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The planet migration due to the disk--planet interaction is one of the mostimportant processes to determine the architecture of planetary systems. Asufficiently massive planet forms a density gap and migrates together with thegap. By carrying out two-dimensional and two-fluid (gas and dust grains)hydrodynamic simulations, we investigated the effects of the dust feedback onthe migration of the gap-opening planet, which was not considered in previousstudies. We found that the gas surface density at the outer edge of the gapbecomes smaller due to the dust feedback, and thus the torque exerted from theouter disk decreases. This mechanism becomes effective as the gap becomes widerand deeper. In particular, when the mass of the planet is Jupiter-size andturbulent viscosity is $\alpha = 3\times 10^{-4}$, the planet can migrateoutward due to the reduction of the torque exerted from the outer disk. Evenfor a smaller planet, the migration becomes significantly slow down. Thistermination of the inward migration triggered by the dust feedback may explainwhy ring and gap structures can be frequently observed within theprotoplanetary disks.

Termination of an inward migration of a gap-opening planet triggered by dust feedback