Density-Dependent Properties of Hadronic Matter in the self-consistent Chiral (σ, π, ω) Mean-Field Model

Density-dependent relations among saturation properties of symmetric nuclear matter and properties of hadronic stars are discussed by applying the conserving chiral nonlinear (sigma, pi, omega) hadronic mean-field theory. The chiral nonlinear (sigma, pi, omega) mean-field theory is an extension of the conserving nonlinear (nonchiral) sigma-omega hadronic mean-field theory which is thermodynamically consistent, relativistic and is a Lorentz-covariant mean-field theory of hadrons. In the extended chiral (sigma, pi, omega) mean-field model, all the masses of hadrons are produced by the breaking of chiral symmetry, which is different from other conventional chiral partner models. By comparing both nonchiral and chiral mean-field approximations, the effects of the chiral symmetry breaking mechanism on the mass of sigma-meson, coefficients of nonlinear interactions and Fermi-liquid properties are investigated in nuclear matter and neutron stars.