论文标题
通过隔离二进制的超级 - 伊德丁顿积聚，污染二进制黑洞的配对质量差距
Polluting the pair-instability mass gap for binary black holes through super-Eddington accretion in isolated binaries
论文作者
论文摘要
单个恒星进化的理论预测黑洞（BHS）的质量分布差距约为45-130m $ _ {\ odot} $，即所谓的“配对稳定质量差距”。我们检查了BHS是否可以从恒星伴侣中获得差异。为此，我们使用种群综合代码模拟了孤立的二进制文件的演变，在那里我们允许超级 - 埃德丁顿积聚。在我们最极端的假设下，我们发现所有合并二进制BH系统中最多约有2％包含一个BH，其中配对质量间隙质量为质量，并且我们发现，少于0.5％的合并系统的总质量大于9000万$ _ {\ odot} $。我们发现没有合并的二进制BH系统，总质量超过100m $ _ {\ odot} $。我们将结果与从几个动态途径到配对质量差距事件的预测进行了比较，并讨论了可区分的特征。我们得出的结论是，经典的孤立二进制形成场景不会显着促进配对质量间隙的污染。隔离二进制通道的预测质量间隙的鲁棒性有望在（i）（i）不同地层通道的相对贡献上，（ii）祖细胞的物理学（包括核反应率）和（iii），（iii），（iii）的相对贡献有望。
The theory for single stellar evolution predicts a gap in the mass distribution of black holes (BHs) between approximately 45-130M$_{\odot}$, the so-called "pair-instability mass gap". We examine whether BHs can pollute the gap after accreting from a stellar companion. To this end, we simulate the evolution of isolated binaries using a population synthesis code, where we allow for super-Eddington accretion. Under our most extreme assumptions, we find that at most about 2% of all merging binary BH systems contains a BH with a mass in the pair-instability mass gap, and we find that less than 0.5% of the merging systems has a total mass larger than 90M$_{\odot}$. We find no merging binary BH systems with a total mass exceeding 100M$_{\odot}$. We compare our results to predictions from several dynamical pathways to pair-instability mass gap events and discuss the distinguishable features. We conclude that the classical isolated binary formation scenario will not significantly contribute to the pollution of the pair-instability mass gap. The robustness of the predicted mass gap for the isolated binary channel is promising for the prospective of placing constraints on (i) the relative contribution of different formation channels, (ii) the physics of the progenitors including nuclear reaction rates, and (iii), tentatively, the Hubble parameter.
