Aonia Terra

Last updated
MOLA map showing boundaries of Aonia Terra and other regions Wikimolaargyre.jpg
MOLA map showing boundaries of Aonia Terra and other regions
MOLA map showing boundaries of Aonia Terra near the south pole and other regions Wikimolasouthpole.jpg
MOLA map showing boundaries of Aonia Terra near the south pole and other regions

Aonia Terra is a region in the southern hemisphere of the planet Mars. It is named after a classical albedo feature Aonia, [1] that was named after the ancient Greek region Aonia.

Contents

It is centered at 60°S97°W / 60°S 97°W / -60; -97 and covers 3900 km at its broadest extent. It covers latitudes 30 to 81 South and longitudes 60 to 163 W. [2] Aonia Terra lies in the Phaethontis, Thaumasia and the Australe quadrangles of Mars. Aonia Terra is an upland area notable for massive cratering including the large Lowell Crater, parts of the region features small craters, in the plain areas, Thaumasia Fossae and parts of the southern area. The feature are bordered by Terra Sirenum within the range of Icaria Fossae to the northwest the highland area which includes Claritas and Coracis Fossae as well as Warrego Valles towards the north, Argyre Planitia to the east and Cavi Angusti, Australe Scopuli and Australe Planum to the south.

Geography

The region consists of a few plana (plains) including Aonia, Icaria, Parva and most of Bosporos as well as the west of Argentea Planum. Other features includes Aonia Mons, Aonia Tholus and Phrixi Rupes.

History

Telescopic images were taken during the mid-19th century. It would be known as Aonius Sinus, one of Schiaparelli's feature names and was thought to be a bay of Mare Australe. It bordered Phaethontis, Icaria and Thaumasia Felix. Aonius Sinus became an official IAU name in 1958. The area's first image was taken in 1967 by Mariner 4 and were blurry and those taken in the east had no detail. The remaining detailed images were finally taken by Mariner 9 in 1971 and 1972. further images were taken by the Viking orbiters later in the 1970s. No main feature name was named until Aonius Sinus became Aonia Terra in 1979. As of 2018, it is one of four features named after Aonius.

Craters

List of craters

The following is a list of craters in Aonia Terra. The crater's central location is of the feature, craters that its central location is in another feature are listed by eastern, western, northern or southern part.

Lowell, the largest crater in Aonia Terra Lowell crater PIA02836.jpg
Lowell, the largest crater in Aonia Terra
Stoney crater, located in the southwest Wikistoney.jpg
Stoney crater, located in the southwest
Ross crater, CTX image Wikiross.jpg
Ross crater, CTX image
Porter crater, CTX image Wikiporter.jpg
Porter crater, CTX image
Lau crater, CTX image Wikilau.jpg
Lau crater, CTX image
NameLocationQuadrangle(s)DiameterYear of approval
Agassiz 69°48′S89°54′W / 69.8°S 89.9°W / -69.8; -89.9 Mare Australe108.77 km1973
AkiThaumasia1979
Babakin Thaumasia
Bianchini 64°12′S95°24′W / 64.2°S 95.4°W / -64.2; -95.4 Thaumasia76 km1973
Brashear 54°08′S119°02′W / 54.14°S 119.03°W / -54.14; -119.03 Thaumasia77.45 km1973
Chamberlin Mare Australe, Phaethontis
Coblentz 50°18′S90°18′W / 50.3°S 90.3°W / -50.3; -90.3 Thaumasia112 km1973
DokuchaevPhaethontis
Douglass 51°48′S70°36′W / 51.8°S 70.6°W / -51.8; -70.6 Thaumasia94.8 km1973
Fontana Thaumasia1973
GariThaumasia
Heaviside 70°42′S95°18′W / 70.7°S 95.3°W / -70.7; -95.3 Mare Australe87.4 km1973
Hussey 59°24′S173°54′W / 59.4°S 173.9°W / -59.4; -173.9 Phaethontis49 km1973
IstokThaumasia
KontumThaumasia2006
KumakThaumasia
Lamont 58°36′S113°36′W / 58.6°S 113.6°W / -58.6; -113.6 Thaumasia76 km1973
Lau 74°24′S107°48′W / 74.4°S 107.8°W / -74.4; -107.8 Mare Australe104.9 km1973
Lowell 52°18′S81°24′W / 52.3°S 81.4°W / -52.3; -81.4 Thaumasia203 km1973
Playfair 78°06′S126°12′W / 78.1°S 126.2°W / -78.1; -126.2 Mare Australe64.2 km1973
Porter 50°48′S113°54′W / 50.8°S 113.9°W / -50.8; -113.9 Thaumasia105 km1973
Reynolds 75°06′S157°54′W / 75.1°S 157.9°W / -75.1; -157.9 Mare Australe97.5 km1973
Ross 57°42′S107°50′W / 57.7°S 107.84°W / -57.7; -107.84 Thaumasia82.51 km1973
Slipher 47°48′S84°36′W / 47.8°S 84.6°W / -47.8; -84.6 Thaumasia127.14 km1973
Smith Mare Australe
Steno 68°00′S115°36′W / 68°S 115.6°W / -68; -115.6 Mare Australe106.9 km1973
Stoney 69°48′S138°36′W / 69.8°S 138.6°W / -69.8; -138.6 Mare Australe161.37 km1973

