  The crustal fraction of moment of inertia in neutron stars is calculated
using $\beta$-equilibrated nuclear matter obtained from density dependent M3Y
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 determined from the thermodynamic stability conditions are found to be
$\rho_t=$ 0.0938 fm$^{-3}$, P$_t=$ 0.5006 MeV fm$^{-3}$ and $x_{p(t)}=$ 0.0308,
respectively. The crustal fraction of the moment of inertia can be extracted
from studying pulsar glitches and is most sensitive to the pressure as well as
density at the transition from the crust to the core. 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 new limit for
the radius of the Vela pulsar: $R \geq 4.10 + 3.36 M/M_\odot$ kms.
