论文标题
超紧凑型矮星系中巨大的黑洞的形成：N体模拟中原始中等质量黑洞的迁移
Formation of massive black holes in ultra-compact dwarf galaxies: migration of primordial intermediate-mass black holes in N-body simulation
论文作者
论文摘要
最近对超紧凑型矮星系（UCD）的观察性研究发现了大量黑洞（MBHS），其质量超过$ {10^6〜 \ rm m_ \ odot} $，在其中央地区。我们在这里认为这些MBH可以通过合并中间质量黑洞（IMBH）来形成，$ {[10^3-10^5]〜{\ rm m} _ {\ rom M} _ {\ odot}} $，在Dwarf Galaxies的Stellar核心内，这是ucds of ucds of ucds of ucds of dwarf calaxies。我们使用N体模拟来数字研究为广泛的模型参数研究。这意味着在这项研究中忽略了IMBH的增长和反馈。我们发现，只有$ 10^5〜 \ rm m_ \ odot $的大规模IMBH沉入其主机矮人的中心区域（$ \ \ \ \ \ \ \ \ rm m_ \ odot $）在大多数dwarf模型中都在小于1 gyr中被其恒星核所困在重力中。我们还发现，具有$ [1-30] \ times 10^3〜 \ rm m_ \ odot $的较轻的IMBHS因低质量dwarfs（$ \ of 10^{9}〜\ rm m_ \ odot $）而进入中心（由于更有效的动态摩擦（DF），此外，我们表明IMBHS可以在中心形成二进制文件，并且很少在到达中心之前，这可能导致IMBH合并，从而发射了Lisa可以检测到的引力波。最后，我们讨论UCD中MBH形成的IMBH数量以及恒星核在IMBH二进制和合并中的物理作用。
Recent observational studies of ultra-compact dwarf galaxies (UCDs) have discovered massive black holes (MBHs) with masses of more than ${10^6~\rm M_\odot}$, in their central regions. We here consider that these MBHs can be formed through merging of intermediate-mass black holes (IMBH), with masses of ${[10^3-10^5]~{\rm M}_{\odot}}$, within the stellar nuclei of dwarf galaxies, which are progenitors of UCDs. We numerically investigate this formation process for a wide range of model parameters using N-body simulations. This means that IMBH growth and feedback is neglected in this study. We find that only massive IMBHs of $10^5~\rm M_\odot$ sink into the central regions of their host dwarf ($\approx 10^{10}~\rm M_\odot$) to be gravitationally trapped by its stellar nucleus within less than 1 Gyr in most dwarf models. We also find that lighter IMBHs with $[1 - 30] \times 10^3~\rm M_\odot$ sink into the centre in low-mass dwarfs ($\approx 10^{9}~\rm M_\odot$) due to more efficient dynamical friction (DF). Additionally, we show that the IMBHs can form binaries in the centre and, rarely, before they reach the centre, which may lead to the IMBHs merging and thus emitting gravitational waves that could be detected by LISA. Finally, we discuss the required number of IMBHs for the MBH formation in UCDs and the physical roles of stellar nuclei in IMBH binaries and mergers.
