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Preprint 22/02

TOWARDS ASTEROSEISMOLOGY OF THE NON-RADIAL PULSATING SDB STAR PG 1605+072

S. FALTER (1), U. HEBER (1), S. DREIZLER (2), S. L. SCHUH (2), O. CORDES (3)

(1) Dr. Remeis-Sternwarte, Universität Erlangen-Nürnberg, Sternwartstr. 7, D-96049 Bamberg, Germany
(2) Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D-72076 Tübingen, Germany
(3) Sternwarte der Universität Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany

To appear in: Proc. XIII Workshop on White Dwarfs, Kluwer Academics NATO Science Series, eds. D. de Martino, R. Kalytis, R. Silvotti, J.E. Solheim

Abstract. The recently discovered new class of sdB pulsators (sdBV) offers a powerful possibility for the investigation of their interior and thus their evolutionary history. The first step towards applying asteroseismologic tools is the identification of pulsation modes. The best target for such an investigation is PG 1605+072 because of its outstanding properties among the sdBVs: it is the brightest object (B = 13 mag), it has the longest periods (~ 500 s) and the largest variations (0.2 mag in the optical) as well as the richest pulsation spectrum with more than 50 modes (see Kilkenny et al. 1999). The rather rapid rotation (v sin i = 39 km/s, Heber et al. 1999) complicates the interpretation of the pulsation spectrum due to non-linear mode splitting.

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Paper (73k gzip'ed Postscript including figures)

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