The Nucleosynthetic Yields of Core-Collapse Supernovae, prospects for the Next Generation of Gamma-Ray Astronomy

TL;DR

This paper investigates how key parameters of core-collapse supernovae influence nucleosynthetic yields, focusing on radio-isotopes relevant for gamma-ray astronomy, to improve understanding of explosion mechanisms and observational prospects.

Contribution

It provides detailed predictions of radioactive isotope yields from supernova models, linking them to explosion parameters and assessing their detectability in remnants.

Findings

Isotopes 43K, 47Ca, 44Sc, 47Sc, 59Fe indicate explosion energy.

Isotopes 48V, 51Cr, 57Co depend on progenitor structure.

Some isotopes are unaffected by explosion parameters.

Abstract

Though the neutrino-driven convection model for the core-collapse explosion mechanism has received strong support in recent years, there are still many uncertainties in the explosion parameters -- such as explosion energy, remnant mass, and end-of-life stellar abundances as initial conditions. Using a broad set of spherically symmetric core-collapse simulations we examine the effects of these key parameters on explosive nucleosynthesis and final explosion yields. Post-bounce temperature and density evolution of ZAMS 15, 20, and 25 solar mass progenitors are post-processed through the Nucleosynthesis Grid (NuGrid) nuclear network to obtain detailed explosive yields. In particular, this study focuses on radio-isotopes that are of particular interest to the next generation of gamma-ray astronomical observations; 43K, 47Ca, 44Sc, 47Sc, 48V, 48Cr, 51Cr, 52Mn, 59Fe, 56Co, 57Co, 57Ni. These nuclides may be key in advancing our understanding of the inner workings of core-collapse supernovae by probing the parameters of the explosion engine. We find that the isotopes that are strong indicators of explosion energy are 43K, 47Ca, 44Sc, 47Sc, and 59Fe, those that are dependent on the progenitor structure are 48V, 51Cr, and 57Co, and those that probe neither are 48Cr, 52Mn, 57Ni, and 56Co. We discuss prospects of observing these radionuclides in supernova remnants.