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Observing the sun at four different wavelengths (450, 670, 880 & 990 nm) allows us to measure the amount of dust suspended in the Martian atmosphere. Particle size (and any growth from water vapour condensation at night) can be inferred and compared to measurements of actual dust grains in the Beagle 2 microscope images.
Dust is raised from the surface by wind action (particularly dust devils) and then slowly settles out again at a different location. During the Southern Hemisphere spring and summer dust storms commonly occur obscuring large areas of the Martian surface (and occasionally the entire globe).
15th February 2001