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 …

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 …

A new table of the nuclear equation of state (EOS) based on realistic nuclear potentials is
constructed for core-collapse supernova numerical simulations. Adopting the EOS of uniform …

Neutron stars provide a cosmic laboratory to study the nature of dark matter particles and
their interactions. Dark matter can be captured by neutron stars via scattering, where kinetic …

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 …

In this review we discuss self-consistent methods to calculate the global structure of strongly
magnetised neutron stars within the general-relativistic framework. We outline why solutions …

The possibility to draw links between the isospin properties of nuclei and the structure of
compact stars is a stimulating perspective. In order to pursue this objective on a sound basis …

We construct a new equation of state (EOS) for numerical simulations of core-collapse
supernovae and neutron-star mergers based on an extended relativistic mean-field model …

The equation of state (EoS) of hot and dense matter is a fundamental input to describe static
and dynamical properties of neutron stars, core-collapse supernovae and binary compact …

The cell structure of β-stable clusters in the inner crust of cold and warm neutron stars is
studied within the Thomas–Fermi approach by using relativistic mean-field nuclear models …