¹ European Southern Observatory, Karl-Schwarzschild-Str. 2, D-8574 Garching bei München, Germany
² Astronomical Institute, Academy of Sciences, CZ-25165 Ondrejov, Czech Republic
³ Landessternwarte Königstuhl, D-69117 Heidelberg, Germany

Recently, the line profile variability (lpv) of two low v sin i Be stars  Cen and  (28) CMa was successfully modelled as nonradial pulsation (nrp) of rapidly rotating stars seen pole-on. In this work, it is shown that the lpv of low v sin i early-type Be stars in general closely resembles these two cases, and is therefore explainable by the same mechanism. The lpv of intermediate to high v sin i Be stars can be explained by the very same model if only the inclination angle of the model is increased. Consequently, early-type Be stars form a distinct, fairly homogeneous class of non-radial low-order g-mode pulsators.

to be published in ASP Conf. Ser.: IAU Coll. 185: Radial and Nonradial Pulsations as Probes of Stellar Physics, Editors: Conny Aerts, Tim Bedding, Joergen Christensen-Dalsgaard

Preprints from triviniu@eso.org
or on the web at http://www.eso.org/~triviniu/Leuven.html