University of Hertfordshire

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From the same journal

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  • 1408.6643v1

    Accepted author manuscript, 999 KB, PDF document

  • C. Travaglio
  • R. Gallino
  • T. Rauscher
  • N. Dauphas
  • F. K. Röpke
  • W. Hillebrandt
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Original languageEnglish
Article number141
JournalThe Astrophysical Journal
Journal publication date10 Nov 2014
Volume795
Issue2
DOIs
Publication statusPublished - 10 Nov 2014

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.

ID: 7756119