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We investigate neutron star moments of inertia from Bayesian posteriorprobability distributions of the nuclear equation of state that incorporateinformation from microscopic many-body theory and empirical data of finitenuclei. We focus on PSR J0737-3039A and predict that for this 1.338 M_sunneutron star the moment of inertia lies in the range $1.04 \times 10^{45}$ gcm$^{2} < I < 1.51 \times 10^{45}$ g cm$^{2}$ at the 95% credibility level,while the most probable value for the moment of inertia is $\tilde I = 1.36\times 10^{45}$ g cm$^{2}$. Assuming a measurement of the PSR J0737-3039Amoment of inertia to 10% precision, we study the implications for neutron starradii and tidal deformabilities. We also determine the crustal component of themoment of inertia and find that for typical neutron star masses of 1.3 M_sun <M < 1.5 M_sun the crust contributes 1% - 6% of the total moment of inertia,below what is needed to explain large pulsar glitches in the scenario of strongneutron entrainment.

Predicting the moment of inertia of pulsar J0737-3039A from Bayesian modeling of the nuclear equation of state