Water on Mars

From Wikipedia, the free encyclopedia
Jump to: navigation, search
For the music group, see Water on Mars (band). For the Doctor Who episode, see The Waters of Mars.
An artist's impression of what ancient Mars may have looked like, based on geological data.
Mars - Utopia Planitia
Martian terrain
Map of terrain
Scalloped terrain led to the discovery of a large amount of underground ice - enough water to fill Lake Superior (November 22, 2016)[1][2][3]

Almost all water on Mars today exists as ice, though it also exists in small quantities as vapor in the atmosphere[4] and occasionally as low-volume liquid brines in shallow Martian soil.[5][6] The only place where water ice is visible at the surface is at the north polar ice cap.[7] Abundant water ice is also present beneath the permanent carbon dioxide ice cap at the Martian south pole and in the shallow subsurface at more temperate latitudes.[8][9][10][11] More than five million cubic kilometers of ice have been identified at or near the surface of modern Mars, enough to cover the whole planet to a depth of 35 meters (115 ft).[12] Even more ice is likely to be locked away in the deep subsurface.[13]

Some liquid water may occur transiently on the Martian surface today, but only under certain conditions.[6][14][15][16] No large standing bodies of liquid water exist, because the atmospheric pressure at the surface averages just 600 pascals (0.087 psi)—about 0.6% of Earth's mean sea level pressure—and because the global average temperature is far too low (210 K (−63 °C; −82 °F)), leading to either rapid evaporation (sublimation) or rapid freezing. Before about 3.8 billion years ago, Mars may have had a denser atmosphere and higher surface temperatures,[17][18] allowing vast amounts of liquid water on the surface,[19][20] [21][22] possibly including a large ocean[23][24][25][26] that may have covered one-third of the planet.[27][28][29] Water has also apparently flowed across the surface for short periods at various intervals more recently in Mars' history.[30][31][32] On December 9, 2013, NASA reported that, based on evidence from the Curiosity rover studying Aeolis Palus, Gale Crater contained an ancient freshwater lake that could have been a hospitable environment for microbial life.[33][34]

Many lines of evidence indicate that water is abundant on Mars and has played a significant role in the planet's geologic history.[35][36] The present-day inventory of water on Mars can be estimated from spacecraft imagery, remote sensing techniques (spectroscopic measurements,[37][38] radar,[39] etc.), and surface investigations from landers and rovers.[40][41] Geologic evidence of past water includes enormous outflow channels carved by floods,[42] ancient river valley networks,[43][44] deltas,[45] and lakebeds;[46][47][48][49] and the detection of rocks and minerals on the surface that could only have formed in liquid water.[50] Numerous geomorphic features suggest the presence of ground ice (permafrost)[51] and the movement of ice in glaciers, both in the recent past[52][53][54][55] and present.[56] 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.

Although the surface of Mars was periodically wet and could have been hospitable to microbial life billions of years ago,[57] the current environment at the surface is dry and subfreezing, probably presenting an insurmountable obstacle for living organisms. In addition, Mars lacks a thick atmosphere, ozone layer, and magnetic field, allowing solar and cosmic radiation to strike the surface unimpeded. The damaging effects of ionizing radiation on cellular structure is another one of the prime limiting factors on the survival of life on the surface.[58][59] Therefore, the best potential locations for discovering life on Mars may be in subsurface environments.[60][61][62] On November 22, 2016, NASA reported finding a large amount of underground ice on the planet Mars - the volume of water detected is equivalent to the volume of water in Lake Superior.[1][2][3]

Understanding water on Mars is vital to assess the planet’s potential for harboring life and for providing usable resources for future human exploration. For this reason, 'Follow the Water' was the science theme of NASA's Mars Exploration Program (MEP) in the first decade of the 21st century. Discoveries by the 2001 Mars Odyssey, Mars Exploration Rovers (MERs), Mars Reconnaissance Orbiter (MRO), and Mars Phoenix Lander have been instrumental in answering key questions about water's abundance and distribution on Mars. The ESA's Mars Express orbiter has also provided essential data in this quest.[63] The Mars Odyssey, Mars Express, MER Opportunity rover, MRO, and Mars Science Lander Curiosity rover are still sending back data from Mars, and discoveries continue to be made.

Historical background[edit]

The notion of water on Mars preceded the space age by hundreds of years. Early telescopic observers correctly assumed that the white polar caps and clouds were indications of water's presence. These observations, coupled with the fact that Mars has a 24-hour day, led astronomer William Herschel to declare in 1784 that Mars probably offered its inhabitants "a situation in many respects similar to ours."[64]

Historical map of Mars from Giovanni Schiaparelli.
Mars canals illustrated by astronomer Percival Lowell, 1898.

By the start of the 20th century, most astronomers recognized that Mars was far colder and drier than Earth. The presence of oceans was no longer accepted, so the paradigm changed to an image of Mars as a "dying" planet with only a meager amount of water. The dark areas, which could be seen to change seasonally, were now thought to be tracts of vegetation.[65] The man most responsible for popularizing this view of Mars was Percival Lowell (1855–1916), who imagined a race of Martians constructing a network of canals to bring water from the poles to the inhabitants at the equator. Although generating tremendous public enthusiasm, Lowell's ideas were rejected by most astronomers. The consensus of the scientific establishment at the time is probably best summarized by English astronomer Edward Walter Maunder (1851–1928) who compared the climate of Mars to conditions atop a twenty-thousand-foot peak on an arctic island[66] where only lichen might be expected to survive.

In the meantime, many astronomers were refining the tool of planetary spectroscopy in hope of determining the composition of the Martian atmosphere. Between 1925 and 1943, Walter Adams and Theodore Dunham at the Mount Wilson Observatory tried to identify oxygen and water vapor in the Martian atmosphere, with generally negative results. The only component of the Martian atmosphere known for certain was carbon dioxide (CO2) identified spectroscopically by Gerard Kuiper in 1947.[67] Water vapor was not unequivocally detected on Mars until 1963.[68]

Mariner 4 acquired this image showing a barren planet (1965)

The composition of the polar caps, assumed to be water ice since the time of Cassini (1666), was questioned by a few scientists in the late 1800s who favored CO2 ice, because of the planet's overall low temperature and apparent lack of appreciable water. This hypothesis was confirmed theoretically by Robert Leighton and Bruce Murray in 1966.[69] Today we know that the winter caps at both poles are primarily composed of CO2 ice, but that a permanent (or perennial) cap of water ice remains during the summer at the northern pole. At the southern pole, a small cap of CO2 ice remains during summer, but this cap too is underlain by water ice.

The final piece of the Martian climate puzzle was provided by Mariner 4 in 1965. Grainy television pictures from the spacecraft showed a surface dominated by impact craters, which implied that the surface was very old and had not experienced the level of erosion and tectonic activity seen on Earth. Little erosion meant that liquid water had probably not played a large role in the planet's geomorphology for billions of years.[70] Furthermore, the variations in the radio signal from the spacecraft as it passed behind the planet allowed scientists to calculate the density of the atmosphere. The results showed an atmospheric pressure less than 1% of Earth’s at sea level, effectively precluding the existence of liquid water, which would rapidly boil or freeze at such low pressures.[71] Thus, a vision of Mars was born of a world much like the Moon, but with just a wisp of an atmosphere to blow the dust around. This view of Mars would last nearly another decade until Mariner 9 showed a much more dynamic Mars with hints that the planet’s past environment was more clement than the present one.

On January 24, 2014, NASA reported that current studies on Mars by the Curiosity and Opportunity rovers will now be searching for evidence of ancient life, including a biosphere based on autotrophic, chemotrophic and/or chemolithoautotrophic microorganisms, as well as ancient water, including fluvio-lacustrine environments (plains related to ancient rivers or lakes) that may have been habitable.[72][73][74][75]

For many years it was thought that the observed remains of floods were caused by the release of water from a global water table, but research published in 2015 reveals regional deposits of sediment and ice emplaced 450 million years earlier to be the source.[76] "Deposition of sediment from rivers and glacial melt filled giant canyons beneath primordial ocean contained within the planet's northern lowlands. It was the water preserved in these canyon sediments that was later released as great floods, the effects of which can be seen today."[42][76]

Evidence from rocks and minerals[edit]

Main article: Composition of Mars

Today, it is widely accepted that Mars had abundant water very early in its history,[77][78] but all large areas of liquid water have since disappeared. A fraction of this water is retained on modern Mars as both ice and locked into the structure of abundant water-rich materials, including clay minerals (phyllosilicates) and sulfates.[79][80][81][82][83] Studies of hydrogen isotopic ratios indicate that asteroids and comets from beyond 2.5 astronomical units (AU) provide the source of Mars' water,[84] that currently totals 6% to 27% of the Earth's present ocean.[84]

History of water on Mars. Numbers represent how many billions of years ago

Water in weathering products (aqueous minerals)[edit]

The primary rock type on the surface of Mars is basalt, a fine-grained igneous rock made up mostly of the mafic silicate minerals olivine, pyroxene, and plagioclase feldspar.[85] When exposed to water and atmospheric gases, these minerals chemically weather into new (secondary) minerals, some of which may incorporate water into their crystalline structures, either as H2O or as hydroxyl (OH). Examples of hydrated (or hydoxylated) minerals include the iron hydroxide goethite (a common component of terrestrial soils); the evaporate minerals gypsum and kieserite; opalline silica; and phyllosilicates (also called clay minerals), such as kaolinite and montmorillonite. All of these minerals have been detected on Mars.[86]

Minerals identified in Stokes crater from CRISM and OMEGA spectrometers. Green=olivine; Light blue=montmorillonite; Red=iron-magnesium phyllosilicate; Dark blue=kaolinite; Orange=pyroxene.

One direct effect of chemical weathering is to consume water and other reactive chemical species, taking them from mobile reservoirs like the atmosphere and hydrosphere and sequestering them in rocks and minerals.[87] The amount of water in the Martian crust stored in hydrated minerals is currently unknown, but may be quite large.[88] For example, mineralogical models of the rock outcroppings examined by instruments on the Opportunity rover at Meridiani Planum suggest that the sulfate deposits there could contain up to 22% water by weight.[89]

On Earth, all chemical weathering reactions involve water to some degree.[90] Thus, many secondary minerals do not actually incorporate water, but still require water to form. Some examples of anhydrous secondary minerals include many carbonates, some sulfates (e.g., anhydrite), and metallic oxides such as the iron oxide mineral hematite. On Mars, a few of these weathering products may theoretically form without water or with scant amounts present as ice or in thin molecular-scale films (monolayers).[91][92] The extent to which such exotic weathering processes operate on Mars is still uncertain. Minerals that incorporate water or form in the presence of water are generally termed "aqueous minerals."

Aqueous minerals are sensitive indicators of the type of environment that existed when the minerals formed. The ease with which aqueous reactions occur (see Gibbs free energy) depends on the pressure, temperature, and on the concentrations of the gaseous and soluble species involved.[93] Two important properties are pH and oxidation-reduction potential (Eh). For example, the sulfate mineral jarosite forms only in low pH (highly acidic) water. Phyllosilicates usually form in water of neutral to high pH (alkaline). Eh is a measure is the oxidation state of an aqueous system. Together Eh and pH indicate the types of minerals that are thermodynamically most likely to form from a given set of aqueous components. Thus, past environmental conditions on Mars, including those conducive to life, can be inferred from the types of minerals present in the rocks.

Hydrothermal alteration[edit]

Aqueous minerals can also form in the subsurface by hydrothermal fluids migrating through pores and fissures. The heat source driving a hydrothermal system may be nearby magma bodies or residual heat from large impacts.[94] One important type of hydrothermal alteration in the Earth’s oceanic crust is serpentinization, which occurs when seawater migrates through ultramafic and basaltic rocks. The water-rock reactions result in the oxidation of ferrous iron in olivine and pyroxene to produce ferric iron (as the mineral magnetite) yielding molecular hydrogen (H2) as a byproduct. The process creates a highly alkaline and reducing (low Eh) environment favoring the formation of certain phyllosilicates (serpentine minerals) and various carbonate minerals, which together form a rock called serpentinite.[95] The hydrogen gas produced can be an important energy source for chemosynthtetic organisms or it can react with CO2 to produce methane gas, a process that has been considered as a non-biological source for the trace amounts of methane reported in the Martian atmosphere.[96] Serpentine minerals can also store a lot of water (as hydroxyl) in their crystal structure. A recent study has argued that hypothetical serpentinites in the ancient highland crust of Mars could hold as much as a 500 metres (1,600 ft)-thick global equivalent layer (GEL) of water.[97] Although some serpentine minerals have been detected on Mars, no widespread outcroppings are evident from remote sensing data.[98] This fact does not preclude the presence of large amounts of sepentinite hidden at depth in the Martian crust.

Weathering rates[edit]

The rates at which primary minerals convert to secondary aqueous minerals vary. Primary silicate minerals crystallize from magma under pressures and temperatures vastly higher than conditions at the surface of a planet. When exposed to a surface environment these minerals are out of equilibrium and will tend to interact with available chemical components to form more stable mineral phases. In general, the silicate minerals that crystallize at the highest temperatures (solidify first in a cooling magma) weather the most rapidly.[99] On the Earth and Mars, the most common mineral to meet this criterion is olivine, which readily weathers to clay minerals in the presence of water.

Olivine is widespread on Mars,[100] suggesting that Mars' surface has not been pervasively altered by water; abundant geological evidence suggests otherwise.[101][102][103][104][105]

Martian meteorites[edit]

Mars meteorite ALH84001

Over 60 meteorites have been found that came from Mars.[106] Some of them contain evidence that they were exposed to water when on Mars. Some Martian meteorites called basaltic shergottites, appear (from the presence of hydrated carbonates and sulfates) to have been exposed to liquid water prior to ejection into space.[107][108] It has been shown that another class of meteorites, the nakhlites, were suffused with liquid water around 620 million years ago and that they were ejected from Mars around 10.75 million years ago by an asteroid impact. They fell to Earth within the last 10,000 years.[109]

In 1996, a group of scientists reported the possible presence of microfossils in the Allan Hills 84001, a meteorite from Mars.[110] Many studies disputed the validity of the fossils.[111][112] It was found that most of the organic matter in the meteorite was of terrestrial origin.[113]

Geomorphic evidence[edit]

Lakes and river valleys[edit]

The 1971 Mariner 9 spacecraft caused a revolution in our ideas about water on Mars. Huge river valleys were found in many areas. Images showed that floods of water broke through dams, carved deep valleys, eroded grooves into bedrock, and traveled thousands of kilometers.[42] Areas of branched streams, in the southern hemisphere, suggested that rain once fell.[114][115][116] The numbers of recognised valleys has increased through time. Research published in June 2010 mapped 40,000 river valleys on Mars, roughly quadrupling the number of river valleys that had previously been identified.[29] Martian water-worn features can be classified into two distinct classes: 1) dendritic (branched), terrestrial-scale, widely distributed, Noachian-age valley networks and 2) exceptionally large, long, single-thread, isolated, Hesperian-age outflow channels. Recent work suggests that there may also be a class of currently enigmatic, smaller, younger (Hesperian to Amazonian) channels in the midlatitudes, perhaps associated with the occasional local melting of ice deposits.[117][118]

Kasei Valles—a major outflow channel—seen in MOLA elevation data. Flow was from bottom left to right. Image is approx. 1600 km across. The channel system extends another 1200 km south of this image to Echus Chasma.

Some parts of Mars show inverted relief. This occurs when sediments are deposited on the floor of a stream and then become resistant to erosion, perhaps by cementation. Later the area may be buried. Eventually, erosion removes the covering layer and the former streams become visible since they are resistant to erosion. Mars Global Surveyor found several examples of this process.[119][120] Many inverted streams have been discovered in various regions of Mars, especially in the Medusae Fossae Formation,[121] Miyamoto Crater,[122] Saheki Crater,[123] and the Juventae Plateau.[124][125]

Inverted stream channels in Antoniadi Crater. Location is Syrtis Major quadrangle

A variety of lake basins have been discovered on Mars.[126] Some are comparable in size to the largest lakes on Earth, such as the Caspian Sea, Black Sea, and Lake Baikal. Lakes that were fed by valley networks are found in the southern highlands. There are places that are closed depressions with river valleys leading into them. These areas are thought to have once contained lakes; one is in Terra Sirenum that had its overflow move through Ma'adim Vallis into Gusev Crater, explored by the Mars Exploration Rover Spirit. Another is near Parana Valles and Loire Vallis.[127] Some lakes are thought to have formed by precipitation, while others were formed from groundwater.[46][47] Lakes are estimated to have existed in the Argyre basin,[35][36] the Hellas basin,[48][128] and maybe in Valles Marineris.[49][128][129][130] It is likely that at times in the Noachian, very many craters hosted lakes. These lakes are consistent with a cold, dry (by Earth standards) hydrological environment somewhat like that of the Great Basin of the western USA during the Last Glacial Maximum.[131]

Research from 2010 suggests that Mars also had lakes along parts of the equator. Although earlier research had showed that Mars had a warm and wet early history that has long since dried up, these lakes existed in the Hesperian Epoch, a much later period. Using detailed images from NASA's Mars Reconnaissance Orbiter, the researchers speculate that there may have been increased volcanic activity, meteorite impacts or shifts in Mars' orbit during this period to warm Mars' atmosphere enough to melt the abundant ice present in the ground. Volcanoes would have released gases that thickened the atmosphere for a temporary period, trapping more sunlight and making it warm enough for liquid water to exist. In this study, channels were discovered that connected lake basins near Ares Vallis. When one lake filled up, its waters overflowed the banks and carved the channels to a lower area where another lake would form.[132][133] These dry lakes would be targets to look for evidence (biosignatures) of past life.

