  We have produced mosaics of the Great Red Spot (GRS) using images taken by
the Galileo spacecraft in May 2000, and have measured the winds of the GRS
using an automated algorithm that does not require manual cloud tracking. Our
technique yields a high-density, regular grid of wind velocity vectors that is
advantageous over a limited number of scattered wind vectors that result from
manual cloud tracking. The high-velocity collar of the GRS is clearly seen from
our velocity vector map, and highest wind velocities are measured to be around
170 m/s. The high resolution of the mosaics have also enabled us to map
turbulent eddies inside the chaotic central region of the GRS, similar to those
mapped by Sada et al. (1996) and Vasavada et al. (1998). Using the wind
velocity measurements, we computed particle trajectories around the GRS as well
as maps of relative and absolute vorticities. We have discovered a narrow ring
of cyclonic vorticity that surrounds the main anti-cyclonic high-velocity
collar. This narrow ring appears to correspond to a ring surrounding the GRS
that is bright in 5-microns (Terrile and Beebe 1979). It appears that this
cyclonic ring is not a transient feature of the GRS, as we have discovered it
in a re-analysis of Galileo data taken in 1996 first analyzed by Vasavada et
al. (1998). We also calculate how absolute vorticity changes as a function of
latitude along a trajectory around the GRS and compare these measurements to
similar ones performed by Dowling and Ingersoll (1988) using Voyager data. We
show no dramatic evolution in the structure of the GRS since the Voyager era
except for additional evidence for a counterrotating GRS core, an increase in
velocity in the main velocity collar, and an overall decrease in the length of
the GRS.
