  We present solutions for Hall equilibria applicable to neutron star crusts.
Such magnetic configurations satisfy a Grad-Shafranov-type equation, which is
solved analytically and numerically. The solutions presented cover a variety of
configurations, from purely poloidal fields connected to an external dipole to
poloidal-toroidal fields connected to an external vacuum field, or fully
confined within the star. We find that a dipole external field should be
supported by a uniformly rotating electron fluid. The energy of the toroidal
magnetic field is generally found to be a few percent of the total magnetic
field energy for the fields with an external component. We discuss the
evolution due to Ohmic dissipation which leads to slowing down of the electron
fluid. We also find that the transition from an MHD equilibrium to a state
governed by Hall effect, generates spontaneously an additional toroidal field
in regions where the electron fraction changes.
