Nuclear Equation of state for Compact Stars and Supernovae

Understand

The equation of state (EoS) of hot and dense matter is a fundamental input to describe static and dynamical properties of neutron stars, core-collapse supernovae and binary compact-star mergers.

• We review the current status of the EoS for compact objects, that have been studied with both ab-initio many-body approaches and phenomenological models.
• We limit ourselves to the description of EoSs with purely nucleonic degrees of freedom, disregarding the appearance of strange baryonic matter and/or quark matter.
• We compare the theoretical predictions with different data coming from both nuclear physics experiments and astrophysical observations.