next previous
Up: Abstract

A&A Supplement series, Vol. 127, February I 1998, 455-461

Received November 21, 1996; accepted May 27, 1997

Monitoring the activity of the Be star OT Geminorumgif

A. Arellano Ferro tex2html_wrap922gif, J.P. Sareyantex2html_wrap924, J.J. Avilatex2html_wrap926, F. Gonzáleztex2html_wrap926, M. Dumonttex2html_wrap930, and GEOStex2html_wrap930 [CHC, MAA, EYR, VRR, FDZ, KCH, MIS, PAR, BSQ, PMP, SCP]

tex2html_wrap934  Departamento de Astronomıa, IFUG, Universidad de Guanajuato Apdo. Postal 144, Guanajuato, Gto. México 36000, México
tex2html_wrap936  Observatoire de la Côte d'Azur, Dept. Fresnel, BP. 229, 06304, Nice Cedex 4, France
tex2html_wrap938  3 Promenade Venezia, 78000, Versailles, France


Observations obtained in 1995-1996 of the Be star OT Geminorum are reported and show that in october 1995 the star reached a very active phase with large variations around a bright plateau, a phase of activity we have also distinguished in previous observations dating from 1960.

The time scales involved are discussed and suggest that the violent variations of the activity propagate very quickly on the whole surface of the star or on a huge portion of it. No likely pulsation periods were found.

The assumption that the detected activity is due to the effects of an hypothetical companion leads to conclude that such companion could not be detected by the present interferometric techniques.

keywords: stars: emission lines, Be; activity; individual (OT Gem)

Copyright by the European Southern Observatory (ESO)