Fig. B.1

Disc temperature as a function of orbital distance and vertical distance to the midplane for the disc that features α = 5 × 10−3, a water abundance of 50%, a solid-to-gas ratio of 1%, and a transition in the dust fragmentation velocity from 1 to 5 m s−1 (Fig. 3). The ice line is indicated as a grey line. The disc is vertically isothermal in the outer regions (not shown), where stellar irradiation dominates over viscous heating.
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