Fig. 11

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Maximum mass that can be accreted through planetesimals for a planet that finishes its migration at a distance of 0.02 AU. The x-axis shows the minimum initial orbital distance where the planet starts its migration and the y-axis shows the maximum possible accreted mass in the form of planetesimals. The vertical lines show the different ice lines in the disk. The vertical dashed lines show the distances where a planet with one and five Jupiter masses can initiate its migration in order to have a supersolar metallicity. The horizontal dashed lines show the amount of planetesimal mass that a planet can accrete by initiating its migration at the indicated distances.
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