Radiogenic p-isotopes from type Ia supernova, nuclear physics uncertainties, and galactic chemical evolution compared with values in primitive meteorites

C. Travaglio, R. Gallino, T. Rauscher, N. Dauphas, F. K. Röpke, W. Hillebrandt

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Abstract

The nucleosynthesis of proton-rich isotopes is calculated for multi-dimensional Chandrasekhar-mass models of Type Ia supernovae (SNe Ia) with different metallicities. The predicted abundances of the short-lived radioactive isotopes 92Nb, 97, 98Tc, and 146Sm are given in this framework. The abundance seeds are obtained by calculating s-process nucleosynthesis in the material accreted onto a carbon-oxygen white dwarf from a binary companion. A fine grid of s-seeds at different metallicities and 13C-pocket efficiencies is considered. A galactic chemical evolution model is used to predict the contribution of SN Ia to the solar system p-nuclei composition measured in meteorites. Nuclear physics uncertainties are critical to determine the role of SNe Ia in the production of 92Nb and 146Sm. We find that, if standard Chandrasekhar-mass SNe Ia are at least 50% of all SN Ia, they are strong candidates for reproducing the radiogenic p-process signature observed in meteorites.

Original languageEnglish
Article number141
JournalThe Astrophysical Journal
Volume795
Issue number2
DOIs
Publication statusPublished - 10 Nov 2014

Keywords

  • Atomic processes
  • Galaxy: abundances
  • Meteorites, meteors, meteoroids
  • Nuclear reactions, nucleosynthesis, abundances
  • Supernovae: general

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