One of the most intriguing questions about neutron stars concerns their maximum mass. The
answer is intimately related to the properties of matter at densities far beyond that found in …

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 …

The onset of hyperons in the core of neutron stars and the consequent softening of the
equation of state have been questioned for a long time. Controversial theoretical predictions …

Motivated by a recent report by Biwas and Bose (Phys Rev D 99: 104002, 2019) that the
observations of GW170817 to constrain the extent of pressure anisotropy in neutron stars …

The impact of anisotropic pressure models in neutron stars (NSs) is increasing their
compactness. Therefore, for the relatively soft NS equation of state (EOS), we can still obtain …

The precise measurements of the high masses of the pulsars PSR J 1614-2230 (M 1614=
1.97±0.04 M⊙) and PSR J 0348-0432 (M 0348= 2.01±0.04 M⊙) provide an important …

We analyze the stellar properties of the relativistic mean-field (RMF) parametrizations shown
to be consistent with the recently studied constraints related to nuclear matter, pure neutron …

Using several relativistic mean-field models (such as GM1, GM3, NL3, TM1, FSUGold, and
IU-FSU) as well as the quark-meson coupling model, we calculate the particle fractions, the …

Due to their compactness, neutron stars are the best study matter in high density and strong-
field gravity. Hartle and Thorne have proposed a good approximation or perturbation …

Context. The existence of 2 M⊙ pulsars puts very strong constraints on the equation of state
(EOS) of neutron stars (NSs) with hyperon cores, which can be satisfied only by special …