Martian gullies

Aonia Terra is the location of many Martian gullies that may be due to recent flowing water. Some are found in many craters near the large craters Lowell, Douglass and Ross. [3] Gullies occur on steep slopes, especially on the walls of craters. Gullies are believed to be relatively young because they have few, if any craters. Moreover, they lie on top of sand dunes which themselves are considered to be quite young. Usually, each gully has an alcove, channel, and apron. Some studies have found that gullies occur on slopes that face all directions, [4] others have found that the greater number of gullies are found on poleward facing slopes, especially from 30 to 44 S. [5]

Although many ideas have been put forward to explain them, [6] the most popular involve liquid water coming from an aquifer, from melting at the base of old glaciers, or from the melting of ice in the ground when the climate was warmer. [7] [8] Because of the good possibility that liquid water was involved with their formation and that they could be very young, scientists are excited. Maybe the gullies are where we should go to find life.

There is evidence for all three theories. Most of the gully alcove heads occur at the same level, just as one would expect of an aquifer. Various measurements and calculations show that liquid water could exist in aquifers at the usual depths where gullies begin. [7] One variation of this model is that rising hot magma could have melted ice in the ground and caused water to flow in aquifers. Aquifers are layer that allow water to flow. They may consist of porous sandstone. The aquifer layer would be perched on top of another layer that prevents water from going down (in geological terms it would be called impermeable). Because water in an aquifer is prevented from going down, the only direction the trapped water can flow is horizontally. Eventually, water could flow out onto the surface when the aquifer reaches a break—like a crater wall. The resulting flow of water could erode the wall to create gullies. [9] Aquifers are quite common on Earth. A good example is "Weeping Rock" in Zion National Park Utah. [10]

As for the next theory, much of the surface of Mars is covered by a thick smooth mantle that is thought to be a mixture of ice and dust. [11] [12] [13] This ice-rich mantle, a few yards thick, smooths the land, but in places it has a bumpy texture, resembling the surface of a basketball. The mantle may be like a glacier and under certain conditions the ice that is mixed in the mantle could melt and flow down the slopes and make gullies. [14] [15] Because there are few craters on this mantle, the mantle is relatively young. The ice-rich mantle may be the result of climate changes. [16] Changes in Mars's orbit and tilt cause significant changes in the distribution of water ice from polar regions down to latitudes equivalent to Texas. During certain climate periods water vapor leaves polar ice and enters the atmosphere. The water comes back to ground at lower latitudes as deposits of frost or snow mixed generously with dust. The atmosphere of Mars contains a great deal of fine dust particles. Water vapor will condense on the particles, then fall down to the ground due to the additional weight of the water coating. When Mars is at its greatest tilt or obliquity, up to 2 cm of ice could be removed from the summer ice cap and deposited at midlatitudes. This movement of water could last for several thousand years and create a snow layer of up to around 10 meters thick. [17] [18] When ice at the top of the mantling layer goes back into the atmosphere, it leaves behind dust, which insulating the remaining ice. [19] Measurements of altitudes and slopes of gullies support the idea that snowpacks or glaciers are associated with gullies. Steeper slopes have more shade which would preserve snow. [5]

Higher elevations have far fewer gullies because ice would tend to sublimate more in the thin air of the higher altitude. [20]

