Pulsational Pair-instability Supernovae
Pulsational Pair-instability Supernovae
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DOI：
10.3847/1538-4357/836/2/244
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发表时间：
2016-08
期刊：
影响因子：
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通讯作者：
S. Woosley
中科院分区：
文献类型：
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作者：
S. Woosley
探索了质量范围为 70–140 M ⊙ 的恒星的最终演化。根据它们的质量损失历史和自转速率，这些恒星将以脉动对不稳定超新星（PPISN）的形式结束其生命，产生各种各样的观测瞬变，总持续时间从几周到几千年不等，光度从 1041 到超过 1044 erg s−1 不等。没有任何非旋转模型辐射超过 5 × 10 50 erg 的光或具有超过 5 × 10 51 erg 的动能，但原则上，在正在探索的磁星驱动爆炸中，更大的能量是可能的。许多事件类似于 SNe Ibn、SNe Icn 和 SNe IIn，并且提到了一些潜在的观测对应物。一些 PPISN 可以长时间处于休眠状态，在第一次猛烈脉冲后数千年产生爆炸。这些休眠超新星包含明亮的沃尔夫-拉叶星，可能嵌入明亮的 X 射线和无线电源中。讨论了 PPISN 与船山二等超新星冒名顶替者、超光度超新星以及引力辐射源的相关性。预计近距离双星中的恒星演化不会产生 52 至 133 M ⊙ 之间的黑洞。
The final evolution of stars in the mass range 70–140 M ⊙ is explored. Depending upon their mass loss history and rotation rates, these stars will end their lives as pulsational pair-instability supernovae (PPISN) producing a great variety of observational transients with total durations ranging from weeks to millennia and luminosities from 1041 to over 1044 erg s−1. No nonrotating model radiates more than 5 × 10 50 erg of light or has a kinetic energy exceeding 5 × 10 51 erg, but greater energies are possible, in principle, in magnetar-powered explosions, which are explored. Many events resemble SNe Ibn, SNe Icn, and SNe IIn, and some potential observational counterparts are mentioned. Some PPISN can exist in a dormant state for extended periods, producing explosions millennia after their first violent pulse. These dormant supernovae contain bright Wolf–Rayet stars, possibly embedded in bright X-ray and radio sources. The relevance of PPISN to supernova impostors like Eta Carinae, to superluminous supernovae, and to sources of gravitational radiation is discussed. No black holes between 52 and 133 M ⊙ are expected from stellar evolution in close binaries.