deletions | additions       diff --git a/Mode Visibility.tex b/Mode Visibility.tex  index 09be84a..34dbcde 100644  --- a/Mode Visibility.tex  +++ b/Mode Visibility.tex 
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\end{equation}  where $\Delta \nu \simeq (2 t_{\rm cross})^{-1}$ \citep{Chaplin_2013} is the large frequency spacing, and $\tau_{0}$ is the damping time of a radial mode with the same frequency. The value of $T^2$ can be easily calculated from a stellar model, whereas the envelope life-time $\tau_{0} \sim 10 \, {\rm days}$ \citep{Dupret_2009,Corsaro_2012} for stars ascending the RGB.  Fig.~\ref{fig:moneyplot} compares our estimate for suppressed dipole mode visibility (equation \ref{eqn:vis}) with the observations of \cite{Mosser_2011}. Our estimate closely aligns with the branch of stars classified by \cite{Mosser_2011} as suppressed pulsators. The striking agreement holds over a large baseline in $\nu_{\rm max}$. The %The  predicted visibility of equation \ref{eqn:vis} has no free parameters, although there is some uncertainty in the value of $\tau_0$. Additional scatter can be accounted for by a range of stellar masses, metallicities, and inclinations in the the observed sample. We conclude that the cores of stars with suppressed dipole modes host a mechanism able to efficiently trap waves tunneling through the evanescent region. This is further supported by the normal $\ell=0$ mode visibility in suppressed pulsators (since radial modes do not propagate within the core) and the lack (or perhaps smaller degree) of suppression observed in $\ell=2$ modes by \citet{Mosser_2011}, as quadrupole modes have a smaller transmission coefficient $T$.  An additional consequence is that the larger effective damping rate for suppressed modes will lead to larger line widths in the oscillation power spectrum. The %The  linewidth of a non-suppressed mode is the mode damping rate $\gamma_{\alpha}$, which in general is not equal to $\tau_{0}^{-1}$ because non-radial mixed modes have some inertia in the core (in contrast to radial modes which are confined to the envelope). The linewidth of a suppressed mode is $\tau_{0}^{-1} + \Delta \nu T^2_{\ell}$ and is generally much larger. The suppressed modes in KIC 8561221 \citep{Garcia_2014} indeed have much larger linewidths. %The second consequence is that, under the assumption that none of the energy tunneling through the evanescent region makes it back to the envelope, {\it only} envelope modes (p modes) will be visible in the suppressed part of the oscillation spectrum. Mixed modes in the usual sense no longer exist. However, if some fraction of the wave energy returns to the surface, there may exist mixed magneto-gravity acoustic modes that could be used to constrain the magnetic field geometry.% because of the strong magnetic field in the g mode cavity. % Although magneto-gravity modes may still exist, their high $\ell$ nature in the core makes them unlikely to be observed at the surface of the star (i.e., they have very large mode inertias).