JUPITER 09:09 U.T. P3.011S6 ]J»r. 16.2003 Note very nlc* STB dprWefllno S and Toi 1h« GRS CanslOtrabl» lr*«raet»n of SEB & GRS p Clay Sharrod - Arkansas sv, Obsanatwy 0.31m Schmi« ■ Olynou! C joäo g f.'5J

CM I » ÎW4 / CM II = 82.4/ CM Ml s »9.3 ""'T^t Swing 5/10 - Fair mo ■ 4m ■ iso »0

Fig. 3.17. A low intensity GRS followed by a faded SEB. Note the coloration event in the northern two-thirds of the EZ. Jupiter on January 15, 2003. South is up. (Credit: P. Clay Sherrod).

During this time, due to much turbulence following the GRS, the SEB following the GRS for several degrees had faded (Fig. 3.17). The GRS itself had also declined in intensity. This fading of the SEB and GRS, and the dusky appearance of the EZ, combined with the coloration of the EZ, made it difficult to make out visually where the GRS/RSH ended and the SEB began! For several degrees following the GRS, the EZ was actually more intense than the SEB! It was still quite easy to discern the GRS against the SEB in CCD images. However, as late as December 2002 the GRS and

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