Triton - Stratospheric molecules and organic sediments

Details Triton - Stratospheric molecules and organic sediments Triton - Stratospheric molecules and organic sediments

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989georl..16..981t&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 16, Aug. 1989, p. 981-984.

Other

16

Abundance, Hydrocarbons, Nitriles, Satellite Atmospheres, Stratosphere, Triton, Electron Flux Density, Methane, Nitrogen, Neptune, Satellites, Triton, Hypotheses, Stratosphere, Molecules, Flux, Organic Material, Sediments, Laboratory Studies, Experiments, Abundance, Plasma, Charged Particles, Magnetosphere, Production Rates, Condensates, Methane, Nitrogen, Photochemistry, Surface, Deposits

Scientific paper

Continuous-flow plasma discharge techniques show production rates of hydrocarbons and nitriles in N2 + CH4 atmospheres appropriate to the stratosphere of Titan, and indicate that a simple eddy diffusion model together with the observed electron flux quantitatively matches the Voyager IRIS observations for all the hydrocarbons, except for the simplest ones. Charged particle chemistry is very important in Triton's stratosphere. In the more CH4-rich case of Titan, many hydrocarbons and nitriles are produced in high yield. If N2 is present, the CH4 fraction is low, but hydrocarbons and nitriles are produced in fair yield, abundances of HCN and C2H2 in Triton's stratosphere exceed 10 to the 19th molecules/sq cm per sec, and NCCN, C3H4, and other species are predicted to be present. These molecules may be detected by IRIS if the stratosphere is as warm as expected. Both organic haze and condensed gases will provide a substantial UV and visible opacity in Triton's atmosphere.

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