Evolution of the surface and core rotation rates (solid and dashed lines respectively) as a function of the stellar radius that increases with time (MS, subgiant, and RGB correspond respectively to Reff/R⊙ between ∼1.0 and 1.8, 1.8 and 3, and higher than 3). We show theoretical predictions for two 1.25 M⊙ models at solar metallicity computed with the prescription for Dh = Dh,h by Mathis et al. (2004; black) and the new prescription including both components of Dh = Dh,v + Dh,h for the case τ = 1/S (green). We compare the model predictions with relevant data for stars with asteroseismic masses between 1.1 and 1.4 M⊙. For SGB stars we show surface and core rotation rates (black and orange dots) derived by Deheuvels et al. (2014). For RGB stars, we plot the core rotation rates derived by Mosser et al. (2012; red dots).
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