Cluster formation in compact stars: relativistic versus Skyrme models

Abstract

We present various properties of nuclear and compact-star matter, comparing the predictions from two kinds of phenomenological approaches: relativistic models (both with constant and density-dependent couplings) and non-relativistic Skyrme-type interactions. We mainly focus on the liquid-gas instabilities that occur at sub-saturation densities, leading to the decomposition of the homogeneous matter into a clusterized phase. Such study is related to the description of neutron-star crust (at zero temperature) and of supernova dynamics (at finite temperature).

Accepted for publication

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Cited by in corpus (47)

• Equations of state for supernovae and compact stars
• Skyrme Interaction and Nuclear Matter Constraints
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• Density dependence of the nuclear symmetry energy: a microscopic perspective
• Equation of state and thickness of the inner crust of neutron stars
• The pasta phase within density dependent hadronic models
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• Warm pasta phase in the Thomas-Fermi approximation
• Spurious finite-size instabilities in nuclear energy density functionals
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• Dynamical properties of nuclear and stellar matter and the symmetry energy
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• A new statistical method for the structure of the inner crust of neutron stars
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• Phase transitions of hadronic to quark matter at finite T and μ_B
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• Transition density and pressure in hot neutron stars
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• Isospin-Asymmetry Dependence of the Thermodynamic Nuclear Equation of State in Many-Body Perturbation Theory
• Neutron-rich nuclei and the equation of state of stellar matter
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