Energy Dependent Isospin Asymmetry in Mean-Field Dynamics

Abstract

The Lagrangian density of relativistic mean-field (RMF) theory with non-linear derivative (NLD) interactions is applied to isospin asymmetric nuclear matter. We study the symmetry energy and the density and energy dependences of nucleon selfenergies. At high baryon densities a soft symmetry energy is obtained. The energy dependence of the isovector selfenergy suppresses the Lane-type optical potential with increasing energy and predicts a $\rho$-meson induced mass splitting between protons and neutrons in isospin asymmetric matter.

21 pages, 8 figures, Nuclear Physics A in press

References in corpus (10)

• Nuclear symmetry energy probed by neutron skin thickness of nuclei
• Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
• Constraints on the symmetry energy and on neutron skins from the pygmy resonances in 68Ni and 132Sn
• Relativistic mean field interaction with density dependent meson-nucleon vertices based on microscopical calculations
• Neutron skin thickness in droplet model with surface width dependence: indications of softness of the nuclear symmetry energy
• Relativistic model for nuclear matter and atomic nuclei with momentum-dependent self-energies
• Isospin effects on sub-threshold kaon production at intermediate energies
• Dirac-Brueckner-Hartree-Fock calculations for isospin asymmetric nuclear matter based on improved approximation schemes
• Isospin dependence of relative yields of $K^{+}$ and $K^0$ mesons at 1.528 AGeV
• Non-Linear derivative interactions in relativistic hadrodynamics

Cited by in corpus (6)

• Equations of state for supernovae and compact stars
• Parametrisations of relativistic energy density functionals with tensor couplings
• Momentum dependent mean-field dynamics of compressed nuclear matter and neutron stars
• Toward relativistic mean-field description of $\bar{\text{N}}$-nucleus reactions
• Formation of double-$\Lambda$ hypernuclei at PANDA
• Neutron star equations of state with optical potential constraint