On September 27, 2012, NASA scientists announced that the Curiosity rover found direct evidence for an ancient streambed in Gale Crater, suggesting an ancient "vigorous flow" of water on Mars.[134][135][136][137] In particular, analysis of the now dry streambed indicated that the water ran at 3.3 km/h (0.92 m/s),[134] possibly at hip-depth. Proof of running water came in the form of rounded pebbles and gravel fragments that could have only been weathered by strong liquid currents. Their shape and orientation suggests long-distance transport from above the rim of the crater, where a channel named Peace Vallis feeds into the alluvial fan.

Lake deltas[edit]

Researchers have found a number of examples of deltas that formed in Martian lakes.[28] Finding deltas is a major sign that Mars once had a lot of liquid water. Deltas usually require deep water over a long period of time to form. Also, the water level needs to be stable to keep sediment from washing away. Deltas have been found over a wide geographical range,[46] though there is some indication that deltas may be concentrated around the edges of the putative former northern ocean of Mars.[138]


Main article: Groundwater on Mars
Layers may be formed by groundwater rising up gradually

By 1979 it was thought that outflow channels formed in single, catastrophic ruptures of subsurface water reservoirs, possibly sealed by ice, discharging colossal quantities of water across an otherwise arid Mars surface.[139][140] In addition, evidence in favor of heavy or even catastrophic flooding is found in the giant ripples in the Athabasca Vallis.[141][142] Many outflow channels begin at Chaos or Chasma features, providing evidence for the rupture that could have breached a subsurface ice seal.[128]

The branching valley networks of Mars are not consistent with formation by sudden catastrophic release of groundwater, both in terms of their dendritic shapes that do not come from a single outflow point, and in terms of the discharges that apparently flowed along them.[143] Instead, some authors have argued that they were formed by slow seepage of groundwater from the subsurface essentially as springs.[144] In support of this interpretation, the upstream ends of many valleys in such networks begin with box canyon or "amphitheater" heads, which on Earth are typically associated with groundwater seepage. There is also little evidence of finer scale channels or valleys at the tips of the channels, which some authors have interpreted as showing the flow appeared suddenly from the subsurface with appreciable discharge, rather than accumulating gradually across the surface.[128] Others have disputed the strong link between amphitheater heads of valleys and formation by groundwater for terrestrial examples,[145] and have argued that the lack of fine scale heads to valley networks is due to their removal by weathering or impact gardening.[128] Most authors accept that most valley networks are at least partly influenced and shaped by groundwater seep processes.

The preservation and cementation of aeolian dune stratigraphy in Burns Cliff in Endurance Crater are thought to have been controlled by flow of shallow groundwater.[146]

Groundwater also plays a vital role in controlling broad scale sedimentation patterns and processes on Mars.[147] According to this hypothesis, groundwater with dissolved minerals came to the surface, in and around craters, and helped to form layers by adding minerals —especially sulfate— and cementing sediments.[146][148][149][150][151][152] In other words, some layers may be formed by groundwater rising up depositing minerals and cementing existing, loose, aeolian sediments. The hardened layers are consequently more protected from erosion. This process may occur instead of layers forming under lakes. A study published in 2011 using data from the Mars Reconnaissance Orbiter, show that the same kinds of sediments exist in a large area that includes Arabia Terra.[153] It has been argued that areas that we know from satellite remote sensing are rich in sedimentary rocks are also those areas that are most likely to experience groundwater upwelling on a regional scale.[154]

Mars ocean hypothesis[edit]

Main article: Mars ocean hypothesis

The Mars ocean hypothesis proposes that the Vastitas Borealis basin was the site of an ocean of liquid water at least once,[21] and presents evidence that nearly a third of the surface of Mars was covered by a liquid ocean early in the planet's geologic history.[126][155] This ocean, dubbed Oceanus Borealis,[21] would have filled the Vastitas Borealis basin in the northern hemisphere, a region that lies 4–5 kilometres (2.5–3.1 mi) below the mean planetary elevation. Two major putative shorelines have been suggested: a higher one, dating to a time period of approximately 3.8 billion years ago and concurrent with the formation of the valley networks in the Highlands, and a lower one, perhaps correlated with the younger outflow channels. The higher one, the 'Arabia shoreline', can be traced all around Mars except through the Tharsis volcanic region. The lower, the 'Deuteronilus', follows the Vastitas Borealis formation.[128]

A study in June 2010 concluded that the more ancient ocean would have covered 36% of Mars.[28][29] Data from the Mars Orbiter Laser Altimeter (MOLA), which measures the altitude of all terrain on Mars, was used in 1999 to determine that the watershed for such an ocean would have covered about 75% of the planet.[156] Early Mars would have required a warmer climate and denser atmosphere to allow liquid water to exist at the surface.[157][158] In addition, the large number of valley networks strongly supports the possibility of a hydrological cycle on the planet in the past.[148][159]

The existence of a primordial Martian ocean remains controversial among scientists, and the interpretations of some features as 'ancient shorelines' has been challenged.[160][161] One problem with the conjectured 2-billion-year-old (2 Ga) shoreline is that it is not flat—i.e., does not follow a line of constant gravitational potential. This could be due to a change in distribution in Mars' mass, perhaps due to volcanic eruption or meteor impact;[162] the Elysium volcanic province or the massive Utopia basin that is buried beneath the northern plains have been put forward as the most likely causes.[148]

In March 2015, scientists stated that evidence exists for an ancient Martian ocean, likely in the planet's northern hemisphere and about the size of Earth's Arctic Ocean, or approximately 19% of the Martian surface. This finding was derived from the ratio of water and deuterium in the modern Martian atmosphere compared to the ratio found on Earth. Eight times as much deuterium was found at Mars than exists on Earth, suggesting that ancient Mars had significantly higher levels of water. Results from the Curiosity rover had previously found a high ratio of deuterium in Gale Crater, though not significantly high enough to suggest the presence of an ocean. Other scientists caution that this new study has not been confirmed, and point out that Martian climate models have not yet shown that the planet was warm enough in the past to support bodies of liquid water.[163]

New evidence for a northern ocean was published in May 2016. A large team of scientists described how some of the surface in Ismenius Lacus quadrangle was altered by two Tsunamis. The Tsunamis were caused by asteroids striking the ocean. Both were thought to have been strong enough to create 30 km diameter craters. The first Tsunami picked up and carried boulders the size of cars or small houses. The backwash from the wave formed channels by rearranging the boulders. The second came in when the ocean was 300 m lower. The second carried a great deal of ice which was dropped in valleys. Calculations show that the average height of the waves would have been 50 m, but the heights would vary from 10 m to 120 m. Numerical simulations show that in this particular part of the ocean two impact craters of the size of 30 km in diameter would form every 30 million years. The implication here is that a great northern ocean may have existed for millions of years. One argument against an ocean has been the lack of shoreline features. These features may have been washed away by these Tsunami events. The parts of Mars studied in this research are Chryse Planitia and northwestern Arabia Terra. These tsunamis affected some surfaces in the Ismenius Lacus quadrangle and in the Mare Acidalium quadrangle.[164][165][166][167]

Present water ice[edit]

Proportion of water ice present in the upper meter of the Martian surface for lower (top) and higher (bottom) latitudes. The percentages are derived through stoichiometric calculations based on epithermal neutron fluxes. These fluxes were detected by the Neutron Spectrometer aboard the 2001 Mars Odyssey spacecraft.

A significant amount of surface hydrogen has been observed globally by the Mars Odyssey Neutron Spectrometer and Gamma Ray Spectrometer.[168] This hydrogen is thought to be incorporated into the molecular structure of ice, and through stoichiometric calculations the observed fluxes have been converted into concentrations of water ice in the upper meter of the Martian surface. This process has revealed that ice is both widespread and abundant on the modern surface. Below 60 degrees of latitude, ice is concentrated in several regional patches, particularly around the Elysium volcanoes, Terra Sabaea, and northwest of Terra Sirenum, and exists in concentrations up to 18% ice in the subsurface. Above 60 degrees latitude, ice is highly abundant. Polewards on 70 degrees of latitude, ice concentrations exceed 25% almost everywhere, and approach 100% at the poles.[169] More recently, the SHARAD and MARSIS radar sounding instruments have begun to be able to confirm whether individual surface features are ice rich. Due to the known instability of ice at current Martian surface conditions, it is thought that almost all of this ice must be covered by a veneer of rocky or dusty material.

The Mars Odyssey neutron spectrometer observations indicate that if all the ice in the top meter of the Martian surface were spread evenly, it would give a Water Equivalent Global layer (WEG) of at least ≈14 centimetres (5.5 in)—in other words, the globally averaged Martian surface is approximately 14% water.[170] The water ice currently locked in both Martian poles corresponds to a WEG of 30 metres (98 ft), and geomorphic evidence favors significantly larger quantities of surface water over geologic history, with WEG as deep as 500 metres (1,600 ft).[170] It is believed that part of this past water has been lost to the deep subsurface, and part to space, although the detailed mass balance of these processes remains poorly understood.[128] The current atmospheric reservoir of water is important as a conduit allowing gradual migration of ice from one part of the surface to another on both seasonal and longer timescales. It is insignificant in volume, with a WEG of no more than 10 micrometres (0.00039 in).[170]

Ice patches[edit]

On July 28, 2005, the European Space Agency announced the existence of a crater partially filled with frozen water;[171] some then interpreted the discovery as an "ice lake".[172] Images of the crater, taken by the High Resolution Stereo Camera on board the European Space Agency's Mars Express orbiter, clearly show a broad sheet of ice in the bottom of an unnamed crater located on Vastitas Borealis, a broad plain that covers much of Mars' far northern latitudes, at approximately 70.5° North and 103° East. The crater is 35 kilometres (22 mi) wide and about 2 kilometres (1.2 mi) deep. The height difference between the crater floor and the surface of the water ice is about 200 metres (660 ft). ESA scientists have attributed most of this height difference to sand dunes beneath the water ice, which are partially visible. While scientists do not refer to the patch as a "lake", the water ice patch is remarkable for its size and for being present throughout the year. Deposits of water ice and layers of frost have been found in many different locations on the planet.

As more and more of the surface of Mars has been imaged by the modern generation of orbiters, it has become gradually more apparent that there are probably many more patches of ice scattered across the Martian surface. Many of these putative patches of ice are concentrated in the Martian midlatitudes (≈30–60° N/S of the equator). For example, many scientists believe that the widespread features in those latitude bands variously described as "latitude dependent mantle" or "pasted-on terrain" consist of dust- or debris-covered ice patches, which are slowly degrading.[128] A cover of debris is required both to explain the dull surfaces seen in the images that do not reflect like ice, and also to allow the patches to exist for an extended period of time without subliming away completely. These patches have been suggested as possible water sources for some of the enigmatic channelized flow features like gullies also seen in those latitudes.

On November 22, 2016, NASA reported finding a large amount of underground ice on the planet Mars - the volume of water detected is equivalent to the volume of water in Lake Superior.[1][2][3]

Equatorial frozen sea[edit]

Surface features consistent with existing pack ice have been discovered in the southern Elysium Planitia.[126] What appear to be plates, ranging in size from 30 metres (98 ft) to 30 kilometres (19 mi), are found in channels leading to a flooded area of approximately the same depth and width as the North Sea. The plates show signs of break up and rotation that clearly distinguish them from lava plates elsewhere on the surface of Mars. The source for the flood is thought to be the nearby geological fault Cerberus Fossae that spewed water as well as lava aged some 2 to 10 million years. It was suggested that the water exited the Cerberus Fossae then pooled and froze in the low, level plains and that such lakes may still exist.[173] Not all scientists agree with these conclusions.[128][174][175]

Polar ice caps[edit]

The Mars Global Surveyor acquired this image of the Martian north polar ice cap in early northern summer.

Both the northern polar cap (Planum Boreum) and the southern polar cap (Planum Australe) are thought to grow in thickness during the winter and partially sublime during the summer. In 2004, the MARSIS radar sounder on the Mars Express satellite targeted the southern polar cap, and was able to confirm that ice there extends to a depth of 3.7 kilometres (2.3 mi) below the surface.[176] In the same year, the OMEGA instrument on the same orbiter revealed that the cap is divided into three distinct parts, with varying contents of frozen water depending on latitude. The first part is the bright part of the polar cap seen in images, centered on the pole, which is a mixture of 85% CO2 ice to 15% water ice.[9] The second part comprises steep slopes known as scarps, made almost entirely of water ice, that ring and fall away from the polar cap to the surrounding plains.[9] The third part encompasses the vast permafrost fields that stretch for tens of kilometres away from the scarps, and is not obviously part of the cap until the surface composition is analysed.[9][177] NASA scientists calculate that the volume of water ice in the south polar ice cap, if melted, would be sufficient to cover the entire planetary surface to a depth of 11 meters (36 ft).[176][178] Observations over both poles and more widely over the planet suggest melting all the surface ice would produce a water equivalent global layer 35 meters deep.[12]

Cross-section of a portion of the north polar ice cap of Mars, derived from satellite radar sounding.

On July 2008, NASA announced that the Phoenix lander had confirmed the presence of water ice at its landing site near the northern polar ice cap (at 68.2° latitude). This was the first ever direct observation of ice from the surface.[179] Two years later, the shallow radar on board the Mars Reconnaissance Orbiter took measurements of the north polar ice cap and determined that the total volume of water ice in the cap is 821,000 cubic kilometres (197,000 cu mi). That is equal to 30% of the Earth's Greenland ice sheet, or enough to cover the surface of Mars to a depth of 5.6 metres (18 ft).[180] Both polar caps reveal abundant fine internal layers when examined in HiRISE and Mars Global Surveyor imagery. Many researchers have attempted to use this layering to attempt to understand the structure, history, and flow properties of the caps,[128] although their interpretation is not straightforward.[181]

Lake Vostok in Antarctica may have implications for liquid water still existing on Mars, because if water existed before the polar ice caps on Mars, it is possible that there is still liquid water below the ice caps.[182]

Ground ice[edit]

For many years, various scientists have suggested that some Martian surfaces look like periglacial regions on Earth.[183] By analogy with these terrestrial features, it has been argued for many years that these are regions of permafrost. This would suggest that frozen water lies right beneath the surface. A common feature in the higher latitudes, patterned ground, can occur in a number of shapes, including stripes and polygons. On the Earth, these shapes are caused by the freezing and thawing of soil.[184] There are other types of evidence for large amounts of frozen water under the surface of Mars, such as terrain softening, which rounds sharp topographical features.[185] Theoretical calculations and analysis have tended to bear out the possibility that these are features are formed by the effects of ground ice. Evidence from Mars Odyssey's Gamma Ray Spectrometer and direct measurements with the Phoenix lander have corroborated that many of these features are intimately associated with the presence of ground ice.[186]

Stages in scallop formation in Hellas quadrangle

Some areas of Mars are covered with cones that resemble those on Earth where lava has flowed on top of frozen ground. The heat of the lava melts the ice, then changes it into steam. The powerful force of the steam works its way through the lava and produces such rootless cones. These features can be found for example in Athabasca Valles, associated with lava flowing along this outflow channel. Larger cones may be made when the steam passes through thicker layers of lava.[187]

Scalloped topography

Certain regions of Mars display scalloped-shaped depressions. The depressions are suspected to be the remains of a degrading ice-rich mantle deposit. Scallops are caused by ice sublimating from frozen soil. A study published in Icarus, found that the landforms of scalloped topography can be made by the subsurface loss of water ice by sublimation under current Martian climate conditions. Their model predicts similar shapes when the ground has large amounts of pure ice, up to many tens of meters in depth.[188] This mantle material was probably deposited from the atmosphere as ice formed on dust when the climate was different due to changes in the tilt of the Mars pole (see "Ice ages", below).[189][190] The scallops are typically tens of meters deep and from a few hundred to a few thousand meters across. They can be almost circular or elongated. Some appear to have coalesced causing a large heavily pitted terrain to form. The process of forming the terrain may begin with sublimation from a crack. There are often polygonal cracks where scallops form, and the presence of scalloped topography seems to be an indication of frozen ground.[125][191]

On November 22, 2016, NASA reported finding a large amount of underground ice in the Utopia Planitia region of Mars.[192] The volume of water detected has been estimated to be equivalent to the volume of water in Lake Superior.[1][2] The volume of water ice in the region were based on measurements from the ground-penetrating radar instrument on Mars Reconnaissance Orbiter, called SHARAD. From the data obtained from SHARAD, “dielectric permittivity”, or the dielectric constant was determined. The dielectric constant value was consistent with a large concentration of water ice.[193][194][195]

These scalloped features are superficially similar to Swiss cheese features, found around the south polar cap. Swiss cheese features are thought to be due to cavities forming in a surface layer of solid carbon dioxide, rather than water ice—although the floors of these holes are probably H2O-rich.[196]

Main article: Scalloped topography



Main article: Glaciers on Mars
View of a 5-km-wide, glacial-like lobe deposit sloping up into a box canyon. The surface has 'moraines', deposits of rocks that show how the glacier advanced.

