars: formation}, | |
owner = {aleksey}, | |
timestamp = {2017.12.12}, | |
} | |
@Article{aharon&perets2015, | |
Title = {{Formation and Evolution of Nuclear Star Clusters with In | |
Situ Star Formation: Nuclear Cores and Age Segregation}}, | |
Author = {{Aharon}, D. and {Perets}, H.~B.}, | |
Journal = {\apj}, | |
Year = {2015}, | |
Month = feb, | |
Pages = {185}, | |
Volume = {799}, | |
Abstract = {Nuclear stellar cluster (NSCs) are known to exist around | |
massive black holes (MBHs) in galactic nuclei. Two | |
formation scenarios were suggested for their origin: (1) | |
buildup of NSCs from consecutive infall of stellar clusters | |
and (2) continuous in situ star formation. Though the | |
cluster infall scenario has been extensively studied, the | |
in situ formation scenario has been hardly explored. Here | |
we use Fokker-Planck (FP) calculations to study the effects | |
of star formation on the buildup of NSCs and its | |
implications for their long-term evolution and their | |
resulting structure. We use the FP equation to describe the | |
evolution of stellar populations and add appropriate source | |
terms to account for the effects of newly formed stars. We | |
show that continuous star formation even 1-2 pc away from | |
the MBH can lead to the buildup of an NSC with properties | |
similar to those of the Milky Way NSC. We find that the | |
structure of the old stellar population in the NSC with in | |
situ star formation could be very similar to the | |
steady-state Bahcall-Wolf cuspy structure. However, its | |
younger populations do not yet achieve a steady state. In | |
particular, formed/evolved NSCs with in situ star formation | |
contain differential age-segregated stellar populations | |
that are not yet fully mixed. Younger stellar populations | |
formed in the outer regions of the NSC have a cuspy | |
structure toward the NSC outskirts, while showing a | |
core-like distribution inward, with younger populations | |
having larger core sizes. In principal, such a structure | |
can give rise to an apparent core-like radial distribution | |
of younger stars, as observed in the Galactic center.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015ApJ...799..185A}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1409.5121}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/799/2/185}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1409.5121}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2015ApJ...799..185A}, | |
Date-added = {2016-10-17 18:55:41 +0000}, | |
Date-modified = {2017-04-23 20:11:54 +0000}, | |
Doi = {10.1088/0004-637X/799/2/185}, | |
Eid = {185}, | |
Eprint = {1409.5121}, | |
Keywords = {Galaxy: center, Galaxy: formation, Galaxy: nucleus, | |
Galaxy: structure, stars: formation, stars: kinematics and | |
dynamics} | |
} | |
@Article{aird+2012, | |
Title = {{PRIMUS: The Dependence of AGN Accretion on Host Stellar | |
Mass and Color}}, | |
Author = {{Aird}, J. and {Coil}, A.~L. and {Moustakas}, J. and | |
{Blanton}, M.~R. and {Burles}, S.~M. and {Cool}, R.~J. and | |
{Eisenstein}, D.~J. and {Smith}, M.~S.~M. and {Wong}, K.~C. | |
and {Zhu}, G.}, | |
Journal = {\apj}, | |
Year = {2012}, | |
Month = feb, | |
Pages = {90}, | |
Volume = {746}, | |
Abstract = {We present evidence that the incidence of active galactic | |
nuclei (AGNs) and the distribution of their accretion rates | |
do not depend on the stellar masses of their host galaxies, | |
contrary to previous studies. We use hard (2-10 keV) X-ray | |
data from three extragalactic fields (XMM-LSS, COSMOS, and | |
ELAIS-S1) with redshifts from the Prism Multi-object Survey | |
to identify 242 AGNs with L 2-10 keV = 1042-44 erg s-1 | |
within a parent sample of ~25,000 galaxies at 0.2 < z < 1.0 | |
over ~3.4 deg2 and to i ~ 23. We find that although the | |
fraction of galaxies hosting an AGN at fixed X-ray | |
luminosity rises strongly with stellar mass, the | |
distribution of X-ray luminosities is independent of mass. | |
Furthermore, we show that the probability that a galaxy | |
will host an AGN can be defined by a universal Eddington | |
ratio distribution that is independent of the host galaxy | |
stellar mass and has a power-law shape with slope -0.65. | |
These results demonstrate that AGNs are prevalent at all | |
stellar masses in the range 9.5 and that the same physical | |
processes regulate AGN activity in all galaxies in this | |
stellar mass range. While a higher AGN fraction may be | |
observed in massive galaxies, this is a selection effect | |
related to the underlying Eddington ratio distribution. We | |
also find that the AGN fraction drops rapidly between z ~ 1 | |
and the present day and is moderately enhanced (factor ~2) | |
in galaxies with blue or green optical colors. | |
Consequently, while AGN activity and star formation appear | |
to be globally correlated, we do not find evidence that the | |
presence of an AGN is related to the quenching of star | |
formation or the color transformation of galaxies.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012ApJ...746...90A}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1107.4368}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/746/1/90}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1107.4368}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2012ApJ...746...90A}, | |
Date-added = {2016-03-16 19:35:16 +0000}, | |
Date-modified = {2016-03-16 19:35:17 +0000}, | |
Doi = {10.1088/0004-637X/746/1/90}, | |
Eid = {90}, | |
Eprint = {1107.4368}, | |
Keywords = {galaxies: active, galaxies: evolution, X-rays: galaxies} | |
} | |
@Article{alexander+2016, | |
Title = {{Discovery of an Outflow from Radio Observations of the Tidal Disruption Event ASASSN-14li}}, | |
Author = {{Alexander}, K.~D. and {Berger}, E. and {Guillochon}, J. and {Zauderer}, B.~A. and {Williams}, P.~K.~G.}, | |
Journal = {\apjl}, | |
Year = {2016}, | |
Month = mar, | |
Pages = {L25}, | |
Volume = {819}, | |
Abstract = {We report the discovery of transient radio emission from the nearby optically discovered tidal disruption event (TDE) ASASSN-14li (distance of 90 Mpc), making it the first typical TDE detected in the radio, and unambiguously pointing to the formation of a non-relativistic outflow with a kinetic energy of ?(4-10) × 1047 erg, a velocity of ?12,000-36,000 km s-1, and a mass of ?3 × 10-5-7 × 10-4 M?. We show that the outflow was ejected on 2014 August 11-25, in agreement with an independent estimate of the timing of super-Eddington accretion based on the optical, ultraviolet, and X-ray observations, and that the ejected mass corresponds to about 1%-10% of the mass accreted in the super-Eddington phase. The temporal evolution of the radio emission also uncovers the circumnuclear density profile, ? (R)\propto {R}-2.5 on a scale of about 0.01 pc, a scale that cannot be probed via direct measurements even in the nearest supermassive black holes. Our discovery of radio emission from the nearest well-studied TDE to date, with a radio luminosity lower than all previous limits, indicates that non-relativistic outflows are ubiquitous in TDEs, and that future, more sensitive, radio surveys will uncover similar events.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016ApJ...819L..25A}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/2041-8205/819/2/L25}, | |
Eid = {L25}, | |
Eprint = {1510.01226}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: nuclei, radiation mechanisms: non-thermal, radio continuum: galaxies, relativistic processes}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2018.03.13} | |
} | |
@Article{alexander+2015, | |
Title = {{Discovery of an outflow from radio observations of the | |
tidal disruption event ASASSN-14li}}, | |
Author = {{Alexander}, K.~D. and {Berger}, E. and {Guillochon}, J. | |
and {Zauderer}, B.~A. and {Williams}, P.~K.~G.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2015}, | |
Month = oct, | |
Abstract = {The tidal disruption of stars by supermassive black holes | |
(SMBH) lights up dormant systems and can be used to probe | |
accretion and outflow processes. Theoretical calculations | |
indicate that most tidal disruption events (TDEs) lead to | |
super-Eddington accretion, which in turn drives outflows. | |
The discovery of luminous radio emission from the | |
$\gamma$-ray TDE Sw J1644+57 revealed the formation of a | |
relativistic jetted outflow, but such events represent | |
$\lesssim 1\%$ of the TDE population. Direct evidence for | |
outflows in the bulk of the TDE population, discovered | |
through optical, ultraviolet (UV), and X-ray observations, | |
has been lacking. Here we report the discovery of transient | |
radio emission from the nearby optically-discovered TDE | |
ASASSN-14li (distance of 90 Mpc), making it the first | |
normal TDE detected in the radio, and unambiguously | |
pointing to the formation of a non-relativistic outflow | |
with a kinetic energy of $\approx 10^{48}$ erg, a velocity | |
of $\approx 12,000-39,000$ km s$^{-1}$, and a mass of | |
$\approx 10^{-4}-10^{-3}$ M$_{\odot}$. We show that the | |
outflow was ejected on 2014 August 11-25, in agreement with | |
an independent estimate of the timing of super-Eddington | |
accretion based on the optical, UV, and X-ray observations, | |
and that the ejected mass corresponds to about $1-10\%$ of | |
the mass accreted in the super-Eddington phase. The | |
temporal evolution of the radio emission also uncovers the | |
circumnuclear density profile, $\rho(R)\propto R^{-2.6}$ on | |
a scale of about 0.01 pc, a scale that cannot be probed via | |
direct measurements even in the nearest SMBHs. Our | |
discovery of radio emission from the nearest TDE to date, | |
with a radio luminosity lower than all previous limits, | |
indicates that non-relativistic outflows are ubiquitous in | |
TDEs, and that future, more sensitive, radio surveys will | |
uncover similar events.}, | |
Adscomment = {5 figures, 2 tables}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015arXiv151001226A}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1510.01226}, | |
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Bdsk-url-1 = {http://arXiv.org/abs/1510.01226}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/2015arXiv151001226A}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:36 +0000}, | |
Eprint = {1510.01226}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena; | |
Untitled; Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{alexander+2017, | |
Title = {{Radio Observations of the Tidal Disruption Event XMMSL1 | |
J0740-85}}, | |
Author = {{Alexander}, K.~D. and {Wieringa}, M.~H. and {Berger}, E. | |
and {Saxton}, R.~D. and {Komossa}, S.}, | |
Journal = {\apj}, | |
Year = {2017}, | |
Month = mar, | |
Pages = {153}, | |
Volume = {837}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017ApJ...837..153A}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/1538-4357/aa6192}, | |
Eid = {153}, | |
Eprint = {1610.03861}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: | |
nuclei, radiation mechanisms: non-thermal, radio continuum: | |
galaxies, relativistic processes}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2017.10.15} | |
} | |
@Article{alexander2017, | |
Title = {{Stellar Dynamics and Stellar Phenomena Near A Massive | |
Black Hole}}, | |
Author = {{Alexander}, T.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2017}, | |
Month = jan, | |
Abstract = {Most galactic nuclei harbor a massive black hole (MBH), | |
whose birth and evolution are closely linked to those of | |
its host galaxy. The unique conditions near the MBH: high | |
velocity and density in the steep potential of a massive | |
singular relativistic object, lead to unusual modes of | |
stellar birth, evolution, dynamics and death. A complex | |
network of dynamical mechanisms, operating on multiple | |
timescales, deflect stars to orbits that intercept the MBH. | |
Such close encounters lead to energetic interactions with | |
observable signatures and consequences for the evolution of | |
the MBH and its stellar environment. Galactic nuclei are | |
astrophysical laboratories that test and challenge our | |
understanding of MBH formation, strong gravity, stellar | |
dynamics, and stellar physics. I review from a theoretical | |
perspective the wide range of stellar phenomena that occur | |
near MBHs, focusing on the role of stellar dynamics near an | |
isolated MBH in a relaxed stellar cusp.}, | |
Adscomment = {41 pp. 6 figures. Author's original version. To appear in | |
Annual Review of Astronomy and Astrophysics. See final | |
published version in ARAA website: | |
www.annualreviews.org/doi/10.1146/annurev-astro-091916-05530}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017arXiv170104762A}, | |
Annote = {Review }, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1701.04762}, | |
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Bdsk-url-1 = {http://arxiv.org/abs/1701.04762}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/2017arXiv170104762A}, | |
Date-added = {2017-01-18 17:33:21 +0000}, | |
Date-modified = {2017-01-18 17:44:07 +0000}, | |
Eprint = {1701.04762}, | |
Keywords = {Astrophysics - Astrophysics of Galaxies} | |
} | |
@Article{talalexander2017, | |
Title = {{Stellar Dynamics and Stellar Phenomena Near a Massive Black Hole}}, | |
Author = {{Alexander}, T.}, | |
Journal = {\araa}, | |
Year = {2017}, | |
Month = aug, | |
Pages = {17-57}, | |
Volume = {55}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017ARA%26A..55...17A}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1146/annurev-astro-091916-055306}, | |
Eprint = {1701.04762} | |
} | |
@Article{alexander&hopman2009, | |
Title = {{Strong Mass Segregation Around a Massive Black Hole}}, | |
Author = {{Alexander}, T. and {Hopman}, C.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = jun, | |
Pages = {1861-1869}, | |
Volume = {697}, | |
Abstract = {We show that the mass-segregation solution for the | |
steady-state distribution of stars around a massive black | |
hole (MBH) has two branches: the well known | |
weak-segregation solution and a strong segregation | |
solution, which is analyzed here for the first time. The | |
nature of the solution depends on the heavy-to-light | |
stellar mass ratio MH /ML and on the unbound population | |
number ratio NH /NL , through the relaxational coupling | |
parameter Delta = 4NHM 2 H /[NLM 2 L (3 + MH /ML )]. When | |
the heavy stars are relatively common (Delta Gt 1), they | |
scatter frequently on each other. This efficient | |
self-coupling leads to weak mass segregation, where the | |
stars form n∠r^{-alpha_{M}} mass-dependent cusps near | |
the MBH, with indices alpha H = 7/4 for the heavy stars and | |
3/2 < alpha L < 7/4 for the light stars (i.e. max(alpha H - | |
alpha L ) sime 1/4). However, when the heavy stars are | |
relatively rare (Delta Lt 1), they scatter mostly on light | |
stars, sink to the center by dynamical friction and settle | |
into a much steeper cusp with 2 lsim alpha H lsim 11/4, | |
while the light stars form a 3/2 < alpha L < 7/4 cusp, | |
resulting in strong segregation (i.e., max(alpha H - alpha | |
L ) sime 1). We show that the present-day mass function of | |
evolved stellar populations with a universal initial mass | |
function (coeval or continuously star forming) separates | |
into two distinct mass scales, ~1 M sun of main sequence | |
and compact dwarfs, and ~10 M sun of stellar black holes | |
(SBHs), and have Delta < 0.1. We conclude that it is likely | |
that many relaxed galactic nuclei are strongly segregated. | |
We review indications of strong segregation in observations | |
of the Galactic center and in results of numeric | |
simulations, and briefly list possible implications of a | |
very high central concentration of SBHs around an MBH.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...697.1861A}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/0808.3150}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/697/2/1861}, | |
Bdsk-url-2 = {http://arXiv.org/abs/0808.3150}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2009ApJ...697.1861A}, | |
Date-added = {2016-01-25 05:17:01 +0000}, | |
Date-modified = {2016-01-25 05:19:07 +0000}, | |
Doi = {10.1088/0004-637X/697/2/1861}, | |
Eprint = {0808.3150}, | |
Keywords = {black hole physics, Galaxy: kinematics and dynamics, | |
stellar dynamics} | |
} | |
@Article{alexander&kumar2001, | |
Title = {{Tidal Spin-up of Stars in Dense Stellar Cusps around | |
Massive Black Holes}}, | |
Author = {{Alexander}, T. and {Kumar}, P.}, | |
Journal = {\apj}, | |
Year = {2001}, | |
Month = mar, | |
Pages = {948-958}, | |
Volume = {549}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2001ApJ...549..948A}, | |
Doi = {10.1086/319436}, | |
Eprint = {astro-ph/0004240}, | |
Keywords = {Galaxy: Center, Galaxy: Kinematics and Dynamics, Galaxies: | |
Nuclei, Stars: Kinematics, Stars: Rotation}, | |
Owner = {aleksey}, | |
Timestamp = {2017.10.09} | |
} | |
@Article{alexander&morris2003, | |
Title = {{Squeezars: Tidally Powered Stars Orbiting a Massive Black | |
Hole}}, | |
Author = {{Alexander}, T. and {Morris}, M.}, | |
Journal = {\apjl}, | |
Year = {2003}, | |
Month = jun, | |
Pages = {L25-L28}, | |
Volume = {590}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2003ApJ...590L..25A}, | |
Doi = {10.1086/376671}, | |
Eprint = {astro-ph/0305061}, | |
Keywords = {Black Hole Physics, Galaxies: Nuclei, Stars: Kinematics} | |
} | |
@Article{alexander&pfuhl2014, | |
Title = {{Constraining the Dark Cusp in the Galactic Center by | |
Long-period Binaries}}, | |
Author = {{Alexander}, T. and {Pfuhl}, O.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = jan, | |
Pages = {148}, | |
Volume = {780}, | |
Abstract = {Massive black holes (MBHs) in galactic nuclei are believed | |
to be surrounded by a high-density stellar cluster, whose | |
mass is mostly in hard-to-detect faint stars and compact | |
remnants. Such dark cusps dominate the dynamics near the | |
MBH: a dark cusp in the Galactic center (GC) of the Milky | |
Way would strongly affect orbital tests of general | |
relativity there; on cosmic scales, dark cusps set the | |
rates of gravitational wave emission events from compact | |
remnants that spiral into MBHs, and they modify the rates | |
of tidal disruption events, to list only some implications. | |
A recently discovered long-period massive young binary | |
(with period P 12 <~ 1 yr, total mass M_{12}\sim {\cal | |
O}(100\, M_{\odot }), and age T 12 ~ 6 × 106 yr), only | |
~0.1 pc from the Galactic MBH, sets a lower bound on the | |
stellar two-body relaxation timescale there, min t | |
rlxvprop(P 12/M 12)2/3 T 12 ~ 107 yr, and, correspondingly, | |
an upper bound on the stellar number density, \max n_{\star | |
}\sim {few\times }10^{8}/\langle M_{\star }^{2}\rangle | |
\,{pc^{-3}} (\langle M_{\star }^{2}\rangle ^{1/2} is the | |
rms stellar mass), based on the binary's survival against | |
evaporation by the dark cusp. However, a conservative | |
dynamical estimate, the drain limit, implies t_{{rlx}} \gt | |
{\cal O}({10^{8}}\,{yr}). Such massive binaries are thus | |
too short-lived and tightly bound to constrain a dense | |
relaxed dark cusp. We explore here in detail the use of | |
longer-period, less massive, and longer-lived binaries (P | |
12 ~ few yr, M 12 ~ 2-4 M &sun;, T 12 ~ 108-1010 yr), | |
presently just below the detection threshold, for probing | |
the dark cusp and develop the framework for translating | |
their future detections among the giants in the GC into | |
dynamical constraints.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...780..148A}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1308.6638}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/780/2/148}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1308.6638}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014ApJ...780..148A}, | |
Date-added = {2016-10-10 16:15:59 +0000}, | |
Date-modified = {2017-08-08 01:22:36 +0000}, | |
Doi = {10.1088/0004-637X/780/2/148}, | |
Eid = {148}, | |
Eprint = {1308.6638}, | |
Keywords = {binaries: general, black hole physics, Galaxy: center, | |
Galaxy: kinematics and dynamics, infrared: stars, stars: | |
kinematics and dynamics} | |
} | |
@Article{allen+2006, | |
Title = {{The relation between accretion rate and jet power in | |
X-ray luminous elliptical galaxies}}, | |
Author = {{Allen}, S.~W. and {Dunn}, R.~J.~H. and {Fabian}, A.~C. | |
and {Taylor}, G.~B. and {Reynolds}, C.~S.}, | |
Journal = {\mnras}, | |
Year = {2006}, | |
Month = oct, | |
Pages = {21-30}, | |
Volume = {372}, | |
Abstract = {Using Chandra X-ray observations of nine nearby, X-ray | |
luminous elliptical galaxies with good optical velocity | |
dispersion measurements, we show that a tight correlation | |
exists between the Bondi accretion rates calculated from | |
the observed gas temperature and density profiles and | |
estimated black hole masses, and the power emerging from | |
these systems in relativistic jets. The jet powers, which | |
are inferred from the energies and time-scales required to | |
inflate cavities observed in the surrounding X-ray emitting | |
gas, can be related to the accretion rates using a | |
power-law model of the form log(PBondi/1043ergs-1) = A + | |
Blog(Pjet/1043ergs-1), with A = 0.65 +/- 0.16 and B = 0.77 | |
+/- 0.20. Our results show that a significant fraction of | |
the energy associated with the rest mass of material | |
entering the Bondi accretion radius (2.2+1.0-0.7 per cent, | |
for Pjet = 1043ergs-1) eventually emerges in the | |
relativistic jets. The data also hint that this fraction | |
may rise slightly with increasing jet power. Our results | |
have significant implications for studies of accretion, jet | |
formation and galaxy formation. The observed tight | |
correlation suggests that the Bondi formulae provide a | |
reasonable description of the accretion process in these | |
systems, despite the likely presence of magnetic pressure | |
and angular momentum in the accreting gas. The similarity | |
of the PBondi and Pjet values argues that a significant | |
fraction of the matter entering the accretion radius flows | |
down to regions close to the black holes, where the jets | |
are presumably formed. The tight correlation between PBondi | |
and Pjet also suggests that the accretion flows are | |
approximately stable over time-scales of a few million | |
years. Our results show that the black hole `engines' at | |
the hearts of large elliptical galaxies and groups can feed | |
back sufficient energy to stem cooling and star formation, | |
leading naturally to the observed exponential cut off at | |
the bright end of the galaxy luminosity function.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006MNRAS.372...21A}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0602549}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2006.10778.x}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0602549}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2006MNRAS.372...21A}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1111/j.1365-2966.2006.10778.x}, | |
Eprint = {astro-ph/0602549}, | |
Keywords = {accretion, accretion discs: black hole physics: galaxies: | |
active: galaxies: jets: X-rays: galaxies, accretion discs, | |
black hole physics, galaxies: active, galaxies: jets, | |
X-rays: galaxies} | |
} | |
@Article{amaro-seoane+2012, | |
Title = {{eLISA: Astrophysics and cosmology in the millihertz | |
regime}}, | |
Author = {Amaro-Seoane, P and Aoudia, S and Babak, S and | |
Bin\'{e}truy, P}, | |
Journal = {e-print arxiv:1201.3621}, | |
Year = {2012}, | |
Month = jan, | |
Archiveprefix = {arXiv}, | |
Arxivid = {astro-ph.CO/1201.3621}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:36 +0000}, | |
Eprint = {1201.3621}, | |
Keywords = {Astrophysics - Galaxy Astrophysics, General Relativity and | |
Quantum Cosmology,Astrophysics - Cosmology and | |
Extragalactic Astroph; Untitled; Untitled1}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{amaro-seoane&chen2014, | |
Title = {{The Fragmenting Past of the Disk at the Galactic Center: | |
The Culprit for the Missing Red Giants}}, | |
Author = {{Amaro-Seoane}, P. and {Chen}, X.}, | |
Journal = {\apjl}, | |
Year = {2014}, | |
Month = jan, | |
Pages = {L18}, | |
Volume = {781}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...781L..18A}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/2041-8205/781/1/L18}, | |
Date-added = {2017-06-10 02:44:19 +0000}, | |
Date-modified = {2017-06-10 02:44:58 +0000}, | |
Doi = {10.1088/2041-8205/781/1/L18}, | |
Eid = {L18}, | |
Eprint = {1310.0458}, | |
Keywords = {Galaxy: center, Galaxy: kinematics and dynamics, methods: | |
analytical, stars: horizontal-branch} | |
} | |
@Article{andronov+2006, | |
Title = {{Mergers of Close Primordial Binaries}}, | |
Author = {{Andronov}, N. and {Pinsonneault}, M.~H. and {Terndrup}, | |
D.~M.}, | |
Journal = {\apj}, | |
Year = {2006}, | |
Month = aug, | |
Pages = {1160-1178}, | |
Volume = {646}, | |
Abstract = {We study the production of main-sequence mergers of | |
tidally synchronized primordial short-period binaries. The | |
principal ingredients of our calculation are the angular | |
momentum loss rates inferred from the spin-down of open | |
cluster stars and the distribution of binary properties in | |
young open clusters. We compare our results with the | |
expected number of systems that experience mass transfer in | |
the post-main-sequence phases of evolution and compute the | |
uncertainties in the theoretical predictions. We estimate | |
that main-sequence mergers can account for the observed | |
number of single blue stragglers in M67. Applied to the | |
blue straggler population, this implies that such mergers | |
are responsible for about one-quarter of the population of | |
halo blue metal-poor stars and at least one-third of the | |
blue stragglers in open clusters for systems older than 1 | |
Gyr. The observed trends as a function of age are | |
consistent with a saturated angular momentum loss rate for | |
rapidly rotating tidally synchronized systems. The | |
predicted number of blue stragglers from main-sequence | |
mergers alone is comparable to the number observed in | |
globular clusters, indicating that the net effect of | |
dynamical interactions in dense stellar environments is to | |
reduce rather than increase the blue straggler population. | |
A population of subturnoff mergers of order 3%-4% of the | |
upper main sequence population is also predicted for stars | |
older than 4 Gyr, which is roughly comparable to the small | |
population of highly Li-depleted halo dwarfs. Other | |
observational tests are discussed.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006ApJ...646.1160A}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/0509309}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/505127}, | |
Bdsk-url-2 = {http://arxiv.org/abs/astro-ph/0509309}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2006ApJ...646.1160A}, | |
Date-added = {2017-08-08 01:27:10 +0000}, | |
Date-modified = {2017-08-08 01:27:43 +0000}, | |
Doi = {10.1086/505127}, | |
Eprint = {astro-ph/0509309}, | |
Keywords = {Stars: Binaries: Close, Stars: Blue Stragglers, Galaxy: | |
Open Clusters and Associations: Individual: Messier Number: | |
M67, Stars: Evolution} | |
} | |
@Article{antonini2014, | |
Title = {{On the Distribution of Stellar Remnants around Massive | |
Black Holes: Slow Mass Segregation, Star Cluster Inspirals, | |
and Correlated Orbits}}, | |
Author = {{Antonini}, F.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = oct, | |
Pages = {106}, | |
Volume = {794}, | |
Abstract = {We use N-body simulations as well as analytical techniques | |
to study the long-term dynamical evolution of stellar black | |
holes (BHs) at the Galactic center (GC) and to put | |
constraints on their number and mass distribution. Starting | |
from models that have not yet achieved a state of | |
collisional equilibrium, we find that timescales associated | |
with cusp regrowth can be longer than the Hubble time. Our | |
results cast doubts on standard models that postulate high | |
densities of BHs near the GC and motivate studies that | |
start from initial conditions that correspond to | |
well-defined physical models. For the first time, we | |
consider the distribution of BHs in a dissipationless model | |
for the formation of the Milky Way nuclear cluster (NC), in | |
which massive stellar clusters merge to form a compact | |
nucleus. We simulate the consecutive merger of ~10 clusters | |
containing an inner dense sub-cluster of BHs. After the | |
formed NC is evolved for ~5 Gyr, the BHs do form a steep | |
central cusp, while the stellar distribution maintains | |
properties that resemble those of the GC NC. Finally, we | |
investigate the effect of BH perturbations on the motion of | |
the GC S-stars as a means of constraining the number of the | |
perturbers. We find that reproducing the quasi-thermal | |
character of the S-star orbital eccentricities requires >~ | |
1000 BHs within 0.1 pc of Sgr A*. A dissipationless | |
formation scenario for the GC NC is consistent with this | |
lower limit and therefore could reconcile the need for high | |
central densities of BHs (to explain the S-stars orbits) | |
with the "missing-cusp" problem of the GC giant star | |
population.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...794..106A}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1402.4865}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/794/2/106}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1402.4865}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014ApJ...794..106A}, | |
Date-added = {2016-01-25 04:55:30 +0000}, | |
Date-modified = {2016-01-25 04:55:31 +0000}, | |
Doi = {10.1088/0004-637X/794/2/106}, | |
Eid = {106}, | |
Eprint = {1402.4865}, | |
Keywords = {galaxies: nuclei, Galaxy: center, Galaxy: formation, | |
stars: black holes, stars: kinematics and dynamics} | |
} | |
@Article{antonini+2015, | |
Title = {{The Coevolution of Nuclear Star Clusters, Massive Black | |
Holes, and Their Host Galaxies}}, | |
Author = {{Antonini}, F. and {Barausse}, E. and {Silk}, J.}, | |
Journal = {\apj}, | |
Year = {2015}, | |
Month = oct, | |
Pages = {72}, | |
Volume = {812}, | |
Abstract = {Studying how nuclear star clusters (NSCs) form and how | |
they are related to the growth of the central massive black | |
holes (MBHs) and their host galaxies is fundamental for our | |
understanding of the evolution of galaxies and the | |
processes that have shaped their central structures. We | |
present the results of a semi-analytical galaxy formation | |
model that follows the evolution of dark matter halos along | |
merger trees, as well as that of the baryonic components. | |
This model allows us to study the evolution of NSCs in a | |
cosmological context, by taking into account the growth of | |
NSCs due to both dynamical-friction-driven migration of | |
stellar clusters and star formation triggered by infalling | |
gas, while also accounting for dynamical heating from | |
(binary) MBHs. We find that in situ star formation | |
contributes a significant fraction (up to ~80%) of the | |
total mass of NSCs in our model. Both NSC growth through in | |
situ star formation and that through star cluster migration | |
are found to generate NSC---host galaxy scaling | |
correlations that are shallower than the same correlations | |
for MBHs. We explore the role of galaxy mergers on the | |
evolution of NSCs and show that observational data on | |
NSC---host galaxy scaling relations provide evidence of | |
partial erosion of NSCs by MBH binaries in luminous | |
galaxies. We show that this observational feature is | |
reproduced by our models, and we make predictions about the | |
NSC and MBH occupation fraction in galaxies. We conclude by | |
discussing several implications for theories of NSC | |
formation.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015ApJ...812...72A}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1506.02050}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/812/1/72}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1506.02050}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2015ApJ...812...72A}, | |
Date-added = {2017-04-23 20:11:54 +0000}, | |
Date-modified = {2017-04-23 20:11:54 +0000}, | |
Doi = {10.1088/0004-637X/812/1/72}, | |
Eid = {72}, | |
Eprint = {1506.02050}, | |
Keywords = {galaxies: evolution, galaxies: formation, galaxies: | |
nuclei, Galaxy: center, quasars: supermassive black holes} | |
} | |
@Article{antonini+2012, | |
Title = {{Dissipationless Formation and Evolution of the Milky Way Nuclear Star Cluster}}, | |
Author = {{Antonini}, F. and {Capuzzo-Dolcetta}, R. and {Mastrobuono-Battisti}, A. and {Merritt}, D.}, | |
Journal = {\apj}, | |
Year = {2012}, | |
Month = may, | |
Pages = {111}, | |
Volume = {750}, | |
Abstract = {In one widely discussed model for the formation of nuclear star clusters (NSCs), massive globular clusters spiral into the center of a galaxy and merge to form the nucleus. It is now known that at least some NSCs coexist with supermassive black holes (SMBHs); this is the case, for instance, in the Milky Way. In this paper, we investigate how the presence of an SMBH at the center of the Milky Way impacts the merger hypothesis for the formation of its NSC. Starting from a model consisting of a low-density nuclear stellar disk and the SMBH, we use direct N-body simulations to follow the successive inspiral and merger of globular clusters. The clusters are started on circular orbits of radius 20 pc, and their initial masses and radii are set up in such a way as to be consistent with the galactic tidal field at that radius. These clusters, decayed orbitally in the central region due to their large mass, were followed in their inspiral events; as a result, the total accumulated mass by ?10 clusters is about 1.5 × 107 M ?. Each cluster is disrupted by the SMBH at a distance of roughly 1 pc. The density profile that results after the final inspiral event is characterized by a core of roughly this radius and an envelope with density that falls off ? ~ r -2. These properties are similar to those of the Milky Way NSC, with the exception of the core size, which in the Milky Way is somewhat smaller. But by continuing the evolution of the model after the final inspiral event, we find that the core shrinks substantially via gravitational encounters in a time (when scaled to the Milky Way) of 10 Gyr as the stellar distribution evolves toward a Bahcall-Wolf cusp. We also show that the luminosity function of the Milky Way NSC is consistent with the hypothesis that 1/2 of the mass comes from old (~10 Gyr) stars, brought in by globular clusters, with the other half due to continuous star formation. We conclude that a model in which a large fraction of the mass of the Milky Way NSC is due to infalling globular clusters is consistent with existing observational constraints.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012ApJ...750..111A}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1088/0004-637X/750/2/111}, | |
Eid = {111}, | |
Eprint = {1110.5937}, | |
Keywords = {galaxies: nuclei, Galaxy: center, Galaxy: evolution, Galaxy: formation, methods: numerical}, | |
Owner = {aleksey}, | |
Timestamp = {2018.04.19} | |
} | |
@Article{antonini&merritt2011, | |
Title = {{Dynamical Friction around Supermassive Black Holes}}, | |
Author = {{Antonini}, F. and {Merritt}, D.}, | |
Journal = {\apj}, | |
Year = {2012}, | |
Month = jan, | |
Pages = {83}, | |
Volume = {745}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012ApJ...745...83A}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1088/0004-637X/745/1/83}, | |
Eid = {83}, | |
Eprint = {1108.1163}, | |
Keywords = {black hole physics, galaxies: kinematics and dynamics, | |
Galaxy: center, gravitational waves} | |
} | |
@Article{antonini&perets2012, | |
Title = {{Secular Evolution of Compact Binaries near Massive Black | |
Holes: Gravitational Wave Sources and Other Exotica}}, | |
Author = {{Antonini}, F. and {Perets}, H.~B.}, | |
Journal = {\apj}, | |
Year = {2012}, | |
Month = sep, | |
Pages = {27}, | |
Volume = {757}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012ApJ...757...27A}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1088/0004-637X/757/1/27}, | |
Eid = {27}, | |
Eprint = {1203.2938}, | |
Keywords = {binaries: close, Galaxy: center, gravitational waves, | |
stars: kinematics and dynamics}, | |
Owner = {aleksey}, | |
Timestamp = {2017.12.19} | |
} | |
@Article{antonini&rasio2016, | |
Title = {{Merging Black Hole Binaries in Galactic Nuclei: | |
Implications for Advanced-LIGO Detections}}, | |
Author = {{Antonini}, F. and {Rasio}, F.~A.}, | |
Journal = {\apj}, | |
Year = {2016}, | |
Month = nov, | |
Pages = {187}, | |
Volume = {831}, | |
Abstract = {Motivated by the recent detection of gravitational waves | |
from the black hole binary merger GW150914, we study the | |
dynamical evolution of (stellar-mass) black holes in | |
galactic nuclei, where massive star clusters reside. With | |
masses of ˜ {10}7 {M}&sun; and sizes of only a few | |
parsecs, nuclear star clusters (NSCs) are the densest | |
stellar systems observed in the local universe and | |
represent a robust environment where black hole binaries | |
can dynamically form, harden, and merge. We show that due | |
to their large escape speeds, NSCs can retain a large | |
fraction of their merger remnants. Successive mergers can | |
then lead to significant growth and produce black hole | |
mergers of several tens of solar masses similar to GW150914 | |
and up to a few hundreds of solar masses, without the need | |
to invoke extremely low metallicity environments. We use a | |
semi-analytical approach to describe the dynamics of black | |
holes in massive star clusters. Our models give a black | |
hole binary merger rate of ≈ 1.5 {{Gpc}}-3 {{yr}}-1 from | |
NSCs, implying up to a few tens of possible detections per | |
year with Advanced LIGO. Moreover, we find a local merger | |
rate of ˜ 1 {{Gpc}}-3 {{yr}}-1 for high mass black hole | |
binaries similar to GW150914; a merger rate comparable to | |
or higher than that of similar binaries assembled | |
dynamically in globular clusters (GCs). Finally, we show | |
that if all black holes receive high natal kicks, ≳ 50 | |
{km} {{{s}}}-1, then NSCs will dominate the local merger | |
rate of binary black holes compared to either GCs or | |
isolated binary evolution.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016ApJ...831..187A}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1606.04889}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.3847/0004-637X/831/2/187}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1606.04889}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2016ApJ...831..187A}, | |
Date-added = {2017-06-09 20:46:06 +0000}, | |
Date-modified = {2017-06-09 20:46:45 +0000}, | |
Doi = {10.3847/0004-637X/831/2/187}, | |
Eid = {187}, | |
Eprint = {1606.04889}, | |
Keywords = {galaxies: nuclei, gravitational waves, stars: black | |
holes}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{araudo+2009, | |
Title = {{High-energy emission from jet-clump interactions in | |
microquasars}}, | |
Author = {{Araudo}, A.~T. and {Bosch-Ramon}, V. and {Romero}, | |
G.~E.}, | |
Journal = {\aap}, | |
Year = {2009}, | |
Month = sep, | |
Pages = {673-681}, | |
Volume = {503}, | |
Abstract = {Context: High-mass microquasars are binary systems | |
consisting of a massive star and an accreting compact | |
object from which relativistic jets are launched. There is | |
considerable observational evidence that winds of massive | |
stars are clumpy. Individual clumps may interact with the | |
jets in high-mass microquasars to produce outbursts of | |
high-energy emission. Gamma-ray flares have been detected | |
in some high-mass X-ray binaries, such as Cygnus X-1, and | |
probably in LS 5039 and LS I+61 303. Aims: We predict the | |
high-energy emission produced by the interaction between a | |
jet and a clump of the stellar wind in a high-mass | |
microquasar. Methods: Assuming a hydrodynamic scenario for | |
the jet-clump interaction, we calculate the spectral energy | |
distributions produced by the dominant non-thermal | |
processes: relativistic bremsstrahlung, synchrotron and | |
inverse Compton radiation, for leptons, and for hadrons, | |
proton-proton collisions. Results: Significant levels of | |
emission in X-rays (synchrotron), high-energy gamma rays | |
(inverse Compton), and very high-energy gamma rays (from | |
the decay of neutral pions) are predicted, with | |
luminosities in the different domains in the range | |
~1032-1035 erg s-1. The spectral energy distributions vary | |
strongly depending on the specific conditions. Conclusions: | |
Jet-clump interactions may be detectable at high and very | |
high energies, and provide an explanation for the fast TeV | |
variability found in some high-mass X-ray binary systems. | |
Our model can help to infer information about the | |
properties of jets and clumpy winds by means of | |
high-sensitivity gamma-ray astronomy.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009A%26A...503..673A}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/0906.4803}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361/200811519}, | |
Bdsk-url-2 = {http://arxiv.org/abs/0906.4803}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2009A%26A...503..673A}, | |
Date-added = {2016-04-26 01:41:56 +0000}, | |
Date-modified = {2016-04-26 01:41:57 +0000}, | |
Doi = {10.1051/0004-6361/200811519}, | |
Eprint = {0906.4803}, | |
Keywords = {gamma rays: theory, X-rays: binaries, radiation | |
mechanisms: non-thermal}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{arca-sedda+2014, | |
Title = {{The globular cluster migratory origin of nuclear star clusters}}, | |
Author = {{Arca-Sedda}, M. and {Capuzzo-Dolcetta}, R.}, | |
Journal = {\mnras}, | |
Year = {2014}, | |
Month = nov, | |
Pages = {3738-3755}, | |
Volume = {444}, | |
Abstract = {Nuclear star clusters (NSCs) are often present in spiral galaxies as well as resolved stellar nuclei (SNi) in elliptical galaxies centres. Ever growing observational data indicate the existence of correlations between the properties of these very dense central star aggregates and those of host galaxies, which constitute a significant constraint for the validity of theoretical models of their origin and formation. In the framework of the well-known `migratory and merger' model for NSC and SN formation, in this paper we obtain, first, by a simple argument the expected scaling of the NSC/SN mass with both time and parent galaxy velocity dispersion in the case of dynamical friction as dominant effect on the globular cluster system evolution. This generalizes previous results by Tremaine et al. and is in good agreement with available observational data showing a shallow correlation between NSC/SN mass and galactic bulge velocity dispersion. Moreover, we give statistical relevance to predictions of this formation model, obtaining a set of parameters to correlate with the galactic host parameters. We find that the correlations between the masses of NSCs in the migratory model and the global properties of the hosts reproduce quite well the observed correlations, supporting the validity of the migratory-merger model. In particular, one important result is the flattening or even decrease of the value of the NSC/SN mass obtained by the merger model as function of the galaxy mass for high values of the galactic mass, i.e. ?3 × 1011 M?, in agreement with some growing observational evidence.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014MNRAS.444.3738A}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1093/mnras/stu1683}, | |
Eprint = {1405.7593}, | |
Keywords = {methods: numerical, galaxies: nuclei, galaxies: star clusters: general}, | |
Owner = {aleksey}, | |
Timestamp = {2018.04.19} | |
} | |
@Article{arca-sedda+2015, | |
Title = {{Henize 2-10: The Ongoing Formation of a Nuclear Star Cluster around a Massive Black Hole}}, | |
Author = {{Arca-Sedda}, M. and {Capuzzo-Dolcetta}, R. and {Antonini}, F. and {Seth}, A.}, | |
Journal = {\apj}, | |
Year = {2015}, | |
Month = jun, | |
Pages = {220}, | |
Volume = {806}, | |
Abstract = {The central region of the galaxy Henize 2-10 hosts a black hole (BH) candidate with a mass {Log}?ft({M}{BH}/{M}? \right)=6.3+/- 1.1. While this putative BH does not appear to coincide with any central stellar overdensity, it is surrounded by 11 young massive clusters with masses above 105 {M}? . The availability of high-quality data on the structure of the galaxy and the age and mass of the clusters provides excellent initial conditions for studying the dynamical evolution of Henize 2-10's nucleus. Here we present a set of N-body simulations in which we model the future evolution of the central clusters and the BH to understand whether and how they will merge to form a nuclear star cluster (NSC). NSCs are present in a majority of galaxies with stellar mass similar to Henize 2-10. While the results depend on the choice of initial conditions, we find that an NSC with mass {M}{NSC}? 4-6× {10}6 {M}? and effective radius {r}{NSC}? 2.6-4.1 pc will form within 0.2 Gyr. This work is the first showing, in a realistic realization of the host galaxy and its star cluster system, that the formation of a bright nucleus is a process that can happen after the formation of a central massive BH leading to a composite NSC+BH central system. The cluster merging process does not significantly affect the kinematics of the BH; when a stationary state is reached, its position changes by ? 1 pc and its velocity by \lt 2 km s-1.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015ApJ...806..220A}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1088/0004-637X/806/2/220}, | |
Eid = {220}, | |
Eprint = {1501.04567}, | |
Keywords = {galaxies: individual: Henize 2{\ndash}10, galaxies: nuclei, galaxies: star clusters: general, methods: numerical}, | |
Owner = {aleksey}, | |
Timestamp = {2018.04.19} | |
} | |
@Article{arca-sedda+2017, | |
Title = {{Gamma-ray and X-ray emission from the Galactic Centre: hints on the nuclear star cluster formation history}}, | |
Author = {{Arca-Sedda}, M. and {Kocsis}, B. and {Brandt}, T.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2017}, | |
Month = sep, | |
Abstract = {The Milky Way centre exhibits an intense flux in the gamma and X-ray bands, whose origin is partly ascribed to the possible presence of a large population of millisecond pulsars (MSPs) and cataclysmic variables (CVs), respectively. However, the number of sources required to generate such an excess is much larger than what is expected from in situ star formation and evolution, opening a series of questions about the formation history of the Galactic nucleus. In this paper we make use of direct $N$-body simulations to investigate whether these sources could have been brought to the Galactic centre by a population of star clusters that underwent orbital decay and formed the Galactic nuclear star cluster (NSC). Our results suggest that the gamma ray emission is compatible with a population of MSPs that were mass segregated in their parent clusters, while the X-ray emission is consistent with a population of CVs born via dynamical interactions in dense star clusters. Combining observations with our modelling, we explore how the observed $\gamma$ ray flux can be related to different NSC formation scenarios. Finally, we show that the high-energy emission coming from the galactic central regions can be used to detect black holes heavier than $10^5\Ms$ in nearby dwarf galaxies.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017arXiv170903119A}, | |
Archiveprefix = {arXiv}, | |
Eprint = {1709.03119}, | |
Keywords = {Astrophysics - Astrophysics of Galaxies}, | |
Owner = {aleksey}, | |
Timestamp = {2018.06.07} | |
} | |
@Article{arca-sedda+2018, | |
Title = {{Ordering the chaos: stellar black hole mergers from non-hierarchical triples}}, | |
Author = {{Arca-Sedda}, M. and {Li}, G. and {Kocsis}, B.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2018}, | |
Month = may, | |
Abstract = {We investigate the evolution of triple, non-hierarchical, black hole (BH) systems making use of 29,000 3-body simulations. Varying the mutual orbital inclination, the three BH masses and the inner and outer eccentricities, we show that retrograde, nearly planar configurations leads to a significant shrinkage of the inner binary. We found an universal trend of triple systems, that they tend to evolve toward prograde configurations, independently on the initial conditions. Moreover, we demonstrate that the orbital flip, driven by the torque exerted from the outer BH on the inner binary (BHB), leads in general to tighter inner orbits. In some cases, the resulting BHB undergoes coalescence within a Hubble time, releasing gravitational waves (GWs). Frequently, the inner BHB merger occurs after a component swap between one of its components and the outer BH. The mass spectrum of the BHBs that underwent the component exchange differs significantly from the case in which the BHB merge without any swap. A large fraction of merging BHBs with initial separation 1 AU enter the 0.001-0.1 Hz frequency band with large eccentricities, possibly being detected by the next generation of detectors. Mergers originating from initially tighter BHB (a ~ 0.01 AU), instead, have a large probability to have eccentricities above 0.7 in the 1 Hz band. Intriguingly, we found that the chirp mass of at least 3 of the GW sources detected by LIGO (GW150914, GW170814 and GW170104) lie in the most probable range of chirp masses for coalescing BHBs formed in a non-hierarchical triple.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2018arXiv180506458A}, | |
Archiveprefix = {arXiv}, | |
Eprint = {1805.06458}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2018.06.05} | |
} | |
@Article{arcavi+2014, | |
Title = {{A Continuum of H- to He-rich Tidal Disruption Candidates | |
With a Preference for E+A Galaxies}}, | |
Author = {{Arcavi}, I. and {Gal-Yam}, A. and {Sullivan}, M. and | |
{Pan}, Y.-C. and {Cenko}, S.~B. and {Horesh}, A. and | |
{Ofek}, E.~O. and {De Cia}, A. and {Yan}, L. and {Yang}, | |
C.-W. and {Howell}, D.~A. and {Tal}, D. and {Kulkarni}, | |
S.~R. and {Tendulkar}, S.~P. and {Tang}, S. and {Xu}, D. | |
and {Sternberg}, A. and {Cohen}, J.~G. and {Bloom}, J.~S. | |
and {Nugent}, P.~E. and {Kasliwal}, M.~M. and {Perley}, | |
D.~A. and {Quimby}, R.~M. and {Miller}, A.~A. and | |
{Theissen}, C.~A. and {Laher}, R.~R.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = sep, | |
Pages = {38}, | |
Volume = {793}, | |
Abstract = {We present the results of a Palomar Transient Factory | |
(PTF) archival search for blue transients that lie in the | |
magnitude range between "normal" core-collapse and | |
superluminous supernovae (i.e., with -21 <= M R (peak) <= - | |
19). Of the six events found after excluding all | |
interacting Type IIn and Ia-CSM supernovae, three (PTF09ge, | |
09axc, and 09djl) are coincident with the centers of their | |
hosts, one (10iam) is offset from the center, and a precise | |
offset cannot be determined for two (10nuj and 11glr). All | |
the central events have similar rise times to the He-rich | |
tidal disruption candidate PS1-10jh, and the event with the | |
best-sampled light curve also has similar colors and | |
power-law decay. Spectroscopically, PTF09ge is He-rich, | |
while PTF09axc and 09djl display broad hydrogen features | |
around peak magnitude. All three central events are in low | |
star formation hosts, two of which are E+A galaxies. Our | |
spectrum of the host of PS1-10jh displays similar | |
properties. PTF10iam, the one offset event, is different | |
photometrically and spectroscopically from the central | |
events, and its host displays a higher star formation rate. | |
Finding no obvious evidence for ongoing galactic nuclei | |
activity or recent star formation, we conclude that the | |
three central transients likely arise from the tidal | |
disruption of a star by a supermassive black hole. We | |
compare the spectra of these events to tidal disruption | |
candidates from the literature and find that all of these | |
objects can be unified on a continuous scale of spectral | |
properties. The accumulated evidence of this expanded | |
sample strongly supports a tidal disruption origin for this | |
class of nuclear transients.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...793...38A}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1405.1415}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/793/1/38}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1405.1415}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014ApJ...793...38A}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1088/0004-637X/793/1/38}, | |
Eid = {38}, | |
Eprint = {1405.1415}, | |
Keywords = {accretion, accretion disks, galaxies: nuclei, quasars: | |
supermassive black holes}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{armas-padilla+2014, | |
Title = {{Swift J1357.2-0933: the faintest black hole?}}, | |
Author = {{Armas Padilla}, M. and {Wijnands}, R. and {Degenaar}, N. | |
and {Mu{\~n}oz-Darias}, T. and {Casares}, J. and {Fender}, | |
R.~P.}, | |
Journal = {\mnras}, | |
Year = {2014}, | |
Month = oct, | |
Pages = {902-905}, | |
Volume = {444}, | |
Abstract = {Swift J1357.2-0933 is a confirmed very faint black hole | |
X-ray transient and has a short estimated orbital period of | |
2.8 h. We observed Swift J1357.2-0933 for ˜50 ks with | |
XMM-Newton in 2013 July during its quiescent state. The | |
source is clearly detected at a 0.5-10 keV unabsorbed flux | |
of ˜3 × 10-15 erg cm-2 s-1. If the source is located at a | |
distance of 1.5 kpc (as suggested in the literature), this | |
would imply a luminosity of ˜8 × 1029 erg s-1, making it | |
the faintest detected quiescent black hole low-mass X-ray | |
binary. This would also imply that there is no indication | |
of a reversal in the quiescence X-ray luminosity versus | |
orbital period diagram down to 2.8 h, as has been predicted | |
theoretically and recently supported by the detection of | |
the 2.4 h orbital period black hole MAXI J1659-152 at a | |
0.5-10 keV X-ray luminosity of ˜1.2 × 1031 erg s-1. | |
However, there is considerable uncertainty in the distance | |
of Swift J1357.2-0933 and it may be as distant as 6.3 kpc. | |
In this case, its quiescent luminosity would be LX ˜ 1.3 | |
× 1031 erg s-1, i.e. similar to MAXI J1659-152 and hence, | |
it would support the existence of such a bifurcation | |
period. We also detected the source in optical at r' ˜ | |
22.3 mag with the Liverpool telescope, simultaneously to | |
our X-ray observation. The X-ray/optical luminosity ratio | |
of Swift J1357.2-0933 agrees with the expected value for a | |
black hole at this range of quiescent X-ray luminosities.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014MNRAS.444..902A}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1404.2134}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stu1487}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1404.2134}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014MNRAS.444..902A}, | |
Date-added = {2017-08-14 18:29:23 +0000}, | |
Date-modified = {2017-08-14 18:29:23 +0000}, | |
Doi = {10.1093/mnras/stu1487}, | |
Eprint = {1404.2134}, | |
Keywords = {accretion, accretion discs, black hole physics, stars: | |
individual: Swift J1357.2-0933, X-rays: binaries}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{armitage+2005, | |
Title = {{Eccentricity of Supermassive Black Hole Binaries | |
Coalescing from Gas-rich Mergers}}, | |
Author = {Armitage, P.\~{}J. and Natarajan, P}, | |
Journal = {\apj}, | |
Year = {2005}, | |
Month = dec, | |
Pages = {921--927}, | |
Volume = {634}, | |
Abstract = {Angular momentum loss to circumbinary gas provides a | |
possible mechanism for overcoming the ``last parsec'' | |
problem and allowing the most massive black hole binaries | |
formed from galactic mergers to coalesce. Here we show that | |
if gas disks also catalyze the merger of the somewhat lower | |
mass binaries detectable with the Laser Interferometer | |
Space Antenna (LISA), then there may be a purely | |
gravitational wave signature of the role of gas in the form | |
of a small but finite eccentricity just prior to merger. | |
Numerical simulations suggest that eccentricity, excited by | |
the interaction between the binary and surrounding gas | |
disk, is only partially damped during the final phase of | |
gravitational radiation-driven inspiral. We estimate a | |
typical eccentricity at 1 week prior to coalescence of | |
e\~{}0.01. Higher terminal eccentricities, which can | |
approach e=0.1, are possible if the binary has an extreme | |
mass ratio. The detection of even a small eccentricity | |
prior to merger by LISA provides a possible discriminant | |
between gas-driven inspirals and those effected by stellar | |
processes.}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/497108}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/497108}, | |
Keywords = {Accretion Disks, Black Hole Physics, Galaxies: Active, | |
Galaxies: Nuclei, Gravitational Waves,Accretion; Untitled; | |
Untitled1} | |
} | |
@Article{armitage+2002, | |
Title = {{Accretion during the Merger of Supermassive Black | |
Holes}}, | |
Author = {Armitage, P.\~{}J. and Natarajan, P}, | |
Journal = {\apjl}, | |
Year = {2002}, | |
Month = mar, | |
Pages = {L9--L12}, | |
Volume = {567}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/339770}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/339770}, | |
Keywords = {Accretion Disks, Black Hole Physics, Galaxies: Active, | |
Galaxies: Nuclei, Galaxies: Quasars: General, Gravitational | |
Waves,Accretion; Untitled; Untitled1} | |
} | |
@Article{armitage+2005a, | |
Title = {{Eccentricity of Supermassive Black Hole Binaries | |
Coalescing from Gas-rich Mergers}}, | |
Author = {{Armitage}, P.~J. and {Natarajan}, P.}, | |
Journal = {\apj}, | |
Year = {2005}, | |
Month = dec, | |
Pages = {921-927}, | |
Volume = {634}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005ApJ...634..921A}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/497108}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/497108}, | |
Eprint = {arXiv:astro-ph/0508493}, | |
Keywords = {Accretion, Accretion Disks, Black Hole Physics, Galaxies: | |
Active, Galaxies: Nuclei, Gravitational Waves; Untitled; | |
Untitled1} | |
} | |
@Article{armitage+2002a, | |
Title = {{Accretion during the Merger of Supermassive Black | |
Holes}}, | |
Author = {{Armitage}, P.~J. and {Natarajan}, P.}, | |
Journal = {\apjl}, | |
Year = {2002}, | |
Month = mar, | |
Pages = {L9-L12}, | |
Volume = {567}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2002ApJ...567L...9A}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/339770}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/339770}, | |
Eprint = {arXiv:astro-ph/0201318}, | |
Keywords = {Accretion, Accretion Disks, Black Hole Physics, Galaxies: | |
Active, Galaxies: Nuclei, Gravitational Waves, Galaxies: | |
Quasars: General; Untitled; Untitled1} | |
} | |
@Article{artymowicz1993, | |
Title = {{On the Wave Excitation and a Generalized Torque Formula | |
for Lindblad Resonances Excited by External Potential}}, | |
Author = {Artymowicz, Pawel}, | |
Journal = {Astrophysical Journal v.419}, | |
Year = {1993}, | |
Month = dec, | |
Pages = {155}, | |
Volume = {419}, | |
Abstract = {The existing theory of density wave excitation in | |
two-dimensional gaseous disks by imposed gravitational | |
potentials makes approximations which prevent a direct | |
analytical description of the shifts in effective positions | |
of Lindblad resonances with respect to radii satisfying | |
orbital commensurability requirement, and of the so-called | |
torque cutoff arising at large azimuthal numbers m of the | |
perturbing potential's pattern. Both phenomena are related | |
to the azimuthal forces acting on gas, neglected in the WKB | |
approximation commonly used in the past. We extend previous | |
theories of Lindblad resonance wherever necessary for a | |
consistent analytical treatment of the problem, | |
particularly for large m. Our analytical approach applies | |
to wave excitation at Lindblad resonances in | |
non-self-gravitating, two-dimensional gas layers | |
(vertically averaged disks or fundamental vertical mode of | |
three-dimensional disks). It explicitly includes the | |
resonance shifts and torque cutoffs. The theory is valid | |
for small perturbing potentials of arbitrary form | |
(including highly localized potentials, e.g., point-mass | |
potential, spiral potential with arbitrary pitch angle, | |
etc.). We present a torque formula generalizing the | |
standard Goldreich-Tremaine formula. Especially useful in | |
the problem of disk-satellite interaction, the torque | |
formula provides insight into the origin of the torque | |
cutoff at m larger than the radius to thickness ratio of | |
the disk. Qualitatively, the cutoff is an effect of: (i) a | |
mild (power-law) intrinsic torque cutoff, independent of | |
the radial profile of the imposed potential, and (ii) a | |
sharp (exponential) cutoff due to shifts in effective | |
resonance location away from the perturber. For m → ∞ | |
the latter effect causes the increasingly localized | |
potential to decouple spatially from the wave generation | |
region. A disk annulus surrounding the corotation radius of | |
every m-armed potential, of width comparable with twice the | |
vertical disk scale height, remains evanescent for waves | |
excited by that harmonic and does not contribute | |
significantly to the total torque between the perturber and | |
the disk. We discuss the role of gas viscosity, | |
self-gravity, and the applicability of a two-dimensional | |
analysis to Lindblad resonances in three-dimensional | |
disks.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=1993ApJ...419..155A%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1086/173469}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/173469}, | |
Keywords = {GALAXIES: KINEMATICS AND DYNAMICS, SOLAR SYSTEM: | |
FORMATION,HYDRODYNAMICS}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=1993ApJ...419..155A\&link\_type=ABSTRACT} | |
} | |
@Article{artymowicz1993a, | |
Title = {{Disk-Satellite Interaction via Density Waves and the | |
Eccentricity Evolution of Bodies Embedded in Disks}}, | |
Author = {Artymowicz, Pawel}, | |
Journal = {Astrophysical Journal v.419}, | |
Year = {1993}, | |
Month = dec, | |
Pages = {166}, | |
Volume = {419}, | |
Abstract = {Using a generalized torque formula for Lindblad resonances | |
in non-self-gravitating gaseous disks we study the | |
interaction of disks with small, embedded bodies (not able | |
to open a gap). For satellites on circular orbits, the | |
generalized torque formula reproduces exactly the torque | |
cutoff occurring at high azimuthal number m of the | |
potential harmonics, originally found seminumerically by | |
Goldreich \{\&\} Tremaine (1980) in the shearing | |
coordinates representation. The cutoff is attributable to | |
the shift in the effective Lindblad resonance position with | |
respect to the nominal resonant radius given by the usual | |
period commensurabilty requirement. We apply the theory to | |
the problem of orbital eccentricity evolution of embedded | |
satellites. We relax some of the assumptions implicit in | |
previous calculations related to this problem, most | |
importantly that of a spatially smooth perturbing | |
potential. We treat the co-orbital and the external | |
Lindblad resonances within a unified formalism. We | |
calculate the total rate of eccentricity damping due to | |
co-orbital resonances and the excitation due to external | |
resonances, the former exceeding the latter by a factor | |
roughly equal to 3, independent of the method of averaging | |
over the vertical disk structure. In application to a solar | |
nebula with embedded planetesimals, the timescales of | |
eccentricity damping for a wide range of planetesimal | |
masses are much shorter than those corresponding to either | |
gas drag, planetesimal growth, or nebular lifetime, and | |
thus relevant to the scenarios of planetary system | |
formation. In application to large (radius > 10 m) | |
particles in Saturn's rings we estimate that the | |
eccentricity is damped on the orbital timescale}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=1993ApJ...419..166A%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1086/173470}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/173470}, | |
Keywords = {PLANETS AND SATELLITES: GENERAL, SOLAR SYSTEM: | |
GENERAL,HYDRODYNAMICS}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=1993ApJ...419..166A\&link\_type=ABSTRACT} | |
} | |
@Article{artymowicz+1991, | |
Title = {{The effect of an external disk on the orbital elements of | |
a central binary}}, | |
Author = {{Artymowicz}, P. and {Clarke}, C.~J. and {Lubow}, S.~H. | |
and {Pringle}, J.~E.}, | |
Journal = {\apjl}, | |
Year = {1991}, | |
Month = mar, | |
Pages = {L35-L38}, | |
Volume = {370}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1991ApJ...370L..35A}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/185971}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/185971}, | |
Keywords = {BINARY STARS, STELLAR EVOLUTION, STELLAR ORBITS, ACCRETION | |
DISKS, ECCENTRICITY, GRAVITATIONAL EFFECTS, STELLAR MASS, | |
STELLAR MODELS} | |
} | |
@Article{artymowicz+1996, | |
Title = {{Mass Flow through Gaps in Circumbinary Disks}}, | |
Author = {Artymowicz, P and Lubow, S.\~{}H.}, | |
Journal = {\apjl}, | |
Year = {1996}, | |
Month = aug, | |
Pages = {L77}, | |
Volume = {467}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/310200}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/310200}, | |
Keywords = {ACCRETION DISKS, GALAXIES: NUCLEI, SOLAR SYSTEM: | |
FORMATION, STARS: AGB AND POST-AGB, STARS: BINARIES: CLOSE, | |
STARS: PLANETARY SYSTEMS, STARS: | |
PRE-MAIN-SEQUENCE,ACCRETION; Untitled; Untitled1} | |
} | |
@Article{artymowicz+1994a, | |
Title = {{Dynamics of binary-disk interaction. 1: Resonances and | |
disk gap sizes}}, | |
Author = {Artymowicz, Pawel and Lubow, Stephen H}, | |
Journal = {Astrophysical Journal}, | |
Year = {1994}, | |
Month = feb, | |
Pages = {651}, | |
Volume = {421}, | |
Abstract = {We investigate the gravitational interaction of a | |
generally eccentric binary star system with circumbinary | |
and circumstellar gaseous disks. The disks are assumed to | |
be coplanar with the binary, geometrically thin, and | |
primarily governed by gas pressure and (turbulent) | |
viscosity but not self-gravity. Both ordinary and eccentric | |
Lindblad resonances are primarily responsible for | |
truncating the disks in binaries with arbitrary | |
eccentricity and nonextreme mass ratio. Starting from a | |
smooth disk configuration, after the gravitational field of | |
the binary truncates the disk on the dynamical timescale, a | |
quasi-equilibrium is achieved, in which the resonant and | |
viscous torques balance each other and any changes in the | |
structure of the disk (e.g., due to global viscous | |
evolution) occur slowly, preserving the average size of the | |
gap. We analytically compute the approximate sizes of disks | |
(or disk gaps) as a function of binary mass ratio and | |
eccentricity in this quasi-equilibrium. Comparing the gap | |
sizes with results of direct simulations using the smoothed | |
particle hydrodynamics (SPH), we obtain a good agreement. | |
As a by-product of the computations, we verify that | |
standard SPH codes can adequately represent the dynamics of | |
disks with moderate viscosity, Reynolds number R | |
approximately 103. For typical viscous disk parameters, and | |
with a denoting the binary semimajor axis, the inner edge | |
location of a circumbinary disk varies from 1.8a to 2.6a | |
with binary eccentricity increasing from 0 to 0.25. For | |
eccentricities 0 less than e less than 0.75, the minimum | |
separation between a component star and the circumbinary | |
disk inner edge is greater than a. Our calculations are | |
relevant, among others, to protobinary stars and the | |
recently discovered T Tau pre-main-sequence binaries. We | |
briefly examine the case of a pre-main-sequence | |
spectroscopic binary GW Ori and conclude that circumbinary | |
disk truncation to the size required by one proposed | |
spectroscopic model cannot be due to Linblad resonances, | |
even if the disk is nonviscous.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=1994ApJ...421..651A%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1086/173679}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/173679}, | |
Keywords = {Accretion Disks, BINARY STARS, ORBITAL RESONANCES | |
(CELESTIAL MECHANICS), PRE-MAIN SEQUENCE STARS, STELLAR | |
ENVELOPES, STELLAR GRAVITATION, STELLAR MASS ACCRETION, | |
STELLAR MODELS, STELLAR SPECTRA, STELLAR | |
SYSTEMS,ASTRONOMICAL SPECTROSCOPY; Untitled; Untitled1}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=1994ApJ...421..651A\&link\_type=ABSTRACT} | |
} | |
@Article{artymowicz+1992, | |
Title = {{Dynamics of ultraharmonic resonances in spiral | |
galaxies}}, | |
Author = {Artymowicz, Pawel and Lubow, Stephen H}, | |
Journal = {Astrophysical Journal}, | |
Year = {1992}, | |
Month = apr, | |
Pages = {129}, | |
Volume = {389}, | |
Abstract = {The mildly nonlinear response of a fluid disk with | |
pressure, viscosity, and self-gravity to spiral stellar | |
forcing is considered as a model of the interstellar medium | |
in spiral galaxies. Nonlinear effects are analyzed through | |
a quasi-linear flow analysis ordered by successive powers | |
of a dimensionless spiral perturbing force, which is the | |
ratio of imposed nonaxisymmetric gravitational to | |
axisymmetric gravitational forces. Waves with mn arms are | |
launched from a position where the wavenumber of a free | |
wave matches n times the wavenumber of the spiral forcing. | |
The launched short wave in the gas is an interarm feature | |
that is more tightly wrapped than the stellar wave. The gas | |
wave extracts energy and angular momentum from the stellar | |
wave, causing it to damp. The application of the results to | |
the stellar disk alone reveals even stronger damping, as | |
stars undergo Landau damping of the short wave. For | |
parameters in M81, damping times are less than 10 exp 9 | |
yr.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=1992ApJ...389..129A%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1086/171192}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/171192}, | |
Keywords = {DENSITY WAVE MODEL, HARMONIC OSCILLATION, HYDRODYNAMICS, | |
INTERSTELLAR GAS, LANDAU DAMPING, POISSON EQUATION, | |
RESONANCE, SPIRAL GALAXIES, STELLAR MOTIONS,GRAVITATIONAL | |
FIELDS}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=1992ApJ...389..129A\&link\_type=ABSTRACT} | |
} | |
@Article{askar+2018, | |
Title = {{MOCCA-SURVEY Database I: Galactic Globular Clusters Harbouring a Black Hole Subsystem}}, | |
Author = {{Askar}, A. and {Arca Sedda}, M. and {Giersz}, M.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2018}, | |
Month = feb, | |
Abstract = {There has been increasing theoretical and observational speculation that certain globular clusters (GCs) could contain a sizeable population of stellar mass black holes (BHs). In this paper, we shortlist at least 29 Galactic GCs that could be hosting a subsystem of BHs (BHS). In a companion paper, we analysed results from a wide array of GC models (simulated with the MOCCA code for cluster simulations) that retained few tens to several hundreds of BHs at 12 Gyr and showed that the properties of the BHS in those GCs correlate with the GC's observable properties. Building on those results, we use available observational properties of 140 Galactic GCs to identify 29 GCs that could potentially be harbouring up to few hundreds of BHs. Utilizing observational properties and theoretical scaling relations, we estimate the density, size and mass of the BHS in these GCs. We also provide numbers for the total BH population and the number of BHs in binary systems that are contained within these GCs. Additionally, we mention other Galactic GCs that could also contain significant number of single BHs or BHs in binary systems.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2018arXiv180205284A}, | |
Archiveprefix = {arXiv}, | |
Eprint = {1802.05284}, | |
Keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics}, | |
Owner = {aleksey}, | |
Timestamp = {2018.04.19} | |
} | |
@Article{askar+2018a, | |
Title = {{MOCCA-SURVEY Database I: Galactic Globular Clusters Harbouring a Black Hole Subsystem}}, | |
Author = {{Askar}, A. and {Sedda}, M.~A. and {Giersz}, M.}, | |
Journal = {\mnras}, | |
Year = {2018}, | |
Month = may, | |
Abstract = {There have been increasing theoretical speculations and observational indications that certain globular clusters (GCs) could contain a sizeable population of stellar mass black holes (BHs). In this paper, we shortlist at least 29 Galactic GCs that could be hosting a subsystem of BHs (BHS). In a companion paper, we analysed results from a wide array of GC models (simulated with the MOCCA code for cluster simulations) that retained few tens to several hundreds of BHs at 12 Gyr and showed that the properties of the BHS in those GCs correlate with the GC's observable properties. Building on those results, we use available observational properties of 140 Galactic GCs to identify 29 GCs that could potentially be harbouring up to a few hundreds of BHs. Utilizing observational properties and theoretical scaling relations, we estimate the density, size and mass of the BHS in these GCs. We also calculate the total number of BHs and the fraction of BHs contained in a binary system for our shortlisted Galactic GCs. Additionally, we mention other Galactic GCs that could also contain significant number of single BHs or BHs in binary systems.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2018MNRAS.tmp.1131A}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1093/mnras/sty1186}, | |
Eprint = {1802.05284}, | |
Keywords = {globular clusters: general, stars: black holes, methods: numerical}, | |
Owner = {aleksey}, | |
Timestamp = {2018.06.11} | |
} | |
@Article{auchettl+2017, | |
Title = {{New Physical Insights about Tidal Disruption Events from | |
a Comprehensive Observational Inventory at X-Ray | |
Wavelengths}}, | |
Author = {{Auchettl}, K. and {Guillochon}, J. and {Ramirez-Ruiz}, | |
E.}, | |
Journal = {\apj}, | |
Year = {2017}, | |
Month = apr, | |
Pages = {149}, | |
Volume = {838}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017ApJ...838..149A}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/1538-4357/aa633b}, | |
Eid = {149}, | |
Eprint = {1611.02291}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: | |
active, X-rays: general}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2017.11.09} | |
} | |
@Article{bade+1996, | |
Title = {{Detection of an extremely soft X-ray outburst in the | |
HII-like nucleus of NGC 5905.}}, | |
Author = {{Bade}, N. and {Komossa}, S. and {Dahlem}, M.}, | |
Journal = {\aap}, | |
Year = {1996}, | |
Month = may, | |
Pages = {L35-L38}, | |
Volume = {309}, | |
Abstract = {NGC 5905 was observed with ROSAT five times, three times | |
during the ROSAT all-sky survey (RASS) and twice in the | |
pointed observing mode. The soft X-ray properties of the | |
nucleus of NGC 5905 derived from the RASS observations, | |
namely high-amplitude flux variability on timescales of | |
days, the extremely soft spectrum (photon index {GAMMA}=4), | |
and high peak luminosity of L_X_=7x10^42^ergs/s, are all | |
inconsistent with its optical classification as HII-type, | |
i.e. starburst galaxy. During the pointed observations | |
taken two years later, the X-ray luminosity was down by a | |
factor of >80. Possible mechanisms, which can produce the | |
high state, are discussed. Tidal disruption of a star near | |
a central black hole is in good agreement with the | |
observations.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1996A%26A...309L..35B}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/abs/1996A%26A...309L..35B}, | |
Date-added = {2016-03-17 17:17:32 +0000}, | |
Date-modified = {2016-03-17 17:17:32 +0000}, | |
Keywords = {GALAXIES: GENERAL, GALAXIES: STARBURST, GALAXIES: | |
INDIVIDUAL: NGC5905, QUASARS: GENERAL, X-RAYS: GALAXIES} | |
} | |
@Article{baganoff+2003, | |
Title = {{Chandra X-Ray Spectroscopic Imaging of Sagittarius A* and | |
the Central Parsec of the Galaxy}}, | |
Author = {{Baganoff}, F.~K. and {Maeda}, Y. and {Morris}, M. and | |
{Bautz}, M.~W. and {Brandt}, W.~N. and {Cui}, W. and | |
{Doty}, J.~P. and {Feigelson}, E.~D. and {Garmire}, G.~P. | |
and {Pravdo}, S.~H. and {Ricker}, G.~R. and {Townsley}, | |
L.~K.}, | |
Journal = {\apj}, | |
Year = {2003}, | |
Month = jul, | |
Pages = {891-915}, | |
Volume = {591}, | |
Abstract = {We report the results of the first-epoch observation with | |
the ACIS-I instrument on the Chandra X-Ray Observatory of | |
