deletions | additions       diff --git a/Mode Visibility.tex b/Mode Visibility.tex  index 729d8c4..f2a40d9 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} for stars ascending the RGB.  A comparison between the theoretical prediction Fig.~\ref{fig:moneyplot} compares our estimate  for the visibility of suppressed  dipole modes for which the energy transmitted to the core is completely lost   %by the magnetic greenhouse effect   and 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} is shown in Fig.~\ref{fig:moneyplot}. as suppressed pulsators.  The striking  agreementis striking, and  holds over a large baseline in $\nu_{\rm max}$. 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. This shows We conclude  that the cores of stars with weaker 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 (since radial modes do not propagate within the core) and the  lack (or perhaps small smaller  degree) of suppression observed in $\ell=2$ modes by \citet{Mosser_2011}, as quadrupole modes have a smaller transmission coefficient $T$. There are two additional consequences for mode visibility. First, the larger effective damping rate for suppressed modes will lead to larger line widths in the oscillation power spectrum. 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.