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

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufm.p11c0134l&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #P11C-0134

Physics

0343 Planetary Atmospheres (5210, 5405, 5704), 3346 Planetary Meteorology (5445, 5739), 5700 Planetary Sciences: Fluid Planets, 5704 Atmospheres (0343, 1060), 5739 Meteorology (3346)

Scientific paper

Multi-filter 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 first 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 about 0.2 scale 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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