An updated view of Jupiter's UV main auroral emission: large-scale analysis of UV and particle data from Juno's first 60 orbits
Abstract
The properties and origins of Jupiter's UV main auroral emission are, at present, not yet fully understood, particularly the extent to which its two distinct zones, the Zone-I and Zone-II aurora, originate from a common source. In this work, remote-sensing and in-situ data from the Juno spacecraft are used to investigate and produce maps of the average properties of the main emission over Juno's first 60 orbits. It is found that the peak in mean energy of electrons precipitating in the main emission is consistently poleward of the energy-flux (or brightness) peak, in both hemispheres and at all local times, and is co-located with the statistical location of the Zone-II aurora. Evidence is presented that the flux-energy relationship of the main emission is adequately characterised by theoretical power laws describing electron acceleration from quasi-static potentials or Alfvénic turbulence and that it shows a modulation with ionospheric electron density consistent with theoretical predictions. Finally, the average energy spectra of precipitating electrons in the Zone-I aurora remain power-law-like between an energy flux of 1 and 100 mW m−2, whereas the average Zone-II spectra develop a distinct ``plateau'' or ``flattop'' shape beyond an energy flux of ∼5 mW m−2. Our results provide some evidence that the Zone-I and Zone-II aurorae are phenomenologically distinct, and the consequences of this interpretation for future investigation of the main emission are discussed.
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BibTeX
@misc{head2026updated,
title = {{An updated view of Jupiter's UV main auroral emission: large-scale analysis of UV and particle data from Juno's first 60 orbits}},
author = {Linus Head and Denis Grodent and Bertrand Bonfond and Nicholas Kruegler and Ali Sulaiman and George Clark and Bilal Benmahi and Guillaume Sicorello and Julie Vinesse and Thomas Greathouse and Rohini Giles and Barry Mauk},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.16602},
eprint = {2610.16602},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.16602},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - An updated view of Jupiter's UV main auroral emission: large-scale analysis of UV and particle data from Juno's first 60 orbits
AU - Linus Head
AU - Denis Grodent
AU - Bertrand Bonfond
AU - Nicholas Kruegler
AU - Ali Sulaiman
AU - George Clark
AU - Bilal Benmahi
AU - Guillaume Sicorello
AU - Julie Vinesse
AU - Thomas Greathouse
AU - Rohini Giles
AU - Barry Mauk
PY - 2026
DA - 2026/10/12
PB - arXiv
DO - 10.48550/arxiv.2610.16602
UR - https://arxiv.org/abs/2610.16602
AB - The properties and origins of Jupiter's UV main auroral emission are, at present, not yet fully understood, particularly the extent to which its two distinct zones, the Zone-I and Zone-II aurora, originate from a common source. In this work, remote-sensing and in-situ data from the Juno spacecraft are used to investigate and produce maps of the average properties of the main emission over Juno's first 60 orbits. It is found that the peak in mean energy of electrons precipitating in the main emission is consistently poleward of the energy-flux (or brightness) peak, in both hemispheres and at all local times, and is co-located with the statistical location of the Zone-II aurora. Evidence is presented that the flux-energy relationship of the main emission is adequately characterised by theoretical power laws describing electron acceleration from quasi-static potentials or Alfvénic turbulence and that it shows a modulation with ionospheric electron density consistent with theoretical predictions. Finally, the average energy spectra of precipitating electrons in the Zone-I aurora remain power-law-like between an energy flux of 1 and 100 mW m^−2, whereas the average Zone-II spectra develop a distinct ``plateau'' or ``flattop'' shape beyond an energy flux of ∼5 mW m^−2. Our results provide some evidence that the Zone-I and Zone-II aurorae are phenomenologically distinct, and the consequences of this interpretation for future investigation of the main emission are discussed.
ER -