The third theory might be possible since climate changes may be enough to simply allow ice in the ground to melt and thus form the gullies. During a warmer climate, the first few meters of ground could thaw and produce a "debris flow" similar to those on the dry and cold Greenland east coast. [21] Since the gullies occur on steep slopes only a small decrease of the shear strength of the soil particles is needed to begin the flow. Small amounts of liquid water from melted ground ice could be enough. [22] [23] Calculations show that a third of a mm of runoff can be produced each day for 50 days of each Martian year, even under current conditions. [24]

Defrosting

As the temperature warms and more sunlight becomes available in the spring, frost starts to disappear. These occur in the southern portion of the region that is also included in the Mare Australe quadrangle (e.g. Heaviside and Stoney). This process begins with the appearance of dark spots. By the time the temperature rises to the melting point of water ice, all ice is gone. The process was first followed with repeated images by the Mars Global Surveyor. [25] With the much greater resolution of HiRISE, it was seen that many spots had the shape of fans.[ citation needed ]

See also

Related Research Articles

<span class="mw-page-title-main">Terra Sirenum</span>

Terra Sirenum is a large region in the southern hemisphere of the planet Mars. It is centered at 39.7°S 150°W and covers 3900 km at its broadest extent. It covers latitudes 10 to 70 South and longitudes 110 to 180 W. Terra Sirenum is an upland area notable for massive cratering including the large Newton Crater. Terra Sirenum is in the Phaethontis quadrangle and the Memnonia quadrangle of Mars. A low area in Terra Sirenum is believed to have once held a lake that eventually drained through Ma'adim Vallis.

<span class="mw-page-title-main">Terra Cimmeria</span> Terra on Mars

Terra Cimmeria is a large Martian region, centered at 34.7°S 145°E and covering 5,400 km (3,400 mi) at its broadest extent. It covers latitudes 15 N to 75 S and longitudes 170 to 260 W. It lies in the Eridania quadrangle. Terra Cimmeria is one part of the heavily cratered, southern highland region of the planet. The Spirit rover landed near the area.

<span class="mw-page-title-main">Promethei Terra</span>

Promethei Terra is a large Martian region covering 3300 km at its broadest extent. It lies to the east of the massive Hellas basin. Like much of the southern part of the planet it is a heavily cratered, highland region. Promethei Terra was named for a classic albedo feature of Mars, with the original name derived from that of the Greek god Prometheus. Promethei Terra lies mostly in the Hellas quadrangle of Mars.

<span class="mw-page-title-main">Hale (Martian crater)</span> Crater on Mars

Hale is a 150 km × 125 km crater at 35.7°S, 323.4°E on Mars, just north of Argyre basin. The crater is in the Argyre quadrangle. It was named after American astronomer George Ellery Hale.

<span class="mw-page-title-main">Arcadia quadrangle</span> Map of Mars

The Arcadia quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The quadrangle is located in the north-central portion of Mars’ western hemisphere and covers 240° to 300° east longitude and 30° to 65° north latitude. The quadrangle uses a Lambert conformal conic projection at a nominal scale of 1:5,000,000 (1:5M). The Arcadia quadrangle is also referred to as MC-3. The name comes from a mountainous region in southern Greece. It was adopted by IAU, in 1958.

<span class="mw-page-title-main">Mare Acidalium quadrangle</span> Map of Mars

The Mare Acidalium quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The quadrangle is located in the northeastern portion of Mars' western hemisphere and covers 300° to 360° east longitude and 30° to 65° north latitude. The quadrangle uses a Lambert conformal conic projection at a nominal scale of 1:5,000,000 (1:5M). The Mare Acidalium quadrangle is also referred to as MC-4.

<span class="mw-page-title-main">Hellas quadrangle</span> Map of Mars

The Hellas quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Hellas quadrangle is also referred to as MC-28 . The Hellas quadrangle covers the area from 240° to 300° west longitude and 30° to 65° south latitude on the planet Mars. Within the Hellas quadrangle lies the classic features Hellas Planitia and Promethei Terra. Many interesting and mysterious features have been discovered in the Hellas quadrangle, including the giant river valleys Dao Vallis, Niger Vallis, Harmakhis, and Reull Vallis—all of which may have contributed water to a lake in the Hellas basin in the distant past. Many places in the Hellas quadrangle show signs of ice in the ground, especially places with glacier-like flow features.

