Time evolution of M_d–M_* (left) and $\dot{M}-M_{\star }$ (right) in the pure wind model (ω ≠ 0). This plot is obtained with disc population synthesis modelling, without any spread in the initial conditions. Each dot represents a disc in the population at different ages as shown in the colour bar. The initial power-law correlation, shown in light blue, is lost as early as ~1 Myr (corresponding to ~2 < t_acc,0 > with these parameters) due to a downward bending corresponding to lower stellar masses. In this simulation, we have used N = 100 discs, α_DW = 10⁻³, λ = 3, ω = 0.25, λ_m,0 = 2.1, λ_acc,0 = 1.5. The set of MHD parameters is based on Tabone et al. (2022a).