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The outward migration of a pair of resonant-orbit planets, driven by tidalinteractions with a gas-dominated disk, is studied in the context of evolvedsolar nebula models. The planets' masses, M1 and M2, correspond to those ofJupiter and Saturn. Hydrodynamical calculations in two and three dimensions areused to quantify the migration rates and analyze the conditions under which theoutward migration mechanism may operate. The planets are taken to be fullyformed after 1e6 and before 3e6 years. The orbital evolution of the planets inan evolving disk is then calculated until the disk's gas is completelydissipated. Orbital locking in the 3:2 mean motion resonance may lead tooutward migration under appropriate conditions of disk viscosity andtemperature. However, resonance locking does not necessarily result in outwardmigration. This is the case, for example, if convergent migration leads tolocking in the 2:1 mean motion resonance, as post-formation disk conditionsseem to suggest. Accretion of gas on the planets may deactivate the outwardmigration mechanism by raising the mass ratio M2/M1 and/or by reducing theaccretion rate toward the star, hence depleting the inner disk. For migratingplanets locked in the 3:2 mean motion resonance, there are stalling radii thatdepend on disk viscosity and on stellar irradiation, when it determines thedisk's thermal balance. Planets locked in the 3:2 orbital resonance that startmoving outward from within 1-2 AU may reach beyond 5 AU only under favorableconditions. However, within the explored space of disk parameters, only a smallfraction - less than a few per cent - of the models predict that the interiorplanet reaches beyond 4 AU.

Outward Migration of Jupiter and Saturn in Evolved Gaseous Disks