deletions | additions       diff --git a/figures/Mosser_comparison/caption.tex b/figures/Mosser_comparison/caption.tex  index db988e3..53037b2 100644  --- a/figures/Mosser_comparison/caption.tex  +++ b/figures/Mosser_comparison/caption.tex 
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Evolution of the average core rotational period as a  function of stellar radius for different assumptions of angular momentum transport in a 1.5$\mso$ model initially rotating at 50$\kms$. We show models without angular momentum transport (green), including transport of angular momentum due to rotational instabilities (purple) and accounting for magnetic torques in radiative regions (red, Spruit-Tayler Tayler-Spruit  magnetic fields). The star symbols indicate the locations of $\KIC$ and $\KID$ as derived using the maximum observed splitting of its their  mixed modes \citep{Beck:2012} and Beck et al. 2014 (arXiv). \citep{Beck:2012,Beck:2014}.  Dashed lines indicate a linear fit to the different curves during the early RGB. The vertical dotted line shows the location of H-core exhaustion. The red dotted line shows the evolution of core rotational period for a model where the resulting Spruit-Tayler Tayler-Spruit  diffusion coefficient has been multiplied by a factor of 100. Stars in the red giant sample of \citet{Mosser:2012} with $R<7.5\rso$ are shown as black dots.  The best fit to the core rotation of thered giants sample of  \citet{Mosser:2012} sample  is also  shown as a dashed blue line (and gray area). line.  \label{period}