Equation of state for $\beta$-stable hot nuclear matter

Abstract

We provide an equation of state for hot nuclear matter in $\beta$-equilibrium by applying a momentum-dependent effective interaction. We focus on the study of the equation of state of high-density and high-temperature nuclear matter, containing leptons (electrons and muons) under the chemical equilibrium condition in which neutrinos have left the system. The conditions of charge neutrality and equilibrium under $\beta$-decay process lead first to the evaluation of proton and lepton fractions and afterwards of internal energy, free energy, pressure and in total to the equation of state of hot nuclear matter. Thermal effects on the properties and equation of state of nuclear matter are assesed and analyzed in the framework of the proposed effective interaction model. Special attention is dedicated to the study of the contribution of the components of $\beta$-stable nuclear matter to the entropy per particle, a quantity of great interest for the study of structure and collapse of supernova.

28 pages, 18 figures

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• Neutron-proton effective mass splitting and thermal evolution in neutron rich matter
• Effects of the equation of state on the core-crust interface of slowly rotating neutron stars
• Thermodynamics of Hot Neutron Stars and Universal Relations
• Neutron Stars and Gravitational Waves: the Key Role of Nuclear Equation of State
• Accurate nuclear symmetry energy at finite temperature within a BHF approach
• Thermal effects on tidal deformability in the last orbits of an inspiraling binary neutron star system
• Crust-core interface and bulk neutron star properties
• Equation of state for dense supernova matter
• Temperature-dependence of single-particle properties in isospin-symmetric and -asymmetric matter within the Dirac-Brueckner-Hartree-Fock model
• Temperature effects on the neutron matter equation of state obtained from chiral effective field theory
• Equation of State of Hot Neutron Star Matter using Finite Range Simple Effective Interaction
• Investigating Possible Existence of Hyper-Heavy Nuclei in Neutron Star Environment
• On the stable configuration of ultra-relativistic material spheres. The solution for the extremely hot gas