Modelling the evolution of solar-mass stars with a range of metallicities using MESA

The nuclides H-1,H-2, He-3,He-4, Li-7, Be-7, B-8, C-12,C-13, N13-15, O14-18, F17-19, Ne18-22, Mg-22, and Mg-24 were used in the code package MESA (Modules for Experiments in Stellar Astrophysics)[Paxton] to model a one-solar-mass star with a range of metallicities, z, from 0 to 0.1. On HR diagrams of each star model's luminosity and effective temperature from before zero-age main sequence (pre-ZAMS) to white dwarf, oscillations were noted in the horizontal branch at intervals from z = 0 to 0.0070. At z = 0, the calculated stellar lifetime is 6.09x10(9) years. The calculated lifetime of the model stars increases to a maximum of 1.25x10(10) years at z = 0.022 and then decreases to 2.59x10(9) years at z = 0.1. A piecewise fit of the model lifetimes vs. metallicity was obtained.