  To fully understand the Be star phenomenon, one must have a reasonable degree
of knowledge about the star beneath the disk, which is often found to be
rapidly rotating. Rapid rotation complicates modelling because fundamental
properties like the stellar luminosity and effective temperature require
knowledge of the angle of inclina- tion at which the star is observed.
Furthermore our knowledge of the structure of rapidly rotating stars is on a
less sure foundation than for non-rotating stars. The uncertainties in the
inclination and the surface properties of a few rapidly rotating stars have
been substantially reduced by interferometric observations over the last
decade, and these stars can be used as tests of rotating stellar models, even
if those stars themselves may not be Be stars. Vega, as an MK standard, is
historically a very important star because it is used for calibration purposes.
However, several studies have suggested that Vega is a rapidly rotating star
viewed at a very low inclination angle, raising questions as to how well we
really know its properties. Appropriate modelling has been challenging and
there is still room for debate over the actual properties of Vega, as opposed
to its observed properties. We have previously shown that under certain
conditions both the stellar surface properties and the deduced surface
properties scale from one model to another with the same surface shape. We used
this scaling algorithm with realistic 2D models to compute high-resolution
spectral energy distributions and interferometric visibilities to determine the
best rotating model fit to Vega. Detailed comparisons between the computed and
observed data will be presented.
