AI 中文总结
该研究解决了恒星最大尺寸的物理起源问题，通过演化模型揭示汉弗莱斯-戴维森极限的弯折是星风向爱丁顿增强质量损失机制转变的表现，其模型可应用于多个天体物理领域。
AI 中文摘要
人们或许会认为质量最大的恒星尺寸也最大，但事实并非如此，这一问题已困扰天文学家数十年。爱丁顿极限通过辐射压与引力的平衡为恒星质量设定了上限，而恒星半径存在的第二条经验边界对现代天体物理学同样影响深远：它会影响LIGO和Virgo所推断的黑洞质量与并合率，决定恒星是保持为炽热、致密的电离源还是膨胀为冷超巨星，进而塑造对遥远未分辨恒星群光谱的解读。半个世纪前，人们发现该半径极限在赫罗图中呈现出特征性的弯折形态，即汉弗莱斯-戴维森极限，但至今仍缺乏具有预测性的第一性原理物理解释。本文表明，该弯折是演化模型中自洽实现的经典星风向爱丁顿增强质量损失机制转变的演化表现。我们的模型准确复现了大质量恒星半径的经验约束，如今已有框架可被纳入双星种群合成、黑洞质量预测、引力波事件率计算以及高红移詹姆斯·韦伯光谱的解读中。
英文摘要
One might expect the most massive stars to also be the largest by size, yet they are not, and this has puzzled astronomers for decades. The Eddington limit sets an upper bound to stellar mass through the balance between radiation pressure and gravity, but a second empirical boundary on stellar radius has equally far-reaching consequences for modern Astrophysics: it affects the black-hole masses and merger rates inferred by LIGO and Virgo, determines whether a star remains a hot, compact ionising source or inflates into a cool supergiant, and thereby shapes how spectra of distant, unresolved stellar populations are interpreted. Half a century ago, this radius limit was shown to trace a characteristic kinked shape in the Hertzsprung-Russell diagram known as the Humphreys-Davidson limit, yet a predictive, first-principle physical explanation has remained elusive. Here we show that this kink is the evolutionary manifestation of a transition from classical stellar outflows to an Eddington-enhanced mass-loss regime implemented self consistently in evolutionary models. With our models accurately reproducing the empirical constraints on the radii of the most massive stars, we now have a framework that can be incorporated into binary population synthesis, black-hole mass predictions, gravitational-wave event rates, and the interpretation of high-redshift James Webb spectra.
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