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Preprint 11k/04


Iron Abundance in Hydrogen-Rich Central Stars of Planetary Nebulae

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

(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) Institut für Astrophysik, Universität, Göttingen, Friedrich-Hund-Platz 1, D-37077 Göttingen, Germany
(4) 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. We report on an on-going analysis of high-resolution UV spectra of hot hydrogen-rich central stars of planetary nebulae (CSPN), obtained with the Hubble Space Telescope and FUSE. Since UV spectra of many CSPN are dominated by Fe and Ni lines, we intend to use them as temperature indicators to check the CSPN temperature scale we have derived earlier from CNO ionization balances. Furthermore, the observed line strengths of heavy metals show large variations between different objects suggesting a possible spread in abundances. We will determine abundances of iron group elements by quantitative spectral analyses with non-LTE model atmospheres.
 

Preprint (236 kb PDF file including figures)
Astrophysics (astro-ph): astro-ph/0411404


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