  We present results of a fully non-local, compressible model of convection for
A-star envelopes. This model quite naturally reproduces a variety of results
from observations and numerical simulations which local models based on a
mixing length do not. Our principal results, which are for models with Teff
between 7200 K and 8500 K, are the following: First, the photospheric
velocities and filling factors are in qualitative agreement with those derived
from observations of line profiles of A-type stars. Second, the He II and H I
convection zones are separated in terms of convective flux and thermal
interaction, but joined in terms of the convective velocity field, in agreement
with numerical simulations. In addition, we attempt to quantify the amount of
overshooting in our models at the base of the He II convection zone.
