Grid of computed systems. Left panel: models of binaries with initial mass ratios, q₀ = M_2, 0/M_1, 0 = 0.6, 0,8, 0.9 in the “ZAMS mass of the primary component, M_1, 0 – initial orbital period, P_orb, 0” plane. Color-coded are the masses of the remnants of primary components of the binaries after RLOF at the point of the lowest luminosity along the post-mass-exchange evolutionary track, obtained by a numerical approximation of the results of the computation of a non-regular grid of models. The legend over the upper panel shows the evolutionary “fate” of the computed binaries. Open squares and circles indicate the formation of HeS stars (in the latter case, with retained H/He envelopes exceeding 0.3 M_⊙). The diamonds show binaries entering common envelopes. Open triangles stand for binaries where case C mass transfer occurred. In the light gray region at the top left of the middle and lower panels, the models for q₀ = 0.9, 0.8 were not computed, since binaries in this region definitely experience case C mass transfer and form common envelopes, or the T_eff of the stripped component never exceeds 25 000 K. Crosses mark the systems forming He WDs. The “pixels” overplotted by dots show the locations of the progenitors of stripped helium remnants with masses < 1 M_⊙. Right panel: color-coded masses of H/He envelopes retained by the remnants of the initial primary components shown in the left panel at L_min along their tracks (with steps 0.01 M_⊙ and 0.1 M_⊙ below and above M_env = 0.1 M_⊙ respectively). All masses are in M_⊙.