deletions | additions       diff --git a/Introduction.tex b/Introduction.tex  index 2b7e06e..b84abe3 100644  --- a/Introduction.tex  +++ b/Introduction.tex 
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While the physics of the Tayler instability is secure, the existence of the Tayler-Spruit dynamo loop is 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}.  In Sec.~\ref{stev} we present the stellar evolution calculations and the details of the implemented physics.   Results for the evolution of core rotation during the early RGB are shown in Sec.~\ref{earlyrgb} for different angular momentum transport mechanisms. Results are compared to \Kepler \textit{Kepler}  asteroseismic observations of mixed modes in red giants. In Sec.~\ref{splittings} we show how the rotational splittings of mixed mode are calculated from the stellar evolution models using \ADIPLS. Sec.~\ref{beyond} presents the angular momentum evolution of our models beyond the early RGB. Predictions for the core rotation rates past the luminosity bump (Sec.~\ref{bump}), during core He-burning (Sec.~\ref{clump}) and in the WD stage (Sec.~\ref{wd}) are shown and compared to the asteroseismically derived values.   %In particular we begin showing models including different physics of angular momentum transport to explain the %rotational splittings observed in the red giant star KIC 8366239 \citep{Beck:2012}.