New equations of state constrained by nuclear physics, observations, and high-density QCD calculations
Abstract: We present new equations of state for applications in core-collapse supernova and neutron star merger simulations. We start by introducing an effective mass parametrization that is fit to recent microscopic calculations up to twice saturation density. This is important to capture the predicted thermal effects, which have been shown to determine the proto-neutron star contraction in supernova simulations. The parameter range of the energy-density functional underlying the equation of state is constrained by chiral effective field theory results at nuclear densities as well as by functional renormalization group computations at high densities based on QCD. We further implement observational constraints from the measurement of heavy neutron stars, the gravitational wave signal of GW170817, and by the recent NICER results. We will discuss the resulting allowed ranges for the equation of state and for the properties of neutron stars.