deletions | additions       diff --git a/Clump.tex b/Clump.tex  index d425b8e..0ddf95f 100644  --- a/Clump.tex  +++ b/Clump.tex 
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\end{enumerate}  After this rapid initial phase, the core rotation rate remains fairly constant during the duration of core He burning.   The clump stars in the \citet{Mosser:2012} sample rotate fairly slowly, with periods in the range $P_{\rm c} \sim 30-240$ d. Similar to the case of the early RGB, these values are about 1 order of magnitude above the predictions of our models including magnetic torques, again pointing toward the requirement for some extra angular momentum transport occurring in previous evolutionary phases.  Note that models including an artificial diffusivity able to reproduce the observed splitting on the early RGB ($\eta ($\nu  \sim 10^4-10^5 \cms$) fail to explain the rotation rates of clump stars, with predicted rotation rates almost two orders of magnitude higher than the observations. This is because the torque required to couple core and envelope increases as the star climbs the RGB, while the artificial diffusivity $\eta$ $\nu$  stays constant. We noted that a combination of an artificial viscosity $\eta $\nu  \sim 10^4-10^5 \cms$ with the Spruit-Tayler magnetic torques can reproduce both the early RGB and the clump observations. %%%%%%%%%%%%%%%%% CHECK PLOT %%%%%%%%%%%%%