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We compare two approaches to describe the inner crust of neutron stars: onthe one hand, the simple coexistence of a liquid (clusters) and a gas phase,and on the other hand, the energy minimization with respect to the densityprofile, including Coulomb and surface effects. We find that thephase-coexistence model gives a reasonable description of the densities in theclusters and in the gas, but the precision is not high enough to obtain thecorrect proton fraction at low baryon densities. We also discuss the surfacetension and neutron skin obtained within the energy minimization.

Liquid-gas coexistence vs. energy minimization with respect to the density profile in the inhomogeneous inner crust of neutron stars