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Symmetry energy: nuclear masses and neutron stars

  • J. M. Pearson
  • N. Chamel
  • A. F. Fantina
  • S. Goriely
Regular Article - Theoretical Physics
Part of the following topical collections:
  1. Topical issue on Nuclear Symmetry Energy

Abstract

We describe the main features of our most recent Hartree-Fock-Bogoliubov nuclear mass models, based on 16-parameter generalized Skyrme forces. They have been fitted to the data of the 2012 Atomic Mass Evaluation, and favour a value of 30MeV for the symmetry coefficient J , the corresponding root-mean square deviation being 0.549MeV. We find that this conclusion is compatible with measurements of neutron-skin thickness. By constraining the underlying interactions to fit various equations of state of neutron matter calculated ab initio our models are well adapted to a realistic and unified treatment of all regions of neutron stars. We use our models to calculate the composition, the equation of state, the mass-radius relation and the maximum mass. Comparison with observations of neutron stars again favours a value of J = 30 MeV.

Keywords

Neutron Star Symmetry Energy Drip Line Skyrme Force Neutron Drip Line 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© SIF, Springer-Verlag Berlin Heidelberg 2014

Authors and Affiliations

  • J. M. Pearson
    • 1
  • N. Chamel
    • 2
  • A. F. Fantina
    • 2
  • S. Goriely
    • 2
  1. 1.Dépt. de PhysiqueUniversité de MontréalMontréalCanada
  2. 2.Institut d’Astronomie et d’AstrophysiqueUniversité Libre de BruxellesBrusselsBelgium

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