3-Dimmensional Simulation of Storm Dynamics on the Giant Planets

Details 3-Dimmensional Simulation of Storm Dynamics on the Giant Planets 3-Dimmensional Simulation of Storm Dynamics on the Giant Planets

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999dps....31.6509h&link_type=abstract

American Astronomical Society, DPS meeting #31, #65.09

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The formation and evolution of convective clouds in the Jovian atmosphere is investigated using an anelastic three dimmensional time-dependent model with parameterized microphysics. The model is a finite-differences one using a non staggered grid. A dimmensional splitting methodology is employed to separate the advective terms from the source terms in the system of non linear equations. A Crank-Nicholson technique is used to solve the advective terms and the source terms are calculated forward in time. The pressure perturbartion is solved using a multigrid method. Sub-grid scale motions are incorporated by means of a one and a half order closure scheme. Previous one and two dimmensional models for axisymmetric local convection fail to incorporate wind shears and the Coriolis effect. The vertical wind shear has an strong influence in the development of organized convection on the Earth and can be very important in Jupiter according to the depth dependence of the zonal winds found by the Galileo Probe. The Coriolis effect is also important for convective storms in mid and high latitudes. The role of water and ammonia in moist convection is investigated with varying deep concentrations. The results of our computations are compared with the dynamics of a singular storm observed at high resolution by the Voyager 1 on Jupiter's South Equatorial Belt in February 1979. The model is designed to be run on the four giant planets to compare how moist convection operates in each case.

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