  We calculate the hydrogen and helium ionization in B[e] envelopes and explore
their dependence on mass-loss and effective temperature. We also present
simulated observations of the Halpha emission line and the C IV 1550 doublet,
and study their behavior. This paper reports our first results in an ongoing
study of B[e] supergiants, and provides a glimpse on the ionization of the most
important elements in self-consistent numerical simulations.
  Our newly developed 2D stellar atmosphere code, ASTAROTH, was used for the
numerical simulations. The code self-consistently solves for the continuum
radiation, non-LTE level populations, and electron temperature in axi-symmetric
stellar envelopes. Observed profiles were calculated by an auxiliary program
developed separately from ASTAROTH.
  In all but one of our models, H remained fully ionized. Due to ionizations
from excited states it is much more difficult to get a H neutral disk than
indicated by previous analytical calculations. Near the poles, the ionization
is high in all models, while helium recombined in the equatorial regions for
all but our lowest mass-loss rate. Although the model parameters were not
adjusted to provide fits to any particular star, the theoretical profiles show
some features seen in the profiles of R126. These include the partially
resolved double peaked profile of Halpha, and the weak emission associated with
the UV C IV resonance line.
