论文标题
隔离二进制进化中各个进化途径对观察到的二进制黑洞人群的贡献的限制
Constraints on the contributions to the observed binary black hole population from individual evolutionary pathways in isolated binary evolution
论文作者
论文摘要
合并二进制黑洞的引力波可以用来揭示大量二进制恒星进化的不知情方面，例如巨大的恒星的演变（包括它们的质量损失速率），共同的信封阶段以及在整个宇宙宇宙历史中形成巨大恒星的速率。在本文中，我们探讨了这些阶段对合并二进制黑洞的合并速率和CHIRP质量分布的预测的\ emph {相关}的影响，旨在确定模型参数之间可能的退化。在我们的许多模型中，很大一部分（超过70％的可检测到的二进制黑洞）来自化学均匀的进化情况。这些模型倾向于过度预测二进制黑洞合并速率，并产生平均太大的系统。我们的首选模型有利于富含氦气的狼 - 射线星的质量减少率，并与最近的理论和观察性发展保持紧张关系。我们确定狼 - 射线恒星的质量损失率与宇宙的金属演变对合并二元黑洞的速率和特性之间的相关性。 Based on the observed mass distribution, we argue that the $\sim 10\%$ of binary black holes with chirp masses greater than $40$ M$_\odot$ (the maximum predicted by our models) are unlikely to have formed through isolated binary evolution, implying a significant contribution (> 10%) from other formation channels such as dense star clusters or active galactic nuclei.我们的模型将在不久的将来就二进制演变的不确定参数推断。
Gravitational waves from merging binary black holes can be used to shed light on poorly understood aspects of massive binary stellar evolution, such as the evolution of massive stars (including their mass-loss rates), the common envelope phase, and the rate at which massive stars form throughout the cosmic history of the Universe. In this paper we explore the \emph{correlated} impact of these phases on predictions for the merger rate and chirp mass distribution of merging binary black holes, aiming to identify possible degeneracies between model parameters. In many of our models, a large fraction (more than 70% of detectable binary black holes) arise from the chemically homogeneous evolution scenario; these models tend to over-predict the binary black hole merger rate and produce systems which are on average too massive. Our preferred models favour enhanced mass-loss rates for helium rich Wolf--Rayet stars, in tension with recent theoretical and observational developments. We identify correlations between the impact of the mass-loss rates of Wolf--Rayet stars and the metallicity evolution of the Universe on the rates and properties of merging binary black holes. Based on the observed mass distribution, we argue that the $\sim 10\%$ of binary black holes with chirp masses greater than $40$ M$_\odot$ (the maximum predicted by our models) are unlikely to have formed through isolated binary evolution, implying a significant contribution (> 10%) from other formation channels such as dense star clusters or active galactic nuclei. Our models will enable inference on the uncertain parameters governing binary evolution in the near future.
