  We present predictions for neutron star tidal deformabilities obtained from a
Bayesian analysis of the nuclear equation of state, assuming a minimal model at
high-density that neglects the possibility of phase transitions. The Bayesian
posterior probability distribution is constructed from priors obtained from
microscopic many-body theory based on realistic two- and three-body nuclear
forces, while the likelihood functions incorporate empirical information about
the equation of state from nuclear experiments. The neutron star crust equation
of state is constructed from the liquid drop model, and the core-crust
transition density is found by comparing the energy per baryon in inhomogeneous
matter and uniform nuclear matter. From the cold $\beta$-equilibrated neutron
star equation of state, we then compute neutron star tidal deformabilities as
well as the mass-radius relationship. Finally, we investigate correlations
between the neutron star tidal deformability and properties of finite nuclei.