Many large areas of Mars either appear to host glaciers, or carry evidence that they used to be present. Much of the areas in high latitudes, especially the Ismenius Lacus quadrangle, are suspected to still contain enormous amounts of water ice.[197][198] Recent evidence has led many planetary scientists to believe that water ice still exists as glaciers across much of the Martian mid- and high latitudes, protected from sublimation by thin coverings of insulating rock and/or dust.[39][56] In January 2009, scientists released the results of a radar study of the glacier-like features called lobate debris aprons in an area called Deuteronilus Mensae, which found widespread evidence of ice lying beneath a few meters of rock debris.[56] Glaciers are associated with fretted terrain, and many volcanoes. Researchers have described glacial deposits on Hecates Tholus,[199] Arsia Mons,[200] Pavonis Mons,[201] and Olympus Mons.[202] Glaciers have also been reported in a number of larger Martian craters in the midlatitudes and above.

Reull Vallis with lineated floor deposits. Location is Hellas quadrangle

Glacier-like features on Mars are known variously as viscous flow features,[203] Martian flow features, lobate debris aprons,[56] or lineated valley fill,[52] depending on the form of the feature, its location, the landforms it is associated with, and the author describing it. Many, but not all, small glaciers seem to be associated with gullies on the walls of craters and mantling material.[204] The lineated deposits known as lineated valley fill are probably rock-covered glaciers that are found on the floors most channels within the fretted terrain found around Arabia Terra in the northern hemisphere. Their surfaces have ridged and grooved materials that deflect around obstacles. Lineated floor deposits may be related to lobate debris aprons, which have been proven to contain large amounts of ice by orbiting radar.[39][56] For many years, researchers interpreted that features called 'lobate debris aprons' were glacial flows and it was thought that ice existed under a layer of insulating rocks.[55][205][206] With new instrument readings, it has been confirmed that lobate debris aprons contain almost pure ice that is covered with a layer of rocks.[39][56]

A ridge interpreted as the terminal moraine of an alpine glacier. Location is Ismenius Lacus quadrangle

Moving ice carries rock material, then drops it as the ice disappears. This typically happens at the snout or edges of the glacier. On Earth, such features would be called moraines, but on Mars they are typically known as moraine-like ridges, concentric ridges, or arcuate ridges.[207] Because ice tends to sublime rather than melt on Mars, and because Mars's low temperatures tend to make glaciers "cold based" (frozen down to their beds, and unable to slide), the remains of these glaciers and the ridges they leave do not appear the exactly same as normal glaciers on Earth. In particular, Martian moraines tend to be deposited without being deflected by the underlying topography, which is thought to reflect the fact that the ice in Martian glaciers is normally frozen down and cannot slide.[128] Ridges of debris on the surface of the glaciers indicate the direction of ice movement. The surface of some glaciers have rough textures due to sublimation of buried ice. The ice evaporates without melting and leaves behind an empty space. Overlying material then collapses into the void.[208] Sometimes chunks of ice fall from the glacier and get buried in the land surface. When they melt, a more or less round hole remains. Many of these "kettle holes" have been identified on Mars.[209]

Despite strong evidence for glacial flow on Mars, there is little convincing evidence for landforms carved by glacial erosion, e.g., U-shaped valleys, crag and tail hills, arêtes, drumlins. Such features are abundant in glaciated regions on Earth, so their absence on Mars has proven puzzling. The lack of these landforms is thought to be related to the cold-based nature of the ice in most recent glaciers on Mars. Because the solar insolation reaching the planet, the temperature and density of the atmosphere, and the geothermal heat flux are all lower on Mars than they are on Earth, modelling suggests the temperature of the interface between a glacier and its bed stays below freezing and the ice is literally frozen down to the ground. This prevents it from sliding across the bed, which is thought to inhibit the ice's ability to erode the surface.[128]

Development of Mars' water inventory[edit]

The variation in Mars's surface water content is strongly coupled to the evolution of its atmosphere and may have been marked by several key stages.

Dry channels near Warrego Valles

Early Noachian era (4.6 Ga to 4.1 Ga)[edit]

Atmospheric loss to space from heavy meteoritic bombardment and hydrodynamic escape.[210] Ejection by meteorites may have removed ~60% of the early atmosphere.[210][211] Significant quantities of phyllosilicates may have formed during this period requiring a sufficiently dense atmosphere to sustain surface water, as the spectrally dominant phyllosilicate group, smectite, suggests moderate water-to-rock ratios.[212] However, the pH-pCO2 between smectite and carbonate show that the precipitation of smectite would constrain pCO2 to a value not more than 1×10−2 atm (1.0 kPa).[212] As a result, the dominant component of a dense atmosphere on early Mars becomes uncertain, if the clays formed in contact with the Martian atmosphere,[213] particularly given the lack of evidence for carbonate deposits. An additional complication is that the ~25% lower brightness of the young Sun would have required an ancient atmosphere with a significant greenhouse effect to raise surface temperatures to sustain liquid water.[213] Higher CO2 content alone would have been insufficient, as CO2 precipitates at partial pressures exceeding 1.5 atm (1,500 hPa), reducing its effectiveness as a greenhouse gas.[213]

Middle to late Noachian era (4.1 Ga to 3.8 Ga)[edit]

Potential formation of a secondary atmosphere by outgassing dominated by the Tharsis volcanoes, including significant quantities of H2O, CO2, and SO2.[210][211] Martian valley networks date to this period, indicating globally widespread and temporally sustained surface water as opposed to catastrophic floods.[210] The end of this period coincides with the termination of the internal magnetic field and a spike in meteoritic bombardment.[210][211] The cessation of the internal magnetic field and subsequent weakening of any local magnetic fields allowed unimpeded atmospheric stripping by the solar wind. For example, when compared with their terrestrial counterparts, 38Ar/36Ar, 15N/14N, and 13C/12C ratios of the Martian atmosphere are consistent with ~60% loss of Ar, N2, and CO2 by solar wind stripping of an upper atmosphere enriched in the lighter isotopes via Rayleigh fractionation.[210] Supplementing the solar wind activity, impacts would have ejected atmospheric components in bulk without isotopic fractionation. Nevertheless, cometary impacts in particular may have contributed volatiles to the planet.[210]

Hesperian era to the present (~3.8 Ga to ~3.5 Ga)[edit]

Atmospheric enhancement by sporadic outgassing events were countered by solar wind stripping of the atmosphere, albeit less intensely than by the young Sun.[211] Catastrophic floods date to this period, favoring sudden subterranean release of volatiles, as opposed to sustained surface flows.[210] While the earlier portion of this era may have been marked by aqueous acidic environments and Tharsis-centric groundwater discharge[214] dating to the late Noachian, much of the surface alteration processes during the latter portion is marked by oxidative processes including the formation of Fe3+ oxides that impart a reddish hue to the Martian surface.[211] Such oxidation of primary mineral phases can be achieved by low-pH (and possibly high temperature) processes related to the formation of palagonitic tephra,[215] by the action of H2O2 that forms photochemically in the Martian atmosphere,[216] and by the action of water,[212] none of which require free O2. The action of H2O2 may have dominated temporally given the drastic reduction in aqueous and igneous activity in this recent era, making the observed Fe3+ oxides volumetrically small, though pervasive and spectrally dominant.[217] Nevertheless, aquifers may have driven sustained, but highly localized surface water in recent geologic history, as evident in the geomorphology of craters such as Mojave.[218] Furthermore, the Lafayette Martian meteorite shows evidence of aqueous alteration as recently as 650 Ma.[210]

Ice ages[edit]

North polar layered deposits of ice and dust

Mars has experienced large scale changes in the amount and distribution of ice on its surface in its relatively recent geological past, and as on Earth, these are known as ice ages.[219] Ice ages on Mars are very different from the ones that the Earth experiences. During a Martian ice age, the poles get warmer, and water ice then leaves the ice caps and is redeposited in mid latitudes.[220] The moisture from the ice caps travels to lower latitudes in the form of deposits of frost or snow mixed with dust. The atmosphere of Mars contains a great deal of fine dust particles, the water vapor condenses on these particles that then fall down to the ground due to the additional weight of the water coating. When ice at the top of the mantling layer returns to the atmosphere, it leaves behind dust that serves to insulate the remaining ice.[220] The total volume of water removed is a few percent of the ice caps, or enough to cover the entire surface of the planet under one meter of water. Much of this moisture from the ice caps results in a thick smooth mantle with a mixture of ice and dust.[189][221][222] This ice-rich mantle, a few meters thick, smoothes the land at lower latitudes, but in places it displays a bumpy texture. Multiple stages of glaciations probably occurred.[223] Because there are few craters on the current mantle, it is thought to be relatively young. It is thought that this mantle was laid in place during a relatively recent ice age.

Ice ages are driven by changes in Mars's orbit and tilt, which can be compared to terrestrial Milankovich cycles. Orbital calculations show that Mars wobbles on its axis far more than Earth does. The Earth is stabilized by its proportionally large moon, so it only wobbles a few degrees. Mars may change its tilt—also known as its obliquity—by many tens of degrees.[190] When this obliquity is high, its poles get much more direct sunlight and heat; this causes the ice caps to warm and become smaller as ice sublimes. Adding to the variability of the climate, the eccentricity of the orbit of Mars changes twice as much as Earth's eccentricity. As the poles sublime, the ice is redeposited closer to the equator, which receive somewhat less solar insolation at these high obliquities. Computer simulations have shown that a 45° tilt of the Martian axis would result in ice accumulation in areas that display glacial landforms.[224] A 2008 study provided evidence for multiple glacial phases during Late Amazonian glaciation at the dichotomy boundary on Mars.[225]

Evidence for recent flows[edit]

See also: Gully (Mars)
Warm-season flows on slope in Newton Crater
Branched gullies
Group of deep gullies

Pure liquid water cannot exist in a stable form on the surface of Mars with its present low atmospheric pressure and low temperature, except at the lowest elevations for a few hours.[177][226] So, a geological mystery commenced in 2006 when observations from NASA's Mars Reconnaissance Orbiter revealed gully deposits that were not there ten years prior, possibly caused by flowing liquid brine during the warmest months on Mars.[227][228][229] The images were of two craters called Terra Sirenum and Centauri Montes that appear to show the presence of liquid water flows on Mars at some point between 1999 and 2001.[228][230][231][232]

There is disagreement in the scientific community as to whether or not gullies are formed by liquid water. It is also possible that the flows that carve gullies are dry,[233] or perhaps lubricated by carbon dioxide. Some studies attest that gullies forming in the southern highlands could not be formed by water due to improper conditions. The low pressure, non-geothermal, colder regions would not give way to liquid water at any point in the year but would be ideal for solid carbon dioxide. The carbon dioxide melting in the warmer summer would yield liquid carbon dioxide which would then form the gullies.[234][235] Even if gullies are carved by flowing water at the surface, the exact source of the water and the mechanisms behind its motion are not well understood.[236]

In August 2011, NASA announced the discovery by Nepalese American undergraduate student Lujendra Ojha[237] of current seasonal changes on steep slopes below rocky outcrops near crater rims in the Southern hemisphere. These dark streaks, now called recurrent slope lineae, were seen to grow downslope during the warmest part of the Martian Summer, then to gradually fade through the rest of the year, recurring cyclically between years.[15] The researchers suggested these marks were consistent with salty water (brines) flowing downslope and then evaporating, possibly leaving some sort of residue.[238][239] The CRISM spectroscopic instrument has since made direct observations of hydrous salts appearing at the same time that these recurrent slope lineae form, confirming in 2015 that these lineae are produced by the flow of liquid brines through shallow soils. The lineae contain hydrated chlorate and perchlorate salts (ClO
), which contain liquid water molecules.[240] The lineae flow downhill in Martian summer, when the temperature is above −23 °C (−9 °F; 250 K).[241] However, the source of the water remains unknown.[6][242][243]

Habitability assessment[edit]

Main article: Life on Mars

Present day life on Mars could occur kilometers below the surface in the hydrosphere, or in subsurface geothermal hot spots, or it could occur on or near the surface. The permafrost layer on Mars is only a couple of centimeters below the surface. Salty brines can be liquid a few centimeters below that but not far down. Most of the proposed surface habitats are within centimeters of the surface. Any life deeper than that is likely to be dormant. Water is close to its boiling point even at the deepest points in the Hellas basin, and so cannot remain liquid for long on the surface of Mars in its present state, except when covered in ice or after a sudden release of water. The Mars atmosphere varies in pressure over geological timescales, and may have been able to host liquid water in the recent geological past.

So far, NASA has pursued a "Follow the water" strategy on Mars and has not searched for biosignatures for life there directly since Viking. The observations by Phoenix in 2008 of potential drops of liquid brines forming on its legs led to a renewed interest in the potential habitability of the surface of Mars. Nilton Renno and his team recently found a way that these droplets could form rapidly when salt and ice touch each other so may have formed when salt and ice from the surface got thrown up onto the legs during the landing.[244] Since then, experiments have led to many suggestions for potential habitats on the surface of Mars. However, though liquid water is now confirmed to occur there in brine layers, it's not yet known whether any of the liquid water on Mars is habitable. This depends on factors such as the exact mix of salts and the local conditions on Mars.

Proposed surface habitats[edit]

This is sorted roughly according to the level of attention in the literature.

  • Droplets of liquid water on salt / ice interfaces This is the result of a research team led by Nilton Renno, professor of atmospheric, oceanic and space sciences at Michigan University.[245][246] He is also project scientist for Curiosity in charge of the REMS weather station on Mars, was also a scientist on the Phoenix lander team.[247] He made the widely reported statement[248][249][250] about "swimming pools for bacteria" on Mars.[251] In the academic paper about this research he writes:[252] "These results have important implications for the understanding of the habitability of Mars because liquid water is essential for life as we know it, and halophilic terrestrial bacteria can thrive in brines". Ice and salt are both common in the higher latitudes of Mars, so these millimeter scale micro-habitats on salt / ice boundaries may likewise be a common feature on Mars.[252]
  • Warm Seasonal flows (Recurrent Slope Lineae) Many dark streaks form seasonally on Mars. Most of these are thought to be due to dry ice and wind effects. However a few of the streaks form in conditions that rule out all the usual mechanisms. These are the Warm Seasonal Flows, also known as Recurrent Slope Lineae.[253] They form on sun facing slopes in the summer when the local temperatures rise above 0C so far too warm for dry ice. They are not correlated at all with the winds and dust storms. They are also remarkably narrow and consistent in width through the length of the streak, when compared to a typical avalanche scar. They develop seasonally over many weeks, gradually extending down the slopes through summer - and then fade away in autumn. There is strong evidence now that they are associated with liquid water, due to seasonal changes in hydrated salts.[254][255][256][257][6] They may also be habitable but this depends on the salinity and the temperature of the water. They are currently classified as "Uncertain regions to be treated as special regions" for purposes of planetary protection.[258] A "special region" is a region where present day Earth life could potentially survive on the surface of Mars. See Habitability section of Seasonal flows on warm Martian slopes for details.
  • Life able to take up water from the 100% night time humidity of the Mars atmosphere A series of experiments by DLR (German aerospace company) in Mars simulation chambers and on the ISS show that some Earth life (Lichens and strains of chrooccocidiopsis, a green algae) can survive Mars surface conditions and photosynthesize and metabolize, slowly, in absence of any water at all. They could make use of the humidity of the Mars atmosphere.[259][260][261][262][263] Though the absolute humidity is low, the relative humidity at night reaches 100% because of the large day / night swings in atmospheric pressure and temperature. The lichens studied in these experiments have protection from UV light due to special pigments only found in lichens, such as parietin and antioxidants such as b-carotene in epilithic lichens. This gives them enough protection to tolerate the light levels in conditions of partial shade in the simulation chambers and make use of the light to photosynthesize. Indeed UV protection pigments have been suggested as potential biomarkers to search for on Mars.[264][265] The experimenters concluded that it is likely that some lichens and cyanobacteria can adapt to Mars conditions, taking advantage of the night time humidity, and that it is possible that life from early Mars could have adapted to these conditions and still survive today in microniches on the surface.[266]
  • Deliquescing salts taking up moisture from the Mars atmosphere Mars is rich in perchlorates - a discovery made by Phoenix, and later confirmed by Curiosity and by analysis of Martian meteorites on Earth. They probably occur over much of its surface.[267] Perchlorates deliquesce more easily than chlorides and at a lower temperature, so they could, potentially, take up water from the atmosphere more readily. The Mars atmosphere is less than 1% of the atmospheric pressure for Earth, still it reaches 100% humidity at night due to the low nighttime temperatures. Thin layers of salty perchlorate rich brines could form a short way below the surface at night and in the early morning. Since the humidity is taken directly from the atmosphere, this does not require the presence of ice on or near the surface. Some microbes on the Earth are able to survive in this way, for instance in salt pillars in the hyper arid core of the Atacama desert. They can do this at a remarkably low relative humidity, presumably making use of deliquescence of the salts.[268] Perchlorates are poisonous to many lifeforms. However, some Haloarchaea are able to tolerate them, and some can use them as a source of energy as well.[269] These layers are predicted to lie a few cms below the surface, and are likely to be thin films or droplets or patches of liquid brine. So,they probably won't be detected from orbit, at least not directly. Some of the layers may form in equatorial regions, and analysis of results from Curiosity in early 2015 has returned indirect evidence for presence of subsurface deliquescing brines in Gale Crater.[270] However the brines detected by Curiosity, though they get warm enough for Earth life, are then thought to be too salty for life, and when the water activity is high enough, they are too cold. Such cold brines may be habitable to native life if it has hydrogen peroxide or perchlorates as part of its biochemistry.[271] Other deliquescing salts on Mars may be more habitable for Earth life.[272]
  • Sun warmed dust grains embedded in ice Möhlmann originally suggested this process in 2011 as a possible way for liquid water to form on Mars, based on a mechanism that produces liquid water in similar conditions in Antarctica. As the sunlight hits the ice, it would preferentially warm up any heat absorbing dust grains trapped inside. These grains would then store heat and form water by melting some of the ice, and the water, covered by ice, would be protected from the vacuum conditions of the atmosphere.[273] They developed this model as a hypothesis to explain presence of extensive deposits of gypsum in the Northern polar ice cap and the dune fields around it, a process that has been been observed in Antarctica.[274][275]
  • Southern hemisphere flow like features (Not to be confused with the Northern Hemisphere flow like features which form under different conditions). These flow out of the dark deposits that form after the dry ice geysers erupt in early Spring. They grow at a rate of around 1.4 meters per Martian sol. All the models for these features, to date, involve some form of water. Möhlmann uses a solid state greenhouse effect in his model, similarly to the process that forms the geysers, but with translucent ice rather than dry ice as the solid state greenhouse layer.[276] In his model, first the ice forms a translucent layer - then as summer approaches, the solid state greenhouse effect raises the temperature of a layer below the surface to 0 °C, so melting it. This is a process familiar on the Earth for instance in Antarctica, where it forms preferentially in "blue ice".[277] On Mars, in his model, the melting layer is 5 to 10 cms below the surface. The liquid water layer starts off millimeters thick in their model, and can develop to be centimeters thick as the season progresses. This requires conditions for bare and optically transparent ice fields on Mars translucent to depths of several centimeters, and it's an open question whether this can happen, but there is nothing to rule it out either. The other open question is whether their assumption of low thermal conductivity of the ice, preventing escape of the heat to the surface, is valid on Mars.[278] This solid state greenhouse effect process favours equator facing slopes at higher lattitudes, close to the poles, over lower lattitudes, where surface ice can form to thicknesses of tens of centimeters. (The examples at Richardson crater are only 18° from the south pole.[279]). Another model for these southern hemisphere flow like features involves ULI water (undercooled liquid water) which forms as a thin layer over surfaces and can melt at well below the usual melting point of ice.This forms on the surfaces of solar heated grains in the ice, which then flows together down the slope, and can supply several litres a day of water to the seepage flows.[253][280] This ULI water would be the water source for liquid brines which then flow down the surface to form the features.
  • Shallow interfacial layers a few molecules thick These interfacial layers occur on boundaries between ice and rock due to intermolecular forces that depress the freezing point of the water. The water flows and acts as a solvent. They may be used by microbes in arctic permafrost, which have been found to metabolize at temperatures as low as -20 °C. Life may be possible in layers as thin as three monolayers, and the model by Stephen Jepsen et al obtained 109 cells/g at -20 °C, though the microbes would spend most of their time in survival mode.[281][282] Models show that interfacial water should form in some regions of Mars, for instance in Richardson crater.[283]
  • Advancing sand dunes bioreactor The idea behind this proposal is that the constantly moving sand dunes of Mars may be able to create a potential environment for life. Raw materials can be replenished, and the chemical disequilibrium needed for life maintained through churning of the sand by the winds. The water source is deliquescing salts.[284]

