Based on more than 3000 high-resolution echelle spectra of 27 early-type Be stars, taken over six yeras, it is shown that the short-term periodic line profile variability of these objects is due to non-radial puslation.
Based on more than 3000 high-resolution echelle spectra of 27 early-type Be stars, taken over six yeras, it is shown that the short-term periodic line profile variability of these objects is due to non-radial puslation. (en)