2020/06/08 by Rakesh K. Yadav, Rakesh Kumar Yadav, Jeremy Bloxham · 45 citations
Biochemistry, Genetics and Molecular Biology · Earth and Planetary Sciences · Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Atmosphere (unit) #Convection #Geology #Geology and Paleoclimatology Research #Geomagnetism and Paleomagnetism Studies #Geometry #Geophysics #Jet (fluid) #Mechanics #Meteorology #Physics #Planet #Polar #Saturn #Thermal #Turbulence #Vortex #Zonal flow (plasma) #astro-ph.EP #physics.comp-ph #physics.flu-dyn
paper · pdf · doi:10.1073/pnas.2000317117
published in Proceedings of the National Academy of Sciences 117(25), 13991-13996 (National Academy of Sciences) · 11 pages, 4 main and 5 supplementary figures, 1 animation, 42 references
openalex publication_date 2020/06/08 · arxiv created 2020/07/17 · arxiv updated 2020/07/20 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Numerous land- and space-based observations have established that Saturn has a persistent hexagonal flow pattern near its north pole. While observations abound, the physics behind its formation is still uncertain. Although several phenomenological models have been able to reproduce this feature, a self-consistent model for how such a large-scale polygonal jet forms in the highly turbulent atmosphere of Saturn is lacking. Here, we present a three-dimensional (3D) fully nonlinear anelastic simulation of deep thermal convection in the outer layers of gas giant planets that spontaneously generates giant polar cyclones, fierce alternating zonal flows, and a high-latitude eastward jet with a polygonal pattern. The analysis of the simulation suggests that self-organized turbulence in the form of giant vortices pinches the eastward jet, forming polygonal shapes. We argue that a similar mechanism is responsible for exciting Saturn's hexagonal flow pattern.