The state of matter in simulations of core-collapse supernovae -- Reflections and recent developments

TL;DR

This review examines the importance of the equation of state in core-collapse supernova simulations, highlighting recent developments and the different phases of matter involved, from nuclei to homogeneous matter.

Contribution

It provides a comprehensive overview of the current state and recent advances in modeling the matter phases in supernova simulations, emphasizing the role of the EOS.

Findings

Different regimes of matter are crucial in supernova modeling

Model EOS are used due to lack of first-principle calculations

The transition from inhomogeneous to homogeneous matter impacts supernova dynamics

Abstract

In this review article we discuss selected developments regarding the role of the equation of state (EOS) in simulations of core-collapse supernovae. There are no first-principle calculations of the state of matter under supernova conditions since a wide range of conditions is covered, in terms of density, temperature and isospin asymmetry. Instead, model EOS are commonly employed in supernova studies. These can be divided into regimes with intrinsically different degrees of freedom: heavy nuclei at low temperatures, inhomogeneous nuclear matter where light and heavy nuclei coexist together with unbound nucleons, and the transition to homogeneous matter at high densities and temperatures. In this article we discuss each of these phases with particular view on their role in supernova simulations.