Initial conditions for the disc around the 1 M_⊙ star used in our simulations (blue). These are compared to the initial conditions of the disc in Bae et al. (2019) (green) in which the PDS70 system (0.85 M_⊙ star) was modelled. For context, the surface density of the minimum mass solar nebula (MMSN; Hayashi 1981) is plotted in orange. Physical initial conditions after the equilibration phase (see Fig. 2) at t = 26 kyr are shown for model M9-3 as a dashed blue line. The panels, from top to bottom, show the radial profile of the: surface density, viscous mass accretion rate (Ṁ_disc = 3πΣν with α = 10⁻³), temperature, and aspect ratio. The initial location of the planets are marked by the vertical, dotted lines which span over all panels and are indicated by the red and cyan circles.