Neutron Star Radii, Deformabilities, and Moments of Inertia from Experimental and Ab Initio Theory Constraints of the ²⁰⁸Pb Neutron Skin Thickness

Recent experimental and ab initio theory investigations of the (Formula presented.) Pb neutron skin thickness have the potential to inform the neutron star equation of state. In particular, the strong correlation between the (Formula presented.) Pb neutron skin thickness and the pressure of neutron matter at normal nuclear densities leads to modified predictions for the radii, tidal deformabilities, and moments of inertia of typical (Formula presented.) neutron stars. In the present work, we study the relative impact of these recent analyses of the (Formula presented.) Pb neutron skin thickness on bulk properties of neutron stars within a Bayesian statistical analysis. Two models for the equation of state prior are employed in order to highlight the role of the highly uncertain high-density equation of state. From our combined Bayesian analysis of nuclear theory, nuclear experiment, and observational constraints on the dense matter equation of state, we find at the 90% credibility level (Formula presented.) km for the radius of a (Formula presented.) neutron star, (Formula presented.) km for the radius of a (Formula presented.) neutron star, (Formula presented.) for the tidal deformability of a (Formula presented.) neutron star, and (Formula presented.) for the moment of inertia of PSR J0737-3039A whose mass is (Formula presented.).