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\begin{document}

\title{Jupiter's Whistler-mode Belts and Electron Slot Region}



\author[1]{Yixin Hao}%
\author[2]{Yuri Y Shprits}%
\author[3]{Doug Menietti}%
\author[4]{Z.-Y. Liu}%
\author[3]{Terrance F. Averkamp}%
\author[5]{Dedong Wang}%
\author[6]{Peter Kollmann}%
\author[3]{George Blair Hospodarsky}%
\author[7]{Alexander Yurievich Drozdov}%
\author[8]{Elias Roussos}%
\author[9]{Norbert Krupp}%
\author[10]{Richard B. Horne}%
\author[10]{Emma E Woodfield}%
\author[11]{Scott J Bolton}%
\affil[1]{GFZ German Research Centre for Geosciences}%
\affil[2]{Helmholtz Centre Potsdam}%
\affil[3]{University of Iowa}%
\affil[4]{Institut de Recherche en Astrophysique et Planétologie (IRAP)}%
\affil[5]{GFZ German Research Center for Geosciences}%
\affil[6]{The Johns Hopkins University Applied Physics Laboratory}%
\affil[7]{University of California Los Angeles}%
\affil[8]{Max Planck Institute for Solar System Research}%
\affil[9]{Max-Planck-Institut fur Sonnensystemforschung}%
\affil[10]{British Antarctic Survey}%
\affil[11]{Southwest Research Institute}%


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  \date{May 18, 2024}


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\begin{abstract}
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 \textless{}
M \textless{} 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.%
\end{abstract}%



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