Abstract
ABSThACT. Five Ha profiles obtained during the 1982-1984 eclipse and three out of the eclipse are presented. The spectra are all of similar dispersions (6-9 /`nm) and were obtained at the observatories of Calar Alto, Almena, Spain, San Pedr0 , Mexico and Rozhen, Bulgaria. Prominent profile variations can be noticed, among the most important are: lack of both blue anct red wing emission as well as the shallowness of the line during the totality. These two features have been observed during the 1955-57 eclipse (Morris 1963, Ph. D. Thesis University of Toronto). During ingress the profile has both winqs in emission as observed in other eclipses. The deep core emission detected by other authors is also present in sane of our eclipse spectra. The spectrum on December 9, 1984, eight months after fourth contact, still shows emission structure in the core of the line, while the two spectra on August 1985 do not show traces of core emission. Ha profiles out of the eclipse are not canmon in the literature and we can not tell if core emission out of eclipse is a canmon phenanenon. Four spectra out of eclipse obtained by Moms (i96. , ibid), do not show core emission. The series of spectra published by Arellano Ferro (1985 Pev. Mex. Astron. and Astrof., 11, 113) is unfortunately of tco low a dispersimn (16 /mm) to unveil any incipient core emission. The blue wing variation that may be connected with the primary F star pulsation (Arellano Ferro 1985, ibid) was not detected in the present out of eclipse spectra but our material is scarce. More spectra obtained at time intervals of weeks are needed to confirm whether the blue wing variation is at all periodic and whether it is related to the underlying stellar pulsation. Spectra and more details will be published elsewhere. o : LINE-PROFILE -- STARS-BINAPY
