Altitude variation of EUV emissions and evidence for proton precipitation at low latitudes in the Saturnian atmosphere

Details Altitude variation of EUV emissions and evidence for proton precipitation at low latitudes in the Saturnian atmosphere Altitude variation of EUV emissions and evidence for proton precipitation at low latitudes in the Saturnian atmosphere

Aug 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986jgr....91.8756y&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 91, Aug. 1, 1986, p. 8756-8770.

Physics

26

Altitude, Extreme Ultraviolet Radiation, Proton Precipitation, Saturn Atmosphere, Atmospheric Models, Lyman Alpha Radiation, Particle Collisions, Radiative Transfer, Voyager Project

Scientific paper

Extreme ultraviolet observations of Saturn from Voyager 1 and 2 are analyzed. The Lyman alpha and H2 band emissions extend throughout the upper atmosphere, from the hydrocarbon homopause to well above the exobase. Analysis of the Lyman alpha emissions with a radiative transfer model indicates that the Lyman alpha source temperature is very high. This suggests that energetic protons or hydrogen atoms are responsible for a fraction of the emissions. Calculation of the solar-scattered component of the emissions based on the neutral atmosphere of Smith et al. (1983) reveals that only 1-2 kR out of a total of 3.5 kR of the observed Lyman alpha intensity is due to solar scatter for the Voyager 2 disk observations; the remainder of the Lyman alpha emissions are collisionally excited. The Lyman alpha and H2 bands are constant in longitude but decrease in local time by a factor of 2 from dawn to dusk. This correlation of the Lyman alpha and H2 band intensities is further evidence that most of the Lyman alpha is collisionally excited.

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