# How Well Do We Know The Supernova Equation of State?

## TL;DR

This paper reviews current equations of state used in supernova and neutron star merger simulations, highlighting their limitations and the need for improved models to better match experimental and observational constraints.

## Contribution

It provides a comprehensive overview of existing EOS models, compares them with constraints, and discusses the challenges in modeling nuclear matter at high densities and finite temperatures.

## Key findings

- Few models meet experimental and astrophysical constraints.
- Significant uncertainties remain in high-density nuclear matter EOS.
- Recent developments have improved EOS tables, but further work is needed.

## Abstract

We give an overview about equations of state (EOS) which are currently available for simulations of core-collapse supernovae and neutron star mergers. A few selected important aspects of the EOS, such as the symmetry energy, the maximum mass of neutron stars, and cluster formation, are confronted with constraints from experiments and astrophysical observations. There are just very few models which are compatible even with this very restricted set of constraints. These remaining models illustrate the uncertainty of the uniform nuclear matter EOS at high densities. In addition, at finite temperatures the medium modifications of nuclear clusters represent a conceptual challenge. In conclusion, there has been significant development in the recent years, but there is still need for further improved general purpose EOS tables.