论文标题
作为SGR A*的邻居的恒星质量黑洞的科学潜力*
Science Potential for Stellar-mass Black Holes as Neighbors of Sgr A*
论文作者
论文摘要
有人建议，可能存在一类恒星质量的黑洞（BHS），居住在（距离$ \ le 10^3 m $）的Galactic Center Massive Black Hole，Sgr a*。可能的地层场景包括大量恒星质量黑洞的质量隔离和/或磁盘迁移，如果SGR a*附近有主动积聚流量，则在$ \ Mathcal {O}（10）$ MYR中。在这项工作中，我们探索了这种类型的对象作为太空传播引力波检测器的源，例如激光干涉仪空间天线（LISA）。我们发现，可以根据这些恒星质量黑洞的轨道平面的动力来探测Sgr a*的旋转。我们还表明，SGR A附近的累积冷暗物质产生的动力摩擦通常会在重力波形中产生小的可测量相移。在SGR A*附近有轴云的情况下，仅当轴支球场的质量在质谱的狭窄范围内时，动态摩擦引起的重力波形才能测量。轴云与恒星质量黑洞之间的重力相互作用可能会引入SGR A*旋转的其他进动。这种额外的进动率通常比自旋诱导的裂纹进动率弱，但仍可能在某个参数方面污染自旋测量。最后，我们指出，这些恒星质量黑洞之间的多体性重力相互作用通常会在丽莎寿命期间可忽略不计。
It has been suggested that there is possibly a class of stellar-mass black holes (BHs) residing near (distance $\le 10^3 M$) the galactic center massive black hole, Sgr A*. Possible formation scenarios include the mass segregation of massive stellar-mass black holes and/or the disk migration if there was an active accretion flow near Sgr A* within $\mathcal{O}(10)$ Myr. In this work, we explore the application of this type of objects as sources of space-borne gravitational wave detectors, such as Laser Interferometer Space Antenna (LISA). We find it is possible to probe the spin of Sgr A* based on the precession of the orbital planes of these stellar-mass black holes moving around Sgr A*. We also show that the dynamical friction produced by accumulated cold dark matter near Sgr A* generally produces small measurable phase shift in the gravitational waveform. In the case that there is an axion cloud near Sgr A*, the dynamical friction induced modification to gravitational waveform is measurable only if the mass of the axion field is in a narrow range of the mass spectrum. Gravitational interaction between the axion cloud and the stellar-mass black holes may introduce additional precession around the spin of Sgr A*. This additional precession rate is generally weaker than the spin-induced Lense-Thirring precession rate, but nevertheless may contaminate the spin measurement in a certain parameter regime. At last, we point out that the multi-body gravitational interaction between these stellar-mass black holes generally causes negligible phase shift during the LISA lifetime.
