We explore the variations in the progenitors of supernovae due to changes in the number of isotopes in a fully-coupled nuclear reaction network and adjustments in the mass resolution. We explore single, non-rotating, solar metallicity stars using MESA, in the mass range of 15-30 solar masses. We discuss the changes in the evolution of the star and the final state of the pre-supernovae star. The choice of network size and numerical resolution is found to have larger impacts on the stellar structure on the from the MS up and to core collapse. We find that up to carbon burning the choice of numerical resolution has the largest impact. After carbon burning the choice of nuclear network plays a larger role in determining the final state of the star. Variations of ~30% in the central electron fraction can be found in the supernovae progenitor as well as changes in the iron core of up to ~10% are possible. We find a minimum mass resolution of ~0.01 solar masses is necessary to achieve convergence in the helium core mass at the 5% level. For the choice of nuclear network, we find a minimum of 127 isotopes, in a fully coupled nuclear network, is needed to attain convergence at the 10% level.
American Astronomical Society Meeting Abstracts #229
- Pub Date:
- January 2017