Arabia Terra

Arabia Terra is a large upland region in the north of Mars that lies mostly in the Arabia quadrangle, but a small part is in the Mare Acidalium quadrangle. It is densely cratered and heavily eroded. This battered topography indicates great age, and Arabia Terra is presumed to be one of the oldest terrains on the planet. It covers as much as at its longest extent, centered roughly at with its eastern and southern regions rising above the north-west. Alongside its many craters, canyons wind through the Arabia Terra, many emptying into the large northern lowlands of the planet, which borders Arabia Terra to the north.

Features

Arabia contains many interesting features. There are some good examples of pedestal craters in the area. A pedestal crater has its ejecta above the surrounding terrain, often forming a steep cliff. The ejecta forms a resistant layer that protects the underlying material from erosion. Mounds and buttes on the floor of some craters display many layers. The layers may have formed by volcanic processes, by wind, or by underwater deposition. Dark slope streaks have been observed in Tikhonravov Basin, a large eroded crater. The streaks appear on steep slopes and change over time. At first they are dark, then turn a lighter color, probably by the deposition of fine, light colored dust from the atmosphere. These streaks are thought to form by dust moving downslope in a way similar to snow avalanches on Earth.

Arabia Terra was named in 1879 after a corresponding albedo feature on a map by Giovanni Schiaparelli, who named it in turn after the Arabian peninsula.

Possible tectonism

Research on the region was undertaken in 1997 and the individuality of the province better defined. An equatorial belt was noted with a crater age distinctly younger than the northern part of the province and of Noachis Terra to the south. This was interpreted as an "incipient back-arc system" provoked by the subduction of Mars lowlands under Arabia Terra during Noachian times. Regional fracture patterns were also explained in this manner, and the rotational instability of the planet as a cause was not supported. It contains extension tectonic
features

Possible volcanism

A 2013 study proposed that a number of craters within Arabia Terra, including Eden Patera, Euphrates Patera, Siloe Patera, and possibly Semeykin crater, Ismenia Patera, Oxus Patera and Oxus Cavus, represent calderas formed by massive explosive volcanic eruptions (supervolcanoes) of Late Noachian to Early Hesperian age. Termed "plains-style caldera complexes", these very low relief volcanic features appear to be older than the large Hesperian-age shield volcanoes of Tharsis or Elysium. Eden Patera, for example, is an irregular, 55 by 85 km depression up to 1.8 km deep, surrounded by ridged basaltic plains. It contains three linked interior depressions, demarcated by arcuate scarps, that have terraces suggestive of lava lake drainage and faults suggestive of collapse. The features indicative of impact origin that would be expected in an impact crater of comparable diameter and depth are absent. The authors regard crustal thinning due to regional extension to be a more likely explanation for the origin of the volcanic activity than putative subduction. Rapid ascent of magma through the thin crust and a consequent relative absence of degassing may explain the more explosive eruption style associated with these paterae relative to that of the shield volcanoes. The eruptions would have contributed to the layered deposits of Arabia Terra, which are among the fine-grained deposits widespread in the equatorial regions of Mars. Total eruptive volumes of at least 4,600–7,200 km³ per caldera complex (over its history) were inferred.

Recent meteoroid impact

A meteorite impacted in Arabia Terra some time between 30 June 2002 and 5 October 2003. A single small crater of about 22.6 meters (about 74 feet) in diameter is surrounded by light and dark-toned ejecta – indicating that this impact excavated to a depth where light colored strata exists. The crater occurs near 20.6 degrees north latitude, 356.8 degrees west longitude, in Arabia Terra. Images of the area show how the impact site appeared to the Mars Odyssey Thermal Emission Imaging System infrared instrument before and after the impact.

In popular culture

In the novel '' The Martian'' by Andy Weir, the protagonist encounters a dust storm in Arabia Terra while traveling from Acidalia Planitia to Schiaparelli crater.

Layers

Many places on Mars show rocks arranged in layers. Rock can form layers in a variety of ways. Volcanoes, wind, or water can produce layers. Layers may be formed by groundwater rising up depositing minerals and cementing sediments. The hardened layers are consequently more protected from erosion. This process may occur instead of layers forming under lakes.

A detailed discussion of layering with many Martian examples can be found in Sedimentary Geology of Mars.

