Shell States of Neutron Rich Matter
arXiv:0805.2774 · doi:10.1103/PhysRevC.78.015801
Abstract
The equation of state (EOS) for nuclear and neutron rich matter is investigated in a Relativistic Mean Field (RMF) model. New shell states are found that minimize the free energy per baryon, calculated in a spherical Wigner-Seitz (WS) approximation, over a significant range of baryon densities. These shell states, that have both inside and outside surfaces, minimize the Coulomb energy of large proton number configurations at the expense of a larger surface energy. This is related to a possible depression in the central density of super heavy nuclei. As the baryon density increases, we find the system changes from normal nuclei, to shell states, and then to uniform matter.
11 pages 18 figures, minor changes, version accepted for Phys. Rev. C
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- Equation of State of Dense Matter from a density dependent relativistic mean field model
- Correlation of the neutron star crust-core properties with the slope of the symmetry energy and the lead skin thickness
- Core-crust transition and crustal fraction of moment of inertia in neutron stars
- Inner crust of neutron stars with mass-fitted Skyrme interaction