Chemical Evolution


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Contact: F.X.Timmes
my one page vitae,
full vitae,
research statement, and
teaching statement.

Galactic chemical evolution: Hydrogen through zinc (1995)

In this paper, using the output from a grid of 60 Type II supernova models of varying mass (11 ≤ M/M ≤ 40) and metallicity (0, 10-4, 0.01, 0.1, and 1 Z), 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 billion year e-folding time scale 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 ≤ [Fe/H] ≤ 0.0 dex. Sampled 4.6 billion years ago at a distance of 8.5 kpc, we find a composition at the solar circle that is in excellent agreement with the solar abundances from hydrogen to zinc:

The source code, a nucleosynthesis data file, and input deck are included in the bzip2 tarball chem.tgz. This paper, describes the chemical evolution code and its results. It's a more-or-less a complete description of our understanding of nucleosynthesis from hydrogen to zinc circa 1995. The nucleosynthesis data file, maltov1.orig, contains isotopic contributions from
• Type II supernovae - Woosley & Weaver 1995 models
• Low mass stars - Renzini & Violi 1986 models
• Six different Type Ia supernovae models
• Three different classical novae models
• Big Bang
You can easily change or modify the plain text file maltov1.orig.

Please cite the relevant references if you publish a piece of work that use these codes, pieces of these codes, or modified versions of them. Offer co-authorship as appropriate.