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R-mode oscillations in uniformly and slowly rotating stars have been investigated. Perturbations of the gravitational potential have been included. Applying an adiabatic analysis to a polytrope of index n = 3, gravitational potential perturbations are shown to be small for r modes in most cases. A nonadiabatic analysis of oscillations with l = the absolute value of m is applied to the models of massive zero-age main-sequence stars and ZZ Ceti type variable stars. All the modes examined for the massive zero-age main-sequence stars are stable whereas r modes in the ZZ Ceti model appear to be overstable. However, the neglect of coupling between oscillations and convection might be important for the latter stars because regions of excitation coincide with convection zones.
Hideyuki Saio (Sat,) studied this question.