Volume 448, Number 2, March III 2006
|Page(s)||697 - 701|
|Section||Stellar structure and evolution|
|Published online||24 February 2006|
A hybrid β Cephei-SPB star in a binary system: γ Pegasi
Observatoire de la Côte d'Azur, Département GEMINI – UMR 6203, BP 4229, 06304 Nice Cedex 4, France e-mail: email@example.com
Accepted: 24 October 2005
High resolution and high signal to noise ratio spectroscopic observations of the classical β Cephei star γ Peg were obtained between 1991 and 2005. The analysis of these data combined with previously published results shows that γ Peg is a spectroscopic binary with an orbital period of 370.5 d. We discovered three new frequencies in addition to the well-known 6.5897 d-1 (0.15175 d) one. That at 6.01 d-1 is a typical β Cephei frequency. The two others at 0.68 and 0.87 d-1 are similar to the high degree g-mode frequencies found in SPB stars. Thus, γ Peg is a hybrid β Cephei-SPB star. Its position in the HR diagram is compatible with such a status. In addition, a small increase of the main period has been detected between the 1995 and 2005 observations.
Key words: stars: binaries: spectroscopic / stars: oscillations / stars: individual: β Cephei / stars: variables: general
© ESO, 2006
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