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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},
year = 2002,
month = mar,
volume = {384},
pages = {112-139},
doi = {10.1051/0004-6361:20020017},
archivePrefix = {arXiv},
eprint = {astro-ph/0201294},
primaryClass = {astro-ph},
adsurl = {https://ui.adsabs.harvard.edu/abs/2002A&A...384..112L},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{boubert+2018,
author = {{Boubert}, D. and {Guillochon}, J. and {Hawkins}, K. and {Ginsburg}, I. and
{Evans}, N.~W. and {Strader}, J.},
title = "{Revisiting hypervelocity stars after Gaia DR2}",
journal = {\mnras},
keywords = {binaries: general, stars: kinematics and dynamics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics},
year = 2018,
month = sep,
volume = {479},
number = {2},
pages = {2789-2795},
doi = {10.1093/mnras/sty1601},
archivePrefix = {arXiv},
eprint = {1804.10179},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018MNRAS.479.2789B},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{warren_brown+2014,
author = {{Brown}, Warren R. and {Geller}, Margaret J. and {Kenyon}, Scott J.},
title = "{MMT Hypervelocity Star Survey. III. The Complete Survey}",
journal = {\apj},
keywords = {Galaxy: center, Galaxy: halo, Galaxy: kinematics and dynamics, stars: early-type, stars: individual: SDSS J111136.44+005856.44 J114146.45+044217.29 J215629.02+005444.18, Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies},
year = 2014,
month = may,
volume = {787},
number = {1},
eid = {89},
pages = {89},
doi = {10.1088/0004-637X/787/1/89},
archivePrefix = {arXiv},
eprint = {1401.7342},
primaryClass = {astro-ph.SR},
adsurl = {https://ui.adsabs.harvard.edu/abs/2014ApJ...787...89B},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{lockmann+2009,
author = {{L{\"o}ckmann}, U. and {Baumgardt}, H. and {Kroupa}, P.},
title = "{Influence of a stellar cusp on the dynamics of young stellar discs and the origin of the S-stars in the Galactic Centre}",
journal = {\mnras},
keywords = {black hole physics, stellar dynamics, methods: N-body simulations, Galaxy: centre, Astrophysics - Astrophysics of Galaxies},
year = 2009,
month = sep,
volume = {398},
number = {1},
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doi = {10.1111/j.1365-2966.2009.15157.x},
archivePrefix = {arXiv},
eprint = {0906.0574},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2009MNRAS.398..429L},
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}
@ARTICLE{ginsburg&loeb2006,
author = {{Ginsburg}, Idan and {Loeb}, Abraham},
title = "{The fate of former companions to hypervelocity stars originating at the Galactic Centre}",
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}
@ARTICLE{bovy2015,
author = {{Bovy}, Jo},
title = "{galpy: A python Library for Galactic Dynamics}",
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author = {{Generozov}, Aleksey and {Madigan}, Ann-Marie},
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}
@ARTICLE{astropy+2018,
author = {{The Astropy Collaboration} and {Price-Whelan}, A.~M. and {Sip{\H o}cz}, B.~M. and
{G{\"u}nther}, H.~M. and {Lim}, P.~L. and {Crawford}, S.~M. and {Contributors}, (.},
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}
@Article{perez+2007,
Author = {P\'erez, Fernando and Granger, Brian E.},
Title = {{IP}ython: a System for Interactive Scientific Computing},
Journal = {Computing in Science and Engineering},
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Number = {3},
Pages = {21--29},
month = may,
year = 2007,
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}
@Article{2020SciPy-NMeth,
author={Virtanen, Pauli
and Gommers, Ralf
and Oliphant, Travis E.
and Haberland, Matt
and Reddy, Tyler
and Cournapeau, David
and Burovski, Evgeni
and Peterson, Pearu
and Weckesser, Warren
and Bright, Jonathan
and van der Walt, St{\'e}fan J.
and Brett, Matthew
and Wilson, Joshua
and Millman, K. Jarrod
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and Nelson, Andrew R. J.
and Jones, Eric
and Kern, Robert
and Larson, Eric
and Carey, C. J.
