The photometric variability of the Be star NW Serpentis

NW Ser is a bright (V = 6.(m) 2), active Be star which is known to vary pho tometrically on a time scale of hours to days. Using both Hipparcos and gro und-based photometry, and using Light curve, autocorrelation, power spectru m analysis and phase dispersion minimalization techniques, we have conclude d that the period is close to 0.(d) 46 - a period typical of stars of this type, and in good agreement with the value of 0.(d) 488, recently determine d by Hubert & Floquet from Hipparcos data. It is possible that the period i s near twice this value, but the evidence is not strong. We also find a per iod of about 5.(d) 5 from both the ground-based and Hipparcos data.