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Mapping Hesperia Planum, MarsHesperia Planum, characterized by a high concentration of mare-type wrinkle ridges and ridge rings [1-4], encompasses > 2 million km2 in the southern highlands of Mars (Fig. 1). The most common interpretation is that the plains were emplaced as flood lavas with total thicknesses of <3 km [4-10]. The wrinkle ridges on its surface make Hesperia Planum the type locale for Hesperian-aged ridged plains on Mars [e.g., 9], and recent investigations reveal that wrinkle-ridge formation occurred in more than one episode [4]. Hesperia Planum s stratigraphic position and crater-retention age [e.g., 9, 11-12] define the base of the Hesperian System. However, preliminary results of geologic mapping reveal that the whole of Hesperia Planum is unlikely to be composed of the same materials, emplaced at the same geologic time. To unravel these complexities, we are generating a 1:1.5M-scale geologic map of Hesperia Planum and its surroundings (Fig. 1). To date, we have identified 4 distinct plains units within Hesperia Planum and are attempting to determine the nature and relative ages of these materials (Fig. 2) [13-15].
Document ID
20080041003
Acquisition Source
Headquarters
Document Type
Conference Paper
Authors
Gregg, Tracy K. P.
(Buffalo Univ. NY, United States)
Crown, David A.
(Planetary Science Inst. Tucson, AZ, United States)
Date Acquired
August 24, 2013
Publication Date
June 23, 2008
Publication Information
Publication: Abstracts of the Annual Meeting of Planetary Geologic Mappers, Flagstaff, AZ, 2008
Subject Category
Geophysics
Distribution Limits
Public
Copyright
Public Use Permitted.
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