Abstract
The hypothesis of the degeneracy between a radial and a nonradial mode as an explanation of the beat phenomenon in the p Cephei stars is examined by means of a linear, adiabatic pulsation analysis using realistic stellar models. The results are in the form of theoretical values of 0 , log g (to eliminate bolometric corrections), the radial pulsation period, and the period difference between the two periods presumed to cause the beats. These results are compared with observational equivalents, and the agreement for a number of the p Cephei stars showing this effect gives support to this hypothesis. On the assumption that this is the correct explanation of the beats, some conclusions may be drawn regarding the properties of the p Cephei stars. Subject headings: p Cephei stars - pulsation
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