Fig. 9.
Change in B − V colour due to presence of secondary as a function of the effective temperature of the primary star during the first 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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