  A quantitative description of the properties of hot nuclear matter will be
needed for the interpretation of the available and forthcoming astrophysical
data, providing information on the post merger phase of a neutron star
coalescence. We have employed a recently developed theoretical model, based on
a phenomenological nuclear Hamiltonian including two- and three-nucleon
potentials, to study the temperature dependence of average and single-particle
properties of nuclear matter relevant to astrophysical applications. The
possibility to represent the results of microscopic calculations using simple
and yet physically motivated parametrisations of thermal effects, suitable for
use in numerical simulations of astrophysical processes, is also discussed.
