Carbon burning in intermediate mass primordial stars
Abstract
The evolution of a zero metallicity 9 Ms star is computed, analyzed and compared with that of a solar metallicity star of identical ZAMS mass. Our computations range from the main sequence until the formation of a massive oxygen-neon white dwarf. Special attention has been payed to carbon burning in conditions of partial degeneracy as well as to the subsequent thermally pulsing Super-AGB phase. The latter develops in a fashion very similar to that of a solar metallicity 9 Ms star, as a consequence of the significant enrichment in metals of the stellar envelope that ensues due to the so-called third dredge-up episode. The abundances in mass of the main isotopes in the final ONe core resulting from the evolution are X(16O) approx 0.59, X(20Ne) approx 0.28 and X(24Mg) approx 0.05. This core is surrounded by a 0.05 Ms buffer mainly composed of carbon and oxygen, and on top of it a He envelope of mass 10-4 Ms
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