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Fig. 3


Planetesimal disk masses within 1 au, 10 au, and the complete disk for three different analytic density slopes and the dynamically formed planetesimal mass. The analytic masses are given at the start of the simulation, while the dynamically formed disk masses are shown after one million years, after most planetesimals have already formed. The dynamic runs do not contain a planetary embryo, they only simulate the disk evolution. The disk parameters, however, are the same as in the population in Fig. 5. We show the mass in planetesimals in the whole disk in the upper panel, the planetesimal mass within 10 au in the middle panel, the planetesimal mass within 1 au in the lower panel, and the corresponding median masses for every setup.

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