Probing the progenitors of spinning binary black-hole mergers with long gamma-ray bursts
Probing the progenitors of spinning binary black-hole mergers with long gamma-ray bursts
复制标题
探测旋转双黑洞合并与长伽马射线爆发的起源
DOI：
10.1051/0004-6361/202141979
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发表时间：
2022
影响因子：
6.5
通讯作者：
Dotter, Aaron
中科院分区：
文献类型：
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作者：
Bavera, Simone S.;Fragos, Tassos;Zapartas, Emmanouil;Ramirez-Ruiz, Enrico;Marchant, Pablo;Kelley, Luke Z.;Zevin, Michael;Andrews, Jeff J.;Coughlin, Scott;Dotter, Aaron
长持续时间的伽马射线暴被认为与大质量快速旋转恒星的核心坍缩和黑洞的形成有关。然而，恒星内部有效的角动量传输，目前支持的小行星地震和引力波的约束，导致主要是缓慢旋转的恒星核心。在这里，我们报告的二进制恒星演化和人口合成的计算，表明在紧密的双星潮汐相互作用不仅可以解释所观察到的子人口的旋转，合并的双黑洞，但也导致长的伽玛射线爆发时，黑洞形成。根据我们的模型对发光长伽马射线爆发的各向同性等效能量分布的校准，我们发现，GWTC-2报告的双黑洞中有10%的双黑洞具有与它们的形成相关的发光长伽马射线爆发，其中GW 190517和GW 190719的概率分别为1085%和1060%。此外，假设他们的平均光束分数，我们的模型预测的速率密度的长伽玛射线暴，作为红移的函数，起源于这个通道。对于一个恒定的光束分数fB <$0.05，我们的模型预测的速率密度与观察到的一个，在整个红移范围内，而在redshiftz∈ [0，2.5]，与观察到的LGRB宿主星系的金属丰度分布的初步比较意味着，20%至85%的观察到的长伽玛射线暴可能来自合并的双黑洞的祖先。 在观测到的发光的长伽马射线暴中，有一个潜在的重要部分与旋转的双黑洞合并的祖先之间存在联系，这使得我们能够在当前一代引力波观测站的视界之外探测后者，并达到宇宙学距离。
Long-duration gamma-ray bursts are thought to be associated with the core-collapse of massive, rapidly spinning stars and the formation of black holes. However, efficient angular momentum transport in stellar interiors, currently supported by asteroseismic and gravitational-wave constraints, leads to predominantly slowly-spinning stellar cores. Here, we report on binary stellar evolution and population synthesis calculations, showing that tidal interactions in close binaries not only can explain the observed subpopulation of spinning, merging binary black holes but also lead to long gamma-ray bursts at the time of black-hole formation. Given our model calibration against the distribution of isotropic-equivalent energies of luminous long gamma-ray bursts, we find that ≈10% of the GWTC-2 reported binary black holes had a luminous long gamma-ray burst associated with their formation, with GW190517 and GW190719 having a probability of ≈85% and ≈60%, respectively, being among them. Moreover, given an assumption about their average beaming fraction, our model predicts the rate density of long gamma-ray bursts, as a function of redshift, originating from this channel. For a constant beaming fractionfB∼ 0.05 our model predicts a rate density comparable to the observed one, throughout the redshift range, while, at redshiftz∈ [0, 2.5], a tentative comparison with the metallicity distribution of observed LGRB host galaxies implies that between 20% to 85% of the observed long gamma-ray bursts may originate from progenitors of merging binary black holes. The proposed link between a potentially significant fraction of observed, luminous long gamma-ray bursts and the progenitors of spinning binary black-hole mergers allows us to probe the latter well outside the horizon of current-generation gravitational wave observatories, and out to cosmological distances.