Equations of state for supernovae and compact stars

TLDR

EoS models must span wide ranges in baryon density, temperature, and isospin asymmetry, capturing transitions from nucleon–nucleus mixtures to uniform, strongly interacting matter that may include hyperons or quarks. The authors review theoretical approaches to the dense‑matter equation of state applicable to core‑collapse supernovae, compact stars, and mergers, emphasizing models that span all scenarios and discussing experimental and observational constraints to guide future research. They survey diverse theoretical frameworks for the dense‑matter EoS, integrating experimental and observational constraints to inform model development across supernovae, compact stars, and merger contexts. They summarize results from applying the reviewed EoS models.

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.