Bottom panel: evolution of the angular velocity as a function of time for models computed with the prescriptions for Dh from Mathis et al. (2004), Zahn (1992), and that of the present paper with the three different characteristic time scales for turbulence (black, red, green (τ = 1/S), blue (τ = 1/(2Ω + S)) and magenta (τ = 1/NΩ), respectively). Scaled on the left is the rotational period in days and on the right the angular velocity in solar units with Ω⊙ = 2.86 × 10−6 s−1. Each cross represents a star belonging to an open cluster which age and mass (between 1.4 and 1.6 M⊙) have been taken from literature. All observational data are taken from Gallet & Bouvier (2015) and Bouvier et al. (2014) and references therein. The solid lines show the evolution of the surface rotation, and dashed lines the evolution of the mean radiative core rotation rate. Top panel: evolution of the normalised core to surface differential rotation rate for the six 1.0 M⊙, Z⊙ models as colour-coded in Fig. 2.
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