Poster abstract details

Be stars are non-supergiant B-type main sequence stars whose spectrum has or had at some time one or more Balmer lines in emission. They are fast rotators which may pulsate as $\beta$ Cephei and/or SPB stars. The amplitudes of the frequencies detected in Be stars vary in timescales of hundred of days or less.
Here we present the analysis of the COROT light curve of the Be star 102719279, which has been observed in the Initial Run and the First Long Run in the Anticenter direction. This allows us to perform a complete study of the changes in time of the frequencies and amplitudes. These results will be compared with other Be stars observed with MOST or COROT.