A method is described for solving the equations that govern the oscillations of rapidly rotating inhomogeneous Newtonian stellar models. A covariant reformulation of the general pulsation equations is presented, which reduces them to a single scalar equation for a single potential. From this potential, all of the properties of the normal mode may be deduced. The techniques developed to solve this complicated eigenvalue problem numerically are described, and solutions to this equation are presented for the l = m f-modes of rigidly rotating stellar models having polytropic equations of state.
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Ipser et al. (1990) studied this question.