<span class="mw-page-title-main">Eridania quadrangle</span> Map of Mars

The Eridania quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Eridania quadrangle is also referred to as MC-29.

<span class="mw-page-title-main">Phaethontis quadrangle</span> Map of Mars

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

<span class="mw-page-title-main">Thaumasia quadrangle</span> Map of Mars

The Thaumasia quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Thaumasia quadrangle is also referred to as MC-25 . The name comes from Thaumas, the god of the clouds and celestial apparitions.

<span class="mw-page-title-main">Argyre quadrangle</span> Map of Mars

The Argyre quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Argyre quadrangle is also referred to as MC-26. It contains Argyre Planitia and part of Noachis Terra.

<span class="mw-page-title-main">Water on Mars</span> Study of past and present water on Mars

Almost all water on Mars today exists as ice, though it also exists in small quantities as vapor in the atmosphere. What was thought to be low-volume liquid brines in shallow Martian soil, also called recurrent slope lineae, may be grains of flowing sand and dust slipping downhill to make dark streaks. While most water ice is buried, it is exposed at the surface across several locations on Mars. In the mid-latitudes, it is exposed by impact craters, steep scarps and gullies. Additionally, water ice is also visible at the surface at the north polar ice cap. Abundant water ice is also present beneath the permanent carbon dioxide ice cap at the Martian south pole. More than 5 million km3 of ice have been detected at or near the surface of Mars, enough to cover the whole planet to a depth of 35 meters (115 ft). Even more ice might be locked away in the deep subsurface. Some liquid water may occur transiently on the Martian surface today, but limited to traces of dissolved moisture from the atmosphere and thin films, which are challenging environments for known life. No evidence of present-day liquid water has been discovered on the planet's surface because under typical Martian conditions, warming water ice on the Martian surface would sublime at rates of up to 4 meters per year. Before about 3.8 billion years ago, Mars may have had a denser atmosphere and higher surface temperatures, potentially allowing greater amounts of liquid water on the surface, possibly including a large ocean that may have covered one-third of the planet. Water has also apparently flowed across the surface for short periods at various intervals more recently in Mars' history. Aeolis Palus in Gale Crater, explored by the Curiosity rover, is the geological remains of an ancient freshwater lake that could have been a hospitable environment for microbial life. The present-day inventory of water on Mars can be estimated from spacecraft images, remote sensing techniques, and surface investigations from landers and rovers. Geologic evidence of past water includes enormous outflow channels carved by floods, ancient river valley networks, deltas, and lakebeds; and the detection of rocks and minerals on the surface that could only have formed in liquid water. Numerous geomorphic features suggest the presence of ground ice (permafrost) and the movement of ice in glaciers, both in the recent past and present. Gullies and slope lineae along cliffs and crater walls suggest that flowing water continues to shape the surface of Mars, although to a far lesser degree than in the ancient past.

<span class="mw-page-title-main">Gorgonum Chaos</span> Chaos on Mars

Gorgonum Chaos is a set of canyons in the Phaethontis quadrangle of Mars. It is located at 37.5° south latitude and 170.9° west longitude. Its name comes from an albedo feature at 24S, 154W. Some of the first gullies on Mars were found in Gorgonum Chaos. It is generally believed that it once contained a lake. Other nearby features are Sirenum Fossae, Maadim Vallis, Ariadnes Colles, and Atlantis Chaos. Some of the surfaces in the region are formed from the Electris deposits.

HiWish is a program created by NASA so that anyone can suggest a place for the HiRISE camera on the Mars Reconnaissance Orbiter to photograph. It was started in January 2010. In the first few months of the program 3000 people signed up to use HiRISE. The first images were released in April 2010. Over 12,000 suggestions were made by the public; suggestions were made for targets in each of the 30 quadrangles of Mars. Selected images released were used for three talks at the 16th Annual International Mars Society Convention. Below are some of the over 4,224 images that have been released from the HiWish program as of March 2016.

