Young low-mass planets embedded in their natal disks have complex interactions with their surrounding material. Canonical models of planet-disk interactions typically predict that planets migrate inward in the Type I regime and eventually engulfed by the central star. Since the solid material (dust or pebbles) is only 1% of the disk mass, its effect on planetary migration is usually neglected. In my talk, I will show that the disk's solid material can play an important role in planetary migration, so its dynamical effects must be taken into account. The highly asymmetric distribution of solid material formed in the vicinity of terrestrial planets can generate even larger torques than the gaseous material of the disk. In our numerical hydrodynamic simulations, we found pebble accreting Earth-mass planets migrating outward. We conclude that high metallicity favors planet formation by inhibiting stellar engulfment of young planets.

recording: www.youtube.com/watch