Description:

Jupiter’s dynamics shapes its clouds but remains largely unknown below this natural observational barrier. Unravelling the underlying three-dimensional flows is thus a primary goal for NASA’s ongoing Juno mission. In parallel, and to take the most of this continuous flux of new data, we have addressed the Jovian dynamics using idealized laboratory experiments complemented by theoretical and numerical analyses. I will present here our main recent results. First, I will explain the formation of the observed long-lived, strong, large Jovian jets by a subcritical, resonant instability between forced Rossby waves and the background flow. Then, I will describe the generic force balance responsible for the three-dimensional pancake-like shape of Jovian vortices, and our prediction of the Great Red Spot’s thickness. Finally, I will comment on the suitable conditions to produce stable clusters of vortices at Jupiter’s poles. Dynamical similitude with mechanisms observed in other natural systems (Earth's oceans, other Giant planets atmosphere, accretion disks, etc.) will be discussed. My main objective is to illustrate the benefits from a constructive, multi-method and interdisciplinary approach of such challenging open questions.