Dynamical Evolution of Cosmic Supermassive Binary Black Holes and Their Gravitational-wave Radiation
Dynamical Evolution of Cosmic Supermassive Binary Black Holes and Their Gravitational-wave Radiation
复制标题
宇宙超大质量双黑洞的动力学演化及其引力波辐射
DOI：
10.3847/1538-4357/ab9594
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发表时间：
2020-05
影响因子：
4.9
通讯作者：
Lu Youjun
中科院分区：
文献类型：
--
作者：
Chen Yunfeng;Yu Qingjuan;Lu Youjun
我们研究具有实际属性分布的星系中特大质量双黑洞（BBHs）的演化，以及来自这些双黑洞的宇宙群体的引力波（GW）辐射。我们对……进行了全面的处理（原句“dy”不完整，可能影响准确理解）
We investigate the evolution of supermassive binary black holes (BBHs) in galaxies with realistic property distributions and the gravitational-wave (GW) radiation from the cosmic population of these BBHs. We incorporate a comprehensive treatment of the dynamical interactions of the BBHs with their environments by including the effects of galaxy triaxial shapes and inner stellar distributions, and generate a large number of BBH evolution tracks. By combining these BBH evolution tracks, galaxy mass functions, galaxy merger rates, and supermassive black hole–host galaxy relations into our model, we obtain statistical distributions of surviving BBHs, BBH coalescence rates, the strength of their GW radiation, and the stochastic GW background (GWB) contributed by the cosmic BBH population. About ∼1%–3% (or ) of supermassive BHs at nearby galactic centers are expected to be binaries with mass ratio (or ). The characteristic strain amplitude of the GWB at frequency is estimated to be , and the upper bound of its results obtained with the different BH–host galaxy relations can be up to , which await testing by future experiments (e.g., the Square Kilometer Array, FAST, Next-Generation Very Large Array). The turnover frequency of the GWB spectrum is at . The uncertainties on the above estimates and prospects for detecting individual sources are also discussed. The application of the cosmic BBH population to the Laser Interferometer Space Antenna (LISA) band provides a lower limit to the detection rate of BBHs by LISA, .
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DOI：
10.1111/j.1745-3933.2011.01073.x
发表时间：
2011-05
影响因子：
--
作者：
A. Sesana;A. Gualandris;M. Dotti
通讯作者：
A. Sesana;A. Gualandris;M. Dotti
DOI：
10.1086/519229
发表时间：
2006-09
期刊：
The Astrophysical Journal
影响因子：
--
作者：
T. Lauer;K. Gebhardt;S. Faber;D. Richstone;S. Tremaine;J. Kormendy;M. Aller;R. Bender;A. Dressler;A. Filippenko;R. Green;L. Ho
通讯作者：
T. Lauer;K. Gebhardt;S. Faber;D. Richstone;S. Tremaine;J. Kormendy;M. Aller;R. Bender;A. Dressler;A. Filippenko;R. Green;L. Ho
DOI：
10.1111/j.1365-2966.2009.14396.x
发表时间：
2008-12
影响因子：
4.8
作者：
C. Conselice;Cui Yang;A. Bluck
通讯作者：
C. Conselice;Cui Yang;A. Bluck
影响因子：
4.8
作者：
S. Rodr'iguez;N. Padilla
通讯作者：
S. Rodr'iguez;N. Padilla
DOI：
10.1088/0004-637x/783/2/85
发表时间：
2013-09
期刊：
The Astrophysical Journal
影响因子：
--
作者：
A. Tomczak;R. Quadri;K. Tran;I. Labbé;C. Straatman;Casey;Papovich;K. Glazebrook;R. Allen
通讯作者：
A. Tomczak;R. Quadri;K. Tran;I. Labbé;C. Straatman;Casey;Papovich;K. Glazebrook;R. Allen