Speaker
Description
Neutron stars and explosive astrophysical systems - such as supernovae
or compact star binary mergers - represent natural laboratories where
extreme states of baryonic matter are populated. Modeling such
environments assumes, among others, good understanding of zero and
finite temperature equations of state (EoS). In this talk I shall first
discuss the relation between nuclear matter EoS and neutron star
properties. Then I shall review thermal properties of a number of
general purpose EoS. Properties of purely nucleonic EoS will be
confronted with properties of EoS which account for hyperons, meson
condensates, Deltaresonances and quarks. Correlations with parameters
of nuclear matter will be discussed along with the dependence on the
theoretical framework.
