UV resonance line dayglow emissions on earth and Jupiter

Details UV resonance line dayglow emissions on earth and Jupiter UV resonance line dayglow emissions on earth and Jupiter

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988jgr....9314623g&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 93, Dec. 1, 1988, p. 14623-14630.

Physics

59

Dayglow, Earth Atmosphere, Jupiter Atmosphere, Resonance Lines, Ultraviolet Spectra, Vibrational Spectra, Atmospheric Composition, Electromagnetic Scattering, Lyman Alpha Radiation, Lyman Beta Radiation, Oxygen Spectra, Upper Atmosphere

Scientific paper

The similarities and differnces between atomic resonance line emissions on earth and Jupiter are studied. For earth, the scattering of the conservative atomic oxygen triplet transition at 1304 A and the nonconservative atomic oxygen sextuplet at 989 A is considered. For Jupiter, the scattering of the conservative atomic hydrogen doublet at 1216 A and the nonconservative atomic hydrogen doublet at 1026 A are addressed. Models are presented for the intensities of the emission features as seen from a distance of several planetary radii, using the same observational geometry for both earth and Jupiter. Variations of the line-integrated emissions across the disk and near the limb of each planet are examined in detail. Line profiles for the emission near the limb and at disk-center are also studied. The models reveal the importance of including inhomogeneities and temperature variations of the atmosphere in scattering models, and indicate that outer planet emissions previously interpreted as 'electroglow' may be solely due to resonant scattering of solar emissions.

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