radionuclides in supernova remnants.'
author:
- 'Andrews, S.'
- 'Fryer, C.'
- 'Even, W.'
- 'Jones, S.'
- 'Pignatari, M.'
bibliography:
- 'references.bib'
title: 'The Nucleosynthetic Yields of Core-Collapse Supernovae, prospects for the Next Generation of Gamma-Ray Astronomy'
---

Introduction
============

Core-collapse supernovae, produced in the violent implosion and subsequent explosion at the end of the life of a massive star, play a dominant role in galactic chemical evolution, synthesizing and injecting the many of the elements up to the iron-peak elements into the universe . Many of these elements are produced in the star during its lifetime through a succession of burning phases. These elements include the bulk of the carbon, oxygen, sodium and magnesium in the ejecta. Additionally, s-process elements synthesized in shell-burning layers like copper and germanium are also ejected in the supernova explosion [@meyer1994; @Pignatari_2010]. Core-collapse supernovae are also thought to be a site for the synthesis of elements beyond the the iron peak up to the first peak of the r-process, or the “weak r-process” [@Arnett_1970; @Wajano2005; @meyer1994 and references therein]. While current beliefs suggest that neutron star mergers, not core-collapse supernovae, are the primary site of r-process nucleosynthesis [@Lattimer1974; @Abbott_2017; @2019arXiv190101410C], this is far 