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Lakes on Mars

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In the summer of 1965, the first close-up pictures from Mars revealed a cratered desert with no signs of water.[1] [2] [3] However, over the decades as more parts of the planet were imaged with better cameras on more sophisticated satellites, Mars showed evidence of past river valleys, lakes, and ice in glaciers and in the ground.[4] It was discovered that the climate of Mars displays huge changes over geologic time because its axis is not stabilized by a large moon like our Earth. [5] [6] [7] Also, some researchers maintain that water could exist for periods of time due to geothermal effects or asteroid impacts.[8] [9] [10] [11] [12] Besides seeing features that were signs of past water, researchers found other types of evidence for past water. Minerals detected in many locations needed water to form.[13] [14] Cite error: A <ref> tag is missing the closing </ref> (see the help page). [15] An instrument in the Mars Odyssey, an orbiting spacecraft, mapped the distribution of water in the near surface.[16][17] [18] When the Phoenix spacecraft fired its rockets to land in the far north, ice was exposed.[19] [20]

  • View underneath lander towards south foot pad, showing patchy exposures of a bright surface that is ice.
    View underneath lander towards south foot pad, showing patchy exposures of a bright surface that is ice.

When water enters a large body of water like a lake a delta may form. Many craters and other depressions on Mars show deltas that resemble those on Earth. In addition, if a lake lies in a depression, channels entering it will all stop at the same height. Such an arrangement is visible around places on Mars that are supposed to have contained large bodies of water—including around a possible ocean in the North.

This article will describe some of places that could have held large lakes. Perhaps, the lakes held water long enough for life to form.

Mars Ocean

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An artist's impression of ancient Mars and its oceans based on geological data
The blue region of low topography in the Martian northern hemisphere is hypothesized to be the site of a primordial ocean of liquid water.[21]

The Mars ocean hypothesis states that nearly a third of the surface of Mars was covered by an ocean of liquid water early in the planet’s geologic history.[22] [23] This primordial ocean, dubbed Paleo-Ocean[21] and Oceanus Borealis,[24] would have filled the Vastitas Borealis basin in the northern hemisphere, a region which lies 4–5 km (2.5–3 miles) below the mean planetary elevation, at a time period of approximately 3.8 billion years ago. Evidence for this ocean includes geographic features resembling ancient shorelines, and the chemical properties of the Martian soil and atmosphere.[25] [26] [27] However for such an ocean to exist early Mars would have required a denser atmosphere and warmer climate to allow liquid water to remain at the surface.[28]

History of observational evidence for Martian oceans

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Features shown by the Viking orbiters in 1976, revealed two possible ancient shorelines near the pole, Arabia and Deuteronilus, each thousands of kilometers long.[29] Several physical features in the present geography of Mars suggest the past existence of a primordial ocean. Networks of gullies that merge into larger channels imply erosion by a liquid agent, and resemble ancient riverbeds on Earth. Enormous channels, 25 km wide and several hundred meters deep, appear to directly flow from underground aquifers in the Southern uplands into the Northern plains.[28] Much of the northern hemisphere of Mars is located at a significantly lower elevation than the rest of the planet (the Martian dichotomy), and is unusually flat. The low elevation would cause water, if it existed, to gather there. An ocean would tend to level out the ground underneath it. The acceptance of a vast northern ocean has waxed and waned over the decades. Beginning in 1998, scientists Michael Malin and Kenneth Edgett set out to investigate with higher-resolution cameras on board the Mars Global Surveyor with a resolution five to ten times better than those of the Viking spacecraft, in places that would test shorelines proposed by others in the scientific literature.[30] Their analysis were inconclusive at best, and reported that the shoreline varies in elevation by several kilometers, rising and falling from one peak to the next for thousands of miles.[31] These trends cast doubt on whether the features truly mark a long-gone sea coast and, have been taken as an argument against the Martian shoreline (and ocean) hypothesis. Research published in 2009 shows a much higher density of stream channels than formerly believed. Regions on Mars with the most valleys are comparable to what is found on the Earth. In the research, the team developed a computer program to identify valleys by searching for U-shaped structures in topographical data.[32] The large amount of valley networks strongly supports rain on the planet in the past. The global pattern of the Martian valleys could be explained with a big northern ocean. A large ocean in the northern hemisphere would explain why there is a southern limit to valley networks; the southernmost regions of Mars, farthest from the water reservoir, would get little rainfall and would develop no valleys. In a similar fashion the lack of rainfall would explain why Martian valleys become shallower from north to south.[33] A 2010 study of deltas on Mars revealed that seventeen of them are found at the altitude of a proposed shoreline for a Martian ocean.[34] This is what would be expected if the deltas were all next to a large body of water.[35] Research published in 2012 using data from MARSIS, a radar on board the Mars Express orbiter, supports the hypothesis of an extinct large, northern ocean. The instrument revealed a dielectric constant of the surface that is similar to those of low-density sedimentary deposits, massive deposits of ground-ice, or a combination of the two. The measurements were not like those of a lava-rich surface.[36]

