标题： 写在大质量恒星中：恒星物理在黑洞形成中的作用 显示英文标题

标题： It's written in the massive stars: The role of stellar physics in the formation of black holes

摘要： 在引力波（GW）源以及新发现的本地黑洞（BH）和中子星（NS）的时代，理解恒星的命运是一个关键问题。并非每一颗大质量恒星都能成功爆炸为超新星并留下一个NS；有些恒星会形成BH。遗迹取决于爆炸物理，但也依赖于最终的核心结构，通常用紧凑性参数或铁核质量来概括，其中高值与BH形成相关联。 几个研究小组报告了这些参数随着质量变化而表现出类似模式，以一个显著的紧凑性峰值为特征，随后在更高质量时出现另一个峰值，这表明存在一种共同的基本物理机制。 在这里，我们通过使用MESA计算从17到50个太阳质量的单星模型来探讨其起源。第一次和第二次紧凑性增加分别源于核心碳和氖燃烧，它们变得中微子主导，这增强了核心收缩，并最终增加了铁核质量和紧凑性。 在碳燃烧期间早期的氖点燃，以及在氧燃烧期间早期的硅点燃有助于抵消核心收缩并减少最终的铁核质量和紧凑性。C/Ne和O燃烧壳之间的合并进一步减少了紧凑性，我们证明这是由于这些层中熵生产增强所致。 我们发现大质量恒星的最终结构并不是随机的，而是早在核心氦耗尽时就已经写入其核心。同样的机制决定了这个核心质量范围内任何恒星的最终结构，包括双星产物，尽管双星相互作用系统地偏移了预期BH形成的范围。 最后，我们讨论了恒星物理不确定性的作用，以及如何将这些发现应用于引力波源的研究。 [摘要] 显示英文摘要

摘要： In the age of gravitational-wave (GW) sources and newly discovered local black holes (BH) and neutron stars (NS), understanding the fate of stars is a key question. Not every massive star is expected to successfully explode as a supernova and leave behind a NS; some stars form BHs. The remnant depends on explosion physics but also on the final core structure, often summarized by the compactness parameter or iron core mass, where high values have been linked to BH formation. Several groups have reported similar patterns in these parameters as a function of mass, characterized by a prominent compactness peak followed by another peak at higher masses, pointing to a common underlying physical mechanism. Here, we investigate its origin by computing single-star models from 17 to 50 solar masses with MESA. The first and second compactness increases originate from core carbon and neon burning, respectively, becoming neutrino dominated, which enhances the core contraction and ultimately increases the iron-core mass and compactness. An early core neon ignition during carbon burning, and an early silicon ignition during oxygen burning help counter the core contraction and decrease the final iron core mass and compactness. Shell mergers between C/Ne and O-burning shells further decrease the compactness and we show that they are due to an enhanced entropy production in these layers. We find that the final structure of massive stars is not random but already written in their cores at core helium exhaustion. The same mechanisms determine the final structure of any star in this core mass range, including binary products, though binary interactions systematical shift the range of expected BH formation. Finally, we discuss the role of stellar physics uncertainties and how to apply these findings to studies of GW sources. [Abridged]