Modelling the evolution of planets in disks

TL;DR

This paper discusses numerical modeling techniques for simulating planetary migration within protoplanetary disks, emphasizing the importance of specific computational methods to accurately capture planet-disk interactions.

Contribution

It highlights key numerical approaches, such as the treatment of Coriolis forces and the FARGO method, crucial for successful simulations of planetary evolution in disks.

Findings

Proper handling of Coriolis forces improves simulation accuracy.

The FARGO method enhances computational efficiency.

Numerical techniques are vital for understanding planet migration.

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.