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See supporting data on Science Online.
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0012219122
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From 11 to 13 December 2000, the ISS acquired a 1 X 2 mosaic every hour for 38 hours, producing 29 pairs of images, each separated from the other by one planetary rotation (10 hours). Wind measurements were taken from these image pairs. Spatial resolution ranged from 122 to 114 km/pixel, resulting in a wind speed precision of ∼3.3 m/s. Images were navigated on the planetary limb, calibrated radiometrically, assembled into spatial mosaics, and mapped with a simple cylindrical projection. Illumination effects were removed by dividing the brightness values by the cosine of the solar incidence angle, Zonal winds were measured with an automatic line-shifting method. Each map line spans 0.1° latitude (∼12S0 km). Because blocks of five lines were shifted and digitally correlated, the latitudinal resolution of our zonal velocity profile is 0. S°.
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We imaged in a continuum spectral region (751 nm) sensitive to clouds at all levels down to great depth, a weak methane absorption band (727 nm) sensitive to somewhat higher cloud tops, and a strong methane band (889 nm) that detects clouds with tops in the upper troposphere (18). Localized regions that are bright at all three wavelengths have high-altitude tops and are optically thick. Similar features in terrestrial satellite images are vertically extensive and associated with deep moist convective insatability (68). A similar Galileo feature was collocated with a previous lightning detection and identified as convection (19). To confirm our storm identifications and to ensure that no other events were missed, we examined scatter plots of the weak methane band versus continuum brightness for both the small region containing the feature (compare fig. S1) and the large-scale region excluding the convective area. Features with high-continuum albedo (i.e., optically thick clouds) and anomalously high brightness in the weak methane band (i.e., high cloud tops) were identified as convective storms.
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0012319977
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Latitudinal shear of the zonal wind is characterized as cyclonic or anticyclonic according to the sense of rotation that would be induced in an object placed into the flow. Cyclonic shear corresponds to counterclockwise rotation in the northern hemisphere and clockwise rotation in the southern hemisphere, as is found poleward of the eastward jets. The opposite sense of rotation defines anticyclonic flow.
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0012218333
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One hundred fifty-six candidate storms were identified in images spanning 1 to 15 December 2000 and 29 December 2000 to 7 January 2001, during which NAC image scale varied from ∼60 to 175 km/pixel. Images were obtained for ∼67% of the available time pre-encounter and ∼20% near- and post-encounter, equivalent to ∼12 continuous days of global imaging. Removing multiple observations of the same storm at different times reduced the number of storms to 64 independent candidates, and an examination of scatter plots of albedo in the three channels eliminated some questionable features, resulting in 43 high-confidence separate storm identifications.
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2 and He and scattering and absorption by aerosols are important opacity sources in the UV. Absorption by ammonia or acetylene averaged over the spectral band between 2S0 and 280 nm is negligible in comparison to that from aerosols. Consequently, we assumed that jovian absorption in the nearUV is attributable to aerosol particles. (A broad gaseous molecular absorption may also be important. If so, its composition is unknown.)
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0012265532
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Several HST images were used to measure polar stratospheric winds, and differences were found when these winds were compared to tropospheric winds (32). A UV-dark oval was found near planetocentric latitude 60°N, having about the same size and shape as Jupiter's Great Red Spot in an HST image obtained in 1997 with a filter having the same spectral characteristics as the UV1 filter on the ISS NAC. It was not seen in other UV images from HST, which were taken on average once or twice per year between 1994 and 1999, although not all images have been examined closely. Therefore, before the Cassini encounter, it was thought that this type of feature was rare or perhaps a singular event.
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Hall and others (47) observed atomic O emissions in the extreme UV, and Brown and Hill (48) detected extended visible emission in Na D lines.
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The best measurement of jovian main ring thickness is that estimated from high-resolution Galileo images: ∼100 km at a phase angle of ∼90° (57). Voyager placed an upper limit on the ring's thickness seen in forward-scattered light (presumably the fine dust component) of 300 km (61). Small dust particles are brightest in forward scattering, whereas Larger particles are brightest in back-scattered light; therefore, it is possible that the small particles have a different vertical distribution than the large particles.
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We gratefully acknowledge the assistance of many individuals in planning and executing the imaging science investigation during the Cassini Jupiter flyby, in particular D. Dawson, K. Grazier, C. Hansen, V. Haemmerte, B. Janes, D. Lytle, and E. McCartney. We also acknowledge the financial support of Cosmos Studios in the creation of atmospheric movies from the Jupiter flyby.
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