Study of hot nuclear matter within rellativistic mean field models

Core-collapse supernovae are one of the most important events in the universe. This is a site for the production of heavier nuclei through r-processes. At the moment of explosion, the temperature of nuclear matter (Neutron star) is high and the density at bounce of the collapsing core goes up to 1.5-2.0 times the nuclear saturation density. It is impossible to study nuclear matter at extreme temperature and density in a laboratory due to its incompressible nature. Hence, an equation of state (EOS), the relation between energy and pressure, is a tool to study nuclear matter at extreme conditions. Relativistic mean field (RMF) model is one of the most successful and widely used models to study nuclear matter ranging from finite nuclei to infinite nuclear matter. We have studied symmetric and asymmetric infinite nuclear matter at finite temperature within RMF models by considering NL3, G2, FSUGarnet and newly predicted IOPB-I and G3 force parameters. We have put different values of temperature and asymmetric coefficient and find the critical parameters; the parameters where both liquid and gas phases of matter exist.