On the binary nucleation of NH4SH in the troposphere of giant planets

Details On the binary nucleation of NH4SH in the troposphere of giant planets On the binary nucleation of NH4SH in the troposphere of giant planets

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007epsc.conf..564g&link_type=abstract

European Planetary Science Congress 2007, Proceedings of a conference held 20-24 August, 2007 in Potsdam, Germany. Online at ht

Physics

Scientific paper

This contribution addresses the formation of solid NH4SH (ammonium hydrogensulfide) nuclei in the troposphere of Jupiter, because based on thermochemical considerations it is believed, that a NH4SH cloud layer exists in the Jovian atmosphere at pressure values between (1 - 2) bar beneath an outermost NH3 cloud (cf. e.g. Rossow (1978), Weidenschilling & Lewis (1973), Atreya et al. (1999)). Since the nominal molecule (monomer) is not present under these tropospheric conditions, the formation of NH4SH nuclei has to be treated by application of a binary nucleation theory. The binary stationary nucleation rate of homogeneous ammonium hydrogensulfide particles is derived here based on the arguments of Mirabel & Katz (1973) and Reiss (1950). We give first results of this modelling approach and discuss further extensions and perspectives aiming at the calculation of clouds in (extra-solar) giant planet atmospheres. References: Atreya S.K., Wong M.H., Owen T.C., Mahaffy P.R., Niemann H.B., de Pater I., Drossart P. & Encrenaz Th. 1999, P& SS, 47, 1243 Mirabel P., Katz J.L. 1973, J. Chem. Phys. 60, 1138 Reiss H. 1950, J. Chem. Phys. 18, 840 Rossow W.B. 1978, Icar. 36, 1 Weidenschilling S.J. & Lewis J.S. 1973, Icar. 20, 405

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