Publication Abstracts

Carlson et al. 1987

Carlson, B.E., M.J. Prather, and W.B. Rossow, 1987: Cloud chemistry on Jupiter. Astrophys. J., 322, 559-572, doi:10.1086/165751.

Chemical equilibrium models have been used to interpret observations and constrain models of Jupiter. We reexamine the chemical reactions controlling the composition of the cloud-forming region from 10 to 0.1 bar and the thermodynamic data used in these models. Aqueous reactions decrease the abundances of NH3 and H2S; these reactions prevent the transport of CO2 from deeper levels, with little or no effect on the abundances of CO or weakly basic species such as PH3. Formation of NH4SH rapidly removes most of the H2S, while for a solar N/S ratio the NH3 abundance decreases by only 20%. If, as suggested by de Pater, the H2S abundance is enhanced by a factor of 5, formation of NH4SH would deplete NH3 by as much as 70% and still be consistent with the observations. Measurements of near solar abundances of NH3 in the 1 bar region require enhanced abundances at depth to offset depletions due to chemical reactions in the clouds. Best agreement with the observations is found for 2 times solar abundances of N, O, and S relative to H.

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BibTeX Citation

  author={Carlson, B. E. and Prather, M. J. and Rossow, W. B.},
  title={Cloud chemistry on Jupiter},
  journal={Astrophys. J.},

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RIS Citation

ID  - ca00700d
AU  - Carlson, B. E.
AU  - Prather, M. J.
AU  - Rossow, W. B.
PY  - 1987
TI  - Cloud chemistry on Jupiter
JA  - Astrophys. J.
VL  - 322
SP  - 559
EP  - 572
DO  - 10.1086/165751
ER  -

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