Effect of Wind-Driven Accretion on Planetary Migration

Can wind-driven accretion modify planetary migration? Planetary migration plays an important role in planet formation models and statistics of observed exoplanets.<br> So far, the theory of planetary migration has focused on the interaction of one or more planets with an inviscid or viscously evolving gaseous disk. Wind-driven accretion, however, additionally influences the gas evolution in a protoplanetary disk and might therefore have an impact on the orbital parameters of a planet within the disk In 2D hydrodynamic simulations, we establish a simplified model of wind-driven accretion in protoplanetary disks treating the wind not explicitly but as a torque on the gas caused by the wind.With this simplified model we investigate the main effects with different wind strengths in a qualitative way rather than quantitatively predicting the outcome. We find that for the co-orbital region, this wind-driven process always injects mass from the outer edge of the co-orbital region and removes mass from the inner edge, in contrast to the viscous evolution, where mass is injected or removed from the co-orbital region depending on the radial density gradients in the disk.<br> As a consequence, the migration behavior can differ strongly, and can under certain conditions drive rapid type-III-like outward migration.

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