Effective mass splitting and neutron star properties at finite temperature

Finite temperature calculation of equation of state (EOS) of charge neutral β-stable n + p + e + μ matter (NSM) at finite temperature T is crucial in the study of formation mechanism of neutron stars (NS) which have temperature as high as ∼ 50 MeV in the core at when they born. In the present work, the objective is to calculate the NS properties at finite T with particular emphasis on the momentum dependence of nucleonic mean fields. Yukawa effective interaction (YEI) has been used in the study that has been successfully used in the calculations of EOS of NSM at finite temperature and thermal evolution of properties of nuclear matter (NM)