In March 2015, scientists stated that evidence exists for an ancient volume of water that could comprise an ocean, likely in the planet's northern hemisphere and about the size of Earth's Arctic Ocean.[37] This finding was derived from the ratio of water and deuterium in the modern Martian atmosphere compared to the ratio found on Earth and derived from telescopic observations. Eight times as much deuterium was inferred at the polar deposits of Mars than exists on Earth (VSMOW), suggesting that ancient Mars had significantly higher levels of water. The representative atmospheric value obtained from the maps (7 VSMOW) is not affected by climatological effects as those measured by localized rovers, although the telescopic measurements are within range to the enrichment measured by the Curiosity rover in Gale Crater of 5-7 VSMOW.[38]

Valles Marineris canyon system

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Valles Marineris is the largest canyon system in the solar system, and much evidence suggests that all or parts of the canyon system contained lakes. It is located in the Coprates quadrangle. The walls of the canyons often contain many layers. The floors of some of the canyons contain large deposits of layered materials. Some researchers believe that the layers were formed when water once filled the canyons.[39] [40] [41] [42] Layered deposits, called interior layered deposits (ILD's), in various parts of Valles Marineris especially Candor Chasma and Juventae Chasma have lead many researchers to believe that they were formed when the whole area was a giant lake. However, many other ideas have been advanced to explain them.[43] High-resolution structural and geologic mapping in west Candor Chasma, presented in March 2015, showed that the deposits on the floor of the Candor chasma are basin filling sediments that were deposited in a wet playa like setting; hence water was involved in their formation.[44] Minerals that generally require water for their formation have been found in ILD’s thus supporting water in the system. The European Space Agency's Mars Express found possible evidence of the sulfates epsomite and kieserite, minerals that form in water. [45] Also, ferric oxide in the form of crystalline grey hematite, which typically requires water for its formation, was detected.[46] [47] [48] Although much controversy exists about a lake in the whole of Valles Marineris, a fairly strong case can be made for smaller lakes. Melas Chasma is especially believed to have once contained a lake as it is deepest part of the Valles Marineris system at eleven kilometers deep from the surrounding surface, from here to the outflow channels are about a 0.03 degree slope upward to the northern plains, which means that if you filled the canyon with fluid, you would have a lake with a depth of one kilometer before the fluid would flow out onto the northern plains.[49]Melas Chasma is the widest segment of the Valles Marineris canyon system,[50] located east of Ius Chasma at 9.8°S, 283.6°E in Coprates quadrangle. It cuts through layered deposits that are thought to be sediments from an old lake that resulted from runoff of the valley networks to the west.[51] Support for abundant, past water in Melas Chasma comes from the discovery by MRO of hydrated sulfates that need water for their formation. [52] Moreover, in a recent study of southwestern Melas Chasma, using high-resolution image, topographic and spectral datasets, eleven fan-shaped landforms were found. These fans add to growing evidence that Melas Chasma once held a lake that had fluctuating levels.[53] [54] A lake could have formed in the southwest part of Melas Chasma from runoff from local valley networks.[55] [56] Keith Harrison and Mary Chapman described strong evidence for a lake in the eastern part of Valles Marineris. It would have had an average depth of only 842 m—much smaller than the 5-10 km depth of parts of Valles Marineris. Still, its volume of 110,000 cubic meters would be comparable to Earth’s Caspian andBlack Seas. The main evidence for such a lake is the presence of benches at the level that models show is where the lake level should be. Also, the low point in Eos Chasma where water would be expected to overflow is marked by fluvial features. The features look like the flow came together at a small point and carried out significant erosion.[57] [58]

Coprates quadrangle
Map of Coprates quadrangle from Mars Orbiter Laser Altimeter (MOLA) data. The highest elevations are red and the lowest are blue.

