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Fig. 12

image

Eccentricity–semi-major axis distribution of the observed giant planets (black triangles) with masses of 0.5 < MP < 5.0MJ and our simulations with different K-damping values (coloured circles) after 100 Myr of evolution. The horizontal lines show the mean eccentricity within each orbital distance bin. While our simulations with low K reproduce the ea distribution exterior to 1 AU, the simulations show too small eccentricities for the planets interior to 1 AU. On the other hand, this might also be related to the limited number of giant planets within this region in our simulations. For planets in the order of Jupiter mass, the low K values match quite nicely (Fig. 7), due to the slightly larger number of planets within that semi-major axis bin in our simulations.

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