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and Feng, Yu
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and VanderPlas, Jake
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and Perktold, Josef
and Cimrman, Robert
and Henriksen, Ian
and Quintero, E. A.
and Harris, Charles R.
and Archibald, Anne M.
and Ribeiro, Ant{\^o}nio H.
and Pedregosa, Fabian
and van Mulbregt, Paul
and Vijaykumar, Aditya
and Bardelli, Alessandro Pietro
and Rothberg, Alex
and Hilboll, Andreas
and Kloeckner, Andreas
and Scopatz, Anthony
and Lee, Antony
and Rokem, Ariel
and Woods, C. Nathan
and Fulton, Chad
and Masson, Charles
and H{\"a}ggstr{\"o}m, Christian
and Fitzgerald, Clark
and Nicholson, David A.
and Hagen, David R.
and Pasechnik, Dmitrii V.
and Olivetti, Emanuele
and Martin, Eric
and Wieser, Eric
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and Wilhelm, Florian
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and Price, Gavin A.
and Ingold, Gert-Ludwig
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and Lee, Gregory R.
and Audren, Herv{\'e}
and Probst, Irvin
and Dietrich, J{\"o}rg P.
and Silterra, Jacob
and Webber, James T.
and Slavi{\v{c}}, Janko
and Nothman, Joel
and Buchner, Johannes
and Kulick, Johannes
and Sch{\"o}nberger, Johannes L.
and de Miranda Cardoso, Jos{\'e} Vin{\'i}cius
and Reimer, Joscha
and Harrington, Joseph
and Rodr{\'i}guez, Juan Luis Cano
and Nunez-Iglesias, Juan
and Kuczynski, Justin
and Tritz, Kevin
and Thoma, Martin
and Newville, Matthew
and K{\"u}mmerer, Matthias
and Bolingbroke, Maximilian
and Tartre, Michael
and Pak, Mikhail
and Smith, Nathaniel J.
and Nowaczyk, Nikolai
and Shebanov, Nikolay
and Pavlyk, Oleksandr
and Brodtkorb, Per A.
and Lee, Perry
and McGibbon, Robert T.
and Feldbauer, Roman
and Lewis, Sam
and Tygier, Sam
and Sievert, Scott
and Vigna, Sebastiano
and Peterson, Stefan
and More, Surhud
and Pudlik, Tadeusz
and Oshima, Takuya
and Pingel, Thomas J.
and Robitaille, Thomas P.
and Spura, Thomas
and Jones, Thouis R.
and Cera, Tim
and Leslie, Tim
and Zito, Tiziano
and Krauss, Tom
and Upadhyay, Utkarsh
and Halchenko, Yaroslav O.
and V{\'a}zquez-Baeza, Yoshiki
and 1.0 Contributors, SciPy},
title={SciPy 1.0: fundamental algorithms for scientific computing in Python},
journal={Nature Methods},
year={2020},
month={Mar},
day={01},
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.},
issn={1548-7105},
doi={10.1038/s41592-019-0686-2},
url={https://doi.org/10.1038/s41592-019-0686-2}
}
@Article{hunter+2007,
Author = {Hunter, J. D.},
Title = {Matplotlib: A 2D graphics environment},
Journal = {Computing in Science \& Engineering},
Volume = {9},
Number = {3},
Pages = {90--95},
abstract = {Matplotlib is a 2D graphics package used for Python for
application development, interactive scripting, and publication-quality
image generation across user interfaces and operating systems.},
publisher = {IEEE COMPUTER SOC},
doi = {10.1109/MCSE.2007.55},
year = 2007
}
@ARTICLE{gualandris+2012,
author = {{Gualandris}, A. and {Mapelli}, M. and {Perets}, H.~B.},
title = "{Eccentric disc instability in stellar discs formed from inspiralling gas clouds in the Galactic Centre}",
journal = {\mnras},
archivePrefix = "arXiv",
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primaryClass = "astro-ph.GA",
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}
@ARTICLE{gualandris&merritt2009,
author = {{Gualandris}, Alessia and {Merritt}, David},
title = "{Perturbations of Intermediate-mass Black Holes on Stellar Orbits in the Galactic Center}",
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year = "2009",
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number = {1},
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primaryClass = {astro-ph.GA},
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}
@ARTICLE{naoz+2019,
author = {{Naoz}, Smadar and {Will}, Clifford M. and {Ramirez-Ruiz}, Enrico and
{Hees}, Aur{\'e}lien and {Ghez}, Andrea M. and {Do}, Tuan},
title = "{A Hidden Friend for the Galactic Center Black Hole, Sgr A*}",
journal = {\apjl},
keywords = {Supermassive black holes, Astrophysical black holes, Galactic center, the Milky Way physics, Gravitation, Gravitational waves, Gravitational wave sources, the Milky Way, Milky Way dynamics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology},
