deletions | additions       diff --git a/subsection_Joule_Damping_Joule_damping__.tex b/subsection_Joule_Damping_Joule_damping__.tex  index d30135e..00d4a90 100644  --- a/subsection_Joule_Damping_Joule_damping__.tex  +++ b/subsection_Joule_Damping_Joule_damping__.tex 
...
\end{equation}  This rotation period is approximately 2 orders of magnitude smaller than the RGB core rotation periods measured by \cite{Mosser_2012}.  Such rapid rotation could be generated by a stellar merger on the RGB, if some of the orbital angular momentum is deposited deep in the core of the red giant where $\nu_{\rm max} < \nu_K$. It is not clear whether this can commonly occur. (***) estimates that mergers while on the lower RGB only occur in $\lesssim 5 \%$ of low mass stars, and thus the rotational explanation has difficulty explaining the larger rates of mode suppression found by \cite{Mosser_2011}. Post-merger RGB stars will likely be rapidly rotating, and thus we may expect that suppressed dipole pulsators should always be rapidly rotating. Although many suppressed dipole pulsators are rapidly rotating (Stello et al. 2015), many are not. In particular, KIC 8561221 (\cite{Garc_a_2014}) (\cite{Garcia_2014})  is slowly rotating. It is unlikely that rapid core rotation can account for all the suppressed pulsators. Rapid core rotation would also require a large amount of differential rotation to exist within the star. Although angular momentum transport is not well understood, the slow rotation rates observed in the cores of many RGB stars (\cite{Mosser_2012,Beck_2011,Deheuvels_2014}) suggests that such large degrees of differential rotation are difficult to sustain as a star evolves up the RGB.