Radiogenic p-isotopes from SNIa, nuclear physics uncertainties and Galactic chemical evolution compared with values in primitive meteorites

TL;DR

This study models nucleosynthesis in Type Ia supernovae to understand their contribution to primitive meteorite isotopic compositions, highlighting the importance of nuclear physics uncertainties.

Contribution

It introduces detailed multi-dimensional models of SNIa nucleosynthesis with varied metallicities and assesses their role in producing p-isotopes in the early solar system.

Findings

SNeIa can significantly contribute to p-isotope abundances in meteorites.

Nuclear physics uncertainties critically affect isotope production predictions.

Standard Chandrasekhar-mass SNeIa could explain observed meteorite isotope signatures.

Abstract

The nucleosynthesis of proton-rich isotopes is calculated for multi-dimensional Chandrasekhar-mass models of Type Ia supernovae with different metallicities. The predicted abundances of the short-lived radioactive isotopes 92Nb, 97Tc, 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 SNIa to the solar system p-nuclei composition measured in meteorites. Nuclear physics uncertainties are critical to determine the role of SNeIa in the production of 92Nb and 146Sm. We find that, if standard Chandrasekhar-mass SNeIa are at least 50% of all SNIa, they are strong candidates for reproducing the radiogenic p-process signature observed in meteorites.