Eolian intracrater deposits on Mars - Physical properties and global distribution

Details Eolian intracrater deposits on Mars - Physical properties and global distribution Eolian intracrater deposits on Mars - Physical properties and global distribution

Dec 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983icar...56..496c&link_type=abstract

Icarus (ISSN 0019-1035), vol. 56, Dec. 1983, p. 496-518.

Physics

64

Deposits, Mars Craters, Planetology, Thermophysical Properties, Wind Effects, Annual Variations, Data Acquisition, Infrared Radiometers, Mariner 9 Space Probe, Particle Size Distribution, Viking Orbiter Spacecraft

Scientific paper

It is noted that more than one-fourth of all craters larger than 25 km in diameter between -50 deg S and 50 deg N have localized deposits of coarse material on the floor which are associated with the dark 'splotches' that are seen visually. If homogeneous, unconsolidated materials are assumed, the measured thermal inertias of these deposits imply effective grain sizes that range from 0.1 mm to 1 cm, with a modal value of 0.9 mm. Even though these deposits are coarser and darker than the surrounding terrains and the greater part of the Martian surface, they are not compositionally distinct from materials with similar albedos. It is thought most likely that these features were formed by entrapment of marginally mobile material that can be transported into, but not out of, crater depressions by the wind. Most of the 'splotch' deposits are coarser than the dune-forming materials occurring in the north polar region and inside extreme southern latitude craters; they probably form low, broad zibar dunes or lag deposits. The distribution of intracrater deposits is seen as suggesting that the intracrater features have been buried in the interior of Arabia and that the dust deposit is less extensive at the margins and may currently be expanding.

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