Farrukh J. Fattoyev

TL;DR: Ab et al. as mentioned in this paper used a set of realistic models of the equation of state (EOS) that yield an accurate description of the properties of finite nuclei, support neutron stars of two solar masses, and provide a Lorentz covariant extrapolation to dense matter are used to confront its predictions against gravitational-wave data.

TL;DR: In this paper, the authors exploit the strong correlation between the thickness of the skin and the slope of the symmetry energy within a specific class of relativistic energy density functionals, and report a value of L=(106±37)

TL;DR: In this article, a relativistic effective interaction that is simultaneously constrained by the properties of finite nuclei, their collective excitations, and neutron-star properties is introduced, and the new effective interaction is fitted to a neutron skin thickness in $^{208}mathrm{Pb} of only ${R}n}ensuremath{-}{R}_{p}=0.16$ fm and yields a moderately large maximum neutron star mass of 1.94

TL;DR: In this paper, Covariant density functional theory was used to investigate the properties of finite nuclei and neutron stars, while enforcing causality at all densities, and it was shown that the stiffening of the equation of state required to support supermassive neutron stars is inconsistent with either constraints obtained from energetic heavy-ion collisions or from the low deformability of medium-mass stars.

TL;DR: In this article, the authors explore the possibility that uncertainties in the equation of state provide enough flexibility for the construction of models that predict a large crustal thickness and consequently a large moment of inertia.