Equation of State Dependence of the Observable Properties of Turbulence-aided Neutrino-driven Core-collapse Supernovae

In the proto-neutron star formed during a core collapse supernova (CCSN), densities can reach manytimes 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 CCSNe. 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 star mass distribution, and nucleosynthesis. 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 form 9M_⊙ to 120M_⊙ using a new model for driving 1D explosions that includes the effects of turbulence and convection. We found that the neutrino and gravitational wave signals depend sensitively on the EOS. A quantitative understanding of how different EOS's affect the outcome of core collapse is crucial to our ability to make predictions.

We acknowledge support from the MSU ACRES REU program, which is supported by the National Science Foundation byGrant ACI-1560168.