Donor star radius (R₂) as a function of its mass (M₂) according to Knigge et al. (2011) (dashed red line) compared to the evolution predicted by MESA for a CV with initial M₁ = 0.9 M_⊙ and M₂ = 0.85 M_⊙ and assuming magnetic wind braking as in CG18b (solid black line). The radii and masses of CV donors derived from observations (McAllister et al. 2019) are shown as blue dots with their respective error bars. It is clear that the prescription based on the complexity of the field fails to reproduce the observations.