Physical properties of Deucalionis, Eos, Xanthe-type units in the central equatorial region of Mars

Details Physical properties of Deucalionis, Eos, Xanthe-type units in the central equatorial region of Mars Physical properties of Deucalionis, Eos, Xanthe-type units in the central equatorial region of Mars

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992msat.work..142s&link_type=abstract

In Lunar and Planetary Inst., Workshop on the Martian Surface and Atmosphere Through Time p 142-143 (SEE N92-28988 19-91)

Physics

Albedo, Classifications, Color, Deposits, Equatorial Regions, Mars (Planet), Mars Surface, Planetary Geology, Planetary Mapping, Viking Mars Program, Landing Sites, Morphology, Organizations, Secular Variations

Scientific paper

Classification and mapping of surficial units in the central equatorial region of Mars (30 degrees N to 20 degrees S, 57 degrees E to 75 degrees W) using enhanced color images and Mars Consortium data, identified three distinct, high albedo, relatively red surficial units in regions with intermediate to high thermal inertias. These units have distinctive properties and morphologies, occur in different, well-defined areas, and show different seasonal and secular patterns of albedo change. Deucalionis units occupy the classical albedo area of Deucalionis Regio, south of Meridiani Sinus and Sabaeus Sinus, and adjacent areas. Eos forms a bright band that separates the dark, relatively blue Meridiani-type units that dominate the southern part of the study area from intermediate albedo, relatively red Oxia units common in the north. Xanthe forms moderately bright, relatively red, Type 1B crater-streaks and uniform sheet-deposits in and adjacent to parts of Chryse Planitia, including the Viking 1 landing site. Xanthe is always associated with Oxia deposits, and has significantly lower albedos than the Eos materials, which it can be confused with.

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