活动星系核垂直分层盘中双黑洞的流体动力学演化
The hydrodynamic evolution of binary black holes embedded within the vertically stratified disks of active galactic nuclei
摘要：
恒星质量的黑洞可以嵌入活动星系核（AGN）的气体盘中。之后，它们的相互作用由它们的气体环境介导。在这项工作中，我们研究了恒星质量的双黑洞（BBH）嵌入活动星系核盘的三维流体动力学模拟和分析方法相结合的演化，专注于环境中的活动星系核盘尺度高度$H$是$\gtrsim$的BBH球的影响。我们使用风洞形式主义嵌入BBHs的本地环境建模和表征不同的吸积制度的基础上的磁盘的本地属性，范围从风为主的准球形。我们使用我们的模拟开发处方的质量吸积和阻力嵌入BBHs。我们使用这些处方，随着活动星系盘模型，可以代表Toomre不稳定的外部区域的活动星系盘，研究的BBH的长期演变，因为他们通过磁盘迁移。我们发现，BBH通常合并在$\lesssim 5-30\,{\rm Myr}$，增加他们的质量显着的过程中，允许BBH进入（或交叉）对不稳定超新星质量间隙。向这些BBH供应气体的速率通常超过爱丁顿极限，有时超过几个数量级。我们的结论是，大多数嵌入式BBH将合并之前迁移显着的磁盘。根据周围气体的条件和到系统的距离，LISA可以检测到气体主导和引力波主导的制度之间的过渡，以吸入足够接近AGN（$\lesssim$ 0.1 pc）形成的BBH。我们还讨论了可能的电磁签名期间和之后的inspiral，发现它一般是不太可能的，但不是不可想象的BBH的热光度超过主机活动星系核。
英文摘要：
Stellar-mass black holes can become embedded within the gaseous disks of active galactic nuclei (AGNs). Afterwards, their interactions are mediated by their gaseous surroundings. In this work, we study the evolution of stellar-mass binary black holes (BBHs) embedded within AGN disks using a combination of three-dimensional hydrodynamic simulations and analytic methods, focusing on environments in which the AGN disk scale height $H$ is $\gtrsim$ the BBH sphere of influence. We model the local surroundings of the embedded BBHs using a wind tunnel formalism and characterize different accretion regimes based on the local properties of the disk, which range from wind-dominated to quasi-spherical. We use our simulations to develop prescriptions for mass accretion and drag for embedded BBHs. We use these prescriptions, along with AGN disk models that can represent the Toomre-unstable outer regions of AGN disks, to study the long-term evolution of the BBHs as they migrate through the disk. We find that BBHs typically merge within $\lesssim 5-30\,{\rm Myr}$, increasing their mass significantly in the process, allowing BBHs to enter (or cross) the pair-instability supernova mass gap. The rate at which gas is supplied to these BBHs often exceeds the Eddington limit, sometimes by several orders of magnitude. We conclude that most embedded BBHs will merge before migrating significantly in the disk. Depending on the conditions of the ambient gas and the distance to the system, LISA can detect the transition between the gas-dominated and gravitational wave dominated regime for inspiraling BBHs that are formed sufficiently close to the AGN ($\lesssim$ 0.1 pc). We also discuss possible electromagnetic signatures during and following the inspiral, finding that it is generally unlikely but not inconceivable for the bolometric luminosity of the BBH to exceed that of the host AGN.
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