Modified gravity theories on a nutshell: Inflation, bounce and late-time evolution

The authors review the present status of self-consistent mean-field (SCMF) models for describing nuclear structure and low-energy dynamics. These models are presented as effective energy-density functionals. The three most widely used variants of SCMF's based on a Skyrme energy functional, a Gogny force, and a relativistic mean-field Lagrangian are considered side by side. The crucial role of the treatment of pairing correlations is pointed out in each case. The authors discuss other related nuclear structure models and present several extensions beyond the mean-field model which are currently used. Phenomenological adjustment of the model parameters is discussed in detail. The performance quality of the SCMF model is demonstrated for a broad range of typical applications.

Self-consistent mean-field models for nuclear structure

A Skyrme parametrization from subnuclear to neutron star densities Part II. Nuclei far from stabilities

Neutron Stars 1: Equation of State and Structure

An equation of state (EOS) of neutron star matter, describing both the neutron star crust and the liquid core, is calculated. It is based on the eective nuclear interaction SLy of the Skyrme type, which is particularly suitable for the application to the calculation of the properties of very neutron rich matter (Chabanat et al. 1997, 1998). The structure of the crust, and its EOS, is calculated in the T = 0 approximation, and under the assumption of the ground state composition. The crust-core transition is a very weakly rst-order phase transition, with relative density jump of about one percent. The EOS of the liquid core is calculated assuming (minimal) npe composition. Parameters of static neutron stars are calculated and compared with existing observational data on neutron stars. The minimum and maximum masses of static neutron stars are 0:094 M and 2:05 M, respectively. Eects of rotation on the minimum and the maximum mass of neutron stars are briefly discussed.

/pdf/a-unified-equation-of-state-of-dense-matter-and-neutron-star-ermn2f76v0.pdf

A unified equation of state of dense matter and neutron star structure

A Skyrme parametrization from subnuclear to neutron star densities

New Skyrme-like effective interactions are proposed suitable for neutron stars, supernovae and neutron-rich nuclei. The parameters of the force are adjusted to the properties of the symmetric infinite nuclear matter, with an additional constraint on the low and high density neutron matter equation of state. Preliminary Hartree-Fock plus BCS calculations along series of isotopes are shown. They seem to solve the problem of large discrepancies observed with other parametrizations.

https://iopscience.iop.org/article/10.1088/0031-8949/1995/T56/034/pdf

R. Schaeffer

Papers

A Skyrme parametrization from subnuclear to neutron star densities Part II. Nuclei far from stabilities

A Skyrme parametrization from subnuclear to neutron star densities

New Skyrme effective forces for supernovae and neutron rich nuclei