  Using the relativistic mean-field theory, we adopt two different methods,
namely, the coexisting phase method and the self-consistent Thomas-Fermi
approximation, to study the impacts of the nuclear symmetry energy on
properties of neutron star crusts within a wide range of densities. It is found
that the nuclear symmetry energy and its density slope play an important role
in determining the pasta phases and the crust-core transition.
