Abstract
The evolution of the orbital eccentricity of a planet due to tidal interaction with a protoplanetary disk is modeled. It is found that the eccentricity of the planet tends to increase when the mass of the planet is large enough to make a gap in the disk, i.e., is larger than about a Saturn mass. The tidal interaction with the protoplanetary disk explains the high eccentricities of the extra-solar planets.
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