# Results from a set of three-dimensional numerical experiments of a hot Jupiter atmosphere

## TL;DR

This study uses three-dimensional numerical simulations to investigate the dynamics of a hot Jupiter atmosphere, revealing the robustness of super-rotating equatorial jets and complex mechanisms behind jet acceleration.

## Contribution

It provides new insights into the stability and driving mechanisms of atmospheric jets on hot Jupiters through extensive 3D modeling.

## Key findings

- Super-rotating equatorial jet is robust across parameter changes.
- Deep atmosphere forcing can diminish the jet.
- Jet acceleration involves complex eddy and mean flow interactions.

## Abstract

We present highlights from a large set of simulations of a hot Jupiter atmosphere, nominally based on HD 209458b, aimed at exploring both the evolution of the deep atmosphere, and the acceleration of the zonal flow or jet. We find the occurrence of a super-rotating equatorial jet is robust to changes in various parameters, and over long timescales, even in the absence of strong inner or bottom boundary drag. This jet is diminished in one simulation only, where we strongly force the deep atmosphere equator-to-pole temperature gradient over long timescales. Finally, although the eddy momentum fluxes in our atmosphere show similarities with the proposed mechanism for accelerating jets on tidally-locked planets, the picture appears more complex. We present tentative evidence for a jet driven by a combination of eddy momentum transport and mean flow.