Hellas Basin

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The Hellas quadrangle contains part of the Hellas Basin, the largest known impact crater on the surface of Mars and the second largest in the solar system. The depth of the crater is 7152 m[59] (23,000 ft) below the standard topographic datum of Mars. The basin is located in the southern highlands of Mars and is thought to have been formed about 3.9 billion years ago, during the Late Heavy Bombardment. It is believed that a giant lake existed in the Hellas Basin early in the planet's history with a possible depth of 5.5 km.[60] Possible shorelines have been discovered. [61] [62] These shorelines are evident in alternating benches and scarps visible in Mars orbiting camera narrow-angle images. A good example of layers that were deposited in Hellas, and then later exposed by erosion is visible in Terby Crater on the North rim of Hellas. It used to be thought that Terby Crater contained a large delta.[63] However, newer observations have lead researchers to think of the layered sequence as part of a group of layers that may have extended all the across Hellas. There is no valley large enough at the northern rim of Terby to have carried the large amount of sediments necessary to produce the layers. [64] Other observations argue against Terby containing a delta. In addition, Mars orbiting laser altimeter (MOLA) data show that the contacts of these sedimentary units mark contours of constant elevation for thousands of km, and in one case all around the basin. [65]

  • Layers in Terby crater may have formed when the Hellas basin was filled with water.
    Layers in Terby crater may have formed when the Hellas basin was filled with water.
  • Northern part of Terby Crater showing many layers, as seen by CTX camera (on Mars Reconnaissance Orbiter). Parts of this image are enlarged in next two images.
    Northern part of Terby Crater showing many layers, as seen by CTX camera (on Mars Reconnaissance Orbiter). Parts of this image are enlarged in next two images.
  • Northern part of Terby Crater showing many layers, as seen by CTX camera (on Mars Reconnaissance Orbiter).
    Northern part of Terby Crater showing many layers, as seen by CTX camera (on Mars Reconnaissance Orbiter).
  • Northern part of Terby Crater showing many layers, as seen by CTX camera (on Mars Reconnaissance Orbiter).
    Northern part of Terby Crater showing many layers, as seen by CTX camera (on Mars Reconnaissance Orbiter).

Channels, believed to be formed by water, enter into the basin on all sides. [66] [67] [68] [69]

Dao Vallis, as seen by THEMIS. Click on image to see relationship of Dao Vallis to other nearby features, especially channels.

Dao Vallis begins near a large volcano, called Hadriaca Patera, so it is thought to have received water when hot magma melted huge amounts of ice in the frozen ground.[70] The partially circular depressions on the left side of the channel in the image to the right suggests that groundwater sapping also contributed water.[71] The Hellas drainage basin may be almost one-fifth the area of the entire northern plains. A lake in Hellas in today's Martian climate would form thick ice at the top that would eventually sublimate away. That is the ice would turn directly from a solid to a gas. This is similar to how dry ice (solid carbon dioxide) behaves on Earth.[72] Glacial features (terminal moraines, drumlins, and eskers) have been found that may have been formed when the water froze.[70] [73] A lake filling the Hellas Basin may have lasted a very long time, particularly if there were some geothermal sources of heat. Consequently, life may have developed here. [74]

  • Hellas Basin Area topography. Crater depth is 7152 m[75] (23,000 ft) below the standard topographic datum of Mars.
    Hellas Basin Area topography. Crater depth is 7152 m[75] (23,000 ft) below the standard topographic datum of Mars.
  • Hellas Basin with graph showing the great depth of the crater. It is the deepest crater on Mars and has the highest surface pressure: 1155 Pa[75] (11.55 mbar, 0.17 psi, or 0.01 atm).
    Hellas Basin with graph showing the great depth of the crater. It is the deepest crater on Mars and has the highest surface pressure: 1155 Pa[75] (11.55 mbar, 0.17 psi, or 0.01 atm).

