In-medium nuclear cluster energies within the Extended Thomas-Fermi approach

Abstract

A recently introduced analytical model for the nuclear density profile[1] is implemented in the Extended Thomas-Fermi (ETF) energy density functional. This allows to (i) shed a new light on the issue of the sign of surface symmetry energy in nuclear mass formulas, which is strongly related to the non-uniformity of the isospin asymmetry in finite nuclei, as well as to (ii) evaluate the in-medium corrections to the nuclear cluster energies in thermodynamic conditions relevant for the description of the (proto)-neutron star crust. The ground state configurations of the model are compared to Hartree-Fock calculations in spherical symmetry for some selected isotopic chains, and systematic errors are quantified. The in-medium modification of the nuclear mass due to the presence of a gas component is shown to strongly depend both on the density and the asymmetry of the nucleon gas. This shows the importance of accounting for such effects in the realistic modelizations of the equation of state for core-collapse supernovae and proto-neutron stars.

15 pages, 9 figures

References in corpus (9)

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• Light nuclei quasiparticle energy shift in hot and dense nuclear matter
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Cited by in corpus (8)

• Constraining supernova equations of state with equilibrium constants from heavy-ion collisions
• Dependence of weak interaction rates on the nuclear composition during stellar core collapse
• Liquid-gas coexistence vs. energy minimization with respect to the density profile in the inhomogeneous inner crust of neutron stars
• EoS constraints from nuclear masses and radii in a meta-modeling approach
• A new statistical method for the structure of the inner crust of neutron stars
• Low density nuclear matter with light clusters in a generalized nonlinear relativistic mean-field model
• Self consistent calculation of the nuclear composition in hot and dense stellar matter
• Parametrization of the surface energy in the ETF approximation