Observations of the Small Amplitude Beta-Cephei Stars

Details Observations of the Small Amplitude Beta-Cephei Stars Observations of the Small Amplitude Beta-Cephei Stars

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982msngr..27...17k&link_type=abstract

The Messenger, No.27, P. 17, 1982

Physics

1

Scientific paper

The reason why stars do sometimes pulsate seems to be satisfactorily explained by the present theory of stellar stability. The small but "irritating" exception is only the group of ßCephei stars: the physical mechanism of their variability remains till today essentially unknown. Observational characteristics of these stars can be summarized as foliows: (i) they are located in a rather narrow instability strip on the H-R diagram in the vicinity of effective temperature of about 20,000° or spectral types B1-B2; (ii) periods are of the order of a few (3-6) hours; (iii) in some cases the shape of spectrallines varies with phase, the lines being broad on the descending and narrow on the ascending branch of the radial velocity curve; (iv) radial velocity curves are sometimes asymmetric or even discontinuous, particularly for the stars with large amplitudes; (v) maximum light occurs near the phase when the descending branch of the radial velocity curve crosses the mean velocity; (vi) in some of these stars two or more close frequencies are excited; in two cases triplets of equally spaced frequencies are observed.

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