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Recent experimental and ab initio theory investigations of the 208Pb neutronskin thickness are sufficiently precise to inform the neutron star equation ofstate. In particular, the strong correlation between the 208Pb neutron skinthickness and the pressure of neutron matter at normal nuclear densities leadsto modified predictions for the radii, tidal deformabilities, and moments ofinertia of typical 1.4 solar-mass neutron stars. In the present work, we studythe relative impact of these recent analyses of the 208Pb neutron skinthickness on bulk properties of neutron stars within a Bayesian statisticalanalysis. Two models for the equation of state prior are employed in order tostudy the role of the highly uncertain high-density equation of state. From ourcombined Bayesian analysis of nuclear theory, nuclear experiment, andobservational constraints on the dense matter equation of state, we find at the90% credibility level $R_{1.4}=12.36^{+0.38}_{-0.73}$ km for the radius of a1.4 solar-mass neutron star, $R_{2.0}=11.96^{+0.94}_{-0.71}$ km for the radiusof a 2.0 solar-mass neutron star, $\Lambda_{1.4}=440^{+103}_{-144}$ for thetidal deformability of a 1.4 solar-mass neutron star, and$I_{1.338}=1.425^{+0.074}_{-0.146}\, \times 10^{45}\,\rm{g\,cm}^{2}$ for themoment of inertia of PSR J0737-3039A whose mass is 1.338 solar masses.

Neutron star radii, deformabilities, and moments of inertia from experimental and ab initio theory constraints on the 208Pb neutron skin thickness