Masses of neutron stars and nuclei

Abstract

We calculate the maximum mass of neutron stars for three different equations of state (EOS) based on generalized Skyrme functionals that are simultaneously fitted to essentially all the 2003 nuclear mass data (the rms deviation is 0.58 MeV in all three cases) and to one or other of three different equations of state of pure neutron matter, each determined by a different many-body calculation using realistic two- and three-body interactions but leading to significantly different degrees of stiffness at the high densities prevailing in neutron-star interiors. The observation of a neutron star with mass 1.97 $\pm$ 0.04 ${\mathcal{M}}_{\odot }$ eliminates the softest of our models (BSk19), but does not discriminate between BSk20 and BSk21. However, nuclear-mass measurements that have been made since our models were constructed strongly favor BSk21, our stiffest functional.

11 pages, 4 figures; Physical Review C in press

References in corpus (8)

• Shapiro delay measurement of a two solar mass neutron star
• Further explorations of Skyrme-Hartree-Fock-Bogoliubov mass formulas. XII: Stiffness and stability of neutron-star matter
• R-Process Nucleosynthesis in Dynamically Ejected Matter of Neutron Star Mergers
• The Skyrme Interaction in finite nuclei and nuclear matter
• Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
• 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
• Unified description of neutron superfluidity in the neutron-star crust with analogy to anisotropic multi-band BCS superconductors

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