Thermal Properties of Asymmetric Nuclear Matter

Abstract

The thermal properties of asymmetric nuclear matter are investigated in a relativistic mean- field approach. We start from free space NN-interactions and derive in-medium self-energies by Dirac-Brueckner theory. By the DDRH procedure we derive in a self-consistent approach density- dependent meson-baryon vertices. At the mean-field level, we include isoscalar and isovector scalar and vector interactions. The nuclear equation of state is investigated for a large range of total baryon densities up to the neutron star regime, the full range of asymmetries from symmetric nuclear matter to pure neutron matter, and temperatures up to T~100 MeV. The isovector-scalar self-energies are found to modify strongly the thermal properties of asymmetric nuclear matter. A striking result is the change of phase transitions when isovector-scalar self-energies are included.

32 pages, 23 figures, 4 tables

References in corpus (6)

• Theory of Core-Collapse Supernovae
• Hot neutron matter from a Self-Consistent Green's Functions approach
• Nuclear matter in the crust of neutron stars derived from realistic NN interactions
• Critical temperature for the nuclear liquid-gas phase transition (from multifragmentation and fission)
• Liquid-gas phase transition in hot asymmetric nuclear matter with density-dependent relativistic mean-field models
• Spinodal Instabilities in Asymmetric Nuclear Matter Based on Realistic $NN$ Interactions

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• Quarkyonic matter and quarkyonic stars in an extended RMF model
• Thermal effects in hot and dilute homogeneous asymmetric nuclear matter
• Effects of inner crusts on $g$-mode oscillations in neutron stars
• Properties and microscopic structures of dense stellar matter in RMF models
• Unified treatment for in-medium light and heavy clusters with RMF models
• Isospin-Asymmetry Dependence of the Thermodynamic Nuclear Equation of State in Many-Body Perturbation Theory