普通包层中中子星的再循环与超新星爆炸
Recycling of Neutron Stars in Common Envelopes and Hypernova Explosions
摘要：
在本文中，我们提出了一个新的合理的机制，超新星爆炸特有的密切的双星系统。研究的起点是由一颗红超巨星和一颗中子星组成的双星演化过程中的共同包络相。当中子星盘旋着向它的伴星中心移动时，它通过盘吸积而旋转起来。根据中子星通过邦迪-霍伊尔机制捕获的气体的特定角动量，当它仍然在公共包层内或与伴核合并后，它可能达到毫秒周期。高吸积率可能导致中子星强烈的差速自转和磁星强磁场的产生。如果磁星风的磁场与$10^{15}\,$ G一样强，它就能吹走共同的包层;如果磁星风与$10^{16}\,$ G一样强，它就能摧毁整个伴星。总爆炸能量可与毫秒脉冲星的转动能量相当，达到$10^{52}\,$ erg。然而，预期仅少量的$^{56}$ Ni以这种方式产生。其结果是一个不寻常的II型超新星，在平台阶段具有非常高的光度，随后亮度急剧下降，光变曲线尾部陡峭。其残骸要么是一颗单独的磁星，要么是一颗包含沃尔夫-拉叶星和磁星的近距离双星。当沃尔夫-拉叶星爆炸时，这将是同一双星中的第三次超新星爆炸。
英文摘要：
In this paper we propose a new plausible mechanism of supernova explosions specific to close binary systems. The starting point is the common envelope phase in the evolution of a binary consisting of a red super giant and a neutron star. As the neutron star spirals towards the center of its companion it spins up via disk accretion. Depending on the specific angular momentum of gas captured by the neutron star via the Bondi-Hoyle mechanism, it may reach millisecond periods either when it is still inside the common envelope or after it has merged with the companion core. The high accretion rate may result in strong differential rotation of the neutron star and generation of the magnetar-strength magnetic field. The magnetar wind can blow away the common envelope if its magnetic field is as strong as $10^{15}\,$G, and can destroy the entire companion if it is as strong as $10^{16}\,$G. The total explosion energy can be comparable to the rotational energy of a millisecond pulsar and reach $10^{52}\,$erg. However, only a small amount of $^{56}$Ni is expected to be produced this way. The result is an unusual type-II supernova with very high luminosity during the plateau phase, followed by a sharp drop in brightness and a steep light-curve tail. The remnant is either a solitary magnetar or a close binary involving a Wolf-Rayet star and a magnetar. When this Wolf-Rayet star explodes this will be a third supernovae explosion in the same binary.
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