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 …

Context. An equation of state (EoS) of dense nuclear matter is a prerequisite for studies of
the structure and evolution of compact stars. A unified EoS should describe the crust and the …

We calculate static properties of non-rotating neutron stars (NS's) using a microscopic
equation of state (EOS) for asymmetric nuclear matter, derived from the Brueckner-Bethe …

Analytical representations are derived for two equations of state (EOSs) of neutron-star
matter: FPS and SLy. Each of these EOSs is unified, that is, it describes the crust and the …

Context. Few unified equations of state for neutron star matter, in which core and crust are
described using the same nuclear model, are available. However the use of non-unified …

The cooling phase of thermonuclear (type-I) X-ray bursts can be used to constrain neutron
star (NS) compactness by comparing the observed cooling tracks of bursts to accurate …

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 …

Aims. In this paper, we study the global properties of neutron stars (NSs), as predicted by the
Brussels-Montreal equations of state (EoSs). These EoSs, which provide a unified …

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 …

Neutron stars, produced at the death of massive stars, are often regarded as giant neutron-
rich nuclei. This picture is especially relevant for low-mass (below about solar mass,) …