MATTER MIXING IN CORE-COLLAPSE SUPERNOVA EJECTA: LARGE DENSITY PERTURBATIONS IN THE PROGENITOR STAR?
MATTER MIXING IN CORE-COLLAPSE SUPERNOVA EJECTA: LARGE DENSITY PERTURBATIONS IN THE PROGENITOR STAR?
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DOI：
10.1088/0004-637x/808/2/164
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发表时间：
2015-07
期刊：
影响因子：
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通讯作者：
J. Mao;M. Ono;S. Nagataki;M. Hashimoto;Hirotaka Ito;J. Matsumoto;M. Dainotti;Shiu-Hang Lee
中科院分区：
文献类型：
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作者：
J. Mao;M. Ono;S. Nagataki;M. Hashimoto;Hirotaka Ito;J. Matsumoto;M. Dainotti;Shiu-Hang Lee
物质混合是核心坍缩超新星（CCSN）爆炸研究中的一个重要课题。在本文中，我们进行了二维流体动力学模拟，以重现在SN 1987A中观测到的高速56Ni团块。这是首次在CCSN祖先中提出大密度摄动来产生瑞利-泰勒（Rayleigh-Taylor）不稳定性并使有效物质混合。在球形爆炸的情况下，在SN祖先的C+O/He和He/H界面上，RT不稳定性都是有效的。在微扰图中显示的径向相干结构对于获得高速56Ni团块是重要的。在某些非球面爆炸情况下，我们还可以获得物质混合特征和高速56Ni团块。我们发现，在我们的工作中，最有利的模型之一是双极和等不对称爆炸的组合，其中至少25%的密度摄动是在CCSN祖先的不同组成界面上引入的。这些模拟结果与SN 1987A的观测结果相当。
Matter mixing is one important topic in the study of core-collapse supernova (CCSN) explosions. In this paper, we perform two-dimensional hydrodynamic simulations to reproduce the high velocity 56Ni clumps observed in SN 1987A. This is the first time that large density perturbation is proposed in the CCSN progenitor to generate Rayleigh–Taylor (RT) instability and make the effective matter mixing. In the case of a spherical explosion, RT instability is efficient at both C+O/He and He/H interfaces of the SN progenitor. Radial coherent structures shown in perturbation patterns are important for obtaining high velocity 56Ni clumps. We can also obtain matter mixing features and high velocity 56Ni clumps in some cases of aspherical explosion. We find that one of the most favorable models in our work has a combination of bipolar and equatorially asymmetric explosions in which at least 25% of density perturbation is introduced at different composition interfaces of the CCSN progenitor. These simulation results are comparable to the observational findings of SN 1987A.