  We argue that, in general, observational studies of Be-star rotation have
paid insufficient attention to the effects of equatorial gravity darkening. We
present new line-profile calculations that emphasize the insensitivity of line
width to rotation for fast rotators. Coupled with a critical review of
observational procedures, these calculations suggest that the observational
parameter v sin(i) may systematically underestimate the true projected
equatorial rotation velocity, ve sin(i), by some tens of per cent for rapid
rotators. The crucial implication of this work is that Be stars may be rotating
much closer to their critical velocities than is generally supposed, bringing a
range of new processes into contention for the elusive physical mechanism
responsible for the circumstellar disk thought to be central to the Be
phenomenon.
