Symmetry Energy in Nuclear Surface

Abstract

Interplay between the dependence of symmetry energy on density and the variation of nucleonic densities across nuclear surface is discussed. That interplay gives rise to the mass dependence of the symmetry coefficient in an energy formula. Charge symmetry of the nuclear interactions allows to introduce isoscalar and isovector densities that are approximately independent of the magnitude of neutron-proton asymmetry.

8 pages, 4 figures, contribution to 15th Nuclear Physics Workshop "Marie & Pierre Curie", Kazimierz, Poland, 2008; minor corrections

References in corpus (2)

• Neutron Star Observations: Prognosis for Equation of State Constraints
• Surface Symmetry Energy

Cited by in corpus (22)

• The Nuclear Equation of State and Neutron Star Masses
• Constraining the Symmetry Parameters of the Nuclear Interaction
• Analytical representations of unified equations of state for neutron-star matter
• Isospin dependent multifragmentation of relativistic projectiles
• Linear response of homogeneous nuclear matter with energy density functionals
• Equation of state for neutron stars with hyperons and quarks in relativistic Hartree-Fock approximation
• Symmetry and Surface Symmetry Energies in Finite Nuclei
• Temperature dependence of the symmetry energy and neutron skins in Ni, Sn, and Pb isotopic chains
• Volume and surface contributions to the nuclear symmetry energy within the coherent density fluctuation model
• Nuclear asymmetry energy and isovector stiffness within the effective surface approximation
• Temperature dependence of the volume and surface contributions to the nuclear symmetry energy within the coherent density fluctuation model
• The symmetry energy in nuclear reactions
• Linear Response Theory with finite-range interactions
• Application of the coherent density fluctuation model to study the nuclear matter properties of finite nuclei within the relativistic mean-field formalism
• Systematic study of surface properties for Ne, Na, Mg, Al and Si isotopes in a coherent density fluctuation model using the relativistic mean field formalism
• Slope-dependent nuclear-symmetry energy within the effective surface approximation
• Symmetry energy and neutron-proton radii studies with a Wigner-Heisenberg monopole-monopole interaction
• Semiclassical approaches to nuclear dynamics
• Neutron stars as a dense liquid drop at equilibrium within the effective surface approximation
• Leptodermic corrections to the TOV equations and nuclear astrophysics within the effective surface approximation
• Macroscopic approaches to rotating neutron stars
• Nuclear constraints on the EoS and rotating neutron stars