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The differential migration of two planets due to planet-disk interaction canresult in capture into the 2:1 eccentricity-type mean-motion resonances. Boththe sequence of 2:1 eccentricity resonances that the system is driven throughby continued migration and the possibility of a subsequent capture into the 4:2inclination resonances are sensitive to the migration rate within the rangeexpected for type II migration. If the migration rate is fast, the resonantpair can evolve into a family of 2:1 eccentricity resonances different fromthose found by Lee (2004). This new family has outer orbital eccentricity e_2 >0.4-0.5, asymmetric librations of both eccentricity resonance variables, andorbits that intersect if they are exactly coplanar. Although this family existsfor an inner-to-outer planet mass ratio m_1/m_2 > 0.2, it is possible to evolveinto this family by fast migration only for m_1/m_2 > 2. Thommes and Lissauer(2003) have found that a capture into the 4:2 inclination resonances ispossible only for m_1/m_2 < 2. We show that this capture is also possible form_1/m_2 > 2 if the migration rate is slightly slower than that adopted byThommes and Lissauer. There is significant theoretical uncertainty in both thesign and the magnitude of the net effect of planet-disk interaction on theorbital eccentricity of a planet. If the eccentricity is damped on a timescalecomparable to or shorter than the migration timescale, e_2 may not be able toreach the values needed to enter either the new 2:1 eccentricity resonances orthe 4:2 inclination resonances. Thus, if future observations of extrasolarplanetary systems were to reveal certain combinations of mass ratio andresonant configuration, they would place a constraint on the strength ofeccentricity damping during migration, as well as on the migration rate itself.

Planetary Migration and Eccentricity and Inclination Resonances in Extrasolar Planetary Systems