Space and Planetary Science; Geophysics; Jupiter; Juno
Abstract :
[en] The Juno spacecraft's polar orbits have enabled direct sampling of Jupiter's low-altitude auroral field lines. While various data sets have identified unique features over Jupiter's main aurora, they are yet to be analyzed altogether to determine how they can be reconciled and fit into the bigger picture of Jupiter's auroral generation mechanisms. Jupiter's main aurora has been classified into distinct “zones”, based on repeatable signatures found in energetic electron and proton spectra. We combine fields, particles, and plasma wave data sets to analyze Zone-I and Zone-II, which are suggested to carry upward and downward field-aligned currents, respectively. We find Zone-I to have well-defined boundaries across all data sets. H+ and/or H3+ cyclotron waves are commonly observed in Zone-I in the presence of energetic upward H+ beams and downward energetic electron beams. Zone-II, on the other hand, does not have a clear poleward boundary with the polar cap, and its signatures are more sporadic. Large-amplitude solitary waves, which are reminiscent of those ubiquitous in Earth's downward current region, are a key feature of Zone-II. Alfvénic fluctuations are most prominent in the diffuse aurora and are repeatedly found to diminish in Zone-I and Zone-II, likely due to dissipation, at higher altitudes, to energize auroral electrons. Finally, we identify significant electron density depletions, by up to 2 orders of magnitude, in Zone-I, and discuss their important implications for the development of parallel potentials, Alfvénic dissipation, and radio wave generation.
Research Center/Unit :
STAR - Space sciences, Technologies and Astrophysics Research - ULiège
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Sulaiman, A. H. ; Department of Physics and Astronomy University of Iowa Iowa City IA USA
Mauk, B. H. ; Applied Physics Laboratory Johns Hopkins University Laurel MD USA
Szalay, J. R. ; Department of Astrophysical Sciences Princeton University Princeton NJ USA
Allegrini, F. ; Southwest Research Institute San Antonio TX USA ; Department of Physics and Astronomy University of Texas at San Antonio San Antonio TX USA
Clark, G. ; Applied Physics Laboratory Johns Hopkins University Laurel MD USA
Gladstone, G. R. ; Southwest Research Institute San Antonio TX USA ; Department of Physics and Astronomy University of Texas at San Antonio San Antonio TX USA
Kotsiaros, S. ; DTU‐Space Technical University of Denmark Kongens Lyngby Denmark
Kurth, W. S. ; Department of Physics and Astronomy University of Iowa Iowa City IA USA
Bagenal, F. ; Laboratory for Atmospheric and Space Physics University of Colorado Boulder Boulder CO USA
Bonfond, Bertrand ; Université de Liège - ULiège > Département d'astrophysique, géophysique et océanographie (AGO) > Labo de physique atmosphérique et planétaire (LPAP)
Connerney, J. E. P. ; Space Research Corporation Annapolis MD USA ; NASA/Goddard Space Flight Center Greenbelt MD USA
Ebert, R. W. ; Southwest Research Institute San Antonio TX USA ; Department of Physics and Astronomy University of Texas at San Antonio San Antonio TX USA
Elliott, S. S. ; Minnetota Institute for Astrophysics School of Physics and Astronomy University of Minnesota Minneapolis MN USA
Gershman, D. J. ; NASA/Goddard Space Flight Center Greenbelt MD USA
Hospodarsky, G. B. ; Department of Physics and Astronomy University of Iowa Iowa City IA USA
Hue, V. ; Southwest Research Institute San Antonio TX USA
Lysak, R. L. ; Minnetota Institute for Astrophysics School of Physics and Astronomy University of Minnesota Minneapolis MN USA
Masters, A. ; Blackett Laboratory Imperial College London London UK
Santolík, O. ; Department of Space Physics Institute of Atmospheric Physics of the Czech Academy of Sciences Prague Czechia ; Faculty of Mathematics and Physics Charles University Prague Czechia
Saur, J. ; Institute of Geophysics and Meteorology University of Cologne Cologne Germany
Bolton, S. J. ; Southwest Research Institute San Antonio TX USA
The Waves, JADE, MAG, and JEDI data used in this article have the data set ID JNO-E/J/SS-WAV-3-CDR-BSTFULL-V1.0, JNO-J/SW-JAD-3-CALIBRATED-V1.0, JNO-J-3-FGM-CAL-V1.0, and JNO-J-JED-3-CDR-V1.0, respectively, and are publicly accessible through the Planetary Plasma Interactions Node in the Planetary Data System (https://pds-ppi.igpp.ucla.edu/). In this study, we use an effective E-field antenna length of 0.5 m. The UVS data have data set ID jnouvs_3001 and are publicly accessible through the Atmospheres Node in the Planetary Data System (https://pds-atmospheres.nmsu.edu/).
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