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Astron. Astrophys. 348, 553-556 (1999)

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The photometric variability of the Be star NW Serpentis

J.R. Percy 1, M.M. Marinova 1, H. Boi 2 and P. Harmanec 3

1 Erindale Campus, and Department of Astronomy, University of Toronto, Mississauga ON L5L 1C6, Canada (jpercy@erin.utoronto.ca)
2 Hvar Observatory, Faculty of Geodesy, University of Zagreb, Ka ieva 26, 10000 Zagreb, Croatia (hbozic@geodet.geof.hr)
3 Astronomical Institute, Academy of Sciences, CZ-251 65 Ond ejov, Bohemia, Czech Republic (hec@sunstel.asu.cas.cz)

Received 6 October 1998 / Accepted 27 March 1999


NW Ser is a bright (V = 6.[FORMULA] 1-6.[FORMULA] 2), active Be star which is known to vary photometrically on a time scale of hours to days. Using both Hipparcos and ground-based photometry, and using light curve, autocorrelation, power spectrum analysis and phase dispersion minimalization techniques, we have concluded that the period is close to 0.[FORMULA] 46 - a period typical of stars of this type, and in good agreement with the value of 0.[FORMULA] 488, recently determined by Hubert & Floquet from Hipparcos data. It is possible that the period is near twice this value, but the evidence is not strong. We also find a period of about 5.[FORMULA] 5 from both the ground-based and Hipparcos data.

Key words: stars: early-type – stars: emission-line, Be – stars: variables: general

Send offprint requests to: J.R. Percy

© European Southern Observatory (ESO) 1999

Online publication: July 26, 1999