Gravitational waves emitted from the coalescence of neutron star binaries open a new
window to probe matter and fundamental physics in unexplored, extreme regimes. To extract …

Because of the development of many-body theories of nuclear matter, the long-standing,
open problem of the equation of state (EOS) of dense matter may be understood in the near …

One of the most common assumptions has been made that the pressure inside the star is
isotropic in nature. However, the pressure is locally anisotropic in nature which is a more …

Background: Very lately, the CREX group presents a skin value Δ R skin 48 (CREX)= 0.
121±0. 026 (exp)±0. 024 (model)= 0. 071∼ 0. 171 fm. Meanwhile, the PREX group reported …

The correlation between the charge radii differences in mirror nuclei pairs and the neutron
skin thickness has been studied with the so-called finite range simple effective interaction …

In this work we consider strange stars formed by quark matter in the color-flavor-locked
(CFL) phase of color superconductivity. The CFL phase is described by a Nambu-Jona …

In the present work, we investigate the effects of short-range correlations (SRC) on the
dimensionless deformability of the binary neutron system related to the GW170817 event …

The detailed knowledge of the inner crust properties of neutron stars might be important to
explain different phenomena such as pulsar glitches or the possibility of an r-process site in …

The effective Gogny interactions of the D1 family were established by D. Gogny more than
forty years ago with the aim to describe simultaneously the mean field and the pairing field …

Background: In our previous paper, we determined r skin 208 (exp)= 0. 278±0. 035 fm from
measured reaction cross sections σ R for p+ 208 Pb scattering, using the Kyushu (chiral) g …