Speaker
Description
The FSU2H equation of state model, originally developed to describe cold neutron star matter with hyperonic cores, is extended to finite temperature [1]. Results are presented for a wide range of temperatures and lepton fractions, which cover the conditionsmet in protoneutron star matter, neutron star mergers and supernova explosions. It is found that the temperature effects on thethermodynamical observables and the composition of the neutron star core are stronger when the hyperonic degrees of freedomare considered. An evaluation of the temperature and density dependence of the thermal index leads to the observation that theso-called Γ law, widely used in neutron star merger simulations, is not appropriate to reproduce the true thermal effects, specially when hyperons start to be abundant in the neutron star core.
[1] H. Kochankovski, A. Ramos and L. Tolos, 2206.11266 [astro-ph.HE]
