Chemical Evolution of Heavy Elements in the Early Galaxy: Implications for Stellar Sources

Publications of the Astronomical Society of Australia

Yong-Zhong Qian¹ 

关键词: Galaxy: evolution;    nuclear reactions;    nucleosynthesis;    abundances;    stars: Population II;    supernovae: general;   

DOI  :  10.1071/AS07042

学科分类：天文学(综合)

来源: CSIRO

【 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 ∼8–11 M⊙ 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.

【 授权许可】

Unknown