Image:Layers in a crater in Arabia.JPG, Layers in Tikonravev Crater in Arabia, as seen by Mars Global Surveyor (MGS). Layers may form from volcanoes, the wind, or by deposition under water. The craters on the left are pedestal craters. Some researchers believe this crater once held a massive lake.
Image:Tikonravev Crater Floor.JPG, Tikonravev Crater floor, as seen by Mars Global Surveyor. Click on image to see dark slope streaks and layers.
Image:Tikhonravov Basin Streaks.JPG, Tikhonravov Basin streaks, as seen by HiRISE. Scale bar is long
Image:Layers in Monument Valley.jpg, Layers in Monument Valley, Arizona. These are accepted as being formed, at least in part, by water deposition. Since Mars contains similar layers, water is considered a major cause of layering on Mars.
Image:Henry Crater Mound.JPG, Henry Crater mound, as seen by HiRISE. The scale bar is long
Image:Cassini crater floor.JPG, Crater in the middle of Cassini, as seen by HiRISE. Layers may have been deposited under water since it is believed that Cassini once held a giant lake.
Image:ESP 025558buttes.jpg, Buttes, as seen by HiRISE under HiWish program. Buttes have layered rocks with a hard resistant cap rock on the top which protects the underlying rocks from erosion.
Image:25558dikes.jpg, Possible dikes and layered structures, as seen by HiRISE under HiWish program.
Image:25558fault.jpg, Possible fault along a butte, as seen by HiRISE under HiWish program.


ESP 047421 1890nicelayers.jpg, Wide view of layers in crater, as seen by HiRISE under HiWish program parts of this image are enlarged in other images that follow.
47421 1890bigbutte.jpg, Close view of layers, as seen by HiRISE under HiWish program Box shows the size of a football field.
47421 1890layeredterrain.jpg, Close view of layers, as seen by HiRISE under HiWish program Box shows the size of a football field.

47421 1890layers5buttes.jpg, Close view of layers, as seen by HiRISE under HiWish program Box shows the size of a football field.

47421 1890layersbutte.jpg, Close view of layers, as seen by HiRISE under HiWish program

47421 1890layersbuttesclose.jpg, Close view of layers, as seen by HiRISE under HiWish program

47421 1890layerssuperclose.jpg, Close view of layers, as seen by HiRISE under HiWish program
47421 1890pointed butte.jpg, Close view of layers, as seen by HiRISE under HiWish program
47421 1890layersdhadow.jpg, Close view of layers, as seen by HiRISE under HiWish program

Channels

Many places on Mars show channels of different sizes. Many of these channels probably carried water, at least for a time. One study that used HiRISE pictures found over 17,000 km of ancient river valleys in Arabia Terra. Many ancient river valleys have been determined to be relatively recent, according to research published in 2016 in the Journal of Geophysical Research: Planets. These valleys carried water into lake basins. One lake, nicknamed "Heart Lake," had a volume similar to Lake Ontario. The climate of Mars may have been such in the past that water ran on its surface. It has been known for some time that Mars undergoes many large changes in its tilt or obliquity because its two small moons lack the gravity to stabilize it, as our moon stabilizes Earth; at times the tilt has even been greater than 80 degrees

Wikichannelsarabia.jpg, Channels in Arabia, as seen by CTX This channel winds along for a good distance and has branches. It ends in a depression that may have been a lake at one time.
WikiESP 039997 2170channels.jpg, Channel in Arabia, as seen by HiRISE under HiWish program.
ESP 039931 2165channels.jpg, Channel within larger channel, as seen by HiRISE under HiWish program The existence of the smaller channel suggests water went through the region at least two times in the past.
ESP 039931 2165close.jpg, Close-up of channel within larger channel, as seen by HiRISE under HiWish program The existence of the smaller channel suggests water went through the region at least two times in the past. The black box represents the size of a football field. Some parts of the surface would be difficult to walk on with the many small hills and depressions.
Wikisklodowska.jpg, Sklodowska (Martian crater), as seen by CTX camera (on Mars Reconnaissance Orbiter). Small channels are visible along the eroded, southern rim.
Wikisklodowskachannels.jpg, Channels in Sklodowska Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of the previous image.
WikisklodowskaESP 035500 2130.jpg, Channels in Sklodowska Crater, as seen by HiRISE under the HiWish program.
ESP 042924 2195channel.jpg, Channel system that travels through part of a crater, as seen by HiRISE under HiWish program
ESP 050914 2130channel.jpg, Channels, as seen by HiRISE under HiWish program

Upper Plains Unit

Parts of northern Arabia Terra contains the upper plains unit. The Upper Plains Unit is the remnants of a 50–100 meter thick mantling in the mid-latitudes. It was first investigated in the Deuteronilus Mensae (Ismenius Lacus quadrangle) region, but it occurs in other places as well. The remnants consist of sets of dipping layers in craters and along mesas.

