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Optical Variability of the Be Star o And during the Period 1975–1998: Rotational Modulation or Multimodal Pulsations?

Published online by Cambridge University Press:  12 April 2016

G. Guerrero ,
J.P. Sareyan ,
M. Alvarez ,
J. Chauville ,
A. Arellano Ferro ,
P. Mathias ,
J. Pena  and
E. Garciá
G. Guerrero
Affiliation:
Osservatorio Astronomico di Brera, via E.Bianchi 46, I-22055 Merate, Italy
J.P. Sareyan
Affiliation:
Observatoire de la Cote d’Azur, Departement Fresnel, B.P.229, F-06003 Nice Cedex, France
M. Alvarez
Affiliation:
Observatorio Astronomico Nacional, UNAM, Apdo 877, Ensenada, B.C.22800, Mexico
J. Chauville
Affiliation:
Observatoire de Paris-Meudon, URA 335 du CNRS, F-92195 Meudon Cedex, France
A. Arellano Ferro
Affiliation:
Instituto de Astronomiá, UNAM, Apdo Postal 70-264, 04510, Mexico D.F., Mexico
P. Mathias
Affiliation:
Observatoire de Paris-Meudon, URA 335 du CNRS, F-92195 Meudon Cedex, France
J. Pena
Affiliation:
Instituto de Astronomiá, UNAM, Apdo Postal 70-264, 04510, Mexico D.F., Mexico
E. Garciá
Affiliation:
Universidad Autónoma de Nuevo León, México

Abstract

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Photometric observations of o And collected from 1994 to 1998 are presented. Neither multimodal pulsations nor rotational modulation seems able to explain completely the complex light curves, but a model based on the pulsations together with some type of magnetic activity could be applicable.

Type
3. Periodic Variations
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 205 - 207
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Sareyan, J.P. et al. 1998, A&A 332, 155 Google Scholar
Vanicek, , 1971, Astrophys. Space Sci. 12, 10 Google Scholar