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Matteo Cantiello edited figures/Mosser_comparison/caption.tex about 10 years ago

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Replace this text with your caption Evolution of the average core rotational period as 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 magnetic fields). The star symbols indicate the locations of $\KIC$ and $\KID$ as derived using the maximum observed splitting of its mixed modes \citep{Beck:2012} and Beck et al. 2014 (arXiv). 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 diffusion coefficient has been multiplied by a factor of 100. The best fit to the core rotation of the red giants sample of \citet{Mosser:2012} is shown as a dashed blue line (and gray area). \label{period}