论文标题
宇宙超级二进制黑洞的动力演化及其重力波辐射
Dynamical evolution of cosmic supermassive binary black holes and their gravitational wave radiation
论文作者
论文摘要
我们研究了具有逼真的特性分布的星系中超质量二元黑洞（BBH）的演变，并从这些BBH的宇宙种群中进行了重力波（GW）辐射。我们通过包括银河系三轴形状和内部恒星分布的影响，并产生大量的BBH进化轨道，对BBHS的动态相互作用进行全面处理。通过将这些BBH进化轨道，星系质量函数，星系合并率和超大质量的黑洞 - 宿主星系关系结合在一起，我们获得了存活的BBHS，BBH合并率的统计分布，GW辐射的强度，其GW辐射的强度以及随机GW背景（GWB）贡献了COSMIC BB BB人群。预计附近银河中心的超质量BHS的约1％-3％（或〜10％）预计将是质量比> 1/3（OR> 1/100）的二进制文件。频率为1/yr时GWB的特征应变振幅估计为$ 2.0^{+1.4} _ { - 0.8} \ times 10^{ - 16} $，其结果的上限以及其在不同的BH-Host Galaxy关系中获得的结果可以达到$ 5.4 \ 5.4 \ 5.4 \ 5.4 \ 5.4 \ 5.4 \ 5.4 \ 5.4 \ e.g { - E.g { - E.g，这是未来的，这是未来的。阵列，快速，下一代非常大的阵列）。 GWB频谱的周转频率为〜0.25NHz。还讨论了以上估计的不确定性和检测单个来源的前景。宇宙BBH种群在激光干涉仪空间天线（LISA）带中的应用为LISA的BBH检测率提供了下限，〜0.9/yr。
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 the 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 ~10%) of supermassive BHs at nearby galactic centers are expected to be binaries with mass ratio >1/3 (or >1/100). The characteristic strain amplitude of the GWB at frequency 1/yr is estimated to be ~$2.0^{+1.4}_{-0.8}\times 10^{-16}$, and the upper bound of its results obtained with the different BH-host galaxy relations can be up to $5.4\times 10^{-16}$, 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 ~0.25nHz. 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, ~0.9/yr.