Gale Crater

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Colorized shaded relief map of Gale crater. The general landing area for Curiosity on the northwestern crater floor, named Aeolis Palus, is circled. (HRSC data)

At 10:32 p.m. PDT on Aug. 5, 2012 (1:32 a.m. EDT on Aug. 6, 2012), the Mars Science Laboratory rover, Curiosity, landed on Mars at 4°30′S 137°24′E / 4.5°S 137.4°E / -4.5; 137.4, at the foot of a layered mountain inside Gale crater. The crater is named for Walter F. Gale (1865-1945), an amateur astronomer from Australia.

Gale is a crater on Mars near the northwestern part of the Aeolis quadrangle. Gale is 154 km (96 mi) in diameter and holds a mountain,Aeolis Mons (previously informally named "Mount Sharp" to pay tribute to geologist Robert P. Sharp) rising higher from the crater floor than Mount Rainier rises above Seattle. Gale is about the combined area of Connecticut and Rhode Island. Much evidence exists that Gale Crater once held a large lake. On August 6, 2012, the Mars Science Laboratory landed on Aeolis Palus near Aeolis Mons in Gale Crater.[76][77] [78] [79] [80] [81] The landing was 2.279 km (1.416 mi) from the target (4°35′31″S 137°26′25″E / 4.591817°S 137.440247°E / -4.591817; 137.440247), closer than any previous rover landing and well within the target area. As the days and months went on with Curiosity studying the surface, more and more discoveries and conclusions were released from NASA detailing the mounting evidence that Gale once contained a large lake. On September 27, 2012, NASA scientists announced that the Curiosity rover found evidence for an ancient streambed suggesting a "vigorous flow" of water on Mars.[82][83] [84] On December 9, 2013, NASA reported that, based on evidence from Curiosity studying Aeolis Palus, Gale Crater contained an ancient freshwater lake which could have been a hospitable environment for microbial life.[85][86] Curiosity found fine-grained sedimentary rocks, which represent an ancient lake that would have been suited to support life based on chemolithoautotrophy. This liquid water environment possessed a neutral pH, low salinity, and iron and sulfur in forms useable to certain types of organisms. Carbon, hydrogen, oxygen, sulfur, nitrogen -- the essential elements for life were measured. Gale’s ancient lake might have lasted hundreds to tens of thousands of years.[87] [88]

Smectite clays (trioctahedral) that are formed in the presence of water were found by Curiosity in sedimentary rocks (mudstones) at Yellowknife Bay in Gale crater. The mudstone samples were named John Klein and Cumberland. They are believed to have formed later than the Noachian period which means that water may have existed there longer than previously thought.

Hole (1.6 cm (0.63 in)) drilled into "John Klein" mudstone.
Spectral Analysis (SAM) of "Cumberland" mudstone.
Clay mineral structure of mudstone.
The Curiosity rover examines mudstone near Yellowknife Bay on Mars (May 2013).

Gale Crater contains a number of alluvial fans and deltas that provide information about lake levels in the past. These formations are: Pancake Delta, Western Delta, Farah Vallis delta and the Peace Vallis Fan.[89] In a press conference on December 8, 2014, Mars scientists discussed observations by Curiosity Rover that show Mars' Mount Sharp was built by sediments deposited in a large lake bed over tens of millions of years. This finding suggests the climate of ancient Mars could have produced long-lasting lakes at many places on the Planet. Rock layers indicate that a huge lake was filled and evaporated many times. The evidence was many deltas that were stacked upon each other.[90] [91] [92][93][94]

Curiosity rover - view of "Sheepbed" mudstone (lower left) and surroundings (February 14, 2013).

[95] [96]

Minerals called clays and sulfates are byproducts of water. They also may preserve signs of past life. The history of water at Gale, as recorded in its rocks, is giving Curiosity lots of clues to study as it pieces together whether Mars ever could have been a habitat for small life forms called microbes. Gale is special because both clays and sulfate minerals, which formed in water under different conditions, can be observed.

Evidence of water on Mars in Gale crater[82] [83] [84]
Peace Vallis and related alluvial fan near the Curiosity landing ellipse and landing site (noted by +).
"Hottah" rock outcrop on Mars - an ancient streambed viewed by Curiosity (September 14, 2012) (close-up) (3-D version).
"Link" rock outcrop on Mars - compared with a terrestrial fluvial conglomerate - suggesting water "vigorously" flowing in a stream.
Curiosity on the way to Glenelg (September 26, 2012).

