| Summary: | One of the key ingredients to the core collapse supernova mechanism is the physics of matter at or near nuclear density. Included in simulations as part of the Equation of State (EoS), nuclear repulsion experienced at high densities is responsible for the bounce shock, which initially causes the outer envelope of the supernova to expand, as well as determining the structure of the newly formed proto-neutron star. Recent years have seen renewed interest in this fundamental piece of supernova physics, resulting in several promising candidate EoS parameterizations. We will present the impact of several of their variations in the nuclear EoS using spherically symmetric, General Relativistic multi group Boltzmann neutrino transport simulations of stellar core bounce and shock propagation.
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