Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared
goal of both nuclear physics and astrophysics. Except possible phase transitions, the density …

Various kinds of isovector nucleon effective masses are used in the literature to characterize
the momentum/energy dependence of the nucleon symmetry potential or self-energy due to …

The uncertainties in neutron star radii and crust properties due to our limited knowledge of
the equation of state are quantitatively analyzed. We first demonstrate the importance of a …

The theory of the nuclear energy-density functional is used to provide a unified and
thermodynamically consistent treatment of all regions of cold non-accreting neutron stars. In …

Within the parameter space of the equation of state (EOS) of dense neutron-rich matter
limited by existing constraints mainly from terrestrial nuclear experiments, we investigate …

Extending our earlier work, a new family of three Hartree-Fock-Bogoliubov (HFB) mass
models, labeled HFB-30, HFB-31, and HFB-32, is presented, along with their underlying …

A clear connection can be established between properties of nuclear matter and finite-nuclei
observables, such as the correlation between the slope of the symmetry energy and the …

The Equation of State (EOS) of uniform neutron-rich nucleonic matter of isospin asymmetry
δ=(ρ n—ρ p)/ρ and density ρ can be expressed in terms of the energy per nucleon E (ρ, δ) …

We examine critically how tightly the density dependence of nuclear symmetry energy E_
sym (ρ)\, E sym (ρ) is constrained by the universal equation of state of the unitary Fermi gas …

Beginning from the proposal of a physically acceptable model to represent the interior of
compact stars, in which their interior is formed by a strange matter distribution described by a …