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The cell structure of $\beta$-stable clusters in the inner crust of cold andwarm neutron stars is studied within the Thomas-Fermi approach usingrelativistic mean field nuclear models. The relative size of the inner crustand the pasta phase of neutron stars is calculated, and the effect of thesymmetry energy slope parameter, $L$, on the profile of the neutron star crustis discussed. It is shown that while the size of the total crust is mainlydetermined by the incompressibility modulus, the relative size of the innercrust depends on $L$. It is found that the inner crust represents a largerfraction of the total crust for smaller values of $L$. Finally, it is shownthat at finite temperature the pasta phase in $\beta$-equilibrium matteressentially melts above $5-6$ MeV, and that the onset density of the rodlikeand slablike structures does not depend on the temperature.

Equation of state and thickness of the inner crust of neutron stars