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Fig. 5

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Position of V390 Aur in the H-R diagram. The adopted effective temperature is determined from our analysis of the Stokes I spectra of V390 Aur. The luminosity is estimated using the parallax from the New Reduction Hipparcos catalogue by van Leeuwen (2007; see text for more details). Standard evolutionary tracks (solid lines) computed for [Fe/H]  = 0 are shown up to the RGB tip for different labelled stellar masses. For the 2.25   M case, the predictions for models with rotation-induced mixing treated as in Charbonnel & Lagarde (2010) are also shown for two initial rotation velocities of 50 and 110 km   s-1 (dotted lines). The dashed lines delimit the first dredge-up, the cooler line marking the deepest penetration of the convective envelope. The dashed-dotted line indicates the beginning of central He-burning for the mass range covered by the tracks.

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