Sagittarius A* (Sgr A*), the compact radio source | |
associated with the supermassive black hole (SMBH) at the | |
dynamical center of the Milky Way. This observation | |
produced the first X-ray (0.5-7 keV) spectroscopic image | |
with arcsecond resolution of the central 17'×17' | |
(40pc×40pc) of the Galaxy. We report the discovery of an | |
X-ray source, CXOGC J174540.0-290027, coincident with Sgr | |
A* within 0.27"+/-0.18". The probability of a false match | |
is estimated to be <~0.5%. The spectrum is well fitted | |
either by an absorbed power law with photon index Gamma~2.7 | |
or by an absorbed optically thin thermal plasma with kT~1.9 | |
keV and column density NH~1×1023 cm-2. The observed flux | |
in the 2-10 keV band is ~1.3×10-13 ergs cm-2 s-1, and the | |
absorption-corrected luminosity is ~2.4×1033 ergs s-1. The | |
X-ray emission at the position of Sgr A* is extended, with | |
an intrinsic size of ~1.4" (FWHM), consistent with the | |
Bondi accretion radius for a 2.6×106 Msolar black hole. A | |
compact component within the source flared by up to a | |
factor of 3 over a period of ~1 hr at the start of the | |
observation. The search for Kalpha line emission from iron | |
was inconclusive, yielding an upper limit on the equivalent | |
width of 2.2 keV. Several potential stellar origins for the | |
X-ray emission at Sgr A* are considered, but we conclude | |
that the various properties of the source favor accretion | |
onto the SMBH as the origin for the bulk of the emission. | |
These data are inconsistent with ``standard'' | |
advection-dominated accretion flow (ADAF) models or Bondi | |
models, unless the accretion rate from stellar winds is | |
much lower than anticipated. The central parsec of the | |
Galaxy contains an ~1.3 keV plasma with electron density | |
ne~26eta-1/2fcm-3, where etaf is the filling factor. This | |
plasma should supply ~10-6 Msolar yr-1 of material to the | |
accretion flow at the Bondi radius, whereas measurements of | |
linear polarization at 150 GHz and above limit the | |
accretion rate near the event horizon to <~10-8 Msolar | |
yr-1, assuming an equipartition magnetic field. Taken | |
together, the X-ray and radio results imply that outflows | |
or convection are playing a role in ADAF models and | |
subequipartition magnetic fields in Bondi models, or else | |
the X-ray emission must be generated predominantly via the | |
synchrotron self-Compton (SSC) process. The measured extent | |
of the source and the detection of short timescale | |
variability are evidence that the emission from Sgr A* | |
contains both thermal and nonthermal emission components at | |
comparable levels. We also discuss the complex structure of | |
the X-ray emission from the Sgr A radio complex and along | |
the Galactic plane. Morphological evidence is presented | |
that Sgr A* and the H II region Sgr A West lie within the | |
hot plasma in the central cavity of Sgr A East, which we | |
interpret as a supernova remnant that may have passed | |
through the position of the SMBH, leading to a period of | |
increased activity that ended within the past ~300 yr. | |
Similarly, we have discovered bright clumps of X-ray | |
emission located on opposite sides of the Galactic plane, | |
along a line passing through the central parsec of the | |
Galaxy. The arrangement of these lobes suggests that Sgr A* | |
may have experienced an earlier period of increased | |
activity lasting several thousand years during which it | |
expelled hot gas in a bipolar outflow oriented roughly | |
perpendicular to the Galactic plane. Additionally, we | |
present an analysis of stellar emission within the central | |
parsec of the Galaxy.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2003ApJ...591..891B}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0102151}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/375145}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0102151}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2003ApJ...591..891B}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/375145}, | |
Eprint = {astro-ph/0102151}, | |
Keywords = {Accretion, Accretion Disks, Black Hole Physics, Galaxies: | |
Active, Galaxy: Center, X-Rays: ISM, X-Rays: Stars} | |
} | |
@Article{bahcall&wolf1977, | |
Title = {{The star distribution around a massive black hole in a | |
globular cluster. II Unequal star masses}}, | |
Author = {{Bahcall}, J.~N. and {Wolf}, R.~A.}, | |
Journal = {\apj}, | |
Year = {1977}, | |
Month = sep, | |
Pages = {883-907}, | |
Volume = {216}, | |
Abstract = {The steady-state distribution of stars around a massive | |
black hole in a globular cluster is determined by solving | |
numerically the coupled time-dependent Boltzmann equations | |
for a system containing stars of two different masses. | |
Similar results are found for an arbitrary spectrum of | |
masses with the aid of approximate analytic solutions of | |
the time-independent equations. The effects of mass | |
segregation are summarized by scaling laws that are derived | |
both by analytic approximations and by numerical solutions. | |
The detectability of a black hole in a globular cluster is | |
discussed in terms of possible observations of the central | |
star distributions.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1977ApJ...216..883B}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/155534}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1977ApJ...216..883B}, | |
Date-added = {2016-01-25 04:52:56 +0000}, | |
Date-modified = {2016-01-25 04:54:29 +0000}, | |
Doi = {10.1086/155534}, | |
Keywords = {Black Holes (Astronomy), Globular Clusters, Star | |
Distribution, Stellar Mass, Binary Stars, Boltzmann | |
Distribution, Boundary Layer Equations, Mass Distribution, | |
Scattering Functions, Steady State, Stellar Motions} | |
} | |
@Article{bahcall&wolf1976, | |
Title = {{Star distribution around a massive black hole in a | |
globular cluster}}, | |
Author = {{Bahcall}, J.~N. and {Wolf}, R.~A.}, | |
Journal = {\apj}, | |
Year = {1976}, | |
Month = oct, | |
Pages = {214-232}, | |
Volume = {209}, | |
Abstract = {The distribution of solar-mass stars around a massive | |
black hole in a globular star cluster is investigated using | |
a basic physical picture in which stars in bound orbits in | |
the gravitational potential well of the black hole diffuse | |
from one bound orbit to another via star-star gravitational | |
scattering. Detailed expressions are derived for the | |
relevant diffusion coefficients, the time-dependent | |
Boltzmann equation is solved numerically, and solutions are | |
found which satisfy the boundary conditions at both zero | |
and large binding energy. The results indicate that the | |
distribution function is approximately a power law | |
throughout most of the black hole's gravitational well, | |
that stars in bound orbits diffuse slowly down the | |
gravitational well under equilibrium conditions, and that a | |
black hole of less than or approximately 1000 solar masses | |
may accrete stars primarily by capture from unbound orbits. | |
Several methods for detecting massive black holes in cores | |
of globular clusters are discussed along with expected | |
large statistical fluctuations close to the black hole and | |
the possible relevance of various stellar accretion | |
processes for globular-cluster X-ray sources.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1976ApJ...209..214B}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/154711}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1976ApJ...209..214B}, | |
Date-added = {2016-10-11 19:00:29 +0000}, | |
Date-modified = {2016-10-11 19:00:29 +0000}, | |
Doi = {10.1086/154711}, | |
Keywords = {Black Holes (Astronomy), Distribution Functions, Globular | |
Clusters, Gravitational Effects, Star Distribution, Stellar | |
Motions, Anisotropy, Density (Number/Volume), Flow | |
Velocity, Gravitational Fields, Stellar Mass, Time | |
Dependence, Velocity Distribution, X Ray Sources} | |
} | |
@Article{bahramian+2014, | |
Title = {{Discovery of the Third Transient X-Ray Binary in the | |
Galactic Globular Cluster Terzan 5}}, | |
Author = {{Bahramian}, A. and {Heinke}, C.~O. and {Sivakoff}, G.~R. | |
and {Altamirano}, D. and {Wijnands}, R. and {Homan}, J. and | |
{Linares}, M. and {Pooley}, D. and {Degenaar}, N. and | |
{Gladstone}, J.~C.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = jan, | |
Pages = {127}, | |
Volume = {780}, | |
Abstract = {We report and study the outburst of a new transient X-ray | |
binary (XRB) in Terzan 5, the third detected in this | |
globular cluster, Swift J174805.3-244637 or Terzan 5 X-3. | |
We find clear spectral hardening in Swift/XRT data during | |
the outburst rise to the hard state, thanks to our early | |
coverage (starting at LX ~ 4 ?1034 erg s-1) of the | |
outburst. This hardening appears to be due to the decline | |
in relative strength of a soft thermal component from the | |
surface of the neutron star (NS) during the rise. We | |
identify a Type I X-ray burst in Swift/XRT data with a long | |
(16 s) decay time, indicative of hydrogen burning on the | |
surface of the NS. We use Swift/BAT, MAXI/GSC, | |
Chandra/ACIS, and Swift/XRT data to study the spectral | |
changes during the outburst, identifying a clear | |
hard-to-soft state transition. We use a Chandra/ACIS | |
observation during outburst to identify the transient's | |
position. Seven archival Chandra/ACIS observations show | |
evidence for variations in Terzan 5 X-3's nonthermal | |
component but not the thermal component during quiescence. | |
The inferred long-term time-averaged mass accretion rate, | |
from the quiescent thermal luminosity, suggests that if | |
this outburst is typical and only slow cooling processes | |
are active in the NS core, such outbursts should recur | |
every ~10 yr.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...780..127B}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1088/0004-637X/780/2/127}, | |
Eid = {127}, | |
Eprint = {1311.4449}, | |
Keywords = {binaries: close, globular clusters: individual: Terzan 5, | |
stars: neutron, X-rays: binaries, X-rays: bursts, X-rays: | |
individual: Swift J174805.3-244637}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2017.12.30} | |
} | |
@Article{bahramian+2017, | |
Title = {{The ultracompact nature of the black hole candidate X-ray | |
binary 47 Tuc X9}}, | |
Author = {{Bahramian}, A. and {Heinke}, C.~O. and {Tudor}, V. and | |
{Miller-Jones}, J.~C.~A. and {Bogdanov}, S. and | |
{Maccarone}, T.~J. and {Knigge}, C. and {Sivakoff}, G.~R. | |
and {Chomiuk}, L. and {Strader}, J. and {Garcia}, J.~A. and | |
{Kallman}, T.}, | |
Journal = {\mnras}, | |
Year = {2017}, | |
Month = may, | |
Pages = {2199-2216}, | |
Volume = {467}, | |
Abstract = {47 Tuc X9 is a low-mass X-ray binary (LMXB) in the | |
globular cluster 47 Tucanae, and was previously thought to | |
be a cataclysmic variable. However, Miller-Jones et al. | |
recently identified a radio counterpart to X9 (inferring a | |
radio/X-ray luminosity ratio consistent with black hole | |
LMXBs), and suggested that the donor star might be a white | |
dwarf. We report simultaneous observations of X9 performed | |
by Chandra, NuSTAR and Australia Telescope Compact Array. | |
We find a clear 28.18 $\pm$ 0.02-min periodic modulation in | |
the Chandra data, which we identify as the orbital period, | |
confirming this system as an ultracompact X-ray binary. Our | |
X-ray spectral fitting provides evidence for photoionized | |
gas having a high oxygen abundance in this system, which | |
indicates a C/O white dwarf donor. We also identify | |
reflection features in the hard X-ray spectrum, making X9 | |
the faintest LMXB to show X-ray reflection. We detect an | |
~6.8-d modulation in the X-ray brightness by a factor of | |
10, in archival Chandra, Swiftand ROSAT data. The | |
simultaneous radio/X-ray flux ratio is consistent with | |
either a black hole primary or a neutron star primary, if | |
the neutron star is a transitional millisecond pulsar. | |
Considering the measured orbital period (with other | |
evidence of a white dwarf donor), and the lack of | |
transitional millisecond pulsar features in the X-ray light | |
curve, we suggest that this could be the first ultracompact | |
black hole X-ray binary identified in our Galaxy.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017MNRAS.467.2199B}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1702.02167}, | |
Bdsk-file-1 = {YnBsaXN0MDDUAQIDBAUGJCVYJHZlcnNpb25YJG9iamVjdHNZJGFyY2hpdmVyVCR0b3ASAAGGoKgHCBMUFRYaIVUkbnVsbNMJCgsMDxJXTlMua2V5c1pOUy5vYmplY3RzViRjbGFzc6INDoACgAOiEBGABIAFgAdccmVsYXRpdmVQYXRoWWFsaWFzRGF0YV8QLy4uLy4uLy4uLy4uL0RvY3VtZW50cy9QYXBlcnMvQmFocmFtaWFuLzIwMTcucGRm0hcLGBlXTlMuZGF0YU8RAZYAAAAAAZYAAgAADE1hY2ludG9zaCBIRAAAAAAAAAAAAAAAAAAAAM1k0ppIKwAAAqErlwgyMDE3LnBkZgAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAACoSuV1SKEtAAAAAAAAAAAAAQABAAACSAAAAAAAAAAAAAAAAAAAAAJQmFocmFtaWFuAAAQAAgAAM1lCtoAAAARAAgAANUivPQAAAABABQCoSuXAQeIBAAFxCoABcQpAAIQ6QACAENNYWNpbnRvc2ggSEQ6VXNlcnM6AGFsZWtzZXk6AERvY3VtZW50czoAUGFwZXJzOgBCYWhyYW1pYW46ADIwMTcucGRmAAAOABIACAAyADAAMQA3AC4AcABkAGYADwAaAAwATQBhAGMAaQBuAHQAbwBzAGgAIABIAEQAEgAxVXNlcnMvYWxla3NleS9Eb2N1bWVudHMvUGFwZXJzL0JhaHJhbWlhbi8yMDE3LnBkZgAAEwABLwAAFQACAA7//wAAgAbSGxwdHlokY2xhc3NuYW1lWCRjbGFzc2VzXU5TTXV0YWJsZURhdGGjHR8gVk5TRGF0YVhOU09iamVjdNIbHCIjXE5TRGljdGlvbmFyeaIiIF8QD05TS2V5ZWRBcmNoaXZlctEmJ1Ryb290gAEACAARABoAIwAtADIANwBAAEYATQBVAGAAZwBqAGwAbgBxAHMAdQB3AIQAjgDAAMUAzQJnAmkCbgJ5AoICkAKUApsCpAKpArYCuQLLAs4C0wAAAAAAAAIBAAAAAAAAACgAAAAAAAAAAAAAAAAAAALV}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stx166}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1702.02167}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2017MNRAS.467.2199B}, | |
Date-added = {2017-04-23 20:20:05 +0000}, | |
Date-modified = {2017-04-23 20:20:06 +0000}, | |
Doi = {10.1093/mnras/stx166}, | |
Eprint = {1702.02167}, | |
Keywords = {accretion, accretion discs, stars: Black holes, stars: | |
neutron, globular clusters: individual: 47 Tuc, X-rays: | |
binaries}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{baker+2006, | |
Title = {{Gravitational-Wave Extraction from an Inspiraling | |
Configuration of Merging Black Holes}}, | |
Author = {{Baker}, J.~G. and {Centrella}, J. and {Choi}, D.-I. and | |
{Koppitz}, M. and {van Meter}, J.}, | |
Journal = {Physical Review Letters}, | |
Year = {2006}, | |
Month = mar, | |
Number = {11}, | |
Pages = {111102}, | |
Volume = {96}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006PhRvL..96k1102B}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1103/PhysRevLett.96.111102}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1103/PhysRevLett.96.111102}, | |
Eid = {111102}, | |
Eprint = {arXiv:gr-qc/0511103}, | |
Keywords = {Numerical relativity, Wave generation and sources, | |
Classical black holes, Relativity and gravitation} | |
} | |
@Article{balbus2001, | |
Title = {{Convective and Rotational Stability of a Dilute Plasma}}, | |
Author = {{Balbus}, S.~A.}, | |
Journal = {\apj}, | |
Year = {2001}, | |
Month = dec, | |
Pages = {909-917}, | |
Volume = {562}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2001ApJ...562..909B}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/323875}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/323875}, | |
Eprint = {astro-ph/0106283}, | |
Keywords = {Accretion, Accretion Disks, Black Hole Physics, | |
Convection, Hydrodynamics, Instabilities, Turbulence} | |
} | |
@Article{bandara+2009, | |
Title = {{A Relationship Between Supermassive Black Hole Mass and | |
the Total Gravitational Mass of the Host Galaxy}}, | |
Author = {{Bandara}, K. and {Crampton}, D. and {Simard}, L.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = oct, | |
Pages = {1135-1145}, | |
Volume = {704}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...704.1135B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/704/2/1135}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1088/0004-637X/704/2/1135}, | |
Eprint = {0909.0269}, | |
Keywords = {black hole physics, galaxies: evolution, galaxies: halos, | |
gravitational lensing, quasars: general} | |
} | |
@Article{banerjee+2010, | |
Title = {{Stellar-mass black holes in star clusters: implications | |
for gravitational wave radiation}}, | |
Author = {{Banerjee}, S. and {Baumgardt}, H. and {Kroupa}, P.}, | |
Journal = {\mnras}, | |
Year = {2010}, | |
Month = feb, | |
Pages = {371-380}, | |
Volume = {402}, | |
Abstract = {We study the dynamics of stellar-mass black holes (BH) in | |
star clusters with particular attention to the formation of | |
BH-BH binaries, which are interesting as sources of | |
gravitational waves (GW). In the present study, we examine | |
the properties of these BH-BH binaries through direct | |
N-body simulations of star clusters using the NBODY6 code | |
on graphical processing unit platforms. We perform | |
simulations for star clusters with <=105 low-mass stars | |
starting from Plummer models with an initial population of | |
BHs, varying the cluster mass and BH-retention fraction. | |
Additionally, we do several calculations of star clusters | |
confined within a reflective boundary mimicking only the | |
core of a massive star cluster which can be performed much | |
faster than the corresponding full cluster integration. We | |
find that stellar-mass BHs with masses ~10Msolar segregate | |
rapidly (~100 Myr time-scale) into the cluster core and | |
form a dense subcluster of BHs within typically 0.2-0.5 pc | |
radius. In such a subcluster, BH-BH binaries can be formed | |
through three-body encounters, the rate of which can become | |
substantial in dense enough BH cores. While most BH | |
binaries are finally ejected from the cluster by recoils | |
received during superelastic encounters with the single | |
BHs, few of them harden sufficiently so that they can merge | |
via GW emission within the cluster. We find that for | |
clusters with N >~ 5 × 104, typically 1-2 BH-BH mergers | |
occur per cluster within the first ~4 Gyr of cluster | |
evolution. Also for each of these clusters, there are a few | |
escaping BH binaries that can merge within a Hubble time, | |
most of the merger times being within a few Gyr. These | |
results indicate that intermediate-age massive clusters | |
constitute the most important class of candidates for | |
producing dynamical BH-BH mergers. Old globular clusters | |
cannot contribute significantly to the present-day BH-BH | |
merger rate since most of the mergers from them would have | |
occurred much earlier. On the other hand, young massive | |
clusters with ages less that 50 Myr are too young to | |
produce significant number of BH-BH mergers. We finally | |
discuss the detection rate of BH-BH inspirals by the `Laser | |
Interferometer Gravitational-Wave Observatory' (LIGO) and | |
`Advanced LIGO' GW detectors. Our results indicate that | |
dynamical BH-BH binaries constitute the dominant channel | |
for BH-BH merger detection.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010MNRAS.402..371B}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/0910.3954}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2009.15880.x}, | |
Bdsk-url-2 = {http://arxiv.org/abs/0910.3954}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2010MNRAS.402..371B}, | |
Date-added = {2017-06-04 23:01:37 +0000}, | |
Date-modified = {2017-06-04 23:02:13 +0000}, | |
Doi = {10.1111/j.1365-2966.2009.15880.x}, | |
Eprint = {0910.3954}, | |
Keywords = {black hole physics, gravitational waves, scattering, | |
stellar dynamics, methods: N-body simulations, galaxies: | |
star clusters}, | |
Primaryclass = {astro-ph.SR} | |
} | |
@Article{barkana2018, | |
Title = {Possible interaction between baryons and dark-matter particles revealed by the first stars}, | |
Author = {Barkana, Rennan}, | |
Journal = {Nature}, | |
Year = {2018}, | |
Month = feb, | |
Pages = {71--}, | |
Volume = {555}, | |
Owner = {aleksey}, | |
Publisher = {Macmillan Publishers Limited, part of Springer Nature. All rights reserved.}, | |
Timestamp = {2018.03.07}, | |
Url = {http://dx.doi.org/10.1038/nature25791} | |
} | |
@Article{barkana2018, | |
Title = {Possible interaction between baryons and dark-matter particles revealed by the first stars}, | |
Author = {Barkana, Rennan}, | |
Journal = {Nature}, | |
Year = {2018}, | |
Month = feb, | |
Pages = {71--}, | |
Volume = {555}, | |
Owner = {aleksey}, | |
Publisher = {Macmillan Publishers Limited, part of Springer Nature. All rights reserved.}, | |
Timestamp = {2018.03.07}, | |
Url = {http://dx.doi.org/10.1038/nature25791} | |
} | |
@Article{barnes+1992, | |
Title = {{Dynamics of interacting galaxies}}, | |
Author = {Barnes, J.\~{}E. and Hernquist, L}, | |
Journal = {\araa}, | |
Year = {1992}, | |
Pages = {705--742}, | |
Volume = {30}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1146/annurev.aa.30.090192.003421}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1146/annurev.aa.30.090192.003421}, | |
Keywords = {ACTIVE GALAXIES,DARK MATTER,DYNAMICS,GALACTIC | |
EVOLUTION,INTERACTING GALAXIES,IRREGULAR | |
GALAXIES,MORPHOLOGY,STARBURST GALAXIES} | |
} | |
@Article{barnes+1996, | |
Title = {{Transformations of Galaxies. II. Gasdynamics in Merging | |
Disk Galaxies}}, | |
Author = {Barnes, Joshua E and Hernquist, Lars}, | |
Journal = {Astrophysical Journal v.471}, | |
Year = {1996}, | |
Month = nov, | |
Pages = {115}, | |
Volume = {471}, | |
Abstract = {In mergers of disk galaxies, gas plays a role quite out of | |
proportion to its relatively modest contribution to the | |
total mass. To study this behavior, we have included | |
gasdynamics in self-consistent simulations of collisions | |
between equal-mass disk galaxies. The large-scale dynamics | |
of bridge- and tail-making, orbit decay, and merging are | |
not much altered by the inclusion of a gaseous component. | |
However, tidal forces during encounters cause otherwise | |
stable disks to develop bars, and the gas in such barred | |
disks, subjected to strong gravitational torques, flows | |
toward the central regions where it may fuel the | |
kiloparsec-scale starbursts seen in some interacting disk | |
systems. Similar torques on the gas during the final stages | |
of a collision yield massive gas concentrations in the | |
cores of merger remnants, which may be plausibly identified | |
with the molecular complexes seen in objects such as NGC | |
520 and Arp 220. This result appears insensitive to the | |
detailed microphysics of the gas, provided that radiative | |
cooling is permitted. The inflowing gas can dramatically | |
alter the stellar morphology of a merger remnant, | |
apparently by deepening the potential well and thereby | |
changing the boundaries between the major orbital | |
families.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=1996ApJ...471..115B%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1086/177957}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1086/177957}, | |
Keywords = {GALAXIES: STRUCTURE, Methods: Numerical, galaxies: | |
interactions,Hydrodynamics}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=1996ApJ...471..115B\&link\_type=ABSTRACT} | |
} | |
@Article{barnes+1991, | |
Title = {{Fueling starburst galaxies with gas-rich mergers}}, | |
Author = {{Barnes}, J.~E. and {Hernquist}, L.~E.}, | |
Journal = {\apjl}, | |
Year = {1991}, | |
Month = apr, | |
Pages = {L65-L68}, | |
Volume = {370}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1991ApJ...370L..65B}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/185978}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:38 +0000}, | |
Doi = {10.1086/185978}, | |
Keywords = {GALACTIC EVOLUTION, GALACTIC NUCLEI, GALACTIC STRUCTURE, | |
INTERGALACTIC MEDIA, STAR FORMATION, STARBURST GALAXIES, | |
ANGULAR MOMENTUM, ASTRONOMICAL MODELS, GAS DYNAMICS, | |
GRAVITATIONAL EFFECTS} | |
} | |
@Article{baror&alexander2016, | |
Title = {{Steady-state Relativistic Stellar Dynamics Around a | |
Massive Black hole}}, | |
Author = {{Bar-Or}, B. and {Alexander}, T.}, | |
Journal = {\apj}, | |
Year = {2016}, | |
Month = apr, | |
Pages = {129}, | |
Volume = {820}, | |
Abstract = {A massive black hole (MBH) consumes stars whose orbits | |
evolve into the small phase-space volume of unstable | |
orbits, the ``loss cone,'' which take them into the MBH, or | |
close enough to interact strongly with it. The resulting | |
phenomena, e.g., tidal heating and disruption, binary | |
capture and hyper-velocity star ejection, gravitational | |
wave (GW) emission by inspiraling compact remnants, or | |
hydrodynamical interactions with an accretion disk, can | |
produce observable signatures and thereby reveal the MBH, | |
affect its mass and spin evolution, test strong gravity, | |
and probe stars and gas near the MBH. These continuous | |
stellar loss and resupply processes shape the central | |
stellar distribution. We investigate relativistic stellar | |
dynamics near the loss cone of a non-spinning MBH in steady | |
state, analytically and by Monte Carlo simulations of the | |
diffusion of the orbital parameters. These take into | |
account Newtonian mass precession due to enclosed stellar | |
mass, in-plane precession due to general relativity, | |
dissipation by GW, uncorrelated two-body relaxation, | |
correlated resonant relaxation (RR), and adiabatic | |
invariance due to secular precession, using a rigorously | |
derived description of correlated post-Newtonian dynamics | |
in the diffusion limit. We argue that general maximal | |
entropy considerations strongly constrain the orbital | |
diffusion in steady state, irrespective of the relaxation | |
mechanism. We identify the exact phase-space separatrix | |
between plunges and inspirals, and predict their | |
steady-state rates. We derive the dependence of the rates | |
on the mass of the MBH, show that the contribution of RR in | |
steady state is small, and discuss special cases where | |
unquenched RR in restricted volumes of phase-space may | |
affect the steady state substantially.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016ApJ...820..129B}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1508.01390}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.3847/0004-637X/820/2/129}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1508.01390}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2016ApJ...820..129B}, | |
Date-added = {2017-08-08 01:16:45 +0000}, | |
Date-modified = {2017-08-08 02:12:33 +0000}, | |
Doi = {10.3847/0004-637X/820/2/129}, | |
Eid = {129}, | |
Eprint = {1508.01390}, | |
Keywords = {black hole physics, galaxies: nuclei, stars: kinematics | |
and dynamics} | |
} | |
@Article{bar-or.fouvry2018, | |
author = {{Bar-Or}, B. and {Fouvry}, J.-B.}, | |
title = {{Scalar Resonant Relaxation of Stars around a Massive Black Hole}}, | |
journal = {\apjl}, | |
year = {2018}, | |
volume = {860}, | |
pages = {L23}, | |
month = jun, | |
abstract = {In nuclear star clusters, the potential is governed by the central massive black hole (MBH), so that stars move on nearly Keplerian orbits and the total potential is almost stationary in time. Yet, the deviations of the potential from the Keplerian one, due to the enclosed stellar mass and general relativity, will cause the stellar orbits to precess. Moreover, as a result of the finite number of stars, small deviations of the potential from spherical symmetry induce residual torques that can change the stars? angular momentum faster than the standard two-body relaxation. The combination of these two effects drives a stochastic evolution of orbital angular momentum, a process named ?resonant relaxation? (RR). Owing to recent developments in the description of the relaxation of self-gravitating systems, we can now fully describe scalar resonant relaxation (relaxation of the magnitude of the angular momentum) as a diffusion process. In this framework, the potential fluctuations due to the complex orbital motion of the stars are described by a random correlated noise with statistical properties that are fully characterized by the stars? mean field motion. On long timescales, the cluster can be regarded as a diffusive system with diffusion coefficients that depend explicitly on the mean field stellar distribution through the properties of the noise. We show here, for the first time, how the diffusion coefficients of scalar RR, for a spherically symmetric system, can be fully calculated from first principles, without any free parameters. We also provide an open source code that evaluates these diffusion coefficients numerically.}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
adsurl = {http://adsabs.harvard.edu/abs/2018ApJ...860L..23B}, | |
archiveprefix = {arXiv}, | |
doi = {10.3847/2041-8213/aac88e}, | |
eid = {L23}, | |
eprint = {1802.08890}, | |
file = {:Bar-Or/bar-or.fouvry2018.pdf:PDF}, | |
keywords = {black hole physics, galaxies: nuclei, gravitation, stars: kinematics and dynamics}, | |
owner = {aleksey}, | |
timestamp = {2019.05.09}, | |
} | |
@Article{bartko+2010, | |
Title = {{An Extremely Top-Heavy Initial Mass Function in the | |
Galactic Center Stellar Disks}}, | |
Author = {{Bartko}, H. and others}, | |
Journal = {\apj}, | |
Year = {2010}, | |
Month = jan, | |
Pages = {834-840}, | |
Volume = {708}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010ApJ...708..834B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/708/1/834}, | |
Doi = {10.1088/0004-637X/708/1/834}, | |
Eprint = {0908.2177}, | |
Keywords = {Galaxy: center, stars: early-type, stars: luminosity | |
function, mass function} | |
} | |
@Article{bartos+2017a, | |
Title = {{Gravitational-Wave Localization Alone Probes AGN Origin | |
of Stellar-Mass Black Hole Mergers}}, | |
Author = {{Bartos}, I. and {Haiman}, Z. and {Marka}, Z. and | |
{Metzger}, B.~D. and {Stone}, N.~C. and {Marka}, S.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2017}, | |
Month = jan, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017arXiv170102328B}, | |
Archiveprefix = {arXiv}, | |
Eprint = {1701.02328}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{bartos+2017, | |
Title = {{Rapid and Bright Stellar-mass Binary Black Hole Mergers | |
in Active Galactic Nuclei}}, | |
Author = {{Bartos}, I. and {Kocsis}, B. and {Haiman}, Z. and | |
{M{\'a}rka}, S.}, | |
Journal = {\apj}, | |
Year = {2017}, | |
Month = feb, | |
Pages = {165}, | |
Volume = {835}, | |
Abstract = {The Laser Interferometer Gravitational-wave Observatory | |
(LIGO) found direct evidence for double black hole binaries | |
emitting gravitational waves. Galactic nuclei are expected | |
to harbor the densest population of stellar-mass black | |
holes. A significant fraction (˜ 30 \% ) of these black | |
holes can reside in binaries. We examine the fate of the | |
black hole binaries in active galactic nuclei, which get | |
trapped in the inner region of the accretion disk around | |
the central supermassive black hole. We show that binary | |
black holes can migrate into and then rapidly merge within | |
the disk well within a Salpeter time. The binaries may also | |
accrete a significant amount of gas from the disk, well | |
above the Eddington rate. This could lead to detectable | |
X-ray or gamma-ray emission, but would require | |
hyper-Eddington accretion with a few percent radiative | |
efficiency, comparable to thin disks. We discuss | |
implications for gravitational-wave observations and black | |
hole population studies. We estimate that Advanced LIGO may | |
detect ˜20 such gas-induced binary mergers per year.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017ApJ...835..165B}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1602.03831}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.3847/1538-4357/835/2/165}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1602.03831}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2017ApJ...835..165B}, | |
Date-added = {2017-06-09 20:41:47 +0000}, | |
Date-modified = {2017-06-09 20:46:28 +0000}, | |
Doi = {10.3847/1538-4357/835/2/165}, | |
Eid = {165}, | |
Eprint = {1602.03831}, | |
Keywords = {gravitational waves, stars: black holes}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{bate+2003, | |
Title = {{Three-dimensional calculations of high- and low-mass | |
planets embedded in protoplanetary discs}}, | |
Author = {{Bate}, M.~R. and {Lubow}, S.~H. and {Ogilvie}, G.~I. and | |
{Miller}, K.~A.}, | |
Journal = {\mnras}, | |
Year = {2003}, | |
Month = may, | |
Pages = {213-229}, | |
Volume = {341}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2003MNRAS.341..213B}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1046/j.1365-8711.2003.06406.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1046/j.1365-8711.2003.06406.x}, | |
Eprint = {arXiv:astro-ph/0301154}, | |
Keywords = {accretion, accretion discs, hydrodynamics, planets and | |
satellites: formation, planetary systems: formation, | |
planetary systems: protoplanetary discs} | |
} | |
@Article{baumgardt+2018, | |
Title = {{The distribution of stars around the Milky Way's central black hole. III. Comparison with simulations}}, | |
Author = {{Baumgardt}, H. and {Amaro-Seoane}, P. and {Sch{\"o}del}, R.}, | |
Journal = {\aap}, | |
Year = {2018}, | |
Month = jan, | |
Pages = {A28}, | |
Volume = {609}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2018A%26A...609A..28B}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1051/0004-6361/201730462}, | |
Eid = {A28}, | |
Eprint = {1701.03818}, | |
Keywords = {methods: numerical, Hertzsprung-Russell and C-M diagrams, stars: kinematics and dynamics, Galaxy: centre, Galaxy: nucleus} | |
} | |
@Article{baumgardt+2017, | |
Title = {{The distribution of stars around the Milky Way's black | |
hole III: Comparison with simulations}}, | |
Author = {{Baumgardt}, H. and {Amaro-Seoane}, P. and {Sch{\"o}del}, | |
R. }, | |
Journal = {ArXiv e-prints}, | |
Year = {2017}, | |
Month = jan, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017arXiv170103818B}, | |
Archiveprefix = {arXiv}, | |
Eprint = {1701.03818}, | |
Keywords = {Astrophysics - Astrophysics of Galaxies} | |
} | |
@Article{becklin+1982, | |
Title = {{Far-infrared observations of Sagittarius A - The | |
luminosity and dust density in the central parsec of the | |
Galaxy}}, | |
Author = {{Becklin}, E.~E. and {Gatley}, I. and {Werner}, M.~W.}, | |
Journal = {\apj}, | |
Year = {1982}, | |
Month = jul, | |
Pages = {135-142}, | |
Volume = {258}, | |
Abstract = {Far-infrared observations of the central 4 arcmin of the | |
Galaxy with 30-arcsec resolution made simultaneously at 30 | |
microns, 50 microns, and 100 microns are presented. The | |
30-micron radiation peaks strongly at the position of the | |
galactic center, as determined from the 2-micron surface | |
brightness and the density of ionized gas. The 50- and | |
100-micron emission is much more extended along the plane | |
and shows two emission lobes, one on either side of the | |
30-micron peak. At the position of the galactic center | |
itself there is a local minimum in the 100-micron surface | |
brightness. It is concluded that the dust density decreases | |
inward over the central few parsecs of the Galaxy and that | |
the dust density in the central parsec is so low that | |
optical and ultraviolet radiation freely traverses this | |
region. The total luminosity of the sources heating the | |
dust which radiates the far-infrared emission from the | |
central few parsecs is deduced to be between 1 x 10 to the | |
7th and 3 x 10 to the 7th solar luminosities.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1982ApJ...258..135B}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/160060}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1982ApJ...258..135B}, | |
Date-added = {2016-04-26 18:06:51 +0000}, | |
Date-modified = {2016-04-26 18:06:52 +0000}, | |
Doi = {10.1086/160060}, | |
Keywords = {Far Infrared Radiation, Galactic Nuclei, Gas Density, | |
Luminous Intensity, Milky Way Galaxy, Radio Sources | |
(Astronomy), Astronomical Photometry, Cosmic Dust, Emission | |
Spectra, Gas Ionization, High Resolution, Hydrogen Clouds, | |
Interstellar Matter, Particle Size Distribution, Stellar | |
Evolution, Surface Properties, Ultraviolet Radiation} | |
} | |
@Article{begelman+1980, | |
Title = {{Massive black hole binaries in active galactic nuclei}}, | |
Author = {Begelman, M.\~{}C. and Blandford, R.\~{}D. and Rees, | |
M.\~{}J.}, | |
Journal = {\nat}, | |
Year = {1980}, | |
Month = sep, | |
Pages = {307--309}, | |
Volume = {287}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1038/287307a0}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1038/287307a0}, | |
Keywords = {ASTROPHYSICS, BINARY STARS, BLACK HOLES (ASTRONOMY), | |
ORBITAL ELEMENTS, STELLAR EVOLUTION, SUPERMASSIVE | |
STARS,ACTIVE GALACTIC NUCLEI} | |
} | |
@Article{begelman1978, | |
Title = {{Black holes in radiation-dominated gas - an analogue of the Bondi accretion problem}}, | |
Author = {{Begelman}, M.~C.}, | |
Journal = {\mnras}, | |
Year = {1978}, | |
Month = jul, | |
Pages = {53-67}, | |
Volume = {184}, | |
Abstract = {The steady flow of a uniform nonrelativistic gas, in which radiation pressure swamps thermal pressure at infinity, is studied in terms of the dynamics of an in-falling gas into a black hole. It is shown that the actual accretion rate depends on the optical depth of a column of unperturbed gas spanning the Bondi radius. Radiation leaks out of the gas as it moves toward the trans-sonic point, and the sound speed decreases inwards in the subsonic region. Thus, the density must increase sharply to maintain pressure. It is suggested that if a super-massive (500,000 solar masses) star is swallowed by a black hole, it will not have time to ignite its nuclear fuel and blow itself apart, and will add substantially to the mass of the hole.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1978MNRAS.184...53B}, | |
Doi = {10.1093/mnras/184.1.53}, | |
Keywords = {Black Holes (Astronomy), Radiation Pressure, Sound Waves, Stellar Envelopes, Stellar Mass Accretion, Thermodynamic Equilibrium, Eddington Approximation, Gas Pressure, Gas Temperature, Interstellar Gas}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.22} | |
} | |
@Article{beloborodov&uhm2006, | |
Title = {{Mechanical Model for Relativistic Blast Waves}}, | |
Author = {{Beloborodov}, A.~M. and {Uhm}, Z.~L.}, | |
Journal = {\apjl}, | |
Year = {2006}, | |
Month = nov, | |
Pages = {L1-L4}, | |
Volume = {651}, | |
Abstract = {Relativistic blast waves can be described using a | |
mechanical model. In this model, the ``blast''-the | |
compressed gas between the forward and reverse shocks-is | |
viewed as one hot body. Equations governing its dynamics | |
are derived from the conservation of mass, energy, and | |
momentum. Simple analytical solutions are obtained in the | |
two limiting cases of an ultrarelativistic and a | |
nonrelativistic reverse shock. Equations are derived for | |
the general explosion problem.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006ApJ...651L...1B}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0607641}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/508807}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0607641}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2006ApJ...651L...1B}, | |
Date-added = {2015-12-07 18:34:47 +0000}, | |
Date-modified = {2015-12-07 18:35:24 +0000}, | |
Doi = {10.1086/508807}, | |
Eprint = {astro-ph/0607641}, | |
Keywords = {Gamma Rays: Bursts, Hydrodynamics, Relativity, Shock | |
Waves} | |
} | |
@Article{benacquista+2013, | |
Title = {{Relativistic Binaries in Globular Clusters}}, | |
Author = {{Benacquista}, M.~J. and {Downing}, J.~M.~B.}, | |
Journal = {Living Reviews in Relativity}, | |
Year = {2013}, | |
Month = mar, | |
Pages = {4}, | |
Volume = {16}, | |
Abstract = {Galactic globular clusters are old, dense star systems | |
typically containing 104-106 stars. As an old population of | |
stars, globular clusters contain many collapsed and | |
degenerate objects. As a dense population of stars, | |
globular clusters are the scene of many interesting close | |
dynamical interactions between stars. These dynamical | |
interactions can alter the evolution of individual stars | |
and can produce tight binary systems containing one or two | |
compact objects. In this review, we discuss theoretical | |
models of globular cluster evolution and binary evolution, | |
techniques for simulating this evolution that leads to | |
relativistic binaries, and current and possible future | |
observational evidence for this population. Our discussion | |
of globular cluster evolution will focus on the processes | |
that boost the production of tight binary systems and the | |
subsequent interaction of these binaries that can alter the | |
properties of both bodies and can lead to exotic objects. | |
Direct N-body integrations and Fokker-Planck simulations of | |
the evolution of globular clusters that incorporate tidal | |
interactions and lead to predictions of relativistic binary | |
populations are also discussed. We discuss the current | |
observational evidence for cataclysmic variables, | |
millisecond pulsars, and low-mass X-ray binaries as well as | |
possible future detection of relativistic binaries with | |
gravitational radiation.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2013LRR....16....4B}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1110.4423}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.12942/lrr-2013-4}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1110.4423}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2013LRR....16....4B}, | |
Date-added = {2017-08-23 22:57:20 +0000}, | |
Date-modified = {2017-08-23 23:06:29 +0000}, | |
Doi = {10.12942/lrr-2013-4}, | |
Eid = {4}, | |
Eprint = {1110.4423}, | |
Keywords = {Pulsars, Black holes, Accretion disks, Globular clusters, | |
Binary systems, Gravitational wave sources, accretion, | |
accretion disks, astronomical observations, astronomy, | |
astrophysics, binary systems, black holes, dynamical | |
systems, gravitational wave sources, neutron stars, | |
pulsars, radio astronomy, stars, white dwarfs}, | |
Primaryclass = {astro-ph.SR} | |
} | |
@Article{bender1988, | |
Title = {{Velocity anisotropies and isophote shapes in elliptical | |
galaxies}}, | |
Author = {{Bender}, R.}, | |
Journal = {\aap}, | |
Year = {1988}, | |
Month = mar, | |
Pages = {L7-L10}, | |
Volume = {193}, | |
Abstract = {Rotation and velocity dispersion data are presented for 17 | |
elliptical galaxies for which no or only insufficient | |
measurements were available. Using data from the | |
literature, the relation between velocity anisotropies and | |
isophote shapes in elliptical galaxies is investigated. It | |
is found that elliptical galaxies most likely can be | |
separated into two classes. Objects having peaked isophotes | |
(indicating weak disk components) are in general consistent | |
with being rotationally flattened, suggesting that these | |
objects are similar to S0 galaxies. In contrast, elliptical | |
galaxies with box-shaped isophotes frequently owe their | |
shape to anisotropies in their velocity dispersion and most | |
likely are triaxial.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1988A%26A...193L...7B}, | |
Bdsk-file-1 = {YnBsaXN0MDDUAQIDBAUGJCVYJHZlcnNpb25YJG9iamVjdHNZJGFyY2hpdmVyVCR0b3ASAAGGoKgHCBMUFRYaIVUkbnVsbNMJCgsMDxJXTlMua2V5c1pOUy5vYmplY3RzViRjbGFzc6INDoACgAOiEBGABIAFgAdccmVsYXRpdmVQYXRoWWFsaWFzRGF0YV8QLC4uLy4uLy4uLy4uL0RvY3VtZW50cy9QYXBlcnMvQmVuZGVyLzE5ODgucGRm0hcLGBlXTlMuZGF0YU8RAYoAAAAAAYoAAgAADE1hY2ludG9zaCBIRAAAAAAAAAAAAAAAAAAAAM1k0ppIKwAAAT3aKggxOTg4LnBkZgAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAABB4hc0Cu9AgAAAAAAAAAAAAQABAAACSAAAAAAAAAAAAAAAAAAAAAGQmVuZGVyABAACAAAzWUK2gAAABEACAAA0Cv1QgAAAAEAFAE92ioBB4gEAAXEKgAFxCkAAhDpAAIAQE1hY2ludG9zaCBIRDpVc2VyczoAYWxla3NleToARG9jdW1lbnRzOgBQYXBlcnM6AEJlbmRlcjoAMTk4OC5wZGYADgASAAgAMQA5ADgAOAAuAHAAZABmAA8AGgAMAE0AYQBjAGkAbgB0AG8AcwBoACAASABEABIALlVzZXJzL2FsZWtzZXkvRG9jdW1lbnRzL1BhcGVycy9CZW5kZXIvMTk4OC5wZGYAEwABLwAAFQACAA7//wAAgAbSGxwdHlokY2xhc3NuYW1lWCRjbGFzc2VzXU5TTXV0YWJsZURhdGGjHR8gVk5TRGF0YVhOU09iamVjdNIbHCIjXE5TRGljdGlvbmFyeaIiIF8QD05TS2V5ZWRBcmNoaXZlctEmJ1Ryb290gAEACAARABoAIwAtADIANwBAAEYATQBVAGAAZwBqAGwAbgBxAHMAdQB3AIQAjgC9AMIAygJYAloCXwJqAnMCgQKFAowClQKaAqcCqgK8Ar8CxAAAAAAAAAIBAAAAAAAAACgAAAAAAAAAAAAAAAAAAALG}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/abs/1988A%26A...193L...7B}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:36 +0000}, | |
Keywords = {Angular Velocity, Elliptical Galaxies, Galactic Rotation, | |
Galactic Structure, Anisotropy, Isophotes, Spectrograms; | |
Untitled; Untitled1} | |
} | |
@Article{bender+1989, | |
Title = {{Isophote shapes of elliptical galaxies. II - Correlations | |
with global optical, radio and X-ray properties}}, | |
Author = {{Bender}, R. and {Surma}, P. and {Doebereiner}, S. and | |
{Moellenhoff}, C. and {Madejsky}, R.}, | |
Journal = {\aap}, | |
Year = {1989}, | |
Month = jun, | |
Pages = {35-43}, | |
Volume = {217}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1989A26A...217...35B}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:36 +0000}, | |
Keywords = {Active Galaxies, Astronomical Photometry, Elliptical | |
Galaxies, Galactic Structure, Isophotes, Charge Coupled | |
Devices, Cosmic X Rays, Light Emission, Mass To Light | |
Ratios, Radio Emission; Untitled; Untitled1} | |
} | |
@Article{bentz2015, | |
Title = {{AGN Reverberation Mapping}}, | |
Author = {{Bentz}, M.~C.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2015}, | |
Month = may, | |
Abstract = {Reverberation mapping is now a well-established technique | |
for investigating spatially-unresolved structures in the | |
nuclei of distant galaxies with actively-accreting | |
supermassive black holes. Structural parameters for the | |
broad emission-line region, with angular sizes of | |
microarcseconds, can be constrained through the | |
substitution of time resolution for spatial resolution. | |
Many reverberation experiments over the last 30 years have | |
led to a practical understanding of the requirements | |
necessary for a successful program. With reverberation | |
measurements now in hand for 60 active galaxies, and more | |
on the horizon, we are able to directly constrain black | |
hole masses, derive scaling relationships that allow large | |
numbers of black hole mass estimates throughout the | |
observable Universe, and begin investigating the detailed | |
geometry and kinematics of the broad line region. | |
Reverberation mapping is therefore one of the few | |
techniques available that will allow a deeper understanding | |
of the physical mechanisms involved in AGN feeding and | |
feedback at very small scales, as well as constraints on | |
the growth and evolution of black holes across cosmic time. | |
In this contribution, I will briefly review the background, | |
implementation, and major results derived from this high | |
angular resolution technique.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015arXiv150504805B}, | |
Archiveprefix = {arXiv}, | |
Eprint = {1505.04805}, | |
Keywords = {Astrophysics - Astrophysics of Galaxies}, | |
Owner = {aleksey}, | |
Timestamp = {2018.02.14} | |
} | |
@Article{berczik+2005, | |
Title = {{Long-term evolution of massive black hole binaries.}}, | |
Author = {Berczik, P and Merritt, D and Spurzem, R}, | |
Journal = {Astron. Nachr.}, | |
Year = {2005}, | |
Month = aug, | |
Pages = {589}, | |
Volume = {326}, | |
Abstract = {Not Available}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2005AN....326R.589B%5C&link%5C_type=CITATIONS}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:36 +0000}, | |
Keywords = {Untitled; Untitled1}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2005AN....326R.589B\&link\_type=CITATIONS} | |
} | |
@Article{berczik+2006, | |
Title = {{Efficient Merger of Binary Supermassive Black Holes in | |
Nonaxisymmetric Galaxies}}, | |
Author = {Berczik, Peter and Merritt, David and Spurzem, Rainer and | |
Bischof, Hans-Peter}, | |
Journal = {\apj}, | |
Year = {2006}, | |
Month = may, | |
Pages = {L21}, | |
Volume = {642}, | |
Abstract = {Binary supermassive black holes (SBHs) form naturally in | |
galaxy mergers, but their long-term evolution is uncertain. | |
In spherical galaxies, N-body simulations show that binary | |
evolution stalls at separations much too large for | |
significant emission of gravitational waves (the | |
``final-parsec problem''). Here we follow the long-term | |
evolution of a massive binary in more realistic, triaxial | |
and rotating galaxy models with particle numbers as high as | |
106. We find that the binary does not stall. The binary | |
hardening rates that we observe are sufficient to allow | |
complete coalescence of binary SBHs in 10 Gyr or less, even | |
in the absence of collisional loss-cone refilling or | |
gasdynamical torques, thus providing a potential solution | |
to the final-parsec problem.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2006ApJ...642L..21B%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1086/504426}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1086/504426}, | |
Keywords = {galaxies: evolution, galaxies: interactions,black hole | |
physics}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2006ApJ...642L..21B\&link\_type=ABSTRACT} | |
} | |
@Article{berentzen+2009, | |
Title = {{Binary Black Hole Merger in Galactic Nuclei: | |
Post-Newtonian Simulations}}, | |
Author = {Berentzen, Ingo and Preto, Miguel and Berczik, Peter and | |
Merritt, David and Spurzem, Rainer}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = apr, | |
Pages = {455}, | |
Volume = {695}, | |
Abstract = {This paper studies the formation and evolution of binary | |
supermassive black holes (SMBHs) in rotating galactic | |
nuclei, focusing on the role of stellar dynamics. We | |
present the first N-body simulations that follow the | |
evolution of the SMBHs from kiloparsec separations all the | |
way to their final relativistic coalescence, and that can | |
robustly be scaled to real galaxies. The N-body code | |
includes post-Newtonian (P N) corrections to the binary | |
equations of motion up to order 2.5; we show that the | |
evolution of the massive binary is only correctly | |
reproduced if the conservative 1 P N and 2 P N terms are | |
included. The orbital eccentricities of the massive | |
binaries in our simulations are often found to remain large | |
until shortly before coalescence. This directly affects not | |
only their orbital evolution rates, but has important | |
consequences as well for the gravitational waveforms | |
emitted during the relativistic inspiral. We estimate | |
gravitational wave amplitudes when the frequencies fall | |
inside the band of the (planned) Laser Interferometer Space | |
Antennae (LISA). We find significant contributions---well | |
above the LISA sensitivity curve---from the higher-order | |
harmonics.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2009ApJ...695..455B%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1088/0004-637X/695/1/455}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1088/0004-637X/695/1/455}, | |
Keywords = {GRAVITATIONAL WAVES, black hole physics, galaxies: | |
evolution, galaxies: interactions, galaxies: kinematics and | |
dynamics,galaxies: nuclei}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2009ApJ...695..455B\&link\_type=ABSTRACT} | |
} | |
@Article{berger+2012, | |
Title = {{Radio Monitoring of the Tidal Disruption Event Swift | |
J164449.3+573451. I. Jet Energetics and the Pristine | |
Parsec-scale Environment of a Supermassive Black Hole}}, | |
Author = {{Berger}, E. and {Zauderer}, B. A. and {Pooley}, G.~G. and | |
{Soderberg}, A.~M. and {Sari}, R. and {Brunthaler}, A. and | |
{Bietenholz}, M.~F.}, | |
Journal = {\apj}, | |
Year = {2012}, | |
Month = mar, | |
Number = {1}, | |
Pages = {36}, | |
Volume = {748}, | |
Abstract = {We present continued radio observations of the tidal | |
disruption event Swift J164449.3+573451 extending to deltat | |
≈ 216 days after discovery. The data were obtained with | |
the EVLA, AMI Large Array, CARMA, the SMA, and the | |
VLBA+Effelsberg as part of a long-term program to monitor | |
the expansion and energy scale of the relativistic outflow, | |
and to trace the parsec-scale environment around a | |
previously dormant supermassive black hole (SMBH). The new | |
observations reveal a significant change in the radio | |
evolution starting at deltat ≈ 1 month, with a | |
brightening at all frequencies that requires an increase in | |
the energy by about an order of magnitude, and an overall | |
density profile around the SMBH of rhovpropr -3/2 (0.1-1.2 | |
pc) with a significant flattening at r ≈ 0.4-0.6 pc. The | |
increase in energy cannot be explained with continuous | |
injection from an Lvpropt -5/3 tail, which is observed in | |
the X-rays. Instead, we conclude that the relativistic jet | |
was launched with a wide range of Lorentz factors, obeying | |
E(> Gamma j )vpropGamma-2.5 j . The similar ratios of | |
duration to dynamical timescale for Sw 1644+57 and | |
gamma-ray bursts (GRBs) suggest that this result may be | |
applicable to GRB jets as well. The radial density profile | |
may be indicative of Bondi accretion, with the inferred | |
flattening at r ~ 0.5 pc in good agreement with the Bondi | |
radius for a ~few × 106 M &sun; black hole. The density at | |
~0.5 pc is about a factor of 30 times lower than inferred | |
for the Milky Way Galactic Center, potentially due to a | |
smaller number of mass-shedding massive stars. From our | |
latest observations (deltat ≈ 216 days) we find that the | |
jet energy is E j, iso ≈ 5 × 1053 erg (Ej ≈ 2.4 × | |
1051 erg for theta j = 0.1), the radius is r ≈ 1.2 pc, | |
the Lorentz factor is Gamma j ≈ 2.2, the ambient density | |
is n ≈ 0.2 cm-3, and the projected angular size is r proj | |
≈ 25 muas, below the resolution of the VLBA+Effelsberg. | |
Assuming no future changes in the observed evolution and a | |
final integrated total energy of Ej ≈ 1052 erg, we | |
predict that the radio emission from Sw 1644+57 should be | |
detectable with the EVLA for several decades and will be | |
resolvable with very long baseline interferometry in a few | |
years.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012ApJ...748...36B}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1112.1697}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/748/1/36}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1112.1697}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2012ApJ...748...36B}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1088/0004-637X/748/1/36}, | |
Eid = {36}, | |
Eprint = {1112.1697}, | |
Keywords = {galaxies: nuclei, techniques: interferometric}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Book{binney&tremaine1987, | |
Title = {{Galactic dynamics}}, | |
Author = {{Binney}, J. and {Tremaine}, S.}, | |
Year = {1987}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1987gady.book.....B}, | |
Booktitle = {Princeton, NJ, Princeton University Press, 1987, 747 p.}, | |
Keywords = {Astrophysics, Celestial Mechanics, Galactic Structure, | |
Milky Way Galaxy, Dark Matter, Galactic Evolution, Jeans | |
Theory, Orbital Mechanics, Potential Theory, Stellar | |
Evolution, Stellar Systems} | |
} | |
@Article{bizouard+2013, | |
Title = {{Pulsar timing arrays}}, | |
Author = {{Bizouard}, M.~A. and {Jenet}, F. and {Price}, R. and | |
{Will}, C.~M.}, | |
Journal = {Classical and Quantum Gravity}, | |
Year = {2013}, | |
Month = oct, | |
Number = {22}, | |
Pages = {220301}, | |
Volume = {30}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2013CQGra..30v0301B}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0264-9381/30/22/220301}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1088/0264-9381/30/22/220301}, | |
Eid = {220301} | |
} | |
@Article{blaes+2001, | |
Title = {{Non-LTE, Relativistic Accretion Disk Fits to 3C\~{}273 | |
and the Origin of the Lyman Limit Spectral Break}}, | |
Author = {Blaes, Omer and Hubeny, Ivan and Agol, Eric and Krolik, | |
Julian H}, | |
Journal = {\apj}, | |
Year = {2001}, | |
Pages = {560--568}, | |
Volume = {563}, | |
Abstract = {We fit general relativistic, geometrically thin accretion | |
disk models with non-LTE atmospheres to near simultaneous | |
multiwavelength data of 3C\~{}273, extending from the | |
optical to the far ultraviolet. Our model fits show no flux | |
discontinuity associated with a hydrogen Lyman edge, but | |
they do exhibit a spectral break which qualitatively | |
resembles that seen in the data. This break arises from | |
relativistic smearing of Lyman emission edges which are | |
produced locally at tens of gravitational radii in the | |
disk. We discuss the possible effects of metal line | |
blanketing on the model spectra, as well as the substantial | |
Comptonization required to explain the observed soft X-ray | |
excess. Our best fit accretion disk model underpredicts the | |
near ultraviolet emission in this source, and also has an | |
optical spectrum which is too red. We discuss some of the | |
remaining physical uncertainties, and suggest in particular | |
that an extension of our models to the slim disk regime | |
and/or including nonzero magnetic torques across the | |
innermost stable circular orbit may help resolve these | |
discrepancies.}, | |
Archiveprefix = {arXiv}, | |
Arxivid = {astro-ph/0108451}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/324045}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1086/324045}, | |
Eprint = {0108451}, | |
File = {:home/aleksey/.local/share/data/Mendeley Ltd./Mendeley | |
Desktop/Downloaded/Blaes et al. - 2001 - Non-LTE, | |
Relativistic Accretion Disk Fits to 3C\~{}273 and the | |
Origin of the Lyman Limit Spectral Break.pdf:pdf}, | |
Keywords = {accretion,accretion disks,galaxies active,quasars | |
individual (3c 273)}, | |
Primaryclass = {astro-ph} | |
} | |
@InProceedings{blaes2004, | |
Title = {{Course 3: Physics Fundamentals of Luminous Accretion | |
Disks around Black Holes}}, | |
Author = {{Blaes}, O.~M.}, | |
Booktitle = {Accretion Discs, Jets and High Energy Phenomena in | |
Astrophysics}, | |
Year = {2004}, | |
Editor = {{Beskin}, V. and {Henri}, G. and {Menard}, F. and {et | |
al.}}, | |
Pages = {137-185}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2004adjh.conf..137B}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:36 +0000}, | |
Eprint = {arXiv:astro-ph/0211368}, | |
Keywords = {Untitled; Untitled1} | |
} | |
@Article{blagorodnova+2017, | |
Title = {{iPTF16fnl: A Faint and Fast Tidal Disruption Event in an | |
E+A Galaxy}}, | |
Author = {{Blagorodnova}, N. and {Gezari}, S. and {Hung}, T. and | |
{Kulkarni}, S.~R. and {Cenko}, S.~B. and {Pasham}, D.~R. | |
and {Yan}, L. and {Arcavi}, I. and {Ben-Ami}, S. and {Bue}, | |
B.~D. and {Cantwell}, T. and {Cao}, Y. and {Castro-Tirado}, | |
A.~J. and {Fender}, R. and {Fremling}, C. and {Gal-Yam}, A. | |
and {Ho}, A.~Y.~Q. and {Horesh}, A. and {Hosseinzadeh}, G. | |
and {Kasliwal}, M.~M. and {Kong}, A.~K.~H. and {Laher}, | |
R.~R. and {Leloudas}, G. and {Lunnan}, R. and {Masci}, | |
F.~J. and {Mooley}, K. and {Neill}, J.~D. and {Nugent}, P. | |
and {Powell}, M. and {Valeev}, A.~F. and {Vreeswijk}, P.~M. | |
and {Walters}, R. and {Wozniak}, P.}, | |
Journal = {\apj}, | |
Year = {2017}, | |
Month = jul, | |
Pages = {46}, | |
Volume = {844}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017ApJ...844...46B}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/1538-4357/aa7579}, | |
Eid = {46}, | |
Eprint = {1703.00965}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: | |
nuclei, stars: individual: iPTF16fnl}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2017.11.09} | |
} | |
@Article{blandford&begelman1999, | |
Title = {{On the fate of gas accreting at a low rate on to a black | |
hole}}, | |
Author = {{Blandford}, R.~D. and {Begelman}, M.~C.}, | |
Journal = {\mnras}, | |
Year = {1999}, | |
Month = feb, | |
Pages = {L1-L5}, | |
Volume = {303}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1999MNRAS.303L...1B}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1046/j.1365-8711.1999.02358.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1046/j.1365-8711.1999.02358.x}, | |
Eprint = {astro-ph/9809083}, | |
Keywords = {ACCRETION, ACCRETION DISCS, BLACK HOLE PHYSICS, | |
HYDRODYNAMICS} | |
} | |
@Article{blandford+1999, | |
Title = {{On the fate of gas accreting at a low rate on to a black | |
hole}}, | |
Author = {{Blandford}, R.~D. and {Begelman}, M.~C.}, | |
Journal = {\mnras}, | |
Year = {1999}, | |
Month = feb, | |
Pages = {L1-L5}, | |
Volume = {303}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1999MNRAS.303L...1B}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1046/j.1365-8711.1999.02358.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1046/j.1365-8711.1999.02358.x}, | |
Eprint = {astro-ph/9809083}, | |
Keywords = {ACCRETION, ACCRETION DISCS, BLACK HOLE PHYSICS, | |
HYDRODYNAMICS} | |
} | |
@Article{blandford&mckee1976, | |
Title = {{Fluid dynamics of relativistic blast waves}}, | |
Author = {{Blandford}, R.~D. and {McKee}, C.~F.}, | |
Journal = {Physics of Fluids}, | |
Year = {1976}, | |
Month = aug, | |
Pages = {1130-1138}, | |
Volume = {19}, | |
Abstract = {A fluid dynamical treatment of an ultra-relativistic spherical blast wave enclosed by a strong shock is presented. A simple similarity solution describing the explosion of a fixed amount of energy in a uniform medium is derived, and this is generalized to include cases in which power is supplied by a central source and the density of the external medium varies with radius. Radiative shocks, in which the escaping photons carry away momentum as well as energy, are also discussed. Formulas that interpolate between the non- and ultra-relativistic limits are proposed.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1976PhFl...19.1130B}, | |
Doi = {10.1063/1.861619}, | |
Keywords = {Detonation Waves, Explosions, Gas Dynamics, Relativistic Velocity, Shock Wave Propagation, Adiabatic Flow, Energy Spectra, Equations Of Motion, Interpolation, Momentum Transfer, Similarity Theorem}, | |
Owner = {aleksey}, | |
Timestamp = {2018.04.03} | |
} | |
@Article{blecha+2008, | |
Title = {{Effects of gravitational-wave recoil on the dynamics and | |
growth of supermassive black holes}}, | |
Author = {{Blecha}, L. and {Loeb}, A.}, | |
Journal = {\mnras}, | |
Year = {2008}, | |
Month = nov, | |
Pages = {1311-1325}, | |
Volume = {390}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2008MNRAS.390.1311B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2008.13790.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1111/j.1365-2966.2008.13790.x}, | |
Eprint = {0805.1420}, | |
Keywords = {accretion, accretion discs , black hole physics , | |
gravitational waves , galaxies: active , galaxies: | |
evolution , galaxies: kinematics and dynamics} | |
} | |
@Article{bloom+2011, | |
Title = {{A Possible Relativistic Jetted Outburst from a Massive | |
Black Hole Fed by a Tidally Disrupted Star}}, | |
Author = {{Bloom}, J.~S. and {Giannios}, D. and {Metzger}, B.~D. and | |
{Cenko}, S.~B. and {Perley}, D.~A. and {Butler}, N.~R. and | |
{Tanvir}, N.~R. and {Levan}, A.~J. and {O'Brien}, P.~T. et | |
al.}, | |
Journal = {Science}, | |
Year = {2011}, | |
Month = jul, | |
Pages = {203-}, | |
Volume = {333}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011Sci...333..203B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1126/science.1207150}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1126/science.1207150}, | |
Eprint = {1104.3257}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{boehle+2016, | |
Title = {{An Improved Distance and Mass Estimate for Sgr A* from a | |
Multistar Orbit Analysis}}, | |
Author = {{Boehle}, A. and {Ghez}, A.~M. and {Sch{\"o}del}, R. and | |
{Meyer}, L. and {Yelda}, S. and {Albers}, S. and | |
{Martinez}, G.~D. and {Becklin}, E.~E. and {Do}, T. and | |
{Lu}, J.~R. and {Matthews}, K. and {Morris}, M.~R. and | |
{Sitarski}, B. and {Witzel}, G.}, | |
Journal = {\apj}, | |
Year = {2016}, | |
Month = oct, | |
Pages = {17}, | |
Volume = {830}, | |
Abstract = {We present new, more precise measurements of the mass and | |
distance of our Galaxy?s central supermassive black hole, | |
Sgr A*. These results stem from a new analysis that more | |
than doubles the time baseline for astrometry of faint | |
stars orbiting Sgr A*, combining 2 decades of speckle | |
imaging and adaptive optics data. Specifically, we improve | |
our analysis of the speckle images by using information | |
about a star?s orbit from the deep adaptive optics data | |
(2005-2013) to inform the search for the star in the | |
speckle years (1995-2005). When this new analysis technique | |
is combined with the first complete re-reduction of Keck | |
Galactic Center speckle images using speckle holography, we | |
are able to track the short-period star S0-38 (K-band | |
magnitude = 17, orbital period = 19 yr) through the speckle | |
years. We use the kinematic measurements from speckle | |
holography and adaptive optics to estimate the orbits of | |
S0-38 and S0-2 and thereby improve our constraints of the | |
mass (M bh) and distance (R o ) of Sgr A*: M bh = (4.02 ? | |
0.16 ? 0.04) ?106 M ? and 7.86 ? 0.14 ? 0.04 kpc. The | |
uncertainties in M bh and R o as determined by the combined | |
orbital fit of S0-2 and S0-38 are improved by a factor of 2 | |
and 2.5, respectively, compared to an orbital fit of S0-2 | |
alone and a factor of ?2.5 compared to previous results | |
from stellar orbits. This analysis also limits the extended | |
dark mass within 0.01 pc to less than 0.13 ?106 M ? at | |
99.7% confidence, a factor of 3 lower compared to prior | |
work.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016ApJ...830...17B}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/0004-637X/830/1/17}, | |
Eid = {17}, | |
Eprint = {1607.05726}, | |
Keywords = {astrometry, Galaxy: center, Galaxy: fundamental | |
parameters, infrared: stars, quasars: supermassive black | |
holes, techniques: high angular resolution}, | |
Owner = {aleksey}, | |
Timestamp = {2018.01.31} | |
} | |
@Article{bogdanovic+2009, | |
Title = {{SDSS J092712.65+294344.0: Recoiling Black Hole or a | |
Subparsec Binary Candidate?}}, | |
Author = {{Bogdanovi{\'c}}, T. and {Eracleous}, M. and {Sigurdsson}, | |
S.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = may, | |
Pages = {288-292}, | |
Volume = {697}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...697..288B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/697/1/288}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1088/0004-637X/697/1/288}, | |
Eprint = {0809.3262}, | |
Keywords = {black hole physics, galaxies: individual: SDSS | |
J092712.65+294344.0, galaxies: nuclei, quasars: emission | |
lines} | |
} | |
@Article{bogdanovic+2008, | |
Title = {{Modeling of Emission Signatures of Massive Black Hole | |
Binaries. I. Methods}}, | |
Author = {{Bogdanovi{\'c}}, T. and {Smith}, B.~D. and {Sigurdsson}, | |
S. and {Eracleous}, M.}, | |
Journal = {\apjs}, | |
Year = {2008}, | |
Month = feb, | |
Pages = {455-480}, | |
Volume = {174}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2008ApJS..174..455B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/521828}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1086/521828}, | |
Eprint = {0708.0414}, | |
Keywords = {Black Hole Physics, Galaxies: Nuclei, Hydrodynamics, Line: | |
Profiles, Radiation Mechanisms: General} | |
} | |
@Article{bondi1952, | |
Title = {{On spherically symmetrical accretion}}, | |
Author = {{Bondi}, H.}, | |
Journal = {\mnras}, | |
Year = {1952}, | |
Pages = {195}, | |
Volume = {112}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1952MNRAS.112..195B}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:36 +0000}, | |
Keywords = {Untitled; Untitled1} | |
} | |
@Article{bonnerot+2016, | |
Title = {{Disc formation from tidal disruptions of stars on eccentric orbits by Schwarzschild black holes}}, | |
Author = {{Bonnerot}, C. and {Rossi}, E.~M. and {Lodato}, G. and {Price}, D.~J. }, | |
Journal = {\mnras}, | |
Year = {2016}, | |
Month = jan, | |
Pages = {2253-2266}, | |
Volume = {455}, | |
Abstract = {The potential of tidal disruption of stars to probe otherwise quiescent supermassive black holes cannot be exploited, if their dynamics is not fully understood. So far, the observational appearance of these events has been derived from analytical extrapolations of the debris dynamical properties just after disruption. By means of hydrodynamical simulations, we investigate the subsequent fallback of the stream of debris towards the black hole for stars already bound to the black hole on eccentric orbits. We demonstrate that the debris circularize due to relativistic apsidal precession which causes the stream to self-cross. The circularization time-scale varies between 1 and 10 times the period of the star, being shorter for more eccentric and/or deeper encounters. This self-crossing leads to the formation of shocks that increase the thermal energy of the debris. If this thermal energy is efficiently radiated away, the debris settle in a narrow ring at the circularization radius with shock-induced luminosities of ?10-103 LEdd. If instead cooling is impeded, the debris form an extended torus located between the circularization radius and the semi-major axis of the star with heating rates ?1-102 LEdd. Extrapolating our results to parabolic orbits, we infer that circularization would occur via the same mechanism in ?1 period of the most bound debris for deeply penetrating encounters to ?10 for grazing ones. We also anticipate the same effect of the cooling efficiency on the structure of the disc with associated luminosities of ?1-10 LEdd and heating rates of ?0.1-1 LEdd. In the latter case of inefficient cooling, we deduce a viscous time-scale generally shorter than the circularization time-scale. This suggests an accretion rate through the disc tracing the fallback rate, if viscosity starts acting promptly.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016MNRAS.455.2253B}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1093/mnras/stv2411}, | |
Eprint = {1501.04635}, | |
Keywords = {accretion, accretion discs, black hole physics, hydrodynamics, galaxies: nuclei}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2018.03.13} | |
} | |
@Article{bonoli+2010, | |
Title = {{On merger bias and the clustering of quasars}}, | |
Author = {{Bonoli}, S. and {Shankar}, F. and {White}, S.~D.~M. and | |
{Springel}, V. and {Wyithe}, J.~S.~B.}, | |
Journal = {\mnras}, | |
Year = {2010}, | |
Month = may, | |
Pages = {399-408}, | |
Volume = {404}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010MNRAS.404..399B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2010.16285.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1111/j.1365-2966.2010.16285.x}, | |
Eprint = {0909.0003}, | |
Keywords = {galaxies: formation, galaxies: high-redshift, quasars: | |
general, cosmology: theory, dark matter}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{boroson+2009, | |
Title = {{A candidate sub-parsec supermassive binary black hole | |
system}}, | |
Author = {{Boroson}, T.~A. and {Lauer}, T.~R.}, | |
Journal = {\nat}, | |
Year = {2009}, | |
Month = mar, | |
Pages = {53-55}, | |
Volume = {458}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009Natur.458...53B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1038/nature07779}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1038/nature07779}, | |
Eprint = {0901.3779}, | |
Primaryclass = {astro-ph.GA} | |
} | |
@Article{bower+2011, | |
Title = {{Constraining the Rate of Relativistic Jets from Tidal | |
Disruptions Using Radio Surveys}}, | |
Author = {{Bower}, G.~C.}, | |
Journal = {\apjl}, | |
Year = {2011}, | |
Month = may, | |
Pages = {L12}, | |
Volume = {732}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...732L..12B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/2041-8205/732/1/L12}, | |
Doi = {10.1088/2041-8205/732/1/L12}, | |
Eid = {L12}, | |
Eprint = {1103.4328}, | |
Keywords = {galaxies: active, radio continuum: galaxies, radio | |
continuum: general, surveys}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{bower2011, | |
Title = {{Constraining the Rate of Relativistic Jets from Tidal | |
Disruptions Using Radio Surveys}}, | |
Author = {{Bower}, G.~C.}, | |
Journal = {\apjl}, | |
Year = {2011}, | |
Month = may, | |
Pages = {L12}, | |
Volume = {732}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...732L..12B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/2041-8205/732/1/L12}, | |
Date-added = {2016-04-17 21:28:26 +0000}, | |
Date-modified = {2016-04-17 21:28:32 +0000}, | |
Doi = {10.1088/2041-8205/732/1/L12}, | |
Eid = {L12}, | |
Eprint = {1103.4328}, | |
Keywords = {galaxies: active, radio continuum: galaxies, radio | |
continuum: general, surveys}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{bower+2013, | |
Title = {{Late-time Radio Emission from X-Ray-selected Tidal | |
Disruption Events}}, | |
Author = {{Bower}, G.~C. and {Metzger}, B.~D. and {Cenko}, S.~B. and | |
{Silverman}, J.~M. and {Bloom}, J.~S.}, | |
Journal = {\apj}, | |
Year = {2013}, | |
Month = feb, | |
Pages = {84}, | |
Volume = {763}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2013ApJ...763...84B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/763/2/84}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1088/0004-637X/763/2/84}, | |
Eid = {84}, | |
Eprint = {1210.0020}, | |
Keywords = {galaxies: active, galaxies: individual: IC 3599 RX | |
J1420+5334 NGC 5905 RX J1624+7554 RX J1242{\ndash}1119 SDSS | |
J132341.97+482701.3 SDSS J131122.15{\ndash}012345.6, | |
galaxies: jets, radio continuum: galaxies}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{bower+2005, | |
Title = {{A Radio Transient 0.1 Parsecs from Sagittarius A*}}, | |
Author = {{Bower}, G.~C. and {Roberts}, D.~A. and {Yusef-Zadeh}, F. and {Backer}, D.~C. and {Cotton}, W.~D. and {Goss}, W.~M. and {Lang}, C.~C. and {Lithwick}, Y.}, | |
Journal = {\apj}, | |
Year = {2005}, | |
Month = nov, | |
Pages = {218-227}, | |
Volume = {633}, | |
Abstract = {We report the discovery of a transient radio source 2.7" (0.1 pc projected distance) south of the Galactic center massive black hole, Sgr A*. The source flared with a peak of at least 80 mJy in 2004 March. The source was resolved by the Very Large Array into two components with a separation of ~0.7" and characteristic sizes of ~0.2". The two components of the source faded with a power-law index of 1.1+/-0.1. We detect an upper limit to the proper motion of the eastern component of ~3×103 km s-1 relative to Sgr A*. We detect a proper motion of ~104 km s-1 for the western component relative to Sgr A*. The transient was also detected at X-ray wavelengths with the Chandra X-Ray Observatory and XMM-Newton and given the designation CXOGC J174540.0-290031. The X-ray source falls in between the two radio components. The maximum luminosity of the X-ray source is ~1036 ergs s-1, significantly sub-Eddington. The radio jet flux density predicted by the X-ray/radio correlation for X-ray binaries is orders of magnitude less than the measured flux density. We conclude that the radio transient is the result of a bipolar jet originating in a single impulsive event from the X-ray source and interacting with the dense interstellar medium of the Galactic center.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005ApJ...633..218B}, | |
Doi = {10.1086/444587}, | |
Eprint = {astro-ph/0507221}, | |
Keywords = {Galaxy: Center, ISM: Jets and Outflows, Radio Continuum: General, X-Rays: Binaries}, | |
Owner = {aleksey}, | |
Timestamp = {2018.05.04} | |
} | |
@Article{bowman2018, | |
Title = {An absorption profile centred at 78 megahertz in the sky-averaged spectrum}, | |
Author = {Bowman, Judd D. and Rogers, Alan E. E. and Monsalve, Raul A. and Mozdzen, Thomas J. and Mahesh, Nivedita}, | |
Journal = {Nature}, | |
Year = {2018}, | |
Month = feb, | |
Pages = {67--}, | |
Volume = {555}, | |
Owner = {aleksey}, | |
Publisher = {Macmillan Publishers Limited, part of Springer Nature. All rights reserved.}, | |
Timestamp = {2018.03.07}, | |
Url = {http://dx.doi.org/10.1038/nature25792} | |
} | |
@Article{bowman2018, | |
Title = {An absorption profile centred at 78 megahertz in the sky-averaged spectrum}, | |
Author = {Bowman, Judd D. and Rogers, Alan E. E. and Monsalve, Raul A. and Mozdzen, Thomas J. and Mahesh, Nivedita}, | |
Journal = {Nature}, | |
Year = {2018}, | |
Month = feb, | |
Pages = {67--}, | |
Volume = {555}, | |
Owner = {aleksey}, | |
Publisher = {Macmillan Publishers Limited, part of Springer Nature. All rights reserved.}, | |
Timestamp = {2018.03.07}, | |
Url = {http://dx.doi.org/10.1038/nature25792} | |
} | |
@InBook{brandenburg2003, | |
Title = {{Computational aspects of astrophysical MHD and | |
turbulence}}, | |
Author = {{Brandenburg}, A.}, | |
Editor = {{Ferriz-Mas}, A. and {N{\'u}{\~n}ez}, M.}, | |
Pages = {269}, | |
Year = {2003}, | |
Abstract = {The advantages of high-order finite difference scheme for | |
astrophysical MHD and turbulence simulations are | |
