deletions | additions       diff --git a/figures/prot/caption.tex b/figures/prot/caption.tex  index 88fccbe..6991eb3 100644  --- a/figures/prot/caption.tex  +++ b/figures/prot/caption.tex 
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Evolution of the average core rotational period as a function of logarithmic time to the end of the calculation (WD cooling sequence). The black and red solid lines show the surface and core rotational periods for our 1.5$\mso$ model rotating with an initial surface velocity of about 50$\kms$ and including angular momentum transport due to Tayler-Spruit magnetic fields in radiative regions (together with transport due to rotational instabilities). The plot shows evolution from the end of H-core burning (terminal age main sequence, TAMS) to the cooling WD sequence (when the luminosity decreases below $\log L/\lso \sim$ −2). The star symbols indicate the location of $\KIC$ and $\KID$ as derived using the maximum observed splitting of their mixed modes, the blue dashed line shows the fit to the core rotation data of early red giants in \citet{Mosser:2012} . \citet{Mosser:2012}.  Grey regions show the range of the inferred core rotation rates for the clump stars of \citet{Mosser:2012} and for ZZ Ceti stars \textbf{(Refs required)}. the typical rotation rate of non magnetic WD \citep[see e.g.][]{Koester:1998,Ferrario:2005,Corsico:2011,Greiss:2014}.  The dotted line shows a model with an imposed core rotation of 30 d on the clump evolving with no angular momentum transport ($j$-conservation) into a WD. \label{period_evolution}