Institut für Astronomie und Astrophysik

Abteilung Astronomie

Preprint 01a/97

DO White Dwarfs

S. Dreizler(1), K. Werner(2), U. Heber(3), N. Reid(4)

(1)Institut für Astronomie und Astrophysik, Universität Kiel, D-24098 Kiel, Germany
(2)Institut für Astronomie und Astrophysik, Astronomie, Universität Tübingen, Waldhäuser Str. 64, D-72076 Tübingen, Germany
(3)Dr. Remeis-Sternwarte, Sternwartstr. 7, D-96049 Bamberg, Germany
(4)Palomar Observatory 105-24, California Institute of Technology, Pasadena, CA 91125, USA

Contribution to the 3rd Conference on Faint Blue Stars, Schenectady USA, October 13-17, 1996

Abstract. For most known DOs detailed NLTE model atmosphere analyses have now become available. We therefore review our current knowledge about hot helium rich (DO) white dwarfs. These stars represent the non-DA white dwarf cooling sequence from the hot end (T_eff ~ 120 000 K) down to the DB gap (T_eff ~ 45 000 K). Determination of effective temperature, surface gravity and atmospheric composition allows a discussion of the evolutionary status of these stars.

Paper (103k gzip'ed Postscript including figures)

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Jürgen Barnstedt (barnstedt AT astro.uni-tuebingen.de) Last updated 04-Aug-1997