deletions | additions       diff --git a/Early RGB.tex b/Early RGB.tex  index 5a9860c..3f25764 100644  --- a/Early RGB.tex  +++ b/Early RGB.tex 
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We recall that, while the physics of the Tayler instability is solid, the existence of the Tayler-Spruit dynamo loop is currently debated on both analytical and numerical grounds \citep{Braithwaite:2006,Zahn:2007}. However observations of the spin rates of compact objects (WD and NS) are in much better agreement with models including this angular momentum transport mechanism \citep{Heger:2005,larends_Yoon_Heger_Herwig_2008}, which has also been discussed in the context of the rigid rotation of the solar core \citep{Eggenberger:2005}, but see also \citet{Denissenkov:2010}.  Finally we checked if an artificial constant diffusivity $\nu$ could explain the observations. We confirm the results of \citet{Eggenberger:2012}: in our $1.5\mso$ model initially rotating with $50\kms$  a diffusivity of $\nu=6\times10^4\cms$ allows to match the observed splittings of \KIC. However not only such constant diffusivity is unphysical, it fails to explain the later evolution and the observations of rotation rates in clump stars and WD (see Sec.~\ref{clump}). We conclude that on the early RGB of low-mass stars none of the angular momentum transport mechanisms usually included in stellar evolution codes can produce enough coupling to explain the asteroseismic derived core spin rates.