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Light Metals in PG1159 Central Stars

Published online by Cambridge University Press:  15 December 2006

E. Reiff ,
D. Jahn ,
T. Rauch ,
K. Werner ,
F. Herwig  and
J.W. Kruk
E. Reiff
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany
D. Jahn
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany
T. Rauch
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany
K. Werner
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany
F. Herwig
Affiliation:
Los Alamos National Laboratory, Bikini Atoll Rd., SM 30, Los Alamos, NM 87545, USA
J.W. Kruk
Affiliation:
Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA
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Abstract

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We present results of a quantitative spectral analysis of a sample comprising eleven hydrogen deficient post-AGB stars of the spectral type PG 1159 with state-of-the-art NLTE model atmospheres. For all objects high resolution spectra obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) are available. The FUV spectra of PG 1159 stars are dominated by lines of helium, carbon and oxygen, and for the first time we also identified lines of several trace elements as sulfur and silicon which allow to determine the abundances of light metals in the atmospheres of these stars. As these stars show nuclear processed former intershell matter on their surface, the determined abundances also allow us to constrain the predictions of evolutionary models and element abundances in AGB stars.

Keywords

stars: abundancesstars: AGB and post-AGBstars: atmospheres
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 489 - 490
Copyright
© 2006 International Astronomical Union