发表机构
Northwestern University; University of Illinois Urbana-Champaign; University of Florida; Université de Genève（西北大学; 伊利诺伊大学厄巴纳-香槟分校; 佛罗里达大学; 日内瓦大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
利用POSYDON种群合成框架预测银河系黑洞种群，揭示其演化起源，并识别出高质星星风演化产生的独特特征，为多观测渠道解释提供框架。
AI 中文摘要
银河系中恒星质量黑洞（BH）的观测图景正在扩展到X射线双星之外，盖亚DR4和罗曼预计将为黑洞种群打开新的窗口。我们使用双星种群合成框架POSYDON来预测现今银河系黑洞种群，并将其与其演化起源联系起来。我们测试了这些预测对双星演化和黑洞形成不确定性的稳健性，包括核心坍缩机制、原生踢、公共包层效率、金属丰度和初始双星分布。在我们的所有模型中，我们发现大多数银河系黑洞是孤立的，恒星并合提供最大贡献，双星瓦解贡献次之。在幸存的双星中，分离的BH-BH系统占主导地位。我们在较高黑洞质量处（基准模型中约为13个太阳质量）识别出一个独特的窄特征，该特征由大质量沃尔夫-拉叶前身星的风驱动演化产生。这一特征在分离的BH-BH双星中尤为突出，并且在不同双星演化和黑洞形成物理的变化中持续存在，但强烈依赖于金属丰度。在较低质量端，这些BH-BH系统主要来源于在黑洞形成前经历稳定质量传输的前身星。最后，为了更直接的观测应用，我们将合成种群嵌入银河系模型中，演化其运动学，对BH-BH透镜进行一阶微引力透镜计算，并在盖亚黑洞的背景下检查具有发光伴星的黑洞系统。在后者中，我们揭示了一个稳健的稳定质量传输种群，这在快速种群合成预测中基本缺失。这些结果为解释跨互补观测渠道的涌现银河系黑洞种群提供了一个演化框架。
英文摘要
The observational landscape of stellar-mass black holes (BHs) in the Milky Way is expanding beyond X-ray binaries, with Gaia DR4 and Roman expected to open new windows onto BH populations. We use the binary population synthesis framework POSYDON to predict the present-day Galactic BH population and connect it to its evolutionary origins. We test the robustness of these predictions to uncertainties in binary evolution and BH formation, including core-collapse mechanisms, natal kicks, common-envelope efficiency, metallicity, and initial binary distributions. Across our models, we find that most Galactic BHs are isolated, with stellar mergers providing the largest contribution and binary disruptions the second largest. Among surviving binaries, detached BH-BH systems dominate. We identify a distinct, narrow feature at higher BH masses ($\simeq13\,\mathrm{M}_{\odot}$ in the fiducial model) produced by wind-driven evolution of massive Wolf-Rayet progenitors. This feature is particularly prominent among detached BH-BH binaries and persists across variations in binary-evolution and BH-formation physics, but depends strongly on metallicity. At lower masses, these BH-BH systems predominantly originate from progenitors that undergo stable mass transfer before BH formation. Finally, for more direct observational applications, we embed the synthetic populations in a Galactic model, evolve their kinematics, perform first-order microlensing calculations for BH-BH lenses, and examine BH systems with luminous companions in the context of the Gaia BHs. In the latter, we uncover a robust stable-mass-transfer population largely absent in rapid population-synthesis predictions. These results provide an evolutionary framework for interpreting the emerging Galactic BH population across complementary observational channels.
CommentsSubmitted to ApJ
