Abstract
The light variation of V711 Tauri was first discovered by Cousins, who suspected the variation with an amplitude of ΔV = 0m.11. This light variation was confirmed by Landis and Hall (1976). This star has been identified as the brightest RS CVn-type star by Bopp and Fekel (1976). Bopp et al. (1977), using Cousins’ old data and their data made nearly 13 years later than those of Cousins, found that the observations show the same light curve shape and amplitude and the minimum light falls very nearly at 0P.0 computed with their ephemeris.
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References
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© 1983 Springer Science+Business Media Dordrecht
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Nha, IS., Oh, J.Y. (1983). Light Curves and Ca II Emissions of V711 Tauri during 1981–82. In: Byrne, P.B., Rodonò, M. (eds) Activity in Red-Dwarf Stars. Astrophysics and Space Science Library, vol 102. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7157-8_53
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DOI: https://doi.org/10.1007/978-94-009-7157-8_53
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