Fig. 5.
Top: Hertzsprung-Russell diagram, showing the location of the best-fit FASTWIND models (FW) and highest likelihood evolutionary models from Brott et al. (2011; BONNSAI). Overplotted are evolutionary tracks for different masses and initial rotation velocities (grey lines), along with isochrones for the 100 km s−1 initial rotation velocity models (blue lines). Bottom: Kiel diagram with an equivalent legend as the HRD above. Using the scaled CNO abundances does not appreciably move the model of the primary in either diagram.
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