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

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

2008-07-04

arxiv.org/abs/0807.0814v1

Pub. Astron. Soc. Australia 25 (2008) 36-43

Astronomy and Astrophysics

Astrophysics

9 pages, 6 figures

Scientific paper

10.1071/AS07042

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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