Example of a M_1,  i = 10.2 M_⊙, q_i = 0.9, and a_i = 39.2 R_⊙ binary star model in which non-conservative mass transfer occurs and for which the non-accreted matter cannot be driven to infinity. Panel a is the same as Fig. 3a (‘ign.’ = ‘ignition’ and ‘exh.’ = ‘exhaustion’). In panel b, the mass-loss rate of the secondary (solid black line) is compared to the maximum mass-loss rate Ṁ_max (dashed lines; pink for f_eff = 1.0, green for f_eff = 0.1) set by Eq. (8). The surface rotation rates (solid blue and orange lines) and mass transfer efficiency (dashed black line) are shown in panel c as a function of the primary mass.