An effective model for nuclear matter with many-body interactions at finite temperature

In this work, the extension for finite temperature of the Many-Body Forces Model (MBF Model) is presented for the first time. The MBF Model describes nuclear matter in a relativistic effective field theory formalism that takes many-body forces into account, by means of a field dependence of the nuclear interaction coupling constants. Assuming that nuclear matter is charge neutral, beta-equilibrated and populated by the baryon octet, electrons and muons, we explore the parameters of the model, different hyperonic coupling schemes and temperature effects to describe basic properties of nuclear matter, including speed of sound, compressibility and adiabatic index. Moreover, the mass-radius relation of compact stars is determined, by solving the Tolman-Oppenheimer-Volkoff (TOV) equations. Our first hand results at finite temperature open the path to a new description of proto-neutron stars using the MBF Model.