Warm Asymmetric Nuclear Matter and Proto-Neutron Star

Abstract

Asymmetric nuclear matter equation of state at finite temperature is studied in SU(2) chiral sigma model using mean field approximation. The effect of temperature on effective mass, entropy, and binding energy is discussed. Treating the system as one with two conserved charges the liquid-gas phase transition is investigated. We have also discussed the effect of proton fraction on critical temperature with and without $\rho$-meson contribution. We have extended our work to study the structure of proto-neutron star with neutron free charge-neutral matter in beta-equilibrium. We found that the mass and radius of the star decreases as it cools from the entropy per baryon S = 2 to S = 0 and the maximum temperature of the core of the star is about 62 MeV for S = 2.

25 pages, 16 figures

References in corpus (7)

• Recent Progress in Quantum Hadrodynamics
• Evolution of Protoneutron Stars
• Hot Nuclear Matter in the Quark Meson Coupling Model
• SU(2) Chiral sigma model and the properties of neutron stars
• Warm asymmetric matter in the Quark Meson Coupling Model
• A nuclear many-body theory at finite temperature applied to protoneutron star
• Phase transition and hybrid star in a SU(2) chiral sigma model

Cited by in corpus (3)

• Equation of state for $\beta$-stable hot nuclear matter
• Temperature and momentum dependence of single-particle properties in hot asymmetric nuclear matter
• Nuclear matter at finite temperature and static properties of proto-neutron star