Temperature as a function of initial orbital distance r₀ and initial time t₀ (top) and the pebble isolation mass as a function of initial orbital distance r₀ and time t₀ (bottom) for the Bitsch et al. (2015a) disc model. The black lines indicate the ice lines of FeS, Fe₃ O₄, H₂ O, NH₃ and CO₂, where the numbers mark their condensation temperatures, see Table 1. The temperature initially decreases very fast due to the decrease of viscous heating. This inturn reduces the pebble isolation mass in the inner disc. As the outer disc (r > 6 AU) is dominated by stellar irradiation, the aspect ratio and thus the pebble isolation mass remain large.