Effect of the Nuclear Equation of State on Relativistic-Turbulence Induced Core-Collapse Supernovae

The nuclear equation of state is an important component in the evolution of core-collapse supernovae. In this talk, I will present a survey of various Equations of State (EoS) in the literature and analyze their effect on spherical core-collapse models in which the effect of three-dimensional turbulence is introduced using a general relativistic version of the Mixing-Length model STIR (Couch et al. 2020). The explosion is quite EoS-dependent and it best correlates with the early-time entropy per baryon at the center of the Proto-Neutron Star (PNS). This is true across all progenitors that develop an iron core. Equations of state that produce larger central entropies result in stronger explosions. In addition to that, they are also correlated with more vigorous PNS convection, with wider convective layers in models exhibiting stronger explosions.