Martian chaos terrain - AbsoluteAstronomy.com

Chaos terrain on Mars

Chaos terrain on Mars is distinctive; nothing on Earth compares to it. Chaos terrain generally consists of irregular groups of large blocks, some tens of kilometres across and a hundred or more meters high. The tilted and flat topped blocks form depressions hundreds of metres deep. A chaotic region can be recognized by a rat's nest of mesas, buttes, and hills, chopped through with valleys which in places look almost patterned. Some parts of this chaotic area have not collapsed completely—they are still formed into large mesas, so they may still contain water ice. Chaos regions formed long ago. By counting craters (more craters in any given area means an older surface) and by studying the valleys' relations with other geological features, scientists have concluded the channels formed 2.0 to 3.8 billion years ago.

Locations

The greatest concentrations of chaotic terrain are in the same locations as giant, ancient river valleys. Because so many large channels seem to originate from chaotic terrain, it is widely believed that chaos terrain is caused by water coming out the ground in the form of massive floods. Most of the chaotic terrain exists in the highlands of Mars, south of Chryse Planitia

Chryse Planitia

Chryse Planitia is a smooth circular plain in the northern equatorial region of Mars close to the Tharsis region to the west, centered at . Chryse Planitia lies partially in the Lunae Palus quadrangle and partially in the Oxia Palus quadrangle...

, in the Oxia Palus quadrangle

Oxia Palus quadrangle

The Oxia Palus quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey Astrogeology Research Program. The Oxia Palus quadrangle is also referred to as MC-11 ....

, and along the Martian dichotomy

Martian dichotomy

The most conspicuous feature of Martian surface geology is a sharp contrast, known as the Martian dichotomy, between the rugged southern highlands and the relatively smooth northern basins. The two hemispheres differ in elevation by 1 to 3 km...

. But some chaos regions can be found in Margaritifer Sinus quadrangle

Margaritifer Sinus quadrangle

The margaritifer Sinus quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey Astrogeology Research Program. The Margaritifer Sinus quadrangle is also referred to as MC-19 ....

, Phaethontis quadrangle

Phaethontis quadrangle

The Phaethontis quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey Astrogeology Research Program. The Phaethontis quadrangle is also referred to as MC-24 ....

, and Lunae Palus quadrangle

Lunae Palus quadrangle

The Lunae Palus quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey Astrogeology Research Program. The quadrangle is also referred to as MC-10 ....

Theories for formation

Many different theories have been advanced for how floods of water came to be released with the formation of chaotic terrain. Evidence for the involvement of water has been found—minerals associated with water, such as grey, crystalline hematite

Hematite

Hematite, also spelled as haematite, is the mineral form of iron oxide , one of several iron oxides. Hematite crystallizes in the rhombohedral system, and it has the same crystal structure as ilmenite and corundum...

and phyllosilicates, are present in chaos regions. Many explanations for the creation of chaos involve the sudden melting of giant reservoirs of ground ice. Some researchers have suggested that a frozen layer, called a cryosphere, developed over a long time period and then something triggered it to rupture and melt suddenly. The rupturing event may have been impacts,
magma movements, seismic activity, volcanic tectonic strains, increased pore pressure, or the dissociation of clathrates. A clathrate composed of carbon dioxide and methane could have explosively dissociated, thereby liquefying water-saturated sediments. A variation of this idea of a cryosphere is that an aquifer was created along with the cryosphere. As more and more ice was added resulting in a thicker cryosphere, the water in the aquifer became pressurized. When something like an impact or movement of magma broke or melted the cryosphere, floods of water under great pressure were released. However, further calculations showed that the great channels could not have been produced with just a single discharge. Later proposals advanced the notion that the geological shapes present in chaos regions could have been made by a series of over a 100 flooding events.

