  Within a microscopic approach the structure of Neutron Stars is usually
studied by modelling the homogeneous nuclear matter of the core by a suitable
Equation of State, based on a many-body theory, and the crust by a functional
based on a more phenomenological approach. We present the first calculation of
Neutron Star overall structure by adopting for the core an Equation of State
derived from the Brueckner-Hartree-Fock theory and for the crust, including the
pasta phase, an Energy Density Functional based on the same Equation of State,
and which is able to describe accurately the binding energy of nuclei
throughout the mass table. Comparison with other approaches is discussed. The
relevance of the crust Equation of state for the Neutron Star radius is
particularly emphasised.
