Numerical simulations of type III planetary migration: III. Outward migration of massive planets

Abstract

We present a numerical study of rapid, so called type III migration for Jupiter-sized planets embedded in a protoplanetary disc. We limit ourselves to the case of outward migration, and study in detail its evolution and physics, concentrating on the structure of the co-rotation and circumplanetary regions, and processes for stopping migration. We also consider the dependence of the migration behaviour on several key parameters. We perform this study using global, two-dimensional hydrodynamical simulations with adaptive mesh refinement. We find that the outward directed type III migration can be started if the initial conditions support $Z>1$, that corresponds to initial value $M_\rmnΔ \ga 1.5$. Unlike the inward directed migration, in the outward migration the migration rate increases due to the growing of the volume of the co-orbital region. We find the migration to be strongly dependent on the rate of the mass accumulation in the circumplanetary disc, leading to two possible regimes of migration, fast and slow. The structure of the co-orbital region and the stopping mechanism differ between these two regimes.

18 pages, 13 figures, submitted to MNRAS

References in corpus (4)

• Halting Type I planet migration in non-isothermal disks
• Cavity opening by a giant planet in a protoplanetary disc and effects on planetary migration
• Numerical simulations of the type III migration:I. Disc model and convergence tests
• Numerical simulations of type III planetary migration: II. Inward migration of massive planets

Cited by in corpus (6)

• Direct Imaging and Spectroscopy of a Planetary Mass Candidate Companion to a Young Solar Analog
• On corotation torques, horseshoe drag and the possibility of sustained stalled or outward protoplanetary migration
• On the width and shape of the corotation region for low-mass planets
• Type III migration in a low viscosity disc
• Constraint on the giant planet production by core accretion
• Numerical simulations of disc-planet interactions