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In this work we study properties of neutron star crusts, where matter isexpected to consist of nuclei surrounded by superfluid neutrons and ahomogeneous background of relativistic electrons. The nuclei are disposed in aCoulomb lattice, and it is believed that the structure of the latticeinfluences considerably the specific heat of the neutronic matter inside thecrust of a neutron star. Using a modern meson--exchange potential in theframework of a local--density approximation we calculate the neutronic specificheat accounting for various shapes of the Coulomb lattice, from spherical tonon--spherical nuclear shapes. We find that a realistic nucleon--nucleonpotential leads to a significant increase in the neutronic specific heat withrespect to that obtained assuming a uniform neutron distribution. The increaseis largest for the non--spherical phase of the crust. These results may haveconsequences for the thermal history of young neutron stars.Comment: Revtex, 5 pages, 4 figures included as uuencoded p

Superfluidity and neutron star crust matter