A Spectrographic Study of Beta Centauri

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Abstract
Using spectra obtained in 1969, it is shown that the radial velocity of β Cen was varying with a period of 0d.157 in 1969. The broad spectral line profiles of the star are examined for changes in shape with the above period. This search is considerably complicated by the fact that the star is a single line spectroscopic binary with components of approximately equal brightness, as in such a binary spurious variations may be caused by the variation in the velocity of one component with respect to the other. However, with the help of a series of graphs of predicted blended profiles it is demonstrated that, for the observations under discussion, any variations found are likely to be intrinsic to the star. Variations in the profiles are, in fact, found with the radial velocity period; the phase relations between the changes in the profiles and the radial velocity curve are the same as in the narrow-lined β CMa stars.

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