highlighted. A number of one-dimensional test cases are | |
presented ranging from various shock tests to Parker-type | |
wind solutions. Applications to magnetized accretion discs | |
and their associated outflows are discussed. Particular | |
emphasis is placed on the possibility of dynamo action in | |
three-dimensional turbulent convection and shear flows, | |
which is relevant to stars and astrophysical discs. The | |
generation of large scale fields is discussed in terms of | |
an inverse magnetic cascade and the consequences imposed by | |
magnetic helicity conservation are reviewed with particular | |
emphasis on the issue of alpha-quenching.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2003and..book..269B}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0109497}, | |
Bdsk-file-1 = {YnBsaXN0MDDUAQIDBAUGJCVYJHZlcnNpb25YJG9iamVjdHNZJGFyY2hpdmVyVCR0b3ASAAGGoKgHCBMUFRYaIVUkbnVsbNMJCgsMDxJXTlMua2V5c1pOUy5vYmplY3RzViRjbGFzc6INDoACgAOiEBGABIAFgAdccmVsYXRpdmVQYXRoWWFsaWFzRGF0YV8QMS4uLy4uLy4uLy4uL0RvY3VtZW50cy9QYXBlcnMvQnJhbmRlbmJ1cmcvMjAwMy5wZGbSFwsYGVdOUy5kYXRhTxEBnAAAAAABnAACAAAMTWFjaW50b3NoIEhEAAAAAAAAAAAAAAAAAAAAzWTSmkgrAAABPdorCDIwMDMucGRmAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAEHiH3QQUghAAAAAAAAAAAABAAEAAAJIAAAAAAAAAAAAAAAAAAAAAtCcmFuZGVuYnVyZwAAEAAIAADNZQraAAAAEQAIAADQQYBhAAAAAQAUAT3aKwEHiAQABcQqAAXEKQACEOkAAgBFTWFjaW50b3NoIEhEOlVzZXJzOgBhbGVrc2V5OgBEb2N1bWVudHM6AFBhcGVyczoAQnJhbmRlbmJ1cmc6ADIwMDMucGRmAAAOABIACAAyADAAMAAzAC4AcABkAGYADwAaAAwATQBhAGMAaQBuAHQAbwBzAGgAIABIAEQAEgAzVXNlcnMvYWxla3NleS9Eb2N1bWVudHMvUGFwZXJzL0JyYW5kZW5idXJnLzIwMDMucGRmAAATAAEvAAAVAAIADv//AACABtIbHB0eWiRjbGFzc25hbWVYJGNsYXNzZXNdTlNNdXRhYmxlRGF0YaMdHyBWTlNEYXRhWE5TT2JqZWN00hscIiNcTlNEaWN0aW9uYXJ5oiIgXxAPTlNLZXllZEFyY2hpdmVy0SYnVHJvb3SAAQAIABEAGgAjAC0AMgA3AEAARgBNAFUAYABnAGoAbABuAHEAcwB1AHcAhACOAMIAxwDPAm8CcQJ2AoECigKYApwCowKsArECvgLBAtMC1gLbAAAAAAAAAgEAAAAAAAAAKAAAAAAAAAAAAAAAAAAAAt0=}, | |
Bdsk-url-1 = {http://arXiv.org/abs/astro-ph/0109497}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/2003and..book..269B}, | |
Booktitle = {Advances in Nonlinear Dynamics}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:36 +0000}, | |
Keywords = {Untitled; Untitled1} | |
} | |
@Article{brandt+2015, | |
Title = {{Disrupted Globular Clusters Can Explain the Galactic | |
Center Gamma-Ray Excess}}, | |
Author = {{Brandt}, T.~D. and {Kocsis}, B.}, | |
Journal = {\apj}, | |
Year = {2015}, | |
Month = oct, | |
Pages = {15}, | |
Volume = {812}, | |
Abstract = {The Fermi satellite has recently detected gamma-ray | |
emission from the central regions of our Galaxy. This may | |
be evidence for dark matter particles, a major component of | |
the standard cosmological model, annihilating to produce | |
high-energy photons. We show that the observed signal may | |
instead be generated by millisecond pulsars that formed in | |
dense star clusters in the Galactic halo. Most of these | |
clusters were ultimately disrupted by evaporation and | |
gravitational tides, contributing to a spherical bulge of | |
stars and stellar remnants. The gamma-ray amplitude, | |
angular distribution, and spectral signatures of this | |
source may be predicted without free parameters, and are in | |
remarkable agreement with the observations. These | |
gamma-rays are from fossil remains of dispersed clusters, | |
telling the history of the Galactic bulge.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015ApJ...812...15B}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1507.05616}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/812/1/15}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1507.05616}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2015ApJ...812...15B}, | |
Date-added = {2017-06-10 01:32:02 +0000}, | |
Date-modified = {2017-06-10 01:32:07 +0000}, | |
Doi = {10.1088/0004-637X/812/1/15}, | |
Eid = {15}, | |
Eprint = {1507.05616}, | |
Keywords = {dark matter, Galaxy: bulge, Galaxy: center, gamma rays: | |
diffuse background, globular clusters: general, pulsars: | |
general}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{brandt+2000, | |
Title = {{On the Nature of Soft X-Ray Weak Quasi-stellar Objects}}, | |
Author = {{Brandt}, W.~N. and {Laor}, A. and {Wills}, B.~J.}, | |
Journal = {\apj}, | |
Year = {2000}, | |
Month = jan, | |
Pages = {637-649}, | |
Volume = {528}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2000ApJ...528..637B}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/308207}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1086/308207}, | |
Eprint = {arXiv:astro-ph/9908016}, | |
Keywords = {GALAXIES: ACTIVE, GALAXIES: NUCLEI, GALAXIES: QUASARS: | |
GENERAL, X-RAYS: GALAXIES} | |
} | |
@Article{breen&heggie2013, | |
Title = {{Dynamical evolution of black hole subsystems in idealized | |
star clusters}}, | |
Author = {{Breen}, P.~G. and {Heggie}, D.~C.}, | |
Journal = {\mnras}, | |
Year = {2013}, | |
Month = jul, | |
Pages = {2779-2797}, | |
Volume = {432}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2013MNRAS.432.2779B}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1093/mnras/stt628}, | |
Eprint = {1304.3401}, | |
Keywords = {methods: numerical, globular clusters: general}, | |
Owner = {aleksey}, | |
Timestamp = {2017.10.20} | |
} | |
@Article{breen&heggie2012, | |
Title = {{Gravothermal oscillations in multicomponent models of | |
star clusters}}, | |
Author = {{Breen}, P.~G. and {Heggie}, D.~C.}, | |
Journal = {\mnras}, | |
Year = {2012}, | |
Month = oct, | |
Pages = {2493-2500}, | |
Volume = {425}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012MNRAS.425.2493B}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1111/j.1365-2966.2012.21688.x}, | |
Eprint = {1207.2672}, | |
Keywords = {methods: numerical, globular clusters: general}, | |
Owner = {aleksey}, | |
Timestamp = {2017.10.20} | |
} | |
@Article{brighenti&mathews2003, | |
Title = {{Feedback Heating in Cluster and Galactic Cooling Flows}}, | |
Author = {{Brighenti}, F. and {Mathews}, W.~G.}, | |
Journal = {\apj}, | |
Year = {2003}, | |
Month = apr, | |
Pages = {580-588}, | |
Volume = {587}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2003ApJ...587..580B}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/368307}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1086/368307}, | |
Eprint = {astro-ph/0301283}, | |
Keywords = {Galaxies: Cooling Flows, Galaxies: Active, Galaxies: | |
Clusters: General, Galaxies: Elliptical and Lenticular, cD, | |
X-Rays: Galaxies, X-Rays: Galaxies: Clusters}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.02} | |
} | |
@Article{brighenti+2003, | |
Title = {{Feedback Heating in Cluster and Galactic Cooling Flows}}, | |
Author = {{Brighenti}, F. and {Mathews}, W.~G.}, | |
Journal = {\apj}, | |
Year = {2003}, | |
Month = apr, | |
Pages = {580-588}, | |
Volume = {587}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2003ApJ...587..580B}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/368307}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1086/368307}, | |
Eprint = {astro-ph/0301283}, | |
Keywords = {Galaxies: Cooling Flows, Galaxies: Active, Galaxies: | |
Clusters: General, Galaxies: Elliptical and Lenticular, cD, | |
X-Rays: Galaxies, X-Rays: Galaxies: Clusters} | |
} | |
@Article{bromberg+2011b, | |
Title = {{Are Low-luminosity Gamma-Ray Bursts Generated by | |
Relativistic Jets?}}, | |
Author = {{Bromberg}, O. and {Nakar}, E. and {Piran}, T.}, | |
Journal = {\apjl}, | |
Year = {2011}, | |
Month = oct, | |
Pages = {L55}, | |
Volume = {739}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...739L..55B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/2041-8205/739/2/L55}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1088/2041-8205/739/2/L55}, | |
Eid = {L55}, | |
Eprint = {1107.1346}, | |
Keywords = {gamma-ray burst: general, ISM: jets and outflows, methods: | |
analytical, stars: Wolf-Rayet, supernovae: general}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{bromberg+2011a, | |
Title = {{The Propagation of Relativistic Jets in External Media}}, | |
Author = {{Bromberg}, O. and {Nakar}, E. and {Piran}, T. and {Sari}, | |
R.}, | |
Journal = {\apj}, | |
Year = {2011}, | |
Month = oct, | |
Pages = {100}, | |
Volume = {740}, | |
Abstract = {Relativistic jets are ubiquitous in astrophysical systems | |
that contain compact objects. They transport large amounts | |
of energy to large distances from the source and their | |
interaction with the ambient medium has a crucial effect on | |
the evolution of the system. The propagation of the jet is | |
characterized by the formation of a shocked "head" at the | |
front of the jet which dissipates the jet's energy and a | |
cocoon that surrounds the jet and potentially collimates | |
it. We present here a self-consistent, analytic model that | |
follows the evolution of the jet and its cocoon, and | |
describes their interaction. We show that the critical | |
parameter that determines the properties of the jet-cocoon | |
system is the dimensionless ratio between the jet's energy | |
density and the rest-mass energy density of the ambient | |
medium. This parameter, together with the jet's injection | |
angle, also determines whether the jet is collimated by the | |
cocoon or not. The model is applicable to relativistic, | |
unmagnetized jets on all scales and may be used to | |
determine the conditions in active galactic nucleus (AGN) | |
jets as well as in gamma-ray bursts (GRBs) or microquasars. | |
It shows that AGN and microquasar jets are hydrodynamically | |
collimated due to the interaction with the ambient medium, | |
while GRB jets can be collimated only inside a star and | |
become uncollimated once they break out.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...740..100B}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1107.1326}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/740/2/100}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1107.1326}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2011ApJ...740..100B}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1088/0004-637X/740/2/100}, | |
Eid = {100}, | |
Eprint = {1107.1326}, | |
Keywords = {galaxies: jets, gamma-ray burst: general, hydrodynamics, | |
ISM: jets and outflows, relativistic processes; Untitled; | |
Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@ARTICLE{warren_brown2015, | |
author = {{Brown}, Warren R.}, | |
title = "{Hypervelocity Stars}", | |
journal = {\araa}, | |
year = 2015, | |
month = aug, | |
volume = {53}, | |
pages = {15-49}, | |
doi = {10.1146/annurev-astro-082214-122230}, | |
adsurl = {https://ui.adsabs.harvard.edu/abs/2015ARA&A..53...15B}, | |
adsnote = {Provided by the SAO/NASA Astrophysics Data System} | |
} | |
@Article{brown+2015, | |
Title = {{Swift J1112.2-8238: a candidate relativistic tidal | |
disruption flare}}, | |
Author = {{Brown}, G.~C. and {Levan}, A.~J. and {Stanway}, E.~R. and | |
{Tanvir}, N.~R. and {Cenko}, S.~B. and {Berger}, E. and | |
{Chornock}, R. and {Cucchiaria}, A.}, | |
Journal = {\mnras}, | |
Year = {2015}, | |
Month = oct, | |
Pages = {4297-4306}, | |
Volume = {452}, | |
Abstract = {We present observations of Swift J1112.2-8238, and | |
identify it as a candidate relativistic tidal disruption | |
flare. The outburst was first detected by Swift/Burst Alert | |
Telescope (BAT) in 2011 June as an unknown, long-lived | |
(order of days) gamma-ray transient source. We show that | |
its position is consistent with the nucleus of a faint | |
galaxy for which we establish a likely redshift of z = 0.89 | |
based on a single emission line that we interpret as the | |
blended [O II] lambda3727 doublet. At this redshift, the | |
peak X-ray/gamma-ray luminosity exceeded 1047 erg s-1, | |
while a spatially coincident optical transient source had | |
i' ˜ 22 (Mg ˜ -21.4 at z = 0.89) during early | |
observations, ˜20 d after the Swift trigger. These | |
properties place Swift J1112.2-8238 in a very similar | |
region of parameter space to the two previously identified | |
members of this class, Swift J1644+57 and Swift J2058+0516. | |
As with those events the high-energy emission shows | |
evidence for variability over the first few days, while | |
late-time observations, almost 3 yr post-outburst, | |
demonstrate that it has now switched off. Swift | |
J1112.2-8238 brings the total number of such events | |
observed by Swift to three, interestingly all detected by | |
Swift over a ˜3 month period (<3 per cent of its total | |
lifetime as of 2015 March). While this suggests the | |
possibility that further examples may be uncovered by | |
detailed searches of the BAT archives, the lack of any | |
prime candidates in the years since 2011 means these events | |
are undoubtedly rare.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015MNRAS.452.4297B}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1507.03582}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stv1520}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1507.03582}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2015MNRAS.452.4297B}, | |
Date-added = {2015-10-07 18:45:37 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1093/mnras/stv1520}, | |
Eprint = {1507.03582}, | |
Keywords = {galaxies: nuclei, gamma-rays: galaxies}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{brown+2016, | |
Title = {Observational constraints on the orbit and location of | |
Planet Nine in the outer solar system}, | |
Author = {{Brown}, Michael~E. and {Batygin}, Konstantin}, | |
Year = {2016}, | |
Month = {Mar}, | |
Abstract = {We use an extensive suite of numerical simulations to | |
constrain the mass and orbit of Planet Nine, the recently | |
proposed perturber in a distant eccentric orbit in the | |
outer solar system. We compare our simulations to the | |
observed population of aligned eccentric high semimajor | |
axis Kuiper belt objects and determine which simulation | |
parameters are statistically compatible with the | |
observations. We find that only a narrow range of orbital | |
elements can reproduce the observations. In particular, the | |
combination of semimajor axis, eccentricity, and mass of | |
Planet Nine strongly dictates the semimajor axis range of | |
the orbital confinement of the distant eccentric Kuiper | |
belt objects. Allowed orbits, which confine Kuiper belt | |
objects with semimajor axis beyond 230 AU, have perihelia | |
roughly between 200 and 350 AU, semimajor axes between 300 | |
and 900 AU, and masses of approximately 10 Earth masses. | |
Orbitally confined objects also generally have orbital | |
planes similar to that of the planet, suggesting that the | |
planet is inclined approximately 30 degrees to the | |
ecliptic. We compare the allowed orbital positions and | |
estimated brightness of Planet Nine to previous and ongoing | |
surveys which would be sensitive to the planet's detection | |
and use these surveys to rule out approximately two-thirds | |
of the planet's orbit. Planet Nine is likely near aphelion | |
with an approximate brightness of $22<V<25$. At opposition, | |
its motion, mainly due to parallax, can easily be detected | |
within 24 hours.}, | |
Adsurl = {http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1603.05712}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1603.05712v1}, | |
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Bdsk-url-1 = {http://arxiv.org/abs/1603.05712v1}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1603.05712}, | |
Date-added = {2016-03-22 15:40:44 +0000}, | |
Date-modified = {2016-03-22 15:40:44 +0000}, | |
Eprint = {1603.05712v1}, | |
Jornal = {ArXiv e-prints}, | |
Primaryclass = {astro-ph.EP} | |
} | |
@Article{buchholz+2009, | |
Title = {{Composition of the galactic center star cluster. | |
Population analysis from adaptive optics narrow band | |
spectral energy distributions}}, | |
Author = {{Buchholz}, R.~M. and {Sch{\"o}del}, R. and {Eckart}, A.}, | |
Journal = {\aap}, | |
Year = {2009}, | |
Month = may, | |
Pages = {483-501}, | |
Volume = {499}, | |
Abstract = {Context: The GC is the closest galactic nucleus, offering | |
the unique possibility of studying the population of a | |
dense stellar cluster surrounding an SMBH. Aims: The goals | |
of this work are to develop a new method of separating | |
early and late type stellar components of a dense stellar | |
cluster based on narrow band filters, applying it to the | |
central parsec of the GC, and conducting a population | |
analysis of this area. Methods: We use AO assisted | |
observations obtained at the ESO VLT in the NIR H-band and | |
7 intermediate bands covering the NIR K-band. A comparison | |
of the resulting SEDs with a blackbody of variable | |
extinction then allows us to determine the presence and | |
strength of a CO absorption feature to distinguish between | |
early and late type stars. Results: This new method is | |
suitable for classifying K giants (and later), as well as | |
B2 main sequence (and earlier) stars that are brighter than | |
15.5 mag in the K band in the central parsec. Compared to | |
previous spectroscopic investigations that are limited to | |
13-14 mag, this represents a major improvement in the depth | |
of the observations and reduces the needed observation | |
time. Extremely red objects and foreground sources can also | |
be reliably removed from the sample. Comparison to sources | |
of known classification indicates that the method has an | |
accuracy of better than ~87%. We classify 312 stars as | |
early type candidates out of a sample of 5914 sources. | |
Several results, such as the shape of the KLF and the | |
spatial distribution of both early and late type stars, | |
confirm and extend previous works. The distribution of the | |
early type stars can be fitted with a steep power law | |
(beta1'' = -1.49 $\pm$ 0.12), alternatively with a broken | |
power law, beta1-10'' = -1.08 $\pm$ 0.12, beta10-20'' = | |
-3.46 $\pm$ 0.58, since we find a drop in the early type | |
density at ~10''. We also detect early type candidates | |
outside of 0.5 pc in significant numbers for the first | |
time. The late type density function shows an inversion in | |
the inner 6'', with a power-law slope of betaR<6'' = 0.17 | |
$\pm$ 0.09. The late type KLF has a power-law slope of 0.30 | |
$\pm$ 0.01, closely resembling the KLF obtained for the | |
bulge of the Milky Way. The early type KLF has a much | |
flatter slope of (0.14 $\pm$ 0.02). Our results agree best | |
with an in-situ star formation scenario. A table of all | |
classified sources (5914) is only available in electronic | |
form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr | |
(130.79.128.5) or via | |
http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/499/483}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009A%26A...499..483B}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/0903.2135}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361/200811497}, | |
Bdsk-url-2 = {http://arxiv.org/abs/0903.2135}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2009A%26A...499..483B}, | |
Date-added = {2017-06-10 02:40:57 +0000}, | |
Date-modified = {2017-06-10 02:41:36 +0000}, | |
Doi = {10.1051/0004-6361/200811497}, | |
Eprint = {0903.2135}, | |
Keywords = {Galaxy: center, stars: early-type, stars: late-type, | |
infrared: stars} | |
} | |
@Article{burrows+2011, | |
Title = {{Relativistic jet activity from the tidal disruption of a | |
star by a massive black hole}}, | |
Author = {{Burrows}, D.~N. and {Kennea}, J.~A. and {Ghisellini}, G. | |
and {Mangano}, V. and {Zhang}, B. and {Page}, K.~L. and | |
{Eracleous}, M. and {Romano}, P. and {Sakamoto}, T. and | |
{Falcone}, A.~D. and {Osborne}, J.~P. and {Campana}, S. and | |
{Beardmore}, A.~P. et al.}, | |
Journal = {\nat}, | |
Year = {2011}, | |
Month = aug, | |
Pages = {421-424}, | |
Volume = {476}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011Natur.476..421B}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1038/nature10374}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1038/nature10374}, | |
Eprint = {1104.4787}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{bustard+2016, | |
Title = {{A Versatile Family of Galactic Wind Models}}, | |
Author = {{Bustard}, C. and {Zweibel}, E.~G. and {D'Onghia}, E.}, | |
Journal = {\apj}, | |
Year = {2016}, | |
Month = mar, | |
Pages = {29}, | |
Volume = {819}, | |
Abstract = {We present a versatile family of model galactic outflows | |
including non-uniform mass and energy source distributions, | |
a gravitational potential from an extended mass source, and | |
radiative losses. The model easily produces steady-state | |
wind solutions for a range of mass-loading factors, | |
energy-loading factors, galaxy mass, and galaxy radius. We | |
find that, with radiative losses included, highly | |
mass-loaded winds must be driven at high central | |
temperatures, whereas low mass-loaded winds can be driven | |
at low temperatures just above the peak of the cooling | |
curve, meaning radiative losses can drastically affect the | |
wind solution even for low mass-loading factors. By | |
including radiative losses, we are able to show that | |
subsonic flows can be ignored as a possible mechanism for | |
expelling mass and energy from a galaxy compared to the | |
more efficient transonic solutions. Specifically, the | |
transonic solutions with low mass loading and high energy | |
loading are the most efficient. Our model also produces | |
low-temperature, high-velocity winds that could explain the | |
prevalence of low-temperature material in observed | |
outflows. Finally, we show that our model, unlike the | |
well-known Chevalier & Clegg model, can reproduce the | |
observed linear relationship between wind X-ray luminosity | |
and star formation rate (SFR) over a large range of SFR | |
from 1-1000 M&sun; yr-1 assuming the wind mass-loading | |
factor is higher for low-mass, and hence, low-SFR galaxies. | |
We also constrain the allowed mass-loading factors that can | |
fit the observed X-ray luminosity versus SFR trend, further | |
suggesting an inverse relationship between mass loading and | |
SFR as explored in advanced numerical simulations.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016ApJ...819...29B}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1509.07130}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.3847/0004-637X/819/1/29}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1509.07130}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2016ApJ...819...29B}, | |
Date-added = {2016-12-07 18:30:51 +0000}, | |
Date-modified = {2016-12-07 18:30:51 +0000}, | |
Doi = {10.3847/0004-637X/819/1/29}, | |
Eid = {29}, | |
Eprint = {1509.07130}, | |
Keywords = {galaxies: evolution, galaxies: fundamental parameters, | |
galaxies: star formation, radiation: dynamics, X-rays: | |
galaxies} | |
} | |
@Article{cote+2006, | |
Title = {{The ACS Virgo Cluster Survey. VIII. The Nuclei of | |
Early-Type Galaxies}}, | |
Author = {{C{\^o}t{\'e}}, P. and {Piatek}, S. and {Ferrarese}, L. | |
and {Jord{\'a}n}, A. and {Merritt}, D. and {Peng}, E.~W. | |
and {Ha{\c s}egan}, M. and {Blakeslee}, J.~P. and {Mei}, S. | |
and {West}, M.~J. and {Milosavljevi{\'c}}, M. and {Tonry}, | |
J.~L.}, | |
Journal = {\apjs}, | |
Year = {2006}, | |
Month = jul, | |
Pages = {57-94}, | |
Volume = {165}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006ApJS..165...57C}, | |
Doi = {10.1086/504042}, | |
Eprint = {astro-ph/0603252}, | |
Keywords = {Galaxies: Clusters: Individual: Name: Virgo, Galaxies: | |
Elliptical and Lenticular, cD, Galaxies: Nuclei, Galaxies: | |
Structure} | |
} | |
@Article{callegari+2009, | |
Title = {{Pairing of Supermassive Black Holes in Unequal-Mass | |
Galaxy Mergers}}, | |
Author = {{Callegari}, S. and {Mayer}, L. and {Kazantzidis}, S. and | |
{Colpi}, M. and {Governato}, F. and {Quinn}, T. and | |
{Wadsley}, J.}, | |
Journal = {\apjl}, | |
Year = {2009}, | |
Month = may, | |
Pages = {L89-L92}, | |
Volume = {696}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...696L..89C}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/696/1/L89}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1088/0004-637X/696/1/L89}, | |
Eprint = {0811.0615}, | |
Keywords = {black hole physics, cosmology: theory, galaxies: | |
interactions, hydrodynamics, methods: numerical} | |
} | |
@Article{campana+2015, | |
Title = {{Multiple tidal disruption flares in the active galaxy IC | |
3599}}, | |
Author = {{Campana}, S. and {Mainetti}, D. and {Colpi}, M. and | |
{Lodato}, G. and {D'Avanzo}, P. and {Evans}, P.~A. and | |
{Moretti}, A.}, | |
Journal = {\aap}, | |
Year = {2015}, | |
Month = sep, | |
Pages = {A17}, | |
Volume = {581}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015A%26A...581A..17C}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361/201525965}, | |
Date-added = {2015-12-07 02:44:25 +0000}, | |
Date-modified = {2015-12-07 02:44:29 +0000}, | |
Doi = {10.1051/0004-6361/201525965}, | |
Eid = {A17}, | |
Eprint = {1502.07184}, | |
Keywords = {galaxies: individual: IC 3599, galaxies: active, X-rays: | |
galaxies, accretion, accretion disks}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{campanelli+2006, | |
Title = {{Accurate Evolutions of Orbiting Black-Hole Binaries | |
without Excision}}, | |
Author = {{Campanelli}, M. and {Lousto}, C.~O. and {Marronetti}, P. | |
and {Zlochower}, Y.}, | |
Journal = {Physical Review Letters}, | |
Year = {2006}, | |
Month = mar, | |
Number = {11}, | |
Pages = {111101}, | |
Volume = {96}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006PhRvL..96k1101C}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1103/PhysRevLett.96.111101}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1103/PhysRevLett.96.111101}, | |
Eid = {111101}, | |
Eprint = {arXiv:gr-qc/0511048}, | |
Keywords = {Numerical relativity, Post-Newtonian approximation, | |
perturbation theory, related approximations, Wave | |
generation and sources, Classical black holes} | |
} | |
@Article{capetti+2005, | |
Title = {{The host galaxy/AGN connection in nearby early-type | |
galaxies. Sample selection and hosts brightness profiles}}, | |
Author = {{Capetti}, A. and {Balmaverde}, B.}, | |
Journal = {\aap}, | |
Year = {2005}, | |
Month = sep, | |
Pages = {73-84}, | |
Volume = {440}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005A%26A...440...73C}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361:20053113}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1051/0004-6361:20053113}, | |
Eprint = {astro-ph/0509448}, | |
Keywords = {galaxies: active, galaxies: bulges, galaxies: elliptical | |
and lenticular, cD, galaxies: nuclei, galaxies: structure} | |
} | |
@Article{cappellari+2013, | |
Title = {{The ATLAS$^{3D}$ project - XV. Benchmark for early-type | |
galaxies scaling relations from 260 dynamical models: | |
mass-to-light ratio, dark matter, Fundamental Plane and | |
Mass Plane}}, | |
Author = {{Cappellari}, M. and {Scott}, N. and {Alatalo}, K. and | |
{Blitz}, L. and {Bois}, M. and {Bournaud}, F. and {Bureau}, | |
M. and {Crocker}, A.~F. and {Davies}, R.~L. and {Davis}, | |
T.~A. and {de Zeeuw}, P.~T. and {Duc}, P.-A. and | |
{Emsellem}, E. and {Khochfar}, S. and {Krajnovi{\'c}}, D. | |
and {Kuntschner}, H. and {McDermid}, R.~M. and {Morganti}, | |
R. and {Naab}, T. and {Oosterloo}, T. and {Sarzi}, M. and | |
{Serra}, P. and {Weijmans}, A.-M. and {Young}, L.~M.}, | |
Journal = {\mnras}, | |
Year = {2013}, | |
Month = jul, | |
Pages = {1709-1741}, | |
Volume = {432}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2013MNRAS.432.1709C}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stt562}, | |
Date-added = {2016-01-15 01:13:06 +0000}, | |
Date-modified = {2016-01-15 01:13:10 +0000}, | |
Doi = {10.1093/mnras/stt562}, | |
Eprint = {1208.3522}, | |
Keywords = {galaxies: elliptical and lenticular, cD, galaxies: | |
evolution, galaxies: formation, galaxies: kinematics and | |
dynamics, galaxies: structure}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{carlberg1990, | |
Title = {{Quasar evolution via galaxy mergers}}, | |
Author = {{Carlberg}, R.~G.}, | |
Journal = {\apj}, | |
Year = {1990}, | |
Month = feb, | |
Pages = {505-511}, | |
Volume = {350}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1990ApJ...350..505C}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/168406}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1086/168406}, | |
Keywords = {COSMOLOGY, GALACTIC EVOLUTION, INTERACTING GALAXIES, | |
QUASARS, ASTRONOMICAL MODELS, DARK MATTER, HALOS, | |
LUMINOSITY, RED SHIFT} | |
} | |
@Book{carslaw+1959, | |
Title = {{Conduction of heat in solids}}, | |
Author = {{Carslaw}, H.~S. and {Jaeger}, J.~C.}, | |
Year = {1959}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1959chs..book.....C}, | |
Booktitle = {Oxford: Clarendon Press, 1959, 2nd ed.}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:36 +0000}, | |
Keywords = {Untitled; Untitled1} | |
} | |
@Article{carson+2015, | |
Title = {{The Structure of Nuclear Star Clusters in Nearby | |
Late-type Spiral Galaxies from Hubble Space Telescope Wide | |
Field Camera 3 Imaging}}, | |
Author = {{Carson}, D.~J. and {Barth}, A.~J. and {Seth}, A.~C. and | |
{den Brok}, M. and {Cappellari}, M. and {Greene}, J.~E. and | |
{Ho}, L.~C. and {Neumayer}, N.}, | |
Journal = {\aj}, | |
Year = {2015}, | |
Month = may, | |
Pages = {170}, | |
Volume = {149}, | |
Abstract = {We obtained Hubble Space Telescope/Wide Field Camera 3 | |
imaging of a sample of ten of the nearest and brightest | |
nuclear clusters (NCs) residing in late-type spiral | |
galaxies, in seven bands that span the near-UV to the | |
near-IR. Structural properties of the clusters were | |
measured by fitting two-dimensional surface brightness | |
profiles to the images using GALFIT. The clusters exhibit a | |
wide range of structural properties, with F814W absolute | |
magnitudes that range from -11.2 to -15.1 mag and F814W | |
effective radii that range from 1.4 to 8.3 pc. For 6 of the | |
10 clusters in our sample, we find changes in the effective | |
radius with wavelength, suggesting radially varying stellar | |
populations. In four of the objects, the effective radius | |
increases with wavelength, indicating the presence of a | |
younger population that is more concentrated than the bulk | |
of the stars in the cluster. However, we find a general | |
decrease in effective radius with wavelength in two of the | |
objects in our sample, which may indicate extended, | |
circumnuclear star formation. We also find a general trend | |
of increasing roundness of the clusters at longer | |
wavelengths, as well as a correlation between the axis | |
ratios of the NCs and their host galaxies. These | |
observations indicate that blue disks aligned with the host | |
galaxy plane are a common feature of NCs in late-type | |
galaxies, but are difficult to detect in galaxies that are | |
close to face-on. In color--color diagrams spanning the | |
near-UV through the near-IR, most of the clusters lie far | |
from single-burst evolutionary tracks, showing evidence for | |
multi-age populations. Most of the clusters have integrated | |
colors consistent with a mix of an old population (>1 Gyr) | |
and a young population (~100--300 Myr). The wide wavelength | |
coverage of our data provides a sensitivity to populations | |
with a mix of ages that would not be possible to achieve | |
with imaging in optical bands only. The surface brightness | |
profiles presented in this work will be used for future | |
stellar population modeling and dynamical studies of the | |
clusters. Based on observations made with the NASA/ESA | |
Hubble Space Telescope, obtained at the Space Telescope | |
Science Institute, which is operated by the Association of | |
Universities for Research in Astronomy, Inc., under NASA | |
contract NAS 5-26555. These observations are associated | |
with program GO-12163.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015AJ....149..170C}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1501.05586}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-6256/149/5/170}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1501.05586}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2015AJ....149..170C}, | |
Date-added = {2015-10-07 18:47:31 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1088/0004-6256/149/5/170}, | |
Eid = {170}, | |
Eprint = {1501.05586}, | |
Keywords = {galaxies: nuclei, galaxies: spiral, galaxies: star | |
clusters: general} | |
} | |
@Article{carson+2015a, | |
Title = {{The Structure of Nuclear Star Clusters in Nearby | |
Late-type Spiral Galaxies from Hubble Space Telescope Wide | |
Field Camera 3 Imaging}}, | |
Author = {{Carson}, D.~J. and {Barth}, A.~J. and {Seth}, A.~C. and | |
{den Brok}, M. and {Cappellari}, M. and {Greene}, J.~E. and | |
{Ho}, L.~C. and {Neumayer}, N.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2015}, | |
Month = jan, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015arXiv150105586C}, | |
Archiveprefix = {arXiv}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {1501.05586}, | |
Keywords = {Astrophysics - Astrophysics of Galaxies; Untitled; | |
Untitled1} | |
} | |
@Article{carter+1982, | |
Title = {{Pancake detonation of stars by black holes in galactic | |
nuclei}}, | |
Author = {{Carter}, B. and {Luminet}, J.~P.}, | |
Journal = {\nat}, | |
Year = {1982}, | |
Month = mar, | |
Pages = {211-214}, | |
Volume = {296}, | |
Abstract = {Recent efforts to understand exotic phenomena in galactic | |
nuclei commonly postulate the presence of a massive black | |
hole accreting gas produced by tidal or collisional | |
disruption of stars. For black holes in the mass range | |
10,000 to 10,000,000 solar masses, individual stars | |
penetrating well inside the Roche radius will undergo | |
compression to a short-lived pancake configuration very | |
similar to that produced by a high velocity symmetric | |
collision of the kind likely to occur in the neighborhood | |
of black holes in the higher mass range greater than about | |
10 to the 9th solar masses. Thermonuclear energy release | |
ensuing in the more extreme events may be sufficient to | |
modify substantially the working of the entire accretion | |
process.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1982Natur.296..211C}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1038/296211a0}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1982Natur.296..211C}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1038/296211a0}, | |
Keywords = {Black Holes (Astronomy), Galactic Nuclei, Stellar Models, | |
Collisions, Compressing, Detonation, Stellar Mass | |
Accretion, Thermonuclear Reactions} | |
} | |
@Article{cenko+2012, | |
Title = {{Swift J2058.4+0516: Discovery of a Possible Second | |
Relativistic Tidal Disruption Flare?}}, | |
Author = {{Cenko}, S.~B. and {Krimm}, H.~A. and {Horesh}, A. and | |
{Rau}, A. and {Frail}, D.~A. and {Kennea}, J.~A. and | |
{Levan}, A.~J. and {Holland}, S.~T. and others}, | |
Journal = {\apj}, | |
Year = {2012}, | |
Month = jul, | |
Pages = {77}, | |
Volume = {753}, | |
Abstract = {We report the discovery by the Swift hard X-ray monitor of | |
the transient source Swift J2058.4+0516 (Sw J2058+05). Our | |
multi-wavelength follow-up campaign uncovered a long-lived | |
(duration >~ months), luminous X-ray (L X, iso ≈ 3 × | |
1047 erg s-1) and radio (nuL nu, iso ≈ 1042 erg s-1) | |
counterpart. The associated optical emission, however, from | |
which we measure a redshift of 1.1853, is relatively faint, | |
and this is not due to a large amount of dust extinction in | |
the host galaxy. Based on numerous similarities with the | |
recently discovered GRB 110328A/Swift J164449.3+573451 (Sw | |
J1644+57), we suggest that Sw J2058+05 may be the second | |
member of a new class of relativistic outbursts resulting | |
from the tidal disruption of a star by a supermassive black | |
hole. If so, the relative rarity of these sources (compared | |
with the expected rate of tidal disruptions) implies that | |
either these outflows are extremely narrowly collimated | |
(theta < 1$\,^{\circ}$) or only a small fraction of tidal | |
disruptions generate relativistic ejecta. Analogous to the | |
case of long-duration gamma-ray bursts and core-collapse | |
supernovae, we speculate that rapid spin of the black hole | |
may be a necessary condition to generate the relativistic | |
component. Alternatively, if powered by gas accretion | |
(i.e., an active galactic nucleus (AGN)), Sw J2058+05 would | |
seem to represent a new mode of variability in these | |
sources, as the observed properties appear largely | |
inconsistent with known classes of AGNs capable of | |
generating relativistic jets (blazars, narrow-line Seyfert | |
1 galaxies).}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012ApJ...753...77C}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1107.5307}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/753/1/77}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1107.5307}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2012ApJ...753...77C}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:39 +0000}, | |
Doi = {10.1088/0004-637X/753/1/77}, | |
Eid = {77}, | |
Eprint = {1107.5307}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: | |
nuclei, X-rays: bursts, X-rays: individual: Sw J1644+57}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{chae+2014, | |
Title = {{Modelling mass distribution in elliptical galaxies: mass | |
profiles and their correlation with velocity dispersion | |
profiles}}, | |
Author = {{Chae}, K.-H. and {Bernardi}, M. and {Kravtsov}, A.~V.}, | |
Journal = {\mnras}, | |
Year = {2014}, | |
Month = feb, | |
Pages = {3670-3687}, | |
Volume = {437}, | |
Abstract = {We assemble a statistical set of global mass models for | |
˜2000 nearly spherical Sloan Digital Sky Survey (SDSS) | |
galaxies at a mean redshift of <z> = 0.12 based on their | |
aperture velocity dispersions and newly derived luminosity | |
profiles in conjunction with published velocity dispersion | |
profiles and empirical properties and relations of galaxy | |
and halo parameters. When two-component (i.e. stellar plus | |
dark) mass models are fitted to the SDSS aperture velocity | |
dispersions, the predicted velocity dispersion profile (VP) | |
slopes within the effective (i.e. projected half-light) | |
radius Reff match well the distribution in observed | |
elliptical galaxies. From a number of input variations the | |
models exhibit for the radial range 0.1Reff < r < Reff a | |
tight correlation <gammae> = (1.865 $\pm$ 0.008) + (-4.93 | |
$\pm$ 0.15)<eta> where <gammae> is the mean slope absolute | |
value of the total mass density and <eta> is the mean slope | |
of the velocity dispersion profile, which leads to a | |
super-isothermal <gammae> = 2.15 $\pm$ 0.04 for <eta> = | |
-0.058 $\pm$ 0.008 in observed elliptical galaxies. | |
Furthermore, the successful two-component models appear to | |
imply a typical slope curvature pattern in the total mass | |
profile because for the observed steep luminosity (stellar | |
mass) profile and the weak lensing inferred halo profile at | |
large radii a total mass profile with monotonically varying | |
slope would require too high dark matter density in the | |
optical region giving rise to too large aperture velocity | |
dispersion and too shallow VP.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014MNRAS.437.3670C}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1305.5471}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stt2163}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1305.5471}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014MNRAS.437.3670C}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1093/mnras/stt2163}, | |
Eprint = {1305.5471}, | |
Keywords = {galaxies: elliptical and lenticular, cD, galaxies: | |
formation, galaxies: haloes, galaxies: kinematics and | |
dynamics, galaxies: structure, dark matter}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{chang+2010, | |
Title = {{Fossil gas and the electromagnetic precursor of | |
supermassive binary black hole mergers}}, | |
Author = {Chang, P and Strubbe, L.\~{}E. and Menou, K and Quataert, | |
E}, | |
Journal = {\mnras}, | |
Year = {2010}, | |
Month = sep, | |
Pages = {2007--2016}, | |
Volume = {407}, | |
Archiveprefix = {arXiv}, | |
Arxivid = {astro-ph.HE/0906.0825}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2010.17056.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1111/j.1365-2966.2010.17056.x}, | |
Eprint = {0906.0825}, | |
Keywords = {accretion discs, binaries: general, black hole physics, | |
galaxies: active, galaxies: nuclei, gravitational waves, | |
quasars: general,accretion; Untitled; Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{chapon+2013, | |
Title = {{Hydrodynamics of galaxy mergers with supermassive black | |
holes: is there a last parsec problem?}}, | |
Author = {Chapon, D and Mayer, L and Teyssier, R}, | |
Journal = {\mnras}, | |
Year = {2013}, | |
Month = mar, | |
Pages = {3114--3122}, | |
Volume = {429}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/sts568}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1093/mnras/sts568}, | |
Keywords = {galaxies: interactions, galaxies: structure, gravitational | |
waves, hydrodynamics, methods: numerical,black hole | |
physics} | |
} | |
@Article{charisi+2016, | |
Title = {{A population of short-period variable quasars from PTF as | |
supermassive black hole binary candidates}}, | |
Author = {{Charisi}, M. and {Bartos}, I. and {Haiman}, Z. and | |
{Price-Whelan}, A.~M. and {Graham}, M.~J. and {Bellm}, | |
E.~C. and {Laher}, R.~R. and {M{\'a}rka}, S.}, | |
Journal = {\mnras}, | |
Year = {2016}, | |
Month = dec, | |
Pages = {2145-2171}, | |
Volume = {463}, | |
Abstract = {Supermassive black hole binaries (SMBHBs) at sub-parsec | |
separations should be common in galactic nuclei, as a | |
result of frequent galaxy mergers. Hydrodynamical | |
simulations of circum-binary discs predict strong periodic | |
modulation of the mass accretion rate on time-scales | |
comparable to the orbital period of the binary. As a | |
result, SMBHBs may be recognized by the periodic modulation | |
of their brightness. We conducted a statistical search for | |
periodic variability in a sample of 35 383 | |
spectroscopically confirmed quasars in the photometric data | |
base of the Palomar Transient Factory (PTF). We analysed | |
Lomb-Scargle periodograms and assessed the significance of | |
our findings by modelling each individual quasar's | |
variability as a damped random walk (DRW). We identified 50 | |
quasars with significant periodicity beyond the DRW model, | |
typically with short periods of a few hundred days. We find | |
33 of these to remain significant after a re-analysis of | |
their periodograms including additional optical data from | |
the intermediate-PTF and the Catalina Real-Time Transient | |
Survey. Assuming that the observed periods correspond to | |
the redshifted orbital periods of SMBHBs, we conclude that | |
our findings are consistent with a population of | |
unequal-mass SMBHBs, with a typical mass ratio as low as q | |
≡ M2/M1 ≈ 0.01.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016MNRAS.463.2145C}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1604.01020}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stw1838}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1604.01020}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2016MNRAS.463.2145C}, | |
Date-added = {2017-06-03 20:02:35 +0000}, | |
Date-modified = {2017-06-03 20:02:40 +0000}, | |
Doi = {10.1093/mnras/stw1838}, | |
Eprint = {1604.01020}, | |
Keywords = {quasars: supermassive black holes} | |
} | |
@Article{chevalier&clegg1985, | |
Title = {{Wind from a starburst galaxy nucleus}}, | |
Author = {{Chevalier}, R.~A. and {Clegg}, A.~W.}, | |
Journal = {\nat}, | |
Year = {1985}, | |
Month = sep, | |
Pages = {44}, | |
Volume = {317}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1985Natur.317...44C}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1038/317044a0}, | |
Date-added = {2016-12-07 18:33:31 +0000}, | |
Date-modified = {2016-12-07 18:33:43 +0000}, | |
Doi = {10.1038/317044a0}, | |
Keywords = {Galactic Nuclei, Starburst Galaxies, Stellar Winds, | |
Supernovae, Astronomical Models, Galactic Radiation, Gas | |
Pressure, X Ray Sources} | |
} | |
@Article{choiwiita+2007, | |
Title = {{Hydrodynamic Interactions of Relativistic Extragalactic | |
Jets with Dense Clouds}}, | |
Author = {{Choi}, E. and {Wiita}, P.~J. and {Ryu}, D.}, | |
Journal = {\apj}, | |
Year = {2007}, | |
Month = feb, | |
Pages = {769-780}, | |
Volume = {655}, | |
Abstract = {We have studied three-dimensional hydrodynamic | |
interactions of relativistic extragalactic jets with | |
two-phase ambient media. These jets propagate through a | |
denser homogeneous gas and then impact clouds with | |
densities 100 to 1000 times higher than the initial beam | |
density. The deflection angle of the jet is influenced more | |
by the density contrast of the cloud than by the beam Mach | |
number of the jet. A relativistic jet with low relativistic | |
beam Mach number can eventually be slightly bent after it | |
crosses the dense cloud; however, we have not seen | |
permanently bent structures in the interaction of a high | |
relativistic beam Mach number jet with a cloud. The | |
relativistic jet impacts on dense clouds do not necessarily | |
destroy the clouds completely, and much of the cloud body | |
can survive as a coherent blob. This enhancement of cloud | |
durability is partly due to the geometric influence of the | |
off-axis collisions we consider and also arises from the | |
lower rate of cloud fragmentation through the | |
Kelvin-Helmholtz instability for relativistic jets. To | |
compare our simulations with observed extragalactic radio | |
jets, we have computed the approximate surface | |
distributions of synchrotron emission at different viewing | |
angles. These surface intensity maps show that relativistic | |
jets interacting with clouds can produce synchrotron | |
emission knots similar to structures observed in many | |
VLBI-scale radio sources. We find that the synchrotron | |
emission increases steeply at the moment of impact and the | |
emission peaks right before the jet passes through the | |
cloud.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...655..769C}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/0610474}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1086/510120}, | |
Bdsk-url-2 = {http://arxiv.org/abs/astro-ph/0610474}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2007ApJ...655..769C}, | |
Date-added = {2016-04-26 01:40:16 +0000}, | |
Date-modified = {2016-04-26 01:46:11 +0000}, | |
Doi = {10.1086/510120}, | |
Eprint = {astro-ph/0610474}, | |
Keywords = {Galaxies: Active, Galaxies: Jets, Hydrodynamics, ISM: | |
Clouds, Methods: Numerical, Relativity} | |
} | |
@Article{chomiuk+2013, | |
Title = {{A Radio-selected Black Hole X-Ray Binary Candidate in the | |
Milky Way Globular Cluster M62}}, | |
Author = {{Chomiuk}, L. and {Strader}, J. and {Maccarone}, T.~J. and | |
{Miller-Jones}, J.~C.~A. and {Heinke}, C. and {Noyola}, E. | |
and {Seth}, A.~C. and {Ransom}, S. }, | |
Journal = {\apj}, | |
Year = {2013}, | |
Month = nov, | |
Pages = {69}, | |
Volume = {777}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2013ApJ...777...69C}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1088/0004-637X/777/1/69}, | |
Eid = {69}, | |
Eprint = {1306.6624}, | |
Keywords = {black hole physics, globular clusters: individual: M62, | |
radio continuum: general, X-rays: general}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2017.12.25} | |
} | |
@Article{chornock+2014, | |
Title = {{The Ultraviolet-bright, Slowly Declining Transient | |
PS1-11af as a Partial Tidal Disruption Event}}, | |
Author = {{Chornock}, R. and {Berger}, E. and {Gezari}, S. and | |
{Zauderer}, B.~A. and {Rest}, A. and {Chomiuk}, L. and | |
{Kamble}, A. and {Soderberg}, A.~M. and {Czekala}, I. and | |
{Dittmann}, J. and {Drout}, M. and {Foley}, R.~J. and | |
{Fong}, W. and {Huber}, M.~E. and {Kirshner}, R.~P. and | |
{Lawrence}, A. and {Lunnan}, R. and {Marion}, G.~H. and | |
{Narayan}, G. and {Riess}, A.~G. and {Roth}, K.~C. and | |
{Sanders}, N.~E. and {Scolnic}, D. and {Smartt}, S.~J. and | |
{Smith}, K. and {Stubbs}, C.~W. and {Tonry}, J.~L. and | |
{Burgett}, W.~S. and {Chambers}, K.~C. and {Flewelling}, H. | |
and {Hodapp}, K.~W. and {Kaiser}, N. and {Magnier}, E.~A. | |
and {Martin}, D.~C. and {Neill}, J.~D. and {Price}, P.~A. | |
and {Wainscoat}, R.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = jan, | |
Pages = {44}, | |
Volume = {780}, | |
Abstract = {We present the Pan-STARRS1 discovery of the long-lived and | |
blue transient PS1-11af, which was also detected by Galaxy | |
Evolution Explorer with coordinated observations in the | |
near-ultraviolet (NUV) band. PS1-11af is associated with | |
the nucleus of an early type galaxy at redshift z = 0.4046 | |
that exhibits no evidence for star formation or active | |
galactic nucleus activity. Four epochs of spectroscopy | |
reveal a pair of transient broad absorption features in the | |
UV on otherwise featureless spectra. Despite the | |
superficial similarity of these features to P-Cygni | |
absorptions of supernovae (SNe), we conclude that PS1-11af | |
is not consistent with the properties of known types of | |
SNe. Blackbody fits to the spectral energy distribution are | |
inconsistent with the cooling, expanding ejecta of a SN, | |
and the velocities of the absorption features are too high | |
to represent material in homologous expansion near a SN | |
photosphere. However, the constant blue colors and slow | |
evolution of the luminosity are similar to previous | |
optically selected tidal disruption events (TDEs). The | |
shape of the optical light curve is consistent with models | |
for TDEs, but the minimum accreted mass necessary to power | |
the observed luminosity is only ~0.002 M &sun;, which | |
points to a partial disruption model. A full disruption | |
model predicts higher bolometric luminosities, which would | |
require most of the radiation to be emitted in a separate | |
component at high energies where we lack observations. In | |
addition, the observed temperature is lower than that | |
predicted by pure accretion disk models for TDEs and | |
requires reprocessing to a constant, lower temperature. | |
Three deep non-detections in the radio with the Very Large | |
Array over the first two years after the event set strict | |
limits on the production of any relativistic outflow | |
comparable to Swift J1644+57, even if off-axis.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...780...44C}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1309.3009}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/780/1/44}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1309.3009}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014ApJ...780...44C}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/780/1/44}, | |
Eid = {44}, | |
Eprint = {1309.3009}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: | |
nuclei}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{chornock+2009, | |
Title = {{SDSS J1536+0441: An Extreme ''Double-peaked Emitter,'' | |
Not a Binary Black Hole}}, | |
Author = {{Chornock}, R. and {Bloom}, J.~S. and {Cenko}, S.~B. and | |
{Silverman}, J.~M. and {Filippenko}, A.~V. and {Hicks}, | |
M.~D. and {Lawrence}, K.~J. and {Chang}, P. and | |
{Comerford}, J.~M. and {George}, M.~R. and {Modjaz}, M. and | |
{Oishi}, J.~S. and {Quataert}, E. and {Strubbe}, L.~E.}, | |
Journal = {The Astronomer's Telegram}, | |
Year = {2009}, | |
Month = mar, | |
Pages = {1}, | |
Volume = {1955}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ATel.1955....1C}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Keywords = {Optical, AGN, Binaries, Black Holes, Quasars; Untitled; | |
Untitled1} | |
} | |
@Article{ciotti+1991, | |
Title = {{Winds, outflows, and inflows in X-ray elliptical | |
galaxies.}}, | |
Author = {{Ciotti}, L. and {D'Ercole}, A. and {Pellegrini}, S. and | |
{Renzini}, A.}, | |
Journal = {\apj}, | |
Year = {1991}, | |
Month = aug, | |
Pages = {380-403}, | |
Volume = {376}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1991ApJ...376..380C}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/170289}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/170289}, | |
Keywords = {Elliptical Galaxies, Galactic Radiation, X Ray Sources, | |
Dark Matter, Stellar Winds, Supernovae} | |
} | |
@Article{ciotti&ostriker2007, | |
Title = {{Radiative Feedback from Massive Black Holes in Elliptical | |
Galaxies: AGN Flaring and Central Starburst Fueled by | |
Recycled Gas}}, | |
Author = {{Ciotti}, L. and {Ostriker}, J.~P.}, | |
Journal = {\apj}, | |
Year = {2007}, | |
Month = aug, | |
Pages = {1038-1056}, | |
Volume = {665}, | |
Abstract = {We show how the observed AGN radiative output from massive | |
black holes at the centers of elliptical galaxies affects | |
the hot ISM of these systems with the aid of a | |
high-resolution hydrodynamical code, where the cooling and | |
heating functions include photoionization plus Compton | |
heating. Radiative heating is a key factor in the | |
self-regulated coevolution of massive BHs and their host | |
galaxies, and (1) the mass accumulated by the central BH is | |
limited by feedback to the range observed today and (2) | |
relaxation instabilities occur so that duty cycles are | |
small enough (<~0.03) to account for the very small | |
fraction of massive ellipticals observed to be in the | |
``on'' QSO phase, when the accretion luminosity approaches | |
the Eddington luminosity. The duty cycle of the hot bubbles | |
inflated at the galactic center during major accretion | |
episodes is of the order of >~0.1-0.4. Major accretion | |
episodes caused by cooling flows in the recycled gas | |
produced by normal stellar evolution trigger nuclear | |
starbursts coincident with AGN flaring. Overall, in the | |
bursting phase (1<~z<~3), the duty cycle of the BH in its | |
``on'' phase is of the order of percents and is unobscured | |
approximately one-third of the time, the obscuration | |
occurring during dusty starbursts. Roughly half of the | |
recycled gas from dying stars is ejected as galactic winds, | |
half is consumed in central starbursts, and less than 1% is | |
accreted onto the central BH. Mechanical energy output from | |
nonrelativistic gas winds integrates to 2.3×1059 ergs, | |
with most of it caused by broad-line AGN outflows. We | |
predict the typical properties of the very metal-rich | |
poststarburst central regions and show that the resulting | |
surface density profiles are well described by S{\'e}rsic | |
profiles.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...665.1038C}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0703057}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1086/519833}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0703057}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2007ApJ...665.1038C}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/519833}, | |
Eprint = {astro-ph/0703057}, | |
Keywords = {Accretion, Accretion Disks, Black Hole Physics, Galaxies: | |
Active, Galaxies: Nuclei, Galaxies: Starburst, Galaxies: | |
Quasars: General; Untitled; Untitled1} | |
} | |
@Article{ciotti+2007a, | |
Title = {{Radiative Feedback from Massive Black Holes in Elliptical | |
Galaxies: AGN Flaring and Central Starburst Fueled by | |
Recycled Gas}}, | |
Author = {{Ciotti}, L. and {Ostriker}, J.~P.}, | |
Journal = {\apj}, | |
Year = {2007}, | |
Month = aug, | |
Pages = {1038-1056}, | |
Volume = {665}, | |
Abstract = {We show how the observed AGN radiative output from massive | |
black holes at the centers of elliptical galaxies affects | |
the hot ISM of these systems with the aid of a | |
high-resolution hydrodynamical code, where the cooling and | |
heating functions include photoionization plus Compton | |
heating. Radiative heating is a key factor in the | |
self-regulated coevolution of massive BHs and their host | |
galaxies, and (1) the mass accumulated by the central BH is | |
limited by feedback to the range observed today and (2) | |
relaxation instabilities occur so that duty cycles are | |
small enough (<~0.03) to account for the very small | |
fraction of massive ellipticals observed to be in the | |
``on'' QSO phase, when the accretion luminosity approaches | |
the Eddington luminosity. The duty cycle of the hot bubbles | |
inflated at the galactic center during major accretion | |
episodes is of the order of >~0.1-0.4. Major accretion | |
episodes caused by cooling flows in the recycled gas | |
produced by normal stellar evolution trigger nuclear | |
starbursts coincident with AGN flaring. Overall, in the | |
bursting phase (1<~z<~3), the duty cycle of the BH in its | |
``on'' phase is of the order of percents and is unobscured | |
approximately one-third of the time, the obscuration | |
occurring during dusty starbursts. Roughly half of the | |
recycled gas from dying stars is ejected as galactic winds, | |
half is consumed in central starbursts, and less than 1% is | |
accreted onto the central BH. Mechanical energy output from | |
nonrelativistic gas winds integrates to 2.3×1059 ergs, | |
with most of it caused by broad-line AGN outflows. We | |
predict the typical properties of the very metal-rich | |
poststarburst central regions and show that the resulting | |
surface density profiles are well described by S{\'e}rsic | |
profiles.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...665.1038C}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0703057}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1086/519833}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0703057}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2007ApJ...665.1038C}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/519833}, | |
Eprint = {astro-ph/0703057}, | |
Keywords = {Accretion, Accretion Disks, Black Hole Physics, Galaxies: | |
Active, Galaxies: Nuclei, Galaxies: Starburst, Galaxies: | |
Quasars: General; Untitled; Untitled1} | |
} | |
@Article{ciotti+2010, | |
Title = {{Feedback from Central Black Holes in Elliptical Galaxies. | |
III. Models with Both Radiative and Mechanical Feedback}}, | |
Author = {{Ciotti}, L. and {Ostriker}, J.~P. and {Proga}, D.}, | |
Journal = {\apj}, | |
Year = {2010}, | |
Month = jul, | |
Pages = {708-723}, | |
Volume = {717}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010ApJ...717..708C}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/717/2/708}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/717/2/708}, | |
Eprint = {1003.0578}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: | |
active, galaxies: nuclei, galaxies: starburst, quasars: | |
general}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{claeys+2014, | |
Title = {{Theoretical uncertainties of the Type Ia supernova rate}}, | |
Author = {{Claeys}, J.~S.~W. and {Pols}, O.~R. and {Izzard}, R.~G. and {Vink}, J. | |
and {Verbunt}, F.~W.~M.}, | |
Journal = {\aap}, | |
Year = {2014}, | |
Month = Mar, | |
Volume = {563}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {https://ui.adsabs.harvard.edu/#abs/2014A&A...563A..83C}, | |
Doi = {10.1051/0004-6361/201322714}, | |
Keywords = {binaries: general, stars: evolution, supernovae: general, Astrophysics - | |
Solar and Stellar Astrophysics} | |
} | |
@InProceedings{cohn1985, | |
Title = {{Direct Fokker-Planck calculations}}, | |
Author = {{Cohn}, H.}, | |
Booktitle = {Dynamics of Star Clusters}, | |
Year = {1985}, | |
Editor = {{Goodman}, J. and {Hut}, P.}, | |
Pages = {161-177}, | |
Series = {IAU Symposium}, | |
Volume = {113}, | |
Abstract = {The use of direct Fokker-Planck calculations for studying | |
star cluster evolution is discussed. Cohn's (1978, 1979) | |
basic algorithm for spherical systems of identical point | |
masses and its application to the study of core collapse is | |
reviewed. Extensions by Merritt (1981) to treat a mass | |
spectrum and by Goodman (1983) to include strong scattering | |
and cluster rotation are discussed. The application of this | |
method to the study of core collapse and cluster life | |
thereafter is reviewed. Prospects for future development of | |
the method are discussed, emphasizing the development of | |
physical realistic models for interpreting Hubble Space | |
Telescope observations of globular cluster structure.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1985IAUS..113..161C}, | |
Keywords = {Computational Astrophysics, Fokker-Planck Equation, Star | |
Clusters, Stellar Evolution, Black Holes (Astronomy), | |
Gravitational Collapse, Hubble Space Telescope, Stellar | |
Rotation}, | |
Owner = {aleksey}, | |
Timestamp = {2018.01.03} | |
} | |
@Article{cohn&kulsrud1978, | |
Title = {{The stellar distribution around a black hole - Numerical | |
integration of the Fokker-Planck equation}}, | |
Author = {{Cohn}, H. and {Kulsrud}, R.~M.}, | |
Journal = {\apj}, | |
Year = {1978}, | |
Month = dec, | |
Pages = {1087-1108}, | |
Volume = {226}, | |
Abstract = {The steady-state stellar distribution around a central | |
black hole in a star cluster is determined by means of a | |
direct numerical integration of the Fokker-Planck equation | |
in energy-angular momentum space. The loss cone in phase | |
space resulting from tidal destruction of stars is treated | |
by means of a detailed boundary-layer analysis. The process | |
of stellar destruction by direct physical collisions is | |
treated by use of the physical collision cross section. The | |
two-dimensional steady-state distribution function, the | |
density and velocity dispersion profiles of the stellar | |
distribution, and stellar consumption rates are presented | |
for black holes in globular cluster environments. The | |
distribution function obtained is in reasonable agreement | |
with that resulting from the Monte Carlo simulations of | |
Shapiro and Marchant (1978); the present loss rate is | |
larger than theirs by a factor of 2.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1978ApJ...226.1087C}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/156685}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1978ApJ...226.1087C}, | |
Date-added = {2016-01-25 18:24:45 +0000}, | |
Date-modified = {2016-01-25 18:24:59 +0000}, | |
Doi = {10.1086/156685}, | |
Keywords = {Black Holes (Astronomy), Fokker-Planck Equation, Numerical | |
Integration, Star Distribution, Stellar Motions, Boundary | |
Layer Equations, Collision Parameters, Density | |
Distribution, Diffusion Coefficient, Distribution | |
Functions, Globular Clusters, Monte Carlo Method, Plasma | |
Loss, Star Clusters, Steady State, Velocity Distribution} | |
} | |
@Article{colpi+2009, | |
Title = {{Massive black hole binary evolution in gas-rich | |
mergers}}, | |
Author = {{Colpi}, M. and {Callegari}, S. and {Dotti}, M. and | |
{Mayer}, L.}, | |
Journal = {Classical and Quantum Gravity}, | |
Year = {2009}, | |
Month = may, | |
Number = {9}, | |
Pages = {094029}, | |
Volume = {26}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009CQGra..26i4029C}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0264-9381/26/9/094029}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0264-9381/26/9/094029}, | |
Eid = {094029}, | |
Eprint = {0904.0385}, | |
Primaryclass = {astro-ph.GA} | |
} | |
@Article{comerford+2011, | |
Title = {{Chandra Observations of a 1.9 kpc Separation Double X-Ray | |
Source in a Candidate Dual Active Galactic Nucleus Galaxy | |
at z = 0.16}}, | |
Author = {Comerford, Julia M and Pooley, David and Gerke, Brian F | |
and Madejski, Greg M}, | |
Journal = {\apjl}, | |
Year = {2011}, | |
Month = aug, | |
Pages = {L19}, | |
Volume = {737}, | |
Abstract = {We report Chandra observations of a double X-ray source in | |
the z = 0.1569 galaxy SDSS J171544.05+600835.7. The galaxy | |
was initially identified as a dual active galactic nucleus | |
(AGN) candidate based on the double-peaked [O III] | |
$\lambda$5007 emission lines, with a line-of-sight velocity | |
separation of 350 km s-1, in its Sloan Digital Sky Survey | |
spectrum. We used the Kast Spectrograph at Lick Observatory | |
to obtain two long-slit spectra of the galaxy at two | |
different position angles, which reveal that the two Type 2 | |
AGN emission components have not only a velocity offset, | |
but also a projected spatial offset of 1.9 h -1 70 kpc on | |
the sky. Chandra/ACIS observations of two X-ray sources | |
with the same spatial offset and orientation as the optical | |
emission suggest that the galaxy most likely contains | |
Compton-thick dual AGNs, although the observations could | |
also be explained by AGN jets. Deeper X-ray observations | |
that reveal Fe K lines, if present, would distinguish | |
between the two scenarios. The observations of a double | |
X-ray source in SDSS J171544.05+600835.7 are a proof of | |
concept for a new, systematic detection method that selects | |
promising dual AGN candidates from ground-based | |
spectroscopy that exhibits both velocity and spatial | |
offsets in the AGN emission features.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2011ApJ...737L..19C%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1088/2041-8205/737/1/L19}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/2041-8205/737/1/L19}, | |
Keywords = {galaxies: active, galaxies: interactions, galaxies: | |
nuclei,galaxies: individual: SDSS J171544.05+600835.7}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2011ApJ...737L..19C\&link\_type=ABSTRACT} | |
} | |
@Article{corbin+2010, | |
Title = {{Pulsar Timing Array Observations of Massive Black Hole | |
Binaries}}, | |
Author = {{Corbin}, V. and {Cornish}, N.~J.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2010}, | |
Month = aug, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010arXiv1008.1782C}, | |
Archiveprefix = {arXiv}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {1008.1782}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena, | |
General Relativity and Quantum Cosmology; Untitled; | |
Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{coriat+2012, | |
Title = {{Revisiting a fundamental test of the disc instability | |
model for X-ray binaries}}, | |
Author = {{Coriat}, M. and {Fender}, R.~P. and {Dubus}, G.}, | |
Journal = {\mnras}, | |
Year = {2012}, | |
Month = aug, | |
Pages = {1991-2001}, | |
Volume = {424}, | |
Abstract = {We revisit a core prediction of the disc instability model | |
(DIM) applied to X-ray binaries. The model predicts the | |
existence of a critical mass-transfer rate, which depends | |
on disc size, separating transient and persistent systems. | |
We therefore selected a sample of 52 persistent and | |
transient neutron star and black hole X-ray binaries and | |
verified if the observed persistent (transient) systems do | |
lie in the appropriate stable (unstable) region of | |
parameter space predicted by the model. We find that, | |
despite the significant uncertainties inherent to these | |
kinds of studies, the data are in very good agreement with | |
the theoretical expectations. We then discuss some | |
individual cases that do not clearly fit into this main | |
conclusion. Finally, we introduce the transientness | |
parameter as a measure of the activity of a source and show | |
a clear trend of the average outburst recurrence time to | |
decrease with transientness in agreement with the DIM | |
predictions. We therefore conclude that, despite | |
difficulties in reproducing the complex details of the | |
light curves, the DIM succeeds in explaining the global | |
behaviour of X-ray binaries averaged over a long enough | |
period of time.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012MNRAS.424.1991C}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1205.5038}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2012.21339.x}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1205.5038}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2012MNRAS.424.1991C}, | |
Date-added = {2017-08-24 17:38:03 +0000}, | |
Date-modified = {2017-08-24 17:38:14 +0000}, | |
Doi = {10.1111/j.1365-2966.2012.21339.x}, | |
Eprint = {1205.5038}, | |
Keywords = {accretion, accretion discs, black hole physics, | |
instabilities, methods: observational, X-rays: binaries}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@InProceedings{corless+1996, | |
Title = {On the Lambert W Function}, | |
Author = {R. M. Corless and G. H. Gonnet and D. E. G. Hare and D. J. | |
Jeffrey and D. E. Knuth}, | |
Booktitle = {ADVANCES IN COMPUTATIONAL MATHEMATICS}, | |
Year = {1996}, | |
Pages = {329--359}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Keywords = {Untitled; Untitled1} | |
} | |
@Article{corrales+2010, | |
Title = {{Hydrodynamical response of a circumbinary gas disc to | |
black hole recoil and mass loss}}, | |
Author = {Corrales, Lia R and Haiman, Zolt\'{a}n and MacFadyen, | |
Andrew}, | |
Journal = {\mnras}, | |
Year = {2010}, | |
Month = may, | |
Pages = {947}, | |
Volume = {404}, | |
Abstract = {Finding electromagnetic (EM) counterparts of future | |
gravitational wave (GW) sources would bring rich scientific | |
benefits. A promising possibility, in the case of the | |
coalescence of a supermassive black hole binary (SMBHB), is | |
that the prompt emission from merger-induced disturbances | |
in a supersonic circumbinary disc may be detectable. We | |
follow the post-merger evolution of a thin, zero-viscosity | |
circumbinary gas disc with two-dimensional simulations, | |
using the hydrodynamic code FLASH. We analyse perturbations | |
arising from the 530 km s-1 recoil of a 106Msolar binary, | |
oriented in the plane of the disc, assuming either a | |
non-radiative gamma-law or a pseudo-isothermal equation of | |
state for the gas. We find that a single-armed spiral shock | |
wave forms and propagates outwards, sweeping up \~{}40 per | |
cent of the mass of the disc. The morphology and evolution | |
of the perturbations agrees well with those of caustics | |
predicted to occur in a collisionless disc. Assuming that | |
the disc radiates nearly instantaneously to maintain a | |
constant temperature, we estimate the amount of dissipation | |
and corresponding post-merger light curve. The luminosity | |
rises steadily on the time-scale of months, and reaches few | |
√\'{o}1043 ergs-1, corresponding to \~{}10 per cent of | |
the Eddington luminosity of the central SMBHB. We also | |
analyse the case in which gravitational wave emission | |
results in a 5 per cent mass loss in the merger remnant. | |
The mass loss reduces the shock overdensities and the | |
overall luminosity of the disc by \~{}15-20 per cent, | |
without any other major effects on the spiral shock pattern.}, | |
Annote = {(c) Journal compilation \{\copyright\} 2010 RAS}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2010MNRAS.404..947C%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1111/j.1365-2966.2010.16324.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1111/j.1365-2966.2010.16324.x}, | |
Keywords = {black hole physics, galaxies: nuclei,gravitational waves}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2010MNRAS.404..947C\&link\_type=ABSTRACT} | |
} | |
@Article{corralsantana+2016, | |
Title = {{BlackCAT: A catalogue of stellar-mass black holes in | |
X-ray transients}}, | |
Author = {{Corral-Santana}, J.~M. and {Casares}, J. and | |
{Mu{\~n}oz-Darias}, T. and {Bauer}, F.~E. and | |
{Mart{\'{\i}}nez-Pais}, I.~G. and {Russell}, D.~M.}, | |
Journal = {\aap}, | |
Year = {2016}, | |
Month = mar, | |
Pages = {A61}, | |
Volume = {587}, | |
Abstract = {Aims: During the last ~50 years, the population of black | |
hole candidates in X-ray binaries has increased | |
considerably, with 59 Galactic objects being detected in | |
transient low-mass X-ray binaries, as well as a few in | |
persistent systems (including ~5 extragalactic binaries). | |
Methods: We collect near-infrared, optical, and X-ray | |
information spread over hundreds of references to study the | |
population of black holes in X-ray transients as a whole. | |
Results: We present the most updated catalogue of black | |
hole transients. This contains X-ray, optical, and | |
near-infrared observations, together with their astrometric | |
and dynamical properties. The catalogue provides new and | |
useful information in both statistical and observational | |
parameters and provides a thorough and complete overview of | |
the black hole population in the Milky Way. Analysing the | |
distances and spatial distribution of the observed systems, | |
we estimate a total population of ~1300 Galactic black hole | |
transients. This means that we have only discovered less | |
than ~5% of the total Galactic distribution. The complete | |
version of this catalogue will be continuously updated at | |
http://www.astro.puc.cl/BlackCAT and in the Virtual | |
Observatory, including finding charts and data in other | |
wavelengths.Tables A.1 to A.4 are also available in | |
electronic form at the CDS via anonymous ftp to | |
(ftp://130.79.128.5) or via | |
http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/587/A61}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016A%26A...587A..61C}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1510.08869}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361/201527130}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1510.08869}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2016A%26A...587A..61C}, | |
Date-added = {2017-08-24 00:55:12 +0000}, | |
Date-modified = {2017-08-24 17:40:15 +0000}, | |
Doi = {10.1051/0004-6361/201527130}, | |
Eid = {A61}, | |
Eprint = {1510.08869}, | |
Keywords = {X-rays: binaries, stars: black holes, catalogs}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{costa+1997, | |
Title = {{Discovery of an X-ray afterglow associated with the {$\gamma$}-ray burst of 28 February 1997}}, | |
Author = {{Costa}, E. and {Frontera}, F. and {Heise}, J. and {Feroci}, M. and {in't Zand}, J. and {Fiore}, F. and {Cinti}, M.~N. and {Dal Fiume}, D. and {Nicastro}, L. and {Orlandini}, M. and {Palazzi}, E. and {Rapisarda\#}, M. and {Zavattini}, G. and {Jager}, R. and {Parmar}, A. and {Owens}, A. and {Molendi}, S. and {Cusumano}, G. and {Maccarone}, M.~C. and {Giarrusso}, S. and {Coletta}, A. and {Antonelli}, L.~A. and {Giommi}, P. and {Muller}, J.~M. and {Piro}, L. and {Butler}, R.~C. }, | |
Journal = {\nat}, | |
Year = {1997}, | |
Month = jun, | |
Pages = {783-785}, | |
Volume = {387}, | |
Abstract = {Establishing the nature of ?-ray bursts is one of the greatest challenges in high-energy astrophysics. The distribution of these bursts is isotropic across the sky, but inhomogeneous in space, with a deficit of faint bursts. It is currently unknown whether ?-ray bursts are produced in our Galaxy or at cosmological distances. The detection and identification of counterparts at other wavelengths are seen as crucial for resolving the origin of the events. Here we report the detection by the Beppo-SAX satellite of an X-ray `afterglow', associated with the ?-ray burst of 28 February 1997 (GRB970228; ref. 3)-the first such detection for any ?-ray burst. The X-ray transient was found to contain a significant fraction of the total energy of the ?-ray burst and, following the initial detection eight hours after the main burst, faded within a few days with a power-law decay function. The rapid locating of this ?-ray burst instigated a multi-wavelength observational campaign that culminated in the identification of a fading optical transient in a position consistent with the X-ray transient reported here.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1997Natur.387..783C}, | |
Doi = {10.1038/42885}, | |
Eprint = {astro-ph/9706065}, | |
Owner = {aleksey}, | |
Timestamp = {2018.04.02} | |
} | |
@Article{coughlin+2014, | |
Title = {{Hyperaccretion during Tidal Disruption Events: Weakly | |
Bound Debris Envelopes and Jets}}, | |
Author = {{Coughlin}, E.~R. and {Begelman}, M.~C.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = feb, | |
Pages = {82}, | |
Volume = {781}, | |
Abstract = {After the destruction of the star during a tidal | |
disruption event (TDE), the cataclysmic encounter between a | |
star and the supermassive black hole (SMBH) of a galaxy, | |
approximately half of the original stellar debris falls | |
back onto the hole at a rate that can initially exceed the | |
Eddington limit by orders of magnitude. We argue that the | |
angular momentum of this matter is too low to allow it to | |
attain a disk-like configuration with accretion proceeding | |
at a mildly super-Eddington rate, the excess energy being | |
carried away by a combination of radiative losses and | |
radially distributed winds. Instead, we propose that the | |
infalling gas traps accretion energy until it inflates into | |
a weakly bound, quasi-spherical structure with gas | |
extending nearly to the poles. We study the structure and | |
evolution of such "zero-Bernoulli accretion" flows as a | |
model for the super-Eddington phase of TDEs. We argue that | |
such flows cannot stop extremely super-Eddington accretion | |
from occurring, and that once the envelope is maximally | |
