Disc evolution for a viscous disc with internal photoevaporation due to X-rays, but with mass loss rates reduced by a factor of 3-4. For the exact values, see Table 2. The reduced rates result in later gap opening and therefore longer disc lifetimes. Host star masses vary from 0.5 M_⊙ (on the left) to 0.1 M_⊙ (on the right). Top: gas surface density as a function of disc radius and time. Bottom: gaseous C/O ratio as a function of disc radius and time. Colour coding, plotting, and simulation parameters are indicated as in Figure 3.