Published October 9, 2021 | Version 1.1.0
Dataset Open

Analysis of Whistler-Mode and Z-Mode Emission in the Juno Primary Mission

  • 1. Department of Physics and Astronomy, University of Iowa, Iowa City, IA, USA
  • 2. Department of Electrical Engineering and Information Science, National Institute of Technology (KOSEN), Niihama College, Niihama, Ehime, Japan
  • 3. Department of Space Physics, IAP, CAS, Prague, Czech Republic; Faculty of Mathematics and Physics, Charles University, Prague, Czech Republic
  • 4. Applied Physics Laboratory, The Johns Hopkins University, Laurel MD, USA
  • 5. Southwest Research Institute, San Antonio, TX, USA; Physics and Astronomy Department, University of Texas at San Antonio, San Antonio, TX, USA
  • 6. Department of Physics, University of Minnesota, Minneapolis, MN, USA
  • 7. Southwest Research Institute, San Antonio, TX, USA


This is the supporting data set for the paper by the same title published in AGU JGR Space Physics, 10.1029/2021JA029885

Key Points:

  • Jovian whistler-mode chorus and Z-mode intensity distributions are surveyed and analyzed at the end of the Juno primary mission
  • Bursty low frequency whistler mode emission implies electrons energies exceeding 100 keV
  • Jovian whistler mode chorus and Z-mode intensity are parametrically fit to frequency, M-shell, and mag-latitude.


At the end of the Juno primary mission we report observations of whistler mode chorus and Z-mode emission.  The Juno orbits are evolving and much better coverage of the whistler mode chorus source region has resulted since the earlier surveys.  Bursty chorus emission extending to ~30° latitude and to frequencies less than the lower hybrid frequency near the source region imply high electron energies (>100 keV).  Average chorus intensity levels peak at ~10-3 nT2 near M-shell of 8-9 and magnetic latitude of  ~5°.  Z-mode emission is identified at higher latitudes generally near and inward of the Io torus with intensity levels as much as two orders of magnitude higher than Z-mode emissions observed at Saturn.  Inferred source regions for the Z-mode are consistent with the inner edge of the Io torus and with auroral field lines that may also support Jovian kilometric and decametric emission.  Parametric fitting functions are evaluated for both whistler mode chorus and Z-mode, describing wave intensity as a function of frequency, magnetic latitude, and M-shell.  Both whistler mode and Z-mode waves may have significant impact on electron scattering and acceleration at Jupiter as recent models indicate.


Version 1.1.0 contains updated file descriptions and an additional data file.


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