Spectroscopy of V471 Tau. II : observations of the Hα line

An analysis of over 200 spectra of V471 Tauri, taken over the interval 1975-1984, is presented. The H-alpha equivalent width is a strong function of phase, going from absorption at phase 0.0 to strong emission at phase 0.5. The absorption profile at phase 0.0 is attenuated and partially filled by em...

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Bibliographic Details
Published in:The Astronomical journal 1991-12, Vol.102 (6), p.2079-2090
Main Authors: BOIS, B, LANNING, H. H, MOCHNACKI, S. W
Format: Article
Language:English
Subjects:
Astronomy
Binary and multiple stars
Earth, ocean, space
Eclipsing binaries
Exact sciences and technology
Stars
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Summary:An analysis of over 200 spectra of V471 Tauri, taken over the interval 1975-1984, is presented. The H-alpha equivalent width is a strong function of phase, going from absorption at phase 0.0 to strong emission at phase 0.5. The absorption profile at phase 0.0 is attenuated and partially filled by emission. A velocity analysis of the emission peaks shows that the strongest emitting region is located at the substellar point. The phase behavior of the H-alpha line was roughly constant over the whole observing period, but the intensity of maximum emission decreased more or less regularly over an interval of ten years. This effect can be correlated with an apparent decrease in the photometric distortion curve amplitude already noted by other workers. However, the preliminary analysis of more recent observations (late 1984, early 1987, 1989) indicates that this trend has reversed. These effects may indicate the presence of a chromospheric activity cycle in the K dwarf, which is surprising for such a rapidly rotating star. (Author)
ISSN:0004-6256
1538-3881
DOI:10.1086/116032