An observational study of the influence of close companions on the pulsations of Beta Cephei stars

Details An observational study of the influence of close companions on the pulsations of Beta Cephei stars An observational study of the influence of close companions on the pulsations of Beta Cephei stars

May 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...121...45w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 121, no. 1, May 1983, p. 45-50. Research supported by the Ministerie voor Nede

Astronomy and Astrophysics

Astrophysics

27

Companion Stars, Early Stars, Eclipsing Binary Stars, Periodic Variations, Stellar Spectrophotometry, Variable Stars, Hertzsprung-Russell Diagram, Orbital Elements, Tides

Scientific paper

The evidence for short-period pulsations of seventeen close binary stars that fall in the zone of the HR diagram defined by the β Cephei stars is discussed. For the eleven stars that have an orbital period shorter than that of α Virginis, the closest known binary among the β Cephei stars, no pulsations were observed above our detection limit. In the cases where variability was found, the ellipsoidal variations could account completely for the observed variations. The only star in our sample for which we detected pulsations is η Orionis; its orbital period is about twice that of α Virginis.
From these results, it is suggested that the tidal interactions have a damping effect on β Cephei type pulsations. This would explain why the observed lower limit of the orbital periods of the binary β Cephei stars is about three times the theoretical lower limit, which corresponds to a contact configuration. It is also suggested that tidal effects are responsible for the variations of the pulsation amplitudes of the three β Cephei stars with shortest known orbital periods: α Virginis, β Cephei and 16 Lacertae.

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