In planetary nomenclature , a chasma / ˈ k æ z m ə / ( plural : chasmata / ˈ k æ z m ə t ə / ) is a deep, elongated, steep-sided depression . As of 2020, the IAU has named 122 such features in the Solar System, on Venus (63), Mars (25), Saturn's satellites Mimas (6), Tethys (2), Dione (8) and Rhea (5), Uranus's satellites Ariel (7), Titania (2) and Oberon (1) and Pluto's satellite Charon (3). An example is Eos Chasma on Mars .
8-640: Echus Chasma is a chasma in the Lunae Planum high plateau north of the Valles Marineris canyon system of Mars . It is in the Coprates quadrangle . Clay has been found within it, meaning that water once sat there for a time. It may have been one of the many lakes that have been advanced for the Martian past. Research from 2010 suggests that Mars had lakes along parts of the equator, which
16-479: Is approximately 100 km long and 10 km wide, with valleys ranging in depth from around 1 km to 4 km. It is the source region of the Kasei Valles outflow channel , which extends northward from it. It is situated just west of Hebes Chasma , to which it does not connect. Chasma Below are images of some of the major chasmata of Mars. The map shows their relative locations. Parts of
24-463: Is common on Mars. However, light-toned deposits may have resulted from rivers, lakes, volcanic ash, or wind blown deposits of sand or dust. The Mars Rovers found light-toned rocks to contain sulfates . Probably having been formed in water, sulfate deposits are of great interest to scientists because they may contain traces of ancient life. Hebes Chasma, a large enclosed valley, may have once held water. Hydrated minerals have been found there. It
32-599: Is shown below in the picture of layers in the canyon wall in Coprates, as seen by Mars Global Surveyor . Because of its closeness to the Tharsis volcanic region, the rock layers may be made of layer after layer of lava flows, probably mixed with deposits of volcanic ash that fell out of the air following big eruptions. It is likely the rock strata in the walls preserve a long geological history of Mars. Dark layers may be due to dark lava flows. The dark volcanic rock basalt
40-566: Is where Echus Chasma lies. Although earlier research had showed that Mars had a warm and wet early history that has long since dried up, these lakes existed in the Hesperian Epoch, a much later period. Using detailed images from NASA's Mars Reconnaissance Orbiter , the researchers speculate that there may have been increased volcanic activity, meteorite impacts or shifts in Mars' orbit during this period to warm Mars' atmosphere enough to melt
48-523: The abundant ice present in the ground. Volcanoes would have released gases that thickened the atmosphere for a temporary period, trapping more sunlight and making it warm enough for liquid water to exist. In this study, channels were discovered that connected lake basins near Ares Vallis . When one lake filled up, its waters overflowed the banks and carved the channels to a lower area where another lake would form. These dry lakes would be targets to look for evidence ( biosignatures ) of past life. Echus Chasma
56-451: The canyon walls almost always show layers. Some layers appear tougher than others. In the image below of Ganges Chasma Layers, as seen by HiRISE , one can see that the upper, light-toned deposits are eroding much faster than the lower darker layers. Some cliffs on Mars show a few darker layers standing out and often breaking into large pieces; these are thought to be hard volcanic rock instead of soft ash deposits. An example of hard layers
64-467: The floor of Candor Chasma contains layered deposits that have been termed interior layered deposits (ILD's). These layers may have formed when the whole area was a giant lake. Some places on Mars contain hydrated sulfate deposits. Sulfate formation involves the presence of water. The European Space Agency 's Mars Express found evidence of perhaps epsomite and kieserite . Scientists want to visit these areas with robotic rovers. Images of rocks in
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