早期银河系重元素的化学演化：恒星源的意义
Chemical Evolution of Heavy Elements in the Early Galaxy: Implications for Stellar Sources
摘要：
概述了早期银河系中重元素的来源。它表明，在贫金属的恒星的丰度的观测，可以用来与恒星模型的基本理解，以指导寻找重r-过程核（r-核）的来源。观测表明，这种来源产生的元素从C到Zn（包括Fe）非常少。这有力地表明，起源于~8-11M_sun的O-Ne-Mg核坍缩超新星（SNe）是重r核的源。结果表明，基于Fe（来自Fe核坍缩SNe）和Eu（来自O-Ne-Mg核坍缩SNe）丰度的双组分模型对贫金属星中所有其他元素的丰度给出了很好的定量预测。
英文摘要：
An overview of the sources for heavy elements in the early Galaxy is given. It is shown that observations of abundances in metal-poor stars can be used along with a basic understanding of stellar models to guide the search for the source of the heavy r-process nuclei (r-nuclei). Observations show that this source produces very little of the elements from C through Zn including Fe. This strongly suggests that O-Ne-Mg core-collapse supernovae (SNe) from progenitors of ~8-11M_sun are the source for the heavy r-nuclei. It is shown that a two-component model based on the abundances of Fe (from Fe core-collapse SNe) and Eu (from O-Ne-Mg core-collapse SNe) gives very good quantitative predictions for the abundances of all the other elements in metal-poor stars.
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