Speaker
Description
We review the equation of state (EoS) models covering a large range
of temperatures, baryon number densities and electron fractions
presently available on the \textsc{CompOSE} database. These models
are intended to be directly usable within numerical simulations of
core-collapse supernovae, binary neutron star mergers and
proto-neutron star evolution. We discuss their compliance with
existing constraints from astrophysical observations and nuclear
data. For a selection of purely nucleonic models in reasonable
agreement with the above constraints, after discussing the
properties of cold matter, we review thermal properties for
thermodynamic conditions relevant for core-collapse supernovae and
binary neutron star mergers. We find that the latter are strongly
influenced by the density dependence of the nucleon effective mass.
The selected bunch of models is used to investigate the EoS
dependence of hot star properties, where entropy per baryon and
electron fraction profiles are inspired from proto-neutron star
evolution. The $\Gamma$-law analytical thermal EoS used in many
simulations is found not to describe well these thermal properties
of the EoS. However, it may offer a fair description of the
structure of hot stars whenever thermal effects on the baryonic part
are small, as shown here for proto-neutron stars starting from
several seconds after bounce.
