Giant Planet Formation by Disk Instability

TL;DR

This review discusses recent advances in the disk instability model for giant planet formation, including simulations, population synthesis, and observational constraints.

Contribution

It summarizes recent developments in hydrodynamical, MHD simulations, and observational tests of the disk instability model.

Findings

Recent simulations support the viability of disk instability for giant planet formation.

Advances in observations can help distinguish this model from core accretion.

Clump-clump collision simulations provide insights into planet formation processes.

Abstract

The disk instability (DI) model for giant planet formation remains an attractive alternative in explaining the formation of giant planets at early times, giant planets at large radial distances, and giant planets orbiting M-stars. In this review, we present recent developments in the disk instability model including hydrodynamical as well as magneto-hydrodynamical (MHD) disk simulations, populations synthesis models, and simulations of clump-clump collisions. We also discuss advances in observations that can be used to constrain and test this formation scenario.