Brandon Barker

In the pro-neutron star formed during a core collapse supernova (CCSN), densities can reach several times nuclear density. Due to uncertainties in nuclear physics, there are several different physical models for the equation of state (EOS) at the densities present in the CCSN environment. The outcomes of CCSN simulations can depend sensitively on the EOS. 1D CCSN simulations are key in predictions of the outcome of stellar evolution, neutron mass distribution, nucleosynthesis, and ultimately, galactic evolution. However, uncertainties in nuclear physics causes changes in these results; simulations using different EOS tables can lead to entirely different predictions. We explore the sensitivity of CCSNe to variations in input nuclear physics. Using 10 different EOS models, we ran 1D CCSN simulations with progenitor masses ranging from 9M to 120M using a new model for driving 1D explosions that includes the crucial effects of turbulence and convection. A quantitative understanding of how different EOs tables affect the outcome of core collapse is crucial to our ability to make predictions.