Hostname: page-component-7479d7b7d-c9gpj Total loading time: 0 Render date: 2024-07-11T10:23:42.108Z Has data issue: false hasContentIssue false
  • English
  • Français

Light Curves and Ca II Emissions of VT11 Tauri During 1981-82

Published online by Cambridge University Press:  12 April 2016

Il-Seong Nha  and
Jun Young Oh
Il-Seong Nha
Affiliation:
Yonsei University Observatory, Seoul, Korea
Jun Young Oh
Affiliation:
Yonsei University Observatory, Seoul, Korea

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The light variation of V711 Tauri was first discovered by Cousins, who suspected the variation with an amplitude of ΔV = 0.mll. 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 0.P0 computed with their ephemeris.

Type
Session III: Observed Activity in Related Objects
Information
International Astronomical Union Colloquium , Volume 71: Activity in Red-Dwarf Stars , 1983 , pp. 409 - 410
Copyright
Copyright © Reidel 1983

References

References:

Blanco, C., Catalano, S., Marilli, E., Rodono, M., and Scaltriti, F., 1981. IBVS 2000.Google Scholar
Bopp, B. W., and Fekel, F., 1976, A. J., 81, 771.Google Scholar
Bopp, B. W., Espenak, F., Hall, D. S., Landis, H. J., Lovell, L. P., and Reucroft, S., 1977, A. J., 82, 47.Google Scholar
Landis, H. J., and Hall, D. S., 1976, IBVS, 1113.Google Scholar
Sarma, M. B. K., and Ausekar, B.D., 1981, A. A., 31, 103.Google Scholar
Weiler, E. J., 1976, IAU Circ. No. 3089.Google Scholar