Abstract
Frequency distributions of υ sin i on a uniform system are presented for O5–B5 stars. Theoretical distributions are given which take into account the effect of observational errors. Some physical implications are discussed. It is found that B stars probably do not rotate as solid bodies. Difficulties are encountered if Be stars are postulated to be rotating near their break-up velocity unless most of them are evolved from the main sequence, or have large differential rotations. A distinct correlation between hydrogen line strength and axial rotation is found.

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