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Mars: Troughed terrain

Sharp, Robert P. (1973) Mars: Troughed terrain. Journal of Geophysical Research, 78 (20). pp. 4063-4072. ISSN 0148-0227. doi:10.1029/JB078i020p04063.

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An assemblage of huge parallel troughs, individually up to 200 km wide and hundreds of kilometers long, forms a belt 500 km wide extending for 2700 km E 15°S through the Tithonius Lacus-Coprates region of equatorial Mars. Some troughs are closed depressions more than 3 km deep, and the maximum trough depth may approach 6 km. These troughs, heading just southeast of the huge Tharsis volcanic ridge, are transitional westward into a festoon of U-shaped hollows and eastward into chaotic and fretted terrain. Parallel linear chains of rimless pits and shallow graben on the adjacent cratered upland suggest structural control of trough development by fractures in the Martian crust. Trough walls show scarring by slides, slumps, and U-shaped avalanche chutes. Some are dissected into narrow sharp anastomosing ridges reminiscent of badland topography. Dendritic tributaries extend 150 km into the bordering upland. These tributaries and the mass movements causing recession of trough walls are attributed to a sapping process possibly involving the evaporation or melting of exposed ground ice. Trough floors range from chaotically rough to rolling and subdued. They are not smoothly graded. In one instance layered materials, possibly 2 km thick, compose a dissected trough floor tableland. Most troughs may be partly filled by such deposits. The major problem of trough genesis involves disposal of about 2 × 10^6 km^3 of material. Running water, solution, deflation, and ground ice deterioration all appear to have significant limitations as the sole or principal agent of trough formation. Subsidence caused by magma withdrawal to supply the extensive nearby volcanic fields or the spreading of crustal plates are both quantitatively adequate. Crustal spreading would have significant implications concerning the conditions and the behavior of the Martian interior, and the lack of any obvious subduction zones would imply planetary expansion. In our ignorance concerning Mars both magma withdrawal and crustal spreading merit continued consideration in respect to trough formation, with some favor to the former because of the obvious large-scale Martian volcanism. Ground ice may have played a significant subsidiary role through sapping to produce extensive recession of trough walls.

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Additional Information:Copyright 1973 by the American Geophysical Union. (Received January 4, 1973; revised March 15, 1973.) So many people have played a part in contributing to the success of the Mariner 9 photographic mission that to enumerate any by name does disservice to others unmentioned. Those people who have had a role in this great scientific adventure will know it and hopefully will take satisfaction from the publication of the results. Contribution 2265, Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California.
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Caltech Division of Geological and Planetary Sciences2265
Issue or Number:20
Record Number:CaltechAUTHORS:20141106-163037022
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Official Citation:Sharp, R. P. (1973), Mars: Troughed terrain, J. Geophys. Res., 78(20), 4063–4072, doi:10.1029/JB078i020p04063.
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:51406
Deposited By: George Porter
Deposited On:07 Nov 2014 01:41
Last Modified:10 Nov 2021 19:10

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