A High-resolution Study of Presupernova Core Structure
A High-resolution Study of Presupernova Core Structure
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DOI：
10.3847/1538-4357/aac2da
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发表时间：
2017-10
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影响因子：
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通讯作者：
T. Sukhbold;S. Woosley;A. Heger
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作者：
T. Sukhbold;S. Woosley;A. Heger
大质量星星死亡时其铁核周围的密度结构对星星是否爆炸有着重要的影响。在这里，我们重复以前的调查前超新星的演变与一些重要的更正，以编码物理和4至10倍更好的质量分辨率在每个星星。前超新星质量的数量也要大得多。超过4000个模型的计算范围从12到60 M的不同质量损失率。增加的空间分辨率对核心结构的影响不大。紧性测度的定性模式及其极值是相同的，但随着模型数量的增加，在以前的研究中看到的分散被几个本地化的分支所取代。Ertl等人和Müller等人的更多基于物理学的分析表明，这些分支比奥康纳和奥特的单参数表征具有更少的分散性。这些分支在质量范围为14-19和22-24 M <$的恒星中特别明显。多值解是演化后期几个碳氧燃烧壳层之间相互干扰的结果。对于一个相关的质量范围来说，一颗星星是否爆炸，可能比其初始质量更能反映其后期演化中微小的、几乎随机的差异。大量的模型允许对超新星前恒星的半径、光度和有效温度、它们的核心结构和残余质量分布进行统计上有意义的陈述。
The density structure surrounding the iron core of a massive star when it dies is known to have a major effect on whether or not the star explodes. Here we repeat previous surveys of presupernova evolution with some important corrections to code physics and four to 10 times better mass resolution in each star. The number of presupernova masses considered is also much larger. Over 4000 models are calculated in the range from 12 to 60 M⊙ with varying mass loss rates. The core structure is not greatly affected by the increased spatial resolution. The qualitative patterns of compactness measures and their extrema are the same, but with the increased number of models, the scatter seen in previous studies is replaced by several localized branches. More physics-based analyses by Ertl et al. and Müller et al. show these branches with less scatter than the single-parameter characterization of O’Connor & Ott. These branches are particularly apparent for stars in the mass ranges 14–19 and 22–24 M⊙. The multivalued solutions are a consequence of interference between several carbon- and oxygen-burning shells during the late stages of evolution. For a relevant range of masses, whether a star explodes or not may reflect the small, almost random differences in its late evolution more than its initial mass. The large number of models allows statistically meaningful statements about the radius, luminosity, and effective temperatures of presupernova stars, their core structures, and their remnant mass distributions.