Comparison of the cumulative and surface mass-loss profile as predicted by the XPE model by Picogna et al. (2019) to the purely viscous accretion rate onto the star. Top panel: viscous accretion rate at 1 au of the Σ₀ = 10 g cm^‒2 and Σ₀ = 100 g cm^‒2 discs as a function of time (black lines, cf. Eq. (35) in Hartmann et al. 1998) vs. the wind mass-loss rates due to photoevaporation for log₁₀(L_x∕erg s^‒1) = 29.54 and log₁₀(L_x∕erg s^‒1) = 30.04 (orange lines, cf. Eq. (A.3)). Bottom panel: surface mass-loss profiles as a function of disc radius. The dashed line shows the full contribution of the primordial surface mass-loss profile, which is active before gap opening (Eq. (A.1)). Assuming that photoevaporation has already opened a gap in the disc, with its outer radius R_hole lying at 10 au, and the column density of the inner disc being less than N_H = 2.5 × 10²² cm⁻², the actual profile that is active is shown as the black solid line.