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Volume 147, 2010
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On the abundance of non-cometary HCN on Jupiter

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Using one-dimensional thermochemical/photochemical kinetics and transport models, we examine the chemistry of nitrogen-bearing species in the Jovian troposphere in an attempt to explain the low observational upper limit for HCN. We track the dominant mechanisms for interconversion of N2–NH3 and HCN–NH3 in the deep, high-temperature troposphere and predict the rate-limiting step for the quenching of HCN at cooler tropospheric altitudes. Consistent with some other investigations that were based solely on time-scale arguments, our models suggest that transport-induced quenching of thermochemically derived HCN leads to very small predicted mole fractions of hydrogen cyanide in Jupiter's upper troposphere. By the same token, photochemical production of HCN is ineffective in Jupiter's troposphere: CH4–NH3 coupling is inhibited by the physical separation of the CH4 photolysis region in the upper stratosphere from the NH3 photolysis and condensation region in the troposphere, and C2H2–NH3 coupling is inhibited by the low tropospheric abundance of C2H2. The upper limits from infrared and submillimetre observations can be used to place constraints on the production of HCN and other species from lightning and thundershock sources.

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The article was received on 11 Mar 2010, accepted on 07 Apr 2010 and first published on 09 Aug 2010

Article type: Paper
DOI: 10.1039/C003954C
Citation: Faraday Discuss., 2010,147, 103-136
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    On the abundance of non-cometary HCN on Jupiter

    J. I. Moses, C. Visscher, T. C. Keane and A. Sperier, Faraday Discuss., 2010, 147, 103
    DOI: 10.1039/C003954C

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