Neutron-rich nuclei and the equation of state of stellar matter

TL;DR

This paper reviews the current understanding of the equation of state for neutron-rich matter in stellar environments, emphasizing nuclear interactions, thermodynamics, and astrophysical implications.

Contribution

It provides a comprehensive overview of the nuclear energy functional and thermodynamic behavior of neutron-rich matter at various temperatures.

Findings

Insights into the nuclear energy functional in isoscalar and isovector channels

Analysis of thermodynamics in nucleonic regimes with electromagnetic and nuclear interactions

Discussion of astrophysical implications and observables of exotic neutron-rich nuclei

Abstract

In this contribution we will review our present understanding of the matter equation of state in the density and temperature conditions where it can be described by nucleonic degrees of freedom. At zero temperature, all the information is contained in the nuclear energy functional in its isoscalar and isovector channels. At finite temperature, particular emphasis will be given to the specificity of the thermodynamics in the nucleonic regime, with the simultaneous presence of long range electromagnetic and short range nuclear interactions. The astrophysical implications of the resulting phase diagram, as well as of different observables of exotic nuclei on the neutron-rich side, will be touched upon.