Vertical wind shear on Jupiter from Cassini images

Details Vertical wind shear on Jupiter from Cassini images Vertical wind shear on Jupiter from Cassini images

Apr 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006jgre..11104004l&link_type=abstract

Journal of Geophysical Research, Volume 111, Issue E4, CiteID E04004

Biology

5

Planetary Sciences: Fluid Planets: Atmospheres (0343, 1060), Planetary Sciences: Astrobiology: Planetary Atmospheres, Clouds, And Hazes (0343), Planetary Sciences: Solid Surface Planets: Meteorology (3346), Atmospheric Processes: Planetary Meteorology (5445, 5739), Atmospheric Composition And Structure: Planetary Atmospheres (5210, 5405, 5704)

Scientific paper

Multifilter images of Jupiter acquired by the Cassini Imaging Science Subsystem (ISS) are used to derive zonal winds at altitudes above and below the visible cloud deck. Small features unique to the ultraviolet images of ISS are tracked to get the systematic high-altitude zonal winds. Comparison between the zonal winds from ultraviolet images and the vertical profile of zonal winds from the Cassini Composite Infrared Spectrometer (CIRS) shows that the zonal winds from the ultraviolet images are from a pressure level that is ~0.2 scale heights higher than the pressure level of the zonal winds from continuum-band images. Deeper zonal winds at different latitudes of the equatorial region are measured by tracking cloud features observed within hot spots on continuum-band images. The deeper zonal winds in this study extend the measurement of the Galileo probe to different latitudes of the equatorial region. Comparison between the Galileo probe and this study suggests that these fast-moving clouds within hot spots are deeper than 3 bars and are therefore probably water clouds.

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