  We address the issues of crustal properties of neutron stars such as crustal
mass, crustal radius, crustal fraction of 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 moment of inertia in
neutron stars have been determined using $\beta$-equilibrated (npe$\mu$) dense
neutron star matter obtained using the extended Skyrme effective interactions
with NRAPR and Brussels-Montreal parameter sets. The maximum mass of neutron
star calculated from these sets is able to reach $\sim$2$M_\odot$ and higher,
corroborating the recently observed masses of compact stars. The crustal
fraction of the moment of inertia depends sensitively on the pressure and
corresponding density at 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 crustal entrainment the crustal fraction of the
total moment of inertia is about 5.5$\%$.

Nuclear Theory;High Energy Astrophysical Phenomena