Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields

Abstract

Type Ia supernova explosions (SN Ia) are fundamental sources of elements for the chemical evolution of galaxies. They efficiently produce intermediate-mass (with Z between 11 and 20) and iron group elements—for example, about 70% of the solar iron is expected to be made by SN Ia. In this work, we calculate complete abundance yields for 39 models of SN Ia explosions, based on three progenitors—a 1.4 M _⊙ deflagration detonation model, a 1.0 M _⊙ double detonation model, and a 0.8 M _⊙ double detonation model—and 13 metallicities, with ^22 Ne mass fractions of 0, 1 × 10 ^−7 , 1 × 10 ^−6 , 1 × 10 ^−5 , 1 × 10 ^−4 , 1 × 10 ^−3 , 2 × 10 ^−3 , 5 × 10 ^−3 , 1 × 10 ^−2 , 1.4 × 10 ^−2 , 5 × 10 ^−2 , and 0.1, respectively. Nucleosynthesis calculations are done using the NuGrid suite of codes, using a consistent nuclear reaction network between the models. Complete tables with yields and production factors are provided online at Zenodo:Yields ( https://doi.org/10.5281/zenodo.8060323 ). We discuss the main properties of our yields in light of the present understanding of SN Ia nucleosynthesis, depending on different progenitor mass and composition. Finally, we compare our results with a number of relevant models from the literature.

Keywords

• Type Ia supernovae
• Nucleosynthesis
• Astrophysical explosive burning
• Nuclear astrophysics