Equations of state for supernovae and compact stars

TL;DR

This paper reviews theoretical models for the equation of state of dense matter, crucial for understanding supernovae, compact stars, and mergers, emphasizing models applicable across diverse conditions and particle compositions.

Contribution

It provides a comprehensive overview of various EoS models applicable to all relevant astrophysical scenarios, integrating theoretical approaches with experimental and observational constraints.

Findings

EoS models cover wide density, temperature, and isospin ranges.

Matter composition varies from nucleon-nuclei-electron mixtures to uniform strongly interacting matter.

Applications of EoS models yield insights into supernovae and compact star phenomena.

Abstract

We review various theoretical approaches for the equation of state (EoS) of dense matter, relevant for the description of core-collapse supernovae, compact stars and compact star mergers. The emphasis is put on models that are applicable to all of these scenarios. Such EoS models have to cover large ranges in baryon number density, temperature and isospin asymmetry. The characteristics of matter change dramatically within these ranges, from a mixture of nucleons, nuclei, and electrons to uniform, strongly interacting matter containing nucleons, and possibly other particles such as hyperons or quarks. As the development of an EoS requires joint efforts from many directions we consider different theoretical approaches and discuss relevant experimental and observational constraints which provide insights for future research. Finally, results from applications of the discussed EoS models are summarized.