论文标题
银河中心紧凑型物体二进制的重力波签名
Gravitational-Wave Signatures from Compact Object Binaries in the Galactic Center
论文作者
论文摘要
几乎每个星系都有一个超级质量的黑洞（SMBH），该黑洞（SMBH）包括银河系，其中包括银河系。最近的研究表明，这些独特的地方有望拥有大量的恒星和紧凑的物体二进制物。这些二进制文件与SMBH形成分层三重系统，并经历了偏心的Kozai-Lidov（EKL）机制。在这里，我们估计了这些紧凑物体在激光干涉仪空间天线（LISA）和激光干涉仪重力波观测站（Ligo）和处女座探测器中的这些紧凑物体中的潜在引力波排放的可检测性。我们在Roche极限越过开始时产生了恒星后的恒星种群，并遵循其进化以紧凑的物体二进制。作为概念验证，我们采用了两种金属，太阳金属（$ z = 0.02 $）和$ 15 \％$ $ $ $ $（$ z = 0.003 $）。我们证明，在观察时间尺度上，丽莎，黑洞二进制（BH-BH）和白矮人二进制文件通过EKL辅助合并通道提供了最突出的GW来源。涉及中子恒星的系统不太明显，但通过不同的合并通道可能很丰富。我们的人口合成$ z = 0.02 $（$ z = 0.003 $）的BH-BH合成为$ \ sim $ $ 4 $（$ 24 $）事件，在1 $ {\ rm gpc}^3 $ sphere中，Ligo与Ligo一起使用。我们还估计了我们银河中心（以及可能的其他星系）内部parsec内可见的二进制数量约为14-150 WD -WD，0-2 NS -BH，0.2-4 NS -NS -NS和0.3-4 NS -NS和0.3-20 BH -BH。
Almost every galaxy has a supermassive black hole (SMBH) residing at its center, the Milky Way included. Recent studies suggest that these unique places are expected to host a high abundance of stellar and compact object binaries. These binaries form hierarchical triple systems with the SMBH and undergo the eccentric Kozai-Lidov (EKL) mechanism. Here we estimate the detectability of potential Gravitational-Wave emissions from these compact objects within the frequency band of the Laser Interferometer Space Antenna (LISA) and Laser Interferometer Gravitational-Wave Observatory (LIGO) and Virgo detectors. We generate a post EKL population of stars at the onset of Roche limit crossing and follow their evolution to compact object binaries. As a proof-of-concept, we adopt two metallicities, solar metallicity ($Z = 0.02$) and $15\%$ of it ($Z = 0.003$). We demonstrate that over the observation timescale of LISA, black hole binaries (BH-BH) and white dwarf binaries provide the most prominent GW sources via the EKL assisted merger channel. Systems involving neutron stars are less observable but possibly abundant through different merger channels. Our population synthesis of BH-BH with $Z = 0.02$ ($Z = 0.003$) translate to $\sim$ $4$ ($24$) events per year with LIGO within a 1 ${\rm Gpc}^3$ sphere. We also estimated the number of binaries visible in the LISA band within the inner parsec of our galactic center (and possibly other galaxies) to be about 14 - 150 WD-WD, 0 - 2 NS-BH, 0.2 - 4 NS-NS, and 0.3 - 20 BH-BH.
