Equation of state of isospin-asymmetric nuclear matter in relativistic mean-field models with chiral limits

Abstract

Using in-medium hadron properties according to the Brown-Rho scaling due to the chiral symmetry restoration at high densities and considering naturalness of the coupling constants, we have newly constructed several relativistic mean-field Lagrangians with chiral limits. The model parameters are adjusted such that the symmetric part of the resulting equation of state at supra-normal densities is consistent with that required by the collective flow data from high energy heavy-ion reactions, while the resulting density dependence of the symmetry energy at sub-saturation densities agrees with that extracted from the recent isospin diffusion data from intermediate energy heavy-ion reactions. The resulting equations of state have the special feature of being soft at intermediate densities but stiff at high densities naturally. With these constrained equations of state, it is found that the radius of a 1.4$M_{\odot }$ canonical neutron star is in the range of 11.9 km$\le$R$\le$13.1 km, and the maximum neutron star mass is around 2.0$M_{\odot }$ close to the recent observations.

14 pages, 3 figures

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Cited by in corpus (7)

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• Neutron-skin thickness of finite nuclei in relativistic mean-field models with chiral limits
• Liquid-gas phase transition in hot asymmetric nuclear matter with density-dependent relativistic mean-field models
• Hyperonic uncertainties in neutron stars, mergers and supernovae
• Mean free paths and in-medium scattering cross sections of energetic nucleons in neutron-rich nucleonic matter within the relativistic impulse approximation
• Neutron star deformability with hyperonization in density-dependent relativistic mean-field models
• Chiral condensate in nuclear matter with vacuum corrections