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

The photometric variability of the Be star NW Serpentis

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

1</sup> 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

Abstract

NW Ser is a bright (V = 6. 1-6. 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. 46 - a period typical of stars of this type, and in good agreement with the value of 0. 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. 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

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Contents

• 1. Introduction
• 2. Analysis
• 3. Results
• 4. Possible variable comparison star
• 5. Discussion
• Acknowledgements
• References

© European Southern Observatory (ESO) 1999

Online publication: July 26, 1999
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