Nitrogen airglow sources - Comparison of Triton, Titan, and earth

Details Nitrogen airglow sources - Comparison of Triton, Titan, and earth Nitrogen airglow sources - Comparison of Triton, Titan, and earth

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991georl..18..689s&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 18, April 1991, p. 689-692.

Physics

29

Airglow, Earth Atmosphere, Nitrogen Ions, Satellite Atmospheres, Titan, Triton, Comparison, Magnetospheric Electron Density, Upper Atmosphere, Planets, Nitrogen, Origin, Source, Earth, Triton, Titan, Satellites, Neptune, Saturn, Airglow, Atmosphere, Solar Effects, Magnetosphere, Magnetic Effects, Spacecraft Observations, Voyager Missions, Emissions, Uvs Instrument, Spectra, Comparisons, Intensity, Precipitation, Models, Electrons, Theoretical Studies, Radiation

Scientific paper

The individual contributions of direct solar excitation, photoelectron excitation, and magnetospheric electron excitation of Triton and Titan airglow observed by the Voyager Ultraviolet Spectrometer (UVS) are quantified. The principal spectral features of Triton's airglow are shown to be consistent with precipitation of magnetospheric electrons with power dissipation about 500 million W. Solar excitation rates of the dominant N2 and N(+) emission features are factors of 2-7 weaker than magnetospheric electron excitation. On Titan, the calculated disk center and bright limb N(+) 1085 A intensities due to solar excitation agree with observed values, while the 970 A feature is mostly N21 c5 band emission. The calculated LBH intensity by photoelectrons suggests that magnetospheric electrons play a minor role in Titan's UV airglow. On earth, solar/photoelectron excitation explains the observed N(+) 1085 A and LBH intensites and accounts for only 40 percent of the N(+) 916 A intensity.

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