Radial evolution of a giant planet in a protoplanetary disk
Kazuhiro Kanagawa (RESCEU, Univ. of Tokyo)
A planet is formed within a protoplanetary disk. The planet migrates within the disk due to disk—planet interaction, which is closely related to an architecture of planetary systems such as these observed by Kepler space telescope. When the planet grows up to a giant planet such as Jupiter, the giant planet forms a density gap around its orbit. Recent ALMA observations have revealed protoplanetary disks with multiple gaps such as the disk of HL Tau. These gap structures may indicate a forming planet embedded in the disk. The migration of the gap-opening planet is important for formation of the planetary systems and also it can tell us a connection between the observations of the protoplanetary disks and current planetary systems.
It is expected that in the ideal case, the gap-opening planet migrates at the viscous drift rate. However, recent hydrodynamic simulations have shown that, in general, the gap-opening planet is not locked to the viscous disk evolution. A new physical model is required to explain the migration speed of such a planet. For this reason, we re-examined the migration of a single planet in a protoplanetary disk, by carrying out the two-dimensional hydrodynamic simulations in a wide parameter range.
We have found that the torque exerted on the gap-opening planet is proportional to the surface density at the bottom of the gap. This result indicates that the reduction of the migration speed of the gap-opening planet can be simply explained by decreasing the surface density at the bottom of the gap. Using the gap model developed in our previous studies, we have constructed an empirical formula of the migration speed of the gap-opening planets, which is consistent with the results obtained before in the hydrodynamic simulations performed by us and other researchers. Our model easily explains why the migration speed of the gap-opening planets can be faster than the viscous gas drift speed. Our model can also predict the planet mass at which the transition from type I to type II migrations occurs and provide a gap-opening criterion in terms of planetary migration.
host contact: Misako Tatsuuma