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The High Resolution Spectrum of the Pulsating, Pre-White Dwarf Star PG 1159-035 (GW VIR) (1)

Published online by Cambridge University Press:  12 April 2016

James Liebert ,
F. Wesemael ,
D. Husfeld ,
R. Wehrse ,
S. G. Starrfield  and
E. M. Sion
James Liebert
Affiliation:
Steward Observatory, University of ArizonaAZ 85721
F. Wesemael
Affiliation:
Steward Observatory, University of ArizonaAZ 85721
D. Husfeld
Affiliation:
Institut für AstronomieundAstrophysik der Universität München, Scheinerstrasse 1 D-8000 München 80
R. Wehrse
Affiliation:
Institut für Theoretische AstrophysikderUniversität Heidelberg, D-6900 Heidelberg, F.R.Germany
S. G. Starrfield
Affiliation:
Department of Physics, Arizona State University Tempe, AZ 85287
E. M. Sion
Affiliation:
Department of Astronomy, Villanova University Villanova, PA 19085

Extract

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First reported at the IAU Colloquium No. 53 on White Dwarfs (McGraw et al. 1979), PG 1159-035 (GW Vir) is the prototype of a new class of very hot, pulsating, pre-white dwarf stars. It shows complicated, nonradial pulsation modes which have been studied exhaustively, both observationally and theoretically. The effective temperature has been crudely estimated as 100,000 K with log g ~ 7 (Wesemael, Green and Liebert 1985, hereafter WGL).

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 114: White Dwarfs , 1989 , pp. 384 - 387
Copyright
Copyright © Springer-Verlag 1989

Footnotes

(2)

Guest Observers with the International Ultraviolet Explorer (IUE) Observatory, which is sponsored and operated by the National Aeronautics and Space Administration, the European Space Agency and the Science Research Council of the United Kingdom.

(1)

Optical data reported here were obtained at the Multiple Mirror Telescope (MMT) Observatory, a facility operated jointly by the Harvard-Smithsonian Center for Astrophysics and the University of Arizona.

References

Bond, H.E., Grauer, A.D., Green, R.F. and Liebert, J. (1984). Astrophys. J. 279, 751 Google Scholar
Husfeld, D. (1987). In The Second Conference on Faint Blue Stars, IAU Coll. 95, edited by Philip, A.G.D., Hayes, D.S. and Liebert, J. (Davis, Schenectady NY) p. 237.Google Scholar
Kudritzki, R. (1987). In The Second Conference on Faint Blue Stars, IAU Coll. 95, edited by Davis Philip, A.G., Hayes, D.S. and Liebert, J.W. (Davis, Schenectady NY), p. 177. Google Scholar
McGraw, J.T., Starrfield, S.G., Liebert, J. and Green, R.F. (1979). In White Dwarfs and Variable Degenerate Stars, Proc. IAU Coll. 53, edited by Van Horn, H.M. and Weidemann, V., (Univ. of Rochester Press, Rochester NY), p. 377. Google Scholar
Sion, E.M., Liebert, J. and Starrfield, S.G. (1985). Astrophys. J. 292, 471 Google Scholar
Starrfield, S.G., Cox, A.N., Kidman, R.B. and Pesnell, W.D. (1984). Astrophys. J. 281, 800 Google Scholar
Vauclair, G. 1989, this conference.Google Scholar
Werner, K., Heber, U. and Hunger, K. 1989, this conference.Google Scholar
Wesemael, F., Green, R.F. and Liebert, J. (1985). Astrophys. J. Suppl. Ser. 58, 379 (WGL).Google Scholar