Pair-instability Supernova Simulations: Progenitor Evolution, Explosion, and Light Curves
Pair-instability Supernova Simulations: Progenitor Evolution, Explosion, and Light Curves
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DOI：
10.3847/1538-4357/aa8461
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发表时间：
2017-06
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影响因子：
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通讯作者：
Matthew S. Gilmer;A. Kozyreva;R. Hirschi;C. Fröhlich;N. Yusof
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文献类型：
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作者：
Matthew S. Gilmer;A. Kozyreva;R. Hirschi;C. Fröhlich;N. Yusof
近年来，对不稳定超新星（PISN）解释超亮超新星的可行性几乎消失了，除了一些缓慢发展的例子。然而，PISNe在其大部分质量范围内都不会超发光。事实上，我们看到的第一个PISN（如果我们还没有看到的话）更有可能不是超发光的。在这里，我们提出了流体动力学模拟PISNe四个恒星模型具有独特的信封属性跨越PISN质量范围。此外，我们计算合成的光变曲线（LC）与当前和未来的观测结果进行比较。我们还调查，在我们最大规模的模型的背景下，混合在超新星喷出物的前景，减轻目前的PISN模型和剩余的超亮候选事件之间的差异。为此，我们提出了第一个出版的3D流体动力学模拟PISNe。在实现1D，2D和3D模拟之间的收敛后，我们研究了超新星喷出物中的混合及其对测热LC的影响。我们观察到轻微的偏离球对称，这与维数增加。我们没有发现显着的影响测热LC，但是，我们得出结论，瑞利-泰勒不稳定性所造成的硅和氧富层之间的混合可能会影响光谱。
In recent years, the viability of the pair-instability supernova (PISN) scenario for explaining superluminous supernovae has all but disappeared except for a few slowly-evolving examples. However, PISNe are not predicted to be superluminous throughout the bulk of their mass range. In fact, it is more likely that the first PISN we see (if we have not seen one already) will not be superluminous. Here, we present hydrodynamic simulations of PISNe for four stellar models with unique envelope properties spanning the PISN mass range. In addition, we compute synthetic light curves (LCs) for comparison with current and future observations. We also investigate, in the context of our most massive model, the prospect of mixing in the supernova ejecta, alleviating discrepancies between current PISN models and the remaining superluminous candidate events. To this end, we present the first published 3D hydrodynamic simulations of PISNe. After achieving convergence between 1D, 2D, and 3D simulations, we examine mixing in the supernova ejecta and its affect on the bolometric LC. We observe slight deviations from spherical symmetry, which increase with the number of dimensions. We find no significant effects on the bolometric LC; however, we conclude that mixing between the silicon and oxygen rich layers caused by the Rayleigh–Taylor instability may affect spectra.