2015
DOI: 10.4236/oalib.1102011
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Density-Dependent Properties of Hadronic Matter in an Extended Chiral (σ, π, ω) Mean-Field Model

Abstract: Density-dependent relations among saturation properties of symmetric nuclear matter and hyperonic matter, the coupling ratios (strengths) of hyperon matter, and properties of hadronic stars are discussed by applying the conserving chiral nonlinear (σ, π, ω) hadronic mean-field theory. The chiral nonlinear (σ, π, ω) mean-field theory is an extension of the conserving nonlinear (nonchiral) σ-ω hadronic mean-field theory which is thermodynamically consistent, relativistic and is a Lorentz-covariant mean-field the… Show more

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Cited by 3 publications
(3 citation statements)
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“…The Fermi-liquid properties of nuclear matter at saturation; the maximum mass and radius of neutron stars. The linear , σ ω mean-field approximation (LHA) [1]) and the chiral Hartree approximation (CHA) [10]) are listed for comparison. The current scalar vertex corrections is denoted as Hedin-Dirac-Hartree-Fock (HDHF) approximation [34] [35].…”
Section: Numerical Results For Nuclear Matter and Neutron Starsmentioning
confidence: 99%
See 1 more Smart Citation
“…The Fermi-liquid properties of nuclear matter at saturation; the maximum mass and radius of neutron stars. The linear , σ ω mean-field approximation (LHA) [1]) and the chiral Hartree approximation (CHA) [10]) are listed for comparison. The current scalar vertex corrections is denoted as Hedin-Dirac-Hartree-Fock (HDHF) approximation [34] [35].…”
Section: Numerical Results For Nuclear Matter and Neutron Starsmentioning
confidence: 99%
“…i σ ω π =  ), are all equivalent to the Hartree (tadpole) approximation when nonlinear interactions are correctly renormalized as effective masses of nucleons and mesons, effective coupling constants, effective sources of equations of motions [1] [7] [8] [9] [10]. The renormalization of interactions is correctly defined and numerically checked by the requirement of thermodynamic consistency, conserving approximations, or the density functional theory (DFT) [17] [18] [19] [20] [21].…”
Section: Introductionmentioning
confidence: 99%
“…Relativistic hadronic models are also essential to examine nuclear fissions and cluster radioactivities in terms of conservation laws and self-consistency [40]- [42]. Astrophysical problems such as the formation of neutron stars require finite temperature and nonlinear hadronic approximations [15] [16] [33]; density and temperature inside stars will increase toward the center of a star, which is expected to produce pion condensations, hyperon generations and hadron-quark neutron stars [7] [8] [10] [31].…”
Section: Introductionmentioning
confidence: 99%