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V. L. Lamothe (SUNY Buffalo), J. I. Moses (LPI)
Because the altitude regions for CH4 and NH3 photodissociation are physically separated from each other in the Jovian atmosphere, the possibility of forming organo-nitrogen compounds on Jupiter has been an uncertain problem [1,2,3,4,5]. Carbon- and nitrogen-bearing species do not interact significantly in laboratory experiments involving ultraviolet irradiation of CH4-NH3-H2 mixtures [6,7]. However, HCN and a variety of complex organo-nitrogen molecules are produced when methane in the above experiments is replaced by unsaturated hydrocarbons such as C2H2 or CH3C2H [8,9]. To determine the formation efficiency of organo-nitrogen compounds on Jupiter, we have added the reaction schemes proposed by [3,8,9] to a photochemical model of the Jovian troposphere and stratosphere. We find that HCN does not form in observable quantities unless a large tropospheric source of C2H2 exists (e.g., via lightning-induced chemistry, see ). Organo-nitrogen reactions are unlikely to be important on Jupiter --- chromophores are most likely due to inorganic compounds. References:\/  Strobel, D. F. (1973), J. Atmos. Sci.\ 30, 1205;  Kaye, J. A., and D. F. Strobel (1983a), Icarus\ 55, 399;  Kaye, J. A., and D. F. Strobel (1983b), Icarus\ 54, 417;  Tokunaga, A. T. et al.\/ (1981), Icarus\ 48, 283;  Bézard, B. et al.\/ (1995), Icarus\ 118, 384;  Raulin, F. et al. (1979), Icarus\ 38, 358;  Ferris, J. P., and J. Y. Morimoto (1981), Icarus\ 48, 118;  Ferris, J. P., and Y. Ishikawa (1988), J. Am. Chem. Soc.\ 110, 4306;  Ferris, J. et\ al.\/ (1992), Icarus\ 95, 54;  Bétremieux, Y., and R. V. Yelle (1999), BAAS\ 31, 1180.