Comparison between the observed orbital period distributions for different mass bins (El-Badry et al. 2022) and the predicted assuming K = 50 and several values of η. The line types and colours indicate the assumed value of η, while each panel corresponds to a different primary mass bin, being 0.10 − 0.30 M_⊙ (top left panel), 0.30 − 0.40 M_⊙ (top right panel), 0.40 − 0.65 M_⊙ (bottom left panel), and 0.65 − 0.90 M_⊙ (bottom right panel). It is clear from the figure, especially when the binaries host only fully convective stars (top left panel), that the strength of magnetic braking does not strongly contribute to shape the distributions. On the other hand, the orbital period distribution of main-sequence binaries is strongly affected by how the magnetic braking torque depends on the star spins as shown by El-Badry et al. (2022).