Vertical wind shear on Jupiter from Cassini images
Abstract
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.
Additional Information
© 2006 American Geophysical Union. Received 12 August 2005; revised 3 January 2006; accepted 12 January 2006; published 14 April 2006. We thank Ulyana Dyudina and Colette Salyk for their helpful suggestions on the technical aspects of this article. Cassini project funds supported this research.Attached Files
Published - 2005JE002556.pdf
Supplemental Material - jgre2072-sup-0001-t01.txt
Supplemental Material - jgre2072-sup-0002-t02.txt
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2013-04-17Created from EPrint's datestamp field
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