deletions | additions       diff --git a/Mode Visibility.tex b/Mode Visibility.tex  index 7e78cdf..3e8beda 100644  --- a/Mode Visibility.tex  +++ b/Mode Visibility.tex 
...
\end{equation}  where $r_1$ and $r_2$ are the lower and upper boundaries of the evanescent zone, respectively. For waves of the same frequency, larger values of $\ell$ have larger values of $r_2$, thus equation \ref{eqn:integral2} demonstrates that high $\ell$ waves have much smaller transmission coefficients through the evanescent zone. The fraction of wave energy transmitted through the evanescent zone is $T^2$.  To estimate the reduced mode visibility due to energy loss in the core, we assume that all mode energy which leaks into the g mode cavity is completely lost. The mode then loses a fraction $T^2$ of its energy in a time $2 t_{\rm cross}$, where $t_{\rm cross}$ is the wave crossing time of the acoustic cavity. {\bf Due to the larger energy loss rate, the mode has less energy $E_{\rm ac}$ within the acoustic cavity and produces a smaller luminosity fluctuation $V$ at the stellar surface, whose amplitude scales as $V^2 \propto E_{\m E_{\rm  ac}$.} We show (supplementary online text) that the ratio of visibility between a suppressed mode and its non-suppressed counterpart is \begin{equation}  \label{eqn:vis}  \frac{V_{\rm sup}^2}{V_{\rm norm}^2} = \bigg[1 + \Delta \nu \, \tau \, T^2 \bigg]^{-1} \, , 
...