Proposed subsurface habitats[edit]

  • Ice covered lakes that form in polar regions after large impacts Models suggest that a crater 30 – 50 km in diameter formed by a comet of a few kilometers in diameter would result in an underground hydrothermal system that remains liquid for thousands of years. This happens even in cold conditions so is not limited to early Mars, so a similar impact based temporary underground hydrothermal system could be created today if there was a large enough impact like C/2013 A1 Siding Spring. The lake is kept heated by the melted rock from the initial impact in hydrothermal systems fed by underground aquifers.[285][286][287][288]
  • Temporary lakes resulting from volcanic activity There is evidence that volcanism formed lakes 210 million years ago on one of the flanks of Arsia Mons, relatively recent in geological terms. This may have consisted of two lakes of around 40 cubic kilometers of water, and a third one of 20 cubic kilometers of water, which probably remained liquid for hundreds, or even of the order of thousands of years.[289]
  • Possibility of geological hot spots in present day Mars There is clear evidence that Mars is not yet geologically inactive[290] This includes, small scale volcanic features associated with some of the volcanoes on Mars which must have formed in the very recent geological past.[291] There's also isotopic evidence from Phoenix of release of CO2 in the recent geological past.[292] It seems likely that there are magma plumes at least deep underground, associated with the occasional surface volcanism on the geological timescale of millions of years. And given that there has been activity on Olympus Mons as recently as four million years ago, it seems unlikely that all activity has stopped permanently. But so far no currently active volcanism has been observed, nor have any present day warm areas have ever been found on the surface, in extensive searches.[293] Another way to search for volcanic activity is through searches of trace gases produced in volcanic eruptions. So far nothing has been observed from Earth but instruments are limited in their sensitivity and get only limited observing time for Mars as well. This is going to be a focus of future searches however. One of the instruments on the the 2016 ExoMars Trace Gas Orbiter is NOMAD (Nadir and Occultation for Mars Discovery), which will search for trace gases indicating current volcanic activity, as well as searching directly for organics that could result from life processes, and the methane plumes.[294] If these hot spots exist, they could keep water liquid through geothermal heating. The water could be trapped under overlying deposits and kept at a pressure high enough to stay liquid. They could also be a source for intermittent surface or near surface water (for instance one of the hypotheses for the RSLs is that they may be occur over geological hot spots deep below the surface that indirectly supply them with water). Another possibility is a volcanic ice tower - a column of ice that can form around volcanic vents, for instance on Mount Erebus, Ross Island, Antarctica.[295] These would be only a few degrees higher in temperature than the surrounding landscape so easy to miss in thermal images from orbit.[296][297][298][299]
  • Potential for cave habitats on Mars As well as the lava tube caves, Mars may have other caves also less visible from orbit. It has most of the same processes that form caves on the Earth, and also has processes unique to Mars that may also create caves, for instance through direct sublimation of ice or dry ice into the atmosphere. Caves are of especial interest on Mars for astrobiology, because they can give protection from some of the harsh surface conditions. If the caves are isolated from the surface, or almost isolated, they may have conditions similar to similarly isolated caves on the Earth. In the "Workshop on Mars 2001", the main possibilities for cave formation listed are:[300] "(1) diversion of channel courses in underground conduits; (2) fractures of surface drainage patterns; chaotic terrain and collapsed areas in general; (4) seepage face in valley walls and/or headwaters; (5) inactive hydrothermal vents and lava tubes." In 2014, Penelope Boston lists some of the main possible types of cave.[301] She divides into the four main categories which she then divides into further subcategories. She also points out a few processes that may be unique to Mars, for instance, the abundance of sulfur on Mars may make sulfuric acid caves more common than they are on Mars. There's also the possibility of liquid CO2 (which forms under pressure, at depth, e.g. in a cliff wall) forming caves. The lava tubes on Mars are far larger than the ones on the Earth. Also Mars could have sublimational caves caused by dry ice and ordinary ice subliming directly into the atmosphere. Some cave habitats on Earth, if shielded from the surface, may be almost exact duplicates of similar habitats on Mars. For instance the Snottites in the toxic sulfur cave Cueva de Villa Luz flourish on Hydrogen Sulfide gas. Some of these species are aerobes (needing only small amounts of oxygen), and others are anaerobes and could survive anywhere on Mars where similar habitats exist. Mars has been shown to be geologically active in the recent geological past through the Phoenix isotope measurements.[292] Although there are no currently known geological hotspots or activity is currently known, there may well be subsurface thermal systems where caves similar to the Cueva de Villa Luz could occur.
  • Hydrosphere - possible layer of liquid water several kilometers below the surface Deep rock habitats on Earth are inhabited by life so may also be on Mars. However they need liquid water to survive, which may possibly exist below the cyrosphere layer of permanently frozen permafrost. In higher lattitudes it starts a few cms below the surface, and may continue down for several kilometers. In equatorial regions the surface of Mars may be completely dry down to a kilometer or more, so the cryosphere starts at the base of that dry layer. If the Mars hydrosphere exists, it lies below the cryosphere, and is a layer where the ice is kept liquid by geothermal heating, and prevented from evaporating by the overlying layers of ice. We don't have any evidence yet of a hydrosphere, but do have evidence of a deep subsurface cryosphere in the form of hydrogen / deuterium isotope ratios in Martian meteorites, which give indirect evidence that Mars must have a subsurface reservoir of water, most likely in the form of ice.[302][303] If it exists, estimates in a paper from 2013 put it's depth at around 5 kilometers below the surface. Whether this layer exists or not depends on the presence or otherwise of perchlorates, and clathrates, and it also depends on the total inventory of water on Mars, so there are many unknowns in the models.[304] If this hydrosphere exists, then it may be more habitable than similar depth zones on Earth because of the lower gravity, leading to larger pore size. Possible metabolisms at this depth could use hydrogen, carbon dioxide, and possibly abiotic hydrocarbons. The carbon for biomass could come from magmatic carbon in basalts which has been detected in Martian meteorites. It could also support methanogens feeding off methane released from serpentinization, and the alteration of basalt could also be a basis for iron respiration.[305] Similar habitats on Earth are inhabited by microbes and even multi-cellular life. So this is a potential habitat of astrobiological interest on Mars. As well as that, if the habitat exists it is a possible reservoir that could replenish surface areas of Mars with life and permit lifeforms to transfer from one part of Mars to another subsurface - a process that is known to happen beneath arctic permafrost layers.[306] It's not feasible to drill down to sample it in the near future. However, liquid may be released to the surface as a result of impact fracturing and other events so making it possible to sample it via surface measurements. One prime place to visit to search for evidence of the deep hydrosphere is McLaughlin Crater. The observations suggest it contained an ancient lake, with alteration minerals rich in Fe and Mg, and the detection of carbonates there suggests that the fluids were alkaline, and are consistent with the expected composition of fluids that emerged from the deep subsurface hydrosphere. The Nature article concludes "Lacustrine clay minerals and carbonates in McLaughlin Crater might be the best evidence for groundwater upwelling activity on Mars, and therefore should be considered a high-priority target for future exploration"[305]

Dormant subsurface life[edit]

Curiosity measured ionizing radiation levels of 76 mGy a year.[307] This level of ionizing radiation is sterilizing for dormant life on the surface of Mars. However, it varies considerably in habitability depending on its orbital eccentricity and the tilt of its axis. If the surface life has been reanimated as recently as 450,000 years ago, which is possible, then our rovers on Mars could find dormant but still viable life at a depth of only one meter below the surface, according to an estimate in the paper that published the Curiosity ionizing radiation measurements.[308]

Habitability factors for non-dormant surface life[edit]

Modern researchers do not consider that ionizing radiation is a limiting factor in habitability assessments for present-day non-dormant surface life. The level of 76 mGy a year measured by Curiosity is similar to levels inside the ISS.[309] In the 2014 Findings of the Second MEPAG Special Regions Science Analysis Group, their conclusion was:[258]

  • "From MSL RAD measurements, ionizing radiation from GCRs at Mars is so low as to be negligible. Intermittent SPEs can increase the atmospheric ionization down to ground level and increase the total dose, but these events are sporadic and last at most a few (2–5) days. These facts are not used to distinguish Special Regions on Mars."

Here a SPE is a Solar Proton Event (solar storm) and a GCR is a Galactic Cosmic Ray. A "Special Region" is a region where Earth life could potentially survive.

UV radiation[edit]

On UV radiation, the report finds [258]

  • "The martian UV radiation environment is rapidly lethal to unshielded microbes but can be attenuated by global dust storms and shielded completely by < 1 mm of regolith or by other organisms."


Though the superoxidizing conditions are harmful to some microbes, there are many microbes that actually metabolize perchlorates on Earth. See Perchlorates - Biology. Nowadays perchlorates on Mars are generally thought as boosting habitability. Even when Phoenix discovered perchlorates in 2008, NASA said that the perchlorates do not rule out life on Mars.[310] For a modern view on them, Cassie Conley, planetary protection officer for NASA is quoted in the New York times as saying:[311] [1]:

"The salts known as perchlorates that lower the freezing temperature of water at the R.S.L.s, keeping it liquid, can be consumed by some Earth microbes. “The environment on Mars potentially is basically one giant dinner plate for Earth organisms,” Dr. Conley said."

Recurrent Slope Lineae - potentially habitable[edit]

These features form on sun-facing slopes at times of the year when the local temperatures reach above the melting point for ice. The streaks grow in spring, widen in late summer and then fade away in autumn. This is hard to model in any other way except as involving liquid water in some form, though the streaks themselves are thought to be a secondary effect and not a direct indication of dampness of the regolith. Although these features are now confirmed to involve liquid water in some form, the water could be either too cold or too salty for life. At present they are treated as potentially habitable, as "Uncertain Regions, to be treated as Special Regions".

The "Special Regions" assessment says of them:[258]

  • "Although no single model currently proposed for the origin of RSL adequately explains all observations, they are currently best interpreted as being due to the seepage of water at > 250 K, with [water activity] unknown and perhaps variable. As such they meet the criteria for Uncertain Regions, to be treated as Special Regions. There are other features on Mars with characteristics similar to RSL, but their relationship to possible liquid water is much less likely"

They were first reported in the paper by McEwan in Science, August 5, 2011.[312] They were already suspected as involving flowing brines back then, as all the other models available involved liquid water in some form. Finally proven pretty much conclusively to involve liquid water in some form, possibly habitable if temperatures and salinity are right - after detection of hydrated salts that change their hydration state rapidly, reported in a paper published on 28 September 2015 along with a press conference [2].[313][256][257][6] The brines were not detected directly, because the resolution of the spectrometer isn't high enough for this, and also the brines probably flow in the morning. MRO is in a slowly precessing sun-synchronous orbit inclined at 93 degrees (orbital period 1 hr 52 minutes). Each time it crosses the Mars equator on the sunny side, South to North, the time is 3:00 pm, in the local solar time on the surface, all year round. This is the worst time of day to spot brines from orbit.[314]

Findings by probes[edit]

Mariner 9[edit]

Meander in Scamander Vallis, as seen by Mariner 9. Such images implied that large amounts of water once flowed on the surface of Mars.

The images acquired by the Mariner 9 Mars orbiter, launched in 1971, revealed the first direct evidence of past water in the form of dry river beds, canyons (including the Valles Marineris, a system of canyons over about 4,020 kilometres (2,500 mi) long), evidence of water erosion and deposition, weather fronts, fogs, and more.[315] The findings from the Mariner 9 missions underpinned the later Viking program. The enormous Valles Marineris canyon system is named after Mariner 9 in honor of its achievements.

Viking program[edit]

Main article: Viking program
Streamlined islands in Maja Valles suggest that large floods occurred on Mars

By discovering many geological forms that are typically formed from large amounts of water, the two Viking orbiters and the two landers caused a revolution in our knowledge about water on Mars. Huge outflow channels were found in many areas. They showed that floods of water broke through dams, carved deep valleys, eroded grooves into bedrock, and traveled thousands of kilometers.[316] Large areas in the southern hemisphere contained branched valley networks, suggesting that rain once fell.[317] Many craters look as if the impactor fell into mud. When they were formed, ice in the soil may have melted, turned the ground into mud, then the mud flowed across the surface.[114][115][183][318] Regions, called "Chaotic Terrain," seemed to have quickly lost great volumes of water that caused large channels to form downstream. Estimates for some channel flows run to ten thousand times the flow of the Mississippi River.[319] Underground volcanism may have melted frozen ice; the water then flowed away and the ground collapsed to leave chaotic terrain. Also, general chemical analysis by the two Viking landers suggested the surface has been either exposed to or submerged in water in the past.[320][321]

Mars Global Surveyor[edit]

Main article: Mars Global Surveyor
Map showing the distribution of hematite in Sinus Meridiani. This data was used to target the landing of the Opportunity rover that found definite evidence of past water.

The Mars Global Surveyor's Thermal Emission Spectrometer (TES) is an instrument able to determine the mineral composition on the surface of Mars. Mineral composition gives information on the presence or absence of water in ancient times. TES identified a large (30,000 square kilometres (12,000 sq mi)) area in the Nili Fossae formation that contains the mineral olivine.[322] It is thought that the ancient asteroid impact that created the Isidis basin resulted in faults that exposed the olivine. The discovery of olivine is strong evidence that parts of Mars have been extremely dry for a long time. Olivine was also discovered in many other small outcrops within 60 degrees north and south of the equator.[323] The probe has imaged several channels that suggest past sustained liquid flows, two of them are found in Nanedi Valles and in Nirgal Vallis.[324]

Inner channel (near top of the image) on floor of Nanedi Valles that suggests that water flowed for a fairly long period. Image from Lunae Palus quadrangle.

