By Alan H. Batten and D. ter Haar (Auth.)
Hardcover: 278 pages writer: Pergamon Press; 1st variation (1973) Language: English ISBN-10: 0080169864 ISBN-13: 978-0080169866
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Extra info for Binary and Multiple Systems of Stars
The mean molecular weight of these layers is thus higher than that of the whole star, and this difference is proposed as a mechanism to drive the pulsations of the star. The observational evidence for supposing all ß Cephei stars to be members of close binary systems is ambiguous. Two of them are listed in the Sixth Catalogue, 16 Lacertae and a Scorpii, although both orbits are of poor quality. It is difficult to separate the velocity variations due to orbital motion from those due to the intrinsic variation, and it is perhaps still not entirely certain that these stars are binaries.
Any possible selection introduced by rotation is then eliminated. Unfortunately, sampling errors are likely to become important, because some clusters contain only very few stars having rotational velocities in a given interval (Abt, 1970). Nevertheless, columns 3 and 4 in Table 2 give the percentage of known and suspected binaries amongst slowly rotating (v sin / < 50 km/sec) and rapidly rotating members (v sin i > 50 km/sec) of the various clusters. Further investigation of the suspected binaries in these clusters is highly desirable.
All the samples are small, however, and the differences between them may not be significant. The Ap spectra are also characterized by sharp lines, and velocity variations are fairly easy to detect. The most obvious selection effect therefore, should favour the discovery of spectroscopic binaries in this group, just as it does for the Am stars. Unless some other unsuspected selection factor is operating, it seems likely that the apparent deficit of spectroscopic binaries amongst Ap stars is real.