Depletion of Ammonia Gas onto Jovian Ices

Details Depletion of Ammonia Gas onto Jovian Ices Depletion of Ammonia Gas onto Jovian Ices

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p11c1351k&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #P11C-1351

Physics

[6220] Planetary Sciences: Solar System Objects / Jupiter

Scientific paper

The altitude profile of ammonia in Jupiter’s atmosphere, as constrained by microwave spectra, is poorly understood. The microwave spectrum of Jupiter is consistent with supersolar ammonia deeper than 6 bar, and subsolar ammonia at pressures less than 2 bar. In addition, the Galileo Probe Mass Spectrometer measured a deep NH3/H2 mixing ratio of approximately five times the protosolar ratio. Consequently, a global-scale depletion mechanism for ammonia gas can be anticipated, operating between the 2 and 6 bar levels. Candidate depletion mechanisms include dynamics, condensation of species with higher nitrogen fractions than NH4SH (including clathrates), and adsorption of ammonia onto NH4SH or water ices. Measured uptake coefficients of ammonia provide valuable constraints for model calculations testing the ammonia depletion hypothesis in Jupiter’s atmosphere. We have begun laboratory experiments designed to measure the uptake of ammonia by H2O and H2O-NH4SH ice mixtures with a Knudsen cell apparatus in the temperature range 130-250 K. These conditions are appropriate to the troposphere of Jupiter around the 2-4 bar pressure level. Initial results show that the uptake coefficient is larger than 10-4 in this temperature range. We also plan model calculations to apply the experimental results to Jupiter's atmosphere and will discuss the key parameters and processes that influence the ammonia uptake and their relevance to Jupiter's atmosphere. This work is supported by the NASA Planetary Atmospheres Program under grant NNX09AB69G.

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