Density and temperature dependence of symmetry energy and incompressibility within relativistic mean field model

The behavior of nuclear matter at high density and nite temperature is one of the challenging problems in contemporary modern nuclear physics. Efforts are being made using various models to understand the symmetry energy and incompressibility. The density dependence of symmetry energy influences the nature and stability of the phases of compact star (CS), the feasibility of direct URCA cooling process within interior of CS, the composition and thickness of inner crust of CS, the frequency of its crustal vibrations and radius of CS. Many correlations have been studied to understand the density behavior of symmetry energy. However, the fundamental origin of this apparent evolution of symmetry energy is still not clear, and it is particularly important to understand to what degree its evolution depends on the density and/or temperature of nuclear matter. Apart from symmetry energy, the nuclear matter equation of state (EOS) also depend upon the values of incompressibility. In recent times the giant monopole resonance has made it possible to find the value of incompressibility. Accurate knowledge of the density and temperature dependence of symmetry energy and incompressibility can lead to plausible EOS of the asymmetric matter