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Rapid spectroscopic and photometric variability in the Be star Alpha Eridani

  • N.V. Leister (a1), E. Janot-Pacheco (a1), M.T.C. Buck (a1), M.P. Dias (a1), A.M. Hubert (a2), H. Hubert (a2), M. Floquet (a2) and D. Briot (a2)...

Extract

We present here a preliminary report on the analysis of simultaneous photometric and spectroscopic observations of the Be star α Eri, taken during 1992 at the Laboratório Nacional de Astrofísica. α Eri (Archenar, HR472, HD10144, B3–4 III-IV) is the brightest Be star in the sky. It shows activity cycles in a time scale of a few years. Balona et al. (1987) presented a comprehensive study of the star based on photometric and spectroscopic observations. They found a periodicity of 1.26 days in both radial velocity and light variations and argued that a spotted star rotating at this period is the simplest working model that explains the observations.

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References

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Balona, L.A.: 1987, M.N 224, 41
Floquet, M., Hubert, A.M., Janot-Pacheco, E., Mekkas, A., Hubert, H. and Leister, N.V.: 1991, A&A 264, 177
Slettebak, A.: 1982, ApJS 50, 55
Walker, G.A.H.: 1991, Rapid Variability of OB Stars: Nature and Diagnostic Value, ESO workshop, ed. Baade, D., 27

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