Mars Pathfinder[edit]

Main article: Mars Pathfinder

The Pathfinder lander recorded the variation of diurnal temperature cycle. It was coldest just before sunrise, about −78 °C (−108 °F; 195 K), and warmest just after Mars noon, about −8 °C (18 °F; 265 K). At this location, the highest temperature never reached the freezing point of water (0 °C (32 °F; 273 K)), too cold for pure liquid water to exist on the surface.

The atmospheric pressure measured by the Pathfinder on Mars is very low —about 0.6% of Earth's, and it would not permit pure liquid water to exist on the surface.[325]

Other observations were consistent with water being present in the past. Some of the rocks at the Mars Pathfinder site leaned against each other in a manner geologists term imbricated. It is suspected that strong flood waters in the past pushed the rocks around until they faced away from the flow. Some pebbles were rounded, perhaps from being tumbled in a stream. Parts of the ground are crusty, maybe due to cementing by a fluid containing minerals.[326] There was evidence of clouds and maybe fog.[326]

Mars Odyssey[edit]

Complex drainage system in Semeykin Crater. Location is Ismenius Lacus quadrangle

The 2001 Mars Odyssey found much evidence for water on Mars in the form of images, and with its spectrometer, it proved that much of the ground is loaded with water ice. Mars has enough ice just beneath the surface to fill Lake Michigan twice.[10] In both hemispheres, from 55° latitude to the poles, Mars has a high density of ice just under the surface; one kilogram of soil contains about 500 grams (18 oz) of water ice. But close to the equator, there is only 2% to 10% of water in the soil.[11] Scientists think that much of this water is also locked up in the chemical structure of minerals, such as clay and sulfates.[327][328] Although the upper surface contains a few percent of chemically-bound water, ice lies just a few meters deeper, as it has been shown in Arabia Terra, Amazonis quadrangle, and Elysium quadrangle that contain large amounts of water ice.[329] Analysis of the data suggests that the southern hemisphere may have a layered structure, suggestive of stratified deposits beneath a now extinct large water mass.[330]

Blocks in Aram showing a possible ancient source of water. Location is Oxia Palus quadrangle

The instruments aboard the Mars Odyssey are only able to study the top meter of soil, while the radar aboard the Mars Reconnaissance Orbiter can measure a few kilometers deep. In 2002, available data were used to calculate that if all soil surfaces were covered by an even layer of water, this would correspond to a global layer of water (GLW) 0.5–1.5 kilometres (0.31–0.93 mi).[331]

Thousands of images returned from Odyssey orbiter also support the idea that Mars once had great amounts of water flowing across its surface. Some images show patterns of branching valleys; others show layers that may have been formed under lakes; even river and lake deltas have been identified.[46][332] For many years researchers thought that glaciers existed under a layer of insulating rocks.[39][55][56][205][206] Lineated valley fill is one example of these rock-covered glaciers. They are found on the floors of some channels. Their surfaces have ridged and grooved materials that deflect around obstacles. Lineated floor deposits may be related to lobate debris aprons, which have been shown by orbiting radar to contain large amounts of ice.[39][56]


Main article: Phoenix (spacecraft)
Permafrost polygons imaged by the Phoenix lander

The Phoenix lander also confirmed the existence of large amounts of water ice in the northern region of Mars.[333][334] This finding was predicted by previous orbital data and theory,[335] and was measured from orbit by the Mars Odyssey instruments.[11] On June 19, 2008, NASA announced that dice-sized clumps of bright material in the "Dodo-Goldilocks" trench, dug by the robotic arm, had vaporized over the course of four days, strongly indicating that the bright clumps were composed of water ice that sublimes following exposure. Even though CO2 (dry ice) also sublimes under the conditions present, it would do so at a rate much faster than observed.[336] On July 31, 2008, NASA announced that Phoenix further confirmed the presence of water ice at its landing site. During the initial heating cycle of a sample, the mass spectrometer detected water vapor when the sample temperature reached 0 °C (32 °F; 273 K).[179] Liquid water cannot exist on the surface of Mars with its present low atmospheric pressure and temperature, except at the lowest elevations for short periods.[177][226][333][337]

Perchlorate (ClO4), a strong oxidizer, was confirmed to be in the soil. The chemical, when mixed with water, can lower the water freezing point in a manner similar to how salt is applied to roads to melt ice.

View underneath Phoenix lander showing water ice exposed by the landing retrorockets

When Phoenix landed, the retrorockets splashed soil and melted ice onto the vehicle.[338] Photographs showed the landing had left blobs of material stuck to the landing struts.[338] The blobs expanded at a rate consistent with deliquescence, darkened before disappearing (consistent with liquefaction followed by dripping), and appeared to merge. These observations, combined with thermodynamic evidence, indicated that the blobs were likely liquid brine droplets.[338][339] Other researchers suggested the blobs could be "clumps of frost."[340][341][342] In 2015 it was confirmed that perchlorate plays a role in forming recurring slope lineae on steep gullies.[6][343]

For about as far as the camera can see, the landing site is flat, but shaped into polygons between 2–3 metres (6 ft 7 in–9 ft 10 in) in diameter which are bounded by troughs that are 20–50 centimetres (7.9–19.7 in) deep. These shapes are due to ice in the soil expanding and contracting due to major temperature changes. The microscope showed that the soil on top of the polygons is composed of rounded particles and flat particles, probably a type of clay.[344] Ice is present a few inches below the surface in the middle of the polygons, and along its edges, the ice is at least 8 inches (200 mm) deep.[337]

Snow was observed to fall from cirrus clouds. The clouds formed at a level in the atmosphere that was around −65 °C (−85 °F; 208 K), so the clouds would have to be composed of water-ice, rather than carbon dioxide-ice (CO2 or dry ice), because the temperature for forming carbon dioxide ice is much lower than −120 °C (−184 °F; 153 K). As a result of mission observations, it is now suspected that water ice (snow) would have accumulated later in the year at this location.[345] The highest temperature measured during the mission, which took place during the Martian summer, was −19.6 °C (−3.3 °F; 253.6 K), while the coldest was −97.7 °C (−143.9 °F; 175.5 K). So, in this region the temperature remained far below the freezing point (0 °C (32 °F; 273 K)) of water.[346]

Mars Exploration Rovers[edit]

Close-up of a rock outcrop
Thin rock layers, not all parallel to each other
Hematite spherules
Partly embedded spherules

The Mars Exploration Rovers, Spirit and Opportunity found a great deal of evidence for past water on Mars. The Spirit rover landed in what was thought to be a large lake bed. The lake bed had been covered over with lava flows, so evidence of past water was initially hard to detect. On March 5, 2004, NASA announced that Spirit had found hints of water history on Mars in a rock dubbed "Humphrey".[347]

As Spirit traveled in reverse in December 2007, pulling a seized wheel behind, the wheel scraped off the upper layer of soil, uncovering a patch of white ground rich in silica. Scientists think that it must have been produced in one of two ways.[348] One: hot spring deposits produced when water dissolved silica at one location and then carried it to another (i.e. a geyser). Two: acidic steam rising through cracks in rocks stripped them of their mineral components, leaving silica behind.[349] The Spirit rover also found evidence for water in the Columbia Hills of Gusev crater. In the Clovis group of rocks the Mössbauer spectrometer (MB) detected goethite,[350] that forms only in the presence of water.[351][352][353] iron in the oxidized form Fe3+,[354] carbonate-rich rocks, which means that regions of the planet once harbored water.[355][356]

The Opportunity rover was directed to a site that had displayed large amounts of hematite from orbit. Hematite often forms from water. The rover indeed found layered rocks and marble- or blueberry-like hematite concretions. Elsewhere on its traverse, Opportunity investigated aeolian dune stratigraphy in Burns Cliff in Endurance Crater. Its operators concluded that the preservation and cementation of these outcrops had been controlled by flow of shallow groundwater.[146] In its years of continuous operation, Opportunity is still sending back evidence that this area on Mars was soaked in liquid water in the past.[357][358]

The MER rovers had been finding evidence for ancient wet environments that were very acidic. In fact, what Opportunity has mostly discovered, or found evidence for, was sulphuric acid, a harsh chemical for life.[40][41][359][360] But on May 17, 2013, NASA announced that Opportunity found clay deposits that typically form in wet environments that are near neutral acidity. This find provides additional evidence about a wet ancient environment possibly favorable for life.[40][41]

Mars Reconnaissance Orbiter[edit]

Springs in Vernal Crater, as seen by HIRISE. These springs may be good places to look for evidence of past life, because hot springs can preserve evidence of life forms for a long time. Location is Oxia Palus quadrangle.

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. A major discovery was finding evidence of ancient hot springs. If they have hosted microbial life, they may contain biosignatures.[361] Research published in January 2010, described strong evidence for sustained precipitation in the area around Valles Marineris.[124][125] The types of minerals there are associated with water. Also, the high density of small branching channels indicates a great deal of precipitation.

Rocks on Mars have been found to frequently occur as layers, called strata, in many different places.[362] Layers form by various ways, including volcanoes, wind, or water.[363] Light-toned rocks on Mars have been associated with hydrated minerals like sulfates and clay.[364]

Layers on the west slope of Asimov Crater. Location is Noachis quadrangle.

The orbiter helped scientists determine that much of the surface of Mars is covered by a thick smooth mantle that is thought to be a mixture of ice and dust.[189][365][366]

The ice mantle under the shallow subsurface is thought to result from frequent, major climate changes. Changes in Mars' 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 returns to the 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.[229] Water vapor condenses on the particles, then they fall down to the ground due to the additional weight of the water coating. When ice at the top of the mantling layer goes back into the atmosphere, it leaves behind dust, which insulates the remaining ice.[220]

In 2008, research with the Shallow Radar on the Mars Reconnaissance Orbiter provided strong evidence that the lobate debris aprons (LDA) in Hellas Planitia and in mid northern latitudes are glaciers that are covered with a thin layer of rocks. Its radar also detected a strong reflection from the top and base of LDAs, meaning that pure water ice made up the bulk of the formation.[39] The discovery of water ice in LDAs demonstrates that water is found at even lower latitudes.[183]

Research published in September 2009, demonstrated that some new craters on Mars show exposed, pure water ice.[367] After a time, the ice disappears, evaporating into the atmosphere. The ice is only a few feet deep. The ice was confirmed with the Compact Imaging Spectrometer (CRISM) on board the Mars Reconnaissance Orbiter.[368]

Curiosity rover[edit]

"Hottah" rock outcrop – an ancient streambed discovered by the Curiosity rover team (September 14, 2012) (close-up) (3-D version).
Rock outcrop on Mars – compared with a terrestrial fluvial conglomerate – suggesting water "vigorously" flowing in a stream.[134][135][136]

Very early in its ongoing mission, NASA's Curiosity rover discovered unambiguous fluvial sediments on Mars. The properties of the pebbles in these outcrops suggested former vigorous flow on a streambed, with flow between ankle- and waist-deep. These rocks were found at the foot of an alluvial fan system descending from the crater wall, which had previously been identified from orbit.[134][135][136]

On October 2012, the first X-ray diffraction analysis of a Martian soil was performed by Curiosity. The results revealed the presence of several minerals, including feldspar, pyroxenes and olivine, and suggested that the Martian soil in the sample was similar to the weathered basaltic soils of Hawaiian volcanoes. The sample used is composed of dust distributed from global dust storms and local fine sand. So far, the materials Curiosity has analyzed are consistent with the initial ideas of deposits in Gale Crater recording a transition through time from a wet to dry environment.[369]

In December 2012, NASA reported that Curiosity performed its first extensive soil analysis, revealing the presence of water molecules, sulfur and chlorine in the Martian soil.[370][371] And in March 2013, NASA reported evidence of mineral hydration, likely hydrated calcium sulfate, in several rock samples including the broken fragments of "Tintina" rock and "Sutton Inlier" rock as well as in veins and nodules in other rocks like "Knorr" rock and "Wernicke" rock.[372][373][374] Analysis using the rover's DAN instrument provided evidence of subsurface water, amounting to as much as 4% water content, down to a depth of 60 cm (2.0 ft), in the rover's traverse from the Bradbury Landing site to the Yellowknife Bay area in the Glenelg terrain.[372]

On September 26, 2013, NASA scientists reported the Mars Curiosity rover detected abundant chemically-bound water (1.5 to 3 weight percent) in soil samples at the Rocknest region of Aeolis Palus in Gale Crater.[375][376][377][378][379][380] In addition, NASA reported the rover found two principal soil types: a fine-grained mafic type and a locally derived, coarse-grained felsic type.[377][379][381] The mafic type, similar to other martian soils and martian dust, was associated with hydration of the amorphous phases of the soil.[381] Also, perchlorates, the presence of which may make detection of life-related organic molecules difficult, were found at the Curiosity rover landing site (and earlier at the more polar site of the Phoenix lander) suggesting a "global distribution of these salts".[380] NASA also reported that Jake M rock, a rock encountered by Curiosity on the way to Glenelg, was a mugearite and very similar to terrestrial mugearite rocks.[382]

On December 9, 2013, NASA reported that the planet Mars had a large freshwater lake (that could have been a hospitable environment for microbial life) based on evidence from the Curiosity rover studying the plain Aeolis Palus near Mount Sharp in Gale Crater.[33][34]

On December 16, 2014, NASA reported detecting an unusual increase, then decrease, in the amounts of methane in the atmosphere of the planet Mars; in addition, organic chemicals were detected in powder drilled from a rock by the Curiosity rover. Also, based on deuterium to hydrogen ratio studies, much of the water at Gale Crater on Mars was found to have been lost during ancient times, before the lakebed in the crater was formed; afterwards, large amounts of water continued to be lost.[383][384][385]

On April 13, 2015, Nature published an analysis of humidity and ground temperature data collected by Curiosity, showing evidence that films of liquid brine water form in the upper 5 cm of Mars's subsurface at night. The water activity and temperature remain below the requirements for reproduction and metabolism of known terrestrial microorganisms.[5][386]

On October 8, 2015, NASA confirmed that lakes and streams existed in Gale crater 3.3 - 3.8 billion years ago delivering sediments to build up the lower layers of Mount Sharp.[387][388]

Interactive Mars map[edit]

Acidalia Planitia Acidalia Planitia Alba Mons Amazonis Planitia Aonia Terra Arabia Terra Arcadia Planitia Arcadia Planitia Argyre Planitia Elysium Mons Elysium Planitia Hellas Planitia Hesperia Planum Isidis Planitia Lucas Planum Lyot (crater) Noachis Terra Olympus Mons Promethei Terra Rudaux (crater) Solis Planum Tempe Terra Terra Cimmeria Terra Sabaea Terra Sirenum Tharsis Montes Utopia Planitia Valles Marineris Vastitas Borealis Vastitas BorealisMap of Mars
Interactive imagemap of the global topography of Mars. Hover your mouse to see the names of over 25 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. Reds and pinks are higher elevation (+3 km to +8 km); yellow is 0 km; greens and blues are lower elevation (down to −8 km). Whites (>+12 km) and browns (>+8 km) are the highest elevations. Axes are latitude and longitude; Poles are not shown.
(also see: Mars Rovers map) (viewdiscuss)

See also[edit]


  1. ^ a b c d Staff (November 22, 2016). "Scalloped Terrain Led to Finding of Buried Ice on Mars". NASA. Retrieved November 23, 2016. 
  2. ^ a b c d "Lake of frozen water the size of New Mexico found on Mars – NASA". The Register. November 22, 2016. Retrieved November 23, 2016. 
  3. ^ a b c "Mars Ice Deposit Holds as Much Water as Lake Superior". NASA. November 22, 2016. Retrieved November 23, 2016. 
  4. ^ Jakosky, B.M.; Haberle, R.M. (1992). "The Seasonal Behavior of Water on Mars". In Kieffer, H.H.; et al. Mars. Tucson, AZ: University of Arizona Press. pp. 969–1016. 
  5. ^ a b Martín-Torres, F. Javier; Zorzano, María-Paz; Valentín-Serrano, Patricia; Harri, Ari-Matti; Genzer, Maria (April 13, 2015). "Transient liquid water and water activity at Gale crater on Mars". Nature Geocience. 8 (5): 357–361. Bibcode:2015NatGe...8..357M. doi:10.1038/ngeo2412. Retrieved April 14, 2015. 
  6. ^ a b c d e f Ojha, L.; Wilhelm, M. B.; Murchie, S. L.; McEwen, A. S.; Wray, J. J.; Hanley, J.; Massé, M.; Chojnacki, M. (2015). "Spectral evidence for hydrated salts in recurring slope lineae on Mars". Nature Geoscience. 8 (11): 829–832. Bibcode:2015NatGe...8..829O. doi:10.1038/ngeo2546. 
  7. ^ Carr, M.H. (1996). Water on Mars. New York: Oxford University Press. p. 197. 
  8. ^ Bibring, J.-P.; Langevin, Yves; Poulet, François; Gendrin, Aline; Gondet, Brigitte; Berthé, Michel; Soufflot, Alain; Drossart, Pierre; Combes, Michel; Bellucci, Giancarlo; Moroz, Vassili; Mangold, Nicolas; Schmitt, Bernard; Omega Team, the; Erard, S.; Forni, O.; Manaud, N.; Poulleau, G.; Encrenaz, T.; Fouchet, T.; Melchiorri, R.; Altieri, F.; Formisano, V.; Bonello, G.; Fonti, S.; Capaccioni, F.; Cerroni, P.; Coradini, A.; Kottsov, V.; et al. (2004). "Perennial Water Ice Identified in the South Polar Cap of Mars". Nature. 428 (6983): 627–630. Bibcode:2004Natur.428..627B. doi:10.1038/nature02461. PMID 15024393. 
  9. ^ a b c d "Water at Martian south pole". European Space Agency (ESA). March 17, 2004. 
  10. ^ a b "Mars Odyssey: Newsroom". Mars.jpl.nasa.gov. May 28, 2002. 
  11. ^ a b c Feldman, W.C.; et al. (2004). "Global Distribution of Near-Surface Hydrogen on Mars". J. Geophysical Research. 109. Bibcode:2004JGRE..10909006F. doi:10.1029/2003JE002160. 
  12. ^ a b Christensen, P. R. (2006). "Water at the Poles and in Permafrost Regions of Mars". GeoScienceWorld Elements. 3 (2): 151–155. 
  13. ^ Carr, 2006, p. 173.
  14. ^ Hecht, M.H. (2002). "Metastability of Liquid Water on Mars". Icarus. 156 (2): 373–386. Bibcode:2002Icar..156..373H. doi:10.1006/icar.2001.6794. 
  15. ^ a b Webster, Guy; Brown, Dwayne (December 10, 2013). "NASA Mars Spacecraft Reveals a More Dynamic Red Planet". NASA. 
  16. ^ "Liquid Water From Ice and Salt on Mars". Geophysical Research Letters. NASA Astrobiology. July 3, 2014. Retrieved August 13, 2014. 
  17. ^ Pollack, J.B. (1979). "Climatic Change on the Terrestrial Planets". Icarus. 37 (3): 479–553. Bibcode:1979Icar...37..479P. doi:10.1016/0019-1035(79)90012-5. 
  18. ^ Pollack, J.B.; Kasting, J.F.; Richardson, S.M.; Poliakoff, K. (1987). "The Case for a Wet, Warm Climate on Early Mars". Icarus. 71 (2): 203–224. Bibcode:1987Icar...71..203P. doi:10.1016/0019-1035(87)90147-3. 
  19. ^ "releases/2015/03/150305140447". sciencedaily.com. Retrieved May 25, 2015. 
  20. ^ Villanueva, G.; Mumma, M.; Novak, R.; Käufl, H.; Hartogh, P.; Encrenaz, T.; Tokunaga, A.; Khayat, A.; Smith, M. (2015). "Strong water isotopic anomalies in the martian atmosphere: Probing current and ancient reservoirs". Science. 348 (6231): 218–221. Bibcode:2015Sci...348..218V. doi:10.1126/science.aaa3630. 
  21. ^ a b c Baker, V.R.; Strom, R.G.; Gulick, V.C.; Kargel, J.S.; Komatsu, G.; Kale, V.S. (1991). "Ancient oceans, ice sheets and the hydrological cycle on Mars". Nature. 352 (6348): 589–594. Bibcode:1991Natur.352..589B. doi:10.1038/352589a0. 
  22. ^ Salese, F.; Ansan, V.; Mangold, N.; Carter, J.; Anouck, O.; Poulet, F.; Ori, G.G. (2016). "A sedimentary origin for intercrater plains north of the Hellas basin: Implications for climate conditions and erosion rates on early Mars". Journal of Geophysical Research: Planets. 121 (11): 2239–2267. doi:10.1002/2016JE005039. 
  23. ^ Parker, T.J.; Saunders, R.S.; Schneeberger, D.M. (1989). "Transitional Morphology in West Deuteronilus Mensae, Mars: Implications for Modification of the Lowland/Upland Boundary". Icarus. 82: 111–145. Bibcode:1989Icar...82..111P. doi:10.1016/0019-1035(89)90027-4. 
  24. ^ Dohm, J.M.; Baker, Victor R.; Boynton, William V.; Fairén, Alberto G.; Ferris, Justin C.; Finch, Michael; Furfaro, Roberto; Hare, Trent M.; Janes, Daniel M.; Kargel, Jeffrey S.; Karunatillake, Suniti; Keller, John; Kerry, Kris; Kim, Kyeong J.; Komatsu, Goro; Mahaney, William C.; Schulze-Makuch, Dirk; Marinangeli, Lucia; Ori, Gian G.; Ruiz, Javier; Wheelock, Shawn J. (2009). "GRS Evidence and the Possibility of Paleooceans on Mars". Planetary and Space Science. 57 (5–6): 664–684. Bibcode:2009P&SS...57..664D. doi:10.1016/j.pss.2008.10.008. 
  25. ^ "PSRD: Ancient Floodwaters and Seas on Mars". Psrd.hawaii.edu. July 16, 2003. 
  26. ^ "Gamma-Ray Evidence Suggests Ancient Mars Had Oceans". SpaceRef. November 17, 2008. 
  27. ^ Clifford, S.M.; Parker, T.J. (2001). "The Evolution of the Martian Hydrosphere: Implications for the Fate of a Primordial Ocean and the Current State of the Northern Plains". Icarus. 154: 40–79. Bibcode:2001Icar..154...40C. doi:10.1006/icar.2001.6671. 
  28. ^ a b c Di Achille, Gaetano; Hynek, Brian M. (2010). "Ancient ocean on Mars supported by global distribution of deltas and valleys". Nature Geoscience. 3 (7): 459–463. Bibcode:2010NatGe...3..459D. doi:10.1038/ngeo891. 
  29. ^ a b c "Ancient ocean may have covered third of Mars". Sciencedaily.com. June 14, 2010. 
  30. ^ Carr, 2006, pp 144–147.
  31. ^ Fassett, C. I.; Dickson, James L.; Head, James W.; Levy, Joseph S.; Marchant, David R. (2010). "Supraglacial and Proglacial Valleys on Amazonian Mars". Icarus. 208 (1): 86–100. Bibcode:2010Icar..208...86F. doi:10.1016/j.icarus.2010.02.021. 
  32. ^ "Flashback: Water on Mars Announced 10 Years Ago". SPACE.com. June 22, 2000. 
  33. ^ a b Chang, Kenneth (December 9, 2013). "On Mars, an Ancient Lake and Perhaps Life". New York Times. 
  34. ^ a b Various (December 9, 2013). "Science – Special Collection – Curiosity Rover on Mars". Science. 
  35. ^ a b Parker, T.; Clifford, S. M.; Banerdt, W. B. (2000). "Argyre Planitia and the Mars Global Hydrologic Cycle" (PDF). Lunar and Planetary Science. XXXI: 2033. Bibcode:2000LPI....31.2033P. 
  36. ^ a b Heisinger, H.; Head, J. (2002). "Topography and morphology of the Argyre basin, Mars: implications for its geologic and hydrologic history". Planet. Space Sci. 50 (10–11): 939–981. Bibcode:2002P&SS...50..939H. doi:10.1016/S0032-0633(02)00054-5. 
  37. ^ Soderblom, L.A. (1992). Kieffer, H.H.; et al., eds. "The Composition and Mineralogy of the Martian Surface from Spectroscopic Observations: 0.3–50 micrometres (1.2×10−5–0.001969 in). In Mars". Tucson, AZ: University of Arizona Press: 557–593. ISBN 0-8165-1257-4. 
  38. ^ Glotch, T.; Christensen, P. (2005). "Geologic and mineralogical mapping of Aram Chaos: Evidence for water-rich history". J. Geophys. Res. 110: E09006. Bibcode:2005JGRE..110.9006G. doi:10.1029/2004JE002389. 
  39. ^ a b c d e f g Holt, J. W.; Safaeinili, A.; Plaut, J. J.; Young, D. A.; Head, J. W.; Phillips, R. J.; Campbell, B. A.; Carter, L. M.; Gim, Y.; Seu, R.; Team, Sharad (2008). "Radar Sounding Evidence for Ice within Lobate Debris Aprons near Hellas Basin, Mid-Southern Latitudes of Mars" (PDF). Lunar and Planetary Science. XXXIX: 2441. Bibcode:2008LPI....39.2441H. 
  40. ^ a b c Amos, Jonathan (June 10, 2013). "Old Opportunity Mars rover makes rock discovery". NASA. BBC News. 
  41. ^ a b c "Mars Rover Opportunity Examines Clay Clues in Rock". Jet Propulsion Laboratory, NASA. May 17, 2013. 
  42. ^ a b c "Regional, Not Global, Processes Led to Huge Martian Floods". Planetary Science Institute. SpaceRef. 11 September 2015. Retrieved 2015-09-12. 
  43. ^ Harrison, K; Grimm, R. (2005). "Groundwater-controlled valley networks and the decline of surface runoff on early Mars". Journal of Geophysical Research. 110: E12S16. Bibcode:2005JGRE..11012S16H. doi:10.1029/2005JE002455. 
  44. ^ Howard, A.; Moore, Jeffrey M.; Irwin, Rossman P. (2005). "An intense terminal epoch of widespread fluvial activity on early Mars: 1. Valley network incision and associated deposits". Journal of Geophysical Research. 110: E12S14. Bibcode:2005JGRE..11012S14H. doi:10.1029/2005JE002459. 
  45. ^ Salese, F.; Di Achille, G.; Neesemann, A.; Ori, G. G.; Hauber, E. (2016). "Hydrological and sedimentary analyses of well-preserved paleofluvial-paleolacustrine systems at Moa Valles, Mars". J. Geophys. Res. Planets. 121: 194–232. doi:10.1002/2015JE004891. 
  46. ^ a b c d Irwin, Rossman P.; Howard, Alan D.; Craddock, Robert A.; Moore, Jeffrey M. (2005). "An intense terminal epoch of widespread fluvial activity on early Mars: 2. Increased runoff and paleolake development". Journal of Geophysical Research. 110: E12S15. Bibcode:2005JGRE..11012S15I. doi:10.1029/2005JE002460. 
  47. ^ a b Fassett, C.; Head, III (2008). "Valley network-fed, open-basin lakes on Mars: Distribution and implications for Noachian surface and subsurface hydrology". Icarus. 198: 37–56. Bibcode:2008Icar..198...37F. doi:10.1016/j.icarus.2008.06.016. 
  48. ^ a b Moore, J.; Wilhelms, D. (2001). "Hellas as a possible site of ancient ice-covered lakes on Mars" (PDF). Icarus. 154 (2): 258–276. Bibcode:2001Icar..154..258M. doi:10.1006/icar.2001.6736. 
  49. ^ a b Weitz, C.; Parker, T. (2000). "New evidence that the Valles Marineris interior deposits formed in standing bodies of water" (PDF). Lunar and Planetary Science. XXXI: 1693. Bibcode:2000LPI....31.1693W. 
  50. ^ "New Signs That Ancient Mars Was Wet". Space.com. October 28, 2008. 
  51. ^ Squyres, S.W.; et al. (1992). "Ice in the Martian Regolith". In Kieffer, H.H. Mars. Tucson, AZ: University of Arizona Press. pp. 523–554. ISBN 0-8165-1257-4. 
  52. ^ a b Head, J.; Marchant, D. (2006). Modifications of the walls of a Noachian crater in Northern Arabia Terra (24 E, 39 N) during northern mid-latitude Amazonian glacial epochs on Mars: Nature and evolution of Lobate Debris Aprons and their relationships to lineated valley fill and glacial systems (abstract). Lunar. Planet. Sci. 37. p. 1128. 
  53. ^ Head, J.; et al. (2006). "Modification if the dichotomy boundary on Mars by Amazonian mid-latitude regional glaciation". Geophys. Res. Lett.: 33. 
  54. ^ Head, J.; Marchant, D. (2006). "Evidence for global-scale northern mid-latitude glaciation in the Amazonian period of Mars: Debris-covered glacial and valley glacial deposits in the 30 – 50 N latitude band (abstract)". Lunar. Planet. Sci. 37: 1127. 
  55. ^ a b c Lewis, Richard (April 23, 2008). "Glaciers Reveal Martian Climate Has Been Recently Active". Brown University. 
  56. ^ a b c d e f g h Plaut, Jeffrey J.; Safaeinili, Ali; Holt, John W.; Phillips, Roger J.; Head, James W.; Seu, Roberto; Putzig, Nathaniel E.; Frigeri, Alessandro (2009). "Radar Evidence for Ice in Lobate Debris Aprons in the Mid-Northern Latitudes of Mars" (PDF). Geophysical Research Letters. 36 (2). Bibcode:2009GeoRL..3602203P. doi:10.1029/2008GL036379. 
  57. ^ Wall, Mike (March 25, 2011). "Q & A with Mars Life-Seeker Chris Carr". Space.com. 
  58. ^ Dartnell, L.R.; Desorgher; Ward; Coates (January 30, 2007). "Modelling the surface and subsurface Martian radiation environment: Implications for astrobiology". Geophysical Research Letters. 34 (2). Bibcode:2007GeoRL..34.2207D. doi:10.1029/2006GL027494. The damaging effect of ionising radiation on cellular structure is one of the prime limiting factors on the survival of life in potential astrobiological habitats. 
  59. ^ Dartnell, L. R.; Desorgher, L.; Ward, J. M.; Coates, A. J. (2007). "Martian sub-surface ionising radiation: biosignatures and geology". Biogeosciences. 4: 545–558. Bibcode:2007BGeo....4..545D. doi:10.5194/bg-4-545-2007. Retrieved June 1, 2013. This ionising radiation field is deleterious to the survival of dormant cells or spores and the persistence of molecular biomarkers in the subsurface, and so its characterisation. [..] Even at a depth of 2 meters beneath the surface, any microbes would likely be dormant, cryopreserved by the current freezing conditions, and so metabolically inactive and unable to repair cellular degradation as it occurs. 
  60. ^ de Morais, A. (2012). "A Possible Biochemical Model for Mars" (PDF). 43rd Lunar and Planetary Science Conference (2012). Retrieved June 5, 2013. The extensive volcanism at that time much possibly created subsurface cracks and caves within different strata, and the liquid water could have been stored in these subterraneous places, forming large aquifers with deposits of saline liquid water, minerals organic molecules, and geothermal heat – ingredients for life as we know on Earth. 
  61. ^ Didymus, JohnThomas (January 21, 2013). "Scientists find evidence Mars subsurface could hold life". Digital Journal – Science. There can be no life on the surface of Mars, because it is bathed in radiation and it's completely frozen. Life in the subsurface would be protected from that. - Prof. Parnell. 
  62. ^ Steigerwald, Bill (January 15, 2009). "Martian Methane Reveals the Red Planet is not a Dead Planet". NASA's Goddard Space Flight Center. NASA. If microscopic Martian life is producing the methane, it likely resides far below the surface, where it's still warm enough for liquid water to exist 
  63. ^ NASA Mars Exploration Program Overview. http://www.nasa.gov/mission_pages/mars/overview/index.html.
  64. ^ Sheehan, 1996, p. 35.
  65. ^ Kieffer, H.H.; Jakosky, B.M; Snyder, C. (1992). "The Planet Mars: From Antiquity to the Present". In Kieffer, H.H.; et al. Mars. Tucson, AZ: University of Arizona Press. pp. 1–33. 
  66. ^ hartmann, 2003, p. 20.
  67. ^ Sheehan, 1996, p. 150.
  68. ^ Spinrad, H.; Münch, G.; Kaplan, L. D. (1963). "Letter to the Editor: the Detection of Water Vapor on Mars". Astrophysical Journal. 137: 1319. Bibcode:1963ApJ...137.1319S. doi:10.1086/147613. 
  69. ^ Leighton, R.B.; Murray, B.C. (1966). "Behavior of Carbon Dioxide and Other Volatiles on Mars". Science. 153 (3732): 136–144. doi:10.1126/science.153.3732.136. PMID 17831495. 
  70. ^ Leighton, R.B.; Murray, B.C.; Sharp, R.P.; Allen, J.D.; Sloan, R.K. (1965). "Mariner IV Photography of Mars: Initial Results". Science. 149 (3684): 627–630. doi:10.1126/science.149.3684.627. PMID 17747569. 
  71. ^ Kliore, A.; et al. (1965). "Occultation Experiment: Results of the First Direct Measurement of Mars's Atmosphere and Ionosphere". Science. 149 (3689): 1243–1248. doi:10.1126/science.149.3689.1243. PMID 17747455. 
  72. ^ Grotzinger, John P. (January 24, 2014). "Introduction to Special Issue – Habitability, Taphonomy, and the Search for Organic Carbon on Mars". Science. 343 (6169): 386–387. Bibcode:2014Sci...343..386G. doi:10.1126/science.1249944. PMID 24458635. 
  73. ^ Various (January 24, 2014). "Special Issue – Table of Contents – Exploring Martian Habitability". Science. 343 (6169): 345–452. 
  74. ^ Various (January 24, 2014). "Special Collection – Curiosity – Exploring Martian Habitability". Science. 
  75. ^ Grotzinger, J.P.; et al. (January 24, 2014). "A Habitable Fluvio-Lacustrine Environment at Yellowknife Bay, Gale Crater, Mars". Science. 343 (6169): 1242777. doi:10.1126/science.1242777. PMID 24324272. 
  76. ^ a b Rodriguez, J. Alexis P.; Kargel, Jeffrey S.; Baker, Victor R.; Gulick, Virginia C.; et al. (8 September 2015). "Martian outflow channels: How did their source aquifers form, and why did they drain so rapidly?". Nature - Scientific Reports. 5: 13404. doi:10.1038/srep13404. Retrieved 2015-09-12. 
  77. ^ Staff (July 2, 2012). "Ancient Mars Water Existed Deep Underground". Space.com. 
  78. ^ Craddock, R.; Howard, A. (2002). "The case for rainfall on a warm, wet early Mars". J. Geophys. Res. 107: E11. Bibcode:2002JGRE..107.5111C. doi:10.1029/2001je001505. 
  79. ^ Head, J.; et al. (2006). "Extensive valley glacier deposits in the northern mid-latitudes of Mars: Evidence for the late Amazonian obliquity-driven climate change". Earth Planet. Sci. Lett. 241: 663–671. Bibcode:2006E&PSL.241..663H. doi:10.1016/j.epsl.2005.11.016. 
  80. ^ Madeleine, J.; et al. (2007). Mars: A proposed climatic scenario for northern mid-latitude glaciation. Lunar Planet. Sci. (Abstract). 38. p. 1778. 
  81. ^ Madeleine, J.; et al. (2009). "Amazonian northern mid-latitude glaciation on Mars: A proposed climate scenario". Icarus. 203: 300–405. Bibcode:2009Icar..203..390M. doi:10.1016/j.icarus.2009.04.037. 
  82. ^ Mischna, M.; et al. (2003). "On the orbital forcing of Martian water and CO2 cycles: A general circulation model study with simplified volatile schemes.". J. Geophys. Res. 108 (E6): 5062. Bibcode:2003JGRE..108.5062M. doi:10.1029/2003je002051. 
  83. ^ Staff (October 28, 2008). "NASA Mars Reconnaissance Orbiter Reveals Details of a Wetter Mars". SpaceRef. NASA. 
  84. ^ a b Lunine, Jonathan I.; Chambers, John; et al. (September 2003). "The Origin of Water on Mars". Icarus. 165 (1): 1–8. Bibcode:2003Icar..165....1L. doi:10.1016/S0019-1035(03)00172-6. Retrieved June 10, 2013. 
  85. ^ Soderblom, L.A.; Bell, J.F. (2008). "Exploration of the Martian Surface: 1992–2007". In Bell, J.F. The Martian Surface: Composition, Mineralogy, and Physical Properties. Cambridge University Press. pp. 3–19. 
  86. ^ Ming, D.W.; Morris, R.V.; Clark, R.C. (2008). "Aqueous Alteration on Mars". In Bell, J.F. The Martian Surface: Composition, Mineralogy, and Physical Properties. Cambridge University Press. pp. 519–540. 
  87. ^ Lewis, J.S. (1997). Physics and Chemistry of the Solar System (revised ed.). San Diego, CA: Academic Press. ISBN 0-12-446742-3. 
  88. ^ Lasue, J.; et al. (2013). "Quantitative Assessments of the Martian Hydrosphere". Space Sci. Rev. 174: 155–212. doi:10.1007/s11214-012-9946-5. 
  89. ^ Clark, B.C.; et al. (2005). "Chemistry and Mineralogy of Outcrops at Meridiani Planum". Earth Planet. Sci. Lett. 240: 73–94. Bibcode:2005E&PSL.240...73C. doi:10.1016/j.epsl.2005.09.040. 
  90. ^ Bloom, A.L. (1978). Geomorphology: A Systematic Analysis of Late Cenozoic Landforms. Englewood Cliffs, N.J: Prentice-Hall. p. 114. 
  91. ^ Boynton, W.V.; et al. (2009). "Evidence for Calcium Carbonate at the Mars Phoenix Landing Site". Science. 325 (5936): 61–4. doi:10.1126/science.1172768. PMID 19574384. 
  92. ^ Gooding, J.L.; Arvidson, R.E.; Zolotov, M. YU. (1992). "Physical and Chemical Weathering". In Kieffer, H.H.; et al. Mars. Tucson, AZ: University of Arizona Press. pp. 626–651. ISBN 0-8165-1257-4. 
  93. ^ Melosh, H.J. (2011). Planetary Surface Processes. Cambridge University Press. p. 296. ISBN 978-0-521-51418-7. 
  94. ^ Abramov, O.; Kring, D.A. (2005). "Impact-Induced Hydrothermal Activity on Early Mars". J. Geophys. Res. 110: E12S09. Bibcode:2005JGRE..11012S09A. doi:10.1029/2005JE002453. 
  95. ^ Schrenk, M.O.; Brazelton, W.J.; Lang, S.Q. (2013). "Serpentinization, Carbon, and Deep Life". Reviews in Mineralogy & Geochemistry. 75: 575–606. doi:10.2138/rmg.2013.75.18. 
  96. ^ Baucom, Martin (March–April 2006). "Life on Mars?". American Scientist. 
  97. ^ Chassefière, E; Langlais, B; Quesnel, Y; Leblanc, F. (2013), "The Fate of Early Mars' Lost Water: The Role of Serpentinization." (PDF), EPSC Abstracts, 8, p. EPSC2013-188 
  98. ^ Ehlmann, B. L.; Mustard, J.F.; Murchie, S.L. (2010). "Geologic Setting of Serpentine Deposits on Mars". Geophys. Res. Lett. 37: L06201. Bibcode:2010GeoRL..37.6201E. doi:10.1029/2010GL042596. 
  99. ^ Bloom, A.L. (1978). Geomorphology: A Systematic Analysis of Late Cenozoic Landforms. Englewood Cliffs, N.J.: Prentice-Hall. ., p. 120
  100. ^ Ody, A.; et al. (2013). "Global Investigation of Olivine on Mars: Insights into Crust and Mantle Compositions". J. Geophys. Res. 118: 234–262. Bibcode:2013JGRE..118..234O. doi:10.1029/2012JE004149. 
  101. ^ Swindle, T. D.; Treiman, A. H.; Lindstrom, D. J.; Burkland, M. K.; Cohen, B. A.; Grier, J. A.; Li, B.; Olson, E. K. (2000). "Noble Gases in Iddingsite from the Lafayette meteorite: Evidence for Liquid water on Mars in the last few hundred million years". Meteoritics and Planetary Science. 35 (1): 107–115. Bibcode:2000M&PS...35..107S. doi:10.1111/j.1945-5100.2000.tb01978.x. 
  102. ^ Gulick, V.; Baker, V. (1989). "Fluvial valleys and martian palaeoclimates". Nature. 341 (6242): 514–516. Bibcode:1989Natur.341..514G. doi:10.1038/341514a0. 
  103. ^ Head, J.; Kreslavsky, M. A.; Ivanov, M. A.; Hiesinger, H.; Fuller, E. R.; Pratt, S. (2001). "Water in Middle Mars History: New Insights From MOLA Data". American Geophysical Union. Bibcode:2001AGUSM...P31A02H. 
  104. ^ Head, J.; et al. (2001). "Exploration for standing Bodies of Water on Mars: When Were They There, Where did They go, and What are the Implications for Astrobiology?". American Geophysical Union. 21: 03. Bibcode:2001AGUFM.P21C..03H. 
  105. ^ David, Leonard (January 20, 2005). "Mars Rover's Meteorite Discovery Triggers Questions". Space.com. Retrieved February 10, 2013. 
  106. ^ Meyer, C. (2012) The Martian Meteorite Compendium; National Aronautics and Space Administration. http://curator.jsc.nasa.gov/antmet/mmc/.
  107. ^ "Shergotty Meteorite – JPL, NASA". NASA. Retrieved December 19, 2010. 
  108. ^ Hamiliton, W.; Christensen, Philip R.; McSween, Harry Y. (1997). "Determination of Martian meteorite lithologies and mineralogies using vibrational spectroscopy". Journal of Geophysical Research. 102: 25593–25603. Bibcode:1997JGR...10225593H. doi:10.1029/97JE01874. 
  109. ^ Treiman, A. (2005). "The nakhlite meteorites: Augite-rich igneous rocks from Mars" (PDF). Chemie der Erde – Geochemistry. 65 (3): 203–270. Bibcode:2005ChEG...65..203T. doi:10.1016/j.chemer.2005.01.004. Retrieved September 8, 2006. 
  110. ^ McKay, D.; Gibson Jr., EK; Thomas-Keprta, KL; Vali, H; Romanek, CS; Clemett, SJ; Chillier, XD; Maechling, CR; Zare, RN (1996). "Search for Past Life on Mars: Possible Relic Biogenic Activity in Martian Meteorite AL84001". Science. 273 (5277): 924–930. Bibcode:1996Sci...273..924M. doi:10.1126/science.273.5277.924. PMID 8688069. 
  111. ^ Gibbs, W.; Powell, C. (August 19, 1996). "Bugs in the Data?". Scientific American. 
  112. ^ "Controversy Continues: Mars Meteorite Clings to Life – Or Does It?". SPACE.com. March 20, 2002. 
  113. ^ Bada, J.; Glavin, DP; McDonald, GD; Becker, L (1998). "A Search for Endogenous Amino Acids in Martian Meteorite AL84001". Science. 279 (5349): 362–365. Bibcode:1998Sci...279..362B. doi:10.1126/science.279.5349.362. PMID 9430583. 
  114. ^ a b Raeburn, P. (1998). "Uncovering the Secrets of the Red Planet Mars". National Geographic. Washington D.C. 
  115. ^ a b Moore, P.; et al. (1990). The Atlas of the Solar System. New York: Mitchell Beazley Publishers. 
  116. ^ Kieffer, Hugh H., ed. (1994). Mars (2nd ed.). Tucson: University of Arizona Press. ISBN 0-8165-1257-4. 
  117. ^ Berman, Daniel C.; Crown, David A.; Bleamaster, Leslie F. (2009). "Degradation of mid-latitude craters on Mars". Icarus. 200: 77–95. Bibcode:2009Icar..200...77B. doi:10.1016/j.icarus.2008.10.026. 
  118. ^ Fassett, Caleb I.; Head, James W. (2008). "The timing of martian valley network activity: Constraints from buffered crater counting". Icarus. 195: 61–89. Bibcode:2008Icar..195...61F. doi:10.1016/j.icarus.2007.12.009. 
  119. ^ Malin, Michael C. (2010). "An overview of the 1985–2006 Mars Orbiter Camera science investigation". The Mars Journal. 5: 1–60. Bibcode:2010IJMSE...5....1M. doi:10.1555/mars.2010.0001. 
  120. ^ "Sinuous Ridges Near Aeolis Mensae". Hiroc.lpl.arizona.edu. January 31, 2007. 
  121. ^ Zimbelman, J.; Griffin, L. (2010). "HiRISE images of yardangs and sinuous ridges in the lower member of the Medusae Fossae Formation, Mars". Icarus. 205: 198–210. Bibcode:2010Icar..205..198Z. doi:10.1016/j.icarus.2009.04.003. 
  122. ^ Newsom, H.; Lanza, Nina L.; Ollila, Ann M.; Wiseman, Sandra M.; Roush, Ted L.; Marzo, Giuseppe A.; Tornabene, Livio L.; Okubo, Chris H.; Osterloo, Mikki M.; Hamilton, Victoria E.; Crumpler, Larry S. (2010). "Inverted channel deposits on the floor of Miyamoto crater, Mars". Icarus. 205: 64–72. Bibcode:2010Icar..205...64N. doi:10.1016/j.icarus.2009.03.030. 
  123. ^ Morgan, A.M.; Howard, A.D.; Hobley, D.E.J.; Moore, J.M.; Dietrich, W.E.; Williams, R.M.E.; Burr, D.M.; Grant, J.A.; Wilson, S.A.; Matsubara, Y. (2014). "Sedimentology and climatic environment of alluvial fans in the martian Saheki crater and a comparison with terrestrial fans in the Atacama Desert". Icarus. 229: 131–156. Bibcode:2014Icar..229..131M. doi:10.1016/j.icarus.2013.11.007. 
  124. ^ a b Weitz, C.; Milliken, R.E.; Grant, J.A.; McEwen, A.S.; Williams, R.M.E.; Bishop, J.L.; Thomson, B.J. (2010). "Mars Reconnaissance Orbiter observations of light-toned layered deposits and associated fluvial landforms on the plateaus adjacent to Valles Marineris". Icarus. 205: 73–102. Bibcode:2010Icar..205...73W. doi:10.1016/j.icarus.2009.04.017. 
  125. ^ a b c Zendejas, J.; Segura, A.; Raga, A.C. (December 2010). "Atmospheric mass loss by stellar wind from planets around main sequence M stars". Icarus. 210 (2): 539–1000. Bibcode:2010Icar..210..539Z. doi:10.1016/j.icarus.2010.07.013. Retrieved December 19, 2010. 
  126. ^ a b c Cabrol, N.; Grin, E., eds. (2010). Lakes on Mars. New York: Elsevier. 
  127. ^ Goldspiel, J.; Squires, S. (2000). "Groundwater sapping and valley formation on Mars". Icarus. 148: 176–192. Bibcode:2000Icar..148..176G. doi:10.1006/icar.2000.6465. 
  128. ^ a b c d e f g h i j k l Carr, Michael H. The Surface of Mars. Cambridge Planetary Science Series (No. 6). ISBN 978-0-511-26688-1. 
  129. ^ McCauley, J. 1978. Geologic map of the Coprates quadrangle of Mars. U.S. Geol. Misc. Inv. Map I-897
  130. ^ Nedell, S.; Squyres, Steven W.; Andersen, David W. (1987). "Origin and evolution of the layered deposits in the Valles Marineris, Mars". Icarus. 70 (3): 409–441. Bibcode:1987Icar...70..409N. doi:10.1016/0019-1035(87)90086-8. 
  131. ^ Matsubara, Yo, Alan D. Howard, and Sarah A. Drummond. "Hydrology of early Mars: Lake basins." Journal of Geophysical Research: Planets 116.E4 (2011).
  132. ^ "Spectacular Mars images reveal evidence of ancient lakes". Sciencedaily.com. January 4, 2010. 
  133. ^ Gupta, Sanjeev; Warner, Nicholas; Kim, Rack; Lin, Yuan; Muller, Jan; -1#Jung-, Shih- (2010). "Hesperian equatorial thermokarst lakes in Ares Vallis as evidence for transient warm conditions on Mars". Geology. 38: 71–74. doi:10.1130/G30579.1. 
  134. ^ a b c d Brown, Dwayne; Cole, Steve; Webster, Guy; Agle, D.C. (September 27, 2012). "NASA Rover Finds Old Streambed On Martian Surface". NASA. 
  135. ^ a b c NASA (September 27, 2012). "NASA's Curiosity Rover Finds Old Streambed on Mars – video (51:40)". NASAtelevision. 
  136. ^ a b c Chang, Alicia (September 27, 2012). "Mars rover Curiosity finds signs of ancient stream". Associated Press. 
  137. ^ "NASA Rover Finds Conditions Once Suited for Ancient Life on Mars". NASA. March 12, 2013. 
  138. ^ Di Achille, Gaetano; Hynek, Brian M. (2010). "Ancient ocean on Mars supported by global distribution of deltas and valleys". Nature Geoscience. 3 (7): 459–463. Bibcode:2010NatGe...3..459D. doi:10.1038/ngeo891. 
  139. ^ Carr, M.H. (1979). "Formation of Martian flood features by release of water from confined aquifers" (PDF). J. Geophys. Res. 84: 2995–3007. Bibcode:1979JGR....84.2995C. doi:10.1029/JB084iB06p02995. 
  140. ^ Baker, V.; Milton, D. (1974). "Erosion by Catastrophic Floods on Mars and Earth". Icarus. 23: 27–41. Bibcode:1974Icar...23...27B. doi:10.1016/0019-1035(74)90101-8. 
  141. ^ "Mars Global Surveyor MOC2-862 Release". Msss.com. Retrieved January 16, 2012. 
  142. ^ Andrews-Hanna, Jeffrey C.; Phillips, Roger J.; Zuber, Maria T. (2007). "Meridiani Planum and the global hydrology of Mars". Nature. 446 (7132): 163–6. Bibcode:2007Natur.446..163A. doi:10.1038/nature05594. PMID 17344848. 
  143. ^ Irwin; Rossman, P.; Craddock, Robert A.; Howard, Alan D. (2005). "Interior channels in Martian valley networks: Discharge and runoff production". Geology. 33 (6): 489–492. doi:10.1130/g21333.1. 
  144. ^ Jakosky, Bruce M. (1999). "Water, Climate, and Life". Science. 283 (5402): 648–649. doi:10.1126/science.283.5402.648. PMID 9988657. 
  145. ^ Lamb, Michael P., et al. "Can springs cut canyons into rock?." Journal of Geophysical Research: Planets (1991–2012) 111.E7 (2006).
  146. ^ a b c Grotzinger, J.P.; Arvidson, R.E.; Bell III, J.F.; Calvin, W.; Clark, B.C.; Fike, D.A.; Golombek, M.; Greeley, R.; Haldemann, A.; Herkenhoff, K.E.; Jolliff, B.L.; Knoll, A.H.; Malin, M.; McLennan, S.M.; Parker, T.; Soderblom, L.; Sohl-Dickstein, J.N.; Squyres, S.W.; Tosca, N.J.; Watters, W.A. (November 25, 2005). "Stratigraphy and sedimentology of a dry to wet eolian depositional system, Burns formation, Meridiani Planum". Earth and Planetary Science Letters. 240 (1): 11–72. Bibcode:2005E&PSL.240...11G. doi:10.1016/j.epsl.2005.09.039. ISSN 0012-821X. 
  147. ^ Michalski, Joseph R.; Niles, Paul B.; Cuadros, Javier; Parnell, John; Rogers, A. Deanne; Wright, Shawn P. (January 20, 2013). "Groundwater activity on Mars and implications for a deep biosphere". Nature Geoscience. 6 (2): 133–138. Bibcode:2013NatGe...6..133M. doi:10.1038/ngeo1706. Retrieved June 17, 2013. Here we present a conceptual model of subsurface habitability of Mars and evaluate evidence for groundwater upwelling in deep basins. 
  148. ^ a b c Zuber, Maria T. (2007). "Planetary Science: Mars at the tipping point". Nature. 447 (7146): 785–786. Bibcode:2007Natur.447..785Z. doi:10.1038/447785a. PMID 17568733. 
  149. ^ Andrews‐Hanna, J. C.; Zuber, M. T.; Arvidson, R. E.; Wiseman, S. M. (2010). "Early Mars hydrology: Meridiani playa deposits and the sedimentary record of Arabia Terra". J. Geophys. Res. 115: E06002. Bibcode:2010JGRE..115.6002A. doi:10.1029/2009JE003485. 
  150. ^ McLennan, S. M.; et al. (2005). "Provenance and diagenesis of the evaporitebearing Burns formation, Meridiani Planum, Mars". Earth Planet. Sci. Lett. 240: 95–121. Bibcode:2005E&PSL.240...95M. doi:10.1016/j.epsl.2005.09.041. 
  151. ^ Squyres, S. W.; Knoll, A. H. (2005). "Sedimentary rocks at Meridiani Planum: Origin, diagenesis, and implications for life on Mars". Earth Planet. Sci. Lett. 240: 1–10. Bibcode:2005E&PSL.240....1S. doi:10.1016/j.epsl.2005.09.038. .
  152. ^ Squyres, S. W.; et al. (2006). "Two years at Meridiani Planum: Results from the Opportunity rover". Science. 313: 1403–1407. doi:10.1126/science. .
  153. ^ Wiseman, M.; Andrews-Hanna, J. C.; Arvidson, R. E.; Mustard, J. F.; Zabrusky, K. J. (2011). Distribution of Hydrated Sulfates Across Arabia Terra Using CRISM Data: Implications for Martian Hydrology. 42nd Lunar and Planetary Science Conference. 
  154. ^ Andrews‐Hanna, Jeffrey C.; Lewis, Kevin W. (2011). "Early Mars hydrology: 2. Hydrological evolution in the Noachian and Hesperian epochs". Journal of Geophysical Research: Planets. 116: E2. Bibcode:2011JGRE..116.2007A. doi:10.1029/2010je003709. 
  155. ^ Clifford, S. M.; Parker, T. J. (2001). "The Evolution of the Martian Hydrosphere: Implications for the Fate of a Primordial Ocean and the Current State of the Northern Plains". Icarus. 154: 40–79. Bibcode:2001Icar..154...40C. doi:10.1006/icar.2001.6671. 
  156. ^ Smith, D.; et al. (1999). "The Gravity Field of Mars: Results from Mars Global Surveyor" (PDF). Science. 286 (5437): 94–97. Bibcode:1999Sci...286...94S. doi:10.1126/science.286.5437.94. PMID 10506567. 
  157. ^ Read, Peter L.; Lewis, S. R. (2004). The Martian Climate Revisited: Atmosphere and Environment of a Desert Planet (Paperback). Chichester, UK: Praxis. ISBN 978-3-540-40743-0. Retrieved December 19, 2010. 
  158. ^ "Martian North Once Covered by Ocean". Astrobio.net. Retrieved December 19, 2010. 
  159. ^ "New Map Bolsters Case for Ancient Ocean on Mars". SPACE.com. November 23, 2009. 
  160. ^ Carr, M.; Head, J. (2003). "Oceans on Mars: An assessment of the observational evidence and possible fate". Journal of Geophysical Research. 108: 5042. Bibcode:2003JGRE..108.5042C. doi:10.1029/2002JE001963. 
  161. ^ "Mars Ocean Hypothesis Hits the Shore". NASA Astrobiology. NASA. January 26, 2001. 
  162. ^ Perron; Taylor, J.; et al. (2007). "Evidence for an ancient Martian ocean in the topography of deformed shorelines". Nature. 447 (7146): 840–843. doi:10.1038/nature05873. 
  163. ^ Kaufman, Marc (March 5, 2015). "Mars Had an Ocean, Scientists Say, Pointing to New Data". The New York Times. Retrieved March 5, 2015. 
  164. ^ http://astrobiology.com/2016/05/ancient-tsunami-evidence-on-mars-reveals-life-potential.html
  165. ^ Rodriguez, J., et al. 2016. Tsunami waves extensively resurfaced the shorelines of an early Martian ocean. Scientific Reports: 6, 25106.
  166. ^ http://www.nature.com/articles/srep25106
  167. ^ Cornell University. "Ancient tsunami evidence on Mars reveals life potential." ScienceDaily. ScienceDaily, 19 May 2016. <www.sciencedaily.com/releases/2016/05/160519101756.htm>.
  168. ^ Boynton, W. V.; et al. (2007). "Concentration of H, Si, Cl, K, Fe, and Th in the low and mid latitude regions of Mars". Journal of Geophysical Research: Planets. 112 (E12). Bibcode:2007JGRE..11212S99B. doi:10.1029/2007JE002887. 
  169. ^ Feldman, W. C.; Prettyman, T. H.; Maurice, S.; Plaut, J. J.; Bish, D. L.; Vaniman, D. T.; Tokar, R. L. (2004). "Global distribution of near-surface hydrogen on Mars". Journal of Geophysical Research. 109: E9. Bibcode:2004JGRE..109.9006F. doi:10.1029/2003JE002160. E09006. 
  170. ^ a b c Feldman, W. C.; et al. (2004). "Global distribution of near-surface hydrogen on Mars". Journal of Geophysical Research. 109 (E9). Bibcode:2004JGRE..109.9006F. doi:10.1029/2003JE002160. 
  171. ^ "Water ice in crater at Martian north pole" (Press release). ESA. July 27, 2005. 
  172. ^ "Ice lake found on the Red Planet". BBC. July 29, 2005. 
  173. ^ Murray, John B.; et al. (2005). "Evidence from the Mars Express High Resolution Stereo Camera for a frozen sea close to Mars' equator". Nature. 434 (7031): 352–356. Bibcode:2005Natur.434..352M. doi:10.1038/nature03379. PMID 15772653. Here we present High Resolution Stereo Camera images from the European Space Agency Mars Express spacecraft that indicate that such lakes may still exist. 
  174. ^ Orosei, R.; Cartacci, M.; Cicchetti, A.; Federico, C.; Flamini, E.; Frigeri, A.; Holt, J. W.; Marinangeli, L.; Noschese, R.; Pettinelli, E.; Phillips, R. J.; Picardi, G.; Plaut, J. J.; Safaeinili, A.; Seu, R. (2008). "Radar subsurface sounding over the putative frozen sea in Cerberus Palus, Mars" (PDF). Lunar and Planetary Science. XXXIX: 1. Bibcode:2007AGUFM.P14B..05O. doi:10.1109/ICGPR.2010.5550143. ISBN 978-1-4244-4604-9. 
  175. ^ Barlow, Nadine G. Mars: an introduction to its interior, surface and atmosphere. Cambridge University Press. ISBN 978-0-521-85226-5. 
  176. ^ a b "Mars' South Pole Ice Deep and Wide". NASA News & Media Resources. NASA. March 15, 2007. 
  177. ^ a b c Kostama, V.-P.; Kreslavsky, M. A.; Head, J. W. (June 3, 2006). "Recent high-latitude icy mantle in the northern plains of Mars: Characteristics and ages of emplacement". Geophysical Research Letters. 33 (11): L11201. Bibcode:2006GeoRL..3311201K. doi:10.1029/2006GL025946. 
  178. ^ Plaut, J. J.; et al. (March 15, 2007). "Subsurface Radar Sounding of the South Polar Layered Deposits of Mars". Science. 316 (5821): 92–95. doi:10.1126/science.1139672. PMID 17363628. 
  179. ^ a b Johnson, John (August 1, 2008). "There's water on Mars, NASA confirms". Los Angeles Times. 
  180. ^ "Radar Map of Buried Mars Layers Matches Climate Cycles". OnOrbit. Retrieved December 19, 2010. 
  181. ^ Fishbaugh, KE; Byrne, Shane; Herkenhoff, Kenneth E.; Kirk, Randolph L.; Fortezzo, Corey; Russell, Patrick S.; McEwen, Alfred (2010). "Evaluating the meaning of "layer" in the Martian north polar layered depsoits and the impact on the climate connection" (PDF). Icarus. 205 (1): 269–282. Bibcode:2010Icar..205..269F. doi:10.1016/j.icarus.2009.04.011. 
  182. ^ Duxbury, N. S.; Zotikov, I. A.; Nealson, K. H.; Romanovsky, V. E.; Carsey, F. D. (2001). "A numerical model for an alternative origin of Lake Vostok and its exobiological implications for Mars" (PDF). Journal of Geophysical Research. 106: 1453. Bibcode:2001JGR...106.1453D. doi:10.1029/2000JE001254. 
  183. ^ a b c Kieffer, Hugh H. (1992). Mars. University of Arizona Press. ISBN 978-0-8165-1257-7. Retrieved March 7, 2011. 
  184. ^ "Polygonal Patterned Ground: Surface Similarities Between Mars and Earth". SpaceRef. September 28, 2002. 
  185. ^ Squyres, S. (1989). "Urey Prize Lecture: Water on Mars". Icarus. 79 (2): 229–288. Bibcode:1989Icar...79..229S. doi:10.1016/0019-1035(89)90078-X. 
  186. ^ Lefort, A.; Russell, P.S.; Thomas, N. (2010). "Scaloped terrains in the Peneus and Amphitrites Paterae region of Mars as observed by HiRISE". Icarus. 205: 259–268. Bibcode:2010Icar..205..259L. doi:10.1016/j.icarus.2009.06.005. 
  187. ^ "NASA – Turbulent Lava Flow in Mars' Athabasca Valles". Nasa.gov. January 11, 2010. 
  188. ^ Dundas, C., S. Bryrne, A. McEwen. 2015. Modeling the development of martian sublimation thermokarst landforms. Icarus: 262, 154-169.
  189. ^ a b c Head, James W.; Mustard, John F.; Kreslavsky, Mikhail A.; Milliken, Ralph E.; Marchant, David R. (2003). "Recent ice ages on Mars". Nature. 426 (6968): 797–802. Bibcode:2003Natur.426..797H. doi:10.1038/nature02114. PMID 14685228. 
  190. ^ a b "HiRISE Dissected Mantled Terrain (PSP_002917_2175)". Arizona University. Retrieved December 19, 2010. 
  191. ^ Lefort, A.; Russell, P.S.; Thomas, N. (2010). "Scalloped terrains in the Peneus and Amphitrites Paterae region of Mars as observed by HiRISE". Icarus. 205: 259–268. Bibcode:2010Icar..205..259L. doi:10.1016/j.icarus.2009.06.005. 
  192. ^ http://www.space.com/34811-mars-ice-more-water-than-lake-superior.html?utm_source=sp-newsletter&utm_medium=email&utm_campaign=20161123-sdc
  193. ^ Bramson, A, et al. 2015. Widespread excess ice in Arcadia Planitia, Mars. Geophysical Research Letters: 42, 6566-6574
  194. ^ https://planetarycassie.com/2016/11/04/widespread-thick-water-ice-found-in-utopia-planitia-mars/
  195. ^ Stuurman, C., et al. 2016. SHARAD detection and characterization of subsurface water ice deposits in Utopia Planitia, Mars. Geophysical Research Letters: 43, 9484_9491.
  196. ^ Byrne, S.; Ingersoll, A. P. (2002). "A Sublimation Model for the Formation of the Martian Polar Swiss-cheese Features". American Astronomical Society. American Astronomical Society. 34: 837. Bibcode:2002DPS....34.0301B. 
  197. ^ Strom, R.G.; Croft, Steven K.; Barlow, Nadine G. (1992). The Martian Impact Cratering Record, Mars. University of Arizona Press. ISBN 0-8165-1257-4. 
  198. ^ "ESA – Mars Express – Breathtaking views of Deuteronilus Mensae on Mars". Esa.int. March 14, 2005. 
  199. ^ Hauber, E.; et al. (2005). "Discovery of a flank caldera and very young glacial activity at Hecates Tholus, Mars". Nature. 434 (7031): 356–61. Bibcode:2005Natur.434..356H. doi:10.1038/nature03423. PMID 15772654. 
  200. ^ Shean, David E.; Head, James W.; Fastook, James L.; Marchant, David R. (2007). "Recent glaciation at high elevations on Arsia Mons, Mars: Implications for the formation and evolution of large tropical mountain glaciers" (PDF). Journal of Geophysical Research. 112 (E3): E03004. Bibcode:2007JGRE..11203004S. doi:10.1029/2006JE002761. 
  201. ^ Shean, D.; et al. (2005). "Origin and evolution of a cold-based mountain glacier on Mars: The Pavonis Mons fan-shaped deposit". Journal of Geophysical Research. 110 (E5): E05001. Bibcode:2005JGRE..11005001S. doi:10.1029/2004JE002360. 
  202. ^ Basilevsky, A.; et al. (2006). "Geological recent tectonic, volcanic and fluvial activity on the eastern flank of the Olympus Mons volcano, Mars". Geophysical Research Letters. 33. L13201. Bibcode:2006GeoRL..3313201B. doi:10.1029/2006GL026396. 
  203. ^ Milliken, R.; et al. (2003). "Viscous flow features on the surface of Mars: Observations from high-resolution Mars Orbiter Camera (MOC) images". Journal of Geophysical Research. 108 (E6): 5057. Bibcode:2003JGRE..108.5057M. doi:10.1029/2002je002005. 
  204. ^ Arfstrom, J.; Hartmann, W. (2005). "Martian flow features, moraine-like ridges, and gullies: Terrestrial analogs and interrelationships". Icarus. 174 (2): 321–35. Bibcode:2005Icar..174..321A. doi:10.1016/j.icarus.2004.05.026. 
  205. ^ a b Head, J. W.; Neukum, G.; Jaumann, R.; Hiesinger, H.; Hauber, E.; Carr, M.; Masson, P.; Foing, B.; Hoffmann, H.; Kreslavsky, M.; Werner, S.; Milkovich, S.; van Gasselt, S.; HRSC Co-Investigator Team (2005). "Tropical to mid-latitude snow and ice accumulation, flow and glaciation on Mars". Nature. 434 (7031): 346–350. Bibcode:2005Natur.434..346H. doi:10.1038/nature03359. PMID 15772652. 
  206. ^ a b Staff (October 17, 2005). "Mars' climate in flux: Mid-latitude glaciers". Marstoday. Brown University. 
  207. ^ Berman, D.; et al. (2005). "The role of arcuate ridges and gullies in the degradation of craters in the Newton Basin region of Mars". Icarus. 178 (2): 465–86. Bibcode:2005Icar..178..465B. doi:10.1016/j.icarus.2005.05.011. 
  208. ^ "Fretted Terrain Valley Traverse". Hirise.lpl.arizona.edu. Retrieved January 16, 2012. 
  209. ^ "Jumbled Flow Patterns". Arizona University. Retrieved January 16, 2012. 
  210. ^ a b c d e f g h i Jakosky, B. M.; Phillips, R. J. (2001). "Mars' volatile and climate history". Nature. 412: 237–244. doi:10.1038/35084184. PMID 11449285. 
  211. ^ a b c d e Chaufray, J. Y.; et al. (2007). "Mars solar wind interaction: Formation of the Martian corona and atmospheric loss to space". Journal of Geophysical Research. 112. Bibcode:2007JGRE..112.9009C. doi:10.1029/2007JE002915. 
  212. ^ a b c Chevrier, V.; et al. (2007). "Early geochemical environment of Mars as determined from thermodynamics of phyllosilicates". Nature. 448: 60–63. doi:10.1038/nature05961. 
  213. ^ a b c Catling, D. C. (2007). "Mars: Ancient fingerprints in the clay". Nature. 448: 31–32. doi:10.1038/448031a. PMID 17611529. 
  214. ^ Andrews-Hanna, J. C.; et al. (2007). "Meridiani Planum and the global hydrology of Mars". Nature. 446: 163–6. doi:10.1038/nature05594. PMID 17344848. 
  215. ^ Morris, R. V.; et al. (2001). "Phyllosilicate-poor palagonitic dust from Mauna Kea Volcano (Hawaii): A mineralogical analogue for magnetic Martian dust?". Journal of Geophysical Research