Holden Crater

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Holden is a 140 km wide crater in the Margaritifer Sinus quadrangle. It is named after Edward Singleton Holden, an American astronomer, and the founder of the Astronomical Society of the Pacific.[97] Like some other craters on Mars, Holden has an outlet channel, Uzboi Vallis, that runs into it. Some features in the crater, especially lake deposits, seem to have been created by flowing water.[98] The crater's rim is cut with gullies, and at the end of some gullies are fan-shaped deposits of material transported by water.[99] [100] The crater is of great interest to scientists because it has some of the best-exposed lake deposits. One of the layers has been found by the Mars Reconnaissance Orbiter to contain clays.[101] [102] [103] Clays only form in the presence of water. It is believed that great amount of water went through this area; one flow was caused by a body of water larger than Earth's Lake Huron. This happened when water burst through a crater rim that was damming it. [104] Holden is an old crater, containing numerous smaller craters, many of which are filled with sediment. The crater's central mountain is also obscured by sediment. Much of the sediment probably originated from river and lake deposits.[105]

Holden
Crater Holden based on THEMIS day-time image


Geologic history of Holden Crater

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Studies of the whole region around Holden Crater have resulted in an understanding of a complex sequence of events that shaped the crater, which included two different lakes. [106] A large series of rivers called the Uzboi-Ladon-Morava (ULM) system drained water from the Argyre Basin, site of a large lake.[107] [108] [109] When an impact occurred and produced Holden Crater, the system was blocked by a crater rim almost a kilometer in height. Eventually water from drainage from the walls, with possibly a contribution from groundwater, collected to make the first lake. [110] [111] [112] This lake was deep and long lasting. The lowest level of sedimentary rocks was deposited in this lake. Much water was inbounded in Uzboi Vallis because the rim of Holden Crater blocked the flow. Some of the backed up water came from Nirgal Vallis which had a discharge of 4800 cubic meters/second. [113] At a certain point the stored water broke through the rim of Holden and created a second, shorter lived lake 200-250 m deep. [114] Water with a depth of at least 50 m entered Holden at a rate that 5-10 times the discharge of the Mississippi River.[115] [116] Cite error: A <ref> tag is missing the closing </ref> (see the help page). Terraces and the presence of large rocks (tens of meters across) support these high discharge rates. [117] [118] [119] [120] [121]


Western Elysium Planitia Paleolake

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There is evidence for a large lake in Western Elysium; however some researchers believe large lava flows can explain the terrain. [122] [123] The basin of this supposed lake has an area of more than 150 km2 and is covered with fractured plates and sinuous ridges that look like pack-ice on the Earth. [124] [125] [126] Sorted patterned ground and erosion patterns in polygonal terrain in the region support ice-rich material; hence a lake. Also, the presence of streamlined islands, cataracts, and dendritic channel systems suggest formation by water from a lake. [127] Some surfaces here show "Rootless cones" which are mounds with pits. They can be caused by explosions of lava with ground ice when lava flows on top of ice-rich ground. The ice melts and turns into a vapor that expands in an explosion that produces a cone or ring. Features like these are found in Iceland, when lavas cover water-saturated substrates. [128] [129] [130]The western Elysium Planitia basin can be described as almost a perfect equipotential surface because it slopes only about 10 m over a 500 km distance—that’s about as level as the Earth’s ocean. [131] This very gentle slope argues against a lava flow. [132] In places, it has been found that the flow surface has been lowered by 50% which is expected if the flow was of water, but not if it were lava. [133] The maximum depth of the lake was estimated to be between 31 and 53 m. [134] The Western Elysium Paleolake is in the southern part of the Elysium quadrangle, south of the Elysium volcanic field and near Cerberus Fossae. It is believed that the water for this paleolake emerged from troughs in Cerberus Fossae. Several opinions have been advanced to explain the exact mechanism, including groundwater discharge and [135] [136] a dike penetrating a cryosphere, [137]

  • Troughs of the Cerberus Fossae group, as seen by HiRISE under the HiWish program.
    Troughs of the Cerberus Fossae group, as seen by HiRISE under the HiWish program.
  • Portion of a trough (fossa) in Elysium, as seen by HiRISE under the HiWish program. Troughs are part of the Cerberus Fossae group.
    Portion of a trough (fossa) in Elysium, as seen by HiRISE under the HiWish program. Troughs are part of the Cerberus Fossae group.

