deletions | additions       diff --git a/KIC8366239.tex b/KIC8366239.tex  index 25b952e..c10ce2a 100644  --- a/KIC8366239.tex  +++ b/KIC8366239.tex 
...
\subsection{The red giant KIC 8366239}  We have chosen to model the red giant $\KIC$, for which \citet{Beck:2012} have observed a minimum rotational splitting of mixed modes of $\delta\nu_{n,\ell} = 0.135\pm0.008 \mu$Hz, arising from a p-dominated mode (mostly probing the slowly rotating stellar envelope). On the other hand the observed maximum values for the g-dominated mixed modes (mostly living in the stellar core) is on the order $0.2\mu$Hz. This confirmed the theoretical expectation that the core of this red giant is rotating faster than its envelope. However the inferred ratio is not very large, implying a ratio of order 10 in the rotation rate between core and envelope ($\Omega_{C}/\Omega_{E}$). This is at odd with the expectations coming from models that only include transport of angular momentum from rotational instabilities and circulations, predicting a ratio $\Omega_{C}/\Omega_{E} \ga 10^3$ for this object   \citep[][ this work]{Eggenberger:2012} assuming typical initial rotational velocities\footnote{Models with very slow initial rotation ($1\kms$) can not reproduce the observation either}. Similar to \citet{Eggenberger:2012} we adopt an initial mass of $1.5\mso$ and calculate models assuming different physics for angular momentum transport. We select the background structure of the different calculations by matching the global asteroseismic properties of $\KIC$ (the frequency of maximum oscillation power, $\nu_{\rm max}$, and the large frequency separation $\Delta \nu$). These are then used in ADIPLS to calculate the splitting of mixed modes for the different assumptions on the angular momentum transport mechanisms at work.   Our calculations confirm the results of \citet{Eggenberger:2012}. Models that only include angular momentum transport due to rotational instabilities and circulations fail to reproduce the observed splittings. The resulting cores are so rapidly rotating that the perturbative approach to the splitting calculation is no more justified. This said, even models with an extremely slow initial rotation of $1 \kms$ result in rotational splittings 1 order of magnitude larger than the observed ones. This is in perfect agreement with the calculations of \citet{Eggenberger:2012}, even if the implementation of the physics of rotation is quite different in the GENEVA code compared to MESA \citep[See Sec.6 in ][]{Paxton:2013}. ][and references therein]{Paxton:2013}.