EUV emission from Titan's upper atmosphere - Voyager 1 encounter

Details EUV emission from Titan's upper atmosphere - Voyager 1 encounter EUV emission from Titan's upper atmosphere - Voyager 1 encounter

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982jgr....87.1361s&link_type=abstract

Journal of Geophysical Research, vol. 87, Mar. 1, 1982, p. 1361-1368.

Astronomy and Astrophysics

Astronomy

131

Astronomical Spectroscopy, Extreme Ultraviolet Radiation, Nitrogen, Satellite Atmospheres, Titan, Carbon Monoxide, Electron Impact, Emission Spectra, Gas Ionization, Lyman Alpha Radiation, Upper Atmosphere, Voyager 1 Spacecraft, Saturn, Satellites, Titan, Ultraviolet, Wavelengths, Emissions, Data, Voyager 1, Atmosphere, Analysis, Spectrum, Electrons, Impacts, Nitrogen, Occultations, Composition, Mixing, Gases, Magnetosphere, Exosphere, Precipitation, Density, Dissociation, Escape, Ionization, Chemistry, Cha

Scientific paper

Most of the observed emission short of Lyman-alpha is shown to be accounted for by electron impact on N2 above 3600 km, in an analysis of Titan's EUV emission spectra obtained at the Voyager 1 encounter. It is determined that N2 is the major component of Titan's upper atmosphere, with 3900-km upper limit mixing ratios of NeI, ArI, CO, H2, and HI of 0.01, 0.06, 0.05, 0.06 and 0.1, respectively. Magnetospheric electron precipitation produces an average dayside electron density of about 3000/cu cm between 3600 and 4000 km, which is the region of bright limb emission, and magnetospheric electron impact dissociation of N2 generates an N atom escape rate of 3 x 10 to the 26th/sec from Titan's exosphere when Titan is within Saturn's magnetosphere.

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