Arabia Terra

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MOLA map showing boundaries for Arabia Terra and other nearby regions. Wikiarabiaboundaries.jpg
MOLA map showing boundaries for Arabia Terra and other nearby regions.
THEMIS daytime infrared image mosaic showing Eden Patera (at center), one of the proposed volcanic caldera complexes in Arabia Terra, and its surroundings Eden Patera THEMIS day IR.jpg
THEMIS daytime infrared image mosaic showing Eden Patera (at center), one of the proposed volcanic caldera complexes in Arabia Terra, and its surroundings
Ice sheet in Oxus Patera, a caldera in Arabia Terra. The scalloped nicks along the spines of the caldera's ridges are likely cracks caused by the expansion and contraction of ice. Oxus Patera, a caldera on Mars.jpg
Ice sheet in Oxus Patera, a caldera in Arabia Terra. The scalloped nicks along the spines of the caldera's ridges are likely cracks caused by the expansion and contraction of ice.

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 4,500 km (2,800 mi) at its longest extent, centered roughly at 21°N6°E / 21°N 6°E / 21; 6 [1] with its eastern and southern regions rising 4 km (13,000 ft) 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.

Contents

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. [3] 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. [4] [5] 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. [6] These streaks are thought by some to form by dust moving downslope in a way similar to snow avalanches on Earth. [7]

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. [8] 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 [9]

Possible volcanism

A 2013 study proposed that a number of craters within Arabia Terra, including Eden Patera, [10] Euphrates Patera, [11] Siloe Patera, [12] and possibly Semeykin crater, [13] Ismenia Patera, [14] Oxus Patera [15] and Oxus Cavus, [16] represent calderas formed by massive explosive volcanic eruptions [17] (supervolcanoes) [18] of Late Noachian to Early Hesperian age. [19] 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. [19] 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. [19] 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. [19]

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. [20]

In the 2011 novel The Martian by Andy Weir, the protagonist encounters a dust storm in Arabia Terra while traveling from Acidalia Planitia to Schiaparelli crater. [21]

Layers

Tikhonravov Basin streaks, as seen by HiRISE. Scale bar is 500 m (1,600 ft) long Tikhonravov Basin Streaks.JPG
Tikhonravov Basin streaks, as seen by HiRISE. Scale bar is 500 m (1,600 ft) long

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. [22] 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. [23]

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. [24] [25] 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. [26] [27] 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 the Moon stabilizes Earth; at times the tilt has even been greater than 80 degrees [28] [29]

Upper Plains Unit

Wide view of dipping layers, upper plains unit, and brain terrain, as seen by HiRISE under HiWish program ESP 044229 2235pyramids.jpg
Wide view of dipping layers, upper plains unit, and brain terrain, as seen by HiRISE under HiWish program

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. [30]

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.

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.

Linear ridge networks

Linear ridge networks are found in various places on Mars in and around craters. [31] 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. [32] [33] [34] Water here could have supported past life in these locations. Clay may also preserve fossils or other traces of past life.

Interactive Mars map

Interactive image map of the global topography of Mars. Hover your mouse over the image to see the names of over 60 prominent geographic features, and click to link to them. Coloring of the base map indicates relative elevations, based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor. Whites and browns indicate the highest elevations (+12 to +8 km); followed by pinks and reds (+8 to +3 km); yellow is 0 km; greens and blues are lower elevations (down to -8 km). Axes are latitude and longitude; Polar regions are noted. (See also: Mars Rovers map and Mars Memorial map) (view * discuss) Mars Map.JPGCydonia MensaeGale craterHolden craterJezero craterLomonosov craterLyot craterMalea PlanumMaraldi craterMareotis TempeMie craterMilankovič craterSisyphi Planum
Interactive icon.svg Interactive image map of the global topography of Mars. Hover your mouse over the image to see the names of over 60 prominent geographic features, and click to link to them. Coloring of the base map indicates relative elevations, based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor . Whites and browns indicate the highest elevations (+12 to +8 km); followed by pinks and reds (+8 to +3 km); yellow is 0 km; greens and blues are lower elevations (down to −8 km). Axes are latitude and longitude; Polar regions are noted.

