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Jupiter's Whistler-mode Belts and Electron Slot Region
  • +11
  • Yixin Hao,
  • Yuri Y Shprits,
  • Doug Menietti,
  • Z.-Y. Liu,
  • Terrance F. Averkamp,
  • Dedong Wang,
  • Peter Kollmann,
  • George Blair Hospodarsky,
  • Alexander Yurievich Drozdov,
  • Elias Roussos,
  • Norbert Krupp,
  • Richard B. Horne,
  • Emma E Woodfield,
  • Scott J Bolton
Yixin Hao
GFZ German Research Centre for Geosciences

Corresponding Author:[email protected]

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Yuri Y Shprits
Helmholtz Centre Potsdam
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Doug Menietti
University of Iowa
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Z.-Y. Liu
Institut de Recherche en Astrophysique et Planétologie (IRAP)
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Terrance F. Averkamp
University of Iowa
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Dedong Wang
GFZ German Research Center for Geosciences
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Peter Kollmann
The Johns Hopkins University Applied Physics Laboratory
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George Blair Hospodarsky
University of Iowa
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Alexander Yurievich Drozdov
University of California Los Angeles
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Elias Roussos
Max Planck Institute for Solar System Research
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Norbert Krupp
Max-Planck-Institut fur Sonnensystemforschung
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Richard B. Horne
British Antarctic Survey
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Emma E Woodfield
British Antarctic Survey
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Scott J Bolton
Southwest Research Institute
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The spatial distribution of whistler-mode wave emissions in the Jovian magnetosphere measured during the first 45 perijove orbits of Juno is investigated. A double-belt structure in whistler-mode wave intensity is revealed. Between the two whistler-mode belts, there exists a region devoid of 100s keV electrons near the magnetic equator at 9 < M < 16. Insufficient source electron population in such an electron “slot” region is a possible explanation for the relatively lower wave activity compared to the whistler-mode belts. The wave intensity of the outer whistler-mode belt measured in the dusk-premidnight sector is significantly stronger than in the postmidnight-dawn sector. We suggest that the inherent dawn-dusk asymmetries in source electron distribution and/or auroral hiss emission rather than the modulation of solar cycle are more likely to result in the azimuthal variation of outer whistler-mode belt intensity during the first 45 Juno perijove orbits.
12 Mar 2024Submitted to ESS Open Archive
15 Mar 2024Published in ESS Open Archive