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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Badman, S.V. et al. (2016). Auroral Processes at the Giant Planets: Energy Deposition, Emission Mechanisms, Morphology and Spectra. In: Szego, K., et al. The Magnetodiscs and Aurorae of Giant Planets. Space Sciences Series of ISSI, vol 50. Springer, New York, NY. https://doi.org/10.1007/978-1-4939-3395-2_5
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