A High-Resolution, 3-D Model of the Great Red SPOT

Details A High-Resolution, 3-D Model of the Great Red SPOT A High-Resolution, 3-D Model of the Great Red SPOT

Sep 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998dps....30.3204c&link_type=abstract

American Astronomical Society, DPS meeting #30, #32.04; Bulletin of the American Astronomical Society, Vol. 30, p.1074

Astronomy and Astrophysics

Astronomy

Scientific paper

The motion in and around Jupiter's Great Red Spot (GRS) is tremendously complex, involving a huge range of spatial scales. The turbulent flow at the periphery contains a large amount of fine-scale filamentary structures while the core appears to contain larger-scale, counter-rotating motion. In the past, many numerical simulation studies have been carried out addressing the possible origin and general stability of the GRS. However, due to the severe limitation in numerical resolution, no past studies have been able to either capture the detailed flow or adequately constrain the vertical stratification parameter, the Rossby deformation radius (L_R). In this work, we present results from a series of high-resolution simulations using an essentially inviscid algorithm based on the advection of deformable patches of a dynamically active tracer, potential vorticity (PV). The algorithm solves the 3-D quasi-geostrophic PV equation, which governs the motion of large-scale, slowly-varying, shallow structures in planetary atmospheres. In order to carefully delineate the effects of stratification on the nonlinear evolution of the GRS, we vary the vertical profile of L_R to correspond to several representative profiles in the Jovian atmosphere. Our simulations show that, at high resolutions, this simple model is able to capture very well the flow features seen in Voyager and Galileo images as well as better constrain L_R for the GRS.

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