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Fig. 1


Change of the eccentricity of a one Jupiter mass planet as function of time for the different damping parameters. The K damping values are derived using the classical type-II migration timescales. The flattening of the damping at the end of the disc lifetime is due to the exponential decay of the gas disc surface in the last 100 kyr, which reduces the gas surface density and thus the damping effects.

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