year = "2020",
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pages = {L8},
doi = {10.3847/2041-8213/ab5e3b},
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eprint = {1912.04910},
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}
@ARTICLE{reid&brunthaler2004,
author = {{Reid}, M.~J. and {Brunthaler}, A.},
title = "{The Proper Motion of Sagittarius A*. II. The Mass of Sagittarius A*}",
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volume = {616},
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primaryClass = {astro-ph},
adsurl = {https://ui.adsabs.harvard.edu/abs/2004ApJ...616..872R},
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}
@ARTICLE{antonini+2010,
author = {{Antonini}, Fabio and {Faber}, Joshua and {Gualandris}, Alessia and
{Merritt}, David},
title = "{Tidal Breakup of Binary Stars at the Galactic Center and Its Consequences}",
journal = {\apj},
keywords = {black hole physics, Galaxy: center, Galaxy: kinematics and dynamics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
year = "2010",
month = "Apr",
volume = {713},
number = {1},
pages = {90-104},
doi = {10.1088/0004-637X/713/1/90},
archivePrefix = {arXiv},
eprint = {0909.1959},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2010ApJ...713...90A},
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}
@Article{wernke&madigan2019,
author = {{Wernke}, Heather N. and {Madigan}, Ann-Marie},
title = {{The Effect of General Relativistic Precession on Tidal Disruption Events from Eccentric Nuclear Disks}},
journal = {\apj},
year = {2019},
volume = {880},
number = {1},
pages = {42},
month = {Jul},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
adsurl = {https://ui.adsabs.harvard.edu/abs/2019ApJ...880...42W},
archiveprefix = {arXiv},
doi = {10.3847/1538-4357/ab2711},
eid = {42},
eprint = {1901.03339},
file = {:Wernke/2019.pdf:PDF;:Wernke/2019.pdf:PDF},
keywords = {celestial mechanics, galaxies: kinematics and dynamics, galaxies: nuclei, Astrophysics - High Energy Astrophysical Phenomena},
primaryclass = {astro-ph.HE},
}
@ARTICLE{mori+2019,
author = {{Mori}, Kaya and {Hailey}, Charles J. and {Mandel}, Shifra and
{Schutt}, Yve E. and {Bachetti}, Matteo and {Coerver}, Anna and
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{Nynka}, Melania and {Ponti}, Gabriele and {Tomsick}, John A.},
title = "{NuSTAR and Chandra Observations of New X-Ray Transients in the Central Parsec of the Galaxy}",
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keywords = {Galactic center, X-ray transient sources, low-mass X-ray binary stars, X-ray telescopes, Astrophysics - High Energy Astrophysical Phenomena},
year = "2019",
month = "Nov",
volume = {885},
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pages = {142},
doi = {10.3847/1538-4357/ab4b47},
archivePrefix = {arXiv},
eprint = {1910.03459},
primaryClass = {astro-ph.HE},
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adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{yelda+2014,
author = {{Yelda}, S. and {Ghez}, A.~M. and {Lu}, J.~R. and {Do}, T. and
{Meyer}, L. and {Morris}, M.~R. and {Matthews}, K.},
title = "{Properties of the Remnant Clockwise Disk of Young Stars in the Galactic Center}",
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month = "Mar",
volume = {783},
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pages = {131},
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eprint = {1401.7354},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2014ApJ...783..131Y},
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}
@ARTICLE{kocsis&tremaine2011,
author = {{Kocsis}, Bence and {Tremaine}, Scott},
title = "{Resonant relaxation and the warp of the stellar disc in the Galactic Centre}",
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doi = {10.1111/j.1365-2966.2010.17897.x},
archivePrefix = {arXiv},
eprint = {1006.0001},
primaryClass = {astro-ph.GA},
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}
@ARTICLE{merritt+2009,
author = {{Merritt}, David and {Gualandris}, Alessia and {Mikkola}, Seppo},
title = "{Explaining the Orbits of the Galactic Center S-Stars}",
journal = {\apjl},
keywords = {galaxies: active, galaxies: evolution, quasars: general, Astrophysics},
year = "2009",
month = "Mar",
volume = {693},
