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Cassini UVIS observations of Jupiter's auroral variability |
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| Authors: | Wayne R Pryor A Ian F Stewart William E McClintock Alain J Jouchoux Donald E Shemansky Robert A West Bruce T Tsurutani George B Hospodarsky Kenneth C Hansen Frank J Crary Norbert Krupp Denis Grodent |
| Institution: | a Central Arizona College, 8470 N. Overfield Road, Coolidge, AZ 85228, USA b Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA c University of Southern California, Los Angeles, CA, USA d Jet Propulsion Laboratory, Pasadena, CA, USA e University of Iowa, Iowa City, IA, USA f University of Michigan, Ann Arbor, MI, USA g Southwest Research Institute, San Antonio, TX, USA h Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany i Boston University, Boston, MA, USA j University of Liege, Liege, Belgium k University College, London, UK |
| Abstract: | The Cassini spacecraft Ultraviolet Imaging Spectrograph (UVIS) obtained observations of Jupiter's auroral emissions in H2 band systems and H Lyman-α from day 275 of 2000 (October 1), to day 81 of 2001 (March 22). Much of the globally integrated auroral variability measured with UVIS can be explained simply in terms of the rotation of Jupiter's main auroral arcs with the planet. These arcs were also imaged by the Space Telescope Imaging Spectrograph (STIS) on Hubble Space Telescope (HST). However, several brightening events were seen by UVIS in which the global auroral output increased by a factor of 2-4. These events persisted over a number of hours and in one case can clearly be tied to a large solar coronal mass ejection event. The auroral UV emissions from these bursts also correspond to hectometric radio emission (0.5-16 MHz) increases reported by the Galileo Plasma Wave Spectrometer (PWS) and Cassini Radio and Plasma Wave Spectrometer (RPWS) experiments. In general, the hectometric radio data vary differently with longitude than the UV data because of radio wave beaming effects. The 2 largest events in the UVIS data were on 2000 day 280 (October 6) and on 2000 days 325-326 (November 20-21). The global brightening events on November 20-21 are compared with corresponding data on the interplanetary magnetic field, solar wind conditions, and energetic particle environment. ACE (Advanced Composition Explorer) solar wind data was numerically propagated from the Earth to Jupiter with an MHD code and compared to the observed event. A second class of brief auroral brightening events seen in HST (and probably UVIS) data that last for ∼2 min is associated with auroral flares inside the main auroral ovals. On January 8, 2001, from 18:45-19:35 UT UVIS H2 band emissions from the north polar region varied quasiperiodically. The varying emissions, probably due to auroral flares inside the main auroral oval, are correlated with low-frequency quasiperiodic radio bursts in the 0.6-5 kHz Galileo PWS data. |
| Keywords: | Auroras Jupiter Solar wind Ultraviolet |
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