Cl

SEB following it were still faded. During the 2002-2003 apparition the northern three-quarters of the equatorial zone continued to display a light yellow-ochre coloration. A CCD image by Eric Ng taken on May 01, 2003 revealed an EZ that was almost entirely colored with a pronounced yellow-ochre appearance (Fig. 3.18). Only the very southern edge of the EZ was bright, like a thin bright line extending all around the planet just north of the SEB. By 2004, the NEBs projections and festoons were again easily seen. These features, along with the continued coloration of the EZ, and the absence of the NTB and NNTB gave the appearance of the NTrZ and NTZ being the brightest regions of the planet.

Sometimes the EZ will display an equatorial band (EB). The EB is most often seen as a thin, bluish-gray band or line running through the length of the EZ. It is not always present, and when present it may be broken or discontinuous. Often, when the EB is present at the same time as the bluish-gray projections of the NEBs, the projections will be seen to loop into the EZ and tie into the EB (Fig. 3.19).

During 2006, the projections and festoons trailing into the EZ were so prominent as to give the EZ a dusky appearance visually. The festoons trailed back into a bluish-gray equatorial band (EB). The area between the EB and the northern edge of the SEB was very bright, easily contrasted against the duskiness of the rest of the EZ. Many of the bluish-gray projections/festoons were accompanied by a bright oval, or porthole, following the projection and tucked u next to it. Some of these were bright enough to see visually. The festoons, portholes, and the various shadings of gray gave the EZ a very stormy appearance, especially visually through an eyepiece. Because of this, the NTrZ and the STrZ both appeared brighter than the EZ (Fig. 3.19).

In the SEBn, especially near the longitude of the GRS, extensive turbulence can be witnessed for several degrees of longitude preceding and following the GRS, as just mentioned. This turbulence is especially prominent following the GRS, where i ^ I h-<0

20030501 12:08UT

CMI=222 9 CM!I=281 2

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10" FS Royce Newtonian. ToUcam Pro. FS4.5. 1/25 sec. 550 frames slacked Tfotlg Kpng

Fig. 3.18. Jupiter on May 1, 2003. Notice the yellow-ochre coloration of the northern two-thirds of the EZ. The NTrZ was the brightest zone on Jupiter at this time. Webcam image with south up. (Credit: Eric Ng).

D. Parker Coral Gables. FL Seeinq gooƶ: 7-fl Trans fair: 4 Mind E G-10 Kts. AN: 19 degs

18 Aug 2006 00:21 55 UT

16-in Newt a f-21 SKYriyx 2-0 camera Aslrodon Fitters: H = | Series: G,B = E Series RRGB 31 fps

CM1=24S3 CM2=114 Z CM3=Z8t 2

Fig. 3.19. Jupiter with prominent festoons trailing into the EZ. Notice at this late date the NTB and NNTB are still absent. August 18, 2006. South is up. (Credit: Donald C. Parker).

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Fig. 3.20. Jupiter on March 8, 2003. Note the wake following the GRS causing a disturbed SEB. South is up. (Credit: Ed Grafton).

Fig. 3.20. Jupiter on March 8, 2003. Note the wake following the GRS causing a disturbed SEB. South is up. (Credit: Ed Grafton).

white ovals can appear in the south equatorial belt (SEB) (Fig. 3.20). These bright ovals can often be seen trailing back from the GRS toward the following side of the planet for several degrees of longitude. This bright area of continuous turbulence can vary in intensity, but is usually easy to make out against the usually darker, reddish-brown color of the SEB itself.

Sometimes, small bright ovals can be seen in the SEB near its northern edge preceding the GRS. There have been several instances of small, bright ovals in the

SEBn that have approached and passed north of the GRS, sometimes being caught up in the currents surrounding the GRS and swirling around the edge of the GRS into the middle of the SEB. Sometimes these bright spots will actually appear to enter into the GRS itself, offering an opportunity to track the anti-cyclonic behavior inside the GRS. This phenomenon was well observed on CCD images of Jupiter taken during September and October 2002.

3.1.6 The South Tropical Region ical nce anet

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