论文标题
了解BPASS中稳定的传质和超级伊德丁顿积聚的高质量二进制黑洞人口
Understanding the high-mass binary black hole population from stable mass transfer and super-Eddington accretion in BPASS
论文作者
论文摘要
随着LVK财团在检测二进制黑洞合并方面取得了显着的成功，已经有可能利用种群特性来限制我们对祖细胞恒星进化的理解。观察到的主要黑洞质量分布的最引人注目的特征是延伸的尾巴高达100m $ _ \ odot $，超过3500万$ _ \ odot $的质量过多。当前，孤立的二元种群合成很难解释这些特征。使用经过良好测试的BPASS详细的恒星二进制演化模型来确定传质稳定性，积聚率和残余质量，我们假设稳定的质量转移质量是超级 - 埃德丁顿积聚的质量。此外，如前所述，过量不是由于脉冲对不稳定性引起的，而是由于质量稳定而引起的。由于更稳定的传质，这些系统能够在哈勃时间内合并，并具有极高的质量比，从而使轨道可以充分收缩以允许合并。这些发现与其他种群合成代码的发现不符，但与使用详细二进制进化模型的其他最新研究一致。
With the remarkable success of the LVK consortium in detecting binary black hole mergers, it has become possible to use the population properties to constrain our understanding of the progenitor stars' evolution. The most striking features of the observed primary black hole mass distributions are the extended tail up to 100M$_\odot$ and an excess of masses at 35M$_\odot$. Currently, isolated binary population synthesis have difficulty explaining these features. Using the well-tested BPASS detailed stellar binary evolution models to determine mass transfer stability, accretion rates, and remnant masses, we postulate that stable mass transfer with super-Eddington accretion is responsible for the extended tail. Furthermore, that the excess is not due to pulsation-pair instability, as previously thought, but due to stable mass transfer. These systems are able to merge within the Hubble time due to more stable mass transfer with extreme mass ratios that allows the orbits to shrink sufficiently to allow for a merger. These finding are at odds with those from other population synthesis codes but in agreement with other recent studies using detailed binary evolution models.
