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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 efolding time scale onto a exponential disk and 1/r^{2} 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:



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