AI 中文总结
该研究针对AGN盘中大质量恒星起源演化的不确定性，建立半解析模型，发现嵌入CCSN遗迹可经特定过程形成第二代大质量恒星，且产星量与SMBH质量相关，为相关研究提供了局域气体循环的新机制。
AI 中文摘要
活动星系核（AGN）盘中大质量恒星的起源与演化仍不确定。我们开发了一个半解析模型，用于追踪嵌入的核心坍缩超新星（CCSN）遗迹的演化，以及随后致密气体云的形成与增长过程。在致密的盘环境中，高效的辐射冷却可强烈压缩遗迹或使其跳过Sedov-Taylor阶段，推动遗迹快速进入辐射扫雪演化阶段。当遗迹失去内部压力支撑后，冷却壳层碎片的部分回流与补充气体可能形成压力受限、潮汐受限的种子云。该云随后通过剪切受限的希尔捕获增长，直至坍缩所需的引力、潮汐、剪切、光电离及磁场条件同时满足。演化结果强烈依赖超大质量黑洞（SMBH）质量与爆炸半径：SMBH质量最低的模型平均每次事件产生不足1颗大质量恒星，而质量最大的SMBH模型可产生数颗至数百颗大质量恒星。对于顶部重的初始质量函数，大质量恒星主导了最终的恒星质量与反馈预算。因此，嵌入的超新星可能为AGN盘中第二代大质量恒星的形成提供局域化的气体循环通道。
英文摘要
The origin and evolution of massive stars in active galactic nucleus (AGN) discs remain uncertain. We develop a semi-analytical model that follows the evolution of an embedded core-collapse supernova (CCSN) remnant and the subsequent formation and growth of a compact gas cloud. In the dense disc environment, efficient radiative cooling can strongly compress or bypass the Sedov-Taylor stage and drive the remnant rapidly into radiative snowplow evolution. After the remnant loses its interior pressure support, partial backflow of cooled shell fragments and refilling gas may initialize a pressure-confined and tidally limited seed cloud. The cloud then grows through shear-limited Hill capture until the gravitational, tidal, shear, photoionization, and magnetic conditions for collapse are simultaneously satisfied. The outcome depends strongly on the supermassive black-hole (SMBH) mass and explosion radius. Models with the lowest SMBH mass yield fewer than one massive star per event on average, whereas the most massive SMBH models can produce from several to several hundred. For a top-heavy initial mass function, massive stars dominate the resulting stellar mass and feedback budget. Embedded supernovae may therefore provide a localized gas-recycling channel for second-generation massive-star formation in AGN discs.
Comments14 pages, 7 figures, 5 tables, accepted for publication in MNRAS
