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We address the crustal properties of neutron stars, such as crustal mass, crustal radius, crustal fraction of the moment of inertia and investigate the crustal and structural properties related to the glitching mechanism observed in pulsars. The mass, radius and crustal fraction of the moment of inertia in neutron stars have been determined using β -equilibrated neutron–proton–electron–muon (npe μ ) dense neutron star matter obtained using the extended Skyrme effective interactions with NRAPR and Brussels–Montreal parameter sets. The maximum mass of the neutron star calculated from these sets is able to reach ∼ 2 M ⊙ and higher, corroborating the recently observed masses of compact stars. The crustal fraction of the moment of inertia depends sensitively on the pressure and the corresponding density at the core–crust transition. The core–crust transition density and pressure together with the extracted minimum crustal fraction of the total moment of inertia provide a limit for the radii of pulsars. Present calculations imply that due to the crustal entrainment, the crustal fraction of the total moment of inertia is about 5.5 % . [ABSTRACT FROM AUTHOR]