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Ultraviolet Variability of the Symbiotic Star AG PEG

Published online by Cambridge University Press:  12 April 2016

D. Chochol ,
Z. Komárek  and
A. Vittone
D. Chochol
Affiliation:
Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Czechoslovakia
Z. Komárek
Affiliation:
Public Observatory, 071 01 Michalovce, Czechoslovakia
A. Vittone
Affiliation:
Osservatorio Astronomico Capodimonte, Via Moiariello 16, 80131 Napoli, Italy

Extract

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Symbiotic star AG Peg consists of a hot subdwarf with a WN6 spectrum and a cool M3 giant, which is not filling its Roche lobe (Boyarchuk 1967, 1985). A detailed study of profiles, equivalent widths and radial velocities of emission lines in optical spectra allowed Hutchings et al. (1975) to conclude that a hot subluminous star approximately 1 M⊙ rotates rapidly and ejects material which streams towards the cool M giant with the mass 3-4 M⊙. UV observations seems to support this model.

UV observations provided from the databank of the IUE satellite were obtained in 1978–81 by different observers. The observational material consists of 12 high dispersion SWP spectra and covers the region 1200 – 2100 A. The spectra were reduced at Trieste observatory using standard IUESIPS package. The radial velocities of emission lines were measured on tracings and corrected for the motion of Earth and satellite.

Type
Session 3. Physics of Individual Objects
Information
International Astronomical Union Colloquium , Volume 103: The Symbiotic Phenomenon , 1988 , pp. 263 - 264
Copyright
Copyright © Kluwer 1988

References

Boyarchuk, A.A.: 1967, Soviet Astr. 10, 783.Google Scholar
Boyarchuk, A.A.: 1985, In: ESA Workshop: Recent Results on Cataclysmic Variables, ESA SP-236, p. 97.Google Scholar
Cowley, A., Stencel, R.: 1973, Astrophys. J. 184, 687.Google Scholar
Hutchings, J.B., Cowley, A.P., Redman, R.O.: 1975, Astrophys. J. 201, 404.CrossRefGoogle Scholar
Meinunger, L.: 1981, Inform. Bull. Var. Stars, No. 2016.Google Scholar
Penston, M.V., Allen, D.A.: 1985, Mon.Not.R.astr.Soc. 54, 229.Google Scholar