In the past year, there have been striking changes in Jupiter's atmosphere. Among these are the Oval BA's change from white to red, two new dark Disturbances in the southern hemisphere, and a 30% change (since 1997) in the aspect ratio of the potential vorticity anomaly of the GRS (not just its associated clouds), as we determined from high-accuracy velocities extracted from HST images. The determination of high-accuracy velocities requires both high-resolution imaging by HST (or flybys), and our novel adaptation of Correlation Image Velocimetry (CIV), a technique that has far greater accuracy than the traditional method (of identifying velocity tie-points by hand). Our proposed observations will test the hypothesis that these changes in Jupiter validate our 2004 prediction: that the merger of the 3 White Ovals in 1998-2000 would lead to climate change on Jupiter. The key is to determine, by indirect means, the temperature at the base of the weather layer, a quantity that cannot be observed directly at any wavelength. The new Red Oval BA's velocities will be used to test our finding that the color change is due to global temperature changes. The change in the GRS's aspect ratio suggests a large (at least 20%) change in the shear of the local velocity since 1997. The latter can be investigated only by determining Jupiter's current zonal winds.

WFPC2/PC1 imaging is done over two consecutive rotations of Jupiter, totalling about 19 hours. The current version of this phase 2 proposal specifies the acquisition of 8 orbits of data--on orbits 1, 2, 3, 5, 7, 9, 10, and 11 out of a sequence of 11 consecutive orbits. A schematic of this sequence is available through mid-2008 at astro.berkeley.edu/~mikewong/G480_hst/timing_v4.png. These observations will be challenging to schedule, requiring us to "hide the SAA" by timing the visits such that significant target science visibility can be achieved during our eight allocated orbits. This Phase II calls for the sequence of orbits 1, 2, 3, 5, 7, 9, 10, and 11 out of 11 consecutive orbits, as shown in the timing diagram at astro.berkeley.edu/~mikewong/G480_hst/timing_v4.png. HOWEVER, the following alternate sequences are equivalent scientifically but may have different scheduling opportunities: 1, 2, 3, 5, 6, 7, 9, and 11 1, 3, 4, 5, 6, 7, 9, and 11 1, 3, 4, 5, 7, 8, 9, and 11 1, 3, 5, 6, 7, 8, 9, and 11 1, 3, 5, 6, 7, 9, 10, and 11 1, 3, 5, 7, 8, 9, 10, and 11 Basically, we can use any sequence of 1, 3, 5, 7, 9, and 11, plus two even numbered orbits--with the exception that combinations of even orbits (2 and 8) or (4 and 10) are not ideal, since these combinations redundantly image the same parts of Jupiter. We will wait until spring 2008 to further refine scheduling for this program. At that time, improved predictions will be available for the orbit of HST, as well as the Jupiter atmospheric features of interest. 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JUPITER FROM EARTH, NOT TRANSIT OF GANYMEDE ACROSS JUPITER FROM EARTH, NOT TRANSIT OF CALLISTO ACROSS JUPITER FROM EARTH EARTH WFPC2 Imaging No F673N WFPC2 Imaging No F502N WFPC2 Imaging No F410M WFPC2 Imaging No F336W WFPC2 Imaging No F255W WFPC2 Imaging No F218W WFPC2 Imaging No F673N WFPC2 Imaging No F502N WFPC2 Imaging No F410M WFPC2 Imaging No FQCH4P15 WFPC2 Imaging No F953N ORBIT *01* of 11 CONSECUTIVE HST ORBITS AROUND THE EARTH (Tic-Visit :proposal-id 11102 :visit-id "01" :proposal-version -1 :trans-version "20071214" :date "10-Apr-2008 16:45:56.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 582608 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11102 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11102 :visit-id "01" :obset-id "A1" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11102 :visit-id "01" :obset-id 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