a) Distribution of initial secondary mass in binaries that lead to the formation of a CEMP star. b) Distribution of initial period of binaries that form CEMP stars. Angular momentum variations are calculated with the spherically simmetric wind assumption (Eq. (4)). The 0.1 dex bins are equally spaced in M₂/M_⊙ (left panel) or log ₁₀(P /days) (right panel). c) and d) As in a) and b), we use γ = 2 in Eq. (10) to compute angular momentum loss. Model sets C_q and E_q (dot-dashed lines) are the result of q-dependent WRLOF defined by Eq. (9). Model sets C and E (dotted lines) are the result of q-independent WRLOF. The solid lines show our default model set A.