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Preprint 11j/04

HST and FUSE Spectroscopy of Hot Hydrogen-Rich Central Stars of Planetary Nebulae

I. Traulsen (1), A.I.D. Hoffmann (1), T. Rauch (1,2), K. Werner (1), S. Dreizler (3), J.W. Kruk (4)

(1) Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D-72076 Tübingen, Germany
(2) Dr.-Remeis-Sternwarte, Universität Erlangen-Nürnberg, Sternwartstr. 7, D-96049 Bamberg, Germany
(3) Institut für Astrophysik, Friedrich-Hund-Platz 1, D-37077 Göttingen, Germany
(4) Department of Physics and Astronomy, 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. High-resolution UV spectra, obtained with HST and FUSE, enable us to analyse hot hydrogen-rich central stars in detail. Up to now, optical hydrogen and helium lines have been used to derive temperature and surface gravity. Those lines, however, are rather insensitive; in particular, neutral helium lines have completely vanished in the hottest central stars. Therefore, we have concentrated on ionization balances of metals, which have a rich line spectrum in the UV, to establish a new temperature scale for our sample. Furthermore, we have determined abundances of light metals, which had been poorly known before. They show considerable variation from star to star. We present results of quantitative spectral analyses performed with non-LTE model atmospheres.
 

Preprint (216 kb PDF file including figures)
Astrophysics (astro-ph): astro-ph/0411403

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