Open Access

Fig. C.1


Final water ice content of planets formed with initial position r0 and around stars with metallicity of [Fe/H] in either non-involving discs with only inward migration (top), evolving discs with only inward migration (middle), and evolving discs with inward and outward migration (bottom). Planets are injected at t0 = 0.5 Myr. The black and yellow lines respectively mark the final orbital position (0.1, 0.3, 0.5 and 1.0 AU) and masses of the planets. In the simulations presented in the top two panels, nearly all planets migrate to the inner edge at 0.1 AU. Green vertical lines depict the H2O and CO2 ice lines at the beginning of the simulations. H2O and CO2 are in icy form exterior to these ice lines. Due to the disc’s evolution in time (middle and bottom), the water ice line moves inwards, so that the water ice line can sweep over slow growing planets initially interior to the water ice line allowing them to have a water ice contribution.

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