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Preprint 11l/04

FUSE spectroscopy of PG1159 Stars

E. Reiff (1), T. Rauch (1,2), K. Werner (1), J.W. Kruk (3)

(1) Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany
(2) Dr.-Remeis-Sternwarte, Universität Erlangen-Nürnberg, Sternwartstr.7, 96049 Bamberg, Germany
(3) Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA

To be published in: 14th European Workshop on White Dwarfs, eds. D. Koester, S. Moehler, ASP Conf. Ser.

Abstract. PG1159 stars are hot hydrogen-deficient post-AGB stars with effective temperatures within a range from 75000 K up to 200000 K. These stars are probably the result of a late helium-shell flash that had occurred during their first descent from the AGB. The lack of hydrogen is caused by flash-induced envelope mixing and burning of H in deeper regions. Now the former intershell matter is seen on the surface of the stars. Hence the stellar atmospheres show metal abundances drastically different from the solar values. Our sample comprises ten PG1159 stars with effective temperatures between 85000 K and 170000 K. We present first results of our spectral analysis based on FUV spectra obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE).
 

Preprint (565 kb PDF file including figures)
Astrophysics (astro-ph): astro-ph/0411337

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