Numerical Modeling Of Moist Convection In Jupiter's Atmosphere With H2O, NH3, And NH4SH Clouds

Details Numerical Modeling Of Moist Convection In Jupiter's Atmosphere With H2O, NH3, And NH4SH Clouds Numerical Modeling Of Moist Convection In Jupiter's Atmosphere With H2O, NH3, And NH4SH Clouds

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.1112s&link_type=abstract

American Astronomical Society, DPS meeting #38, #11.12; Bulletin of the American Astronomical Society, Vol. 38, p.497

Physics

Scientific paper

We develop a two-dimensional numerical model that incorporates condensation of water and ammonia and production reaction of ammonium hydrogensulfide in order to simulate the Jovian moist convection. The stable layers corresponding to these volatiles may affect to the vertical structure of convection, since our estimation of static stability evaluated from the difference between moist and dry adiabats show that each static stability corresponding to ammonia and ammonium hydrogensulfide is as large as 1/3 and 1/5 of that corresponding to water, respectively (Sugiyama et al.,2006). The basic equation of the model is based on quasi-compressible system (Klemp and Wilhelmson, 1978). The cloud microphysics is implemented by using the warm rain bulk parameterization that is used in Nakajima et al. (2000). In this parameterization, each condensible species is divided into three categories "vapor", "cloud", and "rain", and the conversion rate between each category is parameterized. Radiative forcing is given as a function of height.
We successfully perform a preliminary simulation of cloud layers of water, ammonia, ammonium hydrogensulfide by using the same settings as Nakajima et al. (2000). At the conference, we will present a structure of moist convection in Jupiter's atmosphere that established through a large number of life cycles of convective cloud elements, and discuss how stable layers corresponding to these volatiles affect to the vertical structure.

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