Jorge Piekarewicz

TL;DR: An accurate measurement of the neutron radius in 208Pb-via parity violating electron scattering-may have important implications for the structure of the crust of neutron stars.

TL;DR: An accurately calibrated relativistic parametrization is introduced to compute the ground state properties of finite nuclei, their linear response, and the structure of neutron stars, and it produces an equation of state that is considerably softer--both for symmetric nuclear matter and for the symmetry energy.

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