  In this work, we study the general characteristics of Be star light curves
from TESS sectors 1-26 in the light of a model we call the "impulsive magnetic
rotator". It is found that 73 percent of 441 classical Be stars are
short-period variables. The light curves are characterised by non-coherent
periods dominated by the fundamental and first harmonic with variable relative
amplitudes. By comparing the equatorial rotational velocities obtained from the
photometric fundamental periods with the projected rotational velocities,it is
shown that the fundamental period is indistinguishable from the rotation
period. The distributions of the projected rotational velocities and the
equatorial rotational velocities for Be and non-Be stars are discussed. Using
the equatorial rotational velocities of Be stars directly determined from the
photometric period, it is found that, on average, Be stars rotate at about 0.66
of critical velocity. This result is independent of assumptions concerning
gravity darkening. It is shown that the rotational amplitudes of Be stars
increase with effective temperature and are considerably higher than those of
non-Be stars. The amplitude distributions of Be and non-Be stars are also
significantly different. Of particular interest is a large rise in rotational
amplitudes from A0 to B5 for non-Be stars. We suspect that this may be a result
of the increasing importance of a line-driven wind. Perhaps the Be stars are
just those with greatest surface activity with increased mass loss aided by
rapid rotation.
