Dust evolution in protoplanetary disks with a pair of planets in orbital resonance
Abstract
A significant fraction of extra-solar multi-planet systems are populated by planet pairs whose orbits are in, or in proximity of, mean-motion resonances. The 2:1 and 3:2 ratios are particularly common. A pair of giant planets orbiting in a 2:1 or 3:2 resonance and still embedded in a gaseous disk may undergo various regimes of migration, driven by the disk's tidal torques. These include coupled inward and outward migration. Here we concentrate on a pair of planets orbiting in proximity of the 2:1 resonance and study how they affect the evolution of dust in the surrounding of their orbits. By means of 2D and 3D hydrodynamic simulations that include the evolution of both gas and dust, we calculate the distributions of particles in the size range from 0.01 to 10 mm. Disk properties dictate the orbital evolution of the planets, including eccentricity excitation, which can impose distinctive features in the dust distributions. Under appropriate disk conditions, peculiar dust features, such as large cavities, could be connected to the migration history of the planets. We discuss dust configurations that may deliver information on the planets' orbital evolution.
- Publication:
-
42nd COSPAR Scientific Assembly
- Pub Date:
- July 2018
- Bibcode:
- 2018cosp...42E2192M