Vibrations of Be stars.

Details Vibrations of Be stars. Vibrations of Be stars.

Dec 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983msngr..34...28b&link_type=abstract

The Messenger, vol. 34, p. 28-30

Astronomy and Astrophysics

Astronomy

Be Stars:Pulsations, Pulsations:Be Stars

Scientific paper

Two well-attended IAU symposia in 1975 and 1981 (in the respective proceedings the interested reader may find all relevant references) and an IAU colloquium being planned for the mid-eighties, all three devoted exclusively to Be and shell stars, show that stellar astronomers take a very active interest in these strange objects. The first Be star, y Cas, was identified as such by Secchi as early as 1866, and today 2- 3% of all stars in the Bright Star Catalogue are known to belong to this class. The amount of observational data that has been accumulated is therefore vast, and at all times it has been of the best technical quality. For this reason we are now at a stage where for more and more of these stars it becomes possible (or tempting) to search for periodicities in the (sometimes spectacular) spectroscopic variability exhibited on time seales of years by many Be stars. The idea is that these stars might be binaries and that the mass exchange between the two components is the origin of the line emitting shell around the B-type primary. But for many objects it may weil take a few more decades to distinguish with some certainty between true and spurious periods. So far, there is no indication that the binary frequency of Be stars is any higher than the one of "normal" B stars which itself is roughly the same as for 0 through G type stars.

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