inflated, any excess accretion energy escapes through the | |
poles in the form of powerful jets. We compare the | |
predictions of our model to Swift J1644+57, the putative | |
super-Eddington TDE, and show that it can qualitatively | |
reproduce some of its observed features. Similar models, | |
including self-gravity, could be applicable to gamma-ray | |
bursts from collapsars and the growth of SMBH seeds inside | |
quasi-stars.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...781...82C}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1312.5314}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/781/2/82}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1312.5314}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014ApJ...781...82C}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/781/2/82}, | |
Eid = {82}, | |
Eprint = {1312.5314}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: | |
jets, galaxies: nuclei, X-rays: galaxies, X-rays: | |
individual: Swift J1644+57}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{crumley+2016, | |
Title = {{Swift J1644+57: an Ideal Test Bed of Radiation Mechanisms | |
in a Relativistic Super-Eddington Jet}}, | |
Author = {{Crumley}, P. and {Lu}, W. and {Santana}, R. and | |
{Hern{\'a}ndez}, R.~A. and {Kumar}, P. and {Markoff}, S.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2016}, | |
Month = apr, | |
Abstract = {Within the first 10 days after Swift discovered the jetted | |
tidal disruption event (TDE) Sw J1644+57, simultaneous | |
observations in the radio, near-infrared, optical, X-ray | |
and gamma-ray bands were carried out. These multiwavelength | |
data provide a unique opportunity to constrain the emission | |
mechanism and make-up of a relativistic super-Eddington | |
jet. We consider an exhaustive variety of radiation | |
mechanisms for the generation of X-rays in this TDE, and | |
rule out many processes such as SSC, photospheric and | |
proton synchrotron. The infrared to gamma-ray data for Sw | |
J1644+57 are consistent with synchrotron and | |
external-inverse-Compton (EIC) processes provided that | |
electrons in the jet are continuously accelerated on a time | |
scale shorter than ~1% of the dynamical time to maintain a | |
power-law distribution. The requirement of continuous | |
electron acceleration points to magnetic reconnection in a | |
Poynting flux dominated jet. The EIC process may require | |
fine tuning to explain the observed temporal decay of the | |
X-ray lightcurve, whereas the synchrotron process in a | |
magnetic jet needs no fine tuning for this TDE.}, | |
Adscomment = {22 pages, 6 figures. Accepted by MNRAS}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016arXiv160406468C}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1604.06468}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://arxiv.org/abs/1604.06468}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/2016arXiv160406468C}, | |
Date-added = {2016-04-26 22:07:24 +0000}, | |
Date-modified = {2016-04-26 22:07:24 +0000}, | |
Eprint = {1604.06468}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena, | |
Astrophysics - Astrophysics of Galaxies}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{cuadra+2009, | |
Title = {{Massive black hole binary mergers within subparsec scale | |
gas discs}}, | |
Author = {Cuadra, J and Armitage, P J and Alexander, R D and | |
Begelman, M C}, | |
Journal = {\mnras}, | |
Year = {2009}, | |
Month = mar, | |
Pages = {1423}, | |
Volume = {393}, | |
Abstract = {We study the efficiency and dynamics of supermassive black | |
hole binary mergers driven by angular momentum loss to | |
small-scale gas discs. Such binaries form after major | |
galaxy mergers, but their fate is unclear since hardening | |
through stellar scattering becomes very inefficient at | |
subparsec distances. Gas discs may dominate binary dynamics | |
on these scales, and promote mergers. Using numerical | |
simulations, we investigate the evolution of the semimajor | |
axis and eccentricity of binaries embedded within | |
geometrically thin gas discs. Our simulations directly | |
resolve angular momentum transport within the disc, which | |
at the radii of interest is likely dominated by disc | |
self-gravity. We show that the binary decays at a rate | |
which is in good agreement with analytical estimates, while | |
the eccentricity grows. Saturation of eccentricity growth | |
is not observed up to values e >\~{} 0.35. Accretion on to | |
the black holes is variable, and is roughly modulated by | |
the binary orbital frequency. Scaling our results, we | |
analytically estimate the maximum rate of binary decay that | |
is possible without fragmentation occurring within the | |
surrounding gas disc, and compare that rate to an estimate | |
of the stellar dynamical hardening rate. For binary masses | |
in the range 105 <\~{} M <\~{} 108Msolar we find that decay | |
due to gas discs may dominate for separations below a \~{} | |
0.01-0.1pc, in the regime where the disc is optically | |
thick. The minimum merger time-scale is shorter than the | |
Hubble time for M <\~{} 107Msolar. This implies that gas | |
discs could commonly attend relatively low-mass black hole | |
mergers, and that a significant population of binaries | |
might exist at separations of a few hundredths of a parsec, | |
where the combined decay rate is slowest. For more massive | |
binaries, where this mechanism fails to act quickly enough, | |
we suggest that scattering of stars formed within a | |
fragmenting gas disc could act as a significant additional | |
sink of binary angular momentum.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2009MNRAS.393.1423C%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1111/j.1365-2966.2008.14147.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1111/j.1365-2966.2008.14147.x}, | |
Keywords = {Accretion, accretion discs, galaxies: active, galaxies: | |
nuclei,black hole physics; Untitled; Untitled1}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2009MNRAS.393.1423C\&link\_type=ABSTRACT} | |
} | |
@Article{cuadra+2008, | |
Title = {{Variable accretion and emission from the stellar winds in | |
the Galactic Centre}}, | |
Author = {{Cuadra}, J. and {Nayakshin}, S. and {Martins}, F.}, | |
Journal = {\mnras}, | |
Year = {2008}, | |
Month = jan, | |
Pages = {458-466}, | |
Volume = {383}, | |
Abstract = {We present numerical simulations of stellar wind dynamics | |
in the central parsec of the Galactic Centre, studying in | |
particular the accretion of gas on to Sgr A*, the | |
supermassive black hole. Unlike our previous work, here we | |
use state-of-the-art observational data on orbits and wind | |
properties of individual wind-producing stars. Since wind | |
velocities were revised upwards and non-zero eccentricities | |
were considered, our new simulations show fewer clumps of | |
cold gas and no conspicuous disc-like structure. The | |
accretion rate is dominated by a few close `slow-wind | |
stars' (vw <= 750kms-1), and is consistent with the Bondi | |
estimate, but variable on time-scales of tens to hundreds | |
of years. This variability is due to the stochastic infall | |
of cold clumps of gas, as in earlier simulations, and to | |
the eccentric orbits of stars. The present models fail to | |
explain the high luminosity of Sgr A* a few hundred years | |
ago implied by Integral observations, but we argue that the | |
accretion of a cold clump with a small impact parameter | |
could have caused it. Finally, we show the possibility of | |
constraining the total mass-loss rate of the `slow-wind | |
stars' using near infrared observations of gas in the | |
central few arcseconds.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2008MNRAS.383..458C}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/0705.0769}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2007.12573.x}, | |
Bdsk-url-2 = {http://arXiv.org/abs/0705.0769}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2008MNRAS.383..458C}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1111/j.1365-2966.2007.12573.x}, | |
Eprint = {0705.0769}, | |
Keywords = {accretion, accretion discs , stars: winds, outflows , | |
Galaxy: centre , galaxies: active} | |
} | |
@Article{cuadra+2006, | |
Title = {{Galactic Centre stellar winds and Sgr A* accretion}}, | |
Author = {{Cuadra}, J. and {Nayakshin}, S. and {Springel}, V. and | |
{Di Matteo}, T.}, | |
Journal = {\mnras}, | |
Year = {2006}, | |
Month = feb, | |
Pages = {358-372}, | |
Volume = {366}, | |
Abstract = {We present a detailed discussion of our new 3D numerical | |
models for the accretion of stellar winds on to Sgr A*. In | |
our most sophisticated models, we put stellar wind sources | |
on realistic orbits around Sgr A*, we include recently | |
discovered `slow' winds (vw~ 300kms-1), and we account for | |
optically thin radiative cooling. We test our approach by | |
first modelling only one-phase `fast' stellar winds (vw~ | |
1000kms-1). For stellar wind sources fixed in space, the | |
accretion rate is of the order of , fluctuates by <~10 per | |
cent, and is in good agreement with previous models. In | |
contrast, decreases by an order of magnitude for wind | |
sources following circular orbits, and fluctuates by ~50 | |
per cent. Then we allow a fraction of stars to produce slow | |
winds. Much of these winds cool radiatively after being | |
shocked, forming cold clumps and filaments immersed into | |
the X-ray-emitting gas. We investigate two orbital | |
configurations for the stars in this scenario, an isotropic | |
distribution and two rotating discs with perpendicular | |
orientation. The morphology of cold gas is quite sensitive | |
to the orbital distribution of the stars. In both cases, | |
however, most of the accreted gas is hot, producing a | |
quasi-steady `floor' in the accretion rate, of the order of | |
~3 × 10-6Msolaryr-1, consistent with the values deduced | |
from Chandra observations. The cold gas accretes in | |
intermittent, short but powerful accretion episodes, which | |
may give rise to large-amplitude variability in the | |
luminosity of Sgr A* on time-scales of tens to hundreds of | |
years. The circularization radii for the flows are about | |
103 and 104 Schwarzschild radii, for the one- and two-phase | |
wind simulations, respectively, never forming the | |
quasi-spherical accretion flows suggested in some previous | |
work. Our work suggests that, averaged over time-scales of | |
hundreds to thousands of years, the radiative and | |
mechanical luminosity of Sgr A* may be substantially higher | |
than it is in its current state. Further improvements of | |
the wind accretion modelling of Sgr A* will rely on | |
improved observational constraints for the wind velocities, | |
mass-loss rates and stellar orbits.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006MNRAS.366..358C}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0505382}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2005.09837.x}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0505382}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2006MNRAS.366..358C}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1111/j.1365-2966.2005.09837.x}, | |
Eprint = {astro-ph/0505382}, | |
Keywords = {accretion, accretion discs, methods: numerical, stars: | |
winds, outflows, Galaxy: centre, galaxies: active} | |
} | |
@Article{cuadra+2005, | |
Title = {{Accretion of cool stellar winds on to Sgr A*: another | |
puzzle of the Galactic Centre?}}, | |
Author = {{Cuadra}, J. and {Nayakshin}, S. and {Springel}, V. and | |
{Di Matteo}, T.}, | |
Journal = {\mnras}, | |
Year = {2005}, | |
Month = jun, | |
Pages = {L55-L59}, | |
Volume = {360}, | |
Abstract = {Sgr A* is currently being fed by winds from a cluster of | |
gravitationally bound young mass-losing stars. Using | |
observational constraints on the orbits, mass-loss rates | |
and wind velocities of these stars, we numerically model | |
the distribution of gas in the ~ 0.1-10 arcsec region | |
around Sgr A*. We find that radiative cooling of recently | |
discovered slow winds leads to the formation of many cool | |
filaments and blobs, and to a thin and rather light | |
accretion disc on a scale of about an arcsecond. The disc, | |
however, does not extend all the way to our inner boundary. | |
Instead, hot X-ray-emitting gas dominates the inner | |
arcsecond. In our simulations, cool streams of gas | |
frequently enter this region on low angular momentum | |
orbits, and are then disrupted and heated up to the ambient | |
hot gas temperature. The accreting gas around Sgr A* is | |
thus two-phase, with a hot component, observable at X-ray | |
wavelengths, and a cool component, which may be responsible | |
for the majority of the time variability of Sgr A* emission | |
on time-scales of 100-1000 yr. We obtain an accretion rate | |
of a few ×10-6Msolaryr-1, consistent with Chandra | |
estimates, but variable on time-scales even shorter than | |
100 yr. These results strongly depend on the chosen stellar | |
orbits and wind parameters. Further observational input is | |
thus key to a better modelling of the Sgr A* wind | |
accretion.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005MNRAS.360L..55C}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0502044}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1745-3933.2005.00045.x}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0502044}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2005MNRAS.360L..55C}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1111/j.1745-3933.2005.00045.x}, | |
Eprint = {astro-ph/0502044}, | |
Keywords = {accretion, accretion discs, methods: numerical, stars: | |
winds, outflows, Galaxy: centre, galaxies: active} | |
} | |
@Article{cuadra+2015, | |
Title = {{The role of feedback in accretion on Low Luminosity AGN: | |
Sgr A* case study}}, | |
Author = {{Cuadra}, J. and {Nayakshin}, S. and {Wang}, Q.~D.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2015}, | |
Month = mar, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015arXiv150302745C}, | |
Archiveprefix = {arXiv}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {1503.02745}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena; | |
Untitled; Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{dorazio+2013, | |
Title = {{Accretion into the central cavity of a circumbinary | |
disc}}, | |
Author = {{D'Orazio}, D.~J. and {Haiman}, Z. and {MacFadyen}, A.}, | |
Journal = {\mnras}, | |
Year = {2013}, | |
Month = dec, | |
Pages = {2997-3020}, | |
Volume = {436}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2013MNRAS.436.2997D}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stt1787}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1093/mnras/stt1787}, | |
Eprint = {1210.0536}, | |
Keywords = {accretion, accretion discs, black hole physics, | |
gravitational waves, galaxies: active}, | |
Primaryclass = {astro-ph.GA} | |
} | |
@Article{dale+2009, | |
Title = {{Red giant stellar collisions in the Galactic Centre}}, | |
Author = {{Dale}, J.~E. and {Davies}, M.~B. and {Church}, R.~P. and | |
{Freitag}, M.}, | |
Journal = {\mnras}, | |
Year = {2009}, | |
Month = mar, | |
Pages = {1016-1033}, | |
Volume = {393}, | |
Abstract = {We show that collisions with stellar-mass black holes can | |
partially explain the absence of bright giant stars in the | |
Galactic Centre, first noted by Genzel et al. We show that | |
the missing objects are low-mass giants and asymptotic | |
giant branch stars in the range 1-3Msolar. Using detailed | |
stellar evolution calculations, we find that to prevent | |
these objects from evolving to become visible in the | |
depleted K bands, we require that they suffer collisions on | |
the red giant branch, and we calculate the fractional | |
envelope mass losses required. Using a combination of | |
smoothed particle hydrodynamic calculations, restricted | |
three-body analysis and Monte Carlo simulations, we compute | |
the expected collision rates between giants and black | |
holes, and between giants and main-sequence stars in the | |
Galactic Centre. We show that collisions can plausibly | |
explain the missing giants in the 10.5 < K < 12 band. | |
However, depleting the brighter (K < 10.5) objects out to | |
the required radius would require a large population of | |
black hole impactors which would in turn deplete the 10.5 < | |
K < 12 giants in a region much larger than is observed. We | |
conclude that collisions with stellar-mass black holes | |
cannot account for the depletion of the very brightest | |
giants, and we use our results to place limits on the | |
population of stellar-mass black holes in the Galactic | |
Centre.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009MNRAS.393.1016D}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/0811.3111}, | |
Bdsk-file-1 = {YnBsaXN0MDDUAQIDBAUGJCVYJHZlcnNpb25YJG9iamVjdHNZJGFyY2hpdmVyVCR0b3ASAAGGoKgHCBMUFRYaIVUkbnVsbNMJCgsMDxJXTlMua2V5c1pOUy5vYmplY3RzViRjbGFzc6INDoACgAOiEBGABIAFgAdccmVsYXRpdmVQYXRoWWFsaWFzRGF0YV8QKi4uLy4uLy4uLy4uL0RvY3VtZW50cy9QYXBlcnMvRGFsZS8yMDA5LnBkZtIXCxgZV05TLmRhdGFPEQGEAAAAAAGEAAIAAAxNYWNpbnRvc2ggSEQAAAAAAAAAAAAAAAAAAADNZNKaSCsAAAJmTSAIMjAwOS5wZGYAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAmZNHNSdUdwAAAAAAAAAAAAEAAQAAAkgAAAAAAAAAAAAAAAAAAAABERhbGUAEAAIAADNZQraAAAAEQAIAADUnZgsAAAAAQAUAmZNIAEHiAQABcQqAAXEKQACEOkAAgA+TWFjaW50b3NoIEhEOlVzZXJzOgBhbGVrc2V5OgBEb2N1bWVudHM6AFBhcGVyczoARGFsZToAMjAwOS5wZGYADgASAAgAMgAwADAAOQAuAHAAZABmAA8AGgAMAE0AYQBjAGkAbgB0AG8AcwBoACAASABEABIALFVzZXJzL2FsZWtzZXkvRG9jdW1lbnRzL1BhcGVycy9EYWxlLzIwMDkucGRmABMAAS8AABUAAgAO//8AAIAG0hscHR5aJGNsYXNzbmFtZVgkY2xhc3Nlc11OU011dGFibGVEYXRhox0fIFZOU0RhdGFYTlNPYmplY3TSGxwiI1xOU0RpY3Rpb25hcnmiIiBfEA9OU0tleWVkQXJjaGl2ZXLRJidUcm9vdIABAAgAEQAaACMALQAyADcAQABGAE0AVQBgAGcAagBsAG4AcQBzAHUAdwCEAI4AuwDAAMgCUAJSAlcCYgJrAnkCfQKEAo0CkgKfAqICtAK3ArwAAAAAAAACAQAAAAAAAAAoAAAAAAAAAAAAAAAAAAACvg==}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2008.14254.x}, | |
Bdsk-url-2 = {http://arxiv.org/abs/0811.3111}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2009MNRAS.393.1016D}, | |
Date-added = {2017-01-12 20:31:41 +0000}, | |
Date-modified = {2017-01-12 20:31:47 +0000}, | |
Doi = {10.1111/j.1365-2966.2008.14254.x}, | |
Eprint = {0811.3111}, | |
Keywords = {stars: late-type , Galaxy: centre} | |
} | |
@Article{dalton+1993, | |
Title = {{A flux-limited treatment for the conductive evaporation | |
of spherical interstellar gas clouds}}, | |
Author = {{Dalton}, W.~W. and {Balbus}, S.~A.}, | |
Journal = {\apj}, | |
Year = {1993}, | |
Month = feb, | |
Pages = {625-635}, | |
Volume = {404}, | |
Abstract = {In this work, we present and analyze a new analytic | |
solution for the saturated (flux-limited) thermal | |
evaporation of a spherical cloud. This work is | |
distinguished from earlier analytic studies by allowing the | |
thermal conductivity to change continuously from a | |
diffusive to a saturated form, in a manner usually employed | |
only in numerical calculations. This closed form solution | |
will be of interest as a computational benchmark. Using our | |
calculated temperature profiles and mass-loss rates, we | |
model the thermal evaporation of such a cloud under typical | |
interstellar medium (ISM) conditions, with some | |
restrictions. We examine the ionization structure of the | |
cloud-ISM interface and evaluate column densities of | |
carbon, nitrogen, oxygen, neon, and silicon ions toward the | |
cloud. In accord with other investigations, we find that | |
ionization equilibrium is far from satisfied under the | |
assumed conditions. Since the inclusion of saturation | |
effects in the heat flux narrows the thermal interface | |
relative to its classical structure, we also find that | |
saturation effects tend to lower predicted column | |
densities.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1993ApJ...404..625D}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1086/172316}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1993ApJ...404..625D}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/172316}, | |
Keywords = {Clouds, Conductive Heat Transfer, Evaporation, Gas | |
Ionization, Interstellar Gas, Heat Flux, Space Plasmas, | |
Spheres, Temperature Profiles} | |
} | |
@Article{davies+1983, | |
Title = {{Dynamics of yet more ellipticals and bulges}}, | |
Author = {{Davies}, R.~L. and {Illingworth}, G.}, | |
Journal = {\apj}, | |
Year = {1983}, | |
Month = mar, | |
Pages = {516-530}, | |
Volume = {266}, | |
Abstract = {Extensive kinematical studies have shown that elliptical | |
galaxies exhibit a wide variety of dynamical properties. | |
There is evidence that the dynamical properties of | |
elliptical galaxies depend upon their luminosity. In | |
connection with the present investigation, major axis | |
spectra have been obtained. Rotation and velocity | |
dispersion profiles have been derived for four elliptical | |
galaxies NGC 3379, NGC 4839, NGC 4889 and NGC 6909, and for | |
the probable S0 galaxy NGC 584. NGC 3379 is consistent with | |
being a rotationally-flattened isotropic-dispersion | |
constant M/L oblate spheroid. While NGC 584 is classified | |
E/S0, it is most likely an S0. If so, it, along with NGC | |
128 and NGC 4595, has the most luminous bulges for which | |
kinematical data are available. For NGC 4839 and NGC 4889, | |
two of the three brightest galaxies in Coma, virtually no | |
rotation is found.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1983ApJ...266..516D}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/160799}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1983ApJ...266..516D}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/160799}, | |
Keywords = {Elliptical Galaxies, Galactic Rotation, Galactic | |
Structure, Angular Velocity, Luminosity, Plasma Jets, | |
Spectrum Analysis, Velocity Distribution} | |
} | |
@Article{davis+2009, | |
Title = {{The Effects of Magnetic Fields and Inhomogeneities on | |
Accretion Disk Spectra and Polarization}}, | |
Author = {Davis, S.\~{}W. and Blaes, O.\~{}M. and Hirose, S and | |
Krolik, J.\~{}H.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = sep, | |
Pages = {569--584}, | |
Volume = {703}, | |
Archiveprefix = {arXiv}, | |
Arxivid = {astro-ph.HE/0908.0505}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/703/1/569}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/703/1/569}, | |
Eprint = {0908.0505}, | |
Keywords = {X-rays: binaries, accretion disks, black hole physics, | |
polarization,accretion}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{davis+2017, | |
Title = {{WISDOM Project - II. Molecular gas measurement of the | |
supermassive black hole mass in NGC 4697}}, | |
Author = {{Davis}, T.~A. and {Bureau}, M. and {Onishi}, K. and | |
{Cappellari}, M. and {Iguchi}, S. and {Sarzi}, M.}, | |
Journal = {\mnras}, | |
Year = {2017}, | |
Month = jul, | |
Pages = {4675-4690}, | |
Volume = {468}, | |
Abstract = {As part of the mm-Wave Interferometric Survey of Dark | |
Object Masses (WISDOM) project, we present an estimate of | |
the mass of the supermassive black hole (SMBH) in the | |
nearby fast-rotating early-type galaxy NGC 4697. This | |
estimate is based on Atacama Large Millimeter/submillimeter | |
Array (ALMA) cycle-3 observations of the 12CO(2-1) emission | |
line with a linear resolution of 29 pc (0.53 arcsec). We | |
find that NGC 4697 hosts a small relaxed central molecular | |
gas disc with a mass of 1.6 ?107 M?, co-spatial with the | |
obscuring dust disc visible in optical Hubble Space | |
Telescope imaging. We also resolve thermal 1 mm continuum | |
emission from the dust in this disc. NGC 4697 is found to | |
have a very low molecular gas velocity dispersion, ?gas = | |
1.65^{+0.68}_{-0.65} km s-1. This seems to be partially | |
because the giant molecular cloud mass function is not | |
fully sampled, but other mechanisms such as chemical | |
differentiation in a hard radiation field or morphological | |
quenching also seem to be required. We detect a Keplerian | |
increase of the rotation of the molecular gas in the very | |
centre of NGC 4697, and use forward modelling of the ALMA | |
data cube in a Bayesian framework with the KINematic | |
Molecular Simulation (kinms) code to estimate an SMBH mass | |
of (1.3_{-0.17}^{+0.18}) ?108 M? and an I-band | |
mass-to-light ratio of 2.14_{-0.05}^{+0.04} M?/L? (at the | |
99 per cent confidence level). Our estimate of the SMBH | |
mass is entirely consistent with previous measurements from | |
stellar kinematics. This increases confidence in the | |
growing number of SMBH mass estimates being obtained in the | |
ALMA era.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017MNRAS.468.4675D}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1093/mnras/stw3217}, | |
Eprint = {1703.05248}, | |
Keywords = {galaxies: elliptical and lenticular, cD, galaxies: | |
individual: NGC 4697, galaxies: ISM, galaxies: kinematics | |
and dynamics, galaxies: nuclei}, | |
Owner = {aleksey}, | |
Timestamp = {2018.02.07} | |
} | |
@Article{de-colle+2012, | |
Title = {{The Dynamics, Appearance, and Demographics of | |
Relativistic Jets Triggered by Tidal Disruption of Stars in | |
Quiescent Supermassive Black Holes}}, | |
Author = {{De Colle}, F. and {Guillochon}, J. and {Naiman}, J. and | |
{Ramirez-Ruiz}, E.}, | |
Journal = {\apj}, | |
Year = {2012}, | |
Month = dec, | |
Pages = {103}, | |
Volume = {760}, | |
Abstract = {We examine the consequences of a model in which | |
relativistic jets can be triggered in quiescent massive | |
black holes when a geometrically thick and hot accretion | |
disk forms as a result of the tidal disruption of a star. | |
To estimate the power, thrust, and lifetime of the jet, we | |
use the mass accretion history onto the black hole as | |
calculated by detailed hydrodynamic simulations of the | |
tidal disruption of stars. We go on to determine the states | |
of the interstellar medium in various types of quiescent | |
galactic nuclei, and describe how this external matter can | |
affect jets propagating through it. We use this | |
information, together with a two-dimensional hydrodynamic | |
model of the structure of the relativistic flow, to study | |
the dynamics of the jet, the propagation of which is | |
regulated by the density stratification of the environment | |
and by its injection history. The breaking of symmetry | |
involved in transitioning from one to two dimensions is | |
crucial and leads to qualitatively new phenomena. At early | |
times, as the jet power increases, the high pressure of the | |
cocoon collimates the jet, increasing its shock velocity as | |
compared to that of spherical models. We show that small | |
velocity gradients, induced near or at the source, steepen | |
into internal shocks and provide a source of free energy | |
for particle acceleration and radiation along the jet's | |
channel. The jets terminate at a working surface where they | |
interact strongly with the surrounding medium through a | |
combination of shock waves and instabilities; a continuous | |
flow of relativistic fluid emanating from the nucleus | |
supplies this region with mass, momentum, and energy. | |
Information about the t -5/3 decrease in power supply | |
propagates within the jet at the internal sound speed. As a | |
result, the internal energy at the jet head continues to | |
accumulate until long after the peak feeding rate is | |
reached. An appreciable time delay is thus expected between | |
peaks in the short-wavelength radiation emanating near the | |
jet's origin and the long-wavelength emission produced at | |
the head of the jet. Many of the observed properties of the | |
Swift 1644+57/GRB 110328A event can be understood as | |
resulting from accretion onto and jets driven by a 106 M | |
&sun; central mass black hole following the disruption of a | |
sun-like star. With the inclusion of a stochastic | |
contribution to the luminosity due to variations in the | |
feeding rate driven by instabilities near the tidal radius, | |
we find that our model can explain the X-ray light curve | |
without invoking a rarely occurring deep encounter. In | |
conjunction with the number density of black holes in the | |
local universe, we hypothesize that the conditions required | |
to produce the Swift event are not anomalous, but are in | |
fact representative of the jet-driven flare population | |
arising from tidal disruptions.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012ApJ...760..103D}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1205.1507}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/760/2/103}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1205.1507}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2012ApJ...760..103D}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/760/2/103}, | |
Eid = {103}, | |
Eprint = {1205.1507}, | |
Keywords = {galaxies: jets, gamma-ray burst: individual: GRB 110328A, | |
hydrodynamics, methods: numerical, relativistic processes, | |
shock waves}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{delafuentemarcos+2017, | |
Title = {{Binary stripping as a plausible origin of correlated pairs of extreme trans-Neptunian objects}}, | |
Author = {{de la Fuente Marcos}, C. and {de la Fuente Marcos}, R. and {Aarseth}, S.~J.}, | |
Journal = {\apss}, | |
Year = {2017}, | |
Month = nov, | |
Pages = {198}, | |
Volume = {362}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017Ap%26SS.362..198D}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1007/s10509-017-3181-1}, | |
Eid = {198}, | |
Eprint = {1709.06813}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.EP}, | |
Timestamp = {2018.10.11} | |
} | |
@Article{devita+2016, | |
Title = {{A class of spherical, truncated, anisotropic models for | |
application to globular clusters}}, | |
Author = {{de Vita}, R. and {Bertin}, G. and {Zocchi}, A.}, | |
Journal = {\aap}, | |
Year = {2016}, | |
Month = may, | |
Pages = {A16}, | |
Volume = {590}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016A%26A...590A..16D}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1051/0004-6361/201628274}, | |
Eid = {A16}, | |
Eprint = {1603.05993}, | |
Keywords = {globular clusters: general, stars: kinematics and | |
dynamics, globular, clusters: individual: NGC 104 (47 Tuc), | |
globular clusters: individual: NGC 5139, ({$\omega$}Cen)} | |
} | |
@Article{degenaar:2010, | |
Title = {{A four-year baseline Swift study of enigmatic X-ray | |
transients located near the Galactic center}}, | |
Author = {{Degenaar}, N. and {Wijnands}, R.}, | |
Journal = {\aap}, | |
Year = {2010}, | |
Month = dec, | |
Pages = {A69}, | |
Volume = {524}, | |
Abstract = {We report on continued monitoring observations of the | |
Galactic center carried out by the X-ray telescope aboard | |
the Swift satellite in 2008 and 2009. This campaign | |
revealed activity of the five known X-ray transients AX | |
J1745.6-2901, CXOGC J174535.5-290124, GRS 1741-2853, XMM | |
J174457-2850.3 and CXOGC J174538.0-290022. All these | |
sources are known to undergo very faint X-ray outbursts | |
with 2-10 keV peak luminosities of LX, peak 1034-36 erg | |
s-1, although the two confirmed neutron star low-mass X-ray | |
binaries AX J1745.6-2901 and GRS 1741-2853 can also become | |
brighter (LX, peak 1036-37 erg s-1). We discuss the | |
observed long-term lightcurves and X-ray spectra of these | |
five enigmatic transients. In 2008, AX J1745.6-2901 | |
returned to quiescence following an unusually long | |
accretion outburst of more than 1.5 years. GRS 1741-2853 | |
was active in 2009 and displayed the brightest outburst | |
ever recorded for this source, reaching up to a 2-10 keV | |
luminosity of LX 1 × 1037 (D/7.2 kpc)2 erg s-1. This | |
system appears to undergo recurrent accretion outbursts | |
approximately every 2 years. Furthermore, we find that the | |
unclassified transient XMM J174457-2850.3 becomes bright | |
only during short episodes (days) and is often found active | |
in between quiescence (LX 1032 erg s-1) and its maximum | |
outburst luminosity of LX 1036 erg s-1. CXOGC | |
J174535.5-290124 and CXOGC J174538.0-290022, as well as | |
three other very-faint X-ray transients that were detected | |
by Swift monitoring observations in 2006, have very low | |
time-averaged mass-accretion rates of < dot{M} >_long ⪅ 2 | |
× 10-12 M&sun; yr-1. Despite having obtained two years of | |
new data in 2008 and 2009, no new X-ray transients were | |
detected.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010A%26A...524A..69D}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1007.0249}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361/201015322}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1007.0249}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2010A%26A...524A..69D}, | |
Date-added = {2017-07-28 16:46:41 +0000}, | |
Date-modified = {2017-07-28 16:46:41 +0000}, | |
Doi = {10.1051/0004-6361/201015322}, | |
Eid = {A69}, | |
Eprint = {1007.0249}, | |
Keywords = {X-rays: binaries, stars: neutron, accretion, accretion | |
disks, Galaxy: center, X-rays: general}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{degenaar+2010, | |
Title = {{A four-year baseline Swift study of enigmatic X-ray | |
transients located near the Galactic center}}, | |
Author = {{Degenaar}, N. and {Wijnands}, R.}, | |
Journal = {\aap}, | |
Year = {2010}, | |
Month = dec, | |
Pages = {A69}, | |
Volume = {524}, | |
Abstract = {We report on continued monitoring observations of the | |
Galactic center carried out by the X-ray telescope aboard | |
the Swift satellite in 2008 and 2009. This campaign | |
revealed activity of the five known X-ray transients AX | |
J1745.6-2901, CXOGC J174535.5-290124, GRS 1741-2853, XMM | |
J174457-2850.3 and CXOGC J174538.0-290022. All these | |
sources are known to undergo very faint X-ray outbursts | |
with 2-10 keV peak luminosities of LX, peak 1034-36 erg | |
s-1, although the two confirmed neutron star low-mass X-ray | |
binaries AX J1745.6-2901 and GRS 1741-2853 can also become | |
brighter (LX, peak 1036-37 erg s-1). We discuss the | |
observed long-term lightcurves and X-ray spectra of these | |
five enigmatic transients. In 2008, AX J1745.6-2901 | |
returned to quiescence following an unusually long | |
accretion outburst of more than 1.5 years. GRS 1741-2853 | |
was active in 2009 and displayed the brightest outburst | |
ever recorded for this source, reaching up to a 2-10 keV | |
luminosity of LX 1 × 1037 (D/7.2 kpc)2 erg s-1. This | |
system appears to undergo recurrent accretion outbursts | |
approximately every 2 years. Furthermore, we find that the | |
unclassified transient XMM J174457-2850.3 becomes bright | |
only during short episodes (days) and is often found active | |
in between quiescence (LX 1032 erg s-1) and its maximum | |
outburst luminosity of LX 1036 erg s-1. CXOGC | |
J174535.5-290124 and CXOGC J174538.0-290022, as well as | |
three other very-faint X-ray transients that were detected | |
by Swift monitoring observations in 2006, have very low | |
time-averaged mass-accretion rates of < dot{M} >_long ⪅ 2 | |
× 10-12 M&sun; yr-1. Despite having obtained two years of | |
new data in 2008 and 2009, no new X-ray transients were | |
detected.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010A%26A...524A..69D}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1007.0249}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361/201015322}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1007.0249}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2010A%26A...524A..69D}, | |
Date-added = {2017-07-28 16:46:41 +0000}, | |
Date-modified = {2017-08-23 21:00:14 +0000}, | |
Doi = {10.1051/0004-6361/201015322}, | |
Eid = {A69}, | |
Eprint = {1007.0249}, | |
Keywords = {X-rays: binaries, stars: neutron, accretion, accretion | |
disks, Galaxy: center, X-rays: general}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{degenaar+2012, | |
Title = {{A four-year XMM-Newton/Chandra monitoring campaign of the | |
Galactic centre: analysing the X-ray transients}}, | |
Author = {{Degenaar}, N. and {Wijnands}, R. and {Cackett}, E.~M. and | |
{Homan}, J. and {in't Zand}, J.~J.~M. and {Kuulkers}, E. | |
and {Maccarone}, T.~J. and {van der Klis}, M.}, | |
Journal = {\aap}, | |
Year = {2012}, | |
Month = sep, | |
Pages = {A49}, | |
Volume = {545}, | |
Abstract = {We report on the results of a four-year long X-ray | |
monitoring campaign of the central 1.2 square degrees of | |
our Galaxy, performed with Chandra and XMM-Newton between | |
2005 and 2008. Our study focuses on the properties of | |
transient X-ray sources that reach 2-10 keV luminosities of | |
LX ≳ 1034 erg s-1 for an assumed distance of 8 kpc. There | |
are 17 known X-ray transients within the field of view of | |
our campaign, eight of which were detected in outburst | |
during our observations: the transient neutron star | |
low-mass X-ray binaries GRS 1741-2853, AX J1745.6-2901, SAX | |
J1747.0-2853, KS 1741-293 (all four are also known X-ray | |
bursters), and GRO J1744-28 (a 2.1 Hz X-ray pulsar), and | |
the unclassified X-ray transients XMM J174457-2850.3, CXOGC | |
J174535.5-290124 and CXOGC J174541.0-290014. We present | |
their X-ray spectra and flux evolution during our campaign, | |
and discuss our results in light of their historic | |
activity. Our main results include the detection of two | |
thermonuclear X-ray bursts from SAX J1747.0-2853 that were | |
separated by an unusually short time interval of 3.8 min. | |
Investigation of the lightcurves of AX J1745.6-2901 | |
revealed one thermonuclear X-ray burst and a ~1600-s long | |
X-ray eclipse. We found that both XMM J174457-2850.3 and | |
GRO J1744-28 displayed weak X-ray activity above their | |
quiescent levels at LX ~ 1033-34 erg s-1, which is | |
indicative of low-level accretion. We compare this kind of | |
activity with the behaviour of low-luminosity X-ray | |
transients that display 2-10 keV peak luminosities of LX ~ | |
1034 erg s-1 and have never been seen to become brighter. | |
In addition to the eight known X-ray transients, we | |
discovered a previously unknown X-ray source that we | |
designate XMMU J174654.1-291542. This object emits most of | |
its photons above 2 keV and appears to be persistent at a | |
luminosity of LX ~ 1034 erg s-1, although it exhibits | |
strong spectral variability on a time scale of months. | |
Based on its X-ray properties and the possible association | |
with an infrared source, we tentatively classify this | |
object as a cataclysmic variable. No new transients were | |
found during our campaign, reinforcing the conclusion of | |
previous authors that most X-ray transients recurring on a | |
time scale of less than a decade have now been identified | |
near the Galactic centre. Tables 1-3 and Appendix A are | |
only available in electronic form at http://www.aanda.org}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012A%26A...545A..49D}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1204.6043}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361/201219470}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1204.6043}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2012A%26A...545A..49D}, | |
Date-added = {2017-07-28 16:38:32 +0000}, | |
Date-modified = {2017-07-28 16:38:32 +0000}, | |
Doi = {10.1051/0004-6361/201219470}, | |
Eid = {A49}, | |
Eprint = {1204.6043}, | |
Keywords = {accretion, accretion disks, X-rays: binaries, stars: | |
neutron, Galaxy: center, X-rays: general}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{degenaar+2015, | |
Title = {{The Swift X-ray monitoring campaign of the center of the | |
Milky Way}}, | |
Author = {{Degenaar}, N. and {Wijnands}, R. and {Miller}, J.~M. and | |
{Reynolds}, M.~T. and {Kennea}, J. and {Gehrels}, N.}, | |
Journal = {Journal of High Energy Astrophysics}, | |
Year = {2015}, | |
Month = sep, | |
Pages = {137-147}, | |
Volume = {7}, | |
Abstract = {In 2006 February, shortly after its launch, Swift began | |
monitoring the center of the Milky Way with the on board | |
X-Ray Telescope using short 1-ks exposures performed every | |
1-4 days. Between 2006 and 2014 over 1200 observations have | |
been obtained, accumulating to ~= 1.3 Ms of exposure time. | |
This has yielded a wealth of information about the | |
long-term X-ray behavior of the supermassive black hole Sgr | |
A*, and numerous transient X-ray binaries that are located | |
within the 25' ×25' region covered by the campaign. In | |
this review we highlight the discoveries made during these | |
first nine years, which include 1) the detection of seven | |
bright X-ray flares from Sgr A*, 2) the discovery of the | |
magnetar SGR J1745-29, 3) the first systematic analysis of | |
the outburst light curves and energetics of the peculiar | |
class of very-faint X-ray binaries, 4) the discovery of | |
three new transient X-ray sources, 5) the exposure of | |
low-level accretion in otherwise bright X-ray binaries, and | |
6) the identification of a candidate X-ray | |
binary/millisecond radio pulsar transitional object. We | |
also reflect on future science to be done by continuing | |
this Swift's legacy campaign, such as high-cadence | |
monitoring to study how the interaction between the gaseous | |
object 'G2' and Sgr A* plays out in the future.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015JHEAp...7..137D}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1503.07524}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1016/j.jheap.2015.03.005}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1503.07524}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2015JHEAp...7..137D}, | |
Date-added = {2017-08-24 17:37:29 +0000}, | |
Date-modified = {2017-08-24 17:37:29 +0000}, | |
Doi = {10.1016/j.jheap.2015.03.005}, | |
Eprint = {1503.07524}, | |
Keywords = {Accretion, Accretion disks, Black hole physics, Galaxy: | |
center, Stars: neutron, X-rays: binaries}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{denicolo+2005, | |
Title = {{Group, field and isolated early-type galaxies - II. | |
Global trends from nuclear data}}, | |
Author = {{Denicol{\'o}}, G. and {Terlevich}, R. and {Terlevich}, E. | |
and {Forbes}, D.~A. and {Terlevich}, A.}, | |
Journal = {\mnras}, | |
Year = {2005}, | |
Month = apr, | |
Pages = {813-832}, | |
Volume = {358}, | |
Abstract = {We have derived ages, metallicities and enhanced-element | |
ratios [alpha/Fe] for a sample of 83 early-type galaxies | |
essentially in groups, the field or isolated objects. The | |
stellar-population properties derived for each galaxy | |
correspond to the nuclear re/8 aperture extraction. The | |
median age found for Es is 5.8+/-0.6 Gyr and the average | |
metallicity is +0.37+/-0.03 dex. For S0s, the median age is | |
3.0+/-0.6 Gyr and [Z/H]= 0.53+/-0.04 dex. We compare the | |
distribution of our galaxies in the Hbeta-[MgFe] diagram | |
with Fornax galaxies. Our elliptical galaxies are 3-4 Gyr | |
younger than Es in the Fornax cluster. We find that the | |
galaxies lie in a plane defined by [Z/H]= 0.99 logsigma0- | |
0.46 log(age) - 1.60, or in linear terms Z ~sigma0× (age) | |
-0.5. More massive (larger sigma0) and older galaxies | |
present, on average, large [alpha/Fe] values, and therefore | |
must have undergone shorter star-formation time-scales. | |
Comparing group against field/isolated galaxies, it is not | |
clear that environment plays an important role in | |
determining their stellar-population history. In | |
particular, our isolated galaxies show ages differing by | |
more than 8 Gyr. Finally we explore our large spectral | |
coverage to derive log(O/H) metallicity from the Halpha and | |
NIIlambda6584 and compare it with model-dependent [Z/H]. We | |
find that the O/H abundances are similar for all galaxies, | |
and we can interpret it as if most chemical evolution has | |
already finished in these galaxies.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005MNRAS.358..813D}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0412435}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2005.08748.x}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0412435}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2005MNRAS.358..813D}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1365-2966.2005.08748.x}, | |
Eprint = {astro-ph/0412435}, | |
Keywords = {galaxies: abundances, galaxies: elliptical and lenticular, | |
cD, galaxies: evolution, galaxies: nuclei, galaxies: | |
stellar content} | |
} | |
@Article{dexter&oleary2014, | |
Title = {{The Peculiar Pulsar Population of the Central Parsec}}, | |
Author = {{Dexter}, J. and {O'Leary}, R.~M.}, | |
Journal = {\apjl}, | |
Year = {2014}, | |
Month = mar, | |
Pages = {L7}, | |
Volume = {783}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...783L...7D}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/2041-8205/783/1/L7}, | |
Date-added = {2017-06-07 01:13:55 +0000}, | |
Date-modified = {2017-06-07 01:14:18 +0000}, | |
Doi = {10.1088/2041-8205/783/1/L7}, | |
Eid = {L7}, | |
Eprint = {1310.7022}, | |
Keywords = {Galaxy: center, pulsars: general, pulsars: individual: SGR | |
J1745{\ndash}29, stars: neutron}, | |
Primaryclass = {astro-ph.GA} | |
} | |
@Article{di-matteo+2000, | |
Title = {{Low-radiative-efficiency accretion in the nuclei of | |
elliptical galaxies}}, | |
Author = {{Di Matteo}, T. and {Quataert}, E. and {Allen}, S.~W. and | |
{Narayan}, R. and {Fabian}, A.~C.}, | |
Journal = {\mnras}, | |
Year = {2000}, | |
Month = jan, | |
Pages = {507-521}, | |
Volume = {311}, | |
Abstract = {The discovery of hard X-ray emission from a sample of six | |
nearby elliptical galaxies, including the dominant galaxies | |
of the Virgo, Fornax and Centaurus clusters (M87, NGC 1399 | |
and NGC 4696, respectively), and NGC 4472, 4636 and 4649 in | |
the Virgo cluster, has important implications for the study | |
of quiescent supermassive black holes. We describe how the | |
broad-band spectral energy distributions for these | |
galaxies, which accrete from their hot gaseous haloes at | |
rates comparable to their Bondi rates, can be explained by | |
low-radiative-efficiency accretion flows in which a | |
significant fraction of the mass, angular momentum and | |
energy is removed from the flows by winds. The observed | |
suppression of the synchrotron components in the radio band | |
(excluding the case of M87) and the systematically hard | |
X-ray spectra, which are interpreted as thermal | |
bremsstrahlung emission, support the conjecture that | |
significant mass outflow is a natural consequence of | |
systems accreting at low radiative efficiencies. We briefly | |
discuss an alternative model for the observed X-ray | |
emission, in which it is due to non-thermal | |
synchrotron-self-Compton processes in the accretion flows, | |
or outflows. This appears to require implausibly weak | |
magnetic fields. Emission from a collimated jet viewed | |
off-axis should be distinguishable from the bremsstrahlung | |
model by variability and thermal line emission studies. We | |
argue that the difference in radiative efficiency between | |
the nuclei of spiral and elliptical galaxies may arise from | |
the different manner in which interstellar gas is fed into | |
the nuclei. In ellipticals, matter fed from the hot (slowly | |
cooling) interstellar medium (ISM) is likely to be highly | |
magnetized and have low specific angular momentum, which | |
favours low-radiative-efficiency accretion solutions and, | |
possibly, the formation of the observed jets.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2000MNRAS.311..507D}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/9905053}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1046/j.1365-8711.2000.03134.x}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/9905053}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2000MNRAS.311..507D}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1046/j.1365-8711.2000.03134.x}, | |
Eprint = {astro-ph/9905053}, | |
Keywords = {ACCRETION, ACCRETION DISCS, GALAXIES: CLUSTERS: GENERAL, | |
COOLING FLOWS, INTERGALACTIC MEDIUM, GALAXIES: NUCLEI, | |
X-RAYS: GALAXIES} | |
} | |
@Article{di-matteo+2005, | |
Title = {{Energy input from quasars regulates the growth and | |
activity of black holes and their host galaxies}}, | |
Author = {{Di Matteo}, T. and {Springel}, V. and {Hernquist}, L.}, | |
Journal = {\nat}, | |
Year = {2005}, | |
Month = feb, | |
Pages = {604-607}, | |
Volume = {433}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005Natur.433..604D}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1038/nature03335}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1038/nature03335}, | |
Eprint = {astro-ph/0502199} | |
} | |
@Article{di-matteo+2005, | |
Title = {{Energy input from quasars regulates the growth and | |
activity of black holes and their host galaxies}}, | |
Author = {{Di Matteo}, T. and {Springel}, V. and {Hernquist}, L.}, | |
Journal = {\nat}, | |
Year = {2005}, | |
Month = feb, | |
Pages = {604-607}, | |
Volume = {433}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005Natur.433..604D}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1038/nature03335}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1038/nature03335}, | |
Eprint = {astro-ph/0502199}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.02} | |
} | |
@Article{diamond-stanic+2009, | |
Title = {{High-redshift SDSS Quasars with Weak Emission Lines}}, | |
Author = {{Diamond-Stanic}, A.~M. and {Fan}, X. and {Brandt}, W.~N. | |
and {Shemmer}, O. and {Strauss}, M.~A. and {Anderson}, | |
S.~F. and {Carilli}, C.~L. and {Gibson}, R.~R. and {Jiang}, | |
L. and {Kim}, J.~S. and {Richards}, G.~T. and {Schmidt}, | |
G.~D. and {Schneider}, D.~P. and {Shen}, Y. and {Smith}, | |
P.~S. and {Vestergaard}, M. and {Young}, J.~E.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = jul, | |
Pages = {782-799}, | |
Volume = {699}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...699..782D}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/699/1/782}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/699/1/782}, | |
Eprint = {0904.2181}, | |
Keywords = {quasars: emission lines, quasars: general}, | |
Primaryclass = {astro-ph.GA} | |
} | |
@Article{do+2009, | |
Title = {{High Angular Resolution Integral-Field Spectroscopy of | |
the Galaxy's Nuclear Cluster: A Missing Stellar Cusp?}}, | |
Author = {{Do}, T. and {Ghez}, A.~M. and {Morris}, M.~R. and {Lu}, | |
J.~R. and {Matthews}, K. and {Yelda}, S. and {Larkin}, J.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = oct, | |
Pages = {1323-1337}, | |
Volume = {703}, | |
Abstract = {We report on the structure of the nuclear star cluster in | |
the innermost 0.16 pc of the Galaxy as measured by the | |
number density profile of late-type giants. Using laser | |
guide star adaptive optics in conjunction with the integral | |
field spectrograph, OSIRIS, at the Keck II telescope, we | |
are able to differentiate between the older, late-type (~ 1 | |
Gyr) stars, which are presumed to be dynamically relaxed, | |
and the unrelaxed young (~ 6 Myr) population. This | |
distinction is crucial for testing models of stellar cusp | |
formation in the vicinity of a black hole, as the models | |
assume that the cusp stars are in dynamical equilibrium in | |
the black hole potential. In the survey region, we | |
classified 60 stars as early-type (22 newly identified) and | |
74 stars as late-type (61 newly identified). We find that | |
contamination from young stars is significant, with more | |
than twice as many young stars as old stars in our | |
sensitivity range (K' < 15.5) within the central arcsecond. | |
Based on the late-type stars alone, the surface stellar | |
number density profile, Sigma(R) vprop R -Gamma, is flat, | |
with Gamma = -0.27 $\pm$ 0.19. Monte Carlo simulations of | |
the possible de-projected volume density profile, n(r) | |
vpropr -gamma, show that gamma is less than 1.0 at the | |
99.7% confidence level. These results are consistent with | |
the nuclear star cluster having no cusp, with a core | |
profile that is significantly flatter than that predicted | |
by most cusp formation theories, and even allows for the | |
presence of a central hole in the stellar distribution. Of | |
the possible dynamical interactions that can lead to the | |
depletion of the red giants observable in this | |
survey---stellar collisions, mass segregation from stellar | |
remnants, or a recent merger event---mass segregation is | |
the only one that can be ruled out as the dominant | |
depletion mechanism. The lack of a stellar cusp around a | |
supermassive black hole would have important implications | |
for black hole growth models and inferences on the presence | |
of a black hole based upon stellar distributions.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...703.1323D}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/0908.0311}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/703/2/1323}, | |
Bdsk-url-2 = {http://arxiv.org/abs/0908.0311}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2009ApJ...703.1323D}, | |
Date-added = {2017-01-13 17:31:02 +0000}, | |
Date-modified = {2017-01-13 17:31:04 +0000}, | |
Doi = {10.1088/0004-637X/703/2/1323}, | |
Eprint = {0908.0311}, | |
Keywords = {Galaxy: center, infrared: stars, stars: late-type, | |
techniques: high angular resolution, techniques: | |
spectroscopic} | |
} | |
@Article{donas+2007, | |
Title = {{GALEX UV Color Relations for Nearby Early-Type | |
Galaxies}}, | |
Author = {{Donas}, J. and others}, | |
Journal = {\apjs}, | |
Year = {2007}, | |
Month = dec, | |
Pages = {597-606}, | |
Volume = {173}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007ApJS..173..597D}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/516643}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/516643}, | |
Eprint = {astro-ph/0608594}, | |
Keywords = {Galaxies: Elliptical and Lenticular, cD, Galaxies: | |
Photometry, Galaxies: Stellar Content, Ultraviolet: | |
Galaxies} | |
} | |
@Article{dong+2011, | |
Title = {{Density Waves Excited by Low-mass Planets in | |
Protoplanetary Disks. II. High-resolution Simulations of | |
the Nonlinear Regime}}, | |
Author = {Dong, R and Rafikov, R.\~{}R. and Stone, J.\~{}M.}, | |
Journal = {\apj}, | |
Year = {2011}, | |
Month = nov, | |
Pages = {57}, | |
Volume = {741}, | |
Archiveprefix = {arXiv}, | |
Arxivid = {astro-ph.EP/1109.2590}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/741/1/57}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/741/1/57}, | |
Eprint = {1109.2590}, | |
Keywords = {methods: numerical, planet-disk interactions, planets and | |
satellites: formation, protoplanetary disks,hydrodynamics}, | |
Primaryclass = {astro-ph.EP} | |
} | |
@Article{dong+2011a, | |
Title = {{Density Waves Excited by Low-mass Planets in | |
Protoplanetary Disks. I. Linear Regime}}, | |
Author = {Dong, R and Rafikov, R.\~{}R. and Stone, J.\~{}M. and | |
Petrovich, C}, | |
Journal = {\apj}, | |
Year = {2011}, | |
Month = nov, | |
Pages = {56}, | |
Volume = {741}, | |
Archiveprefix = {arXiv}, | |
Arxivid = {astro-ph.EP/1109.1557}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/741/1/56}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/741/1/56}, | |
Eprint = {1109.1557}, | |
Keywords = {methods: numerical, planet-disk interactions, planets and | |
satellites: formation, protoplanetary disks,hydrodynamics}, | |
Primaryclass = {astro-ph.EP} | |
} | |
@Article{donley+2002, | |
Title = {{Large-Amplitude X-Ray Outbursts from Galactic Nuclei: A | |
Systematic Survey using ROSAT Archival Data}}, | |
Author = {{Donley}, J.~L. and {Brandt}, W.~N. and {Eracleous}, M. | |
and {Boller}, T.}, | |
Journal = {\aj}, | |
Year = {2002}, | |
Month = sep, | |
Pages = {1308-1321}, | |
Volume = {124}, | |
Abstract = {In recent years, luminous X-ray outbursts with variability | |
amplitudes as high as ~400 have been serendipitously | |
detected from a small number of active and inactive | |
galaxies. These outbursts may result from the tidal | |
disruptions of stars by supermassive black holes, as well | |
as accretion disk instabilities. In order to place the | |
first reliable constraints on the rate of such outbursts in | |
the universe and to test the stellar tidal disruption | |
hypothesis, we have performed a systematic and complete | |
survey for them by cross-correlating ROSAT All-Sky Survey | |
(RASS) and pointed Position Sensitive Proportional Counter | |
data. We have detected five galaxies that were in outburst | |
during the RASS, three of which show no signs of nuclear | |
activity; these objects had been reported on individually | |
in previous studies. After making reasonable corrections | |
for the complicated selection effects, we conclude that the | |
rate of large-amplitude X-ray outbursts from inactive | |
galaxies in the local universe is ~9.1×10-6 galaxy-1 yr-1. | |
This rate is consistent with the predicted rate of stellar | |
tidal disruption events in such galaxies. When only the two | |
active galaxies are considered, we find a rate for active | |
galaxies of ~8.5×10-4 galaxy-1 yr-1. In order to place | |
tighter constraints on these rates, additional outbursts | |
must be detected.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2002AJ....124.1308D}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/0206291}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/342280}, | |
Bdsk-url-2 = {http://arxiv.org/abs/astro-ph/0206291}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2002AJ....124.1308D}, | |
Date-added = {2016-03-17 16:24:27 +0000}, | |
Date-modified = {2016-03-17 16:24:28 +0000}, | |
Doi = {10.1086/342280}, | |
Eprint = {astro-ph/0206291}, | |
Keywords = {Galaxies: Active, Galaxies: Nuclei, X-Rays} | |
} | |
@Article{donnarumma+2015, | |
Title = {{SKA as a powerful hunter of jetted Tidal Disruption | |
Events}}, | |
Author = {{Donnarumma}, I. and {Rossi}, E.~M. and {Fender}, R. and | |
{Komossa}, S. and {Paragi}, Z. and {Van Velzen}, S. and | |
{Prandoni}, I.}, | |
Journal = {Advancing Astrophysics with the Square Kilometre Array | |
(AASKA14)}, | |
Year = {2015}, | |
Month = apr, | |
Pages = {54}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015aska.confE..54D}, | |
Archiveprefix = {arXiv}, | |
Eid = {54}, | |
Eprint = {1501.04640}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{donovan+2007, | |
Title = {{How Dry Are Red Mergers?}}, | |
Author = {{Donovan}, J.~L. and {Hibbard}, J.~E. and {van Gorkom}, | |
J.~H.}, | |
Journal = {\aj}, | |
Year = {2007}, | |
Month = sep, | |
Pages = {1118-1123}, | |
Volume = {134}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007AJ....134.1118D}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/520676}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/520676}, | |
Eprint = {0706.0734}, | |
Keywords = {galaxies: evolution, galaxies: interactions, galaxies: | |
ISM} | |
} | |
@Article{dotti+2007, | |
Title = {{Supermassive black hole binaries in gaseous and stellar | |
circumnuclear discs: orbital dynamics and gas accretion}}, | |
Author = {Dotti, M and Colpi, M and Haardt, F and Mayer, L}, | |
Journal = {\mnras}, | |
Year = {2007}, | |
Month = aug, | |
Pages = {956}, | |
Volume = {379}, | |
Abstract = {The dynamics of two massive black holes in a rotationally | |
supported nuclear disc of mass Mdisc = 108Msolar is | |
explored using N-body/smoothed particle hydrodynamics | |
simulations. Gas and star particles are copresent in the | |
disc. Described by a Mestel profile, the disc has a | |
vertical support provided by turbulence of the gas, and by | |
stellar velocity dispersion. A primary black hole of mass 4 | |
× 106Msolar is placed at the centre of the disc, while a | |
secondary black hole is set initially on an eccentric | |
corotating orbit in the disc plane. Its mass is in a 1:1, | |
1:4, and 1:10 ratio, relative to the primary. With this | |
choice, we mimic the dynamics of black hole pairs released | |
in the nuclear region at the end of a gas-rich galaxy | |
merger. It is found that, under the action of dynamical | |
friction, the two black holes form a close binary in \~{}10 | |
Myr. The inspiral process is insensitive to the mass | |
fraction in stars and gas present in the disc and is | |
accompanied by the circularization of the orbit. We detail | |
the gaseous mass profile bound to each black hole that can | |
lead to the formation of two small Keplerian discs, | |
weighing \~{}2per cent of the black hole mass, and of size | |
\~{}0.01 pc. The mass of the tightly (loosely) bound | |
particles increases (decreases) with time as the black | |
holes spiral into closer and closer orbits. Double active | |
galactic nucleus activity is expected to occur on an | |
estimated time-scale of <\~{}10 Myr, comparable to the | |
inspiral time-scale. The double nuclear point-like sources | |
that may appear during dynamical evolution will have | |
typical separations of <\~{}10 pc.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2007MNRAS.379..956D%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1111/j.1365-2966.2007.12010.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1365-2966.2007.12010.x}, | |
Keywords = {Hydrodynamics, galaxies: evolution, galaxies: nuclei, | |
galaxies: starburst,black hole physics}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2007MNRAS.379..956D\&link\_type=ABSTRACT} | |
} | |
@Article{dotti+2009, | |
Title = {{SDSSJ092712.65+294344.0: a candidate massive black hole | |
binary}}, | |
Author = {{Dotti}, M. and {Montuori}, C. and {Decarli}, R. and | |
{Volonteri}, M. and {Colpi}, M. and {Haardt}, F.}, | |
Journal = {\mnras}, | |
Year = {2009}, | |
Month = sep, | |
Pages = {L73-L77}, | |
Volume = {398}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009MNRAS.398L..73D}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1745-3933.2009.00714.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1745-3933.2009.00714.x}, | |
Eprint = {0809.3446}, | |
Keywords = {black hole physics, galaxies: kinematics and dynamics, | |
galaxies: nuclei, quasars: individual: | |
SDSSJ092712.65+294344.0} | |
} | |
@Article{dotti+2006, | |
Title = {{On the search of electromagnetic cosmological | |
counterparts to coalescences of massive black hole | |
binaries}}, | |
Author = {{Dotti}, M. and {Salvaterra}, R. and {Sesana}, A. and | |
{Colpi}, M. and {Haardt}, F.}, | |
Journal = {\mnras}, | |
Year = {2006}, | |
Month = oct, | |
Pages = {869-875}, | |
Volume = {372}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006MNRAS.372..869D}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2006.10905.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1365-2966.2006.10905.x}, | |
Eprint = {arXiv:astro-ph/0605624}, | |
Keywords = {accretion, accretion discs, black hole physics, | |
gravitational waves, quasars: general, galaxies: | |
starburst} | |
} | |
@Book{draine2011, | |
Title = {Physics of the interstellar and intergalactic medium}, | |
Author = {Draine, Bruce T.}, | |
Publisher = {Princeton University Press}, | |
Year = {2011}, | |
Address = {Princeton, N.J.}, | |
Series = {Princeton series in astrophysics}, | |
Annote = {LDR 01398cam 2200337 a 4500 001 16343119 005 | |
20110915092319.0 008 100721s2011 njuab b 001 0 eng 906 | |
$a7$bcbc$corignew$d1$eecip$f20$gy-gencatlg 925 0 | |
$aacquire$b2 shelf copies$xpolicy default 955 $bxh00 | |
2010-07-21$ixh07 2010-07-21 to Dewey$wrd11 2010-07-22$afc03 | |
2011-05-24 1 copy rec'd., to CIP ver.$frf10 2011-06-25 | |
Z-CipVer. to BCCD$trf18 2011-09-15 copy 2 added 010 $a | |
2010028285 020 $a9780691122137 (hardback : alk. paper) 020 | |
$a069112213X (hardback : alk. paper) 020 $a9780691122144 | |
(pbk. : alk. paper) 020 $a0691122148 (pbk. : alk. paper) | |
035 $a(OCoLC)ocn649926225 040 | |
$aDLC$cDLC$dYDX$dYDXCP$dBWX$dCDX$dDLC 042 $apcc 050 00 | |
$aQB790$b.D73 2011 082 00 $a523.1/135$222 100 1 $aDraine, | |
Bruce T.,$d1947- 245 10 $aPhysics of the interstellar and | |
intergalactic medium /$cBruce T. Draine. 260 $aPrinceton, | |
N.J. :$bPrinceton University Press,$cc2011. 300 $axviii, | |
540 p. :$bill. (some col.), maps ;$c25 cm. 490 1 | |
$aPrinceton series in astrophysics 504 $aIncludes | |
bibliographical references (p. [511]-528) and index. 650 0 | |
$aInterstellar matter$vTextbooks. 650 0 | |
$aGalaxies$vTextbooks. 650 0 $aAstrophysics$vTextbooks. 830 | |
0 $aPrinceton series in astrophysics. }, | |
Call-number = {QB790}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Dewey-call-number = {523.1/135}, | |
Genre = {Interstellar matter}, | |
ISBN = {9780691122137 (hardback : alk. paper)}, | |
Keywords = {Untitled; Untitled1}, | |
Library-id = {2010028285} | |
} | |
@Article{drake+2011, | |
Title = {{The Discovery and Nature of the Optical Transient | |
CSS100217:102913+404220}}, | |
Author = {{Drake}, A.~J. and {Djorgovski}, S.~G. and {Mahabal}, A. | |
and {Anderson}, J. and {Roy}, R. and {Mohan}, V. and | |
{Ravindranath}, S. and {Frail}, D. and {Gezari}, S. and | |
{Neill}, J.~D. and {Ho}, L.~C. and {Prieto}, J.~L. and | |
{Thompson}, D. and {Thorstensen}, J. and {Wagner}, M. and | |
{Kowalski}, R. and {Chiang}, J. and {Grove}, J.~E. and | |
{Schinzel}, F.~K. and {Wood}, D.~L. and {Carrasco}, L. and | |
{Recillas}, E. and {Kewley}, L. and {Archana}, K.~N. and | |
{Basu}, A. and {Wadadekar}, Y. and {Kumar}, B. and {Myers}, | |
A.~D. and {Phinney}, E.~S. and {Williams}, R. and {Graham}, | |
M.~J. and {Catelan}, M. and {Beshore}, E. and {Larson}, S. | |
and {Christensen}, E.}, | |
Journal = {\apj}, | |
Year = {2011}, | |
Month = jul, | |
Pages = {106}, | |
Volume = {735}, | |
Abstract = {We report on the discovery and observations of the | |
extremely luminous optical transient | |
CSS100217:102913+404220 (CSS100217 hereafter). | |
Spectroscopic observations showed that this transient was | |
coincident with a galaxy at redshift z = 0.147 and reached | |
an apparent magnitude of V ~ 16.3. After correcting for | |
foreground Galactic extinction we determine the absolute | |
magnitude to be MV = -22.7 approximately 45 days after | |
maximum light. Over a period of 287 rest-frame days, this | |
event had an integrated bolometric luminosity of 1.3 × | |
1052 erg based on time-averaged bolometric corrections of | |
~15 from V- and R-band observations. Analysis of the | |
pre-outburst Sloan Digital Sky Survey (SDSS) spectrum of | |
the source shows features consistent with a narrow-line | |
Seyfert 1 galaxy. High-resolution Hubble Space Telescope | |
and Keck follow-up observations show that the event | |
occurred within 150 pc of the nucleus of the galaxy, | |
suggesting a possible link to the active nuclear region. | |
However, the rapid outburst along with photometric and | |
spectroscopic evolution are much more consistent with a | |
luminous supernova. Line diagnostics suggest that the host | |
galaxy is undergoing significant star formation. We use | |
extensive follow-up of the event along with archival | |
Catalina Sky Survey NEO search and SDSS data to investigate | |
the three most likely sources of such an event: (1) an | |
extremely luminous supernova, (2) the tidal disruption of a | |
star by the massive nuclear black hole, and (3) variability | |
of the central active galactic nucleus (AGN). We find that | |
CSS100217 was likely an extremely luminous Type IIn | |
supernova and occurred within the range of the narrow-line | |
region of an AGN. We discuss how similar events may have | |
been missed in past supernova surveys because of confusion | |
with AGN activity.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011ApJ...735..106D}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1103.5514}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/735/2/106}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1103.5514}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2011ApJ...735..106D}, | |
Date-added = {2016-04-20 18:04:41 +0000}, | |
Date-modified = {2016-04-20 18:04:42 +0000}, | |
Doi = {10.1088/0004-637X/735/2/106}, | |
Eid = {106}, | |
Eprint = {1103.5514}, | |
Keywords = {galaxies: active, galaxies: nuclei, galaxies: stellar | |
content, supernovae: general} | |
} | |
@Article{dubus+1999, | |
Title = {{X-ray irradiation in low-mass binary systems}}, | |
Author = {{Dubus}, G. and {Lasota}, J.-P. and {Hameury}, J.-M. and | |
{Charles}, P. }, | |
Journal = {\mnras}, | |
Year = {1999}, | |
Month = feb, | |
Pages = {139-147}, | |
Volume = {303}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1999MNRAS.303..139D}, | |
Doi = {10.1046/j.1365-8711.1999.02212.x}, | |
Eprint = {astro-ph/9809036}, | |
Keywords = {ACCRETION, ACCRETION DISCS, INSTABILITIES, BINARIES : | |
CLOSE, X-RAYS: GENERAL} | |
} | |
@Article{duffell+2012, | |
Title = {{Global Calculations of Density Waves and Gap Formation in | |
Protoplanetary Disks Using a Moving Mesh}}, | |
Author = {Duffell, P.\~{}C. and MacFadyen, A.\~{}I.}, | |
Journal = {\apj}, | |
Year = {2012}, | |
Month = aug, | |
Pages = {7}, | |
Volume = {755}, | |
Archiveprefix = {arXiv}, | |
Arxivid = {astro-ph.EP/1202.5608}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/755/1/7}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/755/1/7}, | |
Eprint = {1202.5608}, | |
Keywords = {methods: numerical, planet-disk interactions, planets and | |
satellites: formation, protoplanetary disks,hydrodynamics}, | |
Primaryclass = {astro-ph.EP} | |
} | |
@Article{dutton+2010, | |
Title = {{The kinematic connection between galaxies and dark matter | |
haloes}}, | |
Author = {{Dutton}, A.~A. and {Conroy}, C. and {van den Bosch}, | |
F.~C. and {Prada}, F. and {More}, S.}, | |
Journal = {\mnras}, | |
Year = {2010}, | |
Month = sep, | |
Pages = {2-16}, | |
Volume = {407}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010MNRAS.407....2D}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2010.16911.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1365-2966.2010.16911.x}, | |
Eprint = {1004.4626}, | |
Keywords = {galaxies: elliptical and lenticular, cD, galaxies: | |
fundamental parameters, galaxies: haloes, galaxies: | |
kinematics and dynamics, galaxies: spiral}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{eckart+2002, | |
Title = {{Stellar orbits near Sagittarius A*}}, | |
Author = {{Eckart}, A. and {Genzel}, R. and {Ott}, T. and {Sch{\"o}del}, R. }, | |
Journal = {\mnras}, | |
Year = {2002}, | |
Month = apr, | |
Pages = {917-934}, | |
Volume = {331}, | |
Abstract = {The SHARP/NTT stellar proper motion data now cover an interval from 1992 to 2000 and allow us to determine orbital accelerations for some of the most central stars of the Galaxy. We confirm the stellar acceleration measurements obtained by Ghez et al. with NIRC at the Keck telescope. Our analysis differs in three main points from that of Ghez et al.: (1) we combine the high-precision but shorter time-scale NIRC/Keck data with the lower precision but longer time-scale SHARP/NTT data set; (2) we statistically correct the observed accelerations for geometrical projection effects; (3) we exclude star S8 from the analysis of the amount and position of the central mass. From the combined SHARP/NTT and NIRC/Keck data sets we show that the stars S2, and most likely S1 and S8 as well, are on bound, fairly inclined (60°<i <80°), and eccentric (0.4<e <0.95) orbits around a central dark mass. The combination of both data sets results in a position of this central mass of and of the nominal radio position of Sgr A*. The mean statistically corrected enclosed mass derived from accelerations is M acc =(5+/-3)×106 Msolar with current radial separations of S1 and S2 from Sgr A* of about 8-10mpc. This enclosed mass estimate is derived from individual stellar orbits as close to the massive black hole at the centre of the Milky Way as currently possible. Although the uncertainties are large, this estimate is fully consistent with the enclosed mass range of (2.6-3.3)×106 Msolar derived by Genzel et al. from radial and/or proper motion velocities of a homogenized sample of sources. Star S8 was excluded from the analysis, since for the current proper motion velocity and radial separation from the centre we find that the measured acceleration requires orbital motion around a compact object with a mass in excess of 3×106 Msolar . The data suggest either that this star was or is subject to a close interaction with a different object or that its position measurements are influenced by the emission of a different cluster star. Therefore we base the analysis of the enclosed mass solely on the available data for stars S1 and S2. We also discuss two late-type stars with projected separations from Sgr A* of about 0.5 and 1arcsec. In addition to proper motions, these stars have known radial velocities. Orbit calculations indicate that such stars are very likely at larger physical distances from the centre and part of the larger scale central stellar cluster with a core radius of approximately 0.3pc.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2002MNRAS.331..917E}, | |
Doi = {10.1046/j.1365-8711.2002.05237.x}, | |
Eprint = {astro-ph/0201031}, | |
Keywords = {black hole physics, stellar dynamics, astrometry, celestial mechanics, Galaxy: centre, infrared: general}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.27} | |
} | |
@Article{edgar2006, | |
Title = {{An alternative approach to viscosity in an accretion | |
disc}}, | |
Author = {Edgar, R.\~{}G.}, | |
Journal = {e-print arxiv:astro-ph/0609756}, | |
Year = {2006}, | |
Month = sep, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Keywords = {Astrophysics; Untitled; Untitled1} | |
} | |
@Article{eftekhari+2017, | |
Title = {{Radio Monitoring of the Tidal Disruption Event Swift | |
J164449.3+573451. III. Late-time Jet Energetics and a | |
Deviation from Equipartition}}, | |
Author = {{Eftekhari}, T. and {Berger}, E. and {Zauderer}, B.~A. and | |
{Margutti}, R. and {Alexander}, K.~D.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2017}, | |
Month = oct, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017arXiv171007289E}, | |
Archiveprefix = {arXiv}, | |
Eprint = {1710.07289}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{emsellem+2007, | |
Title = {{The SAURON project - IX. A kinematic classification for | |
early-type galaxies}}, | |
Author = {{Emsellem}, E. and {Cappellari}, M. and {Krajnovi{\'c}}, | |
D. and {van de Ven}, G. and {Bacon}, R. and {Bureau}, M. | |
and {Davies}, R.~L. and {de Zeeuw}, P.~T. and | |
{Falc{\'o}n-Barroso}, J. and {Kuntschner}, H. and | |
{McDermid}, R. and {Peletier}, R.~F. and {Sarzi}, M.}, | |
Journal = {\mnras}, | |
Year = {2007}, | |
Month = aug, | |
Pages = {401-417}, | |
Volume = {379}, | |
Abstract = {Two-dimensional stellar kinematics of 48 representative | |
elliptical (E) and lenticular (S0) galaxies obtained with | |
the SAURON integral-field spectrograph reveal that | |
early-type galaxies appear in two broad flavours, depending | |
on whether they exhibit clear large-scale rotation or not. | |
We define a new parameter , which involves | |
luminosity-weighted averages over the full two-dimensional | |
kinematic field as a proxy to quantify the observed | |
projected stellar angular momentum per unit mass. We use it | |
as a basis for a new kinematic classification: early-type | |
galaxies are separated into slow and fast rotators, | |
depending on whether they have lambdaR values within their | |
effective radius Re below or above 0.1, respectively. Slow | |
and fast rotators are shown to be physically distinct | |
classes of galaxies, a result which cannot simply be the | |
consequence of a biased viewing angle. Fast rotators tend | |
to be relatively low-luminosity galaxies with MB >~ -20.5. | |
Slow rotators tend to be brighter and more massive | |
galaxies, but are still spread over a wide range of | |
absolute magnitude. Three slow rotators of our sample, | |
among the most massive ones, are consistent with zero | |
rotation. Remarkably, all other slow rotators (besides the | |
atypical case of NGC 4550) contain a large kpc-scale | |
kinematically decoupled core (KDC). All fast rotators | |
(except one galaxy with well-known irregular shells) show | |
well-aligned photometric and kinemetric axes, and small | |
velocity twists, in contrast with most slow rotators which | |
exhibit significant misalignments and velocity twists. | |
These results are supported by a supplement of 18 | |
additional early-type galaxies observed with SAURON. In a | |
companion paper (Paper X), we also show that fast and slow | |
rotators are distinct classes in terms of their orbital | |
distribution. We suggest that gas is a key ingredient in | |
the formation and evolution of fast rotators, and that the | |
slowest rotators are the extreme evolutionary end point | |
reached deep in gravitational potential wells where | |
dissipationless mergers had a major role in the evolution, | |
and for which most of the baryonic angular momentum was | |
expelled outwards. Detailed numerical simulations in a | |
cosmological context are required to understand how to form | |
large-scale KDCs within slow rotators, and more generally | |
to explain the distribution of lambdaR values within | |
early-type galaxies and the distinction between fast and | |
