Numerical simulations of disc-planet interactions

TL;DR

This paper reviews numerical simulations of disc-planet interactions, covering various migration types, gap formation, and the impact of disc thermodynamics and turbulence on planetary migration.

Contribution

It provides a comprehensive overview of recent advances in simulating disc-planet interactions, including the effects of thermodynamics and turbulence on migration.

Findings

Type I migration is affected by disc thermodynamics.

Runaway (Type III) migration occurs for intermediate mass planets.

High-performance computing enables detailed global simulations of magnetised, turbulent discs.

Abstract

The gravitational interaction between a protoplanetary disc and planetary sized bodies that form within it leads to the exchange of angular momentum, resulting in migration of the planets and possible gap formation in the disc for more massive planets. In this article, we review the basic theory of disc-planet interactions, and discuss the results of recent numerical simulations of planets embedded in protoplanetary discs. We consider the migration of low mass planets and recent developments in our understanding of so-called type I migration when a fuller treatment of the disc thermodynamics is included. We discuss the runaway migration of intermediate mass planets (so-called type III migration), and the migration of giant planets (type II migration) and the associated gap formation in the disc. The availability of high performance computing facilities has enabled global simulations of magnetised, turbulent discs to be computed, and we discuss recent results for both low and high mass planets embedded in such discs.