A review is given of various theoretical approaches for the equation of state (EoS) of dense
matter, relevant for the description of core-collapse supernovae, compact stars, and compact …

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 …

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 …

This paper presents a detailed assessment of the ability of the 240 Skyrme interaction
parameter sets in the literature to satisfy a series of criteria derived from macroscopic …

The speed of sound of the matter within neutron stars may contain nonsmooth structure
related to first-or higher-order phase transitions. Here we investigate what are the …

The general behavior of the nuclear equation of state (EOS), relevant for the description of
neutron stars (NSs), is studied within a Bayesian approach applied to a set of models based …

We derive a new equation of state (EoS) for neutron stars (NS) from the outer crust to the
core based on modern microscopic calculations using the Argonne v 18 potential plus three …

The transition density ρ t and pressure P t at the inner edge separating the liquid core from
the solid crust of neutron stars are systematically studied using a modified Gogny (MDI) and …

The standard variational derivation of stellar-matter structure in the Wigner-Seitz
approximation is generalized to the finite-temperature situation where a wide distribution of …

We perform a systematic analysis of the density dependence of nuclear symmetry energy
within the microscopic Brueckner-Hartree-Fock (BHF) approach using the realistic Argonne …