<span class="mw-page-title-main">Gullies on Mars</span> Incised networks of narrow channels and sediments on Mars

Martian gullies are small, incised networks of narrow channels and their associated downslope sediment deposits, found on the planet of Mars. They are named for their resemblance to terrestrial gullies. First discovered on images from Mars Global Surveyor, they occur on steep slopes, especially on the walls of craters. Usually, each gully has a dendritic alcove at its head, a fan-shaped apron at its base, and a single thread of incised channel linking the two, giving the whole gully an hourglass shape. They are estimated to be relatively young because they have few, if any craters. A subclass of gullies is also found cut into the faces of sand dunes, that are themselves considered to be quite young. Linear dune gullies are now considered recurrent seasonal features.

To date, interplanetary spacecraft have provided abundant evidence of water on Mars, dating back to the Mariner 9 mission, which arrived at Mars in 1971. This article provides a mission by mission breakdown of the discoveries they have made. For a more comprehensive description of evidence for water on Mars today, and the history of water on that planet, see Water on Mars.

<span class="mw-page-title-main">Glaciers on Mars</span> Extraterrestrial bodies of ice

Glaciers, loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past. Lobate convex features on the surface known as viscous flow features and lobate debris aprons, which show the characteristics of non-Newtonian flow, are now almost unanimously regarded as true glaciers.

<span class="mw-page-title-main">Evidence of water on Mars found by Mars Reconnaissance Orbiter</span>

The Mars Reconnaissance Orbiter's HiRISE instrument has taken many images that strongly suggest that Mars has had a rich history of water-related processes. Many features of Mars appear to be created by large amounts of water. That Mars once possessed large amounts of water was confirmed by isotope studies in a study published in March 2015, by a team of scientists showing that the ice caps were highly enriched with deuterium, heavy hydrogen, by seven times as much as the Earth. This means that Mars has lost a volume of water 6.5 times what is stored in today's polar caps. The water for a time would have formed an ocean in the low-lying Mare Boreum. The amount of water could have covered the planet about 140 meters, but was probably in an ocean that in places would be almost 1 mile deep.

The common surface features of Mars include dark slope streaks, dust devil tracks, sand dunes, Medusae Fossae Formation, fretted terrain, layers, gullies, glaciers, scalloped topography, chaos terrain, possible ancient rivers, pedestal craters, brain terrain, and ring mold craters.

<span class="mw-page-title-main">Gasa (crater)</span> Crater on Mars

Gasa is an impact rayed crater in the Eridania quadrangle on Mars at 35.68° S and 230.72° W. and is 6.5 km in diameter. Its name was approved in 2009, and it was named after a place in Bhutan. Gullies are evident in the images. It is now believed that the impact that created Gasa happened in a larger crater whose floor was covered with debris-covered glaciers. The larger crater is known as Cilaos, it is located at 35.71° S and 230.52° W. and is 21.4 km in diameter. Its name was approved on 15 August 2016, and it was named after a place in the island of Réunion.

