Equation of State for Proto-Neutron Star

TL;DR

This paper explores the properties of the equation of state for proto-neutron stars, focusing on their inner crust structure, composition near the neutrino-sphere, and the impact of symmetry energy on neutron star characteristics.

Contribution

It introduces new complete equations of state for proto-neutron stars and supernovae, emphasizing the role of symmetry energy and its correlation with neutron star radii.

Findings

Correlation between symmetry energy and neutron star radii

Detailed composition models of PNS matter near neutrino-sphere

Impact of symmetry energy on neutron-rich nuclei properties

Abstract

Physics of the Equation of State (EoS) for proto-neutron star (PNS) concerns properties of neutron rich matter at finite temperature over wide range of densities. In this contribution we discuss the structure of PNS inner crust in a relativisitc mean filed model with spherical Wigner-Setiz approximation, and the composition of matter around neutrino-sphere in PNS in a virial expansion of non-ideal gas composed of nucleons and nuclei. We go on to discuss several new complete EoS for PNS and supernova, whose detailed composition is important for the neutrino dynamics. We focus on one important distinction for various EoS - the density dependence of symmetry energy E'sym, and its interesting correlation with the radii of neutron star, as well as properties of neutron distribution in neutron rich nuclei. Improved understanding of E'sym from terrestrial experiment on neutron distribution of neutron rich nuclei, benchmark calculations via ab initio methods, and statistical analysis on good quality observational data will advance our knowledge on EoS.