Plamen G. Krastev, Francesca Sammarruca
Published 2006-01-22, updated 2006-07-24Version 3
We calculate total masses and radii of neutron stars (NS) for pure neutron matter and nuclear matter in beta-equilibrium. We apply a relativistic nuclear matter equation of state (EOS) derived from Dirac-Brueckner-Hartree-Fock (DBHF) calculations. We use realistic nucleon-nucleon (NN) interactions defined in the framework of the meson exchange potential models. Our results are compared with other theoretical predictions and recent observational data. Suggestions for further study are discussed.
Comments: 13 pages, 9 figures, 1 table; Revised version, accepted for publication in Physical Review C
Journal: Phys.Rev. C74 (2006) 025808
A microscopic equation of state for neutron-rich matter and its effect on neutron star properties
In medium T matrix for neutron matter
Hadron Masses in Medium and Neutron Star Properties
