Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm34a..01g&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SM34A-01
Physics
5706 Aurorae, 7549 Ultraviolet Emissions
Scientific paper
The auroral emissions of Jupiter have been studied from ground-based observatories (e.g., IRTF, CFHT, Keck, Nançay), Earth-orbiting satellites (e.g., IUE, EUVE, HST, ROSAT, Chandra, XMM), flyby spacecraft (e.g., Voyager, Cassini, New Horizons), and orbiting spacecraft platforms (e.g., Galileo) at x-ray, ultraviolet, visible, infrared, and radio wavelengths. While jovian auroral processes are highly variable, the total emitted auroral power is generally a few tens of TW. The main emissions are from various compounds of hydrogen (e.g., H and H2 at UV, visible, and near-IR (2-4 μm) wavelengths; H3+ in the near-IR) excited either directly by a beam of energetic precipitating particles or by secondary electrons produced as the beam slows down in the atmosphere. Very energetic primary particles (or the heat they produce) can penetrate to beneath the homopause, resulting in hydrocarbon auroras---particularly emissions from CH4, C2H2, C2H6, and C2H4 at thermal-IR (7-16 μm) wavelengths (however, these emissions may also be excited by Joule heating). The x-ray and radio emissions are produced by the precipitating particles themselves. The emissions at different wavelengths provide unique and complimentary information about the physical processes operating in the atmospheric and magnetospheric regions where the auroras originate. Here we review our current understanding of auroral emissions from Jupiter, as revealed through multispectral observations.
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