slow rotators.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007MNRAS.379..401E}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0703531}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2007.11752.x}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0703531}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2007MNRAS.379..401E}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1365-2966.2007.11752.x}, | |
Eprint = {astro-ph/0703531}, | |
Keywords = {galaxies: elliptical and lenticular, cD, galaxies: | |
evolution, galaxies: formation, galaxies: kinematics and | |
dynamics, galaxies: structure} | |
} | |
@Article{eracleous+2012, | |
Title = {{A Large Systematic Search for Close Supermassive Binary | |
and Rapidly Recoiling Black Holes}}, | |
Author = {Eracleous, M and Boroson, T.\~{}A. and Halpern, J.\~{}P. | |
and Liu, J}, | |
Journal = {\apjs}, | |
Year = {2012}, | |
Month = aug, | |
Pages = {23}, | |
Volume = {201}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0067-0049/201/2/23}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0067-0049/201/2/23}, | |
Keywords = {line: profiles, quasars: emission lines, quasars: | |
general,galaxies: active} | |
} | |
@Article{eracleous+2010, | |
Title = {{Spectral Energy Distributions of Weak Active Galactic | |
Nuclei Associated with Low-Ionization Nuclear Emission | |
Regions}}, | |
Author = {{Eracleous}, M. and {Hwang}, J.~A. and {Flohic}, | |
H.~M.~L.~G.}, | |
Journal = {\apjs}, | |
Year = {2010}, | |
Month = mar, | |
Pages = {135-148}, | |
Volume = {187}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010ApJS..187..135E}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0067-0049/187/1/135}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0067-0049/187/1/135}, | |
Eprint = {1001.2924}, | |
Keywords = {galaxies: active, galaxies: nuclei, X-rays: galaxies}, | |
Primaryclass = {astro-ph.GA} | |
} | |
@Article{escala+2005, | |
Title = {{The Role of Gas in the Merging of Massive Black Holes in | |
Galactic Nuclei. II. Black Hole Merging in a Nuclear Gas | |
Disk}}, | |
Author = {Escala, A and Larson, R.\~{}B. and Coppi, P.\~{}S. and | |
Mardones, D}, | |
Journal = {\apj}, | |
Year = {2005}, | |
Month = sep, | |
Pages = {152--166}, | |
Volume = {630}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/431747}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/431747}, | |
Keywords = {Cosmology: Theory, Galaxies: Evolution, Galaxies: Nuclei, | |
Galaxies: Quasars: General, Hydrodynamics,Black Hole | |
Physics; Untitled; Untitled1} | |
} | |
@Article{esquej+2007, | |
Title = {{Candidate tidal disruption events from the XMM-Newton | |
slew survey}}, | |
Author = {{Esquej}, P. and {Saxton}, R.~D. and {Freyberg}, M.~J. and | |
{Read}, A.~M. and {Altieri}, B. and {Sanchez-Portal}, M. | |
and {Hasinger}, G.}, | |
Journal = {\aap}, | |
Year = {2007}, | |
Month = feb, | |
Pages = {L49-L52}, | |
Volume = {462}, | |
Abstract = {Context: In recent years, giant amplitude X-ray flares | |
have been observed from a handful of non-active galaxies. | |
The most plausible scenario of these unusual phenomena is | |
tidal disruption of a star by a quiescent supermassive | |
black hole at the centre of the galaxy. Aims: Only a small | |
number of these type of events have been observed and | |
confirmed to date. The discovery of more cases would allow | |
a number of fundamental conclusions to be drawn about | |
properties such as the frequency of tidal disruption | |
events, the distribution of quiescent black hole masses and | |
their influence in the context of galaxy/AGN formation and | |
evolution among others. Methods: Comparing the XMM-Newton | |
Slew Survey Source Catalogue with the ROSAT PSPC All-Sky | |
Survey five galaxies have been detected a factor of up to | |
88 brighter in XMM-Newton with respect to ROSAT PSPC upper | |
limits and presenting a soft X-ray colour. X-ray | |
luminosities of these sources derived from slew | |
observations have been found in the range 1041{-}1044 erg | |
s-1, fully consistent with the tidal disruption model. This | |
model predicts that during the peak of the outburst, flares | |
reach X-ray luminosities up to 1045 erg s-1, which is close | |
to the Eddington luminosity of the black hole, and | |
afterwards a decay of the flux on a time scale of months to | |
years is expected. Multi-wavelength follow-up observations | |
have been performed on these highly variable objects in | |
order to disentangle their nature and to investigate their | |
dynamical evolution. Results: Here we present sources | |
coming from the XMM-Newton Slew Survey that could fit in | |
the paradigm of tidal disruption events. X-ray and optical | |
observations revealed that two of these objects are in full | |
agreement with that scenario and three other sources that, | |
showing signs of optical activity, need further | |
investigation within the transient galactic nuclei | |
phenomena.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007A%26A...462L..49E}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0612340}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361:20066072}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0612340}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2007A%26A...462L..49E}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1051/0004-6361:20066072}, | |
Eprint = {astro-ph/0612340}, | |
Keywords = {surveys, galaxies: general, X-rays: general} | |
} | |
@Article{fabbiano+2011, | |
Title = {{A close nuclear black-hole pair in the spiral galaxy | |
NGC3393}}, | |
Author = {{Fabbiano}, G. and {Wang}, J. and {Elvis}, M. and | |
{Risaliti}, G.}, | |
Journal = {\nat}, | |
Year = {2011}, | |
Month = sep, | |
Pages = {431-434}, | |
Volume = {477}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011Natur.477..431F}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1038/nature10364}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1038/nature10364}, | |
Eprint = {1109.0483}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{faber+1997, | |
Title = {{The Centers of Early-Type Galaxies with HST. IV. Central | |
Parameter Relations.}}, | |
Author = {{Faber}, S.~M. and {Tremaine}, S. and {Ajhar}, E.~A. and | |
{Byun}, Y.-I. and {Dressler}, A. and {Gebhardt}, K. and | |
{Grillmair}, C. and {Kormendy}, J. and {Lauer}, T.~R. and | |
{Richstone}, D.}, | |
Journal = {\aj}, | |
Year = {1997}, | |
Month = nov, | |
Pages = {1771}, | |
Volume = {114}, | |
Abstract = {We analyze Hubble Space Telescope surface-brightness | |
profiles of 61 elliptical galaxies and spiral bulges | |
(hereafter "hot" galaxies). The profiles are parameterized | |
by break radius rbetaand break surface brightness 1beta | |
These are combined with central velocity dispersions, total | |
luminosities, rotation velocities, and isophote shapes to | |
explore correlations among central and global properties. | |
Luminous hot galaxies (Mv<-22) have cuspy cores with steep | |
outer power-law profiles that break at r≈rbeta to shallow | |
inner profiles Iâˆr-gamma with gamma<=0.3. Break radii and | |
core luminosities for these objects are approximately | |
proportional to effective radii and total luminosities. | |
Scaling relations are presented for several core parameters | |
as a function of total luminosity. Cores follow a | |
fundamental plane that parallels the global fundamental | |
plane for hot galaxies but is 30% thicker. Some of this | |
extra thickness may be due to the effect of massive black | |
holes (BHs) on central velocity dispersions. Faint hot | |
galaxies (Mv>-20.5) show steep, largely featureless | |
power-law profiles that lack cores. Measured values of rb | |
and b for these galaxies are limits only. At a limiting | |
radius of 10 pc, the centers of power-law galaxies are up | |
to 1000 times denser in mass and luminosity than the cores | |
of large galaxies. At intermediate magnitudes | |
(-22<Mv<-20.5), core and power-law galaxies coexist, and | |
there is a range in rbeta at a given luminosity of at least | |
two orders of magnitude. Here, central properties correlate | |
strongly with global rotation and shape: core galaxies tend | |
to be boxy and slowly rotating, whereas power-law galaxies | |
tend to be disky and rapidly rotating. A search for inner | |
disks was conducted to test a claim in the literature, | |
based on a smaller sample, that power laws originate from | |
edge-on stellar disks. We find only limited evidence for | |
such disks and believe that the difference between core and | |
power-law profiles reflects a real difference in the | |
spatial distribution of the luminous spheroidal component | |
of the galaxy. The dense power-law centers of disky, | |
rotating galaxies are consistent with their formation in | |
gas-rich mergers. The parallel proposition, that cores are | |
the by-products of gas-free stellar mergers, is less | |
compelling for at least two reasons: (1) dissipationless | |
hierarchical clustering does not appear to produce core | |
profiles like those seen; (2) core galaxies accrete small, | |
dense, gas-free galaxies at a rate sufficient to fill in | |
their low-density cores if the satellites survived and sank | |
to the center (whether the satellites survive is still an | |
open question). An alternative model for core formation | |
involves the orbital decay of massive BHs that are accreted | |
in mergers: the decaying BHs may heat and eject stars from | |
the center, eroding a power law if any exists and scouring | |
out a core. An average BH mass per spheroid of 0.002 times | |
the stellar mass yields cores in fair agreement with | |
observed cores and is consistent with the energetics of | |
AGNs and the kinematic detection of BHs in nearby galaxies. | |
An unresolved issue is why power-law galaxies also do not | |
have cores if this process operates in all hot galaxies.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1997AJ....114.1771F}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/9610055}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1086/118606}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/9610055}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/1997AJ....114.1771F}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/118606}, | |
Eprint = {astro-ph/9610055}, | |
Keywords = {GALAXIES: EARLY-TYPE, GALAXIES: NUCLEI} | |
} | |
@Article{fabian2012, | |
Title = {{Observational Evidence of Active Galactic Nuclei | |
Feedback}}, | |
Author = {{Fabian}, A.~C.}, | |
Journal = {\araa}, | |
Year = {2012}, | |
Month = sep, | |
Pages = {455-489}, | |
Volume = {50}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012ARA%26A..50..455F}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1146/annurev-astro-081811-125521}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1146/annurev-astro-081811-125521}, | |
Eprint = {1204.4114}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{fabian1994, | |
Title = {{Cooling Flows in Clusters of Galaxies}}, | |
Author = {{Fabian}, A.~C.}, | |
Journal = {\araa}, | |
Year = {1994}, | |
Pages = {277-318}, | |
Volume = {32}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1994ARA%26A..32..277F}, | |
Doi = {10.1146/annurev.aa.32.090194.001425} | |
} | |
@Article{fabian+1975, | |
Title = {{Tidal capture formation of binary systems and X-ray | |
sources in globular clusters}}, | |
Author = {{Fabian}, A.~C. and {Pringle}, J.~E. and {Rees}, M.~J.}, | |
Journal = {\mnras}, | |
Year = {1975}, | |
Month = aug, | |
Pages = {15p-18p}, | |
Volume = {172}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1975MNRAS.172P..15F}, | |
Doi = {10.1093/mnras/172.1.15P}, | |
Keywords = {Binary Stars, Globular Clusters, Stellar Radiation, Tides, | |
X Ray Astronomy, X Ray Stars, Error Analysis, Gravitational | |
Effects, Stellar Luminosity, Variable Stars} | |
} | |
@Article{fakhouri+2009, | |
Title = {{Environmental dependence of dark matter halo growth - I. | |
Halo merger rates}}, | |
Author = {{Fakhouri}, O. and {Ma}, C.-P.}, | |
Journal = {\mnras}, | |
Year = {2009}, | |
Month = apr, | |
Pages = {1825-1840}, | |
Volume = {394}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009MNRAS.394.1825F}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2009.14480.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1365-2966.2009.14480.x}, | |
Eprint = {0808.2471}, | |
Keywords = {galaxy: formation , galaxy: halo , cosmology: theory , | |
dark matter , large-scale structure of Universe} | |
} | |
@Article{farr+2017, | |
Title = {{Distinguishing spin-aligned and isotropic black hole | |
populations with gravitational waves}}, | |
Author = {{Farr}, W.~M. and {Stevenson}, S. and {Miller}, M.~C. and | |
{Mandel}, I. and {Farr}, B. and {Vecchio}, A.}, | |
Journal = {\nat}, | |
Year = {2017}, | |
Month = aug, | |
Pages = {426-429}, | |
Volume = {548}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017Natur.548..426F}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1038/nature23453}, | |
Eprint = {1706.01385}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{farrar&piran2014, | |
Title = {{Tidal disruption jets as the source of Ultra-High Energy | |
Cosmic Rays}}, | |
Author = {{Farrar}, G.~R. and {Piran}, T.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2014}, | |
Month = nov, | |
Abstract = {Observations of the spectacular, blazar-like tidal | |
disruption event (TDE) candidates Swift J1644+57 and | |
J2058+05 show that the conditions required for accelerating | |
protons to 10^{20} eV appear to be realized in the outer | |
jet, and possibly in the inner jet as well. Direct and | |
indirect estimates of the rate of jetted-TDEs, and of the | |
energy they inject, are compatible with the observed flux | |
of ultra-high energy cosmic rays (UHECRs) and the abundance | |
of presently contributing sources. Thus TDE-jets can be a | |
major source of UHECRs, even compabile with a pure proton | |
composition.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014arXiv1411.0704F}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1411.0704}, | |
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Bdsk-url-1 = {http://arXiv.org/abs/1411.0704}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/2014arXiv1411.0704F}, | |
Date-added = {2016-01-06 18:15:34 +0000}, | |
Date-modified = {2016-01-06 18:17:00 +0000}, | |
Eprint = {1411.0704}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{farris+2012, | |
Title = {{Binary black hole mergers in magnetized disks: | |
simulations in full general relativity}}, | |
Author = {Farris, B.\~{}D. and Gold, R and Paschalidis, V and | |
Etienne, Z.\~{}B. and Shapiro, S.\~{}L.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2012}, | |
Month = jul, | |
Archiveprefix = {arXiv}, | |
Arxivid = {astro-ph.HE/1207.3354}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {1207.3354}, | |
Keywords = {Astrophysics - Galaxy Astrophysics, General Relativity and | |
Quantum Cosmology,Astrophysics - High Energy Astrophysical | |
Phenomena; Untitled; Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{farris+2012a, | |
Title = {{Binary Black-Hole Mergers in Magnetized Disks: | |
Simulations in Full General Relativity}}, | |
Author = {Farris, B.\~{}D. and Gold, R and Paschalidis, V and | |
Etienne, Z.\~{}B. and Shapiro, S.\~{}L.}, | |
Journal = {Physical Review Letters}, | |
Year = {2012}, | |
Month = nov, | |
Number = {22}, | |
Pages = {221102}, | |
Volume = {109}, | |
Archiveprefix = {arXiv}, | |
Arxivid = {astro-ph.HE/1207.3354}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1103/PhysRevLett.109.221102}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1103/PhysRevLett.109.221102}, | |
Eprint = {1207.3354}, | |
Keywords = {Relativistic fluid dynamics,Numerical studies of black | |
holes and black-hole bi}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{farris+2013, | |
Title = {{Binary Black Hole Accretion From a Circumbinary Disk: Gas | |
Dynamics Inside the Central Cavity}}, | |
Author = {{Farris}, B.~D. and {Duffell}, P. and {MacFadyen}, A.~I. | |
and {Haiman}, Z.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2013}, | |
Month = oct, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2013arXiv1310.0492F}, | |
Archiveprefix = {arXiv}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {1310.0492}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena; | |
Untitled; Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{faucher&loeb2011, | |
Title = {{Pulsar-black hole binaries in the Galactic Centre}}, | |
Author = {{Faucher-Gigu{\`e}re}, C.-A. and {Loeb}, A.}, | |
Journal = {\mnras}, | |
Year = {2011}, | |
Month = aug, | |
Pages = {3951-3961}, | |
Volume = {415}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011MNRAS.415.3951F}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1111/j.1365-2966.2011.19019.x}, | |
Eprint = {1012.0573}, | |
Keywords = {black hole physics, binaries: general, stars: neutron, | |
pulsars: general, Galaxy: centre}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{feldman+2017, | |
Title = {{Colours, star formation rates and environments of | |
star-forming and quiescent galaxies at the cosmic noon}}, | |
Author = {{Feldmann}, R. and {Quataert}, E. and {Hopkins}, P.~F. and | |
{Faucher-Gigu{\`e}re}, C.-A. and {Kere{\v s}}, D.}, | |
Journal = {\mnras}, | |
Year = {2017}, | |
Month = sep, | |
Pages = {1050-1072}, | |
Volume = {470}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017MNRAS.470.1050F}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1093/mnras/stx1120}, | |
Eprint = {1610.02411}, | |
Keywords = {galaxies: evolution, galaxies: formation, galaxies: | |
haloes, galaxies: high-redshift, galaxies: star formation} | |
} | |
@Article{feldmeier+2014, | |
Title = {{Large scale kinematics and dynamical modelling of the Milky Way nuclear star cluster}}, | |
Author = {{Feldmeier}, A. and {Neumayer}, N. and {Seth}, A. and {Sch{\"o}del}, R. and {L{\"u}tzgendorf}, N. and {de Zeeuw}, P.~T. and {Kissler-Patig}, M. and {Nishiyama}, S. and {Walcher}, C.~J.}, | |
Journal = {\aap}, | |
Year = {2014}, | |
Month = oct, | |
Pages = {A2}, | |
Volume = {570}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014A%26A...570A...2F}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1051/0004-6361/201423777}, | |
Eid = {A2}, | |
Eprint = {1406.2849}, | |
Keywords = {Galaxy: nucleus, Galaxy: kinematics and dynamics}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.20} | |
} | |
@Article{feldmeier+2017, | |
Title = {{Triaxial orbit-based modelling of the Milky Way Nuclear Star Cluster}}, | |
Author = {{Feldmeier-Krause}, A. and {Zhu}, L. and {Neumayer}, N. and {van de Ven}, G. and {de Zeeuw}, P.~T. and {Sch{\"o}del}, R. }, | |
Journal = {\mnras}, | |
Year = {2017}, | |
Month = apr, | |
Pages = {4040-4052}, | |
Volume = {466}, | |
Abstract = {We construct triaxial dynamical models for the Milky Way nuclear star cluster using Schwarzschild's orbit superposition technique. We fit the stellar kinematic maps presented in Feldmeier et al. The models are used to constrain the supermassive black hole mass M?, dynamical mass-to-light ratio ? and the intrinsic shape of the cluster. Our best-fitting model has M? = (3.0^{+1.1}_{-1.3}) × 106 M?, ? = (0.90^{+0.76}_{-0.08}) M?/L?, 4.5?m and a compression of the cluster along the line of sight. Our results are in agreement with the direct measurement of the supermassive black hole mass using the motion of stars on Keplerian orbits. The mass-to-light ratio is consistent with stellar population studies of other galaxies in the mid-infrared. It is possible that we underestimate M? and overestimate the cluster's triaxiality due to observational effects. The spatially semiresolved kinematic data and extinction within the nuclear star cluster bias the observations to the near side of the cluster, and may appear as a compression of the nuclear star cluster along the line of sight. We derive a total dynamical mass for the Milky Way nuclear star cluster of MMWNSC = (2.1 ± 0.7) × 107 M? within a sphere with radius r = 2 × reff = 8.4 pc. The best-fitting model is tangentially anisotropic in the central r = 0.5-2 pc of the nuclear star cluster, but close to isotropic at larger radii. Our triaxial models are able to recover complex kinematic substructures in the velocity map.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017MNRAS.466.4040F}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1093/mnras/stw3377}, | |
Eprint = {1701.01583}, | |
Keywords = {Galaxy: center, kinematics and dynamics, Galaxy: centre, Galaxy: kinematics and dynamics}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.20} | |
} | |
@Article{ferrarese&ford2005, | |
Title = {{Supermassive Black Holes in Galactic Nuclei: Past, | |
Present and Future Research}}, | |
Author = {Ferrarese, L and Ford, H}, | |
Journal = {\ssr}, | |
Year = {2005}, | |
Month = feb, | |
Pages = {523--624}, | |
Volume = {116}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1007/s11214-005-3947-6}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1007/s11214-005-3947-6} | |
} | |
@Article{ferrarese+2005, | |
Title = {{Supermassive Black Holes in Galactic Nuclei: Past, | |
Present and Future Research}}, | |
Author = {Ferrarese, L and Ford, H}, | |
Journal = {\ssr}, | |
Year = {2005}, | |
Month = feb, | |
Pages = {523--624}, | |
Volume = {116}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1007/s11214-005-3947-6}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1007/s11214-005-3947-6} | |
} | |
@Article{ferrarese&merritt2000, | |
Title = {{A Fundamental Relation between Supermassive Black Holes | |
and Their Host Galaxies}}, | |
Author = {{Ferrarese}, L. and {Merritt}, D.}, | |
Journal = {\apjl}, | |
Year = {2000}, | |
Month = aug, | |
Pages = {L9-L12}, | |
Volume = {539}, | |
Abstract = {The masses of supermassive black holes correlate almost | |
perfectly with the velocity dispersions of their host | |
bulges, Mbh~??, where ?=4.8+/-0.5. The relation is much | |
tighter than the relation between Mbh and bulge luminosity, | |
with a scatter no larger than expected on the basis of | |
measurement error alone. Black hole masses recently | |
estimated by Magorrian et al. lie systematically above the | |
Mbh-? relation defined by more accurate mass estimates, | |
some by as much as 2 orders of magnitude. The tightness of | |
the Mbh-? relation implies a strong link between black hole | |
formation and the properties of the stellar bulge.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2000ApJ...539L...9F}, | |
Doi = {10.1086/312838}, | |
Eprint = {astro-ph/0006053}, | |
Keywords = {Black Hole Physics, Galaxies: Evolution, Galaxies: | |
Kinematics and Dynamics}, | |
Owner = {aleksey}, | |
Timestamp = {2018.02.02} | |
} | |
@Article{ferrarese+2000, | |
Title = {{A Fundamental Relation between Supermassive Black Holes | |
and Their Host Galaxies}}, | |
Author = {{Ferrarese}, L. and {Merritt}, D.}, | |
Journal = {\apjl}, | |
Year = {2000}, | |
Month = aug, | |
Pages = {L9-L12}, | |
Volume = {539}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2000ApJ...539L...9F}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/312838}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/312838}, | |
Eprint = {arXiv:astro-ph/0006053}, | |
Keywords = {Black Hole Physics, Galaxies: Evolution, Galaxies: | |
Kinematics and Dynamics} | |
} | |
@Article{ferriere2012, | |
Title = {{Interstellar gas within \~{}10 pc of Sagittarius | |
A$^{*}$}}, | |
Author = {{Ferri{\`e}re}, K.}, | |
Journal = {\aap}, | |
Year = {2012}, | |
Month = apr, | |
Pages = {A50}, | |
Volume = {540}, | |
Abstract = {Aims: We seek to obtain a coherent and realistic | |
three-dimensional picture of the interstellar gas out to | |
about 10 pc of the dynamical center of our Galaxy, which is | |
supposed to be at Sgr A*. Methods: We review the existing | |
observational studies on the different gaseous components | |
that have been identified near Sgr A*, and retain all the | |
information relating to their spatial configuration and/or | |
physical state. Based on the collected information, we | |
propose a three-dimensional representation of the | |
interstellar gas, which describes each component in terms | |
of both its precise location and morphology and its | |
thermodynamic properties. Results: The interstellar gas | |
near Sgr A* can be represented by five basic components, | |
which are, by order of increasing size: (1) a central | |
cavity with roughly equal amounts of warm ionized and | |
atomic gases; (2) a ring of mainly molecular gas; (3) a | |
supernova remnant filled with hot ionized gas; (4) a radio | |
halo of warm ionized gas and relativistic particles; and | |
(5) a belt of massive molecular clouds. While the halo gas | |
fills ≈80% of the studied volume, the molecular | |
components enclose ≈ 98% of the interstellar mass.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012A%26A...540A..50F}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1201.6031}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361/201117181}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1201.6031}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2012A%26A...540A..50F}, | |
Date-added = {2016-04-18 23:27:24 +0000}, | |
Date-modified = {2016-04-18 23:27:24 +0000}, | |
Doi = {10.1051/0004-6361/201117181}, | |
Eid = {A50}, | |
Eprint = {1201.6031}, | |
Keywords = {ISM: structure, Galaxy: center, Galaxy: nucleus, ISM: | |
general, ISM: kinematics and dynamics, ISM: supernova | |
remnants} | |
} | |
@Article{floyd+2004, | |
Title = {{The host galaxies of luminous quasars}}, | |
Author = {{Floyd}, D.~J.~E. and {Kukula}, M.~J. and {Dunlop}, J.~S. | |
and {McLure}, R.~J. and {Miller}, L. and {Percival}, W.~J. | |
and {Baum}, S.~A. and {O'Dea}, C.~P.}, | |
Journal = {\mnras}, | |
Year = {2004}, | |
Month = nov, | |
Pages = {196-220}, | |
Volume = {355}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2004MNRAS.355..196F}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2004.08315.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1365-2966.2004.08315.x}, | |
Eprint = {arXiv:astro-ph/0308436}, | |
Keywords = {black hole physics, galaxies: active, galaxies: evolution, | |
quasars: general} | |
} | |
@Article{fraggione&sari2018, | |
Author = {{Fraggione} G., {Sari} R.}, | |
Year = {2018}, | |
Owner = {aleksey}, | |
Timestamp = {2017.12.07} | |
} | |
@Article{fragione&sari2018, | |
Title = {{Steeper Stellar Cusps in Galactic Centers from Binary Disruption}}, | |
Author = {{Fragione}, G. and {Sari}, R.}, | |
Journal = {\apj}, | |
Year = {2018}, | |
Month = jan, | |
Pages = {51}, | |
Volume = {852}, | |
Abstract = {The relaxed distribution of stars around a massive black hole is known to follow a cusp profile, ? (r)\propto {r}-? , with a characteristic slope ? =7/4. This follows from energy conservation and a scattering rate given by two-body encounters. However, we show that the injection of stars close to the black hole, i.e., a source term in the standard cusp picture, modifies this profile. In the steady-state configuration, the cusp develops a central region with a typical slope ? =9/4 in which stars diffuse outward. Binary disruption by the intense tidal field of the massive black hole is among the phenomena that take place in the Galactic Center (GC). In such a disruption, one of the binary members remains bound to the black hole, thus providing a source term of stars close to the black hole. Assuming a binary fraction of 0.1 and an orbital circularization efficiency of 0.35, we show that this source is strong enough to modify the cusp profile within ? 0.07 pc of the GC. If the binary fraction at the influence radius is of order unity and the orbits of all captured stars are efficiently circularized, the steeper cusp extends almost as far as the radius of influence of the black hole.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2018ApJ...852...51F}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/1538-4357/aaa0d7}, | |
Eid = {51}, | |
Eprint = {1712.03242}, | |
Keywords = {binaries: general, Galaxy: center, Galaxy: kinematics and dynamics, stars: kinematics and dynamics }, | |
Owner = {aleksey}, | |
Timestamp = {2018.05.02} | |
} | |
@Article{fragione&sari2017, | |
Title = {{Steeper stellar cusps in galactic centers from binary | |
disruption}}, | |
Author = {{Fragione}, G. and {Sari}, R.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2017}, | |
Month = dec, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017arXiv171203242F}, | |
Archiveprefix = {arXiv}, | |
Eprint = {1712.03242}, | |
Keywords = {Astrophysics - Astrophysics of Galaxies} | |
} | |
@Article{frail+2000, | |
Title = {{A 450 Day Light Curve of the Radio Afterglow of GRB 970508: Fireball Calorimetry}}, | |
Author = {{Frail}, D.~A. and {Waxman}, E. and {Kulkarni}, S.~R.}, | |
Journal = {\apj}, | |
Year = {2000}, | |
Month = jul, | |
Pages = {191-204}, | |
Volume = {537}, | |
Abstract = {We report on the results of an extensive monitoring campaign of the radio afterglow of GRB 970508, lasting 450 days after the burst. The spectral and temporal radio behavior indicate that the fireball has undergone a transition to subrelativistic expansion at t~100 days. This allows us to perform ``calorimetry'' of the explosion. The derived total energy, E0~5×1050 ergs, is well below the ~5×1051 ergs inferred under the assumption of spherical symmetry from gamma-ray and early afterglow observations. A natural consequence of this result, which can also account for deviations at t<100 days from the spherical relativistic fireball model predictions, is that the fireball was initially a wide-angle jet of opening angle ~30°. Our analysis also allows determination of the energy fractions carried by the electrons and magnetic field and the density of the ambient medium surrounding the fireball. We find that during the subrelativistic expansion, the electrons and magnetic field are close to equipartition and the density of the ambient medium is ~1 cm -3. The inferred density rules out the possibility that the fireball expands into a strongly nonuniform medium, as would be expected, e.g., in the case of a massive star progenitor.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2000ApJ...537..191F}, | |
Doi = {10.1086/309024}, | |
Eprint = {astro-ph/9910319}, | |
Keywords = {Gamma Rays: Bursts, Radio Continuum: General}, | |
Owner = {aleksey}, | |
Timestamp = {2018.04.03} | |
} | |
@Book{frank+2002, | |
Title = {{Accretion Power in Astrophysics: Third Edition}}, | |
Author = {{Frank}, J. and {King}, A. and {Raine}, D.~J.}, | |
Year = {2002}, | |
Month = jan, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2002apa..book.....F}, | |
Booktitle = {Accretion Power in Astrophysics, by Juhan Frank and Andrew | |
King and Derek Raine, pp.~398.~ISBN 0521620538.~Cambridge, | |
UK: Cambridge University Press, February 2002.}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Keywords = {Untitled; Untitled1} | |
} | |
@Article{fregeau+2004, | |
Title = {{Stellar collisions during binary-binary and binary-single | |
star interactions}}, | |
Author = {{Fregeau}, J.~M. and {Cheung}, P. and {Portegies Zwart}, | |
S.~F. and {Rasio}, F.~A.}, | |
Journal = {\mnras}, | |
Year = {2004}, | |
Month = jul, | |
Pages = {1-19}, | |
Volume = {352}, | |
Abstract = {Physical collisions between stars occur frequently in | |
dense star clusters, either via close encounters between | |
two single stars, or during strong dynamical interactions | |
involving binary stars. Here we study stellar collisions | |
that occur during binary-single and binary-binary | |
interactions, by performing numerical scattering | |
experiments. Our results include cross-sections, branching | |
ratios and sample distributions of parameters for various | |
outcomes. For interactions of hard binaries containing | |
main-sequence stars, we find that the normalized | |
cross-section for at least one collision to occur (between | |
any two of the four stars involved) is essentially unity, | |
and that the probability of collisions involving more than | |
two stars is significant. Hydrodynamic calculations have | |
shown that the effective radius of a collision product can | |
be 2-30 times larger than the normal main-sequence radius | |
for a star of the same total mass. We study the effect of | |
this expansion, and find that it increases the probability | |
of further collisions considerably. We discuss these | |
results in the context of recent observations of blue | |
stragglers in globular clusters with masses exceeding twice | |
the main-sequence turn-off mass. We also present FEWBODY, a | |
new, freely available numerical toolkit for simulating | |
small-N gravitational dynamics that is particularly suited | |
to performing scattering experiments.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2004MNRAS.352....1F}, | |
Doi = {10.1111/j.1365-2966.2004.07914.x}, | |
Eprint = {astro-ph/0401004}, | |
Keywords = {stellar dynamics, methods: N-body simulations, methods: | |
numerical, binaries: close, blue stragglers, globular | |
clusters: general}, | |
Owner = {aleksey}, | |
Timestamp = {2018.01.14} | |
} | |
@Article{freitag+2006, | |
Title = {{Stellar Remnants in Galactic Nuclei: Mass Segregation}}, | |
Author = {{Freitag}, M. and {Amaro-Seoane}, P. and {Kalogera}, V.}, | |
Journal = {\apj}, | |
Year = {2006}, | |
Month = sep, | |
Pages = {91-117}, | |
Volume = {649}, | |
Abstract = {The study of how stars distribute themselves around a | |
massive black hole (MBH) in the center of a galaxy is an | |
important prerequisite for the understanding of many | |
galactic-center processes. These include the observed | |
overabundance of point X-ray sources at the Galactic center | |
and the prediction of rates and characteristics of tidal | |
disruptions of extended stars by the MBH and of inspirals | |
of compact stars into the MBH, the latter being events of | |
high importance for the future space-borne gravitational | |
wave interferometer LISA. In relatively small galactic | |
nuclei hosting MBHs with masses in the range 105-107 | |
Msolar, the single most important dynamical process is | |
two-body relaxation. It induces the formation of a steep | |
density cusp around the MBH and strong mass segregation, as | |
more massive stars lose energy to lighter ones and drift to | |
the central regions. Using a spherical stellar dynamical | |
Monte Carlo code, we simulate the long-term relaxational | |
evolution of galactic nucleus models with a spectrum of | |
stellar masses. Our focus is the concentration of stellar | |
black holes to the immediate vicinity of the MBH. We | |
quantify this mass segregation for a variety of galactic | |
nucleus models and discuss its astrophysical implications. | |
Special attention is given to models developed to match the | |
conditions in the Milky Way nucleus; we examine the | |
presence of compact objects in connection to recent | |
high-resolution X-ray observations.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006ApJ...649...91F}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0603280}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/506193}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0603280}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2006ApJ...649...91F}, | |
Date-added = {2016-01-18 03:43:05 +0000}, | |
Date-modified = {2016-01-18 03:43:06 +0000}, | |
Doi = {10.1086/506193}, | |
Eprint = {astro-ph/0603280}, | |
Keywords = {Black Hole Physics, Galaxies: Nuclei, Galaxies: Star | |
Clusters, Gravitational Waves, Methods: n-Body Simulations, | |
Stellar Dynamics} | |
} | |
@Article{freitag+2002, | |
Title = {{A new Monte Carlo code for star cluster simulations. II. | |
Central black hole and stellar collisions}}, | |
Author = {{Freitag}, M. and {Benz}, W.}, | |
Journal = {\aap}, | |
Year = {2002}, | |
Month = oct, | |
Pages = {345-374}, | |
Volume = {394}, | |
Abstract = {We have recently written a new code to simulate the long | |
term evolution of spherical clusters of stars. It is based | |
on the pioneering Monte Carlo scheme proposed by H{\'e}non | |
in the 70's. Unlike other implementations of this numerical | |
method which were successfully used to investigate the | |
dynamics of globular clusters, our code has been devised in | |
the specific goal to treat dense galactic nuclei. In a | |
previous paper, we described the basic version of our code | |
which includes 2-body relaxation as the only physical | |
process. In the present work, we go on and include further | |
physical ingredients that are mostly relevant to galactic | |
nuclei, namely the presence of a central (growing) black | |
hole (BH) and collisions between (main sequence) stars. | |
Stars that venture too close to the BH are destroyed by the | |
tidal field. We took particular care of this process | |
because of its importance, both as a channel to feed the BH | |
and a way to produce accretion flares from otherwise | |
quiescent galactic nuclei. Collisions between stars have | |
often been proposed as another mechanism to drive stellar | |
matter into the central BH. Furthermore, non disruptive | |
collisions may create peculiar stellar populations which | |
are of great observational interest in the case of the | |
central cluster of our Galaxy. To get the best handle on | |
the role of this process in galactic nuclei, we include it | |
with unpreceded realism through the use of a set of more | |
than 10 000 collision simulations carried out with a SPH | |
(Smoothed Particle Hydrodynamics) code. Stellar evolution | |
has also been introduced in a simple way, similar to what | |
has been done in previous dynamical simulations of galactic | |
nuclei. To ensure that this physics is correctly simulated, | |
we realized a variety of tests whose results are reported | |
here. This unique code, featuring most important physical | |
processes, allows million particle simulations, spanning a | |
Hubble time, in a few CPU days on standard personal | |
computers and provides a wealth of data only rivalized by | |
N-body simulations.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2002A%26A...394..345F}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0204292}, | |
Bdsk-file-1 = {YnBsaXN0MDDUAQIDBAUGJCVYJHZlcnNpb25YJG9iamVjdHNZJGFyY2hpdmVyVCR0b3ASAAGGoKgHCBMUFRYaIVUkbnVsbNMJCgsMDxJXTlMua2V5c1pOUy5vYmplY3RzViRjbGFzc6INDoACgAOiEBGABIAFgAdccmVsYXRpdmVQYXRoWWFsaWFzRGF0YV8QLS4uLy4uLy4uLy4uL0RvY3VtZW50cy9QYXBlcnMvZnJlaXRhZy8yMDAyLnBkZtIXCxgZV05TLmRhdGFPEQGQAAAAAAGQAAIAAAxNYWNpbnRvc2ggSEQAAAAAAAAAAAAAAAAAAADNZNKaSCsAAAHzvdgIMjAwMi5wZGYAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAfPEsNLB2Z4AAAAAAAAAAAAEAAQAAAkgAAAAAAAAAAAAAAAAAAAAB0ZyZWl0YWcAABAACAAAzWUK2gAAABEACAAA0sIf7gAAAAEAFAHzvdgBB4gEAAXEKgAFxCkAAhDpAAIAQU1hY2ludG9zaCBIRDpVc2VyczoAYWxla3NleToARG9jdW1lbnRzOgBQYXBlcnM6AEZyZWl0YWc6ADIwMDIucGRmAAAOABIACAAyADAAMAAyAC4AcABkAGYADwAaAAwATQBhAGMAaQBuAHQAbwBzAGgAIABIAEQAEgAvVXNlcnMvYWxla3NleS9Eb2N1bWVudHMvUGFwZXJzL2ZyZWl0YWcvMjAwMi5wZGYAABMAAS8AABUAAgAO//8AAIAG0hscHR5aJGNsYXNzbmFtZVgkY2xhc3Nlc11OU011dGFibGVEYXRhox0fIFZOU0RhdGFYTlNPYmplY3TSGxwiI1xOU0RpY3Rpb25hcnmiIiBfEA9OU0tleWVkQXJjaGl2ZXLRJidUcm9vdIABAAgAEQAaACMALQAyADcAQABGAE0AVQBgAGcAagBsAG4AcQBzAHUAdwCEAI4AvgDDAMsCXwJhAmYCcQJ6AogCjAKTApwCoQKuArECwwLGAssAAAAAAAACAQAAAAAAAAAoAAAAAAAAAAAAAAAAAAACzQ==}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361:20021142}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0204292}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2002A%26A...394..345F}, | |
Date-added = {2016-01-18 04:52:02 +0000}, | |
Date-modified = {2016-01-18 04:52:03 +0000}, | |
Doi = {10.1051/0004-6361:20021142}, | |
Eprint = {astro-ph/0204292}, | |
Keywords = {methods: numerical, galaxies: stellar dynamics, galaxies: | |
nuclei, galaxies: star clusters} | |
} | |
@Article{french+2017, | |
Title = {{The Post-starburst Evolution of Tidal Disruption Event Host Galaxies}}, | |
Author = {{French}, K.~D. and {Arcavi}, I. and {Zabludoff}, A.}, | |
Journal = {\apj}, | |
Year = {2017}, | |
Month = feb, | |
Pages = {176}, | |
Volume = {835}, | |
Abstract = {We constrain the recent star formation histories of the host galaxies of eight optical/UV-detected tidal disruption events (TDEs). Six hosts had quick starbursts of <200 Myr duration that ended 10-1000 Myr ago, indicating that TDEs arise at different times in their hosts? post-starburst evolution. If the disrupted star formed in the burst or before, the post-burst age constrains its mass, generally excluding O, most B, and highly massive A stars. If the starburst arose from a galaxy merger, the time since the starburst began limits the coalescence timescale and thus the merger mass ratio to more equal than 12:1 in most hosts. This uncommon ratio, if also that of the central supermassive black hole (SMBH) binary, disfavors the scenario in which the TDE rate is boosted by the binary but is insensitive to its mass ratio. The stellar mass fraction created in the burst is 0.5%-10% for most hosts, not enough to explain the observed 30-200× boost in TDE rates, suggesting that the host?s core stellar concentration is more important. TDE hosts have stellar masses 109.4-1010.3 M?, consistent with the Sloan Digital Sky Survey volume-corrected, quiescent Balmer-strong comparison sample and implying SMBH masses of 105.5-107.5 M?. Subtracting the host absorption line spectrum, we uncover emission lines; at least five hosts have ionization sources inconsistent with star formation that instead may be related to circumnuclear gas, merger shocks, or post-AGB stars.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017ApJ...835..176F}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/1538-4357/835/2/176}, | |
Eid = {176}, | |
Eprint = {1609.04755}, | |
Keywords = {galaxies: evolution, galaxies: nuclei}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.13} | |
} | |
@Article{french+2016, | |
Title = {{Tidal Disruption Events Prefer Unusual Host Galaxies}}, | |
Author = {{French}, K.~D. and {Arcavi}, I. and {Zabludoff}, A.}, | |
Journal = {\apjl}, | |
Year = {2016}, | |
Month = feb, | |
Pages = {L21}, | |
Volume = {818}, | |
Abstract = {Tidal Disruption Events (TDEs) are transient events observed when a star passes close enough to a supermassive black hole to be tidally destroyed. Many TDE candidates have been discovered in host galaxies whose spectra have weak or no line emission yet strong Balmer line absorption, indicating a period of intense star formation that has recently ended. As such, TDE host galaxies fall into the rare class of quiescent Balmer-strong galaxies. Here, we quantify the fraction of galaxies in the Sloan Digital Sky Survey (SDSS) with spectral properties like those of TDE hosts, determining the extent to which TDEs are over-represented in such galaxies.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016ApJ...818L..21F}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/2041-8205/818/1/L21}, | |
Eid = {L21}, | |
Eprint = {1601.04705}, | |
Keywords = {galaxies: evolution, galaxies: nuclei}, | |
Owner = {aleksey}, | |
Timestamp = {2018.10.10} | |
} | |
@Misc{fryxell+2010, | |
Title = {{FLASH: Adaptive Mesh Hydrodynamics Code for Modeling | |
Astrophysical Thermonuclear Flashes}}, | |
Author = {{Fryxell}, B. and {Olson}, K. and {Ricker}, P. and | |
{Timmes}, F.~X. and {Zingale}, M. and {Lamb}, D.~Q. and | |
{MacNeice}, P. and {Rosner}, R. and {Truran}, J.~W. and | |
{Tufo}, H.}, | |
HowPublished = {Astrophysics Source Code Library}, | |
Month = oct, | |
Year = {2010}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010ascl.soft10082F}, | |
Archiveprefix = {ascl}, | |
Eprint = {1010.082}, | |
Keywords = {Software}, | |
Owner = {aleksey}, | |
Timestamp = {2017.11.01} | |
} | |
@Article{fryxell+2000, | |
Title = {{FLASH: An Adaptive Mesh Hydrodynamics Code for Modeling | |
Astrophysical Thermonuclear Flashes}}, | |
Author = {Fryxell, B and Olson, K and Ricker, P and Timmes, F X and | |
Zingale, M and Lamb, D Q and MacNeice, P and Rosner, R and | |
Truran, J W and Tufo, H}, | |
Journal = {\apjs}, | |
Year = {2000}, | |
Month = nov, | |
Pages = {273}, | |
Volume = {131}, | |
Abstract = {We report on the completion of the first version of a | |
new-generation simulation code, FLASH. The FLASH code | |
solves the fully compressible, reactive hydrodynamic | |
equations and allows for the use of adaptive mesh | |
refinement. It also contains state-of-the-art modules for | |
the equations of state and thermonuclear reaction networks. | |
The FLASH code was developed to study the problems of | |
nuclear flashes on the surfaces of neutron stars and white | |
dwarfs, as well as in the interior of white dwarfs. We | |
expect, however, that the FLASH code will be useful for | |
solving a wide variety of other problems. This first | |
version of the code has been subjected to a large variety | |
of test cases and is currently being used for production | |
simulations of X-ray bursts, Rayleigh-Taylor and | |
Richtmyer-Meshkov instabilities, and thermonuclear flame | |
fronts. The FLASH code is portable and already runs on a | |
wide variety of massively parallel machines, including some | |
of the largest machines now extant.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2000ApJS..131..273F%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1086/317361}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/317361}, | |
Keywords = {Abundances, Equation of State, Hydrodynamics, Methods: | |
Numerical, Nucleosynthesis, Stars: General,Nuclear | |
Reactions}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2000ApJS..131..273F\&link\_type=ABSTRACT} | |
} | |
@Article{fujita+2014, | |
Title = {{AGN jet power and feedback controlled by Bondi accretion | |
in brightest cluster galaxies}}, | |
Author = {{Fujita}, Y. and {Kawakatu}, N. and {Shlosman}, I.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2014}, | |
Month = jun, | |
Abstract = {(Abridged) We propose a new method to estimate the Bondi | |
(hot gas) accretion rates onto the supermassive black holes | |
(SMBHs) at the centres of elliptical galaxies. It can be | |
applied even if the Bondi radius is not well-resolved in | |
X-ray observations. This method is based on two simple | |
assumptions: (1) hot gas outside the Bondi radius is in | |
nearly a hydrostatic equilibrium in a gravitational | |
potential, and (2) the gas temperature near the galaxy | |
centre is close to the virial temperature of the galaxy. We | |
apply this method to 28 bright elliptical galaxies in | |
nearby galaxy clusters (27 of them are the brightest | |
cluster galaxies; BCGs). We find a strong correlation | |
between the Bondi accretion rates and the power of jets | |
associated with the SMBHs. For most galaxies, the accretion | |
rates are large enough to account for the jet powers. Our | |
results indicate that hot gas in the elliptical galaxies | |
directly controls the feedback from the active galactic | |
nuclei (AGN), which leads to a stable heating of the | |
cluster cool cores. We also find that more massive SMBHs in | |
BCGs tend to have larger specific growth rates. This may | |
explain the hyper masses (~10^10 Msun) of some of the | |
SMBHs. Comparison between the accretion rates and the X-ray | |
luminosities of the AGN suggests that the AGN in the BCGs | |
are extremely radiatively inefficient compared with X-ray | |
binaries in the Milky Way. Lastly, we find a tight | |
correlation between the Bondi accretion rates and the X-ray | |
luminosities of cool cores. Their relation is nearly linear | |
and the power generated by the Bondi accretion is large | |
enough to compensate the radiative cooling of the cool | |
cores. The results of this study demonstrate that the AGN | |
feedback associated with Bondi accretion is essential to | |
suppress cooling flows in clusters.}, | |
Adscomment = {submitted to MNRAS}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014arXiv1406.6366F}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1406.6366}, | |
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Bdsk-url-1 = {http://arXiv.org/abs/1406.6366}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/2014arXiv1406.6366F}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {1406.6366}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena, | |
Astrophysics - Astrophysics of Galaxies; Untitled; | |
Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{fuller&lai2012, | |
Title = {{Dynamical tides in compact white dwarf binaries: tidal | |
synchronization and dissipation}}, | |
Author = {{Fuller}, J. and {Lai}, D.}, | |
Journal = {\mnras}, | |
Year = {2012}, | |
Month = mar, | |
Pages = {426-445}, | |
Volume = {421}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012MNRAS.421..426F}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1111/j.1365-2966.2011.20320.x}, | |
Eprint = {1108.4910}, | |
Keywords = {hydrodynamics, waves, binaries: close, stars: kinematics | |
and dynamics, white dwarfs}, | |
Primaryclass = {astro-ph.SR} | |
} | |
@Article{fuller&lai2011, | |
Title = {{Tidal excitations of oscillation modes in compact white | |
dwarf binaries - I. Linear theory}}, | |
Author = {{Fuller}, J. and {Lai}, D.}, | |
Journal = {\mnras}, | |
Year = {2011}, | |
Month = apr, | |
Pages = {1331-1340}, | |
Volume = {412}, | |
Abstract = {We study the tidal excitation of gravity modes (g-modes) | |
in compact white dwarf binary systems with periods ranging | |
from minutes to hours. As the orbit of the system decays | |
via gravitational radiation, the orbital frequency | |
increases and sweeps through a series of resonances with | |
the g-modes of the white dwarf. At each resonance, the | |
tidal force excites the g-mode to a relatively large | |
amplitude, transferring the orbital energy to the stellar | |
oscillation. We calculate the eigenfrequencies of g-modes | |
and their coupling coefficients with the tidal field for | |
realistic non-rotating white dwarf models. Using these mode | |
properties, we numerically compute the excited mode | |
amplitude in the linear approximation as the orbit passes | |
though the resonance, including the back reaction of the | |
mode on the orbit. We also derive analytical estimates for | |
the mode amplitude and the duration of the resonance, which | |
accurately reproduce our numerical results for most binary | |
parameters. We find that the g-modes can be excited to a | |
dimensionless (mass-weighted) amplitude up to 0.1, with the | |
mode energy approaching 10-3 of the gravitational binding | |
energy of the star. Therefore the low-frequency (≲10-2 | |
Hz) gravitational waveforms produced by the binaries, | |
detectable by LISA, are strongly affected by the tidal | |
resonances. Our results also suggest that thousands of | |
years prior to the binary merger, the white dwarf may be | |
heated up significantly by tidal interactions. However, | |
more study is needed since the physical amplitudes of the | |
excited oscillation modes become highly non-linear in the | |
outer layer of the star, which can reduce the mode | |
amplitude attained by tidal excitation.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011MNRAS.412.1331F}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1009.3316}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2010.18017.x}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1009.3316}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2011MNRAS.412.1331F}, | |
Date-added = {2017-08-23 20:59:56 +0000}, | |
Date-modified = {2017-08-23 20:59:56 +0000}, | |
Doi = {10.1111/j.1365-2966.2010.18017.x}, | |
Eprint = {1009.3316}, | |
Keywords = {binaries: close, stars: interiors, stars: kinematics and | |
dynamics, stars: oscillations, white dwarfs}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{gultekin+2009, | |
Title = {{The M-{$\sigma$} and M-L Relations in Galactic Bulges, | |
and Determinations of Their Intrinsic Scatter}}, | |
Author = {{G{\"u}ltekin}, K. and {Richstone}, D.~O. and {Gebhardt}, | |
K. and {Lauer}, T.~R. and {Tremaine}, S. and {Aller}, M.~C. | |
and {Bender}, R. and {Dressler}, A. and {Faber}, S.~M. and | |
{Filippenko}, A.~V. and {Green}, R. and {Ho}, L.~C. and | |
{Kormendy}, J. and {Magorrian}, J. and {Pinkney}, J. and | |
{Siopis}, C.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = jun, | |
Pages = {198-221}, | |
Volume = {698}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...698..198G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/698/1/198}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/698/1/198}, | |
Eprint = {0903.4897}, | |
Keywords = {black hole physics, galaxies: general, galaxies: nuclei, | |
galaxies: statistics, stellar dynamics; Untitled; | |
Untitled1}, | |
Primaryclass = {astro-ph.GA} | |
} | |
@Article{gultekin+2009a, | |
Title = {{The M-{$\sigma$} and M-L Relations in Galactic Bulges, | |
and Determinations of Their Intrinsic Scatter}}, | |
Author = {{G{\"u}ltekin}, K. and {Richstone}, D.~O. and {Gebhardt}, | |
K. and {Lauer}, T.~R. and {Tremaine}, S. and {Aller}, M.~C. | |
and {Bender}, R. and {Dressler}, A. and {Faber}, S.~M. and | |
{Filippenko}, A.~V. and {Green}, R. and {Ho}, L.~C. and | |
{Kormendy}, J. and {Magorrian}, J. and {Pinkney}, J. and | |
{Siopis}, C.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = jun, | |
Pages = {198-221}, | |
Volume = {698}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...698..198G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/698/1/198}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/698/1/198}, | |
Eprint = {0903.4897}, | |
Keywords = {black hole physics, galaxies: general, galaxies: nuclei, | |
galaxies: statistics, stellar dynamics; Untitled; | |
Untitled1}, | |
Primaryclass = {astro-ph.GA} | |
} | |
@Article{gunther+2004, | |
Title = {{Evolution of irradiated circumbinary disks}}, | |
Author = {{G{\"u}nther}, R. and {Sch{\"a}fer}, C. and {Kley}, W.}, | |
Journal = {\aap}, | |
Year = {2004}, | |
Month = aug, | |
Pages = {559-566}, | |
Volume = {423}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2004A%26A...423..559G}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361:20040223}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1051/0004-6361:20040223}, | |
Eprint = {arXiv:astro-ph/0405053}, | |
Keywords = {accretion, accretion disks, stars: binaries: | |
spectroscopic, hydrodynamics, methods: numerical} | |
} | |
@Article{gabasch+2004, | |
Title = {{The evolution of the luminosity functions in the FORS | |
Deep Field from low to high redshift. I. The blue bands}}, | |
Author = {{Gabasch}, A. and {Bender}, R. and {Seitz}, S. and {Hopp}, | |
U. and {Saglia}, R.~P. and {Feulner}, G. and {Snigula}, J. | |
and {Drory}, N. and {Appenzeller}, I. and {Heidt}, J. and | |
{Mehlert}, D. and {Noll}, S. and {B{\"o}hm}, A. and | |
{J{\"a}ger}, K. and {Ziegler}, B. and {Fricke}, K.~J.}, | |
Journal = {\aap}, | |
Year = {2004}, | |
Month = jul, | |
Pages = {41-58}, | |
Volume = {421}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2004A%26A...421...41G}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361:20035909}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1051/0004-6361:20035909}, | |
Eprint = {arXiv:astro-ph/0403535}, | |
Keywords = {galaxies: luminosity function, mass function, galaxy: | |
fundamental parameters, galaxies: high-redshift, galaxies: | |
distances and redshifts, galaxies: evolution} | |
} | |
@Article{gabasch+2006, | |
Title = {{The evolution of the luminosity functions in the FORS | |
deep field from low to high redshift. II. The red bands}}, | |
Author = {{Gabasch}, A. and {Hopp}, U. and {Feulner}, G. and | |
{Bender}, R. and {Seitz}, S. and {Saglia}, R.~P. and | |
{Snigula}, J. and {Drory}, N. and {Appenzeller}, I. and | |
{Heidt}, J. and {Mehlert}, D. and {Noll}, S. and | |
{B{\"o}hm}, A. and {J{\"a}ger}, K. and {Ziegler}, B.}, | |
Journal = {\aap}, | |
Year = {2006}, | |
Month = mar, | |
Pages = {101-121}, | |
Volume = {448}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006A%26A...448..101G}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361:20053986}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1051/0004-6361:20053986}, | |
Eprint = {arXiv:astro-ph/0510339}, | |
Keywords = {galaxies: luminosity function, mass function, galaxies: | |
fundamental, parameters, galaxies: high-redshift, galaxies: | |
distances and, redshifts, galaxies: evolution} | |
} | |
@Article{gallo+2008, | |
Title = {{AMUSE-Virgo. I. Supermassive Black Holes in Low-Mass | |
Spheroids}}, | |
Author = {{Gallo}, E. and {Treu}, T. and {Jacob}, J. and {Woo}, | |
J.-H. and {Marshall}, P.~J. and {Antonucci}, R.}, | |
Journal = {\apj}, | |
Year = {2008}, | |
Month = jun, | |
Pages = {154-168}, | |
Volume = {680}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2008ApJ...680..154G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/588012}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/588012}, | |
Eprint = {0711.2073}, | |
Keywords = {Black Hole Physics, Galaxies: Clusters: Individual: Name: | |
Virgo, Galaxies: Nuclei} | |
} | |
@Article{gallo+2010, | |
Title = {{AMUSE-Virgo. II. Down-sizing in Black Hole Accretion}}, | |
Author = {{Gallo}, E. and {Treu}, T. and {Marshall}, P.~J. and | |
{Woo}, J.-H. and {Leipski}, C. and {Antonucci}, R.}, | |
Journal = {\apj}, | |
Year = {2010}, | |
Month = may, | |
Pages = {25-36}, | |
Volume = {714}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010ApJ...714...25G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/714/1/25}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/714/1/25}, | |
Eprint = {1002.3619}, | |
Keywords = {black hole physics, galaxies: clusters: individual: Virgo; | |
Untitled; Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{gallo+2010a, | |
Title = {{AMUSE-Virgo. II. Down-sizing in Black Hole Accretion}}, | |
Author = {{Gallo}, E. and {Treu}, T. and {Marshall}, P.~J. and | |
{Woo}, J.-H. and {Leipski}, C. and {Antonucci}, R.}, | |
Journal = {\apj}, | |
Year = {2010}, | |
Month = may, | |
Pages = {25-36}, | |
Volume = {714}, | |
Abstract = {We complete the census of nuclear X-ray activity in 100 | |
early-type Virgo galaxies observed by the Chandra X-ray | |
Telescope as part of the AMUSE-Virgo survey, down to a | |
(3sigma) limiting luminosity of 3.7 × 1038 erg s-1 over | |
0.5-7 keV. The stellar mass distribution of the targeted | |
sample, which is mostly composed of formally "inactive" | |
galaxies, peaks below 1010 M sun, a regime where the very | |
existence of nuclear supermassive black holes (SMBHs) is | |
debated. Out of 100 objects, 32 show a nuclear X-ray | |
source, including 6 hybrid nuclei which also host a massive | |
nuclear cluster as visible from archival Hubble Space | |
Telescope images. After carefully accounting for | |
contamination from nuclear low-mass X-ray binaries based on | |
the shape and normalization of their X-ray luminosity | |
function (XLF), we conclude that between 24% and 34% of the | |
galaxies in our sample host an X-ray active SMBH (at the | |
95% confidence level). This sets a firm lower limit to the | |
black hole (BH) occupation fraction in nearby bulges within | |
a cluster environment. The differential logarithmic XLF of | |
active SMBHs scales with the X-ray luminosity as L X | |
-0.4$\pm$0.1 up to 1042 erg s-1. At face value, the active | |
fraction---down to our luminosity limit---is found to | |
increase with host stellar mass. However, taking into | |
account selection effects, we find that the average | |
Eddington-scaled X-ray luminosity scales with BH mass as M | |
BH ^{-0.62^{+0.13}_{-0.12}}, with an intrinsic scatter of | |
0.46+0.08 -0.06 dex. This finding can be interpreted as | |
observational evidence for "down-sizing" of BH accretion in | |
local early types, that is, low-mass BHs shine relatively | |
closer to their Eddington limit than higher mass objects. | |
As a consequence, the fraction of active galaxies, defined | |
as those above a fixed X-ray Eddington ratio, decreases | |
with increasing BH mass.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010ApJ...714...25G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1002.3619}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/714/1/25}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1002.3619}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2010ApJ...714...25G}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/714/1/25}, | |
Eprint = {1002.3619}, | |
Keywords = {black hole physics, galaxies: clusters: individual: Virgo; | |
Untitled; Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{gan+2014, | |
Title = {{Active Galactic Nucleus Feedback in an Isolated | |
Elliptical Galaxy: The Effect of Strong Radiative Feedback | |
in the Kinetic Mode}}, | |
Author = {{Gan}, Z. and {Yuan}, F. and {Ostriker}, J.~P. and | |
{Ciotti}, L. and {Novak}, G.~S.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = jul, | |
Pages = {150}, | |
Volume = {789}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...789..150G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/789/2/150}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/789/2/150}, | |
Eid = {150}, | |
Eprint = {1403.0670}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: | |
active, galaxies: elliptical and lenticular, cD, galaxies: | |
evolution, galaxies: nuclei; Untitled; Untitled1} | |
} | |
@Article{gan+2014a, | |
Title = {{Active Galactic Nucleus Feedback in an Isolated | |
Elliptical Galaxy: The Effect of Strong Radiative Feedback | |
in the Kinetic Mode}}, | |
Author = {{Gan}, Z. and {Yuan}, F. and {Ostriker}, J.~P. and | |
{Ciotti}, L. and {Novak}, G.~S.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = jul, | |
Pages = {150}, | |
Volume = {789}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...789..150G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/789/2/150}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/789/2/150}, | |
Eid = {150}, | |
Eprint = {1403.0670}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: | |
active, galaxies: elliptical and lenticular, cD, galaxies: | |
evolution, galaxies: nuclei; Untitled; Untitled1} | |
} | |
@Article{gan+2014b, | |
Title = {{Active Galactic Nucleus Feedback in an Isolated Elliptical Galaxy: The Effect of Strong Radiative Feedback in the Kinetic Mode}}, | |
Author = {{Gan}, Z. and {Yuan}, F. and {Ostriker}, J.~P. and {Ciotti}, L. and {Novak}, G.~S.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = jul, | |
Pages = {150}, | |
Volume = {789}, | |
Abstract = {Based on two-dimensional high-resolution hydrodynamic numerical simulation, we study the mechanical and radiative feedback effects from the central active galactic nucleus (AGN) on the cosmological evolution of an isolated elliptical galaxy. The inner boundary of the simulation domain is carefully chosen so that the fiducial Bondi radius is resolved and the accretion rate of the black hole is determined self-consistently. It is well known that when the accretion rates are high and low, the central AGNs will be in cold and hot accretion modes, which correspond to the radiative and kinetic feedback modes, respectively. The emitted spectrum from the hot accretion flows is harder than that from the cold accretion flows, which could result in a higher Compton temperature accompanied by a more efficient radiative heating, according to previous theoretical works. Such a difference of the Compton temperature between the two feedback modes, the focus of this study, has been neglected in previous works. Significant differences in the kinetic feedback mode are found as a result of the stronger Compton heating. More importantly, if we constrain models to correctly predict black hole growth and AGN duty cycle after cosmological evolution, we find that the favored model parameters are constrained: mechanical feedback efficiency diminishes with decreasing luminosity (the maximum efficiency being ~= 10-3.5), and X-ray Compton temperature increases with decreasing luminosity, although models with fixed mechanical efficiency and Compton temperature can be found that are satisfactory as well. We conclude that radiative feedback in the kinetic mode is much more important than previously thought.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...789..150G}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1088/0004-637X/789/2/150}, | |
Eid = {150}, | |
Eprint = {1403.0670}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: active, galaxies: elliptical and lenticular, cD, galaxies: evolution, galaxies: nuclei}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.07} | |
} | |
@Article{gaskell1996, | |
Title = {{Evidence for Binary Orbital Motion of a Quasar Broad-Line | |
Region}}, | |
Author = {{Gaskell}, C.~M.}, | |
Journal = {\apjl}, | |
Year = {1996}, | |
Month = jun, | |
Pages = {L107}, | |
Volume = {464}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1996ApJ...464L.107G}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/310119}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/310119}, | |
Eprint = {arXiv:astro-ph/9605185}, | |
Keywords = {ACCRETION, ACCRETION DISKS, BLACK HOLE PHYSICS, GALAXIES: | |
ACTIVE, GALAXIES: QUASARS: EMISSION LINES, GALAXIES: | |
QUASARS: GENERAL, GALAXIES: INDIVIDUAL ALPHANUMERIC: 3C | |
390.3} | |
} | |
@Article{gaspari+2015, | |
Title = {{Chaotic cold accretion on to black holes in rotating | |
atmospheres}}, | |
Author = {{Gaspari}, M. and {Brighenti}, F. and {Temi}, P.}, | |
Journal = {\aap}, | |
Year = {2015}, | |
Month = jul, | |
Pages = {A62}, | |
Volume = {579}, | |
Abstract = {The fueling of black holes is one key problem in the | |
evolution of baryons in the universe. Chaotic cold | |
accretion (CCA) profoundly differs from classic accretion | |
models, as Bondi and thin disc theories. Using 3D | |
high-resolution hydrodynamic simulations, we now probe the | |
impact of rotation on the hot and cold accretion flow in a | |
typical massive galaxy. In the hot mode, with or without | |
turbulence, the pressure-dominated flow forms a | |
geometrically thick rotational barrier, suppressing the | |
black hole accretion rate to ~1/3 of the spherical case | |
value. When radiative cooling is dominant, the gas loses | |
pressure support and quickly circularizes in a cold thin | |
disk; the accretion rate is decoupled from the cooling | |
rate, although it is higher than that of the hot mode. In | |
the more common state of a turbulent and heated atmosphere, | |
CCA drives the dynamics if the gas velocity dispersion | |
exceeds the rotational velocity, i.e., turbulent Taylor | |
number Tat< 1. Extended multiphase filaments condense out | |
of the hot phase via thermal instability (TI) and rain | |
toward the black hole, boosting the accretion rate up to | |
100 times the Bondi rate (M* ~ Mcool). Initially, | |
turbulence broadens the angular momentum distribution of | |
the hot gas, allowing the cold phase to condense with | |
prograde or retrograde motion. Subsequent chaotic | |
collisions between the cold filaments, clouds, and a clumpy | |
variable torus promote the cancellation of angular | |
momentum, leading to high accretion rates. As turbulence | |
weakens (Tat > 1), the broadening of the distribution and | |
the efficiency of collisions diminish, damping the | |
accretion rate ∠Tat-1, until the cold disk drives the | |
dynamics. This is exacerbated by the increased difficulty | |
to grow TI in a rotating halo. The simulated sub-Eddington | |
accretion rates cover the range inferred from AGN cavity | |
observations. CCA predicts inner flat X-ray temperature and | |
r-1 density profiles, as recently discovered in M 87 and | |
NGC 3115. The synthetic Halpha images reproduce the main | |
features of cold gas observations in massive ellipticals, | |
as the line fluxes and the filaments versus disk | |
morphology. Such dichotomy is key for the long-term AGN | |
feedback cycle. As gas cools, filamentary CCA develops and | |
boosts AGN heating; the cold mode is thus reduced and the | |
rotating disk remains the sole cold structure. Its | |
consumption leaves the atmosphere in hot mode with | |
suppressed accretion and feedback, reloading the cycle.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015A%26A...579A..62G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1407.7531}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361/201526151}, | |
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Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2015A%26A...579A..62G}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1051/0004-6361/201526151}, | |
Eid = {A62}, | |
Eprint = {1407.7531}, | |
Keywords = {accretion, accretion disks, black hole physics, | |
hydrodynamics, galaxies: ISM, instabilities, turbulence} | |
} | |
@Article{gaspari+2012, | |
Title = {{Mechanical AGN feedback: controlling the thermodynamical | |
evolution of elliptical galaxies}}, | |
Author = {{Gaspari}, M. and {Brighenti}, F. and {Temi}, P.}, | |
Journal = {\mnras}, | |
Year = {2012}, | |
Month = jul, | |
Pages = {190-209}, | |
Volume = {424}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012MNRAS.424..190G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2012.21183.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1365-2966.2012.21183.x}, | |
Eprint = {1202.6054}, | |
Keywords = {hydrodynamics, galaxies: active, intergalactic medium, | |
galaxies: ISM, galaxies: jets, X-rays: galaxies}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{gaspari+2013, | |
Title = {{Chaotic cold accretion on to black holes}}, | |
Author = {{Gaspari}, M. and {Ruszkowski}, M. and {Oh}, S.~P.}, | |
Journal = {\mnras}, | |
Year = {2013}, | |
Month = jul, | |
Pages = {3401-3422}, | |
Volume = {432}, | |
Abstract = {Bondi theory is often assumed to adequately describe the | |
mode of accretion in astrophysical environments. However, | |
the Bondi flow must be adiabatic, spherically symmetric, | |
steady, unperturbed, with constant boundary conditions. | |
Using 3D adaptive mesh refinement simulations, linking the | |
50 kpc to the sub-parsec (sub-pc) scales over the course of | |
40 Myr, we systematically relax the classic assumptions in | |
a typical galaxy hosting a supermassive black hole. In the | |
more realistic scenario, where the hot gas is cooling, | |
while heated and stirred on large scales, the accretion | |
rate is boosted up to two orders of magnitude compared with | |
the Bondi prediction. The cause is the non-linear growth of | |
thermal instabilities, leading to the condensation of cold | |
clouds and filaments when tcool/tff ≲ 10. The clouds | |
decouple from the hot gas, `raining' on to the centre. | |
Subsonic turbulence of just over 100 km s-1 (M > 0.2) | |
induces the formation of thermal instabilities, even in the | |
absence of heating, while in the transonic regime turbulent | |
dissipation inhibits their growth (tturb/tcool ≲ 1). When | |
heating restores global thermodynamic balance, the | |
formation of the multiphase medium is violent, and the mode | |
of accretion is fully cold and chaotic. The recurrent | |
collisions and tidal forces between clouds, filaments and | |
the central clumpy torus promote angular momentum | |
cancellation, hence boosting accretion. On sub-pc scales | |
the clouds are channelled to the very centre via a funnel. | |
In this study, we do not inject a fixed initial angular | |
momentum, though vorticity is later seeded by turbulence. A | |
good approximation to the accretion rate is the cooling | |
rate, which can be used as subgrid model, physically | |
reproducing the boost factor of 100 required by | |
cosmological simulations, while accounting for the frequent | |
fluctuations. Since our modelling is fairly general | |
(turbulence/heating due to AGN feedback, galaxy motions, | |
mergers, stellar evolution), chaotic cold accretion may be | |
common in many systems, such as hot galactic haloes, groups | |
and clusters. In this mode, the black hole can quickly | |
react to the state of the entire host galaxy, leading to | |
efficient self-regulated AGN feedback and the symbiotic | |
Magorrian relation. Chaotic accretion can generate | |
high-velocity clouds, likely leading to strong variations | |
in the AGN luminosity, and the deflection or mass-loading | |
of jets. During phases of overheating, the hot mode becomes | |
the single channel of accretion, though strongly suppressed | |
by turbulence. High-resolution data could determine the | |
current mode of accretion: assuming quiescent feedback, the | |
cold mode results in a quasi-flat-temperature core as | |
opposed to the cuspy profile of the hot mode.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2013MNRAS.432.3401G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1301.3130}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stt692}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1301.3130}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2013MNRAS.432.3401G}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1093/mnras/stt692}, | |
Eprint = {1301.3130}, | |
Keywords = {black hole physics, hydrodynamics, instabilities, | |
turbulence, methods: numerical, galaxies: ISM} | |
} | |
@Article{ge+2012, | |
Title = {{Double-peaked Narrow Emission-line Galaxies from the | |
Sloan Digital Sky Survey. I. Sample and Basic Properties}}, | |
Author = {{Ge}, J.-Q. and {Hu}, C. and {Wang}, J.-M. and {Bai}, | |
J.-M. and {Zhang}, S.}, | |
Journal = {\apjs}, | |
Year = {2012}, | |
Month = aug, | |
Pages = {31}, | |
Volume = {201}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012ApJS..201...31G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0067-0049/201/2/31}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0067-0049/201/2/31}, | |
Eid = {31}, | |
Eprint = {1208.2485}, | |
Keywords = {black hole physics, galaxies: evolution}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{gebhardt+2000, | |
Title = {{A Relationship between Nuclear Black Hole Mass and Galaxy | |
Velocity Dispersion}}, | |
Author = {{Gebhardt}, K. and {Bender}, R. and {Bower}, G. and | |
{Dressler}, A. and {Faber}, S.~M. and {Filippenko}, A.~V. | |
and {Green}, R. and {Grillmair}, C. and {Ho}, L.~C. and | |
{Kormendy}, J. and {Lauer}, T.~R. and {Magorrian}, J. and | |
{Pinkney}, J. and {Richstone}, D. and {Tremaine}, S.}, | |
Journal = {\apjl}, | |
Year = {2000}, | |
Month = aug, | |
Pages = {L13-L16}, | |
Volume = {539}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2000ApJ...539L..13G}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/312840}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/312840}, | |
Eprint = {arXiv:astro-ph/0006289}, | |
Keywords = {Galaxies: General, Galaxies: Nuclei, Galaxies: | |
Statistics} | |
} | |
@Article{gebhardt+2000a, | |
Title = {{A Relationship between Nuclear Black Hole Mass and Galaxy | |
Velocity Dispersion}}, | |
Author = {{Gebhardt}, K. and {Bender}, R. and {Bower}, G. and | |
{Dressler}, A. and {Faber}, S.~M. and {Filippenko}, A.~V. | |
and {Green}, R. and {Grillmair}, C. and {Ho}, L.~C. and | |
{Kormendy}, J. and {Lauer}, T.~R. and {Magorrian}, J. and | |
{Pinkney}, J. and {Richstone}, D. and {Tremaine}, S.}, | |
Journal = {\apjl}, | |
Year = {2000}, | |
Month = aug, | |
Pages = {L13-L16}, | |
Volume = {539}, | |
Abstract = {We describe a correlation between the mass Mbh of a | |
galaxy's central black hole and the luminosity-weighted | |
line-of-sight velocity dispersion ?e within the half-light | |
radius. The result is based on a sample of 26 galaxies, | |
including 13 galaxies with new determinations of black hole | |
masses from Hubble Space Telescope measurements of stellar | |
kinematics. The best-fit correlation is Mbh=1.2(+/-0.2)?08 | |
Msolar(?e/200 km s-1)3.75 (+/-0.3) over almost 3 orders of | |
magnitude in Mbh; the scatter in Mbh at fixed ?e is only | |
0.30 dex, and most of this is due to observational errors. | |
The Mbh-?e relation is of interest not only for its strong | |
predictive power but also because it implies that central | |
black hole mass is constrained by and closely related to | |
properties of the host galaxy's bulge.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2000ApJ...539L..13G}, | |
Doi = {10.1086/312840}, | |
Eprint = {astro-ph/0006289}, | |
Keywords = {Galaxies: General, Galaxies: Nuclei, Galaxies: | |
Statistics}, | |
Owner = {aleksey}, | |
Timestamp = {2018.02.02} | |
} | |
@Article{generozov+2014a, | |
Title = {{Physical Properties of the Inner Shocks in Hot, Tilted | |
Black Hole Accretion Flows}}, | |
Author = {{Generozov}, A. and {Blaes}, O. and {Fragile}, P.~C. and | |
{Henisey}, K.~B.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = jan, | |
Pages = {81}, | |
Volume = {780}, | |
Abstract = {Simulations of hot, pressure-supported, tilted black hole | |
accretion flows, in which the angular momentum of the flow | |
is misaligned with the black hole spin axis, can exhibit | |
two nonaxisymmetric shock structures in the inner regions | |
of the flow. We analyze the strength and significance of | |
these shock structures in simulations with tilt angles of | |
10$\,^{\circ}$ and 15$\,^{\circ}$. By integrating fluid | |
trajectories in the simulations through the shocks and | |
tracking the variations of fluid quantities along these | |
trajectories, we show that these shocks are strong, with | |
substantial compression ratios, in contrast to earlier | |
claims. However, they are only moderately relativistic. We | |
also show that the two density enhancements resembling flow | |
