deletions | additions       diff --git a/Introduction.tex b/Introduction.tex  index 35363d3..3448f21 100644  --- a/Introduction.tex  +++ b/Introduction.tex 
...
It is clear that the next step is testing if models including transport of angular momentum due to Tayler-Spruit magnetic fields can explain the asteroseismic observations. We compare our results with asteroseismic observations of mixed modes splitting in the red giant star KIC 8366239. We further compare predicted core rotation rates with observations of stars during core He-burning and in the WD stage.  We show that it is difficult, even in the presence of magnetic torques due to Tayler-Spruit magnetic fields, to fully account for the evolution of the core rotation rate from the end of the main sequence to the WD stage. We also show that a constant diffusivity, as discussed in \citet{Eggenberger:2012}, can not explain the full  core angular momentum evolution past the red giant branch. core H exhaustion.  % Effect of Rotation  % This impacts observable properties of the star, as well as its evolution. Surface rotation can be measured using spectroscopic observations or from %the modulation of surface features (e.g. stellar spots). Beneath the surface rotational instabilities and circulations do not only transport angular %momentum, but can also lead to compositional mixing. Surface abundances can therefore change already during the main sequence of a rotating star %\citep{Meynet2000,Maeder2012}.