deletions | additions       diff --git a/Mode Visibility.tex b/Mode Visibility.tex  index 2b70c32..490ac99 100644  --- a/Mode Visibility.tex  +++ b/Mode Visibility.tex 
...
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 (\cite{Garcia_2014}) indeed have much larger linewidths.  The second consequence is that {\it only} envelope modes (p-modes) (p modes)  will be visible in the suppressed part of the oscillation spectrum. Mixed modes in the usual sense no longer exist 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).