ESP 044229 2235pyramids.jpg, Wide view of dipping layers, upper plains unit, and brain terrain, as seen by HiRISE under HiWish program
ESP 044229 2235pyramidscroped.jpg, Dipping layers, as seen by HiRISE under HiWish program This is an enlargement of a previous image.

Some regions of the upper plains unit display large fractures and troughs with raised rims; such regions are called ribbed upper plains. Fractures are believed to have started with small cracks from stresses. Stress is suggested to initiate the fracture process since ribbed upper plains are common when debris aprons come together or near the edge of debris aprons—such sites would generate compressional stresses. Cracks exposed more surfaces, and consequently more ice in the material sublimates into the planet's thin atmosphere. Eventually, small cracks become large canyons or troughs.

ESP 042198 2235pyramid.jpg, View of stress cracks and larger cracks that have been enlarged by sublimation (ice changing directly into gas) This may be the start of ribbed terrain.

ESP 042554 2245ribbedterrain.jpg, Evolution of ribbed terrain from stress cracks—cracks to the left eventually will enlarge and become ribbed terrain toward the right side of picture, as seen by HiRISE under HiWish program

This unit also degrades into brain terrain. Brain terrain is a region of maze-like ridges 3–5 meters high. Some ridges may consist of an ice core, so they may be sources of water for future colonists.

44229 2235brainsforming.jpg, Brain terrain is forming from the breakdown of upper plains unit, as seen by HiRISE under HiWish program Arrow points to a place where fractures are forming that will turn into brain terrain.
44229 2235brainsupper.jpg, Brain terrain is forming from the breakdown of upper plains unit, as seen by HiRISE under HiWish program Arrow points to a place where fractures are forming that will turn into brain terrain.

ESP 045363 2190brain.jpg, Wide view of brain terrain being formed, as seen by HiRISE under HiWish program
45363 2190brainsforming.jpg, Brain terrain being formed, as seen by HiRISE under HiWish program Note: this is an enlargement of the previous image using HiView.
45363 2190brainsforming2.jpg, Brain terrain being formed, as seen by HiRISE under HiWish program Note: this is an enlargement of a previous image using HiView.

Linear ridge networks

Linear ridge networks are found in various places on Mars in and around craters. Ridges often appear as mostly straight segments that intersect in a lattice-like manner. They are hundreds of meters long, tens of meters high, and several meters wide. It is thought that impacts created fractures in the surface, these fractures later acted as channels for fluids. Fluids cemented the structures. With the passage of time, surrounding material was eroded away, thereby leaving hard ridges behind.
Since the ridges occur in locations with clay, these formations could serve as a marker for clay which requires water for its formation. Water here could have supported past life in these locations. Clay may also preserve fossils or other traces of past life.

ESP 036316 2015straightridges.jpg, Linear ridge network, as seen by HiRISE under HiWish program Dark line is not part of the picture. Data was not gathered for that area.

36316 2015ridges.jpg, Enlargement of previous image of linear ridge network, as seen by HiRISE under HiWish program

Pingos

Pingos are believed to be present on Mars. They are mounds that contain cracks. They contain pure water ice, so they would be a great source of water for future colonists on Mars

44322 2215pingos.jpg, Arrows point to possible pingos, as seen by HiRISE under HiWish program Pingos contain a core of pure ice.

ESP 051139 2160mantlebrains.jpg, Wide view of ring-mold craters, as seen by HiRISE under HiWish program Location is the Ismenius Lacus quadrangle.

