Abstract
Context.Oscillations in rotating stars with frequency of the same order or smaller than the rotation rate Ω cannot be described by a single spherical harmonic due to the effect of the Coriolis force. This is a serious complication which is usually treated by writing the eigenfunctions as a (truncated) sum of different spherical harmonic degrees for a given m-value, or by neglecting the θ part of the rotation vector (Traditional Approximation).
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