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eprint = {0812.4517},
primaryClass = {astro-ph},
adsurl = {https://ui.adsabs.harvard.edu/abs/2009ApJ...693L..35M},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{tamayo+2019,
author = {{Tamayo}, Daniel and {Rein}, Hanno and {Shi}, Pengshuai and {Hernand
ez}, David M.},
title = "{REBOUNDx: a library for adding conservative and dissipative forces to otherwise symplectic N-body integrations}",
journal = {\mnras},
keywords = {gravitation, methods: numerical, planets and satellites: dynamical evolution and stability, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics},
year = "2020",
month = "Jan",
volume = {491},
number = {2},
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doi = {10.1093/mnras/stz2870},
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eprint = {1908.05634},
primaryClass = {astro-ph.EP},
adsurl = {https://ui.adsabs.harvard.edu/abs/2020MNRAS.491.2885T},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@ARTICLE{rein.spiegel2015,
author = {{Rein}, Hanno and {Spiegel}, David S.},
title = "{IAS15: a fast, adaptive, high-order integrator for gravitational dynamics, accurate to machine precision over a billion orbits}",
journal = {\mnras},
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year = "2015",
month = "Jan",
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archivePrefix = {arXiv},
eprint = {1409.4779},
primaryClass = {astro-ph.EP},
adsurl = {https://ui.adsabs.harvard.edu/abs/2015MNRAS.446.1424R},
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}
@ARTICLE{rein.liu2012,
author = {{Rein}, H. and {Liu}, S. -F.},
title = "{REBOUND: an open-source multi-purpose N-body code for collisional dynamics}",
journal = {\aap},
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year = "2012",
month = "Jan",
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pages = {A128},
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eprint = {1110.4876},
primaryClass = {astro-ph.EP},
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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}",
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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}",
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month = "Feb",
volume = {853},
number = {2},
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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,
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primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2010ApJ...708..834B},
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}
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author = {{Bartko}, H. and {Martins}, F. and {Fritz}, T.~K. and {Genzel}, R. and
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{Sternberg}, A. and {Trippe}, S.},
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month = "Jun",
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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}",
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year = "2013",
month = "Jan",
volume = {763},
number = {1},
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pages = {L10},
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eprint = {1211.4594},
primaryClass = {astro-ph.GA},
adsurl = {https://ui.adsabs.harvard.edu/abs/2013ApJ...763L..10A},
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}
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{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},
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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},
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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},
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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},
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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},
Bdsk-file-1 = {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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},
Bdsk-file-1 = {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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},
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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},
