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

Published online by Cambridge University Press:  05 March 2013

Yong-Zhong Qian
Yong-Zhong Qian*
Affiliation:
School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA. Email: qian@physics.umn.edu
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Abstract

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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.

Keywords

Galaxy: evolutionnuclear reactions, nucleosynthesis, abundancesstars: Population IIsupernovae: general
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 25 , Issue 1 , 2008 , pp. 36 - 43
Copyright
Copyright © Astronomical Society of Australia 2008

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