论文标题
将恒星和中等质量的黑洞融合在密集的簇中：对Ligo，Lisa和下一代重力波检测器的影响
Merging stellar and intermediate-mass black holes in dense clusters: implications for LIGO, LISA and the next generation of gravitational wave detectors
论文作者
论文摘要
我们研究了由两个恒星黑洞（BHS）与居住在一个密集的星团中心居住的中间质量BH（IMBH）之间相互作用引起的中间质量比率灵感（IMRI）的形成。我们利用$ n $ - 体模型，以改变IMBH质量，出色的BH质量谱和星团属性。这些模拟与半分析程序相结合，以表征残留IMBH的演变。 IMRIS组概率达到值$ \ sim 5-50 \％$，较大的值对应于较大的IMBH质量。 Imris映射出恒星的BH质量谱，因此可以用来揭开带有IMBH的星形群中的BH种群。在IMRI阶段之后，IMBH最初几乎最大（几乎是非旋转）倾向于减少（增加）其自旋。如果IMBHS主要通过重复的IMRIS生长，我们表明只有IMBH种子足够大（$ M _ {\ rm SEED}> 300 $ M $ _ \ odot $）才能长达$ M _ {\ rm imbh}> 10^3 $ M $ _ \ odot $ _ \ odot $。假设这些种子以红移$ z \ sim 2-6 $形式形成，我们发现它们的$ 1-5 \％$将达到质量$ \ sim 500-1500 $ m $ _ \ odot $ at Redshift $ z = 0 $，并且会表现出低启动，并且会呈现低启动，$ s _ {\ rm imbh} <0.2 $ 0.2 $ 0.2 $。测量与IMRIS有关的IMBH的质量和自旋可以帮助阐明其形成机制。我们证明，丽莎可以以银河系的imbhs检测IMBH，具有信噪比SNR $ = 10-100 $的球形群集，或者在SNR $ = 8-40 $的大麦哲伦云中。我们提供Ligo的IMRIS合并率（$γ_ {\ rm lig} = 0.003-1.6 $ yr $^{ - 1} $），lisa（$γ_ {\ rm lis lis} = 0.02-60 $ yr $^yr $^{ - 1} $^{ - 1} $} yr $^{ - 1} $）和decigo（$γ_ {\ rm dec} = 6-3000 $ yr $^{ - 1} $）。我们的模拟表明，IMRIS的质量和自旋编码对调节IMBH形成的机制的关键见解，并且不同检测器之间的协同作用将使我们能够完全公开它们。 （简略）
We study the formation of intermediate-mass ratio inspirals (IMRIs) triggered by the interactions between two stellar black holes (BHs) and an intermediate-mass BH (IMBH) inhabiting the centre of a dense star cluster. We exploit $N$-body models varying the IMBH mass, the stellar BH mass spectrum, and the star cluster properties. These simulations are coupled with a semi-analytic procedure to characterise the evolution of the remnant IMBH. The IMRIs formation probability attains values $\sim 5-50\%$, with larger values corresponding to larger IMBH masses. IMRIs map out the stellar BH mass spectrum, thus they might be used to unravel BH populations in star clusters harboring an IMBH. After the IMRI phase, an IMBH initially nearly maximal(almost non-rotating) tends to decrease(increase) its spin. If IMBHs grow mostly via repeated IMRIs, we show that only IMBH seeds sufficiently massive ($M_{\rm seed} > 300$ M$_\odot$) can grow up to $M_{\rm imbh} >10^3$ M$_\odot$ in dense globular clusters. Assuming that these seeds form at a redshift $z\sim 2-6$, we find that around $1-5\%$ of them would reach masses $\sim 500-1500$ M$_\odot$ at redshift $z=0$ and would exhibit low-spins, $S_{\rm imbh} < 0.2$. Measuring the mass and spin of IMBHs involved in IMRIs could help unravelling their formation mechanisms. We show that LISA can detect IMBHs in Milky Way globular clusters with a signal-to-noise ratio SNR$=10-100$, or in the Large Magellanic Cloud with an SNR$=8-40$. We provide the IMRIs merger rate for LIGO ($Γ_{\rm LIG} = 0.003-1.6$ yr$^{-1}$), LISA ($Γ_{\rm LIS} = 0.02-60$ yr$^{-1}$), ET ($Γ_{\rm ET} = 1-600$ yr$^{-1}$), and DECIGO ($Γ_{\rm DEC} = 6-3000$ yr$^{-1}$). Our simulations show that IMRIs' mass and spin encode crucial insights on the mechanisms that regulate IMBH formation and that the synergy among different detectors would enable us to fully unveil them. (Abridged)