References

  1. ↑ "Gazetteer of Planetary Nomenclature | Aonia Terra". usgs.gov. International Astronomical Union . Retrieved June 12, 2018.
  2. ↑ "Mars Feature: Terra, terrae - Terra Cimmeria". Archived from the original on 2010-01-13. Retrieved 2018-06-12.
  3. ↑ U.S. department of the Interior U.S. Geological Survey, Topographic Map of the Eastern Region of Mars M 15M 0/270 2AT, 1991
  4. ↑ Edgett, K. S.; Malin, M. C.; Williams, R. M. E.; Davis, S. D. (March 2003). "Polar- and Middle-Latitude Martian Gullies: A View from MGS MOC After 2 Mars Years in the Mapping Orbit". Lunar and Planetary Science Conference: 1038. Bibcode:2003LPI....34.1038E.
  5. 1 2 Dickson, James L.; Head, James W.; Kreslavsky, Mikhail (June 2007). "Martian gullies in the southern mid-latitudes of Mars: Evidence for climate-controlled formation of young fluvial features based upon local and global topography". Icarus. 188 (2): 315–323. Bibcode:2007Icar..188..315D. doi:10.1016/j.icarus.2006.11.020.
  6. ↑ "PSRD: Gullied Slopes on Mars".
  7. 1 2 Heldmann, Jennifer L; Mellon, Michael T (April 2004). "Observations of martian gullies and constraints on potential formation mechanisms". Icarus. 168 (2): 285–304. Bibcode:2004Icar..168..285H. doi:10.1016/j.icarus.2003.11.024.
  8. ↑ Forget, François; Costard, François; Lognonné, Philippe (2008). Planet Mars: Story of Another World. Praxis. ISBN   978-0-387-48925-4.[ page needed ]
  9. ↑ David, Leonard (12 November 2004). "Mars Gullies Likely Formed By Underground Aquifers". Space.com.
  10. ↑ Harris, Ann G; Tuttle, Esther; Tuttle, Sherwood D (1990). Geology of national parks. Kendall/Hunt. OCLC   904009255.[ page needed ]
  11. ↑ Malin, Michael C.; Edgett, Kenneth S. (25 October 2001). "Mars Global Surveyor Mars Orbiter Camera: Interplanetary cruise through primary mission". Journal of Geophysical Research: Planets. 106 (E10): 23429–23570. Bibcode:2001JGR...10623429M. doi: 10.1029/2000JE001455 . S2CID   129376333.
  12. ↑ Mustard, John F.; Cooper, Christopher D.; Rifkin, Moses K. (July 2001). "Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice". Nature. 412 (6845): 411–414. Bibcode:2001Natur.412..411M. doi:10.1038/35086515. PMID   11473309. S2CID   4409161.
  13. ↑ Carr, Michael H. (25 October 2001). "Mars Global Surveyor observations of Martian fretted terrain". Journal of Geophysical Research: Planets. 106 (E10): 23571–23593. Bibcode:2001JGR...10623571C. doi:10.1029/2000JE001316.
  14. ↑ David, Leonard (14 November 2006). "Martian gullies could be scientific gold mines". MSNBC. Space.com. Archived from the original on December 24, 2013.
  15. ↑ Head, J. W.; Marchant, D. R.; Kreslavsky, M. A. (25 August 2008). "Formation of gullies on Mars: Link to recent climate history and insolation microenvironments implicate surface water flow origin". Proceedings of the National Academy of Sciences. 105 (36): 13258–13263. doi: 10.1073/pnas.0803760105 . PMC   2734344 . PMID   18725636.
  16. ↑ Thompson, Andrea (August 25, 2008). "Melting Glaciers Sculpted Mars Gullies". Space.com.
  17. ↑ Jakosky, Bruce M.; Carr, Michael H. (June 1985). "Possible precipitation of ice at low latitudes of Mars during periods of high obliquity". Nature. 315 (6020): 559–561. Bibcode:1985Natur.315..559J. doi:10.1038/315559a0. S2CID   4312172.
  18. ↑ Jakosky, Bruce M.; Henderson, Bradley G.; Mellon, Michael T. (1995). "Chaotic obliquity and the nature of the Martian climate". Journal of Geophysical Research. 100 (E1): 1579. Bibcode:1995JGR...100.1579J. doi:10.1029/94JE02801.
  19. ↑ "Mars May Be Emerging From An Ice Age" (Press release). NASA/Jet Propulsion Laboratory. December 18, 2003. Retrieved July 18, 2020.
  20. ↑ Hecht, M (April 2002). "Metastability of Liquid Water on Mars" (PDF). Icarus. 156 (2): 373–386. Bibcode:2002Icar..156..373H. doi:10.1006/icar.2001.6794. S2CID   54901139. Archived from the original (PDF) on 2019-03-08.
  21. ↑ Peulvast, Jean-Pierre; Bétard, François; de Oliveira Magalhães, Alexsandra (18 May 2011). "Scarp morphology and identification of large-scale mass movements in tropical tablelands: the eastern Araripe basin (Ceará, Brazil)". Géomorphologie. 17 (1): 33–52. doi:10.4000/geomorphologie.8800.
  22. ↑ Costard, F.; Forget, F.; Mangold, N.; Mercier, D.; Peulvast, J. P. (March 2001). "Debris Flows on Mars: Analogy with Terrestrial Periglacial Environment and Climatic Implications". Lunar and Planetary Science Conference: 1534. Bibcode:2001LPI....32.1534C.
  23. ↑ http://www.spaceref.com:16090/news/viewpr.html?pid=7124%5B%5D,
  24. ↑ Clow, Gary D. (October 1987). "Generation of liquid water on Mars through the melting of a dusty snowpack". Icarus. 72 (1): 95–127. Bibcode:1987Icar...72...95C. doi:10.1016/0019-1035(87)90123-0.
  25. ↑ NASA.gov [ full citation needed ]
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.