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Eolian intracrater deposits on Mars - Physical properties and global distributionIt 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.
Document ID
19840037450
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Christensen, P. R.
(Arizona State University Tempe, AZ, United States)
Date Acquired
August 12, 2013
Publication Date
December 1, 1983
Publication Information
Publication: Icarus
Volume: 56
ISSN: 0019-1035
Subject Category
Lunar And Planetary Exploration
Accession Number
84A20237
Funding Number(s)
CONTRACT_GRANT: NSG-7548
CONTRACT_GRANT: NAGW-263
Distribution Limits
Public
Copyright
Other

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