Exemplary disc evolution shown for initial conditions: M_disc = 0.1 M_⋆ with M_⋆ = 0.25 M_⊙, R_in = 0.04 AU and ℱ_FUV = 10 G₀. We show temporal evolution of the surface density, radial mass flow rate and rate of change in surface density due to outflows (i.e. magnetic disc winds, internal- and external photoevaporation) for all disc wind scenarios. The individual contributions can be distinguished roughly when considering the outflows . External photoevaporation corresponds to the outermost peak while internal photoevaporation acts at ~ 0.3 AU to a few AU. MHD winds remove mass from the whole disc and increase in strength towards the inner disc. Dotted lines show the evolution at 10⁴ yr, dashed lines at 5 × 10⁴ yr. Coloured lines are spaced by 10⁵ yr.