论文标题
块状星系中引力波和潮汐破坏的产生
Generation of gravitational waves and tidal disruptions in clumpy galaxies
论文作者
论文摘要
对中间质量黑洞（IMBH）的更好理解至关重要，因为它们的性质可能会阐明其超大质量对应物的起源和生长。 IMBHS可以居住的场所之一，是$ z \ sim $ 1-3的大量大型星系中存在的大型星形团块。 We perform a series of Fokker-Planck simulations to explore the occurrence of tidal disruption (TD) and gravitational wave (GW) events about an IMBH in a massive star-forming clump, modelling the latter so that its mass ($10^8 \,{\rm M}_{\odot}$) and effective radius ($100$ pc) are consistent with the properties of both observed和模拟团块。我们发现，TD和GW事件率在$ 10^{ - 6} $ - $ 10^{ - 5} $和$ 10^{ - 8} $ - $ 10^{ - 7} $ 10^{ - 7} $ yr $^{ - 1} $，取决于$ prop的初始内部密度propto（$ prop）的假设（或r^{ - 1} $）和中央IMBH的初始质量（$ 10^5 $或$ 10^3 \，{\ rm m} _ {\ odot} $）。通过整合超过$ z $ = 1-3的GW事件速率，我们预计激光干涉仪空间天线将能够检测到来自这些大型团块的每年$ \ sim $ 2 GW事件；这些系统的TD事件的内在速率相反，每年几美元^3 $，其中一小部分将由例如平方公里阵列和高能天体物理学的高级望远镜。总之，我们的结果支持了即将到来的GW和电磁设施的想法，可能有前所未有的机会揭示了潜伏的IMBH人群。
Obtaining a better understanding of intermediate-mass black holes (IMBHs) is crucial, as their properties could shed light on the origin and growth of their supermassive counterparts. Massive star-forming clumps, which are present in a large fraction of massive galaxies at $z \sim$ 1-3, are amongst the venues wherein IMBHs could reside. We perform a series of Fokker-Planck simulations to explore the occurrence of tidal disruption (TD) and gravitational wave (GW) events about an IMBH in a massive star-forming clump, modelling the latter so that its mass ($10^8 \,{\rm M}_{\odot}$) and effective radius ($100$ pc) are consistent with the properties of both observed and simulated clumps. We find that the TD and GW event rates are in the ranges $10^{-6}$-$10^{-5}$ and $10^{-8}$-$10^{-7}$ yr$^{-1}$, respectively, depending on the assumptions for the initial inner density profile of the system ($ρ\propto r^{-2}$ or $\propto r^{-1}$) and the initial mass of the central IMBH ($10^5$ or $10^3\,{\rm M}_{\odot}$). By integrating the GW event rate over $z$ = 1-3, we expect that the Laser Interferometer Space Antenna will be able to detect $\sim$2 GW events per yr coming from these massive clumps; the intrinsic rate of TD events from these systems amounts instead to a few $10^3$ per yr, a fraction of which will be observable by, e.g. the Square Kilometre Array and the Advanced Telescope for High Energy Astrophysics. In conclusion, our results support the idea that the forthcoming GW and electromagnetic facilities may have the unprecedented opportunity of unveiling the lurking population of IMBHs.
