Nucleosynthesis in the Innermost Ejecta of Magnetorotational Supernova Explosions in 3-dimensions

Abstract

Core-collapse supernova (CCSN) explosions powered by rotation and magnetic fields present an interesting astrophysical site for nucleosynthesis that potentially contributes to the production of \(r\)-process elements. Here we present yields of the innermost ejecta in 3D magnetorotational CCSN models simulated using the CoCoNuT-FMT code. Strong magnetic fields tap the rotational energy of the proto-neutron star and lead to earlier and more energetic (\(\sim 3\times 10^{51}\) erg) explosions than typical neutrino-driven CCSNe. Compared to a reference non-magnetic model, the ejecta in the magnetorotational models have much more neutron-rich components with Ye down to \(\sim\)0.25. Our post-processing calculations with the reaction network SkyNet show significant production of weak \(r\)-process elements up to mass number \(\sim\)130. We find negligible differences in the synthesis of heavy elements between two magnetorotational models with different initial field strength of 10\(^{10}\) and 10\(^{12}\) G, in accord with their similar explosion dynamics. The magnetorotational models produce about \(\sim\)0.19 and 0.14 Msun of radioactive \(^{56}\)Ni, on the low end of inferred hypernova nickel masses. The yields are publicly available at Zenodo: doi:10.5281/zenodo.10578981 for comparison with stellar abundance patterns, inclusion in modelling galactic chemical evolution, and comparison with other yield calculations. Our results add to the yet restricted corpus of nucleosynthesis yields from 3D magnetorotational supernova simulations and will help quantify yield uncertainties.