Other
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufm.p31a0534c&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #P31A-0534
Other
0305 Aerosols And Particles (0345, 4801), 5409 Atmospheres: Structure And Dynamics, 5445 Meteorology (3346), 6225 Mars
Scientific paper
Within the Martian atmosphere there exist clouds composed of dust, water ice and carbon dioxide ice. These clouds are involved in the distribution and partitioning of planetary volatiles, including water vapor and carbon dioxide, within the Martian climate system through dynamics and surface exchange. Each of these clouds may influence surface properties, such as albedo and thermal inertia, or the radiative properties of the atmosphere. It is unclear to what extent or magnitude any of these influences occurs or to what extent these cloud might modify each other. In order to better understand the relative role of each cloud type a microphysical cloud and aerosol model has been incorporated into the NASA Ames Mars General Circulation Model (GCM). This cloud model incorporates the microphysical processes of nucleation, condensation and sedimentation for both water and carbon dioxide clouds. Surface exchange is modeled for both water ice and carbon dioxide ice and includes direct condensation to the surface and precipitation. A surface dust lifting scheme is employed that relates the mass of dust lifted to surface wind stress. Presented here are results of simulations compared to observations from the Thermal Emission Spectrometer (TES). In particular global cloud and water vapor distributions are compared to observations as a function of season. Vertical polar distributions of cloud particles are also compared with TES observations. Differences are discussed with respect to sources and sinks of volatiles.
Colaprete Anthony
Haberle Robert M.
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