HR: 0800h
AN: P11C-0134    [Abstracts]
TI: Vertical wind shear on Jupiter from Cassini images
AU: * Li, L
EM: liming@gps.caltech.edu
AF: Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, 91125
AU: Ingersoll, A P
EM: api@gps.caltech.edu
AF: Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, 91125
AU: Vasavada, A R
EM: Ashwin.R.Vasavada@jpl.nasa.gov
AF: Jet Propulsion Laboratory, California Institute of Technology, Pasadena, 91125
AU: Simon-Miller, A A
EM: simon@lepasm.gsfc.nasa.gov
AF: NASA/Goddard Space Flight Center, Code 693, Greenbelt, 20771
AU: Del Genio, A D
EM: Oinegled@aol.com
AF: NASA Goddard Institute for Space Studies, Lamont-Doherty Earth Observatory of Columbia University , New York, 10025
AU: Ewald, S P
EM: spe@caltech.edu
AF: Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, 91125
AU: Porco, C C
EM: carolyn@ciclops.org
AF: Space Science Institute, 4750 Walnut Street, Ste 205, Boulder, Colorado
AU: West, R A
EM: robert.a.west@jpl.nasa.gov
AF: Jet Propulsion Laboratory, California Institute of Technology, Pasadena, 91125
AB: 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.
DE: 0343 Planetary atmospheres (5210, 5405, 5704)
DE: 3346 Planetary meteorology (5445, 5739)
DE: 5700 PLANETARY SCIENCES: FLUID PLANETS
DE: 5704 Atmospheres (0343, 1060)
DE: 5739 Meteorology (3346)
SC: Planetary Sciences [P]
MN: Fall Meeting 2005