The South-South Temperate Region generally extends from latitude 37° south to
53° south. Lying just south of the STB is the STZ, and just south of that is the SSTB.
The south-south temperate region is exceedingly difficult to observe visually. To most observers this region appears as varying intensities of gray, with very few features that can be made out. Sometimes a dim, gray SSTB can be seen. Most often it is actually difficult to distinguish this belt, or the South South Temperate Zone
(SSTZ) for that matter, from the northern edge of the SPR. Like the STB, the SSTB
is a very narrow belt with a light gray coloration. While features here are difficult to observe visually, CCD imaging by amateurs has been quite successful. Normally, a number of small, bright ovals can be seen here, being of great interest to astrono- — q q mers (Fig. 3.28). These ovals can provide our only chance to monitor the drift rates g C
at this latitude. Unlike the much larger STO BA, these south STOs are quite small Jfl g —
and of especially low contrast. Many visual observers have never seen one. Images q ^
with CCD cameras and webcams usually reveal them easily, as they stand out ^ <D
against the slightly darker gray coloration of the SSTB and sStZ. Examination of <D ^
CCD images during recent apparitions suggests that there are always six or more of |£ ^
these ovals each apparition. These ovals are of relatively small size, however, I did measure one oval as 5° in length on a CCD image taken by Cristian Fattinnanzi on
April 02, 2004. Several ovals were seen, quite bright against the dusky, gray SSTZ.
During 2006, several small bright ovals were again observed, being very prominent in CCD/webcam images (Fig. 3.28).
Like the NPR, the SPR often presents little that can be seen by amateurs, even with CCD cameras and webcams. Sometimes imaging can reveal very subtle, thin faint bands and barely noticeable zones marked only by very subtle shading differences. Sometimes small bright ovals are seen. Features that might offer a chance to track currents in this region are short-lived or very difficult to see. I did note during the 2003-2004 apparition what might be described as a very small south polar hood of bluish-gray color, which was also noticeable on CCD images (Fig. 3.29). However, the remarkable work by amateurs using CCDs and webcams caught many features that were of great interest. In fact, the SPR turned out to be much more active than the NPR! Small bright ovals that turned out to be long-lived were seen in the SPR at 60° south latitude, and another one was seen in the south-south-south temperate
JUPITER-2004 04 02 19:46 u.t.
2&0rmm F5 Newtonian
1100/1400 frames stacked with Philips Vesta Pro Cnstian Fatlinnanzi - Macerata. ITALY
Fig. 3.28. Four very bright small ovals are seen in the SSTB of Jupiter in this webcam image taken on April 2, 2004. The GRS can be seen emerging from the following limb of the planet. A prominent bluish-gray plateau with a trailing festoon can be seen on the south edge of the NEB. The northern edge of the NEB is very uneven. South is up. (Credit: Cristian Fattinnanzi).
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