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Fig. 7


Eccentricity as a function of semi-major axis of simulated planetary systems with different damping rates anddifferent number of initial embryos (15, 30, 60 from top to bottom). We only show the planets with masses of at least 0.5 Jupiter masses (for simulations and observations) and only for the K values that match the observations of the eccentricity distribution best (Fig. 6). The horizontal lines depict the mean eccentricity within each radial bin. The black symbols show the data from with planetary masses ranging from 0.5 to 1.25 Jupiter masses, which is roughly the masses the planets in our simulations reach.

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