MOC images also reveal amazing layered outcrops on the floors of some of the Valles Marineris canyons. An example of the wall rock layers can be seen in MOC image 8403, shown above (C). MOC images led to the realization that there are layers in the walls that go down to great depths. The Mars Orbiter Camera on board Mars Global Surveyor has been examining these layers at much higher resolution than was available previously. Some hints of layering in both the canyon walls and within some deposits on the canyon floors were seen in Mariner 9 and Viking orbiter images from the 1970s. Valles Marineris was first observed in 1972 by the Mariner 9 spacecraft, from which the troughs get their name: Valles-valleys, Marineris-Mariner. One of the most striking discoveries of the Mars Global Surveyor mission has been the identification of thousands of meters/feet of layers within the wall rock of the enormous martian canyon system, Valles Marineris. Tiu and Simud Valles consist of a complex of The channel begins at a 2- to 3-km-deep circular depression within a large impact crater, whose floor is partly covered by chaotic material, and ends in Simud Valles. Shalbatana is relatively narrow (10 km wide) but can reach 3 km in depth. This terrain is about 9 km above datum near Valles Marineris and steadily decreases in elevation to 1 km below datum in the Chryse basin. The south Chryse outflow channels are cut an average of 1 km into the cratered highland terrain. Many of the channels flowed north into Chryse Basin. Huge ancient river channels began from Valles Marineris and from adjacent canyons and ran north. Layers of material in the eastern canyons might consist of carbonates deposited in ancient lakes, eolian deposits, or volcanic materials. The connected chasma or valleys of Valles Marineris may have formed from a combination of erosional collapse and structural activity. and from longitude 15 degrees to 102.5 degrees. The image roughly extends from latitude 20 degrees S. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color Mercator projection. The mouth of Ares Valles is the site of the Mars Pathfinder lander. The chaos in the southeast part of the image gives rise to several outflow channels, Shalbatana, Simud, Tiu, and Ares Valles (left to right), that drained north into the Chryse basin. Eos and Capri Chasmata (south to north) are two canyons connected to Valles Marineris. The scene shows the entire Valles Marineris canyon system, over 3,000 km long and averaging 8 km deep, extending from Noctis Labyrinthus, the arcuate system of graben to the west, to the chaotic terrain to the east and related outflow canyons that drain toward the Chryse basin. Valles Marineris and Chryse Outflow ChannelsĪ color image of Valles Marineris, the great canyon and the south Chryse basin- Valles Marineris outflow channels of Mars north toward top.
Many of the channels flowed north into Chryse Basin, which contains the site of the Viking 1 Lander and the future site of the Mars Pathfinder Lander. Layers of material in the eastern canyons might consist of carbonates deposited in ancient lakes. and from longitude 45 degrees to 102.5 degrees. The image extends from latitude 0 degrees to 20 degrees S.
The scene shows the entire canyon system, over 3,000 km long and averaging 8 km deep, extending from Noctis Labyrinthus, the arcuate system of graben to the west, to the chaotic terrain to the east. A color image of Valles Marineris, the great canyon of Mars north toward top.
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