Neutron stars with isovector scalar correlations

Abstract

Neutron stars with the isovector scalar $\delta$-field are studied in the framework of the relativistic mean field ($RMF$) approach in a pure nucleon plus lepton scheme. The $\delta$-field leads to a larger repulsion in dense neutron-rich matter and to a definite splitting of proton and neutron effective masses. Both features are influencing the stability conditions of the neutron stars. Two parametrizations for the effective nonlinear Lagrangian density are used to calculate the nuclear equation of state ($EOS$) and the neutron star properties, and compared to correlated Dirac-Brueckner results. We conclude that in order to reproduce reasonable nuclear structure and neutron star properties within a $RMF$ approach a density dependence of the coupling constants is required.

11 pages, 5 figures, revtex4 style

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• Low densities in asymmetric nuclear matter
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• Neutron star matter based on a parity doublet model including the $a_0(980)$ meson
• Isovector Channel Role of Relativistic Mean Field Models in the Neutrino Mean Free Path
• Dynamical instabilities of warm $np{e}^{-}$ matter: the $\delta$ meson effects
• Phase transitions of hadronic to quark matter at finite T and μ_B
• Application of density dependent parametrization models to asymmetric nuclear matter
• Effects of the Symmetry Energy and its Slope on Neutron Star Properties
• Effect of energy conservation on in-medium $\mbox{NN}\to \mbox{N}Δ$ cross section in isospin-asymmetric nuclear matter
• Moments of inertia of neutron stars in relativistic mean field theory: the role of the isovector scalar channel
• The effects of delta mesons on the baryonic direct Urca processes in neutron star matter
• The influence of $\delta$ meson on the isospin splitting of in-medium $NN\to N\Delta$ cross sections
• Vacuum fluctuation effects on asymmetric nuclear matter