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Preprint 02/99

SPECTROSCOPY OF HOT HYDROGEN DEFICIENT WHITE DWARFS

S. Dreizler

Institut für Astronomie und Astrophysik, Astronomie, Universität Tübingen, Waldhäuser Str. 64, D-72076 Tübingen, Germany

To appear in: Reviews in Modern Astronomy 12, in press

Abstract. UV spectroscopy is the key toward a better understanding of the late evolutionary phases of low and intermediate mass stars. UV spectra, mainly obtained with the Hubble Space Telescope (HST), enable a more precise determi­ nation of the stellar parameters of hot white dwarfs allowing to approach several open questions. About a fifth of all post-AGB stars can not be explained by canonical evolution scenarios because they appear as hydrogen deficient objects. In this work I concentrate on the hot hydrogen deficient stars around the entrance of the white dwarf cooling sequence. From spectral analyses we derive constraints for the evolutionary history, provide spectroscopic support for the asteroseismology, and investigate the transition into the white dwarf phase.

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Paper (447k gzip'ed Postscript including figures)

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