Nuclear and Particle Physics, Astrophysics and Cosmology, T-2

EOS of Dense Matter at Finite Temperature

Gang Shen
Indiana U.

Nuclear matter is usually defined as matter consisted of neutrons and protons with equal number of electrons to keep charge neutrality, whose densities ranges from neutron drip-out density to saturation density and above, i.e., from nonuniform nuclear matter to uniform nuclear matter. The equation of state for nuclear matter is important for understanding the structure of neutron star and the mechanism of supernova explosion. In this project, we will explore the equation of state for non-uniform and uniform nuclear matter at finite temperature in a consistent way by applying the RMF model throughout. For non-uniform nuclear matter, we apply Wigner-Seitz approximation to find the stable state for the system. We will focus on the analyses for phase transition densities in this talk.

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