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Matteo Cantiello edited figures/j_evol_1.5_50_tams_to_wd/caption.tex over 10 years ago

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Replace this text Evolution of the average core rotational period as function of logarithmic time to the end of 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 your caption 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). Luminosity and surface rotational velocity are shown as dashed blue and green lines respectively. 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 $\log\lsun\sim-2$. The star symbol indicates the location of $\KIC$ as derived using the maximum observed splitting of its mixed modes \citep{Beck: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. \label{period_evolution}