Physics
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p51a0333t&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #P51A-0333
Physics
0305 Aerosols And Particles (0345, 4801), 3329 Mesoscale Meteorology, 3337 Numerical Modeling And Data Assimilation, 5445 Meteorology (3346), 6225 Mars
Scientific paper
The observed year-to-year repeatability of Martian atmospheric temperatures and dust opacities in northern spring and summer suggests that the seasonal cycle of Martian atmospheric dustiness cannot be explained uniquely in terms of large (regional and global scale) dust storms. Instead, a steady source of atmospheric dust is needed that generates a seasonal supply pattern that is essentially repeatable. Dust devils have been widely suggested to operate in this role. Theoretical studies to date have mainly focused on analytical models of dust devils as thermodynamic and dynamic systems. In this presentation, we discuss three-dimensional, numerical simulations of the Martian convective boundary layer, and specifically convective vortex/dust devil development. The simulations are undertaken with the Mars MM5 mesoscale atmospheric model developed at Caltech and Cornell University. The model is nonhydrostatic, and employs parameterizations for heat diffusion in the Martian subsurface, radiative heating due to dust and carbon dioxide gas in the visible and thermal infrared, radiatively and dynamically interactive dust, and (where applicable) the cycling of carbon dioxide and water between the surface and atmosphere. In these simulations of the Martian boundary layer, the model is used with a horizontal grid spacing of 20 to 100 m, and with a minimum of 100 points in each direction, and over 50 levels in the vertical direction. We initially simulate a region near the equator, with surface properties characteristic of the Sinus Meridiani ("Hematite") region and for mid southern summer. We also show simulations for a location in the northern tropics and with surface properties consistent with the Amazonis Planitia region. These simulations are conducted near southern spring equinox, a time when Mars Orbiter Camera (MOC) images suggest development of copious, massive dust devil structures. In all cases, we find evidence for the development of convective, vertically aligned vortices. We will discuss the nature and behavior of the various vortices developed in the simulations.
Ewald Shawn P.
Gierasch Peter J.
Richardson Mark I.
Toigo Alessandro
Wilson Raymond
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