arXiv 2602.036292026-02astro-ph.HE

案例A的论证：通过稳定的质交换对双黑洞形成进行详细研究

A case for Case A: detailed look at binary black hole formation through stable mass transfer

Université de Genève（日内瓦大学）；Gravitational Wave Science Center (GWSC), Université de Genève（引力波科学中心（GWSC），日内瓦大学）；Northwestern University（西北大学）；Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University（天体物理交叉探索与研究中心（CIERA），西北大学）；Center for Astrophysics | Harvard & Smithsonian（哈佛-史密森尼天体物理中心）；Harvard Society of Fellows（哈佛学者协会）；The NSF-Simons AI Institute for the Sky (NSF-Simons SkAI)（NSF-Simons 天空人工智能研究所）

Max M. Briel, Tassos Fragos, Monica Gallegos-Garcia, Anarya Ray, Michael Zevin, Abhishek Chattaraj, Jeff J. Andrews, Vicky Kalogera, Seth Gossage, Philipp M. Sr… 展开作者

Max M. Briel, Tassos Fragos, Monica Gallegos-Garcia, Anarya Ray, Michael Zevin, Abhishek Chattaraj, Jeff J. Andrews, Vicky Kalogera, Seth Gossage, Philipp M. Srivastava, Elizabeth Teng

备注：: Accepted in A&A

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AI总结：

本文通过详细二进制模型研究双黑洞合并的形成机制，探讨了稳定质交换通道中初始条件、金属丰度依赖性和质量比反转的影响。

摘要：

在孤立二进制演化中，双黑洞（BBH）合并通常通过稳定质交换（SMT）或共同包层演化形成。近年来，SMT通道受到广泛关注，因为详细的二进制模型显示比以前的研究有更高的质交换稳定性。在本工作中，我们使用详细的二进制模型，在八个金属丰度（从10^-4 Z_太阳到2 Z_太阳）范围内，从零年龄主序到致密物合并进行了全面分析，以自洽地建模SMT通道的BBH合并人口特性，确定其前身的初始条件，并研究其形成和金属丰度依赖性的二进制物理。我们使用人口合成代码POSYDON来确定来自SMT的BBH合并人口。利用其扩展的MESA二进制模型网格，我们确定了BBH合并形成的本质物理。SMT主要产生BBH合并来自P_{ZAMS} ≤10天的系统。在这些系统中，两个恒星之间的初始质交换以及后续剩余恒星与第一个形成的黑洞之间的相互作用发生在各自的供体恒星处于主序星（案例A）时。我们发现更宽的案例B/C系统对贡献有限。没有胎生踢的情况下，由于恒星风质损失导致轨道扩张，SMT通道在Z>0.2Z_太阳以上不会产生BBH合并。主要的黑洞质量分布对金属丰度有强依赖性，而质量比偏好于单位独立于金属丰度，由于质量比反转。此外，χ_{eff}分布在χ_{eff}=0和~0.15处有峰值，其中前者在高金属丰度下消失。一个质量缩放的胎生踢使这个子群体保持不变，但引入了一个低质量、质量比不等的子群体，其由于高偏心率而合并。

英文摘要：

In isolated binary evolution, binary black hole (BBH) mergers are generally formed through stable mass transfer (SMT) or common envelope evolution. In recent years, the SMT channel has received significant attention due to detailed binary models showing increased mass transfer stability compared to previous studies. In this work, we perform a full zero-age-main-sequence to compact object merger analysis using detailed binary models at eight metallicities between $10^{-4}Z_\odot$ and $2Z_\odot$ to self-consistently model the population properties of BBH mergers in the SMT channel, determined their progenitor initial conditional, and investigate the binary physics governing their formation and metallicity dependence. We use the population synthesis code POSYDON to determine the population of BBH mergers from SMT. Using its extended grids of MESA binary models, we determine the essential physics in the formation of BBH mergers. SMT produces BBH mergers predominantly from systems with $P_{ZAMS}\leq10$ days. In these systems, both the initial mass transfer between two stars and the subsequent interaction between the remaining star and the first-born BH take place while the respective donor star is on the main-sequence (Case A). We find a limited contribution from wider Case B/C systems. Without a natal kick, the SMT channel does not produce BBH mergers above $Z>0.2Z_\odot$ due to orbital widening from stellar wind mass loss. The primary BH mass distribution shows a strong dependence on metallicity, while the mass ratio prefers unity independent of metallicity due to mass ratio reversal. Additionally, the $χ_{eff}$ distributions contain peaks at $χ_{eff}=0$ and ~0.15 of which the former disappears at high metallicities. A mass-scaled natal kick leave this sub-population unchanged but introduce a low-mass, unequal mass ratio sub-population that merges due to their high eccentricity.

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