Diverse Supernova Sources for the r-Process and Abundances in Metal-poor Stars
Diverse Supernova Sources for the r-Process and Abundances in Metal-poor Stars
复制标题
r过程的多种超新星源和贫金属恒星的丰度
DOI：
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发表时间：
2001
期刊：
影响因子：
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通讯作者：
Y. Qian
中科院分区：
文献类型：
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作者：
Y. Qian
基于r过程的多种超新星源模型，讨论了贫金属星r过程丰度的色散和平均趋势。该模型的独特之处在于，它的关键参数是从太阳系数据推断出来的，而不依赖于低金属丰度恒星的观测。结果表明，该模型能较好地解释Eu丰度在-3 <$[Fe/H]<$-1以上的分散性和平均趋势。它还表明，该模型提供了一种手段来讨论一般的r-丰度。例如，任何贫金属星星中的银丰度都可以从模型中计算出来，而这些恒星的铕和铁丰度都是观测到的。这种方法在两颗恒星上得到了成功的证明，并且可以通过未来的银数据进一步测试。此外，还计算了贫金属星银丰度的色散和平均趋势，以便与未来的观测结果进行比较。
The dispersion and mean trends of r-process abundances in metal-poor stars are discussed based on a model of diverse supernova sources for the r-process. This model is unique in that its key parameters are inferred from solar system data independent of stellar observations at low metallicities. It is shown that this model provides a good explanation for the observed dispersion and mean trend of Eu abundances over -3 ≲ [Fe/H] ≲ -1. It is also shown that this model provides a means to discuss r-abundances in general. For example, the Ag abundance in any metal-poor star with observed Eu and Fe abundances can be calculated from the model. This approach is demonstrated with success for two stars and can be further tested by future Ag data. The dispersion and mean trend of Ag abundances in metal-poor stars are also calculated for comparison with future observations.