Ut

CM 1=343.9 CM2=217.4 CM3=337.1

Fig. 3.11. A CCD image of Jupiter taken on January1, 2001. Note the two dark condensations or barges imbedded in the middle of the NEB, with a bright oval between them. Most often we see these condensations on the northern edge of the NEB. Also note the split SEB with very little coloration. South is up. (Credit: P. Clay Sherrod).

Fig. 3.11. A CCD image of Jupiter taken on January1, 2001. Note the two dark condensations or barges imbedded in the middle of the NEB, with a bright oval between them. Most often we see these condensations on the northern edge of the NEB. Also note the split SEB with very little coloration. South is up. (Credit: P. Clay Sherrod).

coloration of the barges was beautiful to behold! The dark condensations or spots are cyclonic as observed by spacecraft [9].

By 2002 and continuing into 2003, the NEB had returned to its more normal broad appearance with an even NEBn. The dark condensations, or barges, seen in the late 1990s were for the most part absent during 2002. In place of barges along the NEBn, during the 2001-2002 apparition, at least four small white ovals were seen at the edge of, or just barely imbedded in, the northern edge of the NEB at various locations around the planet. By March 2004, these ovals had disappeared. Instead, the NEB was again narrowing at several positions around the planet. By March 2004, neither white ovals nor dark condensations, nor barges, were seen on the NEBn, except for the long-lived white spot "Z", seen on the edge of the NEBn. The NTrZ was so bright, that white spot "Z" was exceedingly difficult to make out visually, and even difficult to distinguish in many CCD images. The NEBn was very uneven and undulating. In many places, it presented a ragged appearance on the northern edge of the belt, with the reddish-brown dark material of the belt broken up by the bright, white clouds of the NTrZ.

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