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We present an updated and improved equation of state (which we call the NDLEoS) for use in neutron-star structure and supernova simulations. This EoS isbased upon a framework originally developed by Bowers & Wilson, but there arenumerous changes. Among them are: (1) a reformulation in the context of densityfunctional theory; (2) the possibility of the formation of material with a netproton excess (Ye > 0.5); (3) an improved treatment of the nuclear statisticalequilibrium and the transition to heavy nuclei as the density approachesnuclear matter density; (4) an improved treatment of the effects of pions inthe regime above nuclear matter density including the incorporation of all theknown mesonic and baryonic states at high temperature; (5) the effects of3-body nuclear forces at high densities; and (6) the possibility of afirst-order or crossover transition to a QCD chiral symmetry restoration anddeconfinement phase at densities above nuclear matter density. This paperdetails the physics of, and constraints on, this new EoS and describes itsimplementation in numerical simulations. We show comparisons of this EoS withother equations of state commonly used in supernova collapse simulations.

The NDL Equation of State for Supernova Simulations