Mars: Wind profiles and velocities, dust particles, topographic considerations
Dust enters the atmosphere of Mars from outside the planet as meteorite debris and from the surface of Mars due to atmospheric forces. In the lower 10,000 feet of the atmosphere, the suspended dust is almost exclusively of surface origin. Dust is subtracted from the atmosphere of Mars by gravitational forces. The removal of suspended matter from the atmosphere to form surface deposits is accelerated by: 1) surface friction; 2) coagulation of dust particles; 3) vapor condensation on dust; and 4) adhesion of dust to ice (H20?) crystals.
The spread of suspended dust through the atmosphere of Mars is limited to several factors: 1) the balance of forces tending to add and subtract dust described in the above paragraph; 2) vertical extent and size of turbulences in the immediate ground environment; 3) vertical extent and size of turbulences above the immediate ground environment; 4) mean wind velocities; 5) adherence of particles to the surface at contact and as a function of time. Turbulence, which may be measured by the size of eddies or vortices, dominates transport and mixing of dust in an atmosphere. Instead of molecular kinetics, as expressed by molecular viscosity, conductivity, and diffusivity, the spread of particles is described on the basis of eddy viscosity, eddy conductivity, and eddy diffusivity.
To read the rest of this article and gain access to amazing content in The Archive Blog: Planetology, become a member! You will have access to every issue of ENDEAVOR and the Enzmann Chronicles as well.
