超大质量黑洞附近的双星并合--动力学演化的长期效应  

Binary mergers near the supermassive black hole-Secular effect in the orbital evolution

作　　者：刘彬[1] Bin Liu(Institute of Astronomy,School of Physics,Zhejiang University,Hangzhou 310058,China)

机构地区：[1]浙江大学物理学院天文研究所,杭州310058

出　　处：《科学通报》2025年第3期373-386,共14页Chinese Science Bulletin

基　　金：国家自然科学基金海外高层次人才项目资助。

摘　　要：通常情况下,星系中心包含一个超大质量黑洞与环绕其周围的核星团.星团内部广泛分布着恒星、致密星,甚至是双星系统.在这种环境中,许多独特的物理过程相互作用,共同影响双星的演化.随着由并合双黑洞产生的引力波的发现,人们开展大量研究工作来理解双致密星的形成与并合.在此,我们从理论角度回顾了双星如何在中心超大质量黑洞的长期影响下演化直至发生并合,总结了由超大质量黑洞诱导产生并合这一渠道的关键结论,并概述了潜在的可观测特征.The center of a galaxy is expected to contain a supermassive black hole(SMBH)surrounded by a nuclear star cluster.Inside the cluster,there is a broad distribution of stars,compact objects,and even binary systems.In such an environment,the evolution of binaries can be affected by a variety of physical processes.With the discovery of gravitational waves(GWs)from merging black hole binaries(BHBs),extensive research has been conducted to understand the formation and merger of compact binaries.Here,we theoretically review how binaries evolve and eventually merge under the long-term influence of a central SMBH.We summarize the key conclusions of this dynamical channel of mergers,including:(1)Gravitational perturbation from the SMBH induces von Zeipel-Lidov-Kozai(ZLK)eccentricity oscillations of the BHB,which leads to enhanced gravitational radiation and merger of the BHB.The maximum eccentricity of the BHB due to ZLK effect can be derived analytically and the modified merger time of the BHB is presented.In this tertiary induced channel,we find that the spins of black holes(BHs)preferentially lie in the orbital plane when the BHB enters the LIGO band.(2)Because the tertiary(SMBH)mass is much larger than the masses of the inner BHB,several general relativity(GR)effects involving the SMBH can generate extra precessions on the binary orbits and qualitatively change the dynamics,significantly increasing the inclination window for mergers and producing a wide range of spin orientations when the BHB enters LIGO band.For the BHBs that emit GWs in the low-frequency band(0.001–1 Hz),we show that the rate of change of the angular momentum vector of the BHB encodes the information on the spin of the SMBH due to the GR effects.Detecting GWs from compact binaries around SMBHs can provide a new probe of the spins of SMBHs.When the BHB moves around the SMBH in a less inclined orbit,we show that the inner binary can encounter an“apsidal precession resonance”and experience eccentricity excitation during the orbital decay due to gr

关 键 词：黑洞 引力波 N体问题 共振 

分 类 号：P145.8[天文地球—天体物理] P153[天文地球—天文学]