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Introductory report on AG Pegasi*

Published online by Cambridge University Press:  12 April 2016

Extract

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The light history of AG Peg (HD 207757) is characterized by a ~3 mag brightening which took place during 1850-70 followed by a slow decline ever since. In recent times the V magnitude has shown variations between 7.7 and 8.8, and a semi–regular behaviour with maxima 600 to 700 days apart (Mattei 1981). The optical spectrum and its time variation was studied among others by Boyarchuk (1967) and Hutchings et al. (1975) who suggested the presence of a binary system consisting in an M type giant and a WN6 companion surrounded by a nebular region.

Type
Session II – Discussion on Individual Stars
Copyright
Copyright © Reidel 1982

Footnotes

*

Since the original report of CD. Keyes has not arrived in time to be included in the Proceedings, a short abstract was prepared by the Editors partly based on notes taken during Keyes’ talk.

References

Allen, A.D.: 1979, Changing trends in Variable Star Research, IAU Coll. No. 46, Bateson, F.M., Smak, J. and Urch, I.H. (eds.), University of Waikoto, Hamilton, p. 125 Google Scholar
Boyarchuk, A.A.: 1967, Soviet Astronomy AJ, 11, 8 (Astr. Z. 44, 12)Google Scholar
Gallagher, J.S., Holm, A.V., Anderson, C.M., Webbink, R.F.: 1979, Astro-physical J. 229, 994 CrossRefGoogle Scholar
Ghigo, F.D., Cohen, N.L.: 1981, Astrophys. J. 245, 988 Google Scholar
Hutchings, J.B., Cowley, A.P., Redman, R.O.: 1975, Astrophys.J. 201, 404 CrossRefGoogle Scholar
Keyes, C.D., Plavec, M.J.: 1980, The Universe at Ultraviolet Wavelengths, Chapman, R.D. (ed.), NASA CP-217I, p. 443 Google Scholar
Mattei, J.A.: 1981, North American Workshop on Symbiotic Stars, Stencel, R.E. (ed.), JILA and University of Colorado, p. 31 Google Scholar