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 …

It is of great interest to understand the equation of state (EOS) of the neutron star, whose
core includes highly dense matter. However, there are large uncertainties in the theoretical …

In the framework of the Thomas-Fermi approximation, we systematically study the EOSs and
microscopic structures of neutron star matter in a vast density range with nb≈ 10− 10-2 fm …

In this work, we perform a Bayesian inference of the crust–core transition density ρ t of
neutron stars based on the neutron-star radius and neutron-skin thickness data using a …

Complex and exotic nuclear geometries, collectively referred to as “nuclear pasta,” are
expected to appear naturally in dense nuclear matter found in the crusts of neutron stars and …

We explore the possibility of a structured hadron-quark mixed phase forming in the interior of
neutron stars. The quark-meson coupling (QMC) model, which explicitly incorporates the …

We consider the elastic constants of phases with nonspherical nuclei, so-called pasta
phases, predicted to occur in the inner crust of a neutron star. First, we treat perfectly ordered …

We study the effects of nuclear symmetry energy on the mass-radius relation and tidal
deformability of neutron stars, considering the self-consistency of the equation of state …

We study the hadron-quark mixed phase, which may occur in the interior of neutron stars.
The relativistic mean-field model is employed to describe the hadronic phase, while the …

We present the first Bayesian inference of neutron star crust properties to incorporate
neutron skin data, including the recent PREX measurement of the neutron skin of 208 Pb …