The Equation of State of Hot, Dense Matter and Neutron Stars

TL;DR

This paper reviews recent advances in constraining the equation of state of dense matter using neutron star observations, nuclear experiments, and theoretical models, highlighting implications for astrophysics and nuclear physics.

Contribution

It synthesizes recent experimental, observational, and theoretical developments to refine the understanding of the dense matter equation of state relevant for neutron stars.

Findings

Constraints on the equation of state from neutron star mass measurements

Implications for neutron star structure and supernovae

Discussion of thermal properties and heavy-ion collision roles

Abstract

Recent developments in the theory of pure neutron matter and experiments concerning the symmetry energy of nuclear matter, coupled with recent measurements of high-mass neutron stars, now allow for relatively tight constraints on the equation of state of dense matter. We review how these constraints are formulated and describe the implications they have for neutron stars and core-collapse supernovae. We also examine thermal properties of dense matter, which are important for supernovae and neutron star mergers, but which cannot be nearly as well constrained at this time by experiment. In addition, we consider the role of the equation of state in medium-energy heavy-ion collisions.