Martian channel morphology - Maja and Kasei Valles

Details Martian channel morphology - Maja and Kasei Valles Martian channel morphology - Maja and Kasei Valles

Dec 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979jgr....84.7961b&link_type=abstract

Journal of Geophysical Research, vol. 84, Dec. 30, 1979, p. 7961-7983.

Astronomy and Astrophysics

Astrophysics

34

Channels, Geomorphology, Mars Surface, Photogeology, Planetary Mapping, Valleys, Erosion, Geochronology, Image Processing, Mars Craters, Mars Photographs, Photomapping, Satellite-Borne Photography, Topography, Viking Spacecraft

Scientific paper

Detailed geomorphic mapping from Viking imagery of selected portions of Kasei Vallis, Maja Vallis, and vicinity reveals numerous similarities of channel morphology to erosional and depositional features of the Channeled Scabland. Characteristic scabland landforms which occur in Kasei and Maja Valles include erosional grooves, streamlined uplands and hills, scour zones around flow obstacles, inner channels with erosional head cuts, breached ridges and basin (crater) rims, pendant forms (bars), erosional terracing of streamlined hills and channel margins, and possible midchannel bars. These features constitute an assemblage of landforms which on earth is most characteristic of catastrophic flood channeling in jointed bedrock. Prominent mass wastage and sapping features are associated with the high-wall relief in lower Kasei Vallis. Many cliffs along the channel margins exhibit steep upper slopes and gentler lower talus slopes which form the spur-and-gully topography that has also been described along chasma walls in the Valles Marineris. Landslides, debris fans, and debris cones can also be recognized. Much less wall modification occurs in the shallower Maja Vallis. Probably, the steep escarpments of Kasei were created by tectonic processes and subsequent channel incision. These escarpments later receded by mass wasting and sapping.

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