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Title:
Galactic chemical evolution: Hydrogen through zinc
Authors:
Timmes, F. X.; Woosley, S. E.; Weaver, Thomas A.
Affiliation:
AA(Lawrence Livermore National Lab., Livermore, CA, US), AB(Lawrence Livermore National Lab., Livermore, CA, US), AC(Lawrence Livermore National Lab., Livermore, CA, US)
Publication:
Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 98, no. 2, p. 617-658 (ApJS Homepage)
Publication Date:
06/1995
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Abundance, Chemical Evolution, Galactic Evolution, Galactic Structure, Metallicity, Nuclear Fusion, Stellar Mass, Stellar Models, Supernovae, Carbon, Helium, Metals, Nitrogen, Oxygen
DOI:
10.1086/192172
Bibliographic Code:
1995ApJS...98..617T

Abstract

Using the output from a grid of 60 Type II supernova models (Woosley & Weaver 1995) of varying mass (11 approx. less than (M/solar mass) approx. less than 40) and metallicity (0, 10-4, 0.01, and 1 solar metallicity), the chemical evolution of 76 stable isotopes, from hydrogen to zinc, is calculated. The chemical evolution calculation employs a simple dynamical model for the Galaxy (infall with a 4 Gyr e-folding timescale onto a exponential disk and 1/r2 bulge), and standard evolution parameters, such as a Salpeter initial mass function and a quadratic Schmidt star formation rate. The theoretical results are compared in detail with observed stellar abundances in stars with metallicities in the range -3.0 approx. less than (Fe/H) approx. less than 0.0 dex. While our discussion focuses on the solar neighborhood where there are the most observations, the supernova rates, an intrinsically Galactic quality, are also discussed.

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