Argyre basin

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The Argyre basin was created by a giant impact that occurred 70 million years after the Hellas impact.[138] It is believed to have contained a lake early in the history of Mars.[139] The Argyre basin is in the Argyre quadrangle. At least three river valleys (Surius Vallis, Dzigal Vallis, and Palacopus Vallis) drain into it from the south. After the Argyre lake froze solid, the ice formed eskers which are visible today.[140][141] An article written by 22 researchers in Icarus concluded that the impact that formed the Argyre basin probably stuck an ice cap or a thick permafrost layer. Energy from the impact melted the ice and formed a giant lake that eventually sent water to the North. The lake's volume was equal to that of Earth's Mediterranean Sea. The deepest part of the lake may have taken more than a hundred thousand years to freeze, but with the help of heat from the impact, geothermal heating, and dissolved solutes it may have had liquid water for many millions of years. Life may have developed in this time. This region shows a great deal of evidence of glacial activity with flow features, crevasse-like fractures, drumlines, eskers, tarns, aretes, cirques, horns, U-shaped valleys, and terraces. Because of the shapes of Argyre sinuous ridges, the authors concluded that they are eskers.[142]

  • MOLA maps showing the geographic context of Argyre.
    MOLA maps showing the geographic context of Argyre.
  • MOLA map showing boundaries for Argyre Planitia and other regions
    MOLA map showing boundaries for Argyre Planitia and other regions
  • Scene in Argyre quadrangle with gullies, alluvial fans, and hollows, as seen by HiRISE under HiWish program. Enlargements of parts of this image are below.
    Scene in Argyre quadrangle with gullies, alluvial fans, and hollows, as seen by HiRISE under HiWish program. Enlargements of parts of this image are below.
  • Several levels of alluvial fans, as seen by HiRISE under HiWish program. Locations of these fans are indicated in the previous image. Fans are formed with the action of water.
    Several levels of alluvial fans, as seen by HiRISE under HiWish program. Locations of these fans are indicated in the previous image. Fans are formed with the action of water.
  • Small, well-formed alluvial fan, as seen by HiRISE under HiWish program. Location of this fan is shown in an image displayed above. Water is involved with fan formation.
    Small, well-formed alluvial fan, as seen by HiRISE under HiWish program. Location of this fan is shown in an image displayed above. Water is involved with fan formation.

Lakes in Valles Marineris

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Coprates quadrangle
Map of Coprates quadrangle from Mars Orbiter Laser Altimeter (MOLA) data. The highest elevations are red and the lowest are blue.

Over the years, it has been suggested that lakes of various sizes existed in the giant Valles Marineris. [143] [144] [145] [146] However, the matter is still debated. Much discussion centers on the origin of layered structures called interior layered deposits (ILD’s). They are widely distributed in the Valles Marineris system. Some are free-standing mesas and mounds. Interior layered deposits are up to 9 km thick. [147]

Parts of the floors of Candor Chasma and Juventae Chasma contain interior layered deposits. These layers may have formed when the whole area was a giant lake. However, many other ideas have been advanced to explain them.[148] High-resolution structural and geologic mapping in west Candor Chasma, presented in March 2015, showed that the deposits on the floor of the Candor chasma are basin filling sediments that were deposited in a wet playa like setting; hence water was involved in their formation.[149]

One problem with the idea of large lakes in Valles Marineris is that there are no evident sources for the huge amount of water that would be required. Although many small channels exist in the region, there are no major channels. However, much water may have entered the system through the ground. [150] Cite error: A <ref> tag is missing the closing </ref> (see the help page). High-resolution structural and geologic mapping in west Candor Chasma, presented in March 2015, showed that the deposits on the floor of the Candor chasma are basin filling sediments that were deposited in a wet playa like setting; hence water was involved in their formation.[151] Minerals that are usually formed in the presence of water have been discovered in interior layered deposits; thus giving strong support for lakes. Some ILD’s contain hydrated sulfate deposits. Sulfate formation involves the presence of water. The European Space Agency's Mars Express found possible evidence of the sulfates epsomite and kieserite.[152] Likewise, ferric oxides in the form of crystalline grey hematite that probably required water for its formation have been found.[153] [154] [155]

Ritchey Crater

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Ritchey Crater is a crater in the Coprates quadrangle. It is 79 km in diameter and was named after George W. Ritchey, an American astronomer (1864-1945).[156] There is strong evidence that it was once a lake.[157] [158] Ritchey Crater has been suggested as a landing site for a Mars Rover.[159] A thick sequence of sedimentary deposits that include clay is found in the crater.[160] [161] Clay deposits indicate that water was probably present for a time. The presence of fluvial features along crater wall and rim, as well as alluvial/fluvial deposits, support the idea of lots of water being present at some time in the past.

