  The cell structure of $\beta$-stable clusters in the inner crust of cold and
warm neutron stars is studied within the Thomas-Fermi approach using
relativistic mean field nuclear models. The relative size of the inner crust
and the pasta phase of neutron stars is calculated, and the effect of the
symmetry energy slope parameter, $L$, on the profile of the neutron star crust
is discussed. It is shown that while the size of the total crust is mainly
determined by the incompressibility modulus, the relative size of the inner
crust depends on $L$. It is found that the inner crust represents a larger
fraction of the total crust for smaller values of $L$. Finally, it is shown
that at finite temperature the pasta phase in $\beta$-equilibrium matter
essentially melts above $5-6$ MeV, and that the onset density of the rodlike
and slablike structures does not depend on the temperature.
