HCN formation on Jupiter - The coupled photochemistry of ammonia and Acetylene

Details HCN formation on Jupiter - The coupled photochemistry of ammonia and Acetylene HCN formation on Jupiter - The coupled photochemistry of ammonia and Acetylene

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983icar...54..417k&link_type=abstract

Icarus (ISSN 0019-1035), vol. 54, June 1983, p. 417-433. NASA-supported research.

Physics

55

Acetylene, Ammonia, Atmospheric Chemistry, Hydrocyanic Acid, Jupiter Atmosphere, Photochemical Reactions, Atmospheric Models, Pyrolysis, Recombination Reactions, Stratosphere, Troposphere, Ultraviolet Radiation, Jupiter, Phosphine, Formation, Photochemistry, Ammonia, Abundance, Models, Acetylene, Troposphere, Stratosphere, Ultraviolet, Photolysis, Density, Mixing, Clouds, Diffusion, Hydrogen Cyanide

Scientific paper

A model is presented for the formation of HCN in the upper troposphere and lower stratosphere of Jupiter by ultraviolet photolysis of the C2H5N isomer aziridine, a product of the recombination of NH2 and C2H3 radicals, which originate, respectively, from ammonia photolysis and addition of H atoms to acetylene. An HCN column density of ≡2×1017 cm-2 in the tropopause region is predicted. Sensitivity of the HCN column density to the individual rate constants and the eddy diffusion coefficient profile is discussed, as is the possibility of the existence of additional HCN-yielding pathways. Ammonia, which is saturated in the upper troposphere, is strongly depleted by photolysis in the lower stratosphere. Phosphine is also strongly depleted by photolysis and its abundance in the upper troposphere is shown to depend strongly on vertical mixing in the tropopause region. The possibility of the formation of phosphirane is considered but found to be substantially less probable than aziridine.

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