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We have produced mosaics of the Great Red Spot (GRS) using images taken bythe Galileo spacecraft in May 2000, and have measured the winds of the GRSusing an automated algorithm that does not require manual cloud tracking. Ourtechnique yields a high-density, regular grid of wind velocity vectors that isadvantageous over a limited number of scattered wind vectors that result frommanual cloud tracking. The high-velocity collar of the GRS is clearly seen fromour velocity vector map, and highest wind velocities are measured to be around170 m/s. The high resolution of the mosaics have also enabled us to mapturbulent eddies inside the chaotic central region of the GRS, similar to thosemapped by Sada et al. (1996) and Vasavada et al. (1998). Using the windvelocity measurements, we computed particle trajectories around the GRS as wellas maps of relative and absolute vorticities. We have discovered a narrow ringof cyclonic vorticity that surrounds the main anti-cyclonic high-velocitycollar. This narrow ring appears to correspond to a ring surrounding the GRSthat is bright in 5-microns (Terrile and Beebe 1979). It appears that thiscyclonic ring is not a transient feature of the GRS, as we have discovered itin a re-analysis of Galileo data taken in 1996 first analyzed by Vasavada etal. (1998). We also calculate how absolute vorticity changes as a function oflatitude along a trajectory around the GRS and compare these measurements tosimilar ones performed by Dowling and Ingersoll (1988) using Voyager data. Weshow no dramatic evolution in the structure of the GRS since the Voyager eraexcept for additional evidence for a counterrotating GRS core, an increase invelocity in the main velocity collar, and an overall decrease in the length ofthe GRS.

Velocity and Vorticity Measurements of Jupiter's Great Red Spot Using Automated Cloud Feature Tracking