Simulation of Martian Cloud Formation Associated With Topography by the Planetary Weather Research and Forecasting Model

Details Simulation of Martian Cloud Formation Associated With Topography by the Planetary Weather Research and Forecasting Model Simulation of Martian Cloud Formation Associated With Topography by the Planetary Weather Research and Forecasting Model

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p23a0045i&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P23A-0045

Physics

0305 Aerosols And Particles (0345, 4801, 4906), 0320 Cloud Physics And Chemistry, 6225 Mars

Scientific paper

Martian clouds are often seen over volcanoes, Valles Marineris and troughs in Polar Regions. A basic mechanism of cloud formation is that an air parcel with water vapor is lifted in the vertical wind, becomes saturated due to colder surrounding air, and the vapor transforms to water ice. We will show simulation results of cloud formation with the Planetary Weather Research and Forecasting (planetWRF) model. It has been modified at Caltech from the terrestrial mesoscale WRF model developed mainly by the National Center for Atmospheric Research (NCAR). It can simulate, for example, the diurnal / seasonal change of wind direction and temperature profile in a limited area with high spatial resolution. Currently we have two microphysics schemes. The first includes heterogeneous nucleation, growth and sublimation of water ice particles, and sedimentation due to gravity. Particles are allowed to precipitate to the surface and form frost. The second is a much faster, simpler parameterization in which the parameter choices are based on the results of the first method. Using the latter scheme decreases the computational time greatly.

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