The NDL Equation of State for Neutron Star and Supernova Simulations

Astrophysical observations are showing remarkable convergence with laboratory measurements of nuclear properties of neutron matter near saturation density ($\rho_B \sim$ 2.6 $\times$ 10$^{14}$ g/cm$^{3}$). This talk will discuss a new nuclear equation of state, the Notre Dame Livermore EoS (NDL EoS), which is robust enough in the ranges of density ($\rho_B$ = 1 - 10$^{16}$ g/cm$^{3}$, temperature (T = 0 - 175 MeV) and electron fraction ($Y_e$ = 0 - 0.7) for use in current neutron star and supernova simulations. We will contrast the thermodynamic properties and nuclear abundances with modern implementations of the nuclear EoS based on RMF theory and the liquid drop model.