SM057-03
Partial electron density and temperature over Jupiter’s main auroral emission

Wednesday, 16 December 2020: 10:08
Virtual
Frederic Allegrini1, William S Kurth2, Joachim Saur3, Randy Gladstone1, Fran Bagenal4, Scott J Bolton1, George B Clark5, John E P Connerney6, Rob W Ebert7, Masafumi Imai8, Philippe Louarn9, Barry Mauk10, David J McComas11, Jamey R Szalay11, Philip W Valek12 and Robert J Wilson13, (1)Southwest Research Institute, San Antonio, TX, United States, (2)University of Iowa, Department of Physics and Astronomy, Iowa City, IA, United States, (3)University of Cologne, Cologne, Germany, (4)Univ Colorado, Boulder, CO, United States, (5)Johns Hopkins University Applied Physics Laboratory, Laurel, MD, United States, (6)NASA Goddard Space Flight Center, Greenbelt, MD, United States, (7)Southwest Research Institute, Space Science and Engineering, San Antonio, TX, United States, (8)National Institute of Technology, Department of Electrical Engineering and Information Scienc, Ehime, Japan, (9)IRAP, CNRS, Toulouse, France, (10)The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, United States, (11)Princeton University, Department of Astrophysical Sciences, Princeton, NJ, United States, (12)Southwest Research Inst, San Antonio, TX, United States, (13)University of Colorado Boulder, Boulder, CO, United States
Recorded Presentation
Abstract:
Jupiter’s ultraviolet (UV) aurora, the most powerful and intense in the solar system, is caused by energetic electrons precipitating from the magnetosphere into the atmosphere where they excite the molecular hydrogen. Electrons from ~50 eV to ~100 keV are characterized over the auroral regions by the Jovian Auroral Distributions Experiment (JADE) on Juno. Investigating the characteristics of electron distributions at these energies is critical for understanding the source population for the electrons that produce Jupiter’s UV aurora and the mechanisms that accelerated them to keV and MeV energies. In this study, we present a survey of electron distributions and moments derived from JADE in Jupiter’s polar magnetosphere. We quantify the electron properties (e.g. density and temperature) and explore similarities and differences in their distributions over several Juno perijove passes, focusing on regions near the main emission.
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