湿极端质量比吸气可能更常见于星载引力波探测
Wet Extreme Mass Ratio Inspirals May Be More Common For Spaceborne Gravitational Wave Detection
摘要：
极端质量比吸气（EMRI）可根据其形成机制分为干EMRI和湿EMRI。干（或“损失锥”）EMRI，以前被认为是激光干涉仪空间天线的主要EMRI源，主要是由核星团中的多体散射和引力捕获产生的。在这项工作中，我们强调了另一种EMRI形成通道：（湿）EMRI形成的吸积流周围的吸积星系中心的大质量黑洞（MBHs）的协助。在这个通道中，吸积盘捕获了最初在倾斜轨道上运动的恒星质量的黑洞，并随后驱使它们向MBH迁移-这个过程将这些星系中EMRI的形成速度提高了几个数量级。考虑到部分（$\mathcal O(10^{-2}-10^{-1})$）的活动星系核的MBH预计将迅速吸积，我们预测，湿EMRI将贡献一个重要的，甚至占主导地位的部分，所有可探测的EMRI的星载引力波探测器。
英文摘要：
Extreme Mass Ratio Inspirals (EMRIs) can be classified as dry EMRIs and wet EMRIs based on their formation mechanisms. Dry (or the "loss-cone") EMRIs, previously considered as the main EMRI sources for the Laser Interferometer Space Antenna, are primarily produced by multi-body scattering in the nuclear star cluster and gravitational capture. In this work, we highlight an alternative EMRI formation channel: (wet) EMRI formation assisted by the accretion flow around accreting galactic-center massive black holes (MBHs). In this channel, the accretion disk captures stellar-mass black holes that are intially moving on inclined orbits, and subsequently drives them to migrate towards the MBH - this process boosts the formation rate of EMRIs in such galaxies by orders of magnitude. Taking into account the fraction ($\mathcal O(10^{-2}-10^{-1})$) of active galactic nuclei where the MBHs are expected to be rapidly accreting, we forecast that wet EMRIs will contribute an important or even dominant fraction of all detectable EMRIs by spaceborne gravitational wave detectors.
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