Jim Fuller edited Rotation.tex  about 9 years ago

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The centrifugal force can still affect acoustic modes by distorting the spherical symmetry of the background star. This can affect their visibility, as discussed in \cite{Reese_2013}. However, in this case we should expect all modes to be affected, not just the dipole modes. It would also require the surface rotation rate to be a significant fraction of breakup, which for the model in Figure \ref{Fig:Struc} corresponds to a rotation period of $P_K \sim 1.5 \, {\rm days}$. Neither of these effects seems to be observed in the majority of suppressed dipole stars.  However, rotation {\it can} strongly affect the modes in the core of a red giant. The breakup frequency evaluated near the H-burning shell of the model in Figure \ref{Fig:Struc} is $\nu_K {\rm (H-burn)} \sim 8 \times 10^3 \, \mu{\rm Hz} \gg \nu_{\rm max}$, and therefore the Coriolis force can have a strong influence on modes if the core of the star is rapidly rotating. Hence, rotation will only be important in the g-mode cavity of modes with frequencies near $\nu_{\rm max}$. This also requires very strong differential rotation between the core and envelope.  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 $\nu_s > \nu$, 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 $\elll$.  \subsection{Problems with the Rotational Interpretation}