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[30.18] Enhanced Transport in the Polar Mesosphere of Jupiter: Evidence from Cassini UVIS Helium 584 Å~ Airglow

C.D. Parkinson (Caltech), A.I.F. Stewart (LASP), A.-S. Wong (University Michigan), J.M. Ajello (JPL), Y.L. Yung (Caltech)

The eddy diffusion coefficient (K) in the auroral regions of Jupiter is not known. However, due to the intense auroral energy input, eddy mixing is expected to be much more effective and may be responsible for the enhancement of heavy hydrocarbon production in the polar region. We estimate the increased eddy mixing in the Jovian auroral regions by comparing the Cassini Ultraviolet Imaging Spectrograph (UVIS) observations during the 2000 Jupiter flyby with radiative transfer calculations of the He 584 Å~ airglow intensity. We derive the range for the eddy diffusion coefficients at the homopause (K_h) in the auroral regions to be at least 8 x 10⁶ cm² s^-1, and possibly greater than 4 x 10⁷ cm² s^-1. By comparison, equitorial K_h is on the order of 2 x 10⁶ cm² s^-1.

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Bulletin of the American Astronomical Society, 37 #3
© 2004. The American Astronomical Soceity.