Melting of buried ice

More recently, researchers have suggested ways for the formation of chaos without the need for a special triggering event. Tanja Zegers and others calculated that the simple burial of ice-rich sediments could result in the release of huge amounts of water leading to the formation of the large river basins that are associated with most chaos terrains. The group studied Aram Chaos

Aram Chaos

Aram Chaos, centered at 2.6°N, 21.5°W, comprises a heavily eroded impact crater on the planet Mars. It lies at the eastern end of the large canyon Valles Marineris and close to Ares Vallis. Various geological processes have reduced it to a circular area of chaotic terrain...

; a large region of chaos that probably began as a large impact crater. In their model, ice-rich material accumulated in the crater and then became covered with sediment, which prevented the ice from disappearing into the thin atmosphere. Eventually, the heat from the deep subsurface together with the insulating qualities of the covering layer produced a thick water layer. Since dense materials tend to sink into water, the overlying rock broke under the strain. The dense, rocky cap fractured into various sized, tilted blocks. The melt water went to the top and made a channel which eroded more and more as water rushed outward. Along with water from other chaotic regions, there would have been enough erosive force to carve the large river valleys we now observe. There is ample evidence for buried deposits of ice in the form of glaciers, preserved under a thin covering of rock and dirt.
It also seems that Mars has had many ice ages in which ice was deposited, then later buried. These ice ages are caused by the frequent large changes in the tilt of the planet. The tilt of the spin axis of Mars is highly variable due to the lack of a large moon. Observations of many craters have shown that many craters are mostly full of sediments—ice could be one of the sediments. Many craters appear to be very shallow, but observations of younger craters have demonstrated that impact craters start out as sort of bowl shaped; hence a crater that today looks shallow has probably been filled with sediments. Research, published by Rodriguez and others in 2005, suggested that the subsurface of Mars contains an accumulation of old craters that may be filled with water or ice.

Sublimation of an ice-rich layer

Some regions of chaos may have been produced by another means. Galaxias Chaos is different from many other chaotic regions. It does not have associated outflow channels, and it does not display a great elevation difference between it and the surrounding land area, as most of the other chaos regions. Research by Pedersen and Head, published in 2010, suggests that Galaxias Chaos is the site of a volcanic flow that buried an ice-rich layer, called the Vastitas Borealis Formation (VBF). It is generally believed that the VBF is a residue from water-rich materials deposited by large floods. The VBF may have been of varied thickness and may have contained varied amounts of ice. In the thin atmosphere of Mars, this layer would have slowly disappeared by sublimation (changing from a solid directly to a gas). Since some areas would have sublimated more than others, the upper lava cap would not be supported evenly and would crack. Cracks/troughs may have begun from sublimation and shrinkage along the edges of the lava cap. Stress from the undermining of the cap edge would have made cracks in the cap. Places with cracks would undergo more sublimation, then the cracks would widen and form the blocky terrain characteristic of regions of chaos. The sublimation process may have been aided by heat (geothermal flux) from magma movements. There are volcanoes, namely Elysium Montes and Hecates Tholus, nearby which most likely are surrounded by dikes, which would have heated the ground. Also, a warmer period in the past would have increased the amount of water sublimating from the ground.

Importance

Chaos terrain seems to be strong evidence for large amounts of water flowing on Mars in the past. Some of the terrain is not totally broken up, so perhaps more water exists frozen inside some of the blocks.

Chaos regions in Lunae Palus quadrangle
Lunae Palus quadrangle
The Lunae Palus quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey Astrogeology Research Program. The quadrangle is also referred to as MC-10 ....

On April 1, 2010, NASA released the first images under the HiWish program

HiWish program

HiWish is a program created by NASA the so that anyone can suggest a place for the HiRISE camera on the Mars Reconnaissance Orbiter to photograph. It was started in January 2010. The first images were released in April 2010...

in which just plain folk suggested places for HiRISE to photograph. One of the eight locations was Aureum Chaos. The first image below gives a wide view of the area. The next two images are from the HiRISE image.