  • Western side of Ritchey Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).
    Western side of Ritchey Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).
  • Fan along western wall of Ritchey Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of previous image.
    Fan along western wall of Ritchey Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of previous image.

Eridania Lake

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Eridania Lake is a theorized ancient lake with a surface area of roughly 1.1 million square kilometers.[162] [163] [164] It is located at the source of the Ma'adim Vallis outflow channel. It is located at the source of the Ma'adim Vallis outflow channel and extends into Eridania quadrangle and the Phaethontis quadrangle. [165] [166] As Eridania Lake dried out in the late Noachian epoch it divided into a series of smaller lakes.[167] [168] [169][170] Clays which require water for their formation have been found within the borders of this supposed lake. They were identified as Mg/Fe-bearing phyllosilicates and Al-rich phyllosilicates, using with hyperspectral data from CRISM. [171]

Columbus Crater

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Columbus Crater is a crater in the Memnonia quadrangle, is 119 km in diameter, and was named after Christopher Columbus, Italian explorer (1451–1506).[172] [173] Research with an orbiting near-infrared spectrometer, which reveals the types of minerals present based on the wavelengths of light they absorb, found evidence of layers of both clay and sulfates in Columbus crater. This is exactly what would appear if a large lake had slowly evaporated.[174] [175] [176] [177] Moreover, because some layers contained gypsum, a sulfate which forms in relatively fresh water, life could have formed in the crater.[178] The CRISM instrument on the Mars Reconnaissance Orbiter found kaolinite, hydrated sulfates including alunite and possibly jarosite.[179] Further study concluded that gypsum, polyhydrated and monohydrated Mg/Fe-sulfates were common and small deposits of montmorillonite, Fe/Mg-phyllosilicates, and crystalline ferric oxide or hydroxide were found. Thermal emission spectra suggest that some minerals were in the tens of percent range. These minerals suggest that water was present in the crater.[180] [181] Scientists are excited about finding hydrated minerals such as sulfates and clays on Mars because they are usually formed in the presence of water.[182] Places that contain clays and/or other hydrated minerals would be good places to look for evidence of life.[183] Sulfate minerals were found above aluminum-rich clays; this implies that early on , when the clays were formed, the water was more neutral and probably easier for life to develop. Sulfates are usually formed with more acid waters being present.[184]

Columbus Crater
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Columbus crater based on THEMIS day-time image
Diameter119 km
EponymChristopher Columbus, Italian explorer (1451-1506)
  • Columbus Crater Layers, as seen by HiRISE. This false-color image is about 800 feet across. Some of the layers contain hydrated minerals.
    Columbus Crater Layers, as seen by HiRISE. This false-color image is about 800 feet across. Some of the layers contain hydrated minerals.
Wikimedia Commons has media related to Columbus (Martian crater).

References

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  1. ^ http://www.space.com/18787-mariner-4.html
  2. ^ http://www.planetary.org/blogs/emily-lakdawalla/2012/12100800-mariner-4-mars.html
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  179. ^ Murchie, S. et al. 2009. A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter. Journal of Geophysical Research: 114.
  180. ^ https://pubs.er.usgs.gov/publication/70035986
  181. ^ Wray, J., R. Milliken, C. Dundas, G. Swayze, J. Andrews-Hanna, A. Baldridge, M. Chojnacki, J. Bishop, B. Ehlmann, S. Murchie, R. Clark, F. Seelos, L. Tornabene, and S. Squyres. 2011. Columbus crater and other possible groundwater-fed paleolakes of Terra Sirenum, Mars. Journal of Geophysical Research E: Planets DOI: 10.1029/2010JE003694
  182. ^ http://themis.asu.edu/features/nilosyrtis
  183. ^ http://hirise.lpl.arizona.edu/PSP_004046_2080
  184. ^ https://www.nasa.gov/mission_pages/msl/multimedia/pia15099.html#.VTj_UiFVhBd

See also

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