论文标题
高偏心率和高质量表征重力波在银河核中捕获，如地球探测器所见
High Eccentricities and High Masses Characterize Gravitational-wave Captures in Galactic Nuclei as Seen by Earth-based Detectors
论文作者
论文摘要
在银河核（GNS）单个单个近距离相遇期间，重力波（GWS）的发射导致高度偏心的恒星质量黑洞（BH）二进制物的形成和快速合并。物理参数的独特分布使得可以从统计学上区分该来源人群与其他源人群。先前的研究确定了单个GN中该源群体的预期二元参数分布。在这里，我们考虑了动态摩擦，牛顿后校正和观察性偏见的影响，以确定宇宙中所有GN的检测到来源的参数分布。我们发现，检测到的合并的总二元质量分布向更高的质量倾斜。初始峰值GW频率的分布在1-70 Hz之间非常高，约50％的GW捕获源形成了10 Hz以上，E> 〜0.95。首次进入Ligo/处女座/Kagra带时的偏心率满足了92％以上的源> 0.1，而E_10Hz> 0.8> 0.8> 0.8，超过一半的来源。在大约70％以上的偏心率达到10 gm/c^2时，偏心率满足E_10M> 0.1，这使得在GNS中，单个单一的GW捕获事件是当前众所周知的恒星质量 - 质量二进制二进制BH合并通道中最古怪的源人群。我们确定总质量，质量比，源检测距离和偏心率E_10Hz和E_10M之间的相关性。 GW190521的最近测得的源参数位于理论分布的峰值附近，主机环境的估计逃逸速度约为7.5x10^3 km/s -1.2x10^4 km/s，使该源成为该天体合并通道的候选者。
The emission of gravitational waves (GWs) during single-single close encounters in galactic nuclei (GNs) leads to the formation and rapid merger of highly eccentric stellar-mass black hole (BH) binaries. The distinct distribution of physical parameters makes it possible to statistically distinguish this source population from others. Previous studies determined the expected binary parameter distribution for this source population in single GNs. Here we take into account the effects of dynamical friction, post-Newtonian corrections, and observational bias to determine the detected sources' parameter-distributions from all GNs in the Universe. We find that the total binary mass distribution of detected mergers is strongly tilted towards higher masses. The distribution of initial peak GW frequency is remarkably high between 1-70 Hz, ~50% of GW capture sources form above 10 Hz with e >~ 0.95. The eccentricity when first entering the LIGO/Virgo/KAGRA band satisfies e_10Hz > 0.1 for over 92% of sources and e_10Hz > 0.8 for more than half of the sources. At the point when the pericenter reaches 10 GM/c^2 the eccentricity satisfies e_10M > 0.1 for over ~70% of the sources, making single-single GW capture events in GNs the most eccentric source population among the currently known stellar-mass binary BH merger channels in the Universe. We identify correlations between total mass, mass ratio, source detection distance, and eccentricities e_10Hz and e_10M. The recently measured source parameters of GW190521 lie close to the peak of the theoretical distributions and the estimated escape speed of the host environment is ~7.5x10^3 km/s - 1.2x10^4 km/s, making this source a candidate for this astrophysical merger channel.
