Modelling the evolution of planets in disks

Abstract

To explain important properties of extrasolar planetary systems (eg. close-in hot Jupiters, resonant planets) an evolutionary scenario which allows for radial migration of planets in disks is required. During their formation protoplanets undergo a phase in which they are embedded in the disk and interact gravitationally with it. This planet-disk interaction results in torques (through gravitational forces) acting on the planet that will change its angular momentum and result in a radial migration of the planet through the disk. To determine the outcome of this very important process for planet formation, dedicated high resolution numerical modeling is required. This contribution focusses on some important aspects of the numerical approach that we found essential for obtaining successful results. We specifically mention the treatment of Coriolis forces, Cartesian grids, and the FARGO method.

Talk given at JENAM meeting, Vienna 2008

References in corpus (9)

• A comparative study of disc-planet interaction
• Halting Type I planet migration in non-isothermal disks
• On the corotation torque in a radiatively inefficient disk
• Cavity opening by a giant planet in a protoplanetary disc and effects on planetary migration
• On the migration of protogiant solid cores
• Migration of Protoplanets in Radiative Disks
• Growing and moving low-mass planets in non-isothermal disks
• Numerical simulations of the type III migration:I. Disc model and convergence tests
• On The Orbital Evolution of Jupiter Mass Protoplanet Embedded in A Self-Gravity Disk