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the splitting of mixed modes \citep[See also][]{2013A&A...549A..74M}. This measurement   of the interior rotational state of an evolved star provides a new test for   theoretical ideas of angular momentum transport.  Similarly to the case of compact remnants, models solely including $j$-transport due to rotational mixing and circulations can not reproduce the observed splittings \citep{Eggenberger:2012,Marques:2013,Ceillier:2013}, and predict rotation rates 2 to 3 orders of magnitude above the observations. While the adopted treatment of angular momentum transport is approximated and rely on a number of assumptions, \citet{Marques:2013} have shown that even pushing to the limit of the allowed parameter space one can not reproduce the observed values. They claim that ``the seismology of red-giant stars emphasize that an additional mechanism, mechanism  is needed to achieve a slower core rotation of red-giant stars''. The immediate step is testing if models including transport due to TS magnetic fields can explain the asteroseismic observations.  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}.