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arXiv · 2604.09042

Giant Planet Formation by Disk Instability

Ravit Helled·Oliver Schib·Christian Reinhardt·Noah Kubli·Lucio Mayer·Christoph Mordasini·Gabriele Cugno
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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.

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Ravit Helled, Oliver Schib, Christian Reinhardt, Noah Kubli, Lucio Mayer, Christoph Mordasini, Gabriele Cugno. 2026-04-10. Giant Planet Formation by Disk Instability. https://arxiv.org/abs/2604.09042

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