deletions | additions       diff --git a/Rotation.tex b/Rotation.tex  index 3752d55..71ee9ea 100644  --- a/Rotation.tex  +++ b/Rotation.tex 
...
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 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.  If the wave energy is reflected into inertial waves or Rossby waves, it will likely remain trapped in the core, because these waves can only exist in regions where $\nu < 2 \nu_s$. Moreover, these waves are generally composed of a broad spectrum of $\ell$, and will thus be trapped by the evanescent region between the core and envelope. It is therefore conceivable that rapid rotation can suppress the visibilities of dipole modes in a manner similar to the magnetic greenhouse effect.  \subsection{Problems with the Rotational Interpretation}