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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},
Bdsk-file-1 = {YnBsaXN0MDDUAQIDBAUGJCVYJHZlcnNpb25YJG9iamVjdHNZJGFyY2hpdmVyVCR0b3ASAAGGoKgHCBMUFRYaIVUkbnVsbNMJCgsMDxJXTlMua2V5c1pOUy5vYmplY3RzViRjbGFzc6INDoACgAOiEBGABIAFgAdccmVsYXRpdmVQYXRoWWFsaWFzRGF0YV8QLC4uLy4uLy4uLy4uL0RvY3VtZW50cy9QYXBlcnMvQmFyLU9yLzIwMTYucGRm0hcLGBlXTlMuZGF0YU8RAYoAAAAAAYoAAgAADE1hY2ludG9zaCBIRAAAAAAAAAAAAAAAAAAAAM1k0ppIKwAAAs69AAgyMDE2LnBkZgAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAACzrz+1a6JOQAAAAAAAAAAAAQABAAACSAAAAAAAAAAAAAAAAAAAAAGQmFyLU9yABAACAAAzWUK2gAAABEACAAA1a7BeQAAAAEAFALOvQABB4gEAAXEKgAFxCkAAhDpAAIAQE1hY2ludG9zaCBIRDpVc2VyczoAYWxla3NleToARG9jdW1lbnRzOgBQYXBlcnM6AEJhci1PcjoAMjAxNi5wZGYADgASAAgAMgAwADEANgAuAHAAZABmAA8AGgAMAE0AYQBjAGkAbgB0AG8AcwBoACAASABEABIALlVzZXJzL2FsZWtzZXkvRG9jdW1lbnRzL1BhcGVycy9CYXItT3IvMjAxNi5wZGYAEwABLwAAFQACAA7//wAAgAbSGxwdHlokY2xhc3NuYW1lWCRjbGFzc2VzXU5TTXV0YWJsZURhdGGjHR8gVk5TRGF0YVhOU09iamVjdNIbHCIjXE5TRGljdGlvbmFyeaIiIF8QD05TS2V5ZWRBcmNoaXZlctEmJ1Ryb290gAEACAARABoAIwAtADIANwBAAEYATQBVAGAAZwBqAGwAbgBxAHMAdQB3AIQAjgC9AMIAygJYAloCXwJqAnMCgQKFAowClQKaAqcCqgK8Ar8CxAAAAAAAAAIBAAAAAAAAACgAAAAAAAAAAAAAAAAAAALG},
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},
Bdsk-file-1 = {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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},
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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},
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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},
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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 = {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},
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},
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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},
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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},
Bdsk-file-1 = {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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},
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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},
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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},
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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},
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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},
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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},
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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},
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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},
Bdsk-file-1 = {YnBsaXN0MDDUAQIDBAUGJCVYJHZlcnNpb25YJG9iamVjdHNZJGFyY2hpdmVyVCR0b3ASAAGGoKgHCBMUFRYaIVUkbnVsbNMJCgsMDxJXTlMua2V5c1pOUy5vYmplY3RzViRjbGFzc6INDoACgAOiEBGABIAFgAdccmVsYXRpdmVQYXRoWWFsaWFzRGF0YV8QLi4uLy4uLy4uLy4uL0RvY3VtZW50cy9QYXBlcnMvRGVnZW5hYXIvMjAxNS5wZGbSFwsYGVdOUy5kYXRhTxEBkAAAAAABkAACAAAMTWFjaW50b3NoIEhEAAAAAAAAAAAAAAAAAAAAzWTSmkgrAAACyrmUCDIwMTUucGRmAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAALUEk/VxIaXAAAAAAAAAAAABAAEAAAJIAAAAAAAAAAAAAAAAAAAAAhEZWdlbmFhcgAQAAgAAM1lCtoAAAARAAgAANXEvtcAAAABABQCyrmUAQeIBAAFxCoABcQpAAIQ6QACAEJNYWNpbnRvc2ggSEQ6VXNlcnM6AGFsZWtzZXk6AERvY3VtZW50czoAUGFwZXJzOgBEZWdlbmFhcjoAMjAxNS5wZGYADgASAAgAMgAwADEANQAuAHAAZABmAA8AGgAMAE0AYQBjAGkAbgB0AG8AcwBoACAASABEABIAMFVzZXJzL2FsZWtzZXkvRG9jdW1lbnRzL1BhcGVycy9EZWdlbmFhci8yMDE1LnBkZgATAAEvAAAVAAIADv//AACABtIbHB0eWiRjbGFzc25hbWVYJGNsYXNzZXNdTlNNdXRhYmxlRGF0YaMdHyBWTlNEYXRhWE5TT2JqZWN00hscIiNcTlNEaWN0aW9uYXJ5oiIgXxAPTlNLZXllZEFyY2hpdmVy0SYnVHJvb3SAAQAIABEAGgAjAC0AMgA3AEAARgBNAFUAYABnAGoAbABuAHEAcwB1AHcAhACOAL8AxADMAmACYgJnAnICewKJAo0ClAKdAqICrwKyAsQCxwLMAAAAAAAAAgEAAAAAAAAAKAAAAAAAAAAAAAAAAAAAAs4=},
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},
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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 I∝r-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},
Bdsk-file-1 = {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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},
