论文标题
$ 30 \，m_ \ odot $在太阳金属上合并黑洞
The formation of $30\,M_\odot$ merging black holes at solar metallicity
论文作者
论文摘要
在孤立的二进制中形成的黑洞的最大质量由恒星风和二进制组件之间的相互作用确定。与采用快速种群合成模型的研究相比，我们首次考虑了人口合成模型中完全自以为是的详细结构和二进制演化计算，而黑洞二进制文件的形成出现了新的，质性上不同的图片。我们发现合并二进制黑洞可以以不可忽略的速率形成（$ \ sim 4 \ times10^{ - 7} \，m_ \ odot^{ - 1} $在太阳金属上。他们具有初始质量的祖细胞$ \ gtrsim 50 \，m_ \ odot $不会扩展到超级半径，主要避免了大量的尘埃驱动或发光的蓝色可变风。总体而言，祖先恒星在恒星风中的质量减少了，导致黑洞的巨大与$ \ sim 30 \，m_ \ odot $，并且其中大约一半避免了质量转移的发作，然后才形成了第一个出生的黑洞。最后，初始期限为几天的二进制文件，其中一些可能会发生Roche-Lobe Overflow质传质，从而导致轻微旋转的头出生的黑洞，$χ_\ Mathrm {BH1} \ Lesssim 0.2 $，假设有效的Angular-Momentum Transport。
The maximum mass of black holes formed in isolated binaries is determined by stellar winds and the interactions between the binary components. We consider for the first time fully self-consistent detailed stellar structure and binary evolution calculations in population-synthesis models and a new, qualitatively different picture emerges for the formation of black-hole binaries, compared to studies employing rapid population synthesis models. We find merging binary black holes can form with a non-negligible rate ($\sim 4\times10^{-7}\,M_\odot^{-1}$) at solar metallicity. Their progenitor stars with initial masses $\gtrsim 50\,M_\odot$ do not expand to supergiant radii, mostly avoiding significant dust-driven or luminous blue variable winds. Overall, the progenitor stars lose less mass in stellar winds, resulting in black holes as massive as $\sim 30\,M_\odot$, and, approximately half of them avoid a mass-transfer episode before forming the first-born black hole. Finally, binaries with initial periods of a few days, some of which may undergo episodes of Roche-lobe overflow mass transfer, result in mildly spinning first-born black holes, $χ_\mathrm{BH1} \lesssim 0.2$, assuming efficient angular-momentum transport.
