deletions | additions       diff --git a/Mode Visibility.tex b/Mode Visibility.tex  index 616ac20..b099b03 100644  --- a/Mode Visibility.tex  +++ b/Mode Visibility.tex 
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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 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} $\tau^{-1}  + \Delta \nu T^2_{\ell}$ and is generally much larger than that of a non--suppressed mode. The suppressed dipole modes in KIC 8561221 \citep{Garcia_2014} indeed have much larger linewidths than non-suppressed dipole modes in similar stars.