Recent breakthroughs in Skyrme-Hartree-Fock-Bogoliubov mass formulas

Abstract

We review our recent achievements in the construction of microscopic mass tables based on the Hartree-Fock-Bogoliubov method with Skyrme effective interactions. In the latest of our series of HFB-mass models, we have obtained our best fit ever to essentially all the available mass data, by treating the pairing more realistically than in any of our earlier models. The rms deviation on the 2149 measured masses of nuclei with N and Z>8 has been reduced for the first time in a mean field approach to 0.581 MeV. With the additional constraint on the neutron-matter equation of state, this new force is thus very well-suited for the study of neutron-rich nuclei and for the description of astrophysical environments like supernova cores and neutron-star crusts.

Proceedings of the Fifth International Conference on Exotic Nuclei and Atomic Masses, September 7-13 2008, Ryn (Poland). To appear in the European Physical Journal A

References in corpus (5)

• Skyrme-Hartree-Fock-Bogoliubov nuclear mass formulas: Crossing the 0.6 MeV threshold with microscopically deduced pairing
• Microscopic justification of the Equal Filling approximation
• Further explorations of Skyrme-Hartree-Fock-Bogoliubov mass formulas. IX: Constraint of pairing force to ${}^1{S}_0$ neutron-matter gap
• Screening Effects in Superfluid Nuclear and Neutron Matter within Brueckner Theory
• Semi-classical equation of state and specific heats for neutron-star inner crust with proton shell corrections

Cited by in corpus (12)

• Equations of state for supernovae and compact stars
• Spin and spin-isospin instabilities in asymmetric nuclear matter at zero and finite temperatures using Skyrme functionals
• Effective contact pairing forces from realistic calculations in infinite homogeneous nuclear matter
• Nucleosynthesis and observation of the heaviest elements
• Role of the symmetry energy and the neutron-matter stiffness on the tidal deformability of a neutron star with unified equations of state
• Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. IV. Role of the symmetry energy in pasta phases
• ${}^1$S${}_0$ pairing gaps, chemical potential and entrainment matrix in superfluid neutron-star cores for the Brussels-Montreal functionals
• Role of neutron pairing with density-gradient dependence in the semi-microscopic treatment of the inner crust of neutron stars
• Role of the Symmetry Energy on the Structure of Neutron Stars with Unified Equations of State
• Pinning down the superfluid and nuclear equation of state and measuring neutron star mass using pulsar glitches
• The nuclear symmetry energy and other isovector observables from the point of view of nuclear structure
• $\beta$-delayed $\gamma$-proton decay in ${}^{56}$Zn: analysis of the charged-particle spectrum