Nucleosynthesis in Supernovae, Hypernovae/Gamma-ray Bursts and Compact Binary Mergers

Abstract

We present the status and open problems of the astrophysical sites responsible for the nucleosynthesis of Fe-group and heavier elements (with the exception of the s-process). This involves type Ia supernovae with the requirement to have a low Y e -component (for the explanation of 55 Mn), the role of the core collapse supenova explosion mechanism in the composition of the Fe-group (and heavier?) ejecta, the transition between neutron star and black hole remnants as the result of the collapse of massive stars, and the relation of the latter with supernova and/or gamma-ray bursts / hypernovae. In addition, the role of compact binary mergers is discussed, especially with respect to forming the heaviest r-process elements in galactic eveolution.

Dust in Supernovae and Supernova Remnants I: Formation Scenarios

“…For the sake of simplicity, a 1D stratified model of the ejecta is assumed and we shall ignore the details of the explosion mechanism in this discussion. The abundances of post-explosion elements are provided by nucleosynthesis studies and hydrodynamic simulation models of the ejecta (Woosley and Weaver 1995;Thielemann et al 1996Thielemann et al , 2011Thielemann 2017;Limongi et al 2000;Rauscher et al 2002). The final yields from these models correspond to a timescale of 6-7 hours from the explosion.…”