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Astron. Astrophys. 331, 162-166 (1998)

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On the inclination and binarity of the pulsating pre-white dwarf PG 2131 +066 *

Ernst Paunzen 1, Michael König 2 and Stefan Dreizler 2

1 Institut für Astronomie der Universität Wien, Türkenschanzstr. 17, A-1180 Wien, Austria (paunzen@galileo.ast.univie.ac.at)
2 Institut für Astronomie und Astrophysik, - Astronomie -, Universität Tübingen, Waldhäuserstr. 64, D-72076 Tübingen, Germany

Received 29 July 1997 / Accepted 27 October 1997


We report on new spectroscopic data as well as recent results from a temporal analysis of PG 2131 +066 WET time series, yielding a new interpretation of the binarity nature for PG 2131 +066. The newly discovered H [FORMULA] emission features, the estimated low inclination and the found 3.9 h period, support the picture of a close binary system, composed of the nonradial oscillating white dwarf with a cool red dwarf companion. Since the spin and the orbital period are not yet synchronized and because PG 2131 +066 has no X-ray counterpart, we classify it as a progenitor of a cataclysmic variable.

Key words: stars: binaries: close – oscillations – white dwarfs – individual: PG 2131+066

* Based on observations obtained at the German-Spanish Astronomical Center, Calar Alto, operated by the Max Planck Institut für Astronomie Heidelberg jointly with the Spanish National Commission for Astronomy.

Send offprint requests to: E. Paunzen

© European Southern Observatory (ESO) 1998

Online publication: February 4, 1998