恒星风图集II：太阳金属度下的黑洞形成
The Stellar Winds Atlas II: Black Hole Formation at Solar Metallicity
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中文总结 AI 辅助
本研究通过1D MESA恒星演化模型构建“风图集”，系统研究14种风模型，发现太阳金属度下黑洞形成由冷超巨星坍缩或成为WR星的分叉控制，明确黑洞质量预测的关键瓶颈，为测试风模型提供基线。
中文摘要 AI 辅助
恒星风是从大质量恒星预测黑洞（BH）质量的主要不确定性来源。在太阳金属度下，理论模型因不同的风预设而产生差异极大的结果，关键障碍仍是缺乏在共同参数空间内的系统研究。为解决这一问题，我们使用详细的1D MESA恒星演化模型和星族合成技术构建了“风图集”，以估计太阳金属度下的银河系黑洞前身星族群。我们系统研究了14种不同的风模型，涵盖从最传统、应用最广泛的预设到最新的模型。通过评估该广泛网格中的恒星演化，我们发现最终黑洞质量由一个基本分叉决定：恒星是作为冷超巨星坍缩，还是先剥离包层成为沃尔夫-拉叶星（WR）。若恒星进入WR阶段，其强劲的厚风占主导，使最终质量对WR风预设敏感，且基本抹去了前期质量损失历史的影响；相反，作为超巨星发生核心坍缩的恒星会形成质量大得多的黑洞，在初始质量约40倍太阳质量（$M_\text{\textodot}$）处形成一个质量峰。我们的综合评估并非简单重现这些差异结果，而是证明该分叉普遍受冷超巨星阶段高度不确定的质量损失控制。该框架通过确定未来研究的两个关键瓶颈（包层剥离效率和WR质量损失率），强烈约束了黑洞质量预测问题。我们的图集为解释当前理论差异、根据观测约束（如银河系WR/OB星族比）测试风模型提供了明确基线。
英文摘要
Stellar winds are a primary source of uncertainty in predicting the masses of black holes (BHs) from massive stars. At solar metallicity, theoretical models lead to widely divergent results due to differing wind prescriptions. A key obstacle remains the lack of systematic investigations across a common parameter space. To address this, we construct a ``Wind Atlas'' using detailed 1D MESA stellar evolution models and population synthesis techniques to estimate the Galactic population of solar metallicity BH progenitors. We systematically investigate 14 distinct wind models, ranging from the most traditional and widespread prescriptions to the most recent. By evaluating stellar evolution across this extensive grid, we show that the final BH mass is dictated by a fundamental bifurcation: whether a star collapses as a cool supergiant or is first stripped of its envelope to become a Wolf-Rayet (WR) star. If a star enters the WR stage, its strong thick winds dominate, making the final mass sensitive to the WR wind prescription while largely erasing the memory of its prior mass-loss history. Conversely, stars that face core collapse as supergiants form significantly more massive BHs, producing a mass peak around an initial mass of 40 $M_\odot$. Rather than simply reproducing these divergent outcomes, our comprehensive evaluation demonstrates that this bifurcation is universally controlled by the highly uncertain mass loss during the cool supergiant phase. This framework strongly constrains the problem of BH mass prediction by identifying two key bottlenecks for future studies: envelope stripping efficiency and WR mass-loss rates. Our atlas provides a clear baseline for interpreting current theoretical discrepancies and testing wind models against observational constraints, such as the Galactic WR/OB population ratio.
