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Fig. 1


Comparison between the results of B15b (thin lines) and our results (thick lines). The lines starting vertically are the formation tracks of planets starting at 5, 10, 15, 25, 40, and 50 AU. The orange lines are the surface density of pebbles at 2 Myr in the two models. As in B15b, the planets are assumed to start their formation at 2 Myr.

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