  We study the impact of strong magnetic fields on the pasta phases that are
expected to exist in the inner crust of neutron stars. We employ the
relativistic mean field model to describe the nucleon interaction and use the
self-consistent Thomas-Fermi approximation to calculate the nonuniform matter
in neutron star crust. The properties of pasta phases and crust-core transition
are examined. It is found that as the magnetic field strength $B$ is less than
$10^{17}$ G, the effects of magnetic field are not evident comparing with the
results without magnetic field. As $B$ is stronger than $10^{18}$ G, the onset
densities of pasta phases and crust-core transition density decrease
significantly, and the density distributions of nucleons and electrons are also
changed obviously.
