Institut für Astronomie und Astrophysik
Abteilung AstronomieSand 1, D-72076 Tübingen, Germany
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T. Rauch (1), K. Werner (1), M. Ziegler (1), L. Koesterke (2), J. W. Kruk (3), C. M. Oliveira (3)
(1) Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Tübingen, Germany
(2) Texas Advanced Computer Center, University of Texas, Austin, TX 78712, U.S.A.
(3) Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, U.S.A.
To be published in: Proceedings: Future Directions in Ultraviolet Spectroscopy Conference, Annapolis, MD, 2008
Abstract. State-of-the-art non-LTE spectral analysis requires high-resolution and high-S/N observations of strategic metal lines in order to achieve reliable photospheric parameters like, e.g., effective temperature, surface gravity, and element abundances.
Hot stars with effective temperatures higher than about 40000 K exhibit their metal-line spectrum arising from highly ionized species predominantly in the (far) ultraviolet wavelength range.
FUSE observations of hot, compact stars provided the necessary data. With these, it has been, e.g., possible to identify fluorine for the first time in observations of post-AGB stars. The evaluation of ionization equilibria of highly ionized neon, phosphorus, sulfur, and argon provides a new sensitive tool to determine effective temperatures of the hottest stars precisely. Moreover, abundance determinations have put constraints on stellar evolutionary models which, in turn, have improved greatly our picture of post-AGB evolution.
Key words: Stellar evolution, Stellar atmospheres, Mass loss, Abundances, white dwarfs
Preprint (107 kb PDF file including figures)
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Last modified 10 Nov 2008