Relativistic equation of state at subnuclear densities in the Thomas-Fermi approximation

Abstract

We study the non-uniform nuclear matter using the self-consistent Thomas--Fermi approximation with a relativistic mean-field model. The non-uniform matter is assumed to be composed of a lattice of heavy nuclei surrounded by dripped nucleons. At each temperature $T$, proton fraction $Y_p$, and baryon mass density ${\rho }_B$, we determine the thermodynamically favored state by minimizing the free energy with respect to the radius of the Wigner--Seitz cell, while the nucleon distribution in the cell can be determined self-consistently in the Thomas--Fermi approximation. A detailed comparison is made between the present results and previous calculations in the Thomas--Fermi approximation with a parameterized nucleon distribution that has been adopted in the widely used Shen EOS.

26 pages, 9 figures

References in corpus (4)

• Neutron Star Observations: Prognosis for Equation of State Constraints
• Theory of Core-Collapse Supernovae
• Appearance of Light Clusters in Post-bounce Evolution of Core-Collapse Supernovae
• The pasta phase within density dependent hadronic models

Cited by in corpus (6)

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• Light clusters, pasta phases and phase transitions in core-collapse supernova matter
• Symmetry energy of hot nuclei in the relativistic Thomas-Fermi approximation
• Nuclear pasta in hot and dense matter and its influence on the equation of state for astrophysical simulations
• The phase transition in hot $\Lambda$ hypernuclei within relativistic Thomas-Fermi approximation
• Nuclear Matter and Finite Nuclei: Relativistic Thomas-Fermi Approximation Versus Relativistic Mean-Field Approach