论文标题
关于恒星背景中巨大黑洞二进制的偏心演变
On the eccentricity evolution of massive black hole binaries in stellar backgrounds
论文作者
论文摘要
我们通过一组大量的三个身体散射实验来研究与未结合的恒星相互作用的偏心巨大黑洞二进制（MBHB）的动力演化。与以前的研究相比，我们将调查扩展到MBHB质量比为$ q = m_2/m_1 = 10^{ - 4} $，其中$ m_1 $和$ m_2 $分别是主要和次要孔的质量。与较高质量比的简单推断相反，我们发现对于$ q \ lyssim 10^{ - 3} $，偏心率的增长率变为负，即，随着二进制{\ it循环}的收缩。这种行为是由于在亚稳态的反旋转轨道中捕获的相互作用恒星的子集。这些恒星倾向于从二进制中提取角动量，以$ q>>> 10^{ - 3} $促进偏心率的增长，但倾向于将角动量注入二元动力，以$ q <10^{ - 3} $以圆形化的速度朝向循环。这种行为的物理起源需要详细研究该恒星子集的轨道，目前正在研究中。我们的发现可能会对中间MBHS（IMBHS）产生重要的影响（例如，推定的$ 10^3 \ rm m _ {\ odot} $ Black Hole Inspiralling在Sgra $^*$上启发了Black Hole。
We study the dynamical evolution of eccentric massive black hole binaries (MBHBs) interacting with unbound stars by means of an extensive set of three body scattering experiments. Compared to previous studies, we extend the investigation down to a MBHB mass ratio of $q=m_2/m_1=10^{-4}$, where $m_1$ and $m_2$ are the masses of the primary and secondary hole respectively. Contrary to a simple extrapolation from higher mass ratios, we find that for $q\lesssim 10^{-3}$ the eccentricity growth rate becomes negative, i.e., the binary {\it circularises} as it shrinks. This behaviour is due to the subset of interacting stars captured in metastable counter-rotating orbits; those stars tend to extract angular momentum from the binary, promoting eccentricity growth for $q>10^{-3}$, but tend to inject angular momentum into the binary driving it towards circularisation for $q<10^{-3}$. The physical origin of this behaviour requires a detailed study of the orbits of this subset of stars and is currently under investigation. Our findings might have important consequences for intermediate MBHs (IMBHs) inspiralling onto MBHs (e.g. a putative $10^3\rm M_{\odot}$ black hole inspiralling onto SgrA$^*$).
