Binary fraction indicators in resolved stellar populations and supernova-type ratios
Binary fraction indicators in resolved stellar populations and supernova-type ratios
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DOI：
10.1093/mnras/staa2089
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发表时间：
2020-07
影响因子：
4.8
通讯作者：
E. Stanway;J. Eldridge;A. Chrimes
中科院分区：
文献类型：
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作者：
E. Stanway;J. Eldridge;A. Chrimes
恒星群体的双星比例会对其性质产生显著影响，特别是不同大质量星星类型的数量，以及超新星结束生命的相对子类型率。在这里，我们使用具有随初始质量变化的二元分数的二元粒子数合成模型来测试对解析的恒星粒子数和超新星的影响，并询问这些模型是否可以在不同的质量和金属丰度状态下限制鲜为人知的二元分数。我们发现，沃尔夫-拉叶星星亚型比是有价值的二进制诊断，但需要大样本来区分模型。探索了在光谱学上将恒星模型分类为沃尔夫-拉叶星的不确定性。热核、剥离的包层和其他核心坍缩超新星的比例可能证明是一个更容易获得的测试，即将进行的调查将足以限制z < 1星系群中的高质量和低质量双星比例。
The binary fraction of a stellar population can have pronounced effects on its properties, and in particular the number counts of different massive star types, and the relative subtype rates of the supernovae which end their lives. Here we use binary population synthesis models with a binary fraction that varies with initial mass to test the effects on resolved stellar populations and supernovae, and ask whether these can constrain the poorly-known binary fraction in different mass and metallicity regimes. We show that Wolf-Rayet star subtype ratios are valuable binary diagnostics, but require large samples to distinguish by models. Uncertainties in which stellar models would be spectroscopically classified as Wolf-Rayet stars are explored. The ratio of thermonuclear, stripped envelope and other core-collapse supernovae may prove a more accessible test and upcoming surveys will be sufficient to constrain both the high mass and low mass binary fraction in the z < 1 galaxy population.