  We examine the equilibrium of a magnetized neutron-star-crust. We calculate
axially symmetric models in which an elastic force balances solenoidal motion
driven by a Lorentz force. A large variety of equilibrium models are allowed by
incorporating the elastic shear deformation; in addition,
toroidal-magnetic-field dominated models are available. These results
remarkably differ from those in barotropic fluid stars. We demonstrate some
models wherein the magnetic energy exceeds the elastic energy. The excess comes
from the fact that a large amount of magnetic energy is associated with the
irrotational part of the magnetic force, which is balanced with gravity and
pressure. It is sufficient for equilibrium models that the minor solenoidal
part is balanced by a weak elastic force. We find that the elasticity in the
crust plays an important role on the magnetic-field confinement. Further, we
present the spatial distribution of the shear-stress at the elastic limit, by
which the crust-fracture location can be identified. The result has useful
implications for realistic crust-quake models.
