Solar wind dynamic pressure and electric field as the main factors controlling Saturn's aurorae

F. J. Crary (), J. T. Clarke, M. K. Dougherty, P. G. Hanlon, K. C. Hansen, J. T. Steinberg, B. L. Barraclough, A. J. Coates, J.-C. Gérard, D. Grodent, W. S. Kurth, D. G. Mitchell, A. M. Rymer and D. T. Young
Additional contact information
F. J. Crary: Southwest Research Institute
J. T. Clarke: Boston University
M. K. Dougherty: Imperial College of Science and Technology
P. G. Hanlon: Imperial College of Science and Technology
K. C. Hansen: The University of Michigan
J. T. Steinberg: Los Alamos National Laboratory
B. L. Barraclough: Los Alamos National Laboratory
A. J. Coates: University College London, Mullard Space Science Laboratory
J.-C. Gérard: Université de Liège
D. Grodent: Université de Liège
W. S. Kurth: The University of Iowa
D. G. Mitchell: Johns Hopkins University
A. M. Rymer: University College London, Mullard Space Science Laboratory
D. T. Young: Southwest Research Institute

Nature, 2005, vol. 433, issue 7027, 720-722

Abstract: Saturn's aurora The cover shows Hubble Space Telescope (HST) images of Saturn and its polar auroral emissions on 24, 26 and 28 January 2004. Visible wavelength images are combined with ultraviolet images of the south polar region. The strong brightening of the aurora on 28 January corresponded with a large disturbance in the solar wind. These images were obtained during a campaign by the Cassini spacecraft to measure the solar wind approaching Saturn and the Saturn kilometric emissions, and the combined results are presented in three letters in this issue. Saturn's aurorae differ in shape and form from those seen on Earth and on Jupiter, and they also differ in their response to the solar wind. Saturn's strongest radio emissions appear to be closely tied to the polar aurora.

Date: 2005
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DOI: 10.1038/nature03333

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