The Nucleosynthetic Yields of Core-collapse Supernovae: Prospects for the Next Generation of Gamma-Ray Astronomy

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. The post-bounce temperature and density evolution of zero-age main-sequence 15, 20, and 25 solar mass progenitors are post-processed through the Nucleosynthesis Grid 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: K-43, Ca-47, Sc-44, Sc-47, V-48, Cr-48, Cr-51, Mn-52, Fe-59, Co-56, Co-57, and Ni-57. 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 K-43, Ca-47, Sc-44, Sc-47, and Fe-59, those that are dependent on the progenitor structure are V-48, Cr-51, and Co-57, and those that probe neither are Cr-48, Mn-52, Ni-57, and Co-56. We discuss the prospects of observing these radionuclides in supernova remnants.