On the fate of the secondary white dwarf in double-degenerate double-detonation Type Ia supernovae
On the fate of the secondary white dwarf in double-degenerate double-detonation Type Ia supernovae
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关于双简并双爆 Ia 型超新星中次级白矮星的命运
DOI：
10.1093/mnras/stac3107
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发表时间：
2022
影响因子：
4.8
通讯作者：
Röpke, F. K.
中科院分区：
文献类型：
--
作者：
Pakmor, R.;Callan, F. P.;Collins, C. E.;de Mink, S. E.;Holas, A.;Kerzendorf, W. E.;Kromer, M.;Neunteufel, P. G.;O’Brien, John T.;Röpke, F. K.
Ia型超新星的起源系统和爆炸机制仍然是未知的。目前最受青睐的祖先包括双简并系统，由两个碳氧白色矮星和薄氦壳组成。在双爆方案中，剧烈的吸积导致氦在质量更大的主白色矮星上爆炸，在其核心变成碳爆炸并将其爆炸。我们研究了次级白色矮星的命运，重点关注如果次级爆炸而不是幸存，爆炸的喷出物和可观测量的变化。我们模拟了一个双星系统，一个碳氧白色矮星，每个都有氦壳层。我们遵循系统自洽地从螺旋到点火，通过爆炸，到合成观测。我们证实，主要的白色矮星爆炸自洽。然而，次级白色矮星周围的氦爆炸未能引发碳爆炸。我们重新启动模拟点燃的碳爆炸在次级白色矮星的手和比较两个爆炸的喷出物和可观的。我们发现在km s-1的外层喷射物是不可分辨的。光变曲线和光谱非常相似，直到爆炸和喷出物更球形比暴力合并模型。内部喷出物的差异显着减缓了辐射热光变曲线的下降速度后，最大的模型与二次爆炸的百分之20。我们希望未来的合成3D星云光谱能够证实或排除这两种模型。
The progenitor systems and explosion mechanism of Type Ia supernovae are still unknown. Currently favoured progenitors include double-degenerate systems consisting of two carbon-oxygen white dwarfs with thin helium shells. In the double-detonation scenario, violent accretion leads to a helium detonation on the more massive primary white dwarf that turns into a carbon detonation in its core and explodes it. We investigate the fate of the secondary white dwarf, focusing on changes of the ejecta and observables of the explosion if the secondary explodes as well rather than survives. We simulate a binary system of aand acarbon-oxygen white dwarf withhelium shells each. We follow the system self-consistently from inspiral to ignition, through the explosion, to synthetic observables. We confirm that the primary white dwarf explodes self-consistently. The helium detonation around the secondary white dwarf, however, fails to ignite a carbon detonation. We restart the simulation igniting the carbon detonation in the secondary white dwarf by hand and compare the ejecta and observables of both explosions. We find that the outer ejecta atkm s−1are indistinguishable. Light curves and spectra are very similar untilafter explosion and the ejecta are much more spherical than violent merger models. The inner ejecta differ significantly slowing down the decline rate of the bolometric light curve after maximum of the model with a secondary explosion by ∼20 per cent. We expect future synthetic 3D nebular spectra to confirm or rule out either model.