Fig. 10.
Ratio of the flux of the primary to the secondary in the V band, FV, pri/FV, sec, as a function of the temperature of the primary star during the main BSG stage of the primary (before mass transfer takes place). The values were computed for our MESA models with initial primary masses of 12, 15, 20 and 30 M⊙, log(P/days) = 3.0 and mass ratio q = 0.9.
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