利用POPKIN对银河系中恒星质量黑洞的普查。I. 孤立黑洞
A Census of Stellar-mass Black Holes in the Milky Way with POPKIN. I. Isolated Black Holes
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中文总结 AI 辅助
本文提出POPKIN框架，结合恒星演化与轨道动力学，模拟银河系孤立黑洞种群，发现其丰度主要由超新星处方决定，并预测微透镜事件可约束黑洞形成物理。
中文摘要 AI 辅助
引力波观测已揭示出数百个恒星质量黑洞，然而在银河系中已知的仅有约二十余个，且几乎全部位于双星系统中。我们提出了POPKIN，一个Python框架，它将单星和双星演化与银河系轨道动力学相结合，以追踪从零年龄主序到现今孤立黑洞（IBH）种群的黑色洞前身星。在十个模型中，变化超新星（SN）处方、质量转移效率和公共包层抛射效率，总IBH丰度主要由SN处方控制。我们的基准模型采用最近提出的依赖于金属丰度和剥离历史的SN处方，预测银河系中约有$\sim4\times10^7$个IBH，其中包括在太阳1千秒差距（kpc）范围内约有$\sim8\times10^4$个；其他SN处方预测约有$\sim(1-2)\times10^8$个IBH。基准模型产生双峰质量分布，峰值分别在约$9\\,M_{\odot}$和$20\\,M_{\odot}$附近，在$13-17\\,M_{\odot}$范围内存在亏损。这使其区别于其他处方，其中一些处方填充了$2-5\\,M_{\odot}$质量间隙区域。未受踢的IBH在银道面附近沿近圆轨道运行，典型本动速度为$20-30\\,\rm{km\\,s^{-1}}$，而受踢系统经历更强的径向迁移，速度范围更广。我们估计约有$\sim5\times10^3$个吸积IBH，其$F_{\rm X}>10^{-14}\\,\rm{erg\\,s^{-1}\\,cm^{-2}}$，几乎全部未受踢；此估计对采用的辐射效率和热流处理敏感。对于类似罗曼（Roman）的巡天，我们的基准模型预测在五年内，在$1.70\\,\rm{deg^2}$的有效面积上，在巡天选择效应之前，约有$\sim360$个内在IBH微透镜事件。我们提出，来自IBH的长时标微透镜事件可以强烈约束控制恒星质量黑洞形成的SN物理。
英文摘要
Gravitational-wave observations have revealed hundreds of stellar-mass black holes, yet only about two dozen are known in the Milky Way, almost all in binaries. We present POPKIN, a Python framework that couples single- and binary-star evolution with Galactic orbital dynamics to trace black-hole progenitors from the zero-age main sequence to the present-day isolated black-hole (IBH) population. Across ten models varying the supernova (SN) prescription, mass-transfer efficiency, and common-envelope ejection efficiency, the total IBH abundance is controlled primarily by the SN prescription. Our fiducial model, with a recently proposed metallicity- and stripping-history-dependent SN prescription, predicts $\sim4\times10^7$ IBHs in the Galaxy, including $\sim8\times10^4$ within $1\,\rm{kpc}$ of the Sun; alternative SN prescriptions predict $\sim(1-2)\times10^8$ IBHs. The fiducial model yields a bimodal mass distribution, peaking near $9\,M_{\odot}$ and $20\,M_{\odot}$, with a deficit at $13-17\,M_{\odot}$. This distinguishes it from alternative prescriptions, some of which populate the $2-5\,M_{\odot}$ mass-gap region. Non-kicked IBHs follow nearly circular orbits near the Galactic plane, with typical peculiar velocities of $20-30\,\rm{km\,s^{-1}}$, whereas kicked systems undergo stronger radial migration and span a broader velocity range. We estimate $\sim5\times10^3$ accreting IBHs with $F_{\rm X}>10^{-14}\,\rm{erg\,s^{-1}\,cm^{-2}}$, nearly all non-kicked; this estimate is sensitive to the adopted radiative-efficiency and hot-flow treatments. For a Roman-like bulge survey, our fiducial model predicts $\sim360$ intrinsic IBH microlensing events over five years in a $1.70\,\rm{deg^2}$ effective area, before survey-selection effects. We propose that long-timescale microlensing events from IBHs can strongly constrain the SN physics governing stellar-mass black hole formation.
发表机构
- Nanjing University（南京大学）
- Tsung-Dao Lee Institute, Shanghai Jiao-Tong University（上海交大东京大学研究院）
机构由 AI 辅助整理，请以论文原文为准。
