Neutron-skin thickness of finite nuclei in relativistic mean-field models with chiral limits

Abstract

We study several structure properties of finite nuclei using relativistic mean-field Lagrangians constructed according to the Brown-Rho scaling due to the chiral symmetry restoration at high densities. The models are consistent with current experimental constraints for the equations of state of symmetric matter at both normal and supra-normal densities and of asymmetric matter at sub-saturation densities. It is shown that these models can successfully describe the binding energies and charge radii of finite nuclei. Compared to calculations with usual relativistic mean-field models, these models give a reduced thickness of neutron skin in ^{208}Pb between 0.17 fm and 0.21 fm. The reduction of the predicted neutron skin thickness is found to be due to not only the softening of the symmetry energy but also the scaling property of $\rho$ meson required by the partial restoration of chiral symmetry.

Accepted version to appear in PRC (2007)

References in corpus (8)

• Neutron-Rich Nuclei in Heaven and Earth
• Relativistic model for nuclear matter and atomic nuclei with momentum-dependent self-energies
• Neutron density distributions from antiprotonic 208Pb and 209Bi atoms
• The long journey from the giant-monopole resonance to the nuclear-matter incompressibility
• Probing the Nuclear Symmetry Energy with Heavy-Ion Reactions Induced by Neutron-Rich Nuclei
• Late Hadronization and Matter Formed at RHIC: Vector Manifestation, Brown-Rho Scaling and Hadronic Freedom
• Equation of state of isospin-asymmetric nuclear matter in relativistic mean-field models with chiral limits
• Charge density of light exotic nuclei and $\rho NN$ tensor coupling

Cited by in corpus (5)

• Isospin-dependent properties of asymmetric nuclear matter in relativistic mean-field models
• Influence of the single-particle structure on the nuclear surface and the neutron skin
• Liquid-gas phase transition in hot asymmetric nuclear matter with density-dependent relativistic mean-field models
• Neutron star deformability with hyperonization in density-dependent relativistic mean-field models
• Chiral condensate in nuclear matter with vacuum corrections