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Nucleosynthesis in Massive Population II Stars

Published online by Cambridge University Press:  14 August 2015

David S. P. Dearborn  and
Virginia Trimble
David S. P. Dearborn
Affiliation:
Steward Observatory, U. Arizona
Virginia Trimble
Affiliation:
Steward Observatory, U. Arizona

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According to the conventional wisdom, the first stars formed in our Galaxy, including the massive ones responsible for most heavy element synthesis, must have had metal abundances much lower than solar. They may also have had somewhat lower helium abundances, corresponding to an enrichment ΔY/ΔZ = 2.7 ± 1.0 over the history of the Galaxy, a larger ratio than is readily accounted for by standard (Arnett-type) supernovae (Hacyan et al. 1977) or by mass shed from lower mass stars (Gingold 1977). But early nucleosynthesis must have occurred in stars with Pop II compositions. Several authors (Ezer and Cameron 1969; Cary 1974; Chiosi and Nasi 1974; Trimble et al. 1973) have modelled and evolved such stars, but none of the studies followed the stars far enough from the main sequence to be able to say anything very quantitative about their contribution to galactic chemical evolution. We address here the question of the effects of initial composition upon helium and heavy element production in massive stars.

Type
Part VII: Theoretical Papers and Summary
Information
Symposium - International Astronomical Union , Volume 80: The HR Diagram , 1978 , pp. 375 - 378
Copyright
Copyright © Reidel 1978 

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