Electron acceleration to MeV energies at Jupiter and Saturn

Kollmann, P.; Roussos, E.; Paranicas, C.; Woodfield, Emma E. ORCID: https://orcid.org/0000-0002-0531-8814; Mauk, B.H.; Clark, G.; Smith, D.C.; Vandegriff, J.. 2018 Electron acceleration to MeV energies at Jupiter and Saturn. Journal of Geophysical Research: Space Physics, 123 (11). 9110-9129. https://doi.org/10.1029/2018JA025665

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Text ©2018. The Authors. This is an open access article under the terms of the Creative Commons Attribution License, which permits use, distribution and reproduction in any medium, provided the original work is properly cited. Kollmann_et_al-2018-Journal_of_Geophysical_Research__Space_Physics.pdf - Published Version Available under License Creative Commons Attribution 4.0. Download (3MB) | Preview

Abstract/Summary

The radiation belts and magnetospheres of Jupiter and Saturn show significant intensities of relativistic electrons with energies up to tens of MeV. To date, the question on how the electrons reach such high energies is not fully answered. This is largely due to the lack of high‐quality electron spectra in the MeV energy range that models could be fit to. We reprocess data throughout the Galileo orbiter mission in order to derive Jupiter's electron spectra up to tens of MeV. In the case of Saturn, the spectra from the Cassini orbiter are readily available and we provide a systematic analysis aiming to study their acceleration mechanisms. Our analysis focuses on the magnetospheres of these planets, at distances of L > 20 and L > 4 for Jupiter and Saturn, respectively, where electron intensities are not yet at radiation belt levels. We find no support that MeV electrons are dominantly accelerated by wave‐particle interactions in the magnetospheres of both planets at these distances. Instead, electron acceleration is consistent with adiabatic transport. While this is a common assumption, confirmation of this fact is important since many studies on sources, losses, and transport of energetic particles rely on it. Adiabatic heating can be driven through various radial transport mechanisms, for example injections driven by the interchange instability or radial diffusion. We cannot distinguish these processes at Saturn with our technique. For Jupiter, we suggest that the dominating acceleration process is radial diffusion because injections are never observed at MeV energies.

Item Type:	Publication - Article
Digital Object Identifier (DOI):	https://doi.org/10.1029/2018JA025665
ISSN:	21699380
Additional Keywords:	radiation belts, energetic particles
Date made live:	08 Nov 2018 15:22 +0 (UTC)
URI:	https://nora.nerc.ac.uk/id/eprint/521449

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