Top: vertical temperature profile of the RMHD run (black line) and the viscous RHD runs (green lines) for the high-resolution models at 1 AU. Model H2D uses a constant alpha. Model H2D^∗ uses a vertical dependence of α ~ 1/ρ which is more similar to the RMHD run. Bottom: relative temperature profile compared to the initial passive disc, for models H2D^∗ and H3D. On both panels, the background colour shows the region of the disc where the gas is optically thin to its own thermal radiation and to the irradiation by the star. The grey background colour shows the region where the gas is optically thick to its own radiation. We note that there is also a small region in the disc where the gas is optically thin to its own radiation but still optically thick for the irradiation by the star.