  A set of microscopic, covariant density-functional, and non-relativistic
Skyrme-type equations of state is employed to study the structure of purely
nucleonic neutron stars at finite temperature. After examining the agreement
with presently available astrophysical observational constraints, we find that
the magnitude of thermal effects depends on the nucleon effective mass as well
as on the stiffness of the cold equation of state. We evidence a fairly small
but model-dependent effect of finite temperature on stellar stability that is
correlated with the relative thermal pressure inside the star.
