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.

arXiv comment26 pages, 9 figures

References in corpus (20)

• Neutron Star Observations: Prognosis for Equation of State Constraints
• Theory of Core-Collapse Supernovae
• Strange Quark Matter and Compact Stars
• Statistical Model for a Complete Supernova Equation of State
• A New Mechanism for Core-Collapse Supernova Explosions
• Postbounce evolution of core-collapse supernovae: Long-term effects of equation of state
• Relativistic Equation of State for Core-Collapse Supernova Simulations
• Nuclear pasta structures and the charge screening effect
• Appearance of Light Clusters in Post-bounce Evolution of Core-Collapse Supernovae
• The pasta phase within density dependent hadronic models
• A new baryonic equation of state at sub-nuclear densities for core-collapse simulations
• Saturation of nuclear matter and radii of unstable nuclei
• Warm pasta phase in the Thomas-Fermi approximation
• New equations of state based on the liquid drop model of heavy nuclei and quantum approach to light nuclei for core-collapse supernova simulations
• The neutron star inner crust and symmetry energy
• Equation of State of Dense Matter from a density dependent relativistic mean field model
• Emergence of hyperons in failed supernovae: trigger of the black hole formation
• The equation of state and composition of hot, dense matter in core-collapse supernovae
• Thomas-Fermi theory for atomic nuclei revisited
• Nuclei beyond the drip line

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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
• Effects of finite size and symmetry energy on the phase transition of stellar matter at subnuclear densities
• 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