  We investigate the ionization structure in the non-spherical winds and disks
of B[e] stars. Especially the luminous B[e] supergiants seem to have outflowing
disks which are neutral in hydrogen already close to the stellar surface. The
existence of neutral material so close to the central star is surprising and
needs to be investigated in detail. We perform our model calculations mainly in
the equatorial plane, trying to find a plausible scenario that leads to
recombination in the vicinity of the hot stars. Two different approaches are
presented that both result in a hydrogen neutral equatorial region. We
especially focus on the influence of stellar rotation which is known to play a
significant role in shaping non-spherical winds. We show that a rotating star
can have a neutral equatorial wind, even without the need of a density
enhancement due to bi-stability or wind compression, but simply due to
graviational darkening in combination with the known high mass-loss rates of
the B[e] stars and especially the B[e] supergiants.
