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Fig. 8


Position of the stars in the Hertzsprung–Russell diagram (upper panels) and in the Kiel log g– logTeff diagram (lower panels). Squares and circles stand for the components of HD 17505Aa and HD 206267Aa, respectively. The filled (resp. empty) symbols correspond to the primary (resp. secondary) star. In the left panels, evolutionary tracks for single massive stars at solar metallicity and initially rotating at 0.4 × vcrit from Ekström et al. (2012) are overplotted. The dashed red lines correspond to isochrones of 1.0, 3.2, and 5.0 Myr. The right panels illustrate comparison with evolutionary tracks from Brott et al. (2011). The solid lines yield tracks with initial rotational velocities near to 100 km s−1 (112, 111, 110, 109, and 109 km s−1 for the 15, 20, 25, 30, and 35 M models) whilst the dashed tracks correspond to initial rotational velocities near to 200 km s−1 (216, 214, and 213 km s−1 for the 35, 40, and 50 M models).

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