Giant Planet Formation by Disk Instability
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.
Cite
@article{arxiv.2604.09042,
title = {Giant Planet Formation by Disk Instability},
author = {Ravit Helled and Oliver Schib and Christian Reinhardt and Noah Kubli and Lucio Mayer and Christoph Mordasini and Gabriele Cugno},
journal= {arXiv preprint arXiv:2604.09042},
year = {2026}
}
Comments
Chapter accepted for publication in the NCCR PlanetS Legacy Book: Benz, W. et al. (Eds), The National Center for Competence in Research, PlanetS: A Swiss-wide network expanding planetary sciences. Springer (2026)