A hybrid β Cephei-SPB star in a binary system: γ Pegasi

Details A hybrid β Cephei-SPB star in a binary system: γ Pegasi A hybrid β Cephei-SPB star in a binary system: γ Pegasi

Mar 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006a%26a...448..697c&link_type=abstract

Astronomy and Astrophysics, Volume 448, Issue 2, March III 2006, pp.697-701

Astronomy and Astrophysics

Astrophysics

20

Stars: Binaries: Spectroscopic, Stars: Oscillations, Stars: Individual: Β Cephei, Stars: Variables: General

Scientific paper

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.

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