Testing the role of SNe Ia for Galactic chemical evolution of p-nuclei with 2D models and with s-process seeds at different metallicities

TL;DR

This study investigates how Type Ia supernovae contribute to the production of p-nuclei in the galaxy using 2D models and varying s-process seed distributions at different metallicities, highlighting their significant role in galactic chemical evolution.

Contribution

It provides a detailed analysis of p-process nucleosynthesis in SNIa with different s-process seed distributions and assesses their contribution to solar p-nuclei using galactic chemical evolution models.

Findings

SNIa explosions produce significant p-nuclei across the mass range.

Production factors for p-nuclei are relatively flat, within a factor of 3.

Uncertainties in nuclear data affect the production of certain isotopes like 94Mo.

Abstract

The bulk of p isotopes is created in the 'gamma processes' mainly by sequences of photodisintegrations and beta decays in explosive conditions in Type Ia supernovae (SNIa) or in core collapse supernovae (ccSN). The contribution of different stellar sources to the observed distribution of p-nuclei in the Solar System is still under debate. We explore single degenerate Type Ia supernovae in the framework of two-dimensional SNIa delayed-detonation explosion models. Travaglio et al. (2011, TRV11) discussed the sensitivity of p-nuclei production to different SNIa models, i.e. delayed detonations of different strength, deflagrations, and the dependence on selected s-process seed distributions. Here we present a detailed study of p-process nucleosynthesis occuring in SNIa with s-process seeds at different metallicities. Based on the delayed-detonation model DDT-a of TRV11, we analyze the dependence of p-nucleosynthesis on the s-seed distribution obtained from different strengths of the 13C-pocket. Using a Galactic chemical evolution code (see Travaglio et al. 2004) we study the contribution of SNIa to the solar stable p-nuclei. We find that explosions of Chandrasekhar-mass single degenerate systems produce a large amount of p-nuclei in our Galaxy, both in the range of light (A < 120) and heavy p-nuclei, at almost flat average production factors (within a factor of about 3). We discussed in details p-isotopes such as 94Mo with a behavior diverging from the average, which we attribute to uncertainties in the nuclear data or in SNIa modelling.