deletions | additions       diff --git a/Mode Visibility.tex b/Mode Visibility.tex  index 3c903b9..4b9edfc 100644  --- a/Mode Visibility.tex  +++ b/Mode Visibility.tex 
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\label{eqn:vis}  \frac{V_{\rm sup}^2}{V_\alpha^2} = \bigg[1 + \Delta \nu \tau_{0} T^2 \bigg]^{-1} \, ,  \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} \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 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.