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Fig. 8


Final planetary masses (left) and final water ice content (right) of the planets formed in our simulations as function of the planetary starting position r0 and starting time in the disc t0 around a star with [Fe/H] = 0.0. Yellow lines indicate the final planetary positions in AU after 5 Myr and black lines mark the final planetary masses in Earth masses. Green lines in the right panel mark the ice lines of H2O, CO2, CH4 and CO. Planets forming very early in the disc migrate all the way down to 0.1 AU. The majority of planets are trapped in the region of outward migration until the end of the disc’s lifetime. The decrease in the water ice fraction at large initial distances is caused by the accretion of CO2, CH4, and CO intothe planet, which reduces the relative water ice fraction of the planet, but increases the total ice fraction of the planet.

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