51139 2160ringmold.jpg, Close view of Ring-mold crater, as seen by HiRISE under HiWish program
51139 2160ringmolds.jpg, Group of ring-mold craters, as seen by HiRISE under HiWish program

Mesas

Wikictxp13clifflda.jpg, Wide view of mesa with CTX showing cliff face and location of lobate debris apron (LDA). Location is Ismenius Lacus quadrangle.
Wikifretesp 028313 2220cliff.jpg, Enlargement of previous CTX image of mesa This image shows the cliff face and detail in the LDA. Image taken with HiRISE under HiWish program. Location is Ismenius Lacus quadrangle.
Image:25755concentriccracks.jpg, Large group of concentric cracks, as seen by HiRISE, under HiWish program. These may have formed when ice under this place disappeared from the ground.
25755 2200collapse.jpg, Tilted layers formed when ground collapsed, as seen by HiRISE, under HiWish program.
25755 2200tiltedlayers.jpg, Tilted layers formed from ground collapse, as seen by HiRISE, under HiWish program.
25755 2200blocksforming.jpg, Mesas breaking up into blocks, as seen by HiRISE, under HiWish program.
43201 2160blocks.jpg, Enlarged view of a group of mesas, as seen by HiRISE under HiWish program One surface is forming square shapes.

46050 1775race.jpg, Mesa, as seen by HiRISE under HiWish program This may make for a good race around a mesa someday in the far future.

Fractures forming blocks

In places large fractures break up surfaces. Sometimes straight edges are formed and large cubes are created by the fractures.

44757 2185wide.jpg, Wide view of mesas that are forming fractures, as seen by HiRISE under HiWish program.
44757 2185zoom.jpg, Enlarged view of a part of previous image, as seen by HiRISE under HiWish program. The rectangle represents the size of a football field.
44757 2185closeleft.jpg, Close-up of blocks being formed, as seen by HiRISE under HiWish program as seen by HiRISE under HiWish program.
44757 2185blocks.jpg, Close-up of blocks being formed, as seen by HiRISE under HiWish program The rectangle represents the size of a football field, so blocks are the size of buildings.
44757 2185cosefractures.jpg, Close-up of blocks being formed, as seen by HiRISE under HiWish program as seen by HiRISE under HiWish program. Many long fractures are visible on the surface.
44757 2185edgebrains.jpg, Surface breaking up, as seen by HiRISE under HiWish program as seen by HiRISE under HiWish program. Near the top the surface is eroding into brain terrain.
ESP 045377 2170odd.jpg, Wide view showing light-toned feature that is breaking into blocks, as seen by HiRISE under HiWish program
45377 2170blocks.jpg, Close view showing blocks being formed, as seen by HiRISE under HiWish program Note: this is an enlargement of the previous image. Box represents size of football field.

Glaciers

ESP 045085 2205flow.jpg, Wide view of flow moving down valley, as seen by HiRISE under HiWish program Location is Ismenius Lacus quadrangle.
45085 2205close.jpg, Close view of part of glacier, as seen by HiRISE under HiWish program Box shows size of football field.
45085 2205mantlethickness.jpg, Close view of mantle, as seen by HiRISE under HiWish program Arrows show craters along edge which highlight the thickness of mantle.

Gallery

File:Meridianicropped.png, Annotated elevation map of Opportunity landing site and some surrounding craters including Endeavour and Miyamato
Image:ArabiaTerraOblique.jpg, An oblique view of Arabia Terra produced by ''Mars Global Surveyor''
Image:Pasteur Crater Floor.JPG, Pasteur Crater floor, as seen by HiRISE. The scale bar is long
45085 2205mantlethickness.jpg, Close view of mantle, as seen by HiRISE under HiWish program Arrows show craters along edge which highlight the thickness of mantle.
45377 2170troughinsidetroughs.jpg, Pits and troughs, as seen by HiRISE under HiWish program Pits may have formed from water/ice leaving the ground.

Interactive Mars map

Map of quadrangles

For mapping purposes, the United States Geological Survey divides the surface of Mars into thirty " quadrangles", each named for a prominent physiographic feature within that quadrangle. The quadrangles can be seen and explored via the interactive image map below.

See also

* Climate of Mars
* Geography of Mars
* Geology of Mars
* Impact crater
* List of craters on Mars
* List of quadrangles on Mars

References

External links

High resolution video
by Seán Doran of overflight of a layered area in Arabia Terra

{{Authority control

Terrae on Mars
Arabia quadrangle
Mare Acidalium quadrangle