Relativistic mean-field study of neutron-rich nuclei

Abstract

A relativistic mean-field model is used to study the ground-state properties of neutron-rich nuclei. Nonlinear isoscalar-isovector terms, unconstrained by present day phenomenology, are added to the model Lagrangian in order to modify the poorly known density dependence of the symmetry energy. These new terms soften the symmetry energy and reshape the theoretical neutron drip line without compromising the agreement with existing ground-state information. A strong correlation between the neutron radius of 208Pb and the binding energy of valence orbitals is found: the smaller the neutron radius of 208Pb, the weaker the binding energy of the last occupied neutron orbital. Thus, models with the softest symmetry energy are the first ones to drip neutrons. Further, in anticipation of the upcoming one-percent measurement of the neutron radius of 208Pb at the Thomas Jefferson Laboratory, a close relationship between the neutron radius of 208Pb and neutron radii of elements of relevance to atomic parity-violating experiments is established.

14 pages, 5 figures

References in corpus (8)

• Magic numbers in exotic nuclei and spin-isospin properties of {\it NN} interaction
• Neutron Radii in Mean-Field Models
• The neutron radii of Lead and neutron stars
• Constraining URCA cooling of neutron stars from the neutron radius of 208Pb
• New Constraints on Neutron Star Cooling from Chandra Observations of 3C58
• Discerning the neutron density distribution of 208Pb from nucleon elastic scattering
• The long journey from the giant-monopole resonance to the nuclear-matter incompressibility
• Self-consistent description of nuclear compressional modes

Cited by in corpus (49)

• Isospin Asymmetry in Nuclei and Neutron Stars
• Building relativistic mean field models for finite nuclei and neutron stars
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• Searching for isovector signatures in the neutron-rich oxygen and calcium isotopes
• Pygmy dipole resonance as a constraint on the neutron skin of heavy nuclei
• Incompressibility of neutron-rich matter
• Pygmy Resonances and Neutron Skins
• Constraining the High-Density Behavior of Nuclear Symmetry Energy with the Tidal Polarizability of Neutron Stars
• Pulsar Glitches: The Crust may be Enough
• Unmasking the nuclear matter equation of state
• Do we understand the incompressibility of neutron-rich matter?
• Impact of the symmetry energy on the outer crust of non-accreting neutron stars
• Low densities in nuclear and neutron matters and in the nuclear surface
• Properties of the nuclear medium
• Origin of the neutron skin thickness of 208Pb in nuclear mean-field models
• Sensitivity of the Moment of Inertia of Neutron Stars to the Equation of State of Neutron-Rich Matter
• Why is Tin so soft?
• Atomic Parity Non-Conservation, Neutron Radii, and Effective Field Theories of Nuclei
• Nuclear matter symmetry energy and the symmetry energy coefficient in the mass formula
• Validating relativistic models of nuclear structure against theoretical, experimental, and observational constraints
• Relativistic models of the neutron-star matter equation of state
• Symmetry Energy Constraints from Giant Resonances: A Theoretical Overview
• New analysis method of the halo phenomenon in finite many-fermion systems. First applications to medium-mass atomic nuclei
• Insensitivity of the elastic proton-nucleus reaction to the neutron radius of 208Pb
• Charge density of light exotic nuclei and $\rho NN$ tensor coupling
• Relativistic mean field plus exact pairing approach to open shell nuclei
• Effects of a weakly interacting light U boson on the nuclear equation of state and properties of neutron stars in relativistic models
• Pasta properties of the neutron star within effective relativistic mean-field model
• Low density nuclear matter with light clusters in a generalized nonlinear relativistic mean-field model
• Role of the symmetry energy on the neutron-drip transition in accreting and nonaccreting neutron stars
• Influence of the symmetry energy on the giant monopole resonance of neutron-rich nuclei
• Effects of the density dependence of nuclear symmetry energy on properties of superheavy nuclei
• A Bayesian mixture model approach to quantifying the empirical nuclear saturation point
• On three topical aspects of the N=28 isotonic chain
• The Dirac oscillator: an alternative basis for nuclear structure calculations
• Roles of isoscalar hyperons in probing the density dependence of the nuclear symmetry energy
• Giant monopole energies from a constrained relativistic mean-field approach
• Nuclear breathing mode in neutron-rich Nickel isotopes: sensitivity to the symmetry energy and the role of the continuum
• The Auxiliary Field Diffusion Monte Carlo Method for Nuclear Physics and Nuclear Astrophysics
• Emergence of low-energy monopole strength in the neutron-rich calcium isotopes
• The Quest for the Heaviest Uranium Isotope
• Application of relativistic mean field and effective field theory density to calculate scattering observables for Ca isotopes
• Calculation of a complete set of spin observables for proton elastic scattering from stable and unstable nuclei
• Validity of the relativistic impulse approximation for elastic proton-nucleus scattering at energies lower than 200 MeV
• Energy-dependent Lorentz covariant parameterization of the NN interaction between 50 and 200 MeV
• Isovector Giant Dipole Resonance of Stable Nuclei in a Consistent Relativistic Random Phase Approximation
• Parity Violation, the Neutron Radius of Lead, and Neutron Stars
• Sensitivity of deexcitation energies of superdeformed secondary minima to the density dependence of symmetry energy with the relativistic mean-field theory
• Associated hyperon-kaon production via neutrino-nucleus scattering