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. [35] [36] The quadrangles can be seen and explored via the interactive image map below.

MGS MOC Wide Angle Map of Mars PIA03467.jpg
MGS MOC Wide Angle Map of Mars PIA03467.jpg
Interactive icon.svg Clickable image of the 30 cartographic quadrangles of Mars, defined by the USGS. [35] [39] Quadrangle numbers (beginning with MC for "Mars Chart") [40] and names link to the corresponding articles. North is at the top; 0°N180°W / 0°N 180°W / 0; -180 is at the far left on the equator. The map images were taken by the Mars Global Surveyor.
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See also

Related Research Articles

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References

  1. ↑ "Arabia Terra". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
  2. "Arabia Terra". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
  3. ↑ "HiRISE | the Margin of a Pedestal Crater (PSP_008508_1870)".
  4. ↑ "HiRISE - Layers in Central Mound of Henry Crater. (PSP_009008_1915)". hirise.lpl.arizona.edu. Retrieved 23 March 2018.
  5. ↑ "HiRISE - Layers in Arabia Terra (PSP_004434_1885)". hirise.lpl.arizona.edu. Retrieved 23 March 2018.
  6. ↑ "HiRISE - Slope Streaks in Tikhonravov Basin (PSP_007531_1935)". hirise.lpl.arizona.edu. Retrieved 23 March 2018.
  7. ↑ "HiRISE - Layering and Slope Streaks in Henry Crater (PSP_006569_1915)". hirise.lpl.arizona.edu. Retrieved 23 March 2018.
  8. ↑ Anguita, F.; et al. (1997). "Arabia Terra, Mars: Tectonic and Palaeoclimatic Evolution of a Remarkable Sector of Martian Lithosphere". Earth, Moon, and Planets . 77 (1): 55–72. Bibcode:1997EM&P...77...55A. doi:10.1023/A:1006143106970. S2CID   116142883.
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  10. ↑ "Eden Patera". [USGS planetary nomenclature page]. USGS . Retrieved 2013-10-17.
  11. ↑ "Euphrates Patera". [USGS planetary nomenclature page]. USGS . Retrieved 2013-10-17.
  12. ↑ "Siloe Patera". [USGS planetary nomenclature page]. USGS . Retrieved 2013-10-17.
  13. ↑ "Semeykin". [USGS planetary nomenclature page]. USGS . Retrieved 2013-10-17.
  14. ↑ "Ismenia Patera". [ USGS planetary nomenclature page]. USGS . Retrieved 2013-10-17.
  15. ↑ "Oxus Patera". [USGS planetary nomenclature page]. USGS . Retrieved 2013-10-17.
  16. ↑ "Oxus Cavus". [ USGS planetary nomenclature page]. USGS . Retrieved 2013-10-17.
  17. ↑ Witze, A. (2013). "Ancient supervolcanoes revealed on Mars". Nature. doi: 10.1038/nature.2013.13857 .
  18. ↑ Brian Wu (25 May 2015). "European Space Agency May Have Discovered a Supervolcano on Mars". Science Times.
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  26. ↑ "Some ancient Mars lakes formed long after others". sciencedaily.com. Retrieved 23 March 2018.
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  28. ↑ name; Touma, J.; Wisdom, J. (1993). "The Chaotic Obliquity of Mars". Science. 259 (5099): 1294–1297. Bibcode:1993Sci...259.1294T. doi:10.1126/science.259.5099.1294. PMID   17732249. S2CID   42933021.
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  30. ↑ Carr, M. 2001.
  31. ↑ Head, J., J. Mustard. 2006. Breccia dikes and crater-related faults in impact craters on Mars: Erosion and exposure on the floor of a crater 75 km in diameter at the dichotomy boundary, Meteorit. Planet Science: 41, 1675–1690.
  32. ↑ Mangold; et al. (2007). "Mineralogy of the Nili Fossae region with OMEGA/Mars Express data: 2. Aqueous alteration of the crust". J. Geophys. Res. 112 (E8): E08S04. Bibcode:2007JGRE..112.8S04M. doi: 10.1029/2006JE002835 .
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