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Fe-peak element abundances in disk and halo stars

Published online by Cambridge University Press:  09 March 2010

Maria Bergemann  and
Thomas Gehren
Maria Bergemann
Affiliation:
Max-Planck Institute for Astrophysics, Karl-Schwarzschildt str. 1 87541, Garching, Germany email: mbergema@mpa-garching.mpg.de
Thomas Gehren
Affiliation:
University Observatory Munich, Scheiner str. 1 81679, Munich, Germany email: thomas.gehren@gmx.de
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Abstract

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At present none of galactic chemical evolution (GCE) models provides a self-consistent description of observed trends for all iron-peak elements with metallicity simultaneously. The question is whether the discrepancy is due to deficiencies of GCE models, such as stellar yields, or due to erroneous spectroscopically-determined abundances of these elements in metal-poor stars. The present work aims at a critical reevaluation of the abundance trends for several odd and even-Z Fe-peak elements, which are important for understanding explosive nucleosynthesis in supernovae.

Keywords

Line: formationLine: profilesStars: abundancesNucleosynthesis
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 348 - 349
Copyright
Copyright © International Astronomical Union 2010

References

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