黑洞并合的质量与自旋性质揭示其形成于三合星系统
Mass and spin properties of black-hole mergers reveal formation in triples
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中文总结 AI 辅助
本研究通过层级三合星系统动力学与恒星演化模拟，首次同时复现双黑洞并合的低质量主体在质量峰、自旋分布和质量比上的关键特征，并预测高质量端并合率下降。
中文摘要 AI 辅助
解读观测到的双黑洞并合的形成通道仍然是引力波天文学中一个核心的开放问题。随着数百次探测的积累，推断出的质量与自旋分布展现出丰富的多样性，这很难与传统的孤立双星或致密恒星环境中的形成场景相协调。在此，我们考虑层级三合星系统中存在的大比例大质量前身星，并研究由第三体伴星的引力扰动驱动的黑洞并合。对其动力学和恒星演化的模拟重现了并合群体的关键特征，包括：i) 在$m_1\sim10\\,\rm M_\odot$处出现主导群体的尖锐主质量峰；ii) 在峰内及峰外，具有大自旋轨道角的系统占相当比例，与自旋参数$\chi_{\rm eff}$和$\chi_p$的偏斜分布相匹配；iii) 质量比分布偏向于相等质量，且斜率匹配。我们进一步预测在$m_1\sim30\\,\rm M_\odot$附近并合率急剧下降，这与推断特征的位置相吻合，可能标志着另一个通道主导高质量尾部。我们的层级三合星模型首次证明了一种形成场景，能够同时再现推断出的双黑洞并合低质量主体的主要性质。
英文摘要
Deciphering the formation channels of the observed binary black hole mergers remains a central open problem in gravitational-wave astronomy. With hundreds of detections, the inferred distribution of masses and spins reveals a rich diversity which is difficult to reconcile with traditional formation scenarios from isolated binary stars or dense stellar environments. Here, we consider the large fraction of massive progenitor stars found in hierarchical triples and investigate black hole mergers driven by gravitational perturbations from tertiary companions. Simulations of their dynamics and stellar evolution reproduce key features of the merger population, including: i) a sharp primary mass peak at $m_1\sim10\,\rm M_\odot$ dominating the population; ii) substantial fractions of systems with large spin-orbit angles within and beyond the peak, matching the skewed distributions of the spin parameters $χ_{\rm eff}$ and $χ_p$; iii) a mass-ratio distribution favouring equal masses with matching slopes. We further predict a sharp decline of mergers near $m_1\sim30\,\rm M_\odot$, coincident with the location of inferred features that may signal another channel dominating the high-mass tail. Our models of hierarchical triples demonstrate, for the first time, a formation scenario which simultaneously reproduces the principal properties inferred for the low-mass bulk of binary black hole mergers.
发表机构
- Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）
- Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文学中心）
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