  The mass, radius and crustal fraction of moment of inertia in neutron stars
are calculated using $\beta$-equilibrated nuclear matter obtained from Skyrme
effective interaction. The transition density, pressure and proton fraction at
the inner edge separating the liquid core from the solid crust of the neutron
stars are determined from the thermodynamic stability conditions using the
KDE0v1 set. The neutron star masses obtained by solving the
Tolman-Oppenheimer-Volkoff equations using neutron star matter obtained from
this set is able to describe highly massive compact stars $\sim$2$M_{\odot}$.
The crustal fraction of the moment of inertia can be extracted from studying
pulsar glitches. This fraction is highly dependent on the core-crust transition
pressure and corresponding density. These results for pressure and density at
core-crust transition together with the observed minimum crustal fraction of
the total moment of inertia provide a limit for the radius of the Vela
pulsar:$R\geq$ 3.69+3.44 M/$M_{\odot}$. Present calculations suggest that the
crustal fraction of the total moment of inertia can be at most 3.6% due to
crustal entrainment caused by Bragg reflection of unbound neutrons by lattice
ions.
