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Orbits of known extrasolar planets that are located outside the tidalcircularization regions of their parent stars are often substantiallyeccentric. By contrast, planetary orbits in our Solar System are approximatelycircular, reflecting planet formation within a nearly axisymmetric, circumsolardisk. We propose that orbital eccentricities may be generated by divergentorbital migration of two planets in a viscously accreting circumstellar disk.The migration is divergent in the sense that the ratio of the orbital period ofthe outer planet to that of the inner planet grows. As the period ratiodiverges, the planets traverse, but are not captured into, a series ofmean-motion resonances that amplify their orbital eccentricities in roughinverse proportion to their masses. Strong viscosity gradients inprotoplanetary disks offer a way to reconcile the circular orbits of SolarSystem gas giants with the eccentric orbits of currently known extrasolarplanets.Comment: Final revised version, accepted by ApJ Letters. Includes discussion  from the community at larg

Excitation of Orbital Eccentricities of Extrasolar Planets by Repeated Resonance Crossings