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.
|Original language||English (US)|
|Number of pages||8|
|Journal||Publications of the Astronomical Society of Australia|
|State||Published - 2008|
Copyright 2008 Elsevier B.V., All rights reserved.
- Galaxy: evolution
- Nuclear reactions, nucleosynthesis, abundances
- Stars: Population II
- Supernovae: general