Pulsational Pair-instability Supernovae in Very Close Binaries
Pulsational Pair-instability Supernovae in Very Close Binaries
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DOI：
10.3847/1538-4357/ab3426
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发表时间：
2018-10
期刊：
影响因子：
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通讯作者：
P. Marchant;M. Renzo;R. Farmer;K. M. W. Pappas;R. Taam;S. D. de Mink;V. Kalogera
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文献类型：
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作者：
P. Marchant;M. Renzo;R. Farmer;K. M. W. Pappas;R. Taam;S. D. de Mink;V. Kalogera
对不稳定性和脉动对不稳定性超新星（PPISNe）至今尚未被明确观测到。然而，它们是探测到的最重的二元黑洞（BBH）合并的祖先的有希望的候选者。如果这些BBH是双星演化的产物，那么PPISNe可能发生在非常接近的双星中。出于这一动机，我们讨论了PPISN发生与密切的二进制同伴的影响，以及这些事件对合并BBH通过二进制进化的形成有什么影响。为此，我们使用梅萨软件工具计算了一组贫金属（Z = 10）单氦星模型。对于脉冲前质量>50 M的PPISN祖先，我们发现，脉冲后，热量沉积在整个星星层保持约束，导致它扩大到100 R以上的时期为102-104年，这取决于祖先的质量。这导致长寿命阶段的洛希瓣溢出，甚至共同的包络事件，如果有一个密切的双同伴，导致额外的电磁瞬变与PPISN爆发。如果我们忽略这些相互作用的影响，我们发现，从PPISNe的质量损失减少了最终BH自旋的30%，诱导偏心率低于阈值的丽莎天文台的可探测性，并可以产生一个双峰分布的测量啁啾质量BBH合并地面探测器观察到。
Pair-instability and pulsational pair-instability supernovae (PPISNe) have not been unambiguously observed so far. They are, however, promising candidates for the progenitors of the heaviest binary black hole (BBH) mergers detected. If these BBHs are the product of binary evolution, then PPISNe could occur in very close binaries. Motivated by this, we discuss the implications of a PPISN happening with a close binary companion and what impact these events have on the formation of merging BBHs through binary evolution. For this, we have computed a set of models of metal-poor (Z⊙/10) single helium stars using the MESA software instrument. For PPISN progenitors with pre-pulse masses >50 M⊙ we find that, after a pulse, heat deposited throughout the layers of the star that remain bound causes it to expand to more than 100 R⊙ for periods of 102–104 yr depending on the mass of the progenitor. This results in long-lived phases of Roche lobe overflow or even common-envelope events if there is a close binary companion, leading to additional electromagnetic transients associated with PPISN eruptions. If we ignore the effect of these interactions, we find that mass loss from PPISNe reduces the final BH spin by ∼30%, induces eccentricities below the threshold of detectability of the LISA observatory, and can produce a double-peaked distribution of measured chirp masses in BBH mergers observed by ground-based detectors.