发表机构
Saint Mary’s University; Universitat de Barcelona (UB); ICREA; Institut d’Estudis Espacials de Catalunya (IEEC); Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik; Max Planck Institute for Astronomy; Department of Physics and Astronomy, University of Heidelberg（圣玛丽大学; 巴塞罗那大学; 加泰罗尼亚高级研究院; 加泰罗尼亚空间研究所; 海德堡大学天文学中心理论天体物理研究所; 马克斯·普朗克天文学研究所; 海德堡大学物理与天文系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过多种黑洞形成与踢出处方拟合银河系球状星团，发现初始密度与黑洞质量分数线性相关，且模型结果对处方稳健，影响双黑洞并合与中等质量黑洞增长。
AI 中文摘要
球状星团（GCs）中的恒星质量黑洞（BHs）种群在其动力学演化中起着关键作用，然而围绕其形成和保留的机制尚不确定。在本工作中，我们扩展了论文I的分析，通过将耦合的快速星团演化模型和多质量平衡模型拟合到大量银河系球状星团样本，并采用多种恒星演化、黑洞形成和超新星（SN）原生踢的处方。我们探讨了采用SSE或PARSEC（通过SEVN）处方对黑洞初始-最终质量关系的影响，快速或延迟的SN回落机制，以及一个临时踢强度网格，该网格会弹出所有形成的黑洞的40%至80%。尽管所有模型从显著不同的初始黑洞种群出发，但由于初始星团密度与初始黑洞质量分数之间发现的相关性，它们都再现了相同的当前条件。在（对数）初始半质量密度与初始黑洞质量分数之间发现了线性关系，其中SEVN模型导致的中值密度（$\rho_{h,0} \sim 10^{7.2\pm1.1}\\,{M_\odot pc^{-3}}$）比SSE（$\rho_{h,0} \sim 10^{6.4\pm0.9}\\,{M_\odot pc^{-3}}$）高出近一个数量级。我们还发现，先前推断的底部轻初始质量函数和当前黑洞质量分数相对稳健，不受所假设的恒星演化模型和原生踢处方的影响。最后，我们讨论了这些结果对动力学双黑洞并合的预期数量和性质以及中等质量黑洞增长的影响。
英文摘要
The populations of stellar-mass black holes (BHs) in globular clusters (GCs) play a key role in their dynamical evolution, however the mechanisms surrounding their formation and retention are uncertain. In this work, we extend the analysis of Paper I by fitting coupled rapid cluster evolution and multimass equilibrium models to a large sample of Milky Way GCs, under a variety of prescriptions for stellar evolution, BH formation and supernovae (SN) natal kicks. We explore the impacts of adopting SSE or PARSEC (through SEVN) prescriptions for BH initial-final mass relations, the rapid or delayed SN fallback mechanisms, and an ad hoc grid of kick strengths ejecting between 40 and 80 per cent of all BHs formed. All models reproduce the same present-day conditions despite starting from notably different initial BH populations, due to the correlation found between the initial cluster densities and initial BH mass fractions. A linear relationship is found between the (log) initial half-mass density and the initial BH mass fraction, with the SEVN models resulting in median densities ($ρ_{h,0} \sim 10^{7.2\pm1.1}\,{M_\odot pc^{-3}}$) nearly an order of magnitude higher than those of SSE ($ρ_{h,0} \sim 10^{6.4\pm0.9}\,{M_\odot pc^{-3}}$). We also find that both the bottom-light initial mass functions and the present-day BH mass fractions previously inferred are relatively robust against the stellar evolution models and natal kick prescriptions assumed. Finally, we discuss the implications of these results on the expected numbers and properties of dynamical binary-BH mergers, and the growth of intermediate-mass BHs.
Comments17 pages, 12 figures. Submitted to ApJ, comments welcome
