Time evolution of the gas surface density profiles (top panels) and of the mass accretion and photoevaporation mass-loss rates (bottom panels) for massive discs around stars with masses between 2.5 M_⊙ (left panel), 3 M_⊙ (middle panel), and 4.0 M_⊙ (right panel) with α₀ = 10⁻³. In this case, the X-ray photoevaporation rate for primordial discs has been computed by directly using Eqs. (B1)–(B3) from Appendix B in Owen et al. (2012). As in Figs. 1–3, the short dashed blue and lilac curves represent the mass-loss rates but integrated along the disc domain. For comparison we also plotted the mass accretion and photoevaporation mass-loss rates (represented by the long dashed red, blue, and lilac curves) computed by considering the X-ray photoevaporation rate for primordial discs, as in K21. Our general result seems to be a direct consequence of considering the effects of stellar evolution on disc evolution as they are apparently independent of the details of modelling X-ray photoevaporation. We still predict homogeneous, revenant, and outside-in evolution, with the only difference being that the transitions from one case to the next shift to larger stellar masses.