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Spectral Energy Distribution (119–685 nm) in 16 Shell Stars and a Tentative Model for Accreting be Stars

Published online by Cambridge University Press:  14 August 2015

Mirek J. Plavec ,
Jan J. Dobias ,
Janet L. Weiland  and
Remington P.S. Stone
Mirek J. Plavec
Affiliation:
Department of Astronomy, University of California, Los Angeles
Jan J. Dobias
Affiliation:
Department of Astronomy, University of California, Los Angeles
Janet L. Weiland
Affiliation:
Department of Astronomy, University of California, Los Angeles
Remington P.S. Stone
Affiliation:
Lick Observatory, University of California

Abstract

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I.U.E. low-dispersion spectra and spectral scans made with the Lick Observatory IDS scanners have been combined for 16 shell stars. Eleven objects can be represented by Kurucz model atmospheres, although some of them display strong shell-type line spectra. Five among them are known binaries. The six remaining objects (all interacting binaries) display complex spectra. A model involving continuum and line radiation from a hydrogen cloud surrounding the accreting component is proposed. A generalization of this model with optically thick segments of the cloud promises to explain even more exotic objects such as β Lyrae, W Serpentis and possibly ∊ Aurigae.

Type
VII. UV Observations and Mass Loss
Information
Symposium - International Astronomical Union , Volume 98: Be Stars , 1982 , pp. 445 - 450
Copyright
Copyright © Reidel 1982 

References

Cowley, A.P.: 1967, Astrophys. J., 147, 609.Google Scholar
Flower, P.J.: 1977, Astron. Astrophys., 54, 31.Google Scholar
Gehrz, R.D., Hackwell, J.A. and Jones, T.W.: 1974, Astrophys. J., 191, 675.Google Scholar
Hack, M.: 1962, Mem. Astron. Soc. Ital., 32, 3.Google Scholar
Hack, M. and Selvelli, P.L.: 1978, Nature, 276, 376.Google Scholar
Hall, D.S.: 1969, Bull. Amer. Astron. Soc., 1, 345.Google Scholar
Hayes, D.S.: 1978, in “The HR Diagram” (ed. Phillips, A.G.D. and Hayes, D.S.): Reidel, p. 65.CrossRefGoogle Scholar
Huang, S.S.: 1965, Astrophys. J., 141, 976.Google Scholar
Kurucz, R.L.: 1979, Astrophys. J. Suppl., 40, 1.Google Scholar
Madej, J. and Paczynski, B.: 1977, Veröff. Bamberg 11 #121, 313.Google Scholar
Plavec, M.J.: 1980, in “Close Binary Stars: Observation and Interpretation” (eds. Plavec, M.J., Popper, D.M. and Ulrich, R.K.): Reidel, p. 251.Google Scholar
Plavec, M.J. and Sakimoto, P.J.: 1978, Bull. Amer. Astron. Soc., 10, 609.Google Scholar
Pringle, J.E.: 1977, Mon. Not. R.A.S., 178, 195.Google Scholar
Schmidt-Kaler, Th.: 1965, in Landolt-Börnstein (ed. Voigt, H.H.): Springer, Bd. I, p. 309.Google Scholar
Wilson, R.E.: 1974, Astrophys. J., 189, 319.Google Scholar