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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},
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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 = {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},
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},
Bdsk-file-1 = {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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},
Bdsk-url-2 = {http://arXiv.org/abs/1407.7531},
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},
Bdsk-file-1 = {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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},
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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},
Bdsk-file-1 = {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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},
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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},
Bdsk-file-1 = {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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},
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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},
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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},
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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},
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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},
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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},
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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},
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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},
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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},
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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},
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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},
Bdsk-file-1 = {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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},
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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},
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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},
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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},
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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},
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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},
Bdsk-file-1 = {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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},
Bdsk-file-1 = {YnBsaXN0MDDUAQIDBAUGJCVYJHZlcnNpb25YJG9iamVjdHNZJGFyY2hpdmVyVCR0b3ASAAGGoKgHCBMUFRYaIVUkbnVsbNMJCgsMDxJXTlMua2V5c1pOUy5vYmplY3RzViRjbGFzc6INDoACgAOiEBGABIAFgAdccmVsYXRpdmVQYXRoWWFsaWFzRGF0YV8QLS4uLy4uLy4uLy4uL0RvY3VtZW50cy9QYXBlcnMvS2llZmZlci8yMDE2LnBkZtIXCxgZV05TLmRhdGFPEQGQAAAAAAGQAAIAAAxNYWNpbnRvc2ggSEQAAAAAAAAAAAAAAAAAAADNZNKaSCsAAAK29wEIMjAxNi5wZGYAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAAArb2yNVg1LgAAAAAAAAAAAAEAAQAAAkgAAAAAAAAAAAAAAAAAAAAB0tpZWZmZXIAABAACAAAzWUK2gAAABEACAAA1WEM+AAAAAEAFAK29wEBB4gEAAXEKgAFxCkAAhDpAAIAQU1hY2ludG9zaCBIRDpVc2VyczoAYWxla3NleToARG9jdW1lbnRzOgBQYXBlcnM6AEtpZWZmZXI6ADIwMTYucGRmAAAOABIACAAyADAAMQA2AC4AcABkAGYADwAaAAwATQBhAGMAaQBuAHQAbwBzAGgAIABIAEQAEgAvVXNlcnMvYWxla3NleS9Eb2N1bWVudHMvUGFwZXJzL0tpZWZmZXIvMjAxNi5wZGYAABMAAS8AABUAAgAO//8AAIAG0hscHR5aJGNsYXNzbmFtZVgkY2xhc3Nlc11OU011dGFibGVEYXRhox0fIFZOU0RhdGFYTlNPYmplY3TSGxwiI1xOU0RpY3Rpb25hcnmiIiBfEA9OU0tleWVkQXJjaGl2ZXLRJidUcm9vdIABAAgAEQAaACMALQAyADcAQABGAE0AVQBgAGcAagBsAG4AcQBzAHUAdwCEAI4AvgDDAMsCXwJhAmYCcQJ6AogCjAKTApwCoQKuArECwwLGAssAAAAAAAACAQAAAAAAAAAoAAAAAAAAAAAAAAAAAAACzQ==},
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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