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arXiv 2103.07884astro-ph.SR
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在核心坍缩超新星之前的一个特殊热核超新星的罕见事件

Rare events of a peculiar thermonuclear supernova that precedes a core collapse supernova

Ealeal Bear, Noam Soker

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Accepted for publication in Monthly Notices of the Royal Astronomical Society
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摘要：

我们研究恒星双星演化，导致形成一个白矮星（WD），爆炸的热核超新星在一个共同的信封演化（CEE）的终止前不久，其同伴的核心爆炸作为核心坍缩超新星（CCSN）。核心的CCSN爆炸是红超巨星（RSG）的残余，可能发生在WD作为热核超新星爆炸后的几个月到几年，即，Ia型奇特超新星（奇特SN Ia）。使用演化代码MESA-binary，我们模拟了初始质量为6-7.5Mo的双星系统的演化。质量更大的恒星，主星，将质量转移到次级恒星，并留下CO WD残留物。次级粒子变得足够大，以CCSN结束。当次级双星演化到RSG相时，它吞没了WD，系统经历了一个CEE，最终以WD-核心双星系统结束，轨道间距为a_f ~ 1- 5 Ro。我们的模拟结果表明，在CEE之后的t_{CEE-CCSN} ~ 3000 - 10^5年，地核爆炸为CCSN。我们假设，如果WD吸积来自核心的富氦气体，它可能会爆炸为超新星Ia的双重爆炸方案的框架内的超新星Ia和奇特的超新星Ia。我们预测一个奇特的Ia超新星在几个月到几年内会发生CCSN。

英文摘要：

We study stellar binary evolution that leads to the formation of a white dwarf (WD) that explodes in a thermonuclear supernova at the termination of a common envelope evolution (CEE) shortly before the core of its companion explodes as a core-collapse supernova (CCSN). The CCSN explosion of the core, which is the remnant of a red supergiant (RSG) star, might take place few months to several years after the explosion of the WD as a thermonuclear supernova, i.e., a type Ia peculiar supernova (peculiar SN Ia). Using the evolutionary code MESA-binary we simulate evolution of binary systems with stars of initial masses of 6-7.5Mo. The more massive star, the primary, transfers mass to the secondary star and leaves a CO WD remnant. The secondary becomes massive enough to end in a CCSN. As the secondary evolves to the RSG phase it engulfs the WD and the system experience a CEE that ends with a WD-core binary system at an orbital separation of a_f ~ 1-5Ro. Our simulations show that the core explodes as a CCSN at t_{CEE-CCSN} ~ 3000 - 10^5 yr after the CEE. We assume that if the WD accretes helium-rich gas from the core it might explode as a SN Ia in the frame of the double detonation scenario for SNe Ia and peculiar SNe Ia. We predict the very rare occurrence of a peculiar SN Ia followed within months to years by a CCSN.

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