deletions | additions       diff --git a/Rotation.tex b/Rotation.tex  index 63d1416..f92dc26 100644  --- a/Rotation.tex  +++ b/Rotation.tex 
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We can speculate on the effect of rotation on a dipole wave as it travels from a slowly rotating envelope to a rapidly rotating core. We will assume the rotation rate increases gradually such that a WKB analysis remains valid. In this case, the effects of rotation on the high order gravity waves is captured by the traditional approximation, in which the Coriolis force changes the gravity waves into Hough waves. The Hough waves are very similar to gravity waves except that their angular structure and radial wavelength are altered. When $2 \nu_s > \nu$, the angular structure of the dipole waves will be strongly altered, and the angular structure of the wave will be composed of a broad spectrum of angular degrees $\ell$. This spectrum generally depends on the $m$ value of the incoming wave, i.e., whether the incoming wave was axisymmetric, prograde, or retrogade relative to the spin.  One key difference between the symmetry-breaking effects of rotation compared to a magnetic field is that rotation (in the WKB limit) will not generate create  an evanescent region. Therefore, the waves will not be reflected by rapidly rotating layers (although prograde waves may be absorbed at critical layers), and the waves will continue to propagate toward the center of the star as Hough waves. When they reflect near the center of the star, our WKB analysis breaks down. At this point, the waves may be reflected onto the same branch of Hough waves, or energy may be transferred to other Hough wave branches, or to inertial waves or Rossby waves. If the wave energy is reflected back onto the same Hough wave branch, the wave will propagate outward and transform back into a dipole wave in the slowly rotating layers. In this case we would not expect to observe mode suppression, although the g-mode period spacing would be strongly altered because of the different radial wavelength of the Hough waves.