streams in their shape are in fact merely post-shock | |
compressions, as fluid trajectories cut across, rather than | |
flow along, them. The dissipation associated with the | |
shocks is a substantial fraction (sime 3%-12%) of the rest | |
mass energy advected into the hole, and therefore | |
comparable to the dissipation expected from turbulence. The | |
shocks should therefore make order unity changes in the | |
observed properties of black hole accretion flows that are | |
tilted.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...780...81G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1311.5565}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/780/1/81}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1311.5565}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014ApJ...780...81G}, | |
Date-added = {2016-01-18 17:08:50 +0000}, | |
Date-modified = {2016-01-18 17:08:51 +0000}, | |
Doi = {10.1088/0004-637X/780/1/81}, | |
Eid = {81}, | |
Eprint = {1311.5565}, | |
Keywords = {accretion, accretion disks, black hole physics, | |
magnetohydrodynamics: MHD, shock waves, turbulence}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{generozov+2014, | |
Title = {{Lyman edges in supermassive black hole binaries}}, | |
Author = {{Generozov}, A. and {Haiman}, Z.}, | |
Journal = {\mnras}, | |
Year = {2014}, | |
Month = sep, | |
Pages = {L64-L68}, | |
Volume = {443}, | |
Abstract = {We propose a new spectral signature for supermassive black | |
hole binaries (SMBHBs) with circumbinary gas discs: a sharp | |
drop in flux bluewards of the Lyman limit. A prominent edge | |
is produced if the gas dominating the emission in the Lyman | |
continuum region of the spectrum is sufficiently cold (T | |
≲ 20 000 K) to contain significant neutral hydrogen. | |
Circumbinary discs may be in this regime if the binary | |
torques open a central cavity in the disc and clear most of | |
the hot gas from the inner region, and if any residual UV | |
emission from the individual BHs is either dim or | |
intermittent. We model the vertical structure and spectra | |
of circumbinary discs using the radiative transfer code | |
TLUSTY, and identify the range of BH masses and binary | |
separations producing a Lyman edge. We find that compact | |
supermassive (M ≳ 108 M&sun;) binaries with orbital | |
periods of ˜0.1-10 yr, whose gravitational waves are | |
expected to be detectable by pulsar timing arrays, could | |
have prominent Lyman edges. Such strong spectral edge | |
features are not typically present in AGN spectra and could | |
serve as corroborating evidence for the presence of an | |
SMBHB.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014MNRAS.443L..64G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1403.0002}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1093/mnrasl/slu075}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1403.0002}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014MNRAS.443L..64G}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1093/mnrasl/slu075}, | |
Eprint = {1403.0002}, | |
Keywords = {accretion, accretion discs, black hole physics, galaxies: | |
active}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{generozov+2017, | |
Title = {{The influence of circumnuclear environment on the radio | |
emission from TDE jets}}, | |
Author = {{Generozov}, A. and {Mimica}, P. and {Metzger}, B.~D. and | |
{Stone}, N.~C. and {Giannios}, D. and {Aloy}, M.~A.}, | |
Journal = {\mnras}, | |
Year = {2017}, | |
Month = jan, | |
Pages = {2481-2498}, | |
Volume = {464}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017MNRAS.464.2481G}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1093/mnras/stw2439}, | |
Eprint = {1605.08437}, | |
Keywords = {black hole physics}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2017.10.13} | |
} | |
@Article{generozov+2015, | |
Title = {{Circumnuclear media of quiescent supermassive black | |
holes}}, | |
Author = {{Generozov}, A. and {Stone}, N.~C. and {Metzger}, B.~D.}, | |
Journal = {\mnras}, | |
Year = {2015}, | |
Month = oct, | |
Pages = {775-796}, | |
Volume = {453}, | |
Abstract = {We calculate steady-state, one-dimensional hydrodynamic | |
profiles of hot gas in slowly accreting (`quiescent') | |
galactic nuclei for a range of central black hole masses | |
M*, parametrized gas heating rates, and observationally | |
motivated stellar density profiles. Mass is supplied to the | |
circumnuclear medium by stellar winds, while energy is | |
injected primarily by stellar winds, supernovae, and black | |
hole feedback. Analytic estimates are derived for the | |
stagnation radius (where the radial velocity of the gas | |
passes through zero) and the large-scale gas inflow rate, | |
dot{M}, as a function of M* and the gas heating efficiency, | |
the latter being related to the star formation history. We | |
assess the conditions under which radiative instabilities | |
develop in the hydrostatic region near the stagnation | |
radius, both in the case of a single burst of star | |
formation and for the average star formation history | |
predicted by cosmological simulations. By combining a | |
sample of measured nuclear X-ray luminosities, LX, of | |
nearby quiescent galactic nuclei with our results for | |
dot{M}(M_{bullet }), we address whether the nuclei are | |
consistent with accreting in a steady state, thermally | |
stable manner for radiative efficiencies predicted for | |
radiatively inefficiency accretion flows. We find thermally | |
stable accretion cannot explain the short average growth | |
times of low-mass black holes in the local Universe, which | |
must instead result from gas being fed in from large radii, | |
due either to gas inflows or thermal instabilities acting | |
on larger, galactic scales. Our results have implications | |
for attempts to constrain the occupation fraction of | |
upermassive black holes in low-mass galaxies using the mean | |
LX-M* correlation, as well as the predicted diversity of | |
the circumnuclear densities encountered by relativistic | |
outflows from tidal disruption events.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015MNRAS.453..775G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1505.00268}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stv1607}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1505.00268}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2015MNRAS.453..775G}, | |
Date-added = {2015-10-07 18:46:06 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1093/mnras/stv1607}, | |
Eprint = {1505.00268}, | |
Keywords = {black hole physics, galaxies: active}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{generozov+2018, | |
Title = {{An overabundance of black hole X-ray binaries in the Galactic Centre from tidal captures}}, | |
Author = {{Generozov}, A. and {Stone}, N.~C. and {Metzger}, B.~D. and {Ostriker}, J.~P.}, | |
Journal = {\mnras}, | |
Year = {2018}, | |
Month = aug, | |
Pages = {4030-4051}, | |
Volume = {478}, | |
Abstract = {A large population of X-ray binaries (XRBs) was recently discovered within the central parsec of the Galaxy by Hailey et al. While the presence of compact objects on this scale due to radial mass segregation is, in itself, unsurprising, the fraction of binaries would naively be expected to be small because of how easily primordial binaries are dissociated in the dynamically hot environment of the nuclear star cluster (NSC). We propose that the formation of XRBs in the central parsec is dominated by the tidal capture of stars by black holes (BHs) and neutron stars (NSs). We model the time-dependent radial density profiles of stars and compact objects in the NSC with a Fokker-Planck approach, using the present-day stellar population and rate of in situ massive star (and thus compact object) formation as observational constraints. Of the ?1-4 × 104 BHs that accumulate in the central parsec over the age of the Galaxy, we predict that ?60-200 currently exist as BH-XRBs formed from tidal capture, consistent with the population seen by Hailey et al. A somewhat lower number of tidal capture NS-XRBs is also predicted. We also use our observationally calibrated models for the NSC to predict rates of other exotic dynamical processes, such as the tidal disruption of stars by the central supermassive BH (?10-4 per year at z = 0).}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2018MNRAS.478.4030G}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1093/mnras/sty1262}, | |
Eprint = {1804.01543}, | |
Keywords = {black holes physics, X-rays: binaries}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2018.10.10} | |
} | |
@Article{genzel+1997, | |
Title = {{On the nature of the dark mass in the centre of the Milky Way}}, | |
Author = {{Genzel}, R. and {Eckart}, A. and {Ott}, T. and {Eisenhauer}, F.}, | |
Journal = {\mnras}, | |
Year = {1997}, | |
Month = oct, | |
Pages = {219-234}, | |
Volume = {291}, | |
Abstract = {We discuss constraints on the properties and nature of the dark mass concentration at the core of the Milky Way. We present 0.15-arcsec astrometric K-band maps in five epochs beween 1992 and 1996. From these we derive imposed stellar proper motions within 3 arcsec of the compact radio source SgrA* whose infrared counterpart may have been detected, for the first time, in a deep image in 1996 June. We also report lambda/Deltalambda~35 speckle spectroscopy and show that several of the SgrA* (infrared) cluster members are likely early-type stars of mass ~15 to 20 Msolar. All available checks, including a first comparison with high-resolution maps that are now becoming available from other groups, support our previous conclusion that there are several fast-moving stars (>=10^3 km s^-1) in the immediate vicinity (0.01 pc) of SgrA*. From the stellar radial and proper motion data, we infer that a dark mass of 2.61 (+/-0.15_stat)(+/-0.35_stat+sys)x10^6 Msolar must reside within about one light-week of the compact radio source. Its density must be 2.2x10^12 Msolar pc^-3 or greater. There is no stable configuration of normal stars, stellar remnants or substellar entities at that density. From an equipartition argument we infer that at least 5 per cent of the dark mass (>=10^5 Msolar) is associated with the compact radio source SgrA* itself and is concentrated on a scale of less than 15 times the Schwarzschild radius of a 2.6x10^6-Msolar black hole. The corresponding density is 3x10^20 Msolar pc^-3 or greater. If one accepts these arguments it is hard to escape the conclusion that there must be a massive black hole at the core of the Milky Way.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1997MNRAS.291..219G}, | |
Doi = {10.1093/mnras/291.1.219}, | |
Keywords = {BLACK HOLE PHYSICS, ASTROMETRY, CELESTIAL MECHANICS, STELLAR DYNAMICS, GALAXY: CENTRE, INFRARED: GENERAL}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.27} | |
} | |
@Article{genzel+03, | |
Title = {{The Stellar Cusp around the Supermassive Black Hole in | |
the Galactic Center}}, | |
Author = {{Genzel}, R. and {Sch{\"o}del}, R. and {Ott}, T. and | |
{Eisenhauer}, F. and {Hofmann}, R. and {Lehnert}, M. and | |
{Eckart}, A. and {Alexander}, T. and {Sternberg}, A. and | |
{Lenzen}, R. and {Cl{\'e}net}, Y. and {Lacombe}, F. and | |
{Rouan}, D. and {Renzini}, A. and {Tacconi-Garman}, L.~E.}, | |
Journal = {\apj}, | |
Year = {2003}, | |
Month = sep, | |
Pages = {812-832}, | |
Volume = {594}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2003ApJ...594..812G}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/377127}, | |
Doi = {10.1086/377127}, | |
Eprint = {astro-ph/0305423}, | |
Keywords = {Black Hole Physics, Galaxies: Nuclei, Galaxy: Center, | |
Stars: Formation} | |
} | |
@Article{genzel+2003, | |
Title = {{The Stellar Cusp around the Supermassive Black Hole in | |
the Galactic Center}}, | |
Author = {{Genzel}, R. and {Sch{\"o}del}, R. and {Ott}, T. and | |
{Eisenhauer}, F. and {Hofmann}, R. and {Lehnert}, M. and | |
{Eckart}, A. and {Alexander}, T. and {Sternberg}, A. and | |
{Lenzen}, R. and {Cl{\'e}net}, Y. and {Lacombe}, F. and | |
{Rouan}, D. and {Renzini}, A. and {Tacconi-Garman}, L.~E.}, | |
Journal = {\apj}, | |
Year = {2003}, | |
Month = sep, | |
Pages = {812-832}, | |
Volume = {594}, | |
Abstract = {We analyze deep near-IR adaptive optics imaging (taken | |
with NAOS/CONICA on the Very Large Telescope at the | |
European Southern Observatory, Chile), as well as new | |
proper-motion data of the nuclear star cluster of the Milky | |
Way. The surface density distribution of faint (H<=20, | |
Ks<=19) stars peaks within 0.2" of the black hole candidate | |
Sgr A*. The radial density distribution of this stellar | |
``cusp'' follows a power law of exponent alpha~1.3-1.4. The | |
K-band luminosity function of the overall nuclear stellar | |
cluster (within 9'' of Sgr A*) resembles that of the | |
large-scale Galactic bulge but shows an excess of stars at | |
Ks<=14. It fits population synthesis models of an old, | |
metal-rich stellar population with a contribution from | |
young, early, and late-type stars at the bright end. In | |
contrast, the cusp within <=1.5" of Sgr A* appears to have | |
a featureless luminosity function, suggesting that old, | |
low-mass, horizontal-branch/red-clump stars are lacking. | |
Likewise, there appear to be fewer late-type giants. The | |
innermost cusp also contains a group of moderately bright, | |
early-type stars that are tightly bound to the black hole. | |
We interpret these results as evidence that the stellar | |
properties change significantly from the outer cluster (>=a | |
few arcseconds) to the dense innermost region around the | |
black hole. We find that most of the massive early-type | |
stars at distances of 1"-10" from Sgr A* are located in two | |
rotating and geometrically thin disks. These disks are | |
inclined at large angles and counterrotate with respect to | |
each other. Their stellar content is essentially the same, | |
indicating that they formed at the same time. We conclude | |
that of the possible formation scenarios for these massive | |
stars the most probable one is that 5-8 million years ago | |
two clouds fell into the center, collided, were shock | |
compressed, and then formed two rotating (accretion) disks | |
orbiting the central black hole. For the OB stars in the | |
central arcsecond, on the other hand, a stellar merger | |
model is the most appealing explanation. These stars may | |
thus be ``super-blue stragglers,'' formed and | |
``rejuvenated'' through mergers of lower mass stars in the | |
very dense (>=108 Msolar pc-3) environment of the cusp. The | |
``collider model'' also accounts for the lack of giants | |
within the central few arcseconds. The star closest to Sgr | |
A* in 2002, S2, exhibits a 3.8 mum excess. We propose that | |
the mid-IR emission comes either from the accretion flow | |
around the black hole itself or from dust in the accretion | |
flow that is heated by the ultraviolet emission of S2.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2003ApJ...594..812G}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/0305423}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1086/377127}, | |
Bdsk-url-2 = {http://arxiv.org/abs/astro-ph/0305423}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2003ApJ...594..812G}, | |
Date-added = {2016-04-08 22:00:20 +0000}, | |
Date-modified = {2016-04-08 22:00:21 +0000}, | |
Doi = {10.1086/377127}, | |
Eprint = {astro-ph/0305423}, | |
Keywords = {Black Hole Physics, Galaxies: Nuclei, Galaxy: Center, | |
Stars: Formation} | |
} | |
@Article{genzel+1996, | |
Title = {{The Dark Mass Concentration in the Central Parsec of the | |
Milky Way}}, | |
Author = {{Genzel}, R. and {Thatte}, N. and {Krabbe}, A. and | |
{Kroker}, H. and {Tacconi-Garman}, L.~E.}, | |
Journal = {\apj}, | |
Year = {1996}, | |
Month = nov, | |
Pages = {153}, | |
Volume = {472}, | |
Abstract = {We report ˜1" resolution K-band (2 mum) imaging | |
spectroscopy of the central parsec of our Galaxy. The | |
derived radial velocities for 223 early- and late-type | |
stars probe the nuclear mass distribution to spatial scales | |
of 0.1 pc. We find a statistically very significant | |
increase of projected stellar velocity dispersion from | |
about 55 km s-1 at p ˜5 pc to 180 km s-1 at p ˜0.1 pc. | |
The stars are also rotating about the dynamic center. The | |
late-type stars follow general Galactic rotation, while the | |
early-type stars show counter-rotation. Fitting | |
simultaneously the observed projected surface densities and | |
velocity dispersions, we derive the intrinsic volume | |
densities and radial velocity dispersions as a function of | |
distance from the dynamic center for both types of stars. | |
We then derive the mass distribution between 0.1 and 5 pc | |
from the Jeans equation assuming an isotropic velocity | |
field. Our analysis requires a compact central dark mass of | |
2.5-3.2 x 106 Msun, at 6-8 sigma significance. The dark | |
mass has a density of 109 Msun pc-3 or greater and a mass | |
to 2 mum luminosity of >= 100. The increase in | |
mass-to-luminosity ratio can be reduced but not eliminated | |
even if extreme anisotropic velocity distributions are | |
considered. The dark mass cannot be a cluster of solar mass | |
remnants (such as neutron stars). It is either a compact | |
cluster of 10-20 Msun black holes or a single massive black | |
hole.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1996ApJ...472..153G}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1086/178051}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1996ApJ...472..153G}, | |
Date-added = {2017-04-25 22:06:57 +0000}, | |
Date-modified = {2017-04-25 22:06:57 +0000}, | |
Doi = {10.1086/178051}, | |
Keywords = {CELESTIAL MECHANICS, STELLAR DYNAMICS, GALAXY: CENTER, | |
INFRARED: STARS, TECHNIQUES: RADIAL VELOCITIES} | |
} | |
@Article{georgiev&boker2014, | |
Title = {{Nuclear star clusters in 228 spiral galaxies in the | |
HST/WFPC2 archive: catalogue and comparison to other | |
stellar systems}}, | |
Author = {{Georgiev}, I.~Y. and {B{\"o}ker}, T.}, | |
Journal = {\mnras}, | |
Year = {2014}, | |
Month = jul, | |
Pages = {3570-3590}, | |
Volume = {441}, | |
Abstract = {We present a catalogue of photometric and structural | |
properties of 228 nuclear star clusters (NSCs) in nearby | |
late-type disc galaxies. These new measurements are derived | |
from a homogeneous analysis of all suitable Wide Field | |
Planetary Camera 2 (WFPC2) images in the Hubble Space | |
Telescope (HST) archive. The luminosity and size of each | |
NSC are derived from an iterative point spread function | |
(PSF) fitting technique, which adapts the fitting area to | |
the effective radius (reff) of the NSC and uses a | |
WFPC2-specific PSF model tailored to the position of each | |
NSC on the detector. The luminosities of NSCs are <=108 LV, | |
&sun;, and their integrated optical colours suggest a wide | |
spread in age. We confirm that most NSCs have sizes similar | |
to globular clusters (GCs), but find that the largest and | |
brightest NSCs occupy the regime between ultra-compact | |
dwarf (UCD) and the nuclei of early-type galaxies in the | |
size-luminosity plane. The overlap in size, mass, and | |
colour between the different incarnations of compact | |
stellar systems provides a support for the notion that at | |
least some UCDs and the most massive Galactic GCs may be | |
remnant nuclei of disrupted disc galaxies. We find | |
tentative evidence for the NSCs' reff to be smaller when | |
measured in bluer filters and discuss possible implications | |
of this result. We also highlight a few examples of complex | |
nuclear morphologies, including double nuclei, extended | |
stellar structures, and nuclear F606W excess from either | |
recent (circum-)nuclear star formation and/or a weak active | |
galactic nucleus. Such examples may serve as case studies | |
for ongoing NSC evolution via the two main suggested | |
mechanisms, namely cluster merging and in situ star | |
formation.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014MNRAS.441.3570G}, | |
Annote = {Useful for nuclear star cluster sizes}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1404.5956}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stu797}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1404.5956}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014MNRAS.441.3570G}, | |
Date-added = {2015-12-02 18:04:32 +0000}, | |
Date-modified = {2015-12-07 02:47:37 +0000}, | |
Doi = {10.1093/mnras/stu797}, | |
Eprint = {1404.5956}, | |
Keywords = {galaxies: spiral, galaxies: star clusters: general} | |
} | |
@Article{georgiev+2014, | |
Title = {{Nuclear star clusters in 228 spiral galaxies in the | |
HST/WFPC2 archive: catalogue and comparison to other | |
stellar systems}}, | |
Author = {{Georgiev}, I.~Y. and {B{\"o}ker}, T.}, | |
Journal = {\mnras}, | |
Year = {2014}, | |
Month = jul, | |
Pages = {3570-3590}, | |
Volume = {441}, | |
Abstract = {We present a catalogue of photometric and structural | |
properties of 228 nuclear star clusters (NSCs) in nearby | |
late-type disc galaxies. These new measurements are derived | |
from a homogeneous analysis of all suitable Wide Field | |
Planetary Camera 2 (WFPC2) images in the Hubble Space | |
Telescope (HST) archive. The luminosity and size of each | |
NSC are derived from an iterative point spread function | |
(PSF) fitting technique, which adapts the fitting area to | |
the effective radius (reff) of the NSC and uses a | |
WFPC2-specific PSF model tailored to the position of each | |
NSC on the detector. The luminosities of NSCs are <=108 LV, | |
&sun;, and their integrated optical colours suggest a wide | |
spread in age. We confirm that most NSCs have sizes similar | |
to globular clusters (GCs), but find that the largest and | |
brightest NSCs occupy the regime between ultra-compact | |
dwarf (UCD) and the nuclei of early-type galaxies in the | |
size-luminosity plane. The overlap in size, mass, and | |
colour between the different incarnations of compact | |
stellar systems provides a support for the notion that at | |
least some UCDs and the most massive Galactic GCs may be | |
remnant nuclei of disrupted disc galaxies. We find | |
tentative evidence for the NSCs' reff to be smaller when | |
measured in bluer filters and discuss possible implications | |
of this result. We also highlight a few examples of complex | |
nuclear morphologies, including double nuclei, extended | |
stellar structures, and nuclear F606W excess from either | |
recent (circum-)nuclear star formation and/or a weak active | |
galactic nucleus. Such examples may serve as case studies | |
for ongoing NSC evolution via the two main suggested | |
mechanisms, namely cluster merging and in situ star | |
formation.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014MNRAS.441.3570G}, | |
Annote = {Useful for nuclear star cluster sizes}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1404.5956}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stu797}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1404.5956}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014MNRAS.441.3570G}, | |
Date-added = {2015-12-02 18:04:32 +0000}, | |
Date-modified = {2015-12-07 02:47:37 +0000}, | |
Doi = {10.1093/mnras/stu797}, | |
Eprint = {1404.5956}, | |
Keywords = {galaxies: spiral, galaxies: star clusters: general} | |
} | |
@Article{gergely+2012, | |
Title = {{The typical mass ratio and typical final spin in | |
supermassive black hole mergers}}, | |
Author = {Gergely, L.\~{}\'{A}. and Biermann, P.\~{}L.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2012}, | |
Month = aug, | |
Archiveprefix = {arXiv}, | |
Arxivid = {gr-qc/1208.5251}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {1208.5251}, | |
Keywords = {Astrophysics - Galaxy Astrophysics,General Relativity and | |
Quantum Cosmology; Untitled; Untitled1}, | |
Primaryclass = {gr-qc} | |
} | |
@Article{gezari+2008, | |
Title = {{UV/Optical Detections of Candidate Tidal Disruption | |
Events by GALEX and CFHTLS}}, | |
Author = {{Gezari}, S. and {Basa}, S. and {Martin}, D.~C. and | |
{Bazin}, G. and {Forster}, K. and {Milliard}, B. and | |
{Halpern}, J.~P. and {Friedman}, P.~G. and {Morrissey}, P. | |
and {Neff}, S.~G. and {Schiminovich}, D. and {Seibert}, M. | |
and {Small}, T. and {Wyder}, T.~K.}, | |
Journal = {\apj}, | |
Year = {2008}, | |
Month = apr, | |
Pages = {944-969}, | |
Volume = {676}, | |
Abstract = {We present two luminous UV/optical flares from the nuclei | |
of apparently inactive early-type galaxies at z = 0.37 and | |
0.33 that have the radiative properties of a flare from the | |
tidal disruption of a star. In this paper we report the | |
second candidate tidal disruption event discovery in the UV | |
by the GALEX Deep Imaging Survey and present simultaneous | |
optical light curves from the CFHTLS Deep Imaging Survey | |
for both UV flares. The first few months of the UV/optical | |
light curves are well fitted with the canonical t-5/3 | |
power-law decay predicted for emission from the fallback of | |
debris from a tidally disrupted star. Chandra ACIS X-ray | |
observations during the flares detect soft X-ray sources | |
with Tbb = (2--5) × 105 K or Gamma > 3 and place limits on | |
hard X-ray emission from an underlying AGN down to LX(2--10 | |
keV) lesssim 1041 ergs s-1. Blackbody fits to the | |
UV/optical spectral energy distributions of the flares | |
indicate peak flare luminosities of gtrsim1044-1045 ergs | |
s-1. The temperature, luminosity, and light curves of both | |
flares are in excellent agreement with emission from a | |
tidally disrupted main-sequence star onto a central black | |
hole of several times 107 M☉. The observed detection rate | |
of our search over ~2.9 deg2 of GALEX Deep Imaging Survey | |
data spanning from 2003 to 2007 is consistent with tidal | |
disruption rates calculated from dynamical models, and we | |
use these models to make predictions for the detection | |
rates of the next generation of optical synoptic surveys. | |
Some of the data presented herein were obtained at the W. | |
M. Keck Observatory, which is operated as a scientific | |
partnership among the California Institute of Technology, | |
the University of California, and the National Aeronautics | |
and Space Administration. The Observatory was made possible | |
by the generous financial support of the W. M. Keck | |
Foundation.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2008ApJ...676..944G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/0712.4149}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1086/529008}, | |
Bdsk-url-2 = {http://arxiv.org/abs/0712.4149}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2008ApJ...676..944G}, | |
Date-added = {2016-03-17 17:09:56 +0000}, | |
Date-modified = {2016-03-17 17:09:56 +0000}, | |
Doi = {10.1086/529008}, | |
Eid = {944-969}, | |
Eprint = {0712.4149}, | |
Keywords = {galaxies: nuclei, ultraviolet: galaxies, X-rays: | |
galaxies} | |
} | |
@Article{gezari+2012, | |
Title = {{An ultraviolet-optical flare from the tidal disruption of | |
a helium-rich stellar core}}, | |
Author = {{Gezari}, S. and {Chornock}, R. and {Rest}, A. and | |
{Huber}, M.~E. and {Forster}, K. and {Berger}, E. and | |
{Challis}, P.~J. and {Neill}, J.~D. and others}, | |
Journal = {\nat}, | |
Year = {2012}, | |
Month = may, | |
Pages = {217-220}, | |
Volume = {485}, | |
Abstract = {The flare of radiation from the tidal disruption and | |
accretion of a star can be used as a marker for | |
supermassive black holes that otherwise lie dormant and | |
undetected in the centres of distant galaxies. Previous | |
candidate flares have had declining light curves in good | |
agreement with expectations, but with poor constraints on | |
the time of disruption and the type of star disrupted, | |
because the rising emission was not observed. Recently, two | |
`relativistic' candidate tidal disruption events were | |
discovered, each of whose extreme X-ray luminosity and | |
synchrotron radio emission were interpreted as the onset of | |
emission from a relativistic jet. Here we report a luminous | |
ultraviolet-optical flare from the nuclear region of an | |
inactive galaxy at a redshift of 0.1696. The observed | |
continuum is cooler than expected for a simple accreting | |
debris disk, but the well-sampled rise and decay of the | |
light curve follow the predicted mass accretion rate and | |
can be modelled to determine the time of disruption to an | |
accuracy of two days. The black hole has a mass of about | |
two million solar masses, modulo a factor dependent on the | |
mass and radius of the star disrupted. On the basis of the | |
spectroscopic signature of ionized helium from the unbound | |
debris, we determine that the disrupted star was a | |
helium-rich stellar core.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2012Natur.485..217G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1205.0252}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1038/nature10990}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1205.0252}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2012Natur.485..217G}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1038/nature10990}, | |
Eprint = {1205.0252}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{gezari+2009, | |
Title = {{Luminous Thermal Flares from Quiescent Supermassive Black | |
Holes}}, | |
Author = {{Gezari}, S. and {Heckman}, T. and {Cenko}, S.~B. and | |
{Eracleous}, M. and {Forster}, K. and {Gon{\c c}alves}, | |
T.~S. and {Martin}, D.~C. and {Morrissey}, P. and {Neff}, | |
S.~G. and {Seibert}, M. and {Schiminovich}, D. and {Wyder}, | |
T.~K.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = jun, | |
Pages = {1367-1379}, | |
Volume = {698}, | |
Abstract = {A dormant supermassive black hole lurking in the center of | |
a galaxy will be revealed when a star passes close enough | |
to be torn apart by tidal forces, and a flare of | |
electromagnetic radiation is emitted when the bound | |
fraction of the stellar debris falls back onto the black | |
hole and is accreted. Although the tidal disruption of a | |
star is a rare event in a galaxy, ≈10-4 yr-1, | |
observational candidates have emerged in all-sky X-ray and | |
deep ultraviolet (UV) surveys in the form of luminous | |
UV/X-ray flares from otherwise quiescent galaxies. Here we | |
present the third candidate tidal disruption event | |
discovered in the Galaxy Evolution Explorer (GALEX) Deep | |
Imaging Survey: a 1.6 × 1043 erg s-1 UV/optical flare from | |
a star-forming galaxy at z = 0.1855. The UV/optical | |
spectral energy distribution (SED) during the peak of the | |
flare measured by GALEX and Palomar Large Field Camera | |
imaging can be modeled as a single temperature blackbody | |
with T bb = 1.7 × 105 K and a bolometric luminosity of 3 | |
× 1045 erg s-1, assuming an internal extinction with E(B - | |
V)gas = 0.3. The Chandra upper limit on the X-ray | |
luminosity during the peak of the flare, LX (2 - 10 | |
keV)<1041 erg s-1, is 2 orders of magnitude fainter than | |
expected from the ratios of UV to X-ray flux density | |
observed in active galaxies. We compare the light curves | |
and broadband properties of all three tidal disruption | |
candidates discovered by GALEX, and find that (1) the light | |
curves are well fitted by the power-law decline expected | |
for the fallback of debris from a tidally disrupted | |
solar-type star and (2) the UV/optical SEDs can be | |
attributed to thermal emission from an envelope of debris | |
located at roughly 10 times the tidal disruption radius of | |
a ≈107 M sun central black hole. We use the observed peak | |
absolute optical magnitudes of the flares (-17.5>Mg > - | |
18.9) to predict the detection capabilities of upcoming | |
optical synoptic surveys.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...698.1367G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/0904.1596}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/698/2/1367}, | |
Bdsk-url-2 = {http://arxiv.org/abs/0904.1596}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2009ApJ...698.1367G}, | |
Date-added = {2016-03-17 16:56:47 +0000}, | |
Date-modified = {2016-03-17 16:56:47 +0000}, | |
Doi = {10.1088/0004-637X/698/2/1367}, | |
Eprint = {0904.1596}, | |
Keywords = {black hole physics, galaxies: nuclei, ultraviolet: ISM, | |
X-rays: galaxies}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{gezari+2006, | |
Title = {{Ultraviolet Detection of the Tidal Disruption of a Star | |
by a Supermassive Black Hole}}, | |
Author = {{Gezari}, S. and {Martin}, D.~C. and {Milliard}, B. and | |
{Basa}, S. and {Halpern}, J.~P. and {Forster}, K. and | |
{Friedman}, P.~G. and {Morrissey}, P. and {Neff}, S.~G. and | |
{Schiminovich}, D. and {Seibert}, M. and {Small}, T. and | |
{Wyder}, T.~K.}, | |
Journal = {\apjl}, | |
Year = {2006}, | |
Month = dec, | |
Pages = {L25-L28}, | |
Volume = {653}, | |
Abstract = {A supermassive black hole in the nucleus of a galaxy will | |
be revealed when a star passes close enough to be torn | |
apart by tidal forces and a flare of radiation is emitted | |
by the stream of stellar debris that plunges into the black | |
hole. Since common active galactic nuclei have accreting | |
black holes that can also produce flares, a convincing | |
demonstration that a stellar tidal disruption has occurred | |
generally begins with a ``normal'' galaxy that has no | |
evidence of prior nuclear activity. Here we report a | |
luminous UV flare from an elliptical galaxy at z=0.37 in | |
the Groth field of the GALEX Deep Imaging Survey that has | |
no evidence of a Seyfert nucleus from optical spectroscopy | |
and X-ray imaging obtained during the flare. | |
Multiwavelength data collected at the time of the event, | |
and for 2 years following, allow us to constrain, for the | |
first time, the spectral energy distribution of a candidate | |
tidal disruption flare from optical through X-rays. The | |
luminosity and temperature of the radiation and the decay | |
curve of the flare are in excellent agreement with | |
theoretical predictions for the tidal disruption of a star, | |
and provide the strongest empirical evidence for a stellar | |
disruption event to date.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006ApJ...653L..25G}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/0612069}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/509918}, | |
Bdsk-url-2 = {http://arxiv.org/abs/astro-ph/0612069}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2006ApJ...653L..25G}, | |
Date-added = {2016-03-17 17:07:53 +0000}, | |
Date-modified = {2016-03-17 17:07:54 +0000}, | |
Doi = {10.1086/509918}, | |
Eprint = {astro-ph/0612069}, | |
Keywords = {Galaxies: Nuclei, Ultraviolet: Galaxies} | |
} | |
@Article{ghez+2003, | |
Title = {{The First Measurement of Spectral Lines in a Short-Period Star Bound to the Galaxy's Central Black Hole: A Paradox of Youth}}, | |
Author = {{Ghez}, A.~M. and {Duch{\^e}ne}, G. and {Matthews}, K. and {Hornstein}, S.~D. and {Tanner}, A. and {Larkin}, J. and {Morris}, M. and {Becklin}, E.~E. and {Salim}, S. and {Kremenek}, T. and {Thompson}, D. and {Soifer}, B.~T. and {Neugebauer}, G. and {McLean}, I.}, | |
Journal = {\apjl}, | |
Year = {2003}, | |
Month = apr, | |
Pages = {L127-L131}, | |
Volume = {586}, | |
Abstract = {We have obtained the first detection of spectral absorption lines in one of the high-velocity stars in the vicinity of the Galaxy's central supermassive black hole. Both Br? (2.1661 ?m) and He I (2.1126 ?m) are seen in absorption in S0-2 with equivalent widths (2.8+/-0.3 and 1.7+/-0.4 Å) and an inferred stellar rotational velocity (220+/-40 km s-1) that are consistent with that of an O8-B0 dwarf, which suggests that it is a massive (~15 Msolar) young (less than 10 Myr) main-sequence star. This presents a major challenge to star formation theories, given the strong tidal forces that prevail over all distances reached by S0-2 in its current orbit (130-1900 AU) and the difficulty in migrating this star inward during its lifetime from farther out where tidal forces should no longer preclude star formation. The radial velocity measurements (z>=-510+/-40 km s-1) and our reported proper motions for S0-2 strongly constrain its orbit, providing a direct measure of the black hole mass of 4.1(+/-0.6)×106(R0/8 kpc)3 Msolar. The Keplerian orbit parameters have uncertainties that are reduced by a factor of 2-3 compared to previously reported values and include, for the first time, an independent solution for the dynamical center; this location, while consistent with the nominal infrared position of Sgr A*, is localized to a factor of 5 more precisely (+/-2 mas). Furthermore, the ambiguity in the inclination of the orbit is resolved with the addition of the radial velocity measurement, indicating that the star is behind the black hole at the time of closest approach and counterrevolving against the Galaxy. With further radial velocity measurements in the next few years, the orbit of S0-2 will provide the most robust estimate of the distance to the Galactic center.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2003ApJ...586L.127G}, | |
Doi = {10.1086/374804}, | |
Eprint = {astro-ph/0302299}, | |
Keywords = {Black Hole Physics, Galaxy: Center, Galaxy: Kinematics and Dynamics, Infrared: Stars, Techniques: High Anular Resolution, Techniques: Spectroscopic}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.27} | |
} | |
@Article{ghez+1998, | |
Title = {{High Proper-Motion Stars in the Vicinity of Sagittarius A*: Evidence for a Supermassive Black Hole at the Center of Our Galaxy}}, | |
Author = {{Ghez}, A.~M. and {Klein}, B.~L. and {Morris}, M. and {Becklin}, E.~E. }, | |
Journal = {\apj}, | |
Year = {1998}, | |
Month = dec, | |
Pages = {678-686}, | |
Volume = {509}, | |
Abstract = {Over a 2 year period we have conducted a diffraction-limited imaging study at 2.2 ?m of the inner 6" × 6" of the central stellar cluster of the Galaxy using the W. M. Keck 10 m telescope. The K-band images obtained in 1995 June, 1996 June, and 1997 May have the highest angular resolution obtained at near-infrared wavelengths from ground or space (?res = 0.05" = 0.002 pc) and reveal a large population of faint stars. We use an unbiased approach for identifying and selecting stars to be included in this proper-motion study, which results in a sample of 90 stars with brightness ranging from K = 9-17 mag and two-dimensional velocities as large as 1400 +/- 100 km s-1. Compared to earlier work (Eckart et al. 1997; Genzel et al. 1997), the source confusion is reduced by a factor of 9, the number of stars with proper-motion measurement in the central 25 arcsec2 of our Galaxy is doubled, and the accuracy of the velocity measurements in the central 1 arcsec2 is improved by a factor of 4. The peaks of both the stellar surface density and the velocity dispersion are consistent with the position of the unusual radio source and black hole candidate Sgr A*, which suggests that Sgr A* is coincident (+/-0.1") with the dynamical center of the Galaxy. As a function of distance from Sgr A*, the velocity dispersion displays a falloff well-fitted by Keplerian motion (?v ~ r-0.5+/-0.1) about a central dark mass of 2.6 +/- 0.2 × 106 M? confined to a volume of at most 10-6 pc3, which is consistent with earlier results. Although uncertainties in the measurements mathematically allow for the matter to be distributed over this volume as a cluster, no realistic cluster is physically tenable. Thus, independent of the presence of Sgr A*, the large inferred central density of at least 1012 M? pc-3, which exceeds the volume-averaged mass densities found at the center of any other galaxy, leads us to the conclusion that our Galaxy harbors a massive central black hole.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1998ApJ...509..678G}, | |
Doi = {10.1086/306528}, | |
Eprint = {astro-ph/9807210}, | |
Keywords = {BLACK HOLE PHYSICS, GALAXY: CENTER, GALAXY: KINEMATICS AND DYNAMICS, INFRARED: STARS, STARS: KINEMATICS, TECHNIQUES: IMAGE PROCESSING, Black Hole Physics, Galaxy: Center, Galaxy: Kinematics and Dynamics, Infrared: Stars, Stars: Kinematics, Techniques: Image Processing}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.27} | |
} | |
@Article{ghez+2000, | |
Title = {{The accelerations of stars orbiting the Milky Way's central black hole}}, | |
Author = {{Ghez}, A.~M. and {Morris}, M. and {Becklin}, E.~E. and {Tanner}, A. and {Kremenek}, T.}, | |
Journal = {\nat}, | |
Year = {2000}, | |
Month = sep, | |
Pages = {349-351}, | |
Volume = {407}, | |
Abstract = {Recent measurements of the velocities of stars near the centre of the Milky Way have provided the strongest evidence for the presence of a supermassive black hole in a galaxy, but the observational uncertainties poorly constrain many of the black hole's properties. Determining the accelerations of stars in their orbits around the centre provides much more precise information about the position and mass of the black hole. Here we report measurements of the accelerations of three stars located ~0.005pc (projected on the sky) from the central radio source Sagittarius A* (Sgr A*); these accelerations are comparable to those experienced by the Earth as it orbits the Sun. These data increase the inferred minimum mass density in the central region of the Galaxy by an order of magnitude relative to previous results, and localize the dark mass to within 0.05 +/- 0.04arcsec of the nominal position of Sgr A*. In addition, the orbital period of one of the observed stars could be as short as 15 years, allowing us the opportunity in the near future to observe an entire period.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2000Natur.407..349G}, | |
Doi = {10.1038/35030032}, | |
Eprint = {astro-ph/0009339}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.27} | |
} | |
@Article{giannios&metzger2011, | |
Title = {{Radio transients from stellar tidal disruption by massive | |
black holes}}, | |
Author = {{Giannios}, D. and {Metzger}, B.~D.}, | |
Journal = {\mnras}, | |
Year = {2011}, | |
Month = sep, | |
Pages = {2102-2107}, | |
Volume = {416}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011MNRAS.416.2102G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2011.19188.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-12-07 03:09:15 +0000}, | |
Doi = {10.1111/j.1365-2966.2011.19188.x}, | |
Eprint = {1102.1429}, | |
Keywords = {black hole physics, galaxies: nuclei}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{gibson+2008, | |
Title = {{Are Optically Selected Quasars Universally X-Ray | |
Luminous? X-Ray-UV Relations in Sloan Digital Sky Survey | |
Quasars}}, | |
Author = {{Gibson}, R.~R. and {Brandt}, W.~N. and {Schneider}, | |
D.~P.}, | |
Journal = {\apj}, | |
Year = {2008}, | |
Month = oct, | |
Pages = {773-786}, | |
Volume = {685}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2008ApJ...685..773G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/590403}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/590403}, | |
Eprint = {0808.2603}, | |
Keywords = {Galaxies: Active, Galaxies: Nuclei, Galaxies: Quasars: | |
Absorption Lines, Galaxies: Quasars: Emission Lines, | |
X-Rays: General} | |
} | |
@Article{giocoli+2010, | |
Title = {{The substructure hierarchy in dark matter haloes}}, | |
Author = {{Giocoli}, C. and {Tormen}, G. and {Sheth}, R.~K. and {van | |
den Bosch}, F.~C.}, | |
Journal = {\mnras}, | |
Year = {2010}, | |
Month = may, | |
Pages = {502-517}, | |
Volume = {404}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010MNRAS.404..502G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2010.16311.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1365-2966.2010.16311.x}, | |
Eprint = {0911.0436}, | |
Keywords = {galaxies: haloes, galaxies: interactions, cosmology: | |
theory, dark matter}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{gnedin+2014, | |
Title = {{Co-evolution of Galactic Nuclei and Globular Cluster | |
Systems}}, | |
Author = {{Gnedin}, O.~Y. and {Ostriker}, J.~P. and {Tremaine}, S.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = apr, | |
Pages = {71}, | |
Volume = {785}, | |
Abstract = {We revisit the hypothesis that dense galactic nuclei are | |
formed from inspiraling globular clusters. Recent advances | |
in the understanding of the continuous formation of | |
globular clusters over cosmic time and the concurrent | |
evolution of the galaxy stellar distribution allow us to | |
construct a simple model that matches the observed spatial | |
and mass distributions of clusters in the Galaxy and the | |
giant elliptical galaxy M87. In order to compare with | |
observations, we model the effects of dynamical friction | |
and dynamical evolution, including stellar mass loss, tidal | |
stripping of stars, and tidal disruption of clusters by the | |
growing galactic nucleus. We find that inspiraling globular | |
clusters form a dense central structure, with mass and | |
radius comparable to the typical values in observed nuclear | |
star clusters (NSCs) in late-type and low-mass early-type | |
galaxies. The density contrast associated with the NSC is | |
less pronounced in giant elliptical galaxies. Our results | |
indicate that the NSC mass as a fraction of mass of the | |
galaxy stellar spheroid scales as M_{NSC}/{M_{*}}≈ 0.0025 | |
{M_{*}}_{,11}^{-0.5}. Thus disrupted globular clusters | |
could contribute most of the mass of NSCs in galaxies with | |
stellar mass below 1011 M &sun;. The inner part of the | |
accumulated cluster may seed the growth of a central black | |
hole via stellar dynamical core collapse, thereby relieving | |
the problem of how to form luminous quasars at high | |
redshift. The seed black hole may reach ~105 M &sun; within | |
<~ 1 Gyr of the beginning of globular cluster formation.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...785...71G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1308.0021}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/785/1/71}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1308.0021}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014ApJ...785...71G}, | |
Date-added = {2017-04-24 01:41:25 +0000}, | |
Date-modified = {2017-04-24 01:41:26 +0000}, | |
Doi = {10.1088/0004-637X/785/1/71}, | |
Eid = {71}, | |
Eprint = {1308.0021}, | |
Keywords = {galaxies: evolution, galaxies: formation, galaxies: | |
nuclei, galaxies: star clusters: general, globular | |
clusters: general} | |
} | |
@Article{gold+2013, | |
Title = {{Accretion disks around binary black holes of unequal | |
mass: GRMHD simulations near decoupling}}, | |
Author = {{Gold}, R. and {Paschalidis}, V. and {Etienne}, Z.~B. and | |
{Shapiro}, S.~L. and {Pfeiffer}, H.~P.}, | |
Journal = {Physical Review, submitted; e-print arXiv:1312.0600}, | |
Year = {2013}, | |
Month = dec, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2013arXiv1312.0600G}, | |
Archiveprefix = {arXiv}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {1312.0600}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena, | |
Astrophysics - Cosmology and Extragalactic Astrophysics, | |
General Relativity and Quantum Cosmology; Untitled; | |
Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{goldreich+2002, | |
Title = {{Formation of Kuiper-belt binaries by dynamical friction and three-body encounters}}, | |
Author = {{Goldreich}, P. and {Lithwick}, Y. and {Sari}, R.}, | |
Journal = {\nat}, | |
Year = {2002}, | |
Month = dec, | |
Pages = {643-646}, | |
Volume = {420}, | |
Abstract = {The Kuiper belt is a disk of icy bodies that orbit the Sun beyond Neptune; the largest known members are Pluto and its companion Charon. A few per cent of Kuiper-belt bodies have recently been found to be binaries with wide separations and mass ratios of the order of unity. Collisions were too infrequent to account for the observed number of binaries, implying that these binaries formed through collisionless interactions mediated by gravity. These interactions are likely to have been most effective during the period of runaway accretion, early in the Solar System's history. Here we show that a transient binary forms when two large bodies penetrate one another's Hill sphere (the region where their mutual forces are larger than the tidal force of the Sun). The loss of energy needed to stabilize the binary orbit can then occur either through dynamical friction from surrounding small bodies, or through the gravitational scattering of a third large body. Our estimates slightly favour the former mechanism. We predict that five per cent of Kuiper-belt objects are binaries with apparent separations greater than 0.2arcsec, and that most are in tighter binaries or systems of higher multiplicity.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2002Natur.420..643G}, | |
Doi = {10.1038/nature01227}, | |
Eprint = {astro-ph/0208490}, | |
Owner = {aleksey}, | |
Timestamp = {2018.10.11} | |
} | |
@Article{goldreich&nicholson1989, | |
Title = {{Tidal friction in early-type stars}}, | |
Author = {{Goldreich}, P. and {Nicholson}, P.~D.}, | |
Journal = {\apj}, | |
Year = {1989}, | |
Month = jul, | |
Pages = {1079-1084}, | |
Volume = {342}, | |
Abstract = {Theoretical and observational results related to tides in early-type stars are summarized. The results suggest that the tidal torque on an early-type star is concentrated near the boundary between the convective core and the radiative envelope, and that a train of gravity waves which is excited at this boundary outwardly transports the angular momentum removed from the fluid by the torque. Tidal despinning to synchronous rotation is shown to proceed from the outside to the inside of the star. The present model can account for the previous finding that Zahn's (1975, 1977) theory for tidal evolution in early-type close binaries is compatible with the observed rates of orbit circularization, while significantly underestimating the observed rates of spin synchronization.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1989ApJ...342.1079G}, | |
Doi = {10.1086/167665}, | |
Keywords = {Binary Stars, Computational Astrophysics, Early Stars, Stellar Motions, Tides, Angular Momentum, Gravitational Waves, Perturbation Theory, Stellar Envelopes, Stellar Rotation, Torque}, | |
Owner = {aleksey}, | |
Timestamp = {2019.02.02} | |
} | |
@Article{goldreich+1980a, | |
Title = {{Disk-satellite interactions}}, | |
Author = {{Goldreich}, P. and {Tremaine}, S.}, | |
Journal = {\apj}, | |
Year = {1980}, | |
Month = oct, | |
Pages = {425-441}, | |
Volume = {241}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1980ApJ...241..425G}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/158356}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:06:12 +0000}, | |
Doi = {10.1086/158356}, | |
Keywords = {JUPITER (PLANET), MOMENTUM TRANSFER, NATURAL SATELLITES, | |
PLANETARY EVOLUTION, PROTOPLANETS, ANGULAR MOMENTUM, | |
CELESTIAL MECHANICS, RESONANCE, SOLAR SYSTEM; Untitled; | |
Untitled1} | |
} | |
@Article{goldreich+1979, | |
Title = {{The excitation of density waves at the Lindblad and | |
corotation resonances by an external potential}}, | |
Author = {Goldreich, P and Tremaine, S}, | |
Journal = {Astrophysical Journal}, | |
Year = {1979}, | |
Month = nov, | |
Pages = {857}, | |
Volume = {233}, | |
Abstract = {The linear response of a differentially rotating | |
two-dimensional gas disk, both with and without | |
self-gravity, to a rigidly rotating external potential is | |
calculated on the assumptions that the speed of sound is | |
much smaller that the orbital velocity and that the | |
external potential varies on the scale of the disk radius. | |
The results show that: (1) the external potential exerts | |
torques on the disk only at the Lindblad and corotation | |
resonances; (2) the torque is positive at the outer | |
Lindblad resonance and negative at the inner Lindblad | |
resonance; (3) the torque at corotation has the sign of the | |
radial vorticity gradient; and (4) the torques are of the | |
same order of magnitude at both types of resonance and | |
independent of the speed of sound in the disk. It is found | |
that the external potential also excites density waves in | |
the vicinity of the Lindblad and corotation resonances, | |
that the long trailing wave is excited at a Lindblad | |
resonance, and that short trailing waves are excited at the | |
corotation resonance. The behavior of particle disks is | |
briefly discussed, and the external torques on particle | |
disks are proven to be identical to those on gas disks}, | |
Annote = {A\{\&\}AA ID. AAA026.151.054}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=1979ApJ...233..857G%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1086/157448}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/157448}, | |
Keywords = {DENSITY WAVE MODEL, GALACTIC STRUCTURE, Hydrodynamics, | |
RESONANCE, ROTATING DISKS, STELLAR MOTIONS, WAVE | |
EXCITATION,ASTRODYNAMICS}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=1979ApJ...233..857G\&link\_type=ABSTRACT} | |
} | |
@Article{goodman2003, | |
Title = {{Self-gravity and quasi-stellar object discs}}, | |
Author = {Goodman, Jeremy}, | |
Journal = {Monthly Notice of the Royal Astronomical Society}, | |
Year = {2003}, | |
Month = mar, | |
Pages = {937}, | |
Volume = {339}, | |
Abstract = {The outer parts of standard steady-state accretion discs | |
around quasi-stellar objects (QSOs) are prone to | |
self-gravity, and they might be expected to fragment into | |
stars rather than feed the central black hole. Possible | |
solutions to this well-known problem are examined with an | |
emphasis on general dynamic constraints. Irradiation by the | |
QSO is insufficient for stability even if the outer disc is | |
strongly warped. Marginal local gravitational instability | |
enhances viscous transport but extends the stable regions | |
only modestly. Compton cooling in the observed QSO | |
radiation field rules out hot thick discs unless the local | |
accretion rate is vastly super-Eddington. The formation of | |
stars or stellar-mass black holes, and the release of | |
energy in these objects by fusion or accretion, may help to | |
stabilize the remaining gas in an otherwise standard disc. | |
But at fixed mass accretion rate, the energy inputs | |
required for stability increase with radius; beyond a | |
parsec, they approach the total QSO luminosity and are | |
probably unsustainable by stars. Magnetic torques from a | |
wind or corona, and gravitational torques from bars or | |
global spirals, may increase the accretion speed and reduce | |
the density of the disc. But dynamical arguments suggest | |
that the accretion speed is at most sonic, so that | |
instability still sets in beyond about a parsec. | |
Alternatively, the QSO could be fed by stellar collisions | |
in a very dense stellar cluster, but the velocity | |
dispersion would have to be much higher than observed in | |
nearby galactic nuclei containing quiescent black holes. In | |
view of these difficulties, we suggest that QSO discs do | |
not extend beyond a thousand Schwarzschild radii or so. | |
Then they must be frequently replenished with gas of small | |
specific angular momentum.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2003MNRAS.339..937G%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1046/j.1365-8711.2003.06241.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1046/j.1365-8711.2003.06241.x}, | |
Keywords = {Accretion, accretion discs, gravitation,quasars: general} | |
} | |
@Article{goodman&dickson1998, | |
Title = {{Dynamical Tide in Solar-Type Binaries}}, | |
Author = {{Goodman}, J. and {Dickson}, E.~S.}, | |
Journal = {\apj}, | |
Year = {1998}, | |
Month = nov, | |
Pages = {938-944}, | |
Volume = {507}, | |
Abstract = {Circularization of late-type main-sequence binaries is | |
usually attributed to turbulent convection, while that of | |
early-type binaries is explained by resonant excitation of | |
g-modes. We show that the latter mechanism also operates in | |
solar-type stars and is at least as effective as convection | |
despite inefficient damping of g-modes in the radiative | |
core. The maximum period at which this mechanism can | |
circularize a binary composed of solar-type stars in 1010 | |
yr is as low as 3 days, if the modes are damped by | |
radiative diffusion only and g-mode resonances are fixed, | |
or as high as 6 days if one allows for evolution of the | |
resonances and for nonlinear damping near inner turning | |
points. Even the larger theoretical period falls short of | |
the observed transition period by a factor of 2.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1998ApJ...507..938G}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/9801289}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/306348}, | |
Bdsk-url-2 = {http://arxiv.org/abs/astro-ph/9801289}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/1998ApJ...507..938G}, | |
Date-added = {2017-06-10 02:14:02 +0000}, | |
Date-modified = {2017-06-10 02:14:55 +0000}, | |
Doi = {10.1086/306348}, | |
Eprint = {astro-ph/9801289}, | |
Keywords = {STARS: BINARIES: CLOSE, STARS: BINARIES: SPECTROSCOPIC, | |
STARS: INTERIORS, STARS: OSCILLATIONS, Stars: Binaries: | |
Close, Stars: Binaries: Spectroscopic, Stars: Interiors, | |
Stars: Oscillations} | |
} | |
@Article{goodman&tan2004, | |
Title = {{Supermassive Stars in Quasar Disks}}, | |
Author = {{Goodman}, J. and {Tan}, J.~C.}, | |
Journal = {\apj}, | |
Year = {2004}, | |
Month = jun, | |
Pages = {108-118}, | |
Volume = {608}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2004ApJ...608..108G}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/386360}, | |
Date-added = {2017-06-24 01:02:18 +0000}, | |
Date-modified = {2017-06-24 01:02:30 +0000}, | |
Doi = {10.1086/386360}, | |
Eprint = {astro-ph/0307361}, | |
Keywords = {Accretion, Accretion Disks, Gravitation, Galaxies: | |
Quasars: General, Stars: Formation} | |
} | |
@Article{governato+2009, | |
Title = {{Forming a large disc galaxy from a z {\lt} 1 major | |
merger}}, | |
Author = {{Governato}, F. and {Brook}, C.~B. and {Brooks}, A.~M. and | |
{Mayer}, L. and {Willman}, B. and {Jonsson}, P. and | |
{Stilp}, A.~M. and {Pope}, L. and {Christensen}, C. and | |
{Wadsley}, J. and {Quinn}, T.}, | |
Journal = {\mnras}, | |
Year = {2009}, | |
Month = sep, | |
Pages = {312-320}, | |
Volume = {398}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009MNRAS.398..312G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2009.15143.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1365-2966.2009.15143.x}, | |
Eprint = {0812.0379}, | |
Keywords = {methods: N-Body simulations , galaxies: evolution , | |
galaxies: formation , galaxies: interactions} | |
} | |
@Article{graham+2009, | |
Title = {{Quantifying the coexistence of massive black holes and | |
dense nuclear star clusters}}, | |
Author = {{Graham}, A.~W. and {Spitler}, L.~R.}, | |
Journal = {\mnras}, | |
Year = {2009}, | |
Month = aug, | |
Pages = {2148-2162}, | |
Volume = {397}, | |
Abstract = {In large spheroidal stellar systems, such as elliptical | |
galaxies, one invariably finds a 106-109Msolar supermassive | |
black hole at their centre. In contrast, within dwarf | |
elliptical galaxies one predominantly observes a | |
105-107Msolar nuclear star cluster. To date, few galaxies | |
have been found with both types of nuclei coexisting and | |
even less have had the masses determined for both central | |
components. Here, we identify one dozen galaxies housing | |
nuclear star clusters and supermassive black holes whose | |
masses have been measured. This doubles the known number of | |
such hermaphrodite nuclei - which are expected to be | |
fruitful sources of gravitational radiation. Over the host | |
spheroid (stellar) mass range 108-1011Msolar, we find that | |
a galaxy's nucleus-to-spheroid (baryon) mass ratio is not a | |
constant value but decreases from a few per cent to ~0.3 | |
per cent such that log[(MBH + MNC)/Msph] = -(0.39 +/- 0.07) | |
log[Msph/1010Msolar] - (2.18 +/- 0.07). Once dry merging | |
commences and the nuclear star clusters disappear, this | |
ratio is expected to become a constant value. As a | |
byproduct of our investigation, we have found that the | |
projected flux from resolved nuclear star clusters is well | |
approximated with S{\'e}rsic functions having a range of | |
indices from ~0.5 to ~3, the latter index describing the | |
Milky Way's nuclear star cluster.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009MNRAS.397.2148G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/0907.5250}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2009.15118.x}, | |
Bdsk-url-2 = {http://arXiv.org/abs/0907.5250}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2009MNRAS.397.2148G}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1365-2966.2009.15118.x}, | |
Eprint = {0907.5250}, | |
Keywords = {black hole physics , galaxies: nuclei , galaxies: | |
structure}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@InProceedings{granot2007, | |
Title = {{The Structure and Dynamics of GRB Jets}}, | |
Author = {{Granot}, J.}, | |
Booktitle = {Revista Mexicana de Astronomia y Astrofisica, vol. 27}, | |
Year = {2007}, | |
Month = mar, | |
Pages = {140-165}, | |
Series = {Revista Mexicana de Astronomia y Astrofisica, vol.~27}, | |
Volume = {27}, | |
Abstract = {There are several lines of evidence which suggest that the relativistic outflows in gamma-ray bursts (GRBs) are collimated into narrow jets. The jet structure has important implications for the true energy release and the event rate of GRBs, and can constrain the mechanism responsible for the acceleration and collimation of the jet. Nevertheless, the jet structure and its dynamics as it sweeps up the external medium and decelerates, are not well understood. In this review I discuss our current understanding of GRB jets, stressing their structure and dynamics.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007RMxAC..27..140G}, | |
Eprint = {astro-ph/0610379}, | |
Keywords = {gamma rays: bursts, hydrodynamics, ISM: Jets and outflows, relativity}, | |
Owner = {aleksey}, | |
Timestamp = {2018.04.04} | |
} | |
@Article{granot&sari2002, | |
Title = {{The Shape of Spectral Breaks in Gamma-Ray Burst Afterglows}}, | |
Author = {{Granot}, J. and {Sari}, R.}, | |
Journal = {\apj}, | |
Year = {2002}, | |
Month = apr, | |
Pages = {820-829}, | |
Volume = {568}, | |
Abstract = {Gamma-ray burst afterglows are well described by synchrotron emission from relativistic blast waves expanding into an external medium. The blast wave is believed to amplify the magnetic field and accelerate the electrons into a power-law distribution of energies promptly behind the shock. These electrons then cool both adiabatically and by emitting synchrotron and inverse Compton radiation. The resulting spectra are known to consist of several power-law segments, which smoothly join at certain break frequencies. Here, we give a complete description of all possible spectra under those assumptions and find that there are five possible regimes, depending on the ordering of the break frequencies. The flux density is calculated by integrating over all of the contributions to a given photon arrival time from all of the shocked region using the Blandford & McKee solution. This allows us to calculate more accurate expressions for the value of these break frequencies and describe the shape of the spectral breaks around them. This also provides the shape of breaks in the light curves caused by the passage of a break frequency through the observed band. These new, more exact, estimates are different from more simple calculations by typically a factor of a few, and they describe some new regimes that were previously ignored.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2002ApJ...568..820G}, | |
Doi = {10.1086/338966}, | |
Eprint = {astro-ph/0108027}, | |
Keywords = {Gamma Rays: Bursts, Gamma Rays: Theory, Radiation Mechanisms: Nonthermal, Shock Waves}, | |
Owner = {aleksey}, | |
Timestamp = {2018.04.04} | |
} | |
@Article{granot+02, | |
Title = {{The Shape of Spectral Breaks in Gamma-Ray Burst | |
Afterglows}}, | |
Author = {{Granot}, J. and {Sari}, R.}, | |
Journal = {\apj}, | |
Year = {2002}, | |
Month = apr, | |
Pages = {820-829}, | |
Volume = {568}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2002ApJ...568..820G}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/338966}, | |
Doi = {10.1086/338966}, | |
Eprint = {astro-ph/0108027}, | |
Keywords = {Gamma Rays: Bursts, Gamma Rays: Theory, Radiation | |
Mechanisms: Nonthermal, Shock Waves} | |
} | |
@Article{graur+2015, | |
Title = {{A unified explanation for the supernova rate-galaxy mass | |
dependence based on supernovae detected in Sloan galaxy | |
spectra}}, | |
Author = {{Graur}, O. and {Bianco}, F.~B. and {Modjaz}, M.}, | |
Journal = {\mnras}, | |
Year = {2015}, | |
Month = jun, | |
Pages = {905-925}, | |
Volume = {450}, | |
Abstract = {Using a method to discover and classify supernovae (SNe) | |
in galaxy spectra, we detect 91 Type Ia SNe (SNe Ia) and 16 | |
Type II SNe (SNe II) among ˜740 000 galaxies of all types | |
and ˜215 000 star-forming galaxies without active galactic | |
nuclei, respectively, in Data Release 9 of the Sloan | |
Digital Sky Survey. Of these SNe, 15 SNe Ia and eight SNe | |
II are new discoveries reported here for the first time. We | |
use our SN samples to measure SN rates per unit mass as a | |
function of galaxy stellar mass, star-formation rate (SFR), | |
and specific SFR (sSFR), as derived by the MPA-JHU Galspec | |
pipeline. We show that correlations between SN Ia and SN II | |
rates per unit mass and galaxy stellar mass, SFR, and sSFR | |
can be explained by a combination of the respective SN | |
delay-time distributions (the distributions of times that | |
elapse between the formation of a stellar population and | |
all ensuing SNe), the ages of the surveyed galaxies, the | |
redshifts at which they are observed, and their star | |
formation histories. This model was first suggested by | |
Kistler et al. for the SN Ia rate-mass correlation, but is | |
expanded here to SNe II and to correlations with galaxy SFR | |
and sSFR. Finally, we measure a volumetric SN II rate at | |
redshift 0.075 of RII, V = 0.621^{+0.197}_{-0.154} (stat) | |
^{+0.024}_{-0.063} (sys) × 10^{-4} yr-1 Mpc-3. Assuming | |
that SNe IIP and IIL account for 60 per cent of all | |
core-collapse (CC) SNe, the CC SN rate is RCC, V = | |
1.04^{+0.33}_{-0.26} (stat) ^{+0.04}_{-0.11} (sys) × | |
10^{-4} yr-1 Mpc-3.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015MNRAS.450..905G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1412.7991}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stv713}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1412.7991}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2015MNRAS.450..905G}, | |
Date-added = {2015-11-06 22:02:42 +0000}, | |
Date-modified = {2015-11-06 22:02:43 +0000}, | |
Doi = {10.1093/mnras/stv713}, | |
Eprint = {1412.7991}, | |
Keywords = {methods: observational, surveys, supernovae: general}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{graur+2018, | |
Title = {{A Dependence of the Tidal Disruption Event Rate on Global Stellar Surface Mass Density and Stellar Velocity Dispersion}}, | |
Author = {{Graur}, O. and {French}, K.~D. and {Zahid}, H.~J. and {Guillochon}, J. and {Mandel}, K.~S. and {Auchettl}, K. and {Zabludoff}, A.~I.}, | |
Journal = {\apj}, | |
Year = {2018}, | |
Month = jan, | |
Pages = {39}, | |
Volume = {853}, | |
Abstract = {The rate of tidal disruption events (TDEs), {R}{TDE}, is predicted to depend on stellar conditions near the super-massive black hole (SMBH), which are on difficult-to-measure sub-parsec scales. We test whether {R}{TDE} depends on kpc-scale global galaxy properties, which are observable. We concentrate on stellar surface mass density, {{{? }}}{M\star }, and velocity dispersion, {? }v, which correlate with the stellar density and velocity dispersion of the stars around the SMBH. We consider 35 TDE candidates, with and without known X-ray emission. The hosts range from star-forming to quiescent to quiescent with strong Balmer absorption lines. The last (often with post-starburst spectra) are overrepresented in our sample by a factor of {35}-17+21 or {18}-7+8, depending on the strength of the H? absorption line. For a subsample of hosts with homogeneous measurements, {{{? }}}{M\star }={10}9-{10}10 {M}? /{{{kpc}}}2, higher on average than for a volume-weighted control sample of Sloan Digital Sky Survey galaxies with similar redshifts and stellar masses. This is because (1) most of the TDE hosts here are quiescent galaxies, which tend to have higher {{{? }}}{M\star } than the star-forming galaxies that dominate the control, and (2) the star-forming hosts have higher average {{{? }}}{M\star } than the star-forming control. There is also a weak suggestion that TDE hosts have lower {? }v than for the quiescent control. Assuming that {R}{TDE}\propto {{{? }}}{M\star }? × {? }v? , and applying a statistical model to the TDE hosts and control sample, we estimate \hat{? }=0.9+/- 0.2 and \hat{? }=-1.0+/- 0.6. This is broadly consistent with {R}{TDE} being tied to the dynamical relaxation of stars surrounding the SMBH.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2018ApJ...853...39G}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/1538-4357/aaa3fd}, | |
Eid = {39}, | |
Eprint = {1707.02986}, | |
Keywords = {black hole physics, galaxies: evolution, galaxies: nuclei}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2018.10.03} | |
} | |
@Article{greene&ho2007, | |
Title = {{The Mass Function of Active Black Holes in the Local Universe}}, | |
Author = {{Greene}, J.~E. and {Ho}, L.~C.}, | |
Journal = {\apj}, | |
Year = {2007}, | |
Month = sep, | |
Pages = {131-148}, | |
Volume = {667}, | |
Abstract = {We present the first measurement of the BH mass function for broad-line active galaxies in the local universe. Using the ~8500 broad-line active galaxies from SDSS DR4, we construct a broad-line luminosity function that agrees very well with the local soft X-ray luminosity function. Using standard virial relations, we then convert observed broad-line luminosities and widths into BH masses. A mass function constructed in this way has the unique capability to probe the mass region <106 Msolar, which, while insignificant in terms of total BH mass density, nevertheless may place important constraints on the mass distribution of seed BHs in the early universe. The characteristic local active BH has a mass of ~107 Msolar radiating at 10% of the Eddington rate. The active fraction is a strong function of BH mass; at both higher and lower masses the active mass function falls more steeply than one would infer from the distribution of bulge luminosity. The deficit of local massive radiating BHs is a well-known phenomenon, while we present the first robust measurement of a decline in the space density of active BHs at low mass.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...667..131G}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1086/520497}, | |
Eprint = {0705.0020}, | |
Keywords = {Galaxies: Active, Galaxies: Nuclei, Galaxies: Seyfert}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.07} | |
} | |
@Article{greene+2007, | |
Title = {{A New Sample of Low-Mass Black Holes in Active | |
Galaxies}}, | |
Author = {{Greene}, J.~E. and {Ho}, L.~C.}, | |
Journal = {\apj}, | |
Year = {2007}, | |
Month = nov, | |
Pages = {92-104}, | |
Volume = {670}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...670...92G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/522082}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1086/522082}, | |
Eprint = {0707.2617}, | |
Keywords = {Galaxies: Active, Galaxies: Nuclei, Galaxies: Seyfert} | |
} | |
@Article{greene+2010, | |
Title = {{Precise Black Hole Masses from Megamaser Disks: Black | |
Hole-Bulge Relations at Low Mass}}, | |
Author = {{Greene}, J.~E. and {Peng}, C.~Y. and {Kim}, M. and {Kuo}, | |
C.-Y. and {Braatz}, J.~A. and {Impellizzeri}, C.~M.~V. and | |
{Condon}, J.~J. and {Lo}, K.~Y. and {Henkel}, C. and | |
{Reid}, M.~J.}, | |
Journal = {\apj}, | |
Year = {2010}, | |
Month = sep, | |
Pages = {26-45}, | |
Volume = {721}, | |
Abstract = {The black hole (BH)-bulge correlations have greatly | |
influenced the last decade of efforts to understand galaxy | |
evolution. Current knowledge of these correlations is | |
limited predominantly to high BH masses (M BHgsim108 M sun) | |
that can be measured using direct stellar, gas, and maser | |
kinematics. These objects, however, do not represent the | |
demographics of more typical L < L* galaxies. This study | |
transcends prior limitations to probe BHs that are an order | |
of magnitude lower in mass, using BH mass measurements | |
derived from the dynamics of H2O megamasers in | |
circumnuclear disks. The masers trace the Keplerian | |
rotation of circumnuclear molecular disks starting at radii | |
of a few tenths of a pc from the central BH. Modeling of | |
the rotation curves, presented by Kuo et al., yields BH | |
masses with exquisite precision. We present stellar | |
velocity dispersion measurements for a sample of nine | |
megamaser disk galaxies based on long-slit observations | |
using the B&C spectrograph on the Dupont telescope and the | |
Dual Imaging Spectrograph on the 3.5 m telescope at Apache | |
Point. We also perform bulge-to-disk decomposition of a | |
subset of five of these galaxies with Sloan Digital Sky | |
Survey imaging. The maser galaxies as a group fall below | |
the M BH-sigma* relation defined by elliptical galaxies. We | |
show, now with very precise BH mass measurements, that the | |
low-scatter power-law relation between M BH and sigma* seen | |
in elliptical galaxies is not universal. The elliptical | |
galaxy M BH-sigma* relation cannot be used to derive the BH | |
mass function at low mass or the zero point for active BH | |
masses. The processes (perhaps BH self-regulation or minor | |
merging) that operate at higher mass have not effectively | |
established an M BH-sigma* relation in this low-mass | |
regime.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010ApJ...721...26G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1007.2851}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/721/1/26}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1007.2851}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2010ApJ...721...26G}, | |
Date-added = {2016-05-25 19:55:05 +0000}, | |
Date-modified = {2016-05-25 19:55:05 +0000}, | |
Doi = {10.1088/0004-637X/721/1/26}, | |
Eprint = {1007.2851}, | |
Keywords = {galaxies: active, galaxies: bulges, galaxies: nuclei, | |
galaxies: Seyfert}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{greiner+2015, | |
Title = {{A very luminous magnetar-powered supernova associated with an ultra-long {$\gamma$}-ray burst}}, | |
Author = {{Greiner}, J. and {Mazzali}, P.~A. and {Kann}, D.~A. and {Kr{\"u}hler}, T. and {Pian}, E. and {Prentice}, S. and {Olivares E.}, F. and {Rossi}, A. and {Klose}, S. and {Taubenberger}, S. and {Knust}, F. and {Afonso}, P.~M.~J. and {Ashall}, C. and {Bolmer}, J. and {Delvaux}, C. and {Diehl}, R. and {Elliott}, J. and {Filgas}, R. and {Fynbo}, J.~P.~U. and {Graham}, J.~F. and {Guelbenzu}, A.~N. and {Kobayashi}, S. and {Leloudas}, G. and {Savaglio}, S. and {Schady}, P. and {Schmidl}, S. and {Schweyer}, T. and {Sudilovsky}, V. and {Tanga}, M. and {Updike}, A.~C. and {van Eerten}, H. and {Varela}, K.}, | |
Journal = {\nat}, | |
Year = {2015}, | |
Month = jul, | |
Pages = {189-192}, | |
Volume = {523}, | |
Abstract = {A new class of ultra-long-duration (more than 10,000 seconds) ?-ray bursts has recently been suggested. They may originate in the explosion of stars with much larger radii than those producing normal long-duration ?-ray bursts or in the tidal disruption of a star. No clear supernova has yet been associated with an ultra-long-duration ?-ray burst. Here we report that a supernova (SN 2011kl) was associated with the ultra-long-duration ?-ray burst GRB 111209A, at a redshift z of 0.677. This supernova is more than three times more luminous than type Ic supernovae associated with long-duration ?-ray bursts, and its spectrum is distinctly different. The slope of the continuum resembles those of super-luminous supernovae, but extends further down into the rest-frame ultraviolet implying a low metal content. The light curve evolves much more rapidly than those of super-luminous supernovae. This combination of high luminosity and low metal-line opacity cannot be reconciled with typical type Ic supernovae, but can be reproduced by a model where extra energy is injected by a strongly magnetized neutron star (a magnetar), which has also been proposed as the explanation for super-luminous supernovae.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015Natur.523..189G}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1038/nature14579}, | |
Eprint = {1509.03279}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2018.04.12} | |
} | |
@Article{greiner+2000, | |
Title = {{RX J1420.4+5334 - another tidal disruption event?}}, | |
Author = {{Greiner}, J. and {Schwarz}, R. and {Zharikov}, S. and | |
{Orio}, M.}, | |
Journal = {\aap}, | |
Year = {2000}, | |
Month = oct, | |
Pages = {L25-L28}, | |
Volume = {362}, | |
Abstract = {We have discovered a transient X-ray source, RX | |
J1420.4+5334, which displays a ROSAT flux variation of >≈ | |
150 between the ROSAT All-Sky-Survey in 1990 and a | |
preceding pointed ROSAT observations in July 1990. Optical | |
observations suggest a non-active galaxy as the only | |
visible counterpart. We therefore tentatively identify RX | |
J1420.4+5334 as a tidal disruption event in a non-active | |
galaxy. Partly based on observations collected at the | |
German-Spanish Astronomical Centre, Calar Alto, operated by | |
the MPI f{\"u}r Astronomie, Heidelberg, jointly with the | |
Spanish National Commission for Astronomy, and the WIYN | |
telescope, operated the the University of Wisconsin, | |
Indiana University, Yale University, and the National | |
Optical Astronomy Observatories.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2000A%26A...362L..25G}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/0009430}, | |
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Bdsk-url-1 = {http://arxiv.org/abs/astro-ph/0009430}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/2000A%26A...362L..25G}, | |
Date-added = {2016-03-17 17:21:13 +0000}, | |
Date-modified = {2016-03-17 17:21:14 +0000}, | |
Eprint = {astro-ph/0009430}, | |
Keywords = {ACCRETION, ACCRETION DISKS, GALAXIES: ACTIVE, GALAXIES: | |
INDIVIDUAL:, GALAXIES: NUCLEI, X-RAYS: GALAXIES} | |
} | |
@Article{greisen1966, | |
Title = {{End to the Cosmic-Ray Spectrum?}}, | |
Author = {{Greisen}, K.}, | |
Journal = {Physical Review Letters}, | |
Year = {1966}, | |
Month = apr, | |
Pages = {748-750}, | |
Volume = {16}, | |
Abstract = {Not Available}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1966PhRvL..16..748G}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1103/PhysRevLett.16.748}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1966PhRvL..16..748G}, | |
Date-added = {2016-01-06 18:29:55 +0000}, | |
Date-modified = {2016-01-06 18:29:55 +0000}, | |
Doi = {10.1103/PhysRevLett.16.748} | |
} | |
@Article{groot+1997, | |
Title = {{GRB 970228}}, | |
Author = {{Groot}, P.~J. and {Galama}, T.~J. and {van Paradijs}, J. and {Strom}, R. and {Telting}, J. and {Rutten}, R.~G.~M. and {Pettini}, M. and {Tanvir}, N. and {Naber}, R. and {Kouveliotou}, C. and {in 't Zand}, J. and {Heise}, J. and {Costa}, E. and {Feroci}, M. and {Piro}, L. and {Frontera}, F. and {Zavattini}, G. and {Nicastro}, L. and {Palazzi}, E. }, | |
Journal = {\iaucirc}, | |
Year = {1997}, | |
Month = mar, | |
Volume = {6584}, | |
Abstract = {IAUC 6584 available at Central Bureau for Astronomical Telegrams.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1997IAUC.6584....1G}, | |
Owner = {aleksey}, | |
Timestamp = {2018.04.02} | |
} | |
@Article{grupe+1999, | |
Title = {{RX J1624.9+7554: a new X-ray transient AGN}}, | |
Author = {{Grupe}, D. and {Thomas}, H.-C. and {Leighly}, K.~M.}, | |
Journal = {\aap}, | |
Year = {1999}, | |
Month = oct, | |
Pages = {L31-L34}, | |
Volume = {350}, | |
Abstract = {We report the discovery of a new X-ray transient AGN, RX | |
J1624.9+7554. This object appeared to be bright in the | |
ROSAT All-Sky Survey, but had turned off in two pointed | |
observations about one and a half years later. The optical | |
identification spectrum shows a non-emission line spectrum | |
of a spiral galaxy at z=0.064. We will discuss several | |
hypotheses that can explain the peculiar behaviour of this | |
object.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1999A%26A...350L..31G}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/9909101}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://arxiv.org/abs/astro-ph/9909101}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1999A%26A...350L..31G}, | |
Date-added = {2016-03-17 16:38:59 +0000}, | |
Date-modified = {2016-03-17 16:39:00 +0000}, | |
Eprint = {astro-ph/9909101}, | |
Keywords = {ACCRETION, ACCRETION DISKS, GALAXIES: ACTIVE, GALAXIES: | |
NUCLEI, GALAXIES: INDIVIDUAL: RX J1624.9+7554} | |
} | |
@Article{gualandris&merritt2007, | |
Title = {{Dynamics around supermassive black holes}}, | |
Author = {{Gualandris}, A. and {Merritt}, D.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2007}, | |
Month = aug, | |
Abstract = {The dynamics of galactic nuclei reflects the presence of | |
supermassive black holes (SBHs) in many ways. Single SBHs | |
act as sinks, destroying a mass in stars equal to their own | |
mass in roughly one relaxation time and forcing nuclei to | |
expand. Formation of binary SBHs displaces a mass in stars | |
roughly equal to the binary mass, creating low-density | |
cores and ejecting hyper-velocity stars. Gravitational | |
radiation recoil can eject coalescing binary SBHs from | |
nuclei, resulting in offset SBHs and lopsided cores. We | |
review recent work on these mechanisms and discuss the | |
observable consequences.}, | |
Adscomment = {Invited talk. To appear in '2007 STScI Spring Symposium: | |
Black Holes', eds. M. Livio A. M. Koekemoer. (Cambridge | |
University Press, in press) 26 pages, 12 figures}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007arXiv0708.3083G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/0708.3083}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://arXiv.org/abs/0708.3083}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/2007arXiv0708.3083G}, | |
Date-added = {2016-01-25 21:15:48 +0000}, | |
Date-modified = {2016-01-25 21:18:37 +0000}, | |
Eprint = {0708.3083}, | |
Keywords = {Astrophysics} | |
} | |
@Article{guetta+2005, | |
Title = {{The Luminosity and Angular Distributions of Long-Duration | |
Gamma-Ray Bursts}}, | |
Author = {{Guetta}, D. and {Piran}, T. and {Waxman}, E.}, | |
Journal = {\apj}, | |
Year = {2005}, | |
Month = jan, | |
Pages = {412-419}, | |
Volume = {619}, | |
Abstract = {The realization that the total energy of gamma-ray bursts | |
(GRBs) is correlated with their jet break angles motivates | |
the search for a similar relation between the peak | |
luminosity L and the jet break angles, L~?-2. Such a | |
relation implies that the GRB luminosity function | |
determines the angular distribution. We rederive the GRB | |
luminosity function using the BATSE peak flux distribution | |
and compare the predicted distribution with the observed | |
redshift distribution. The luminosity function can be | |
approximated by a broken power law with a break peak | |
luminosity of 4.4?051 ergs s-1, a typical jet angle of 0.12 | |
rad, and a local GRB rate of 0.44h365 Gpc-3 yr-1. The | |
angular distribution implied by L~?-2 agrees well with the | |
observed one and implies a correction factor to the local | |
rate due to beaming of 75+/-25 (instead of 500, as commonly | |
used). The inferred overall local GRB rate is 33+/-11h365 | |
Gpc-3 yr-1. The luminosity function and angle distribution | |
obtained within the universal structured jet model, where | |
the angular distribution is essentially ~? and hence the | |
luminosity function must be ~L-2, deviate from the | |
observations at low peak fluxes and, correspondingly, at | |
large angles. The corresponding correction factor for the | |
universal structure jet is ~20+/-10.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005ApJ...619..412G}, | |
Doi = {10.1086/423125}, | |
Eprint = {astro-ph/0311488}, | |
Keywords = {Cosmology: Observations, Gamma Rays: Bursts}, | |
Owner = {aleksey}, | |
Timestamp = {2017.12.26} | |
} | |
@Article{guillochon+2014, | |
Title = {{PS1-10jh: The Disruption of a Main-sequence Star of | |
Near-solar Composition}}, | |
Author = {{Guillochon}, J. and {Manukian}, H. and {Ramirez-Ruiz}, | |
E.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = mar, | |
Pages = {23}, | |
Volume = {783}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...783...23G}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/783/1/23}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/783/1/23}, | |
Eid = {23}, | |
Eprint = {1304.6397}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: | |
active, gravitational lensing: weak, hydrodynamics, | |
methods: numerical}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{guillochon+2016, | |
Title = {{Unbound Debris Streams and Remnants Resulting from the Tidal Disruptions of Stars by Supermassive Black Holes}}, | |
Author = {{Guillochon}, J. and {McCourt}, M. and {Chen}, X. and {Johnson}, M.~D. and {Berger}, E.}, | |
Journal = {\apj}, | |
Year = {2016}, | |
Month = may, | |
Pages = {48}, | |
Volume = {822}, | |
Abstract = {The kinetic energy of a star in orbit about a supermassive black hole is a significant fraction of its rest mass energy when its periapse is comparable to its tidal radius. Upon its destruction, a fraction of this energy is extracted and injected into the stellar debris, half of which becomes unbound from the black hole, with the fastest material moving at ? 0.03c. In this paper, we present a formalism for determining the fate of these unbound debris streams (UDSs) as they depart from the black hole and interact with the surrounding gas. As the density and velocity varies along the length of a UDS, we find that hydrodynamical drag quickly shapes UDSs into loop-like structures, with the densest portions of the streams leading portions of lower density. As UDSs travel outwards, their drag against the ISM increases quadratically with distance, which causes UDSs to deposit their momentum and energy into the ambient medium before the surrounding shocked ISM has a chance to cool. This sudden injection of ? {10}50 erg into the ambient medium generates a Sedov-like unbound debris remnant (UDR) that mimics supernova remnants (SNRs) in energetics and appearance, accelerates particles which will produce cosmic rays and synchrotron emission, and provides momentum feedback into the molecular clouds surrounding a black hole. We estimate that a few of these UDRs might be present within a couple degrees of the Galactic Center masquerading as SNRs, and that the UDR scenario is a plausible explanation for Sgr A east.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016ApJ...822...48G}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/0004-637X/822/1/48}, | |
Eid = {48}, | |
Eprint = {1509.08916}, | |
Keywords = {black hole physics, gravitation, quasars: supermassive black holes}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2018.03.13} | |
} | |
@Article{guillochon+2015a, | |
Title = {{Unbound Debris Streams and Remnants Resulting From the | |
Tidal Disruptions of Stars by Supermassive Black Holes}}, | |
Author = {{Guillochon}, J. and {McCourt}, M. and {Chen}, X. and | |
{Johnson}, M.~D. and {Berger}, E.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2015}, | |
Month = sep, | |
Abstract = {The kinetic energy of a star in orbit about a supermassive | |
black hole is a significant fraction of its rest mass | |
energy when its periapse is comparable to its tidal radius. | |
Upon its destruction, a fraction of this energy is | |
extracted and injected into the stellar debris, half of | |
which becomes unbound from the black hole, with the fastest | |
material moving at $\sim 0.03 c$. In this paper, we present | |
a formalism for determining the fate of these unbound | |
debris streams (UDSs) as they depart from the black hole | |
and interact with the surrounding gas. As the density and | |
velocity varies along the length of a UDS, we find that | |
hydrodynamical drag quickly shapes UDSs into loop-like | |
structures, with the densest portions of the streams | |
leading portions of lower density. As UDSs travel outwards, | |
their drag against the ISM increases quadratically with | |
distance, which causes UDSs to deposit their momentum and | |
energy into the ambient medium before the surrounding | |
shocked ISM has a chance to cool. This sudden injection of | |
$\sim 10^{50}$ erg into the ambient medium generates a | |
Sedov-like unbound debris remnant (UDR) that mimics | |
supernova remnants (SNRs) in energetics and appearance, | |
accelerates particles which will produce cosmic rays and | |
synchrotron emission, and provides momentum feedback into | |
the molecular clouds surrounding a black hole. We estimate | |
that a few of these UDRs might be present within a couple | |
degrees of the Galactic Center masquerading as SNRs, and | |
that the UDR scenario is a plausible explanation for Sgr A | |
East.}, | |
Adscomment = {16 pages, 9 figures. Submitted to ApJ}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015arXiv150908916G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1509.08916}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://arXiv.org/abs/1509.08916}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/2015arXiv150908916G}, | |
Date-added = {2015-10-02 14:28:13 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {1509.08916}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena, | |
Astrophysics - Solar and Stellar Astrophysics; Untitled; | |
Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{guillochon+2015b, | |
Title = {{A Dark Year for Tidal Disruption Events}}, | |
Author = {{Guillochon}, J. and {Ramirez-Ruiz}, E.}, | |
Journal = {\apj}, | |
Year = {2015}, | |
Month = aug, | |
Pages = {166}, | |
Volume = {809}, | |
Abstract = {Main-sequence disruptions of stars by supermassive black | |
holes result in the production of an extended, | |
geometrically thin debris stream winding repeatedly around | |
the black hole. In the absence of black hole spin, in-plane | |
relativistic precession causes this stream to intersect | |
with itself after a single winding. In this paper we show | |
that relativistic precessions arising from black hole spin | |
can induce deflections out of the original orbital plane | |
that prevent the stream from self-intersecting even after | |
many windings. This naturally leads to a ``dark period'' in | |
which the flare is not observable for some time, persisting | |
for up to a dozen orbital periods of the most bound | |
material, which translates to years for disruptions around | |
black holes with masses ~ {10}7{M}o . When the stream | |
eventually self-intersects, the distance from the black | |
hole and the angle at which this collision occurs determine | |
the rate of energy dissipation. We find that more-massive | |
black holes ({M}{{h}}≳ {10}7{M}o ) tend to have more | |
violent stream self-intersections, resulting in prompt | |
accretion. For these tidal disruption events (TDEs), the | |
accretion rate onto the black hole should still closely | |
follow the original fallback rate after a fixed delay time | |
{t}{delay}, {\dot{M}}{acc}(t+{t}{delay})={\dot{M}}{fb}(t). | |
For lower black hole masses ({M}{{h}}≲ {10}6), we find | |
that flares are typically slowed down by about an order of | |
magnitude, resulting in the majority of TDEs being | |
sub-Eddington at peak. This also implies that current | |
searches for TDEs are biased toward prompt flares, with | |
slowed flares likely having been unidentified.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015ApJ...809..166G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1501.05306}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/809/2/166}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1501.05306}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2015ApJ...809..166G}, | |
Date-added = {2015-10-07 18:46:48 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/809/2/166}, | |
Eid = {166}, | |
Eprint = {1501.05306}, | |
Keywords = {black hole physics, galaxies: active, gravitation}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{guillochon&ramirezruiz2013, | |
Title = {{Hydrodynamical Simulations to Determine the Feeding Rate | |
of Black Holes by the Tidal Disruption of Stars: The | |
Importance of the Impact Parameter and Stellar Structure}}, | |
Author = {{Guillochon}, J. and {Ramirez-Ruiz}, E.}, | |
Journal = {\apj}, | |
Year = {2013}, | |
Month = apr, | |
Pages = {25}, | |
Volume = {767}, | |
Abstract = {The disruption of stars by supermassive black holes has | |
been linked to more than a dozen flares in the cores of | |
galaxies out to redshift z ~ 0.4. Modeling these flares | |
properly requires a prediction of the rate of mass return | |
to the black hole after a disruption. Through | |
hydrodynamical simulation, we show that aside from the full | |
disruption of a solar mass star at the exact limit where | |
the star is destroyed, the common assumptions used to | |
estimate \dot{M}(t), the rate of mass return to the black | |
hole, are largely invalid. While the analytical | |
approximation to tidal disruption predicts that the | |
least-centrally concentrated stars and the deepest | |
encounters should have more quickly-peaked flares, we find | |
that the most-centrally concentrated stars have the | |
quickest-peaking flares, and the trend between the time of | |
peak and the impact parameter for deeply penetrating | |
encounters reverses beyond the critical distance at which | |
the star is completely destroyed. We also show that the | |
most-centrally concentrated stars produced a characteristic | |
drop in \dot{M}(t) shortly after peak when a star is only | |
partially disrupted, with the power law index n being as | |
extreme as -4 in the months immediately following the peak | |
of a flare. Additionally, we find that n asymptotes to ~= - | |
2.2 for both low- and high-mass stars for approximately | |
half of all stellar disruptions. Both of these results are | |
significantly steeper than the typically assumed n = -5/3. | |
As these precipitous decay rates are only seen for events | |
in which a stellar core survives the disruption, they can | |
be used to determine if an observed tidal disruption flare | |
produced a surviving remnant. We provide fitting formulae | |
for four fundamental quantities of tidal disruption as | |
functions of the star's distance to the black hole at | |
pericenter and its stellar structure: the total mass lost, | |
the time of peak, the accretion rate at peak, and the | |
power-law index shortly after peak. These results should be | |
taken into consideration when flares arising from tidal | |
disruptions are modeled.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2013ApJ...767...25G}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1206.2350}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/767/1/25}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1206.2350}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2013ApJ...767...25G}, | |
Date-added = {2015-09-07 19:52:30 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/767/1/25}, | |
Eid = {25}, | |
Eprint = {1206.2350}, | |
Keywords = {accretion, accretion disks, black hole physics, | |
gravitation, hydrodynamics, methods: numerical}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{haring+2004, | |
Title = {{On the Black Hole Mass-Bulge Mass Relation}}, | |
Author = {{H{\"a}ring}, N. and {Rix}, H.-W.}, | |
Journal = {\apjl}, | |
Year = {2004}, | |
Month = apr, | |
Pages = {L89-L92}, | |
Volume = {604}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2004ApJ...604L..89H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/383567}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/383567}, | |
Eprint = {arXiv:astro-ph/0402376}, | |
Keywords = {Galaxies: Bulges, Galaxies: Kinematics and Dynamics} | |
} | |
@Article{haan+2009, | |
Title = {{Dynamical Evolution of AGN Host Galaxies---Gas | |
In/Out-Flow Rates in Seven NUGA Galaxies}}, | |
Author = {Haan, Sebastian and Schinnerer, Eva and Emsellem, Eric and | |
Garc\'{\i}a-Burillo, Santiago and Combes, Francoise and | |
Mundell, Carole G and Rix, Hans-Walter}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = feb, | |
Pages = {1623}, | |
Volume = {692}, | |
Abstract = {To examine the role of the host galaxy structure in | |
fueling nuclear activity, we estimated gas flow rates from | |
several kpc down to the inner few 10 pc for seven nearby | |
spiral galaxies, selected from the NUclei of GAlaxies | |
sample. We calculated gravitational torques from | |
near-infrared images and determined gas in/out-flow rates | |
as a function of radius and location within the galactic | |
disks, based on high angular resolution interferometric | |
observations of molecular (CO using Plateau de Bure | |
interferometer) and atomic (H I using the Very Large Array) | |
gas. The results are compared with kinematic evidence for | |
radial gas flows and the dynamical state of the galaxies | |
(via resonances) derived from several different methods. We | |
show that gravitational torques are very efficient at | |
transporting gas from the outer disk all the way into the | |
galaxies centers at \~{}100 pc; previously assumed | |
dynamical barriers to gas transport, such as the corotation | |
resonance of stellar bars, seem to be overcome by | |
gravitational torque induced gas flows from other | |
nonaxisymmetric structures. The resulting rates of gas mass | |
inflow range from 0.01 to 50 M sun yr-1 and are larger for | |
the galaxy center than for the outer disk. Our gas flow | |
maps show the action of nested bars within larger bars for | |
three galaxies. Noncircular streaming motions found in the | |
kinematic maps are larger in the center than in the outer | |
disk and appear to correlate only loosely with the | |
in/out-flow rates as a function of radius. We demonstrate | |
that spiral gas disks are very dynamic systems that undergo | |
strong radial evolution on timescales of a few rotation | |
periods (e.g., 5 × 108 yrs at a radius of 5 kpc), due to | |
the effectiveness of gravitational torques in | |
redistributing the cold galactic gas.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2009ApJ...692.1623H%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1088/0004-637X/692/2/1623}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0004-637X/692/2/1623}, | |
Keywords = {Accretion, galaxies: ISM, galaxies: Seyfert, galaxies: | |
active, galaxies: individual: NGC3368 NGC3627 NGC4321 NGC, | |
galaxies: kinematics and dynamics, radio lines: | |
galaxies,Accretion Disks}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2009ApJ...692.1623H\&link\_type=ABSTRACT} | |
} | |
@Article{habibi+2017, | |
Title = {{Twelve Years of Spectroscopic Monitoring in the Galactic | |
Center: The Closest Look at S-stars near the Black Hole}}, | |
Author = {{Habibi}, M. and {Gillessen}, S. and {Martins}, F. and | |
{Eisenhauer}, F. and {Plewa}, P.~M. and {Pfuhl}, O. and | |
{George}, E. and {Dexter}, J. and {Waisberg}, I. and {Ott}, | |
T. and {von Fellenberg}, S. and {Baub{\"o}ck}, M. and | |
{Jimenez-Rosales}, A. and {Genzel}, R.}, | |
Journal = {\apj}, | |
Year = {2017}, | |
Month = oct, | |
Pages = {120}, | |
Volume = {847}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017ApJ...847..120H}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/1538-4357/aa876f}, | |
Eid = {120}, | |
Eprint = {1708.06353}, | |
Keywords = {astrometry, Galaxy: center, infrared: stars, stars: | |
early-type, stars: fundamental parameters, techniques: | |
radial velocities}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.SR}, | |
Timestamp = {2017.12.12} | |
} | |
@Article{haehnelt+2002a, | |
Title = {{Multiple supermassive black holes in galactic bulges}}, | |
Author = {Haehnelt, Martin G and Kauffmann, Guinevere}, | |
Journal = {Monthly Notice of the Royal Astronomical Society}, | |
Year = {2002}, | |
Month = nov, | |
Pages = {L61}, | |
Volume = {336}, | |
Abstract = {We study the number and interaction rates of supermassive | |
black holes in galactic bulges as predicted by hierarchical | |
models of galaxy formation in which the spheroidal | |
components of galaxies are formed by mergers. In bright | |
ellipticals, the number of events that can eject a central | |
supermassive binary black hole is large. Central binaries | |
must therefore merge in less than a Hubble time - otherwise | |
there will be too much scatter in the M*-$\sigma$* relation | |
and too many off-centre galactic nuclei. We propose that | |
binary black holes are able to merge during the major gas | |
accretion events that trigger QSO activity in galaxies. If | |
this is the case, less than 10 per cent of faint | |
ellipticals and 40 per cent of bright ellipticals are | |
predicted to harbour binary black holes with near equal | |
masses at their centres. This binary may be ejected away | |
from the centre of the galaxy or even into intergalactic | |
space in up to 20 per cent of the most luminous | |
ellipticals. The number of low-mass black holes that can | |
interact with the central object is predicted to be a | |
strong function of galaxy luminosity. In most faint | |
ellipticals, no black holes fall into the centre of the | |
galaxy after the last major gas accretion event, but in the | |
most luminous ellipticals, an average of 10 low-mass black | |
holes interact with the central supermassive object after | |
this time. It is expected that stars will be ejected from | |
galaxy cores as these low mass ratio binaries harden. | |
Multiple black holes in galactic bulges thus provide a | |
natural explanation for the strong systematic trends in the | |
observed central density profiles of ellipticals as a | |
function of luminosity.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2002MNRAS.336L..61H%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1046/j.1365-8711.2002.06056.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1046/j.1365-8711.2002.06056.x}, | |
Keywords = {BLACK HOLE PHYSICS, binaries: general, galaxies: | |
nuclei,galaxies: formation; Untitled; Untitled1}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2002MNRAS.336L..61H\&link\_type=ABSTRACT} | |
} | |
@Article{haggard+2010, | |
Title = {{The Field X-ray AGN Fraction to z = 0.7 from the Chandra | |
Multiwavelength Project and the Sloan Digital Sky Survey}}, | |
Author = {{Haggard}, D. and {Green}, P.~J. and {Anderson}, S.~F. and | |
{Constantin}, A. and {Aldcroft}, T.~L. and {Kim}, D.-W. and | |
{Barkhouse}, W.~A.}, | |
Journal = {\apj}, | |
Year = {2010}, | |
Month = nov, | |
Pages = {1447-1468}, | |
Volume = {723}, | |
Abstract = {We employ the Chandra Multiwavelength Project (ChaMP) and | |
the Sloan Digital Sky Survey (SDSS) to study the fraction | |
of X-ray-active galaxies in the field to z = 0.7. We | |
utilize spectroscopic redshifts from SDSS and ChaMP, as | |
well as photometric redshifts from several SDSS catalogs, | |
to compile a Parent sample of more than 100,000 SDSS | |
galaxies and nearly 1600 Chandra X-ray detections. Detailed | |
ChaMP volume completeness maps allow us to investigate the | |
local fraction of active galactic nuclei (AGNs), defined as | |
those objects having broadband X-ray luminosities LX (0.5-8 | |
keV) >=1042 erg s-1, as a function of absolute optical | |
magnitude, X-ray luminosity, redshift, mass, and host | |
color/morphological type. In five independent samples | |
complete in redshift and i-band absolute magnitude, we | |
determine the field AGN fraction to be between 0.16% ? | |
0.06% (for z <= 0.125 and -18>Mi > - 20) and 3.80% ? 0.92% | |
(for z <= 0.7 and Mi < -23). We find excellent agreement | |
between our ChaMP/SDSS field AGN fraction and the Chandra | |
cluster AGN fraction, for samples restricted to similar | |
redshift and absolute magnitude ranges: 1.19% ? 0.11% of | |
ChaMP/SDSS field galaxies with 0.05 < z < 0.31 and absolute | |
R-band magnitude more luminous than MR < -20 are AGNs. Our | |
results are also broadly consistent with measures of the | |
field AGN fraction in narrow, deep fields, though | |
differences in the optical selection criteria, redshift | |
coverage, and possible cosmic variance between fields | |
introduce larger uncertainties in these comparisons.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010ApJ...723.1447H}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1088/0004-637X/723/2/1447}, | |
Eprint = {1004.1638}, | |
Keywords = {galaxies: active, galaxies: nuclei, surveys, X-rays: | |
galaxies}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2018.02.23} | |
} | |
@InProceedings{hailey&mori2017, | |
Title = {{NuSTAR observations of black hole binary candidates in | |
the Galactic Center and its environs}}, | |
Author = {{Hailey}, C.~J. and {Mori}, K.}, | |
Booktitle = {AAS/High Energy Astrophysics Division}, | |
Year = {2017}, | |
Month = aug, | |
Pages = {109.12}, | |
Series = {AAS/High Energy Astrophysics Division}, | |
Volume = {16}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017HEAD...1610912H}, | |
Eid = {109.12}, | |
Owner = {aleksey}, | |
Timestamp = {2017.10.13} | |
} | |
@Article{hailey+2018, | |
Title = {A density cusp of quiescent X-ray binaries in the central parsec of the Galaxy}, | |
Author = {Hailey, C.~J. and Mori, K. and Bauer, F.~E. and Berkowitz, M.~E. and Hong, J. and Hord, B.~J.}, | |
Journal = {Nature}, | |
Year = {2018}, | |
Month = apr, | |
Pages = {70--}, | |
Volume = {556}, | |
Owner = {aleksey}, | |
Publisher = {Macmillan Publishers Limited, part of Springer Nature. All rights reserved.}, | |
Timestamp = {2018.04.07}, | |
Url = {http://dx.doi.org/10.1038/nature25029} | |
} | |
@Article{haiman+2009a, | |
author = {Haiman, Zolt\'{a}n and Kocsis, Bence and Menou, Kristen}, | |
title = {{The Population of Viscosity- and Gravitational Wave-driven Supermassive Black Hole Binaries Among Luminous Active Galactic Nuclei}}, | |
journal = {\apj}, | |
year = {2009}, | |
volume = {700}, | |
pages = {1952}, | |
month = aug, | |
abstract = {Supermassive black hole binaries (SMBHBs) in galactic | |
nuclei are thought to be a common by-product of major | |
galaxy mergers. We use simple disk models for the | |
circumbinary gas and for the binary-disk interaction to | |
follow the orbital decay of SMBHBs with a range of total | |
masses (M) and mass ratios (q), through physically distinct | |
regions of the disk, until gravitational waves (GWs) take | |
over their evolution. Prior to the GW-driven phase, the | |
viscous decay is generically in the stalled | |
"secondary-dominated" regime. SMBHBs spend a non-negligible | |
fraction of a fiducial time of 107 yr at orbital periods | |
between days lsimt orblsim yr, and we argue that they may | |
be sufficiently common to be detectable, provided they are | |
luminous during these stages. A dedicated optical or X-ray | |
survey could identify coalescing SMBHBs statistically, as a | |
population of periodically variable quasars, whose | |
abundance obeys the scaling N var vprop t $\alpha$ var | |
within a range of periods around t var\~{} tens of weeks. | |
SMBHBs with M lsim 107 M sun, with 0.5 lsim $\alpha$ lsim | |
1.5, would probe the physics of viscous orbital decay, | |
whereas the detection of a population of higher-mass | |
binaries, with $\alpha$ = 8/3, would confirm that their | |
decay is driven by GWs. The lowest-mass SMBHBs (M lsim | |
105-6 M sun) enter the GW-driven regime at short orbital | |
periods, when they are already in the frequency band of the | |
Laser Interferometric Space Antenna (LISA). While viscous | |
processes are negligible in the last few years of | |
coalescence, they could reduce the amplitude of any | |
unresolved background due to near-stationary LISA sources. | |
We discuss modest constraints on the SMBHB population | |
already available from existing data, and the sensitivity | |
and sky coverage requirements for a detection in future | |
surveys. SMBHBs may also be identified from velocity shifts | |
in their spectra; we discuss the expected abundance of | |
SMBHBs as a function of their orbital velocity.}, | |
bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2009ApJ...700.1952H%5C&link%5C_type=ABSTRACT}, | |
bdsk-url-2 = {http://dx.doi.org/10.1088/0004-637X/700/2/1952}, | |
date-added = {2015-10-29 19:33:44 +0000}, | |
date-modified = {2015-10-29 20:04:54 +0000}, | |
doi = {10.1088/0004-637X/700/2/1952}, | |
file = {:Haiman/2009.pdf:PDF}, | |
keywords = {black hole physics, galaxies: nuclei,gravitational waves; Untitled; Untitled1}, | |
url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2009ApJ...700.1952H\&link\_type=ABSTRACT}, | |
} | |
@Article{haiman+2009, | |
Title = {{Identifying decaying supermassive black hole binaries | |
from their variable electromagnetic emission}}, | |
Author = {Haiman, Z and Kocsis, B and Menou, K and Lippai, Z and | |
Frei, Z}, | |
Journal = {Class. Quantum Grav.}, | |
Year = {2009}, | |
Month = may, | |
Number = {9}, | |
Pages = {94032}, | |
Volume = {26}, | |
Archiveprefix = {arXiv}, | |
Arxivid = {0811.1920}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0264-9381/26/9/094032}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:40 +0000}, | |
Doi = {10.1088/0264-9381/26/9/094032}, | |
Eprint = {0811.1920} | |
} | |
@Article{halpern+1988, | |
Title = {{A test of the massive binary black hole hypothesis - ARP | |
102B}}, | |
Author = {{Halpern}, J.~P. and {Filippenko}, A.~V.}, | |
Journal = {\nat}, | |
Year = {1988}, | |
Month = jan, | |
Pages = {46-48}, | |
Volume = {331}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1988Natur.331...46H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1038/331046a0}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1038/331046a0}, | |
Keywords = {ACTIVE GALACTIC NUCLEI, ASTRONOMICAL MODELS, ASTRONOMICAL | |
SPECTROSCOPY, BLACK HOLES (ASTRONOMY), ELLIPTICAL GALAXIES, | |
EMISSION SPECTRA, H ALPHA LINE, RED SHIFT, SPECTRUM | |
ANALYSIS} | |
} | |
@Article{harper-clark+2009, | |
Title = {{One-Dimensional Dynamical Models of the Carina Nebula | |
Bubble}}, | |
Author = {{Harper-Clark}, E. and {Murray}, N.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = mar, | |
Pages = {1696-1712}, | |
Volume = {693}, | |
Abstract = {We have tested the two main theoretical models of bubbles | |
around massive star clusters, Castor et al. and Chevalier & | |
Clegg, against observations of the well-studied Carina | |
nebula. The Castor et al. theory overpredicts the X-ray | |
luminosity in the Carina bubble by a factor of 60 and | |
expands too rapidly, by a factor of 4; if the correct | |
radius and age are used, the predicted X-ray luminosity is | |
even larger. In contrast, the Chevalier & Clegg model | |
underpredicts the X-ray luminosity by a factor of 10. We | |
modify the Castor et al. theory to take into account lower | |
stellar wind mass-loss rates, radiation pressure, gravity, | |
and escape of or energy loss from the hot shocked gas. We | |
argue that energy is advected rather than radiated from the | |
bubble. We undertake a parameter study for reduced stellar | |
mass-loss rates and for various leakage rates and are able | |
to find viable models. The X-ray surface brightness in | |
Carina is highest close to the bubble wall, which is | |
consistent with conductive evaporation from cold clouds. | |
The picture that emerges is one in which the hot gas | |
pressure is far below that found by dividing the | |
time-integrated wind luminosity by the bubble volume; | |
rather, the pressure in the hot gas is set by pressure | |
equilibrium with the photoionized gas at T = 104 K. It | |
follows that the shocked stellar winds are not dynamically | |
important in forming the bubbles.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...693.1696H}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/0812.2906}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/693/2/1696}, | |
Bdsk-url-2 = {http://arXiv.org/abs/0812.2906}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2009ApJ...693.1696H}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1088/0004-637X/693/2/1696}, | |
Eprint = {0812.2906}, | |
Keywords = {ISM: bubbles} | |
} | |
@Article{hascoet+2014, | |
Title = {{Estimates for Lorentz Factors of Gamma-Ray Bursts from | |
Early Optical Afterglow Observations}}, | |
Author = {{Hasco{\"e}t}, R. and {Beloborodov}, A.~M. and {Daigne}, | |
F. and {Mochkovitch}, R.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = feb, | |
Pages = {5}, | |
Volume = {782}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...782....5H}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1304.5813}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/782/1/5}, | |
Date-added = {2016-05-26 15:42:13 +0000}, | |
Date-modified = {2016-05-26 15:42:22 +0000}, | |
Doi = {10.1088/0004-637X/782/1/5}, | |
Eid = {5}, | |
Eprint = {1304.5813}, | |
Keywords = {gamma-ray burst: general}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{hayasaki2009, | |
Title = {{A New Mechanism for Massive Binary Black-Hole | |
Evolution}}, | |
Author = {{Hayasaki}, K.}, | |
Journal = {\pasj}, | |
Year = {2009}, | |
Month = feb, | |
Pages = {65-}, | |
Volume = {61}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009PASJ...61...65H}, | |
Archiveprefix = {arXiv}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {0805.3408}, | |
Keywords = {accretion, accretion disks, binaries:general, black hole | |
physics, galaxies:nuclei; Untitled; Untitled1} | |
} | |
@Article{hayasaki+2015a, | |
Title = {{Detection of Gravitational Wave Emission by Supermassive | |
Black Hole Binaries Through Tidal Disruption Flares}}, | |
Author = {{Hayasaki}, K. and {Loeb}, A.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2015}, | |
Month = oct, | |
Abstract = {Galaxy mergers produce binaries of supermassive black | |
holes, which emit gravitational waves prior to their | |
coalescence. We perform three-dimensional hydrodynamic | |
simulations to study the tidal disruption of stars by such | |
a binary in the final centuries of its life. We find that | |
the gas stream of the stellar debris moves chaotically in | |
the binary potential and forms accretion disks around both | |
black holes. The accretion light curve is modulated over | |
the binary orbital period owing to relativistic beaming. | |
This periodic signal allows to detect the decay of the | |
binary orbit due to gravitational wave emission by | |
observing two tidal disruption events that are separated by | |
more than a decade.}, | |
Adscomment = {14pages, 4 figures, submitted}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015arXiv151005760H}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1510.05760}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://arXiv.org/abs/1510.05760}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/2015arXiv151005760H}, | |
Date-added = {2015-10-23 16:15:54 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {1510.05760}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena, | |
Astrophysics - Astrophysics of Galaxies, General Relativity | |
and Quantum Cosmology; Untitled; Untitled1}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{hayasaki+2008, | |
Title = {{Periodic light variations from the triple-disk system | |
around supermassive binary black holes}}, | |
Author = {Hayasaki, K and Mineshige, S}, | |
Journal = {ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: The 10th | |
International Symposium on Origin of Matter and Evolution | |
of Galaxies: From the Dawn of Universe to the Formation of | |
Solar System. AIP Conference Proceedings}, | |
Year = {2008}, | |
Month = may, | |
Pages = {406}, | |
Volume = {1016}, | |
Abstract = {We investigate accretion flows around supermassive binary | |
black holes (BBHs) with the orbital eccentricity e = 0.5, | |
the semi-major axis a = 0.01 pc, and the low mass ratio of | |
the secondary black hole (BH) to the primary BH q = 0.1. In | |
the simulations we consider a triple-disk system composing | |
of two accretion disks around BHs and one circumbinary disk | |
surrounding the two. The circumbinary disk works as a mass | |
reservoir. We confirm that a non-axisymmetric accretion | |
disk is formed around each BH. The X-ray luminosity of the | |
secondary BH exhibits the double peaks every binary orbit, | |
whereas that of the primary BH shows a single peak. Such | |
properties can not be seen in the case of equal mass BBHs | |
and therefore provide a potentially important observational | |
signature of supermassive BBHs with low mass ratios.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2008AIPC.1016..406H%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1063/1.2943607}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1063/1.2943607}, | |
Keywords = {Accretion, Infall, Supergiant stars, and accretion | |
disks,Physics of black holes}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2008AIPC.1016..406H\&link\_type=ABSTRACT} | |
} | |
@InProceedings{hayasaki+2007a, | |
Title = {{SPH Simulations of Accretion Flows onto Supermassive | |
Binary Black Holes from Circumbinary Disks}}, | |
Author = {{Hayasaki}, K. and {Mineshige}, S. and {Sudou}, H.}, | |
Booktitle = {The Central Engine of Active Galactic Nuclei}, | |
Year = {2007}, | |
Editor = {{Ho}, L.~C. and {Wang}, J.-W.}, | |
Month = oct, | |
Pages = {59}, | |
Series = {Astronomical Society of the Pacific Conference Series}, | |
Volume = {373}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007ASPC..373...59H}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {astro-ph/0612526}, | |
Keywords = {Untitled; Untitled1} | |
} | |
@Article{hayasaki+2007, | |
Title = {{Binary Black Hole Accretion Flows in Merged Galactic | |
Nuclei}}, | |
Author = {{Hayasaki}, K. and {Mineshige}, S. and {Sudou}, H.}, | |
Journal = {\pasj}, | |
Year = {2007}, | |
Month = apr, | |
Pages = {427-441}, | |
Volume = {59}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007PASJ...59..427H}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Eprint = {arXiv:astro-ph/0609144}, | |
Keywords = {accretion, accretion disks, binary black holes, black hole | |
physics, galaxies: nuclei; Untitled; Untitled1} | |
} | |
@Article{hayasaki+2007b, | |
Title = {{Binary Black Hole Accretion Flows in Merged Galactic | |
Nuclei}}, | |
Author = {Hayasaki, Kimitake and Mineshige, Shin and Sudou, | |
Hiroshi}, | |
Journal = {Publications of the Astronomical Society of Japan}, | |
Year = {2007}, | |
Month = apr, | |
Pages = {427}, | |
Volume = {59}, | |
Abstract = {We consider accretion flows from circumbinary disks onto | |
supermassive binary black holes on a subparsec scale of the | |
galactic center based on a smoothed particles hydrodynamics | |
(SPH) code. Simulation models are presented for four cases; | |
that is, a circular binary and an eccentric one, each with | |
equal and unequal masses. We find that the circumblack-hole | |
disks are formed around each black hole regardless of the | |
simulation parameters. There are two-step mechanisms that | |
cause accretion flow. First, tidally induced elongation of | |
the circumbinary disk triggers mass inflow toward two | |
closest points on the circumbinary disk. Then, the gas is | |
increasingly accumulated on these two points owing to the | |
gravitational attraction of black holes. Second, when the | |
gas can pass across the maximum loci of the effective | |
binary potential, it starts to overflow via their two | |
points, and freely infalls to each black hole. In circular | |
binaries, the gas continues to be supplied from the | |
circumbinary disk, (i.e., the gap between the circumbinary | |
disk and the binary black hole is always closed). In | |
eccentric cases, the mass supply undergoes periodic on/off | |
transitions during one orbital period because of the | |
variation of the periodic potential. The gap starts to | |
close after the apoastron, and to open again after the next | |
periastron passage. Due to the gap closing/opening cycles, | |
the mass-capture rates are eventually strongly phase | |
dependent. This could provide observable diagnosis for the | |
presence of supermassive binary black holes in merged | |
galactic nuclei.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2007PASJ...59..427H%5C&link%5C_type=ABSTRACT}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Keywords = {Accretion, Accretion Disks, black hole physics, galaxies: | |
nuclei,binary black holes; Untitled; Untitled1}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2007PASJ...59..427H\&link\_type=ABSTRACT} | |
} | |
@Article{hayasaki+2009, | |
Title = {{A New Approach for Probing Circumbinary Disks}}, | |
Author = {Hayasaki, Kimitake and Okazaki, Atsuo T}, | |
Journal = {\apjl}, | |
Year = {2009}, | |
Month = jan, | |
Pages = {L5}, | |
Volume = {691}, | |
Abstract = {Circumbinary disks are considered to exist in a wide | |
variety of astrophysical objects, e.g., young binary stars, | |
protoplanetary systems, and massive binary black hole | |
systems in active galactic nuclei (AGNs). However, there is | |
no definite evidence for the circumbinary disk except for | |
some in a few young binary star systems. In this Letter, we | |
study possible oscillation modes in circumbinary disks | |
around eccentric and circular binaries. We find that | |
prograde, nonaxisymmetric waves are induced in the inner | |
part of the circumbinary disk by the tidal potential of the | |
binary. Such waves would cause variabilities in emission | |
line profiles from circumbinary disks. Because of prograde | |
precession of the waves, the distance between each | |
component of the binary and the inner edge of the | |
circumbinary disk varies with the beat period between the | |
precession period of the wave and the binary orbital | |
period. As a result, light curves from the circumbinary | |
disks are also expected to vary with the same period. The | |
current study thus provides a new method to detect | |
circumbinary disks in various astrophysical systems.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2009ApJ...691L...5H%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1088/0004-637X/691/1/L5}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1088/0004-637X/691/1/L5}, | |
Keywords = {Accretion, Accretion Disks, binaries: general, black hole | |
physics, galaxies: nuclei, planetary systems: | |
protoplanetary disks,stars: formation}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2009ApJ...691L...5H\&link\_type=ABSTRACT} | |
} | |
@Article{hayasaki+2016, | |
Title = {{Circularization of tidally disrupted stars around spinning supermassive black holes}}, | |
Author = {{Hayasaki}, K. and {Stone}, N. and {Loeb}, A.}, | |
Journal = {\mnras}, | |
Year = {2016}, | |
Month = oct, | |
Pages = {3760-3780}, | |
Volume = {461}, | |
Abstract = {We study the circularization of tidally disrupted stars on bound orbits around spinning supermassive black holes by performing 3D smoothed particle hydrodynamic simulations with post-Newtonian corrections. Our simulations reveal that debris circularization depends sensitively on the efficiency of radiative cooling. There are two stages in debris circularization if radiative cooling is inefficient: first, the stellar debris streams self-intersect due to relativistic apsidal precession; shocks at the intersection points thermalize orbital energy and the debris forms a geometrically thick, ring-like structure around the black hole. The ring rapidly spreads via viscous diffusion, leading to the formation of a geometrically thick accretion disc. In contrast, if radiative cooling is efficient, the stellar debris circularizes due to self-intersection shocks and forms a geometrically thin ring-like structure. In this case, the dissipated energy can be emitted during debris circularization as a precursor to the subsequent tidal disruption flare. The circularization time-scale is remarkably long in the radiatively efficient cooling case, and is also sensitive to black hole spin. Specifically, Lense-Thirring torques cause dynamically important nodal precession, which significantly delays debris circularization. On the other hand, nodal precession is too slow to produce observable signatures in the radiatively inefficient case. Since the stellar debris is optically thick and its photon diffusion time is likely longer than the time-scale of shock heating, our inefficient cooling scenario is more generally applicable in eccentric tidal disruption events (TDEs). However, in parabolic TDEs for MBH ? 2 × 106 M?, the spin-sensitive behaviour associated with efficient cooling may be realized.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016MNRAS.461.3760H}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1093/mnras/stw1387}, | |
Eprint = {1501.05207}, | |
Keywords = {accretion, accretion discs, black hole physics, gravitational waves, hydrodynamics}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2018.03.13} | |
} | |
@Article{hayasaki+2013, | |
Title = {{Finite, intense accretion bursts from tidal disruption of | |
stars on bound orbits}}, | |
Author = {{Hayasaki}, K. and {Stone}, N. and {Loeb}, A.}, | |
Journal = {\mnras}, | |
Year = {2013}, | |
Month = sep, | |
Pages = {909-924}, | |
Volume = {434}, | |
Abstract = {We study accretion processes for tidally disrupted stars | |
approaching supermassive black holes on bound orbits, by | |
performing three-dimensional smoothed particle | |
hydrodynamics simulations with a pseudo-Newtonian | |
potential. We find that there is a critical value of the | |
orbital eccentricity below which all the stellar debris | |
remains bound to the black hole. For high but subcritical | |
eccentricities, all the stellar mass is accreted on to the | |
black hole in a finite time, causing a significant | |
deviation from the canonical t-5/3 mass fallback rate. When | |
a star is on a moderately eccentric orbit and its | |
pericentre distance is deeply inside the tidal disruption | |
radius, there can be several orbit crossings of the debris | |
streams due to relativistic precession. This dissipates | |
orbital energy in shocks, allowing for rapid | |
circularization of the debris streams and formation of an | |
accretion disc. The resultant accretion rate greatly | |
exceeds the Eddington rate and differs strongly from the | |
canonical rate of t-5/3. By contrast, there is little | |
dissipation due to orbital crossings for the equivalent | |
simulation with a purely Newtonian potential. This shows | |
that general relativistic precession is crucial for | |
accretion disc formation via circularization of stellar | |
debris from stars on moderately eccentric orbits.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2013MNRAS.434..909H}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1210.1333}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stt871}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1210.1333}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2013MNRAS.434..909H}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1093/mnras/stt871}, | |
Eprint = {1210.1333}, | |
Keywords = {accretion, accretion discs, black hole physics, | |
gravitational waves, hydrodynamics}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{hayasaki+2018, | |
Title = {{Classification of Tidal Disruption Events Based on Stellar Orbital Properties}}, | |
Author = {{Hayasaki}, K. and {Zhong}, S. and {Li}, S. and {Berczik}, P. and {Spurzem}, R.}, | |
Journal = {\apj}, | |
Year = {2018}, | |
Month = mar, | |
Pages = {129}, | |
Volume = {855}, | |
Abstract = {We study the rates of tidal disruption of stars on bound to unbound orbits by intermediate-mass to supermassive black holes using high-accuracy direct N-body experiments. Stars from the star cluster approaching the black hole can have three types of orbit: eccentric, parabolic, and hyperbolic. Since the mass fallback rate shows different variabilities depending on the orbital type, we can classify tidal disruption events (TDEs) into three main categories: eccentric, parabolic, and hyperbolic. The respective TDEs are characterized by two critical values of the orbital eccentricity: the lower critical eccentricity is the one below which stars on eccentric orbits cause finite, intense accretion, and the upper critical eccentricity is the one above which stars on hyperbolic orbits cause no accretion. Moreover, we find that parabolic TDEs can be divided into three subclasses: precisely parabolic, marginally eccentric, and marginally hyperbolic. We analytically derive that the mass fallback rate of marginally eccentric TDEs can be flatter and slightly higher than the standard fallback rate proportional to t ?5/3, whereas it can be flatter and lower for marginally hyperbolic TDEs. We confirm using N-body experiments that only a few eccentric, precisely parabolic, and hyperbolic TDEs can occur in a spherical stellar system with a single intermediate-mass to supermassive black hole. A substantial fraction of the stars approaching the black hole would cause marginally eccentric or marginally hyperbolic TDEs.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2018ApJ...855..129H}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/1538-4357/aab0a5}, | |
Eid = {129}, | |
Eprint = {1802.06798}, | |
Keywords = {accretion, accretion disks, black hole physics, galaxies: nuclei, galaxies: star clusters: general, methods: numerical, stars: kinematics and dynamics }, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2018.06.07} | |
} | |
@Article{hayasaki+2017, | |
Author = {{Haysaki}, K. and {Author 2} and {Author 3}} | |
} | |
@Article{heckman&best2014, | |
Title = {{The Coevolution of Galaxies and Supermassive Black Holes: | |
Insights from Surveys of the Contemporary Universe}}, | |
Author = {{Heckman}, T.~M. and {Best}, P.~N.}, | |
Journal = {\araa}, | |
Year = {2014}, | |
Month = aug, | |
Pages = {589-660}, | |
Volume = {52}, | |
Abstract = {We summarize what large surveys of the contemporary | |
Universe have taught us about the physics and phenomenology | |
of the processes that link the formation and evolution of | |
galaxies with their central supermassive black holes. We | |
present a picture in which the population of active | |
galactic nuclei (AGNs) can be divided into two distinct | |
populations. The radiative-mode AGNs are associated with | |
black holes (BHs) that produce radiant energy powered by | |
accretion at rates in excess of ˜1% of the Eddington | |
limit. They are primarily associated with less massive BHs | |
growing in high-density pseudobulges at a rate sufficient | |
to produce the total mass budget in these BHs in ˜10 Gyr. | |
The circumnuclear environment contains high-density cold | |
gas and associated star formation. Major mergers are not | |
the primary mechanism for transporting this gas inward; | |
secular processes appear dominant. Stellar feedback is | |
generic in these objects, and strong AGN feedback is seen | |
only in the most powerful AGNs. In jet-mode AGNs the bulk | |
of energetic output takes the form of collimated outflows | |
(jets). These AGNs are associated with the more massive BHs | |
in more massive (classical) bulges and elliptical galaxies. | |
Neither the accretion onto these BHs nor star formation in | |
their host bulge is significant today. These AGNs are | |
probably fueled by the accretion of slowly cooling hot gas | |
that is limited by the feedback/heating provided by AGN | |
radio sources. Surveys of the high-redshift Universe paint | |
a similar picture. Noting that the volume-averaged ratio of | |
star formation to BH growth has remained broadly constant | |
over the past 10 Gyrs, we argue that the processes that | |
linked the cosmic evolution of galaxies and BHs are still | |
at play today.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ARA%26A..52..589H}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1403.4620}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1146/annurev-astro-081913-035722}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1403.4620}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014ARA%26A..52..589H}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1146/annurev-astro-081913-035722}, | |
Eprint = {1403.4620}, | |
Primaryclass = {astro-ph.GA} | |
} | |
@Article{heckman+2014, | |
Title = {{The Coevolution of Galaxies and Supermassive Black Holes: | |
Insights from Surveys of the Contemporary Universe}}, | |
Author = {{Heckman}, T.~M. and {Best}, P.~N.}, | |
Journal = {\araa}, | |
Year = {2014}, | |
Month = aug, | |
Pages = {589-660}, | |
Volume = {52}, | |
Abstract = {We summarize what large surveys of the contemporary | |
Universe have taught us about the physics and phenomenology | |
of the processes that link the formation and evolution of | |
galaxies with their central supermassive black holes. We | |
present a picture in which the population of active | |
galactic nuclei (AGNs) can be divided into two distinct | |
populations. The radiative-mode AGNs are associated with | |
black holes (BHs) that produce radiant energy powered by | |
accretion at rates in excess of ˜1% of the Eddington | |
limit. They are primarily associated with less massive BHs | |
growing in high-density pseudobulges at a rate sufficient | |
to produce the total mass budget in these BHs in ˜10 Gyr. | |
The circumnuclear environment contains high-density cold | |
gas and associated star formation. Major mergers are not | |
the primary mechanism for transporting this gas inward; | |
secular processes appear dominant. Stellar feedback is | |
generic in these objects, and strong AGN feedback is seen | |
only in the most powerful AGNs. In jet-mode AGNs the bulk | |
of energetic output takes the form of collimated outflows | |
(jets). These AGNs are associated with the more massive BHs | |
in more massive (classical) bulges and elliptical galaxies. | |
Neither the accretion onto these BHs nor star formation in | |
their host bulge is significant today. These AGNs are | |
probably fueled by the accretion of slowly cooling hot gas | |
that is limited by the feedback/heating provided by AGN | |
radio sources. Surveys of the high-redshift Universe paint | |
a similar picture. Noting that the volume-averaged ratio of | |
star formation to BH growth has remained broadly constant | |
over the past 10 Gyrs, we argue that the processes that | |
linked the cosmic evolution of galaxies and BHs are still | |
at play today.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ARA%26A..52..589H}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1403.4620}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1146/annurev-astro-081913-035722}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1403.4620}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014ARA%26A..52..589H}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1146/annurev-astro-081913-035722}, | |
Eprint = {1403.4620}, | |
Primaryclass = {astro-ph.GA} | |
} | |
@Article{heckman+2004, | |
Title = {{Present-Day Growth of Black Holes and Bulges: The Sloan | |
Digital Sky Survey Perspective}}, | |
Author = {{Heckman}, T.~M. and {Kauffmann}, G. and {Brinchmann}, J. | |
and {Charlot}, S. and {Tremonti}, C. and {White}, | |
S.~D.~M.}, | |
Journal = {\apj}, | |
Year = {2004}, | |
Month = sep, | |
Pages = {109-118}, | |
Volume = {613}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2004ApJ...613..109H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/422872}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/422872}, | |
Eprint = {astro-ph/0406218}, | |
Keywords = {Galaxies: Active, Galaxies: Bulges, Galaxies: Evolution, | |
Galaxies: Nuclei, Galaxies: Stellar Content} | |
} | |
@Article{heggie1975, | |
Title = {{Binary evolution in stellar dynamics}}, | |
Author = {{Heggie}, D.~C.}, | |
Journal = {\mnras}, | |
Year = {1975}, | |
Month = dec, | |
Pages = {729-787}, | |
Volume = {173}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1975MNRAS.173..729H}, | |
Doi = {10.1093/mnras/173.3.729}, | |
Keywords = {Binary Stars, Many Body Problem, Stellar Evolution, | |
Equations Of Motion, Kinetic Energy, Numerical Integration, | |
Stellar Motions}, | |
Owner = {aleksey}, | |
Timestamp = {2017.12.19} | |
} | |
@Article{heinke+2015, | |
Title = {{The nature of very faint X-ray binaries: hints from light | |
curves}}, | |
Author = {{Heinke}, C.~O. and {Bahramian}, A. and {Degenaar}, N. and | |
{Wijnands}, R.}, | |
Journal = {\mnras}, | |
Year = {2015}, | |
Month = mar, | |
Pages = {3034-3043}, | |
Volume = {447}, | |
Abstract = {Very faint X-ray binaries (VFXBs), defined as having peak | |
luminosities LX of 1034-1036 erg s-1, have been uncovered | |
in significant numbers, but remain poorly understood. We | |
analyse three published outburst light curves of two | |
transient VFXBs using the exponential and linear decay | |
formalism of King & Ritter. The decay time-scales and brink | |
luminosities suggest orbital periods of order 1 h. We | |
review various estimates of VFXB properties, and compare | |
these with suggested explanations of the nature of VFXBs. | |
We suggest that: (1) VFXB outbursts showing linear decays | |
might be explained as partial drainings of the disc of | |
`normal' X-ray transients, and many VFXB outbursts may | |
belong to this category; (2) VFXB outbursts showing | |
exponential decays are best explained by old, short-period | |
systems involving mass transfer from a low-mass white dwarf | |
or brown dwarf; (3) persistent (or quasi-persistent) VFXBs, | |
which maintain an LX of 1034-1035 erg s-1 for years, may be | |
explained by magnetospheric choking of the accretion flow | |
in a propeller effect, permitting a small portion of the | |
flow to accrete on to the neutron star's surface. We thus | |
predict that (quasi-) persistent VFXBs may also be | |
transitional millisecond pulsars, turning on as millisecond | |
radio pulsars when their LX drops below 1032 erg s-1.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2015MNRAS.447.3034H}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1412.4097}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stu2652}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1412.4097}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2015MNRAS.447.3034H}, | |
Date-added = {2017-07-28 18:58:53 +0000}, | |
Date-modified = {2017-07-28 19:55:49 +0000}, | |
Doi = {10.1093/mnras/stu2652}, | |
Eprint = {1412.4097}, | |
Keywords = {accretion, accretion discs, X-rays: binaries, X-rays: | |
individual: CXOGC J174540.0-290005, X-rays: individual: XMM | |
J174457-2850.3}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{heinke+2005a, | |
Title = {{Three Additional Quiescent Low-Mass X-Ray Binary | |
Candidates in 47 Tucanae}}, | |
Author = {{Heinke}, C.~O. and {Grindlay}, J.~E. and {Edmonds}, | |
P.~D.}, | |
Journal = {\apj}, | |
Year = {2005}, | |
Month = mar, | |
Pages = {556-564}, | |
Volume = {622}, | |
Abstract = {We identify through their X-ray spectra one certain (W37) | |
and two probable (W17 and X4) quiescent low-mass X-ray | |
binaries (qLMXBs) containing neutron stars in a long | |
Chandra X-ray exposure of the globular cluster 47 Tucanae, | |
in addition to the two previously known qLMXBs. W37's | |
spectrum is dominated by a blackbody-like component | |
consistent with radiation from the hydrogen atmosphere of a | |
10 km neutron star. W37's light curve shows strong X-ray | |
variability, which we attribute to variations in its | |
absorbing column depth, and eclipses with a probable 3.087 | |
hr period. For most of our exposures, W37's blackbody-like | |
emission (assumed to be from the neutron star surface) is | |
almost completely obscured, yet some soft X-rays (of | |
uncertain origin) remain. Two additional candidates, W17 | |
and X4, present X-ray spectra dominated by a harder | |
component, fitted by a power law of photon index ~1.6-3. An | |
additional soft component is required for both W17 and X4, | |
which can be fitted with a 10 km hydrogen atmosphere | |
neutron star model. X4 shows significant variability, which | |
may arise from either its power-law or hydrogen atmosphere | |
spectral component. Both W17 and X4 show rather low X-ray | |
luminosities, LX(0.5-10keV)~5?031 ergs s-1. All three | |
candidate qLMXBs would be difficult to identify in other | |
globular clusters, suggesting an additional reservoir of | |
fainter qLMXBs in globular clusters that may be of similar | |
numbers as the group of previously identified objects. The | |
number of millisecond pulsars inferred to exist in 47 Tuc | |
is less than 10 times larger than the number of qLMXBs in | |
47 Tuc, indicating that for typical inferred lifetimes of | |
10 and 1 Gyr, respectively, their birthrates are | |
comparable.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005ApJ...622..556H}, | |
Doi = {10.1086/427795}, | |
Eprint = {astro-ph/0412137}, | |
Keywords = {Accretion, Accretion Disks, Stars: Binaries: Close, Stars: | |
Binaries: Eclipsing, Galaxy: Globular Clusters: Individual: | |
NGC Number: NGC 104, Stars: Neutron, X-Rays: Binaries}, | |
Owner = {aleksey}, | |
Timestamp = {2018.01.02} | |
} | |
@Article{heinke+2005, | |
Title = {{A Deep Chandra Survey of the Globular Cluster 47 Tucanae: | |
Catalog of Point Sources}}, | |
Author = {{Heinke}, C.~O. and {Grindlay}, J.~E. and {Edmonds}, P.~D. | |
and {Cohn}, H.~N. and {Lugger}, P.~M. and {Camilo}, F. and | |
{Bogdanov}, S. and {Freire}, P.~C.}, | |
Journal = {\apj}, | |
Year = {2005}, | |
Month = jun, | |
Pages = {796-824}, | |
Volume = {625}, | |
Abstract = {We have detected 300 X-ray sources within the half-mass | |
radius (2.79 arcmin) of the globular cluster 47 Tucanae in | |
a deep (281 ks) Chandra exposure. We perform photometry and | |
simple spectral fitting for our detected sources and | |
construct luminosity functions, X-ray color-magnitude, and | |
color-color diagrams. Eighty-seven X-ray sources show | |
variability on timescales from hours to years. Thirty-one | |
of the new X-ray sources are identified with | |
chromospherically active binaries from the catalogs of | |
Albrow and coworkers. The radial distributions of detected | |
sources imply that roughly 70 are background sources of | |
some kind. The radial distribution of the known millisecond | |
pulsar (MSP) systems is consistent with that expected from | |
mass segregation, if the average neutron star mass is | |
1.39+/-0.19 Msolar. Most source spectra are well fitted by | |
thermal plasma models, except for quiescent low-mass X-ray | |
binaries (qLMXBs; containing accreting neutron stars) and | |
MSPs. We identify three new candidate qLMXBs with | |
relatively low X-ray luminosities. One of the brightest | |
cataclysmic variables (CVs; X10) shows evidence (a 4.7 hr | |
period pulsation and strong soft X-ray emission) for a | |
magnetically dominated accretion flow as in AM Her systems. | |
Most of the bright CVs require intrinsic NH columns of | |
order 1021 cm-2, suggesting a possible DQ Her nature. A | |
group of X-ray sources associated with bright (sub)giant | |
stars also requires intrinsic absorption. By comparing the | |
X-ray colors, luminosities, variability, and quality of | |
spectral fits of the detected MSPs to those of unidentified | |
sources, we estimate that a total of ~25 MSPs exist in 47 | |
Tuc (<60 at 95% confidence), regardless of their radio | |
beaming fraction. We estimate that the total number of | |
neutron stars in 47 Tuc is of order 300, reducing the | |
discrepancy between theoretical neutron star retention | |
rates and observed neutron star populations in globular | |
clusters. Comprehensive tables of source properties and | |
simple spectral fits are provided electronically.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005ApJ...625..796H}, | |
Doi = {10.1086/429899}, | |
Eprint = {astro-ph/0503132}, | |
Keywords = {Galaxy: Globular Clusters: Individual: NGC Number: NGC | |
104, Stars: Novae, Cataclysmic Variables, Stars: Pulsars: | |
General, Stars: Neutron, X-Rays: Binaries}, | |
Owner = {aleksey}, | |
Timestamp = {2017.12.30} | |
} | |
@Article{heinke+2003, | |
Title = {{Analysis of the Quiescent Low-Mass X-Ray Binary | |
Population in Galactic Globular Clusters}}, | |
Author = {{Heinke}, C.~O. and {Grindlay}, J.~E. and {Lugger}, P.~M. | |
and {Cohn}, H.~N. and {Edmonds}, P.~D. and {Lloyd}, D.~A. | |
and {Cool}, A.~M. }, | |
Journal = {\apj}, | |
Year = {2003}, | |
Month = nov, | |
Pages = {501-515}, | |
Volume = {598}, | |
Abstract = {Quiescent low-mass X-ray binaries (qLMXBs) containing | |
neutron stars have been identified in several globular | |
clusters using Chandra or XMM X-ray observations, via their | |
distinctive soft thermal spectra. We report a complete | |
census of the qLMXB population in these clusters, | |
identifying three additional probable qLMXBs in NGC 6440. | |
We conduct several analyses of the qLMXB population and | |
compare it with the harder, primarily cataclysmic variable | |
(CV), population of low-luminosity X-ray sources with | |
1031ergss-1<LX<1032.5 ergs s-1. The radial distribution of | |
our qLMXB sample suggests an average system mass of | |
1.5+0.3-0.2 Msolar, consistent with a neutron star and | |
low-mass companion. Spectral analysis reveals that no | |
globular cluster qLMXBs, other than the transient in NGC | |
6440, require an additional hard power-law component, as | |
often observed in field qLMXBs. We identify an empirical | |
lower luminosity limit of ~1032 ergs s-1 among globular | |
cluster qLMXBs. The bolometric luminosity range of qLMXBs | |
implies (in the deep crustal heating model of Brown and | |
collaborators) low time-averaged mass-transfer rates, below | |
the disk stability criterion. The X-ray luminosity | |
functions of the CV populations alone in NGC 6397 and 47 | |
Tuc are shown to differ. The distribution of qLMXBs among | |
globular clusters is consistent with their dynamical | |
formation by either tidal capture or exchange encounters, | |
allowing us to estimate that 7 times more qLMXBs than | |
bright LMXBs reside in globular clusters. The distribution | |
of harder sources (primarily CVs) has a weaker dependence | |
on density than that of the qLMXBs. Finally, we discuss | |
possible effects of core collapse and globular cluster | |
destruction on X-ray source populations.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2003ApJ...598..501H}, | |
Doi = {10.1086/378885}, | |
Eprint = {astro-ph/0305445}, | |
Keywords = {Galaxy: Globular Clusters: General, Galaxy: Globular | |
Clusters: Individual: NGC Number: NGC 6440, Stars: Novae, | |
Cataclysmic Variables, Stars: Neutron, Stellar Dynamics, | |
X-Rays: Binaries}, | |
Owner = {aleksey}, | |
Timestamp = {2018.01.04} | |
} | |
@Article{heinke+2006, | |
Title = {{Faint X-Ray Sources in the Globular Cluster Terzan 5}}, | |
Author = {{Heinke}, C.~O. and {Wijnands}, R. and {Cohn}, H.~N. and | |
{Lugger}, P.~M. and {Grindlay}, J.~E. and {Pooley}, D. and | |
{Lewin}, W.~H.~G.}, | |
Journal = {\apj}, | |
Year = {2006}, | |
Month = nov, | |
Pages = {1098-1111}, | |
Volume = {651}, | |
Abstract = {We report our analysis of a Chandra X-ray observation of | |
the rich globular cluster Terzan 5, in which we detect 50 | |
sources to a limiting 1.0-6 keV X-ray luminosity of 3?031 | |
ergs s-1 within the half-mass radius of the cluster. | |
Thirty-three of these have LX>1032 ergs s-1, the largest | |
number yet seen in any globular cluster. In addition to the | |
quiescent low-mass X-ray binary (LMXB; identified by | |
Wijnands et al.), another 12 relatively soft sources may be | |
quiescent LMXBs. We compare the X-ray colors of the harder | |
sources in Terzan 5 to the Galactic center sources studied | |
by Muno and collaborators and find the Galactic center | |
sources to have harder X-ray colors, indicating a possible | |
difference in the populations. We cannot clearly identify a | |
metallicity dependence in the production of low-luminosity | |
X-ray binaries in Galactic globular clusters, but a | |
metallicity dependence of the form suggested by Jord? et | |
al. for extragalactic LMXBs is consistent with our data.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006ApJ...651.1098H}, | |
Doi = {10.1086/507884}, | |
Eprint = {astro-ph/0606253}, | |
Keywords = {Galaxy: Globular Clusters: Individual: Name: Terzan 5, | |
Stars: Novae, Cataclysmic Variables, Stars: Neutron, | |
X-Rays: Binaries}, | |
Owner = {aleksey}, | |
Timestamp = {2018.01.02} | |
} | |
@Article{henon1969, | |
Title = {{Rates of Escape from Isolated Clusters with an Arbitrary | |
Mass Distribution}}, | |
Author = {{Henon}, M.}, | |
Journal = {\aap}, | |
Year = {1969}, | |
Month = jun, | |
Pages = {151}, | |
Volume = {2}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1969A%26A.....2..151H} | |
} | |
@Article{hernquist1989, | |
Title = {{Tidal triggering of starbursts and nuclear activity in | |
galaxies}}, | |
Author = {{Hernquist}, L.}, | |
Journal = {\nat}, | |
Year = {1989}, | |
Month = aug, | |
Pages = {687-691}, | |
Volume = {340}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1989Natur.340..687H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1038/340687a0}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1038/340687a0}, | |
Keywords = {ACTIVE GALACTIC NUCLEI, BLACK HOLES (ASTRONOMY), STAR | |
FORMATION, STARBURST GALAXIES, TIDES, ANGULAR MOMENTUM, | |
INTERSTELLAR GAS, QUASARS, STAR DISTRIBUTION} | |
} | |
@Article{hernquist+1995, | |
Title = {{Excitation of Activity in Galaxies by Minor Mergers}}, | |
Author = {{Hernquist}, L. and {Mihos}, J.~C.}, | |
Journal = {\apj}, | |
Year = {1995}, | |
Month = jul, | |
Pages = {41}, | |
Volume = {448}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1995ApJ...448...41H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/175940}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/175940}, | |
Eprint = {arXiv:astro-ph/9501090}, | |
Keywords = {GALAXIES: ACTIVE, GALAXIES: EVOLUTION, GALAXIES: | |
INTERACTIONS, GALAXIES: ISM, GALAXIES: KINEMATICS AND | |
DYNAMICS, GALAXIES: STARBURST} | |
} | |
@Article{hillas1984, | |
Title = {{The Origin of Ultra-High-Energy Cosmic Rays}}, | |
Author = {{Hillas}, A.~M.}, | |
Journal = {\araa}, | |
Year = {1984}, | |
Pages = {425-444}, | |
Volume = {22}, | |
Abstract = {Contents: (1) Why bother with ultra-high-energy cosmic | |
rays? (2) Observational data: Energy spectrum and | |
composition of high-energy particles. Observed anisotropy | |
of high-energy cosmic rays. Specific identified sources of | |
cosmic rays. (3) Acceleration mechanisms: Problems | |
associated with statistical acceleration. Direct | |
acceleration. Final comments. (4) Propagation of cosmic | |
rays: Propagation from extragalactic sources. Propagation | |
from galactic sources. (5) Conclusions.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1984ARA%26A..22..425H}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1146/annurev.aa.22.090184.002233}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1984ARA%26A..22..425H}, | |
Date-added = {2016-01-19 00:47:13 +0000}, | |
Date-modified = {2016-01-19 00:47:13 +0000}, | |
Doi = {10.1146/annurev.aa.22.090184.002233} | |
} | |
@Article{hills1988, | |
Title = {{Hyper-velocity and tidal stars from binaries disrupted by a massive Galactic black hole}}, | |
Author = {{Hills}, J.~G.}, | |
Journal = {\nat}, | |
Year = {1988}, | |
Month = feb, | |
Pages = {687-689}, | |
Volume = {331}, | |
Abstract = {A close but newtonian encounter between a tightly bound binary and a 106M_sun; black hole causes one binary component to become bound to the black hole and the other to be ejected at up to 4,000 km s-1. The discovery of even one such hyper-velocity star coming from the Galactic centre would be nearly definitive evidence for a massive black hole. The new companion of the black hole has a high orbital velocity which increases further as its orbit shrinks by tidal dissipation. The gravitational energy released by the orbit shrinkage of such a tidal star can be comparable to its total nuclear energy release.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1988Natur.331..687H}, | |
Doi = {10.1038/331687a0}, | |
Keywords = {Binary Stars, Black Holes (Astronomy), Gravitational Effects, Milky Way Galaxy, Stellar Orbits, Companion Stars, Ejection, Stellar Evolution}, | |
Owner = {aleksey}, | |
Timestamp = {2018.05.30} | |
} | |
@Article{hills1975, | |
Title = {{Possible power source of Seyfert galaxies and QSOs}}, | |
Author = {{Hills}, J.~G.}, | |
Journal = {\nat}, | |
Year = {1975}, | |
Month = mar, | |
Pages = {295-298}, | |
Volume = {254}, | |
Abstract = {The possible presence of massive black holes in the nuclei | |
of galaxies has been suggested many times. In addition, | |
there is considerable observational evidence for high | |
stellar densities in these nuclei. I show that the tidal | |
breakup of stars passing within the Roche limit of a black | |
hole initiates a chain of events that may explain many of | |
the observed principal characteristics of QSOs and the | |
nuclei of Seyfert galaxies.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1975Natur.254..295H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1038/254295a0}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1975Natur.254..295H}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1038/254295a0}, | |
Keywords = {Black Holes (Astronomy), Mass Transfer, Quasars, Seyfert | |
Galaxies, Galactic Nuclei, Gas Flow, Roche Limit, Stellar | |
Mass, Stellar Mass Ejection} | |
} | |
@Article{hirata+2010, | |
Title = {{Reducing the weak lensing noise for the gravitational | |
wave Hubble diagram using the non-Gaussianity of the | |
magnification distribution}}, | |
Author = {{Hirata}, C.~M. and {Holz}, D.~E. and {Cutler}, C.}, | |
Journal = {\prd}, | |
Year = {2010}, | |
Month = jun, | |
Number = {12}, | |
Pages = {124046}, | |
Volume = {81}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010PhRvD..81l4046H}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1103/PhysRevD.81.124046}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1103/PhysRevD.81.124046}, | |
Eid = {124046}, | |
Eprint = {1004.3988}, | |
Keywords = {Gravitational-wave astrophysics, Dark energy, | |
Gravitational lenses and luminous arcs, Observational | |
cosmology}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{hirose+2009a, | |
Title = {{Turbulent Stresses in Local Simulations of | |
Radiation-dominated Accretion Disks, and the Possibility of | |
the Lightman-Eardley Instability}}, | |
Author = {{Hirose}, S. and {Blaes}, O. and {Krolik}, J.~H.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = oct, | |
Pages = {781-788}, | |
Volume = {704}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...704..781H}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/704/1/781}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1088/0004-637X/704/1/781}, | |
Eprint = {0908.1117}, | |
Keywords = {accretion, accretion disks, instabilities, MHD, X-rays: | |
binaries}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{hirose+2009, | |
Title = {{Radiation-Dominated Disks are Thermally Stable}}, | |
Author = {{Hirose}, S. and {Krolik}, J.~H. and {Blaes}, O.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = jan, | |
Pages = {16-31}, | |
Volume = {691}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...691...16H}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/691/1/16}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1088/0004-637X/691/1/16}, | |
Eprint = {0809.1708}, | |
Keywords = {accretion, accretion disks, instabilities, MHD, radiative | |
transfer} | |
} | |
@Article{ho2009, | |
Title = {{Radiatively Inefficient Accretion in Nearby Galaxies}}, | |
Author = {{Ho}, L.~C.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = jul, | |
Pages = {626-637}, | |
Volume = {699}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...699..626H}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/699/1/626}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1088/0004-637X/699/1/626}, | |
Eprint = {0906.4104}, | |
Keywords = {black hole physics, galaxies: active, galaxies: nuclei, | |
galaxies: Seyfert}, | |
Primaryclass = {astro-ph.GA} | |
} | |
@Article{ho2009a, | |
Title = {{Origin and Dynamical Support of Ionized Gas in Galaxy | |
Bulges}}, | |
Author = {{Ho}, L.~C.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = jul, | |
Pages = {638-648}, | |
Volume = {699}, | |
Abstract = {We combine ionized gas ([N II] lambda6583) and stellar | |
central velocity dispersions for a sample of 345 galaxies, | |
with and without active galactic nuclei (AGNs), to study | |
the dynamical state of the nuclear gas and its physical | |
origin. The gas dispersions strongly correlate with the | |
stellar dispersions over the velocity range of sigma ≈ | |
30-350 km s-1, such that sigma g /sigma* ≈ 0.6-1.4, with | |
an average value of 0.80. These results are independent of | |
Hubble type (for galaxies from E to Sbc), the presence or | |
absence of a bar, or local galaxy environment. For galaxies | |
of type Sc and later and that have sigma* lsim 40 km s-1, | |
the gas seems to have a minimum threshold of sigma g ≈ 30 | |
km s-1, such that sigma g /sigma* always exceeds 1. Within | |
the sample of AGNs, sigma g /sigma* increases with nuclear | |
luminosity or Eddington ratio, a possible manifestation of | |
AGN feedback associated with accretion disk winds or | |
outflows. This extra source of nongravitational line | |
broadening should be removed when trying to use sigma g to | |
estimate sigma*. We show that the mass budget of the | |
narrow-line region (NLR) can be accounted for by mass loss | |
from evolved stars. The kinematics of the gas, dominated by | |
random motions, largely reflect the velocity field of the | |
hot gas in the bulge. Lastly, we offer a simple explanation | |
for the correlation between line width and line luminosity | |
observed in the NLR of AGNs.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...699..638H}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/0906.4103}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/699/1/638}, | |
Bdsk-url-2 = {http://arXiv.org/abs/0906.4103}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2009ApJ...699..638H}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1088/0004-637X/699/1/638}, | |
Eprint = {0906.4103}, | |
Keywords = {galaxies: active, galaxies: bulges, galaxies: ISM, | |
galaxies: kinematics and dynamics, galaxies: nuclei, | |
galaxies: Seyfert}, | |
Primaryclass = {astro-ph.GA} | |
} | |
@Article{ho2008, | |
Title = {{Nuclear Activity in Nearby Galaxies}}, | |
Author = {{Ho}, L.~C.}, | |
Journal = {\araa}, | |
Year = {2008}, | |
Month = sep, | |
Pages = {475-539}, | |
Volume = {46}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2008ARA%26A..46..475H}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1146/annurev.astro.45.051806.110546}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1146/annurev.astro.45.051806.110546}, | |
Eprint = {0803.2268} | |
} | |
@Article{ho1999, | |
Title = {{The Spectral Energy Distributions of Low-Luminosity | |
Active Galactic Nuclei}}, | |
Author = {{Ho}, L.~C.}, | |
Journal = {\apj}, | |
Year = {1999}, | |
Month = may, | |
Pages = {672-682}, | |
Volume = {516}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1999ApJ...516..672H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/307137}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/307137}, | |
Eprint = {astro-ph/9905012}, | |
Keywords = {GALAXIES: ACTIVE, GALAXIES: NUCLEI, GALAXIES: SEYFERT, | |
Galaxies: Active, Galaxies: Nuclei, Galaxies: Seyfert} | |
} | |
@Article{hobbs+2005, | |
Title = {{A statistical study of 233 pulsar proper motions}}, | |
Author = {{Hobbs}, G. and {Lorimer}, D.~R. and {Lyne}, A.~G. and | |
{Kramer}, M.}, | |
Journal = {\mnras}, | |
Year = {2005}, | |
Month = jul, | |
Pages = {974-992}, | |
Volume = {360}, | |
Abstract = {We present and analyse a catalogue of 233 pulsars with | |
proper motion measurements. The sample contains a wide | |
variety of pulsars including recycled objects and those | |
associated with globular clusters or supernova remnants. | |
After taking the most precise proper motions for those | |
pulsars for which multiple measurements are available, the | |
majority of the proper motions (58 per cent) are derived | |
from pulsar timing methods, 41 per cent using | |
interferometers and the remaining 1 per cent using optical | |
telescopes. Many of the one-dimensional (1D) and | |
two-dimensional (2D) speeds (referring to speeds measured | |
in one coordinate only and the magnitudes of the transverse | |
velocities, respectively) derived from these measurements | |
are somewhat lower than earlier estimates because of the | |
use of the most recent electron density model in | |
determining pulsar distances. The mean 1D speeds for the | |
normal and recycled pulsars are 152(10) and 54(6)kms-1, | |
respectively. The corresponding mean 2D speeds are 246(22) | |
and 87(13)kms-1. PSRs B2011+38 and B2224+64 have the | |
highest inferred 2D speeds of ~1600 km s-1. We study the | |
mean speeds for different subsamples and find that, in | |
general, they agree with previous results. Applying a novel | |
deconvolution technique to the sample of 73 pulsars with | |
characteristic ages less than 3Myr, we find the mean | |
three-dimensional (3D) pulsar birth velocity to be | |
400(40)kms-1. The distribution of velocities is well | |
described by a Maxwellian distribution with 1D rms sigma= | |
265 km s-1. There is no evidence for a bimodal velocity | |
distribution. The proper motions for PSRs B1830-08 and | |
B2334+61 are consistent with their proposed associations | |
with the supernova remnants W41 and G114.3+0.3, | |
respectively.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005MNRAS.360..974H}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/0504584}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2005.09087.x}, | |
Bdsk-url-2 = {http://arxiv.org/abs/astro-ph/0504584}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2005MNRAS.360..974H}, | |
Date-added = {2017-05-29 19:28:59 +0000}, | |
Date-modified = {2017-05-29 19:28:59 +0000}, | |
Doi = {10.1111/j.1365-2966.2005.09087.x}, | |
Eprint = {astro-ph/0504584}, | |
Keywords = {stars: kinematics, pulsars: general} | |
} | |
@Article{holoien+2016, | |
Title = {{ASASSN-15oi: a rapidly evolving, luminous tidal disruption event at 216 Mpc}}, | |
Author = {{Holoien}, T.~W.-S. and {Kochanek}, C.~S. and {Prieto}, J.~L. and {Grupe}, D. and {Chen}, P. and {Godoy-Rivera}, D. and {Stanek}, K.~Z. and {Shappee}, B.~J. and {Dong}, S. and {Brown}, J.~S. and {Basu}, U. and {Beacom}, J.~F. and {Bersier}, D. and {Brimacombe}, J. and {Carlson}, E.~K. and {Falco}, E. and {Johnston}, E. and {Madore}, B.~F. and {Pojmanski}, G. and {Seibert}, M.}, | |
Journal = {\mnras}, | |
Year = {2016}, | |
Month = dec, | |
Pages = {3813-3828}, | |
Volume = {463}, | |
Abstract = {We present ground-based and Swift photometric and spectroscopic observations of the tidal disruption event (TDE) ASASSN-15oi, discovered at the centre of 2MASX J20390918-3045201 (d ? 216 Mpc) by the All-Sky Automated Survey for SuperNovae. The source peaked at a bolometric luminosity of L ? 1.3 × 1044 erg s-1 and radiated a total energy of E ? 6.6 × 1050 erg over the first ?3.5 months of observations. The early optical/UV emission of the source can be fit by a blackbody with temperature increasing from T ? 2 × 104 K to T ? 4 × 104 K while the luminosity declines from L ? 1.3 × 1044 erg s-1 to L ? 2.3 × 1043 erg s-1, requiring the photosphere to be shrinking rapidly. The optical/UV luminosity decline during this period is most consistent with an exponential decline, L? e^{-(t-t_0)/?}, with ? ? 46.5 d for t0 ? 57241.6 (MJD), while a power-law decline of L ? (t - t0)-? with t0 ? 57 212.3 and ? = 1.62 provides a moderately worse fit. ASASSN-15oi also exhibits roughly constant soft X-ray emission that is significantly weaker than the optical/UV emission. Spectra of the source show broad helium emission lines and strong blue continuum emission in early epochs, although these features fade rapidly and are not present ?3 months after discovery. The early spectroscopic features and colour evolution of ASASSN-15oi are consistent with a TDE, but the rapid spectral evolution is unique among optically selected TDEs.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016MNRAS.463.3813H}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1093/mnras/stw2272}, | |
Eprint = {1602.01088}, | |
Keywords = {accretion, accretion discs, black hole physics, galaxies: nuclei}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2018.06.11} | |
} | |
@Article{holoien+2016a, | |
Title = {{Six months of multiwavelength follow-up of the tidal | |
disruption candidate ASASSN-14li and implied TDE rates from | |
ASAS-SN}}, | |
Author = {{Holoien}, T.~W.-S. and {Kochanek}, C.~S. and {Prieto}, | |
J.~L. and {Stanek}, K.~Z. and {Dong}, S. and {Shappee}, | |
B.~J. and {Grupe}, D. and {Brown}, J.~S. and {Basu}, U. and | |
{Beacom}, J.~F. and {Bersier}, D. and {Brimacombe}, J. and | |
{Danilet}, A.~B. and {Falco}, E. and {Guo}, Z. and {Jose}, | |
J. and {Herczeg}, G.~J. and {Long}, F. and {Pojmanski}, G. | |
and {Simonian}, G.~V. and {Szczygie{\l}}, D.~M. and | |
{Thompson}, T.~A. and {Thorstensen}, J.~R. and {Wagner}, | |
R.~M. and {Wo{\'z}niak}, P.~R.}, | |
Journal = {\mnras}, | |
Year = {2016}, | |
Month = jan, | |
Pages = {2918-2935}, | |
Volume = {455}, | |
Abstract = {We present ground-based and Swift photometric and | |
spectroscopic observations of the candidate tidal | |
disruption event (TDE) ASASSN-14li, found at the centre of | |
PGC 043234 (d ~= 90 Mpc) by the All-Sky Automated Survey | |
for SuperNovae (ASAS-SN). The source had a peak bolometric | |
luminosity of L ~= 1044 erg s-1 and a total integrated | |
energy of E ~= 7 × 1050 erg radiated over the ˜6 months | |
of observations presented. The UV/optical emission of the | |
source is well fitted by a blackbody with roughly constant | |
temperature of T ˜ 35 000 K, while the luminosity declines | |
by roughly a factor of 16 over this time. The optical/UV | |
luminosity decline is broadly consistent with an | |
exponential decline, L∠e^{-t/t_0}, with t0 ~= 60 d. | |
ASASSN-14li also exhibits soft X-ray emission comparable in | |
luminosity to the optical and UV emission but declining at | |
a slower rate, and the X-ray emission now dominates. | |
Spectra of the source show broad Balmer and helium lines in | |
emission as well as strong blue continuum emission at all | |
epochs. We use the discoveries of ASASSN-14li and | |
ASASSN-14ae to estimate the TDE rate implied by ASAS-SN, | |
finding an average rate of r ~= 4.1 × 10-5 yr-1 per galaxy | |
with a 90 per cent confidence interval of (2.2-17.0) × | |
10-5 yr-1 per galaxy. ASAS-SN found roughly 1 TDE for every | |
70 Type Ia supernovae in 2014, a rate that is much higher | |
than that of other surveys.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016MNRAS.455.2918H}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1507.01598}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stv2486}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1507.01598}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2016MNRAS.455.2918H}, | |
Date-added = {2016-04-17 23:31:31 +0000}, | |
Date-modified = {2016-04-17 23:31:32 +0000}, | |
Doi = {10.1093/mnras/stv2486}, | |
Eprint = {1507.01598}, | |
Keywords = {accretion, accretion discs, black hole physics, galaxies: | |
nuclei}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{holoien+2014, | |
Title = {{ASASSN-14ae: a tidal disruption event at 200 Mpc}}, | |
Author = {{Holoien}, T.~W.-S. and {Prieto}, J.~L. and {Bersier}, D. | |
and {Kochanek}, C.~S. and {Stanek}, K.~Z. and {Shappee}, | |
B.~J. and {Grupe}, D. and {Basu}, U. and {Beacom}, J.~F. | |
and {Brimacombe}, J. and {Brown}, J.~S. and {Davis}, A.~B. | |
and {Jencson}, J. and {Pojmanski}, G. and {Szczygie{\l}}, | |
D.~M.}, | |
Journal = {\mnras}, | |
Year = {2014}, | |
Month = dec, | |
Pages = {3263-3277}, | |
Volume = {445}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014MNRAS.445.3263H}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1405.1417}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stu1922}, | |
Date-added = {2015-09-04 17:25:13 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1093/mnras/stu1922}, | |
Eprint = {1405.1417}, | |
Keywords = {accretion, accretion discs, black hole physics, galaxies: | |
nuclei} | |
} | |
@Article{holz+2005, | |
Title = {{Using Gravitational-Wave Standard Sirens}}, | |
Author = {{Holz}, D.~E. and {Hughes}, S.~A.}, | |
Journal = {\apj}, | |
Year = {2005}, | |
Month = aug, | |
Pages = {15-22}, | |
Volume = {629}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005ApJ...629...15H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/431341}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/431341}, | |
Eprint = {arXiv:astro-ph/0504616}, | |
Keywords = {Black Hole Physics, Cosmology: Observations, Cosmology: | |
Theory, Galaxies: Nuclei, Cosmology: Gravitational Lensing, | |
Gravitational Waves} | |
} | |
@Article{holzer+1970, | |
Title = {{The Theory of Stellar Winds and Related Flows}}, | |
Author = {{Holzer}, T.~E. and {Axford}, W.~I.}, | |
Journal = {\araa}, | |
Year = {1970}, | |
Pages = {31}, | |
Volume = {8}, | |
Abstract = {Not Available}, | |
Adscomment = {AAA ID. AAA004.064.030}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1970ARA%26A...8...31H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1146/annurev.aa.08.090170.000335}, | |
Bdsk-url-2 = {http://adsabs.harvard.edu/abs/1970ARA%26A...8...31H}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1146/annurev.aa.08.090170.000335} | |
} | |
@Article{holzwarth+2007, | |
Title = {{Theoretical mass loss rates of cool main-sequence | |
stars}}, | |
Author = {{Holzwarth}, V. and {Jardine}, M.}, | |
Journal = {\aap}, | |
Year = {2007}, | |
Month = feb, | |
Pages = {11-21}, | |
Volume = {463}, | |
Abstract = {Context: The stellar mass loss rate is important for the | |
rotational evolution of a star and for its interaction with | |
the circumstellar environment. The analysis of astrospheric | |
absorption features enables an empirical determination of | |
mass loss rates of cool stars other than the Sun. Aims: We | |
develop a model for the wind properties of cool | |
main-sequence stars, which comprises their wind ram | |
pressures, mass fluxes, and terminal wind velocities. | |
Methods: The wind properties are determined through a | |
polytropic magnetised wind model, assuming power laws for | |
the dependence of the thermal and magnetic wind parameters | |
on the stellar rotation rate. We use the empirical data to | |
constrain theoretical wind scenarios, which are | |
characterised by different rates of increase of the wind | |
temperature, wind density, and magnetic field strength. | |
Results: Scenarios based on moderate rates of increase | |
yield wind ram pressures in agreement with most empirical | |
constraints, but cannot account for some moderately | |
rotating targets, whose high apparent mass loss rates are | |
inconsistent with observed coronal X-ray and magnetic | |
properties. For fast magnetic rotators, the | |
magneto-centrifugal driving of the outflow can produce | |
terminal wind velocities far in excess of the surface | |
escape velocity. Disregarding this aspect in the analyses | |
of wind ram pressures leads to overestimations of stellar | |
mass loss rates. The predicted mass loss rates of cool | |
main-sequence stars do not exceed about ten times the solar | |
value. Conclusions: .Our results are in contrast with | |
previous investigations, which found a strong increase of | |
the stellar mass loss rates with the coronal X-ray flux. | |
Owing to the weaker dependence, we expect the impact of | |
stellar winds on planetary atmospheres to be less severe | |
and the detectability of magnetospheric radio emission to | |
be lower then previously suggested. Considering the | |
rotational evolution of a 1 {M&sun;} star, the mass loss | |
rates and the wind ram pressures are highest during the | |
pre-main sequence phase.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007A%26A...463...11H}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0611430}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1051/0004-6361:20066486}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0611430}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2007A%26A...463...11H}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1051/0004-6361:20066486}, | |
Eprint = {astro-ph/0611430}, | |
Keywords = {stars: winds, outflows, stars: mass-loss, stars: magnetic, | |
fields, stars: late-type, stars: planetary systems} | |
} | |
@Article{hopkins+2006, | |
Title = {{A Unified, Merger-driven Model of the Origin of | |
Starbursts, Quasars, the Cosmic X-Ray Background, | |
Supermassive Black Holes, and Galaxy Spheroids}}, | |
Author = {Hopkins, P.\~{}F. and Hernquist, L and Cox, T.\~{}J. and | |
{Di Matteo}, T and Robertson, B and Springel, V}, | |
Journal = {\apjs}, | |
Year = {2006}, | |
Month = mar, | |
Pages = {1--49}, | |
Volume = {163}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/499298}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/499298}, | |
Keywords = {Galaxies: Active, Galaxies: Evolution, Galaxies: Nuclei, | |
Galaxies: Quasars: General,Cosmology: Theory} | |
} | |
@Article{hopkins+2007a, | |
Title = {{Observational Evidence for the Coevolution of Galaxy | |
Mergers, Quasars, and the Blue/Red Galaxy Transition}}, | |
Author = {{Hopkins}, P.~F. and {Bundy}, K. and {Hernquist}, L. and | |
{Ellis}, R.~S.}, | |
Journal = {\apj}, | |
Year = {2007}, | |
Month = apr, | |
Pages = {976-996}, | |
Volume = {659}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...659..976H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/512091}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/512091}, | |
Eprint = {arXiv:astro-ph/0601621}, | |
Keywords = {Cosmology: Theory, Galaxies: Active, Galaxies: Evolution, | |
Galaxies: Quasars: General} | |
} | |
@Article{hopkins+2008, | |
Title = {{A Cosmological Framework for the Co-Evolution of Quasars, | |
Supermassive Black Holes, and Elliptical Galaxies. I. | |
Galaxy Mergers and Quasar Activity}}, | |
Author = {{Hopkins}, P.~F. and {Hernquist}, L. and {Cox}, T.~J. and | |
{Kere{\v s}}, D.}, | |
Journal = {\apjs}, | |
Year = {2008}, | |
Month = apr, | |
Pages = {356-389}, | |
Volume = {175}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2008ApJS..175..356H}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/524362}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/524362}, | |
Eprint = {0706.1243}, | |
Keywords = {Cosmology: Theory, Galaxies: Active, Galaxies: Evolution, | |
Galaxies: Quasars: General} | |
} | |
@Article{hopkins&quataert2010, | |
Title = {{How do massive black holes get their gas?}}, | |
Author = {{Hopkins}, P.~F. and {Quataert}, E.}, | |
Journal = {\mnras}, | |
Year = {2010}, | |
Month = sep, | |
Pages = {1529-1564}, | |
Volume = {407}, | |
Abstract = {We use multiscale smoothed particle hydrodynamic simulations to study the inflow of gas from galactic scales (~10kpc) down to <~ 0.1pc, at which point the gas begins to resemble a traditional, Keplerian accretion disc. The key ingredients of the simulations are gas, stars, black holes (BHs), self-gravity, star formation and stellar feedback (via a subgrid model); BH feedback is not included. We use ~100 simulations to survey a large parameter space of galaxy properties and subgrid models for the interstellar medium physics. We generate initial conditions for our simulations of galactic nuclei (<~ 300pc) using galaxy-scale simulations, including both major galaxy mergers and isolated bar-(un)stable disc galaxies. For sufficiently gas-rich, disc-dominated systems, we find that a series of gravitational instabilities generates large accretion rates of up to ~ 1-10 Msolar yr-1 on to the BH (i.e. at <~ 0.1pc) this is comparable to what is needed to fuel the most luminous quasars. The BH accretion rate is highly time variable for a given set of conditions in the galaxy at ~kpc. At radii of >rsim 10 pc, our simulations resemble the `bars-within-bars' model of Shlosman et al., but we show that the gas can have a diverse array of morphologies, including spirals, rings, clumps and bars; the duty cycle of these features is modest, complicating attempts to correlate BH accretion with the morphology of gas in galactic nuclei. At ~ 1-10 pc, the gravitational potential becomes dominated by the BH and bar-like modes are no longer present. However, we show that the gas can become unstable to a standing, eccentric disc or a single-armed spiral mode (m = 1), in which the stars and gas precess at different rates, driving the gas to sub-pc scales (again for sufficiently gas-rich, disc-dominated systems). A proper treatment of this mode requires including star formation and the self-gravity of both the stars and gas (which has not been the case in many previous calculations). Our simulations predict a correlation between the BH accretion rate and the star formation rate at different galactic radii. We find that nuclear star formation is more tightly coupled to active galactic nucleus activity than the global star formation rate of a galaxy, but a reasonable correlation remains even for the latter.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2010MNRAS.407.1529H}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1111/j.1365-2966.2010.17064.x}, | |
Eprint = {0912.3257}, | |
Keywords = {galaxies: active, galaxies: evolution, quasars: general, cosmology: theory}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.CO}, | |
Timestamp = {2018.10.01} | |
} | |
@Article{hopkins+2007, | |
Title = {{An Observational Determination of the Bolometric Quasar | |
Luminosity Function}}, | |
Author = {{Hopkins}, P.~F. and {Richards}, G.~T. and {Hernquist}, | |
L.}, | |
Journal = {\apj}, | |
Year = {2007}, | |
Month = jan, | |
Pages = {731-753}, | |
Volume = {654}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...654..731H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/509629}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/509629}, | |
Eprint = {arXiv:astro-ph/0605678}, | |
Keywords = {Cosmology: Observations, Galaxies: Active, Galaxies: | |
Evolution, Galaxies: Luminosity Function, Mass Function, | |
Infrared: Galaxies, Galaxies: Quasars: General, | |
Ultraviolet: Galaxies, X-Rays: Galaxies} | |
} | |
@Article{hopman2009, | |
Title = {{Binary Dynamics Near a Massive Black Hole}}, | |
Author = {{Hopman}, C.}, | |
Journal = {\apj}, | |
Year = {2009}, | |
Month = aug, | |
Pages = {1933-1951}, | |
Volume = {700}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...700.1933H}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1088/0004-637X/700/2/1933}, | |
Eprint = {0906.0374}, | |
Keywords = {binaries: general, black hole physics, Galaxy: center, | |
stellar dynamics}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.CO}, | |
Timestamp = {2017.12.19} | |
} | |
@Article{hopman&alexander2006, | |
Title = {{Resonant Relaxation near a Massive Black Hole: The | |
Stellar Distribution and Gravitational Wave Sources}}, | |
Author = {{Hopman}, C. and {Alexander}, T.}, | |
Journal = {\apj}, | |
Year = {2006}, | |
Month = jul, | |
Pages = {1152-1163}, | |
Volume = {645}, | |
Abstract = {Resonant relaxation (RR) of orbital angular momenta occurs | |
near massive black holes (MBHs) where the potential is | |
spherical and stellar orbits are nearly Keplerian and so do | |
not precess significantly. The resulting coherent torques | |
efficiently change the magnitude of the angular momenta and | |
rotate the orbital inclination in all directions. As a | |
result, many of the tightly bound stars very near the MBH | |
are rapidly destroyed by falling into the MBH on low | |
angular momentum orbits, while the orbits of the remaining | |
stars are efficiently randomized. We solve numerically the | |
Fokker-Planck equation in energy for the steady state | |
distribution of a single-mass population with an RR sink | |
term. We find that the steady state current of stars, which | |
sustains the accelerated drainage close to the MBH, can be | |
<~10 larger than that due to noncoherent two-body | |
relaxation alone. RR mostly affects tightly bound stars, | |
and so it increases only moderately the total tidal | |
disruption rate, which is dominated by stars originating | |
from less bound orbits farther away. We show that the event | |
rate of gravitational wave (GW) emission from inspiraling | |
stars, originating much closer to the MBH, is dominated by | |
RR dynamics. The GW event rate depends on the uncertain | |
efficiency of RR. The efficiency indicated by the few | |
available simulations implies rates <~10 times higher than | |
those predicted by two-body relaxation, which would improve | |
the prospects of detecting such events by future GW | |
detectors, such as LISA. However, a higher, but still | |
plausible, RR efficiency can lead to the drainage of all | |
tightly bound stars and strong suppression of GW events | |
from inspiraling stars. We apply our results to the | |
Galactic MBH and show that the observed dynamical | |
properties of stars there are consistent with RR.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006ApJ...645.1152H}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/0601161}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/504400}, | |
Bdsk-url-2 = {http://arxiv.org/abs/astro-ph/0601161}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2006ApJ...645.1152H}, | |
Date-added = {2017-08-08 00:57:31 +0000}, | |
Date-modified = {2017-08-08 01:06:40 +0000}, | |
Doi = {10.1086/504400}, | |
Eprint = {astro-ph/0601161}, | |
Keywords = {Black Hole Physics, Galaxy: Center, Gravitational Waves, | |
Stellar Dynamics} | |
} | |
@Article{hopman&alexander2006a, | |
Title = {{The Effect of Mass Segregation on Gravitational Wave | |
Sources near Massive Black Holes}}, | |
Author = {{Hopman}, C. and {Alexander}, T.}, | |
Journal = {\apjl}, | |
Year = {2006}, | |
Month = jul, | |
Pages = {L133-L136}, | |
Volume = {645}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006ApJ...645L.133H}, | |
Doi = {10.1086/506273}, | |
Eprint = {astro-ph/0603324}, | |
Keywords = {Black Hole Physics, Galaxy: Center, Gravitational Waves, | |
Stellar Dynamics}, | |
Owner = {aleksey}, | |
Timestamp = {2017.12.12} | |
} | |
@Article{hubeny+2001, | |
Title = {{Non-LTE Models and Theoretical Spectra of Accretion Disks | |
in Active Galactic Nuclei. IV. Effects of Compton | |
Scattering and Metal Opacities}}, | |
Author = {{Hubeny}, I. and {Blaes}, O. and {Krolik}, J.~H. and | |
{Agol}, E.}, | |
Journal = {\apj}, | |
Year = {2001}, | |
Month = oct, | |
Pages = {680-702}, | |
Volume = {559}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2001ApJ...559..680H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/322344}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/322344}, | |
Eprint = {arXiv:astro-ph/0105507}, | |
Keywords = {Accretion, Accretion Disks, Galaxies: Active, Galaxies: | |
Nuclei, Radiative Transfer} | |
} | |
@Article{hubeny+1998, | |
Title = {{Non-LTE Models and Theoretical Spectra of Accretion Disks | |
in Active Galactic Nuclei. II. Vertical Structure of the | |
Disk}}, | |
Author = {{Hubeny}, I. and {Hubeny}, V.}, | |
Journal = {\apj}, | |
Year = {1998}, | |
Month = oct, | |
Pages = {558-576}, | |
Volume = {505}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1998ApJ...505..558H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/306207}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/306207}, | |
Eprint = {arXiv:astro-ph/9804288}, | |
Keywords = {ACCRETION, ACCRETION DISKS, GALAXIES: ACTIVE, GALAXIES: | |
NUCLEI, RADIATIVE TRANSFER} | |
} | |
@Article{hubeny+1997, | |
Title = {{Non-LTE Models and Theoretical Spectra of Accretion Disks | |
in Active Galactic Nuclei}}, | |
Author = {{Hubeny}, I. and {Hubeny}, V.}, | |
Journal = {\apjl}, | |
Year = {1997}, | |
Month = jul, | |
Pages = {L37}, | |
Volume = {484}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1997ApJ...484L..37H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/310774}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/310774}, | |
Eprint = {arXiv:astro-ph/9705085}, | |
Keywords = {ACCRETION, ACCRETION DISKS, GALAXIES: ACTIVE, GALAXIES: | |
NUCLEI, RADIATIVE TRANSFER} | |
} | |
@Article{hubeny+1995, | |
Title = {{Non-LTE line-blanketed model atmospheres of hot stars. 1: | |
Hybrid complete linearization/accelerated lambda iteration | |
method}}, | |
Author = {{Hubeny}, I. and {Lanz}, T.}, | |
Journal = {\apj}, | |
Year = {1995}, | |
Month = feb, | |
Pages = {875-904}, | |
Volume = {439}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1995ApJ...439..875H}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/175226}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/175226}, | |
Keywords = {HOT STARS, ITERATIVE SOLUTION, NUMERICAL ANALYSIS, | |
RADIATIVE TRANSFER, STELLAR ATMOSPHERES, STELLAR MODELS, | |
ABSORPTIVITY, EQUILIBRIUM EQUATIONS, JACOBI MATRIX METHOD, | |
LINE SPECTRA, LINEARIZATION, NEWTON-RAPHSON METHOD} | |
} | |
@Article{hurley+2000, | |
Title = {{Comprehensive analytic formulae for stellar evolution as | |
a function of mass and metallicity}}, | |
Author = {{Hurley}, J.~R. and {Pols}, O.~R. and {Tout}, C.~A.}, | |
Journal = {\mnras}, | |
Year = {2000}, | |
Month = jul, | |
Pages = {543-569}, | |
Volume = {315}, | |
Abstract = {We present analytic formulae that approximate the | |
evolution of stars for a wide range of mass M and | |
metallicity Z. Stellar luminosity, radius and core mass are | |
given as a function of age, M and Z, for all phases from | |
the zero-age main sequence up to, and including, the | |
remnant stages. For the most part we find continuous | |
formulae accurate to within 5 per cent of detailed models. | |
These formulae are useful for purposes such as population | |
synthesis that require very rapid but accurate evaluation | |
of stellar properties, and in particular for use in | |
combination with N-body codes. We describe a mass-loss | |
prescription that can be used with these formulae, and | |
investigate the resulting stellar remnant distribution.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2000MNRAS.315..543H}, | |
Doi = {10.1046/j.1365-8711.2000.03426.x}, | |
Eprint = {astro-ph/0001295}, | |
Keywords = {METHODS: ANALYTICAL, STARS: EVOLUTION, STARS: FUNDAMENTAL | |
PARAMETERS, STARS: MASS-LOSS, STARS: POPULATION II, | |
GALAXIES: STELLAR CONTENT}, | |
Owner = {aleksey}, | |
Timestamp = {2017.12.25} | |
} | |
@Article{ivanov&novikov2001, | |
Title = {{A New Model of a Tidally Disrupted Star}}, | |
Author = {{Ivanov}, P.~B. and {Novikov}, I.~D.}, | |
Journal = {\apj}, | |
Year = {2001}, | |
Month = mar, | |
Pages = {467-482}, | |
Volume = {549}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2001ApJ...549..467I}, | |
Doi = {10.1086/319050}, | |
Eprint = {astro-ph/0005107}, | |
Keywords = {Black Hole Physics, Celestial Mechanics, Stellar Dynamics, | |
Hydrodynamics}, | |
Owner = {aleksey}, | |
Timestamp = {2017.10.09} | |
} | |
@Article{ivanov+2007, | |
Title = {{Orbital circularisation of white dwarfs and the formation | |
of gravitational radiation sources in star clusters | |
containing an intermediate mass black hole}}, | |
Author = {{Ivanov}, P.~B. and {Papaloizou}, J.~C.~B.}, | |
Journal = {\aap}, | |
Year = {2007}, | |
Month = dec, | |
Pages = {121-135}, | |
Volume = {476}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007A%26A...476..121I}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1051/0004-6361:20077105}, | |
Eprint = {0709.0480}, | |
Keywords = {black hole physics, gravitational waves, stellar dynamics, | |
white dwarfs, galaxies: star clusters, stars: | |
oscillations} | |
} | |
@Article{ivanov+1999, | |
Title = {{The evolution of a supermassive binary caused by an | |
accretion disc}}, | |
Author = {Ivanov, P B and Papaloizou, J C B and Polnarev, A G}, | |
Journal = {\mnras}, | |
Year = {1999}, | |
Month = jul, | |
Pages = {79}, | |
Volume = {307}, | |
Abstract = {The interaction between a massive binary and a | |
non-self-gravitating circumbinary accretion disc is | |
considered. The shape of the stationary twisted disc | |
produced by the binary is calculated. It is shown that the | |
inner part of the disc must lie in the binary orbital plane | |
for any value of the viscosity. When the inner disc | |
mid-plane is aligned with the binary orbital plane on the | |
scales of interest and it rotates in the same sense as the | |
binary, the modification to the disc structure and the rate | |
of decay of the binary orbit, assumed circular, caused by | |
tidal exchange of angular momentum with the disc, are | |
calculated. It is shown that the modified disc structure is | |
well described by a self-similar solution of the non-linear | |
diffusion equation governing the evolution of the disc | |
surface density. The calculated time-scale for decay of the | |
binary orbit is always smaller than the `accretion' | |
time-scale t\_acc=m/Msolar (m is the mass of the secondary | |
component, and Msolar is the disc accretion rate), and is | |
determined by the ratio of the secondary mass m, assumed to | |
be much smaller than the primary mass, the disc mass inside | |
the initial binary orbit, and the form of viscosity in the | |
disc.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=1999MNRAS.307...79I%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1046/j.1365-8711.1999.02623.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1046/j.1365-8711.1999.02623.x}, | |
Keywords = {BLACK HOLE PHYSICS, GALAXIES: INTERACTIONS, HYDRODYNAMICS, | |
accretion discs, galaxies: nuclei,Accretion; Untitled; | |
Untitled1}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=1999MNRAS.307...79I\&link\_type=ABSTRACT} | |
} | |
@Article{ivanova+2005, | |
Title = {{The evolution of binary fractions in globular clusters}}, | |
Author = {{Ivanova}, N. and {Belczynski}, K. and {Fregeau}, J.~M. | |
and {Rasio}, F.~A.}, | |
Journal = {\mnras}, | |
Year = {2005}, | |
Month = apr, | |
Pages = {572-584}, | |
Volume = {358}, | |
Abstract = {We study the evolution of binary stars in globular | |
clusters using a new Monte Carlo approach combining a | |
population synthesis code (STARTRACK) and a simple | |
treatment of dynamical interactions in the dense cluster | |
core using a new tool for computing three- and four-body | |
interactions (FEWBODY). We find that the combination of | |
stellar evolution and dynamical interactions (binary-single | |
and binary-binary) leads to a rapid depletion of the binary | |
population in the cluster core. The maximum binary fraction | |
today in the core of a typical dense cluster such as 47 | |
Tuc, assuming an initial binary fraction of 100 per cent, | |
is only ~5-10 per cent. We show that this is in good | |
agreement with recent Hubble Space Telescope observations | |
of close binaries in the core of 47 Tuc, provided that a | |
realistic distribution of binary periods is used to | |
interpret the results. Our findings also have important | |
consequences for the dynamical modelling of globular | |
clusters, suggesting that `realistic models' should | |
incorporate much larger initial binary fractions than has | |
usually been the case in the past.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005MNRAS.358..572I}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/0501131}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2005.08804.x}, | |
Bdsk-url-2 = {http://arxiv.org/abs/astro-ph/0501131}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2005MNRAS.358..572I}, | |
Date-added = {2017-08-08 01:32:03 +0000}, | |
Date-modified = {2017-08-08 01:32:08 +0000}, | |
Doi = {10.1111/j.1365-2966.2005.08804.x}, | |
Eprint = {astro-ph/0501131}, | |
Keywords = {stellar dynamics, methods: N-body simulations, binaries: | |
close, binaries: general, globular clusters: general, | |
globular clusters: individual: NGC 104 (47 Tucanae)} | |
} | |
@Article{ivanova+2008, | |
Title = {{Formation and evolution of compact binaries in globular | |
clusters - II. Binaries with neutron stars}}, | |
Author = {{Ivanova}, N. and {Heinke}, C.~O. and {Rasio}, F.~A. and | |
{Belczynski}, K. and {Fregeau}, J.~M.}, | |
Journal = {\mnras}, | |
Year = {2008}, | |
Month = may, | |
Pages = {553-576}, | |
Volume = {386}, | |
Abstract = {In this paper, the second of a series, we study the | |
stellar dynamical and evolutionary processes leading to the | |
formation of compact binaries containing neutron stars | |
(NSs) in dense globular clusters. For this study, 70 dense | |
clusters were simulated independently, with a total stellar | |
mass ~2 × 107Msolar, exceeding the total mass of all dense | |
globular clusters in our Galaxy. We find that, in order to | |
reproduce the empirically derived formation rate of | |
low-mass X-ray binaries (LMXBs), we must assume that NSs | |
can be formed via electron-capture supernovae with typical | |
natal kicks smaller than in core-collapse supernovae. Our | |
results explain the observed dependence of the number of | |
LMXBs on `collision number' as well as the large scatter | |
observed between different globular clusters. We predict | |
that the number of quiescent LMXBs in different clusters | |
should not have a strong metallicity dependence. We compare | |
the results obtained from our simulations with the observed | |
population of millisecond pulsars (MSPs). We find that in | |
our cluster model the following mass-gaining events create | |
populations of MSPs that do not match the observations | |
(either they are inconsistent with the observed LMXB | |
production rates, or the inferred binary periods or | |
companion masses are not observed among radio bMSPs): (i) | |
accretion during a common-envelope event with a NS formed | |
through electron-capture supernovae (ECSNe), and (ii) mass | |
transfer (MT) from a white dwarf donor. Some processes lead | |
only to a mild recycling - physical collisions or MT in a | |
post-accretion-induced collapse system. In addition, for | |
MSPs, we distinguish low magnetic field (long-lived) and | |
high magnetic field (short-lived) populations, where in the | |
latter NSs are formed as a result of accretion-induced | |
collapse or merger-induced collapse. With this distinction | |
and by considering only those mass-gaining events that | |
appear to lead to NS recycling, we obtain good agreement of | |
our models with the numbers and characteristics of observed | |
MSPs in 47 Tuc and Terzan 5, as well as with the cumulative | |
statistics for MSPs detected in globular clusters of | |
different dynamical properties. We find that significant | |
production of merging double NSs potentially detectable as | |
short gamma-ray bursts occurs only in very dense, most | |
likely core-collapsed clusters.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2008MNRAS.386..553I}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/0706.4096}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2008.13064.x}, | |
Bdsk-url-2 = {http://arxiv.org/abs/0706.4096}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2008MNRAS.386..553I}, | |
Date-added = {2017-07-03 06:25:07 +0000}, | |
Date-modified = {2017-07-03 06:25:13 +0000}, | |
Doi = {10.1111/j.1365-2966.2008.13064.x}, | |
Eprint = {0706.4096}, | |
Keywords = {stellar dynamics , binaries: close , binaries: general , | |
stars: neutron , pulsars: general , globular clusters: | |
general , X-rays: binaries} | |
} | |
@Article{ivanova&kalogera2006, | |
Title = {{The Brightest Point X-Ray Sources in Elliptical Galaxies | |
and the Mass Spectrum of Accreting Black Holes}}, | |
Author = {{Ivanova}, N. and {Kalogera}, V.}, | |
Journal = {\apj}, | |
Year = {2006}, | |
Month = jan, | |
Pages = {985-994}, | |
Volume = {636}, | |
Abstract = {We propose that the shape of the upper-end X-ray | |
luminosity function (XLF) observed in elliptical galaxies | |
for point sources carries valuable information about the | |
black hole (BH) mass spectrum among old X-ray transients | |
formed in the galaxies. Here we present the line of | |
arguments and analysis that support this connection and the | |
methodology for deriving the BH mass spectrum slope from | |
the observed XLF slope. We show that this underlying BH | |
mass spectrum is modified by a weighting factor that is | |
related to the transient duty cycle, and it generally | |
depends on the host galaxy age, the BH mass, and the X-ray | |
binary (XRB) donor type (main-sequence, red giant, or white | |
dwarf donors). We find that the observed XLF is dominated | |
by transient BH systems in outburst (a prediction possibly | |
testable by future observations) but that the assumption of | |
a constant duty cycle for all systems leads to results | |
inconsistent with current observations. We also find that | |
the derived BH mass slope depends on the strength of the | |
angular momentum loss due to magnetic braking for | |
main-sequence donors. More specifically, we find that for | |
``standard'' magnetic braking, BH XRBs with red giant | |
donors dominate the upper-end XLF but that for weaker | |
magnetic braking prescriptions, main-sequence donors are | |
found to be dominant. The methodology presented here can be | |
used in the future as our understanding of the transient | |
duty and its dependence on binary and mass transfer | |
properties improves. Under certain assumptions for this | |
dependence, we derive a differential BH mass spectrum slope | |
of ~=2.5 an upper BH mass cutoff at ~=20 Msolar is needed | |
to understand the very brightest of the BH XRBs in | |
elliptical galaxies. We also show that our quantitative | |
results are robust against expected variations by factors | |
of a few of the outburst peak X-ray luminosities. We expect | |
that our analysis will eventually help to constrain binary | |
population synthesis models and the adopted relations | |
between black holes and the masses of their progenitors.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006ApJ...636..985I}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/0506471}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/498059}, | |
Bdsk-url-2 = {http://arxiv.org/abs/astro-ph/0506471}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2006ApJ...636..985I}, | |
Date-added = {2017-08-08 01:25:36 +0000}, | |
Date-modified = {2017-08-08 01:26:35 +0000}, | |
Doi = {10.1086/498059}, | |
Eprint = {astro-ph/0506471}, | |
Keywords = {Galaxies: Elliptical and Lenticular, cD, Methods: | |
Statistical, X-Rays: Binaries} | |
} | |
@Book{jackson1998, | |
Title = {{Classical Electrodynamics, 3rd Edition}}, | |
Author = {{Jackson}, J.~D.}, | |
Year = {1998}, | |
Month = jul, | |
Abstract = {A revision of the defining book covering the physics and classical mathematics necessary to understand electromagnetic fields in materials and at surfaces and interfaces. The third edition has been revised to address the changes in emphasis and applications that have occurred in the past twenty years.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1998clel.book.....J}, | |
Booktitle = {Classical Electrodynamics, 3rd Edition, by John David Jackson, pp.~832.~ISBN 0-471-30932-X.~Wiley-VCH , July 1998.}, | |
Owner = {aleksey}, | |
Pages = {832}, | |
Timestamp = {2019.02.02} | |
} | |
@Article{jarosik+2011, | |
Title = {{Seven-year Wilkinson Microwave Anisotropy Probe (WMAP) | |
Observations: Sky Maps, Systematic Errors, and Basic | |
Results}}, | |
Author = {{Jarosik}, N. and {Bennett}, C.~L. and {Dunkley}, J. and | |
{Gold}, B. and {Greason}, M.~R. and {Halpern}, M. and | |
{Hill}, R.~S. and {Hinshaw}, G. and {Kogut}, A. and | |
{Komatsu}, E. and {Larson}, D. and {Limon}, M. and {Meyer}, | |
S.~S. and {Nolta}, M.~R. and {Odegard}, N. and {Page}, L. | |
and {Smith}, K.~M. and {Spergel}, D.~N. and {Tucker}, G.~S. | |
and {Weiland}, J.~L. and {Wollack}, E. and {Wright}, | |
E.~L.}, | |
Journal = {\apjs}, | |
Year = {2011}, | |
Month = feb, | |
Pages = {14}, | |
Volume = {192}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2011ApJS..192...14J}, | |
Archiveprefix = {arXiv}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0067-0049/192/2/14}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1088/0067-0049/192/2/14}, | |
Eid = {14}, | |
Eprint = {1001.4744}, | |
Keywords = {cosmic background radiation, space vehicles: instruments}, | |
Primaryclass = {astro-ph.CO} | |
} | |
@Article{jenet+2005, | |
Title = {{Detecting the Stochastic Gravitational Wave Background | |
Using Pulsar Timing}}, | |
Author = {{Jenet}, F.~A. and {Hobbs}, G.~B. and {Lee}, K.~J. and | |
{Manchester}, R.~N.}, | |
Journal = {\apjl}, | |
Year = {2005}, | |
Month = jun, | |
Pages = {L123-L126}, | |
Volume = {625}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2005ApJ...625L.123J}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/431220}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/431220}, | |
Eprint = {arXiv:astro-ph/0504458}, | |
Keywords = {Gravitational Waves, Stars: Pulsars: General} | |
} | |
@Article{jenkins+2001, | |
Title = {{The mass function of dark matter haloes}}, | |
Author = {{Jenkins}, A. and {Frenk}, C.~S. and {White}, S.~D.~M. and | |
{Colberg}, J.~M. and {Cole}, S. and {Evrard}, A.~E. and | |
{Couchman}, H.~M.~P. and {Yoshida}, N.}, | |
Journal = {\mnras}, | |
Year = {2001}, | |
Month = feb, | |
Pages = {372-384}, | |
Volume = {321}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2001MNRAS.321..372J}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1046/j.1365-8711.2001.04029.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1046/j.1365-8711.2001.04029.x}, | |
Eprint = {arXiv:astro-ph/0005260}, | |
Keywords = {GRAVITATION, METHODS: NUMERICAL, COSMOLOGY: THEORY, DARK | |
MATTER, gravitation, methods: numerical, cosmology: theory, | |
dark matter} | |
} | |
@Article{jeongahn.malhotra2017, | |
Title = {{Simplified Derivation of the Collision Probability of Two Objects in Independent Keplerian Orbits}}, | |
Author = {{JeongAhn}, Y. and {Malhotra}, R.}, | |
Journal = {\aj}, | |
Year = {2017}, | |
Month = may, | |
Pages = {235}, | |
Volume = {153}, | |
Abstract = {Many topics in planetary studies demand an estimate of the collision probability of two objects moving on nearly Keplerian orbits. In the classic works of {\"{O}}pik and Wetherill, the collision probability was derived by linearizing the motion near the collision points, and there is now a vast amount of literature using their method. We present here a simpler and more physically motivated derivation for non-tangential collisions in Keplerian orbits, as well as for tangential collisions that were not previously considered. Our formulas have the added advantage of being manifestly symmetric in the parameters of the two colliding bodies. In common with the {\"{O}}pik-Wetherill treatments, we linearize the motion of the bodies in the vicinity of the point of orbit intersection (or near the points of minimum distance between the two orbits) and assume a uniform distribution of impact parameter within the collision radius. We point out that the linear approximation leads to singular results for the case of tangential encounters. We regularize this singularity by use of a parabolic approximation of the motion in the vicinity of a tangential encounter.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017AJ....153..235J}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.3847/1538-3881/aa6aa7}, | |
Eid = {235}, | |
Eprint = {1701.03096}, | |
Keywords = {celestial mechanics, meteorites, meteors, meteoroids, minor planets, asteroids: general, planetary systems}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.EP}, | |
Timestamp = {2018.10.11} | |
} | |
@Article{jiang+2017, | |
Title = {{Super-Eddington Accretion Disks around Supermassive black Holes}}, | |
Author = {{Jiang}, Y.-F. and {Stone}, J. and {Davis}, S.~W.}, | |
Journal = {ArXiv e-prints}, | |
Year = {2017}, | |
Month = sep, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2017arXiv170902845J}, | |
Archiveprefix = {arXiv}, | |
Eprint = {1709.02845}, | |
Keywords = {Astrophysics - High Energy Astrophysical Phenomena}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{jiang+2014, | |
Title = {{A Global Three-dimensional Radiation Magneto-hydrodynamic | |
Simulation of Super-Eddington Accretion Disks}}, | |
Author = {{Jiang}, Y.-F. and {Stone}, J.~M. and {Davis}, S.~W.}, | |
Journal = {\apj}, | |
Year = {2014}, | |
Month = dec, | |
Pages = {106}, | |
Volume = {796}, | |
Abstract = {We study super-Eddington accretion flows onto black holes | |
using a global three-dimensional radiation | |
magneto-hydrodynamical simulation. We solve the | |
time-dependent radiative transfer equation for the specific | |
intensities to accurately calculate the angular | |
distribution of the emitted radiation. Turbulence generated | |
by the magneto-rotational instability provides | |
self-consistent angular momentum transfer. The simulation | |
reaches inflow equilibrium with an accretion rate ~220 L | |
Edd/c 2 and forms a radiation-driven outflow along the | |
rotation axis. The mechanical energy flux carried by the | |
outflow is ~20% of the radiative energy flux. The total | |
mass flux lost in the outflow is about 29% of the net | |
accretion rate. The radiative luminosity of this flow is | |
~10 L Edd. This yields a radiative efficiency ~4.5%, which | |
is comparable to the value in a standard thin disk model. | |
In our simulation, vertical advection of radiation caused | |
by magnetic buoyancy transports energy faster than photon | |
diffusion, allowing a significant fraction of the photons | |
to escape from the surface of the disk before being | |
advected into the black hole. We contrast our results with | |
the lower radiative efficiencies inferred in most models, | |
such as the slim disk model, which neglect vertical | |
advection. Our inferred radiative efficiencies also exceed | |
published results from previous global numerical | |
simulations, which did not attribute a significant role to | |
vertical advection. We briefly discuss the implications for | |
the growth of supermassive black holes in the early | |
universe and describe how these results provided a basis | |
for explaining the spectrum and population statistics of | |
ultraluminous X-ray sources.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014ApJ...796..106J}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1410.0678}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1088/0004-637X/796/2/106}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1410.0678}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014ApJ...796..106J}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1088/0004-637X/796/2/106}, | |
Eid = {106}, | |
Eprint = {1410.0678}, | |
Keywords = {accretion, accretion disks, magnetohydrodynamics: MHD, | |
methods: numerical, radiative transfer}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{johnson&quataert2007, | |
Title = {{The Effects of Thermal Conduction on Radiatively Inefficient Accretion Flows}}, | |
Author = {{Johnson}, B.~M. and {Quataert}, E.}, | |
Journal = {\apj}, | |
Year = {2007}, | |
Month = may, | |
Pages = {1273-1281}, | |
Volume = {660}, | |
Abstract = {We quantify the effects of electron thermal conduction on the properties of hot accretion flows, under the assumption of spherical symmetry. Electron heat conduction is important for low accretion rate systems where the electron cooling time is longer than the conduction time of the plasma, such as Sgr A* in the Galactic center. For accretion flows with density profiles similar to the Bondi solution [n(r)~r-3/2], we show that heat conduction leads to supervirial temperatures, implying that conduction significantly modifies the dynamics of the accretion flow. We then self-consistently solve for the dynamics of spherical accretion in the presence of saturated conduction and electron heating. We find that the accretion rate onto the central object can be reduced by ~1-3 orders of magnitude relative to the canonical Bondi rate. Electron conduction may thus be an important ingredient in explaining the low radiative efficiencies and low accretion rates inferred from observations of low-luminosity galactic nuclei. The solutions presented in this paper may also describe the nonlinear saturation of the magnetothermal instability in hot accretion flows.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...660.1273J}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0608467}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1086/513065}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0608467}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2007ApJ...660.1273J}, | |
Date-added = {2015-05-01 15:18:14 +0000}, | |
Date-modified = {2015-05-01 15:18:16 +0000}, | |
Doi = {10.1086/513065}, | |
Eprint = {astro-ph/0608467}, | |
Keywords = {Accretion, Accretion Disks, Galaxy: Center}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.02} | |
} | |
@Article{johnson+2007, | |
Title = {{The Effects of Thermal Conduction on Radiatively Inefficient Accretion Flows}}, | |
Author = {{Johnson}, B.~M. and {Quataert}, E.}, | |
Journal = {\apj}, | |
Year = {2007}, | |
Month = may, | |
Pages = {1273-1281}, | |
Volume = {660}, | |
Abstract = {We quantify the effects of electron thermal conduction on the properties of hot accretion flows, under the assumption of spherical symmetry. Electron heat conduction is important for low accretion rate systems where the electron cooling time is longer than the conduction time of the plasma, such as Sgr A* in the Galactic center. For accretion flows with density profiles similar to the Bondi solution [n(r)~r-3/2], we show that heat conduction leads to supervirial temperatures, implying that conduction significantly modifies the dynamics of the accretion flow. We then self-consistently solve for the dynamics of spherical accretion in the presence of saturated conduction and electron heating. We find that the accretion rate onto the central object can be reduced by ~1-3 orders of magnitude relative to the canonical Bondi rate. Electron conduction may thus be an important ingredient in explaining the low radiative efficiencies and low accretion rates inferred from observations of low-luminosity galactic nuclei. The solutions presented in this paper may also describe the nonlinear saturation of the magnetothermal instability in hot accretion flows.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...660.1273J}, | |
Arxivurl = {http://arXiv.org/abs/astro-ph/0608467}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1086/513065}, | |
Bdsk-url-2 = {http://arXiv.org/abs/astro-ph/0608467}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2007ApJ...660.1273J}, | |
Date-added = {2015-05-01 15:18:14 +0000}, | |
Date-modified = {2015-05-01 15:18:16 +0000}, | |
Doi = {10.1086/513065}, | |
Eprint = {astro-ph/0608467}, | |
Keywords = {Accretion, Accretion Disks, Galaxy: Center}, | |
Owner = {aleksey}, | |
Timestamp = {2018.03.02} | |
} | |
@Article{katz1975, | |
Title = {{Two kinds of stellar collapse}}, | |
Author = {{Katz}, J.~I.}, | |
Journal = {\nat}, | |
Year = {1975}, | |
Month = feb, | |
Pages = {698}, | |
Volume = {253}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1975Natur.253..698K}, | |
Doi = {10.1038/253698a0}, | |
Keywords = {Binary Stars, Globular Clusters, Gravitational Collapse, | |
Stellar Evolution, X Ray Sources, Astrophysics, Orbital | |
Elements, Stellar Mass Ejection, X Ray Stars} | |
} | |
@Article{kauffmann+2000, | |
Title = {{A unified model for the evolution of galaxies and | |
quasars}}, | |
Author = {Kauffmann, G and Haehnelt, M}, | |
Journal = {\mnras}, | |
Year = {2000}, | |
Month = jan, | |
Pages = {576--588}, | |
Volume = {311}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1046/j.1365-8711.2000.03077.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1046/j.1365-8711.2000.03077.x}, | |
Keywords = {GALAXIES: FORMATION, GALAXIES: NUCLEI, QUASARS: | |
GENERAL,BLACK HOLE PHYSICS; Untitled; Untitled1} | |
} | |
@Article{kauffmann&heckman2009, | |
Title = {{Feast and Famine: regulation of black hole growth in | |
low-redshift galaxies}}, | |
Author = {{Kauffmann}, G. and {Heckman}, T.~M.}, | |
Journal = {\mnras}, | |
Year = {2009}, | |
Month = jul, | |
Pages = {135-147}, | |
Volume = {397}, | |
Abstract = {We analyse the observed distribution of Eddington ratios | |
(L/LEdd) as a function of supermassive black hole mass for | |
a large sample of nearby galaxies drawn from the Sloan | |
Digital Sky Survey. We demonstrate that there are two | |
distinct regimes of black hole growth in nearby galaxies. | |
The first is associated with galaxies with significant star | |
formation [M*/starformationrate (SFR) ~ a Hubble time] in | |
their central kiloparsec regions, and is characterized by a | |
broad lognormal distribution of accretion rates peaked at a | |
few per cent of the Eddington limit. In this regime, the | |
Eddington ratio distribution is independent of the mass of | |
the black hole and shows little dependence on the central | |
stellar population of the galaxy. The second regime is | |
associated with galaxies with old central stellar | |
populations (M*/SFR >> a Hubble time), and is characterized | |
by a power-law distribution function of Eddington ratios. | |
In this regime, the time-averaged mass accretion rate on to | |
black holes is proportional to the mass of stars in the | |
galaxy bulge, with a constant of proportionality that | |
depends on the mean stellar age of the stars. This result | |
is once again independent of black hole mass. We show that | |
both the slope of the power law and the decrease in the | |
accretion rate on to black holes in old galaxies are | |
consistent with population synthesis model predictions of | |
the decline in stellar mass loss rates as a function of | |
mean stellar age. Our results lead to a very simple picture | |
of black hole growth in the local Universe. If the supply | |
of cold gas in a galaxy bulge is plentiful, the black hole | |
regulates its own growth at a rate that does not further | |
depend on the properties of the interstellar medium. Once | |
the gas runs out, black hole growth is regulated by the | |
rate at which evolved stars lose their mass.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009MNRAS.397..135K}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/0812.1224}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2009.14960.x}, | |
Bdsk-url-2 = {http://arXiv.org/abs/0812.1224}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2009MNRAS.397..135K}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2016-03-17 16:54:19 +0000}, | |
Doi = {10.1111/j.1365-2966.2009.14960.x}, | |
Eprint = {0812.1224}, | |
Keywords = {galaxies: active , galaxies: bulges , galaxies: evolution | |
, galaxies: nuclei , galaxies: stellar content} | |
} | |
@Article{kazantzidis+2005, | |
Title = {{The Fate of Supermassive Black Holes and the Evolution of | |
the M\_\{BH\}-\{$\sigma$\} Relation in Merging Galaxies: | |
The Effect of Gaseous Dissipation}}, | |
Author = {Kazantzidis, S and Mayer, L and Colpi, M and Madau, P and | |
Debattista, V.\~{}P. and Wadsley, J and Stadel, J and | |
Quinn, T and Moore, B}, | |
Journal = {\apjl}, | |
Year = {2005}, | |
Month = apr, | |
Pages = {L67--L70}, | |
Volume = {623}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/430139}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1086/430139}, | |
Keywords = {Cosmology: Theory, Galaxies: Interactions, Hydrodynamics, | |
Methods: Numerical,Black Hole Physics} | |
} | |
@Article{kelley+2014, | |
Title = {{Tidal disruption and magnetic flux capture: powering a | |
jet from a quiescent black hole}}, | |
Author = {{Kelley}, L.~Z. and {Tchekhovskoy}, A. and {Narayan}, R.}, | |
Journal = {\mnras}, | |
Year = {2014}, | |
Month = dec, | |
Pages = {3919-3938}, | |
Volume = {445}, | |
Abstract = {The transient Swift J1644+57 is believed to have been | |
produced by an unlucky star wandering too close to a | |
supermassive black hole (BH) leading to a tidal disruption | |
event. This unusual flare displayed highly super-Eddington | |
X-ray emission which likely originated in a relativistic, | |
collimated jet. This presents challenges to modern | |
accretion and jet theory as upper limits of prior BH | |
activity, which we obtain from the radio afterglow of this | |
event, imply that both the pre-disruption BH and stellar | |
magnetic fluxes fall many orders of magnitude short of what | |
is required to power the observed X-ray luminosity. We | |
argue that a pre-existing, `fossil' accretion disc can | |
contain a sufficient reservoir of magnetic flux and that | |
the stellar debris stream is capable of dragging this flux | |
into the BH. To demonstrate this, we perform local, 3D | |
magnetohydrodynamic simulations of the disc-stream | |
interaction and demonstrate that the interface between the | |
two is unstable to mixing. This mixing entrains a | |
sufficient amount of fossil disc magnetic flux into the | |
infalling stellar debris to power the jet. We argue that | |
the interaction with the fossil disc can have a pronounced | |
effect on the structure and dynamics of mass fallback and | |
likely the resulting transient. Finally, we describe | |
possible ramifications of these interactions on unresolved | |
problems in tidal disruption dynamics, in particular, the | |
efficiency of debris circularization, and effects of the | |
disruption on the pre-existing BH system.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2014MNRAS.445.3919K}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arXiv.org/abs/1410.0366}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.1093/mnras/stu2041}, | |
Bdsk-url-2 = {http://arXiv.org/abs/1410.0366}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2014MNRAS.445.3919K}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1093/mnras/stu2041}, | |
Eprint = {1410.0366}, | |
Keywords = {accretion, accretion discs, MHD, galaxies: jets, galaxies: | |
kinematics and dynamics, quasars: supermassive black | |
holes}, | |
Primaryclass = {astro-ph.HE} | |
} | |
@Article{keshet+2009, | |
Title = {{Analytic Study of Mass Segregation Around a Massive Black Hole}}, | |
Author = {{Keshet}, U. and {Hopman}, C. and {Alexander}, T.}, | |
Journal = {\apjl}, | |
Year = {2009}, | |
Month = jun, | |
Pages = {L64-L67}, | |
Volume = {698}, | |
Abstract = {We analyze the distribution of stars of arbitrary mass function ?(m) around a massive black hole (MBH). Unless ? is strongly dominated by light stars, the steady-state distribution function approaches a power law in specific energy x ? -E/m?2 < x max with index p = m/4M 0, where E is the energy, ? is the typical velocity dispersion of unbound stars, and M 0 is the mass averaged over m?xp max. For light-dominated ?, p can grow as large as 3/2?much steeper than previously thought. A simple prescription for the stellar density profile around MBHs is provided. We illustrate our results by applying them to stars around the MBH in the Milky Way.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...698L..64K}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1088/0004-637X/698/1/L64}, | |
Eprint = {0901.4343}, | |
Keywords = {black hole physics, Galaxy: kinematics and dynamics, stellar dynamics}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.GA}, | |
Timestamp = {2018.03.28} | |
} | |
@Article{khan+2011, | |
Title = {{Efficient Merger of Binary Supermassive Black Holes in | |
Merging Galaxies}}, | |
Author = {Khan, Fazeel Mahmood and Just, Andreas and Merritt, | |
David}, | |
Journal = {\apj}, | |
Year = {2011}, | |
Month = may, | |
Pages = {89}, | |
Volume = {732}, | |
Abstract = {In spherical galaxies, binary supermassive black holes | |
(SMBHs) have difficulty reaching sub-parsec separations due | |
to depletion of stars on orbits that intersect the massive | |
binary---the "final parsec problem." Galaxies that form via | |
major mergers are substantially non-spherical, and it has | |
been argued that the centrophilic orbits in triaxial | |
galaxies might provide stars to the massive binary at a | |
high enough rate to avoid stalling. Here we test that idea | |
by carrying out fully self-consistent merger simulations of | |
galaxies containing central SMBHs. We find hardening rates | |
of the massive binaries that are indeed much higher than in | |
spherical models and essentially independent of the number | |
of particles used in the simulations. Binary eccentricities | |
remain high throughout the simulations. Our results | |
constitute a fully stellar-dynamical solution to the final | |
parsec problem and imply a potentially high rate of events | |
for low-frequency gravitational wave detectors like LISA.}, | |
Bdsk-url-1 = {http://adsabs.harvard.edu/cgi-bin/nph-data%5C_query?bibcode=2011ApJ...732...89K%5C&link%5C_type=ABSTRACT}, | |
Bdsk-url-2 = {http://dx.doi.org/10.1088/0004-637X/732/2/89}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:41 +0000}, | |
Doi = {10.1088/0004-637X/732/2/89}, | |
Keywords = {GRAVITATIONAL WAVES, galaxies: interactions, galaxies: | |
kinematics and dynamics, galaxies: nuclei,galaxies: | |
evolution}, | |
Url = {http://adsabs.harvard.edu/cgi-bin/nph-data\_query?bibcode=2011ApJ...732...89K\&link\_type=ABSTRACT} | |
} | |
@Article{kieffer&bogdanovic2016, | |
Title = {{Can Star-Disk Collisions Explain the Missing Red Giants | |
Problem in the Galactic Center?}}, | |
Author = {{Kieffer}, T.~F. and {Bogdanovi{\'c}}, T.}, | |
Journal = {\apj}, | |
Year = {2016}, | |
Month = jun, | |
Pages = {155}, | |
Volume = {823}, | |
Abstract = {Observations have revealed a relative paucity of red giant | |
(RG) stars within the central 0.5 pc in the Galactic Center | |
(GC). Motivated by this finding we investigate the | |
hypothesis that collisions of stars with a fragmenting | |
accretion disk are responsible for the observed dearth of | |
evolved stars. We use three-dimensional hydrodynamic | |
simulations to model a star with radius 10 R &sun; and mass | |
1 M &sun;, representative of the missing population of RGs, | |
colliding with high density clumps. We find that multiple | |
collisions with clumps of column density ≳108 g cm-2 can | |
strip a substantial fraction of the star's envelope and in | |
principle render it invisible to observations. Simulations | |
confirm that repeated impacts are particularly efficient in | |
driving mass loss as partially stripped RGs expand and have | |
increased cross sections for subsequent collisions. Because | |
the envelope is unbound on account of the kinetic energy of | |
the star, any significant amount of stripping of the RG | |
population in the GC should be mirrored by a systematic | |
decay of their orbits and possibly by their enhanced | |
rotational velocity. To be viable, this scenario requires | |
that the total mass of the fragmenting disk has been | |
several orders of magnitude higher than that of the | |
early-type stars which now form the stellar disk in the | |
GC.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016ApJ...823..155K}, | |
Archiveprefix = {arXiv}, | |
Arxivurl = {http://arxiv.org/abs/1602.03527}, | |
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Bdsk-url-1 = {http://dx.doi.org/10.3847/0004-637X/823/2/155}, | |
Bdsk-url-2 = {http://arxiv.org/abs/1602.03527}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2016ApJ...823..155K}, | |
Date-added = {2017-06-10 02:44:19 +0000}, | |
Date-modified = {2017-06-10 02:44:35 +0000}, | |
Doi = {10.3847/0004-637X/823/2/155}, | |
Eid = {155}, | |
Eprint = {1602.03527}, | |
Keywords = {Galaxy: center, hydrodynamics, stars: late-type} | |
} | |
@Article{kiel&hurley2006, | |
Title = {{Populating the Galaxy with low-mass X-ray binaries}}, | |
Author = {{Kiel}, P.~D. and {Hurley}, J.~R.}, | |
Journal = {\mnras}, | |
Year = {2006}, | |
Month = jul, | |
Pages = {1152-1166}, | |
Volume = {369}, | |
Abstract = {We perform binary population-synthesis calculations to | |
investigate the incidence of low-mass X-ray binaries | |
(LMXBs) and their birth rate in the Galaxy. We use a | |
binary-evolution algorithm that models all the relevant | |
processes including tidal circularization and | |
synchronization. Parameters in the evolution algorithm that | |
are uncertain and may affect X-ray binary formation are | |
allowed to vary during the investigation. We agree with | |
previous studies that under standard assumptions of binary | |
evolution the formation rate and number of black hole (BH) | |
LMXBs predicted by the model are more than an order of | |
magnitude less than what is indicated by observations. We | |
find that the common-envelope process cannot be manipulated | |
to produce significant numbers of BH LMXBs. However, by | |
simply reducing the mass-loss rate from helium stars | |
adopted in the standard model, to a rate that agrees with | |
the latest data, we produce a good match to the | |
observations. Including LMXBs that evolve from | |
intermediate-mass systems also leads to favourable results. | |
We stress that constraints on the X-ray binary population | |
provided by observations are used here merely as a guide as | |
surveys suffer from incompleteness and much uncertainty is | |
involved in the interpretation of results.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2006MNRAS.369.1152K}, | |
Arxivurl = {http://arxiv.org/abs/astro-ph/0605080}, | |
Bdsk-file-1 = {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}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2006.10400.x}, | |
Bdsk-url-2 = {http://arxiv.org/abs/astro-ph/0605080}, | |
Bdsk-url-3 = {http://adsabs.harvard.edu/abs/2006MNRAS.369.1152K}, | |
Date-added = {2017-08-24 01:07:58 +0000}, | |
Date-modified = {2017-08-24 01:12:19 +0000}, | |
Doi = {10.1111/j.1365-2966.2006.10400.x}, | |
Eprint = {astro-ph/0605080}, | |
Keywords = {binaries: close: stars: evolution: stars: low-mass, brown | |
dwarfs: stars: neutron: Galaxy: stellar content: X-rays: | |
binaries, binaries: close, stars: evolution, stars: | |
low-mass, brown dwarfs, stars: neutron, Galaxy: stellar | |
content, X-rays: binaries} | |
} | |
@Article{king2003, | |
Title = {{Black Holes, Galaxy Formation, and the | |
M$_{BH}$-{$\sigma$} Relation}}, | |
Author = {{King}, A.}, | |
Journal = {\apjl}, | |
Year = {2003}, | |
Month = oct, | |
Pages = {L27-L29}, | |
Volume = {596}, | |
Abstract = {Recent X-ray observations of intense high-speed outflows | |
in quasars suggest that supercritical accretion on to the | |
central black hole may have an important effect on a host | |
galaxy. I revisit some ideas of Silk & Rees and assume that | |
such flows occur in the final stages of building up the | |
black hole mass. It is now possible to model explicitly the | |
interaction between the outflow and the host galaxy. This | |
is found to resemble a momentum-driven stellar wind bubble, | |
implying a relation MBH=(fg?/2?G2)?4~=1.5?08?4200 Msolar | |
between black hole mass and bulge velocity dispersion | |
(fg=gas fraction of total matter density, ?=electron | |
scattering opacity), without free parameters. This is | |
remarkably close to the observed relation in both slope and | |
normalization. This result suggests that the central black | |
holes in galaxies gain most of their mass in phases of | |
super-Eddington accretion, which are presumably obscured or | |
at high redshift. Observed super-Eddington quasars are | |
apparently late in growing their black hole masses.}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2003ApJ...596L..27K}, | |
Doi = {10.1086/379143}, | |
Eprint = {astro-ph/0308342}, | |
Keywords = {Accretion, Accretion Disks, Black Hole Physics, Galaxies: | |
Formation, Galaxies: Nuclei, Galaxies: Quasars: General}, | |
Owner = {aleksey}, | |
Timestamp = {2018.02.07} | |
} | |
@Article{king+2007, | |
Title = {{Accretion disc viscosity: how big is alpha?}}, | |
Author = {{King}, A.~R. and {Pringle}, J.~E. and {Livio}, M.}, | |
Journal = {\mnras}, | |
Year = {2007}, | |
Month = apr, | |
Pages = {1740-1746}, | |
Volume = {376}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2007MNRAS.376.1740K}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1111/j.1365-2966.2007.11556.x}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:42 +0000}, | |
Doi = {10.1111/j.1365-2966.2007.11556.x}, | |
Eprint = {arXiv:astro-ph/0701803}, | |
Keywords = {accretion, accretion discs} | |
} | |
@Book{kippenhahn&weigert1990, | |
Title = {{Stellar Structure and Evolution}}, | |
Author = {{Kippenhahn}, R. and {Weigert}, A.}, | |
Year = {1990}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1990sse..book.....K}, | |
Booktitle = {Stellar Structure and Evolution, XVI, 468 pp.~192 figs..~ | |
Springer-Verlag Berlin Heidelberg New York.~Also Astronomy | |
and Astrophysics Library}, | |
Date-added = {2015-10-29 19:33:44 +0000}, | |
Date-modified = {2015-10-29 20:02:37 +0000}, | |
Keywords = {STELLAR STRUCTURE, STELLAR EVOLUTION; Untitled; | |
Untitled1} | |
} | |
@Article{kochanek2016, | |
Title = {{Tidal disruption event demographics}}, | |
Author = {{Kochanek}, C.~S.}, | |
Journal = {\mnras}, | |
Year = {2016}, | |
Month = sep, | |
Pages = {371-384}, | |
Volume = {461}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/2016MNRAS.461..371K}, | |
Archiveprefix = {arXiv}, | |
Doi = {10.1093/mnras/stw1290}, | |
Eprint = {1601.06787}, | |
Keywords = {stars: black holes, quasars: supermassive black holes}, | |
Owner = {aleksey}, | |
Primaryclass = {astro-ph.HE}, | |
Timestamp = {2017.12.12} | |
} | |
@Article{kochanek1994, | |
Title = {{The aftermath of tidal disruption: The dynamics of thin | |
gas streams}}, | |
Author = {{Kochanek}, C.~S.}, | |
Journal = {\apj}, | |
Year = {1994}, | |
Month = feb, | |
Pages = {508-520}, | |
Volume = {422}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1994ApJ...422..508K}, | |
Bdsk-url-1 = {http://dx.doi.org/10.1086/173745}, | |
Doi = {10.1086/173745}, | |
Keywords = {Active Galactic Nuclei, Active Galaxies, Astronomical | |
Models, Black Holes (Astronomy), Gas Streams, | |
Hydrodynamics, Mathematical Models, Deposition, Gas | |
Dynamics, Precession, Stellar Orbits, Stellar Structure} | |
} | |
@Article{kochanek1992, | |
Title = {{The dynamical evolution of tidal capture binaries}}, | |
Author = {{Kochanek}, C.~S.}, | |
Journal = {\apj}, | |
Year = {1992}, | |
Month = feb, | |
Pages = {604-620}, | |
Volume = {385}, | |
Adsnote = {Provided by the SAO/NASA Astrophysics Data System}, | |
Adsurl = {http://adsabs.harvard.edu/abs/1992ApJ...385..604K}, | |
Doi = {10.1086/170966}, | |
Keywords = {Binary Stars, Globular Clusters, Stellar Evolution, | |
Stellar Motions, Capture Effect, Main Sequence Stars, | |
Neutron Stars, Pulsars, Stellar Mass, Tides}, | |
Owner = {aleksey}, | |
Timestamp = {2017.12. |
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