Relativistic Hartree-Fock calculations of charged-current neutrino opacities reveal large discrepancies and a substantial shift in medium-dependent modifications compared to standard relativistic mean-field models.
Nuclear Matter in Relativistic Mean Field Theory with Isovector Scalar Meson
2 Pith papers cite this work. Polarity classification is still indexing.
2
Pith papers citing it
abstract
Relativistic mean field (RMF) theory of nuclear matter with the isovector scalar mean field corresponding to the delta-meson [a_0(980)] is studied. While the delta-meson mean field vanishes in symmetric nuclear matter, it can influence properties of asymmetric nuclear matter in neutron stars. The RMF contribution due to delta-field to the nuclear symmetry energy is negative. To fit the empirical value, E_s=30 MeV, a stronger rho-meson coupling is required than in the absence of the delta-field. The energy per particle of neutron matter is then larger at high densities than the one with no delta-field included. Also, the proton fraction of beta-stable matter increases. Splitting of proton and neutron effective masses due to the delta-field can affect transport properties of neutron star matter.
years
2026 2verdicts
UNVERDICTED 2representative citing papers
An extended linear sigma model with delta meson and negative sigma_piN produces a symmetry-energy plateau and stiffer EOS that satisfies neutron-star and nuclear constraints.
citing papers explorer
-
Charged-current neutrino opacity within the relativistic Hartree-Fock framework for astrophysical simulations of core-collapse supernovae and binary neutron star mergers
Relativistic Hartree-Fock calculations of charged-current neutrino opacities reveal large discrepancies and a substantial shift in medium-dependent modifications compared to standard relativistic mean-field models.
-
Nuclear matter properties and neutron star structures from an extended linear sigma model
An extended linear sigma model with delta meson and negative sigma_piN produces a symmetry-energy plateau and stiffer EOS that satisfies neutron-star and nuclear constraints.