Abstract
The ionospheric response to auroral precipitation at the giant planets is reviewed, using models and observations. The emission processes for aurorae at radio, infrared, visible, ultraviolet, and X-ray wavelengths are described, and exemplified using ground- and space-based observations. Comparisons between the emissions at different wavelengths are made, where possible, and interpreted in terms of precipitating particle characteristics or atmospheric conditions. Finally, the spatial distributions and dynamics of the various components of the aurorae (moon footprints, low-latitude, main oval, polar) are related to magnetospheric processes and boundaries, using theory, in situ, and remote observations, with the aim of distinguishing between those related to internally-driven dynamics, and those related to the solar wind interaction.
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Acknowledgements
The authors acknowledge the support of EUROPLANET RI project (Grant agreement no.: 228319) funded by EU; and also the support of the International Space Science Institute (Bern). SVB was supported by a Royal Astronomical Society Research Fellowship. MG was partially supported by the Science and Technology Facilities Council (STFC) through the Consolidated Grant to Imperial College London. C. Tao was supported by a JSPS Postdoctoral Fellowship for Research Abroad. The Editor thanks the work of two anonymous referees.
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Badman, S.V., Branduardi-Raymont, G., Galand, M. et al. Auroral Processes at the Giant Planets: Energy Deposition, Emission Mechanisms, Morphology and Spectra. Space Sci Rev 187, 99–179 (2015). https://doi.org/10.1007/s11214-014-0042-x
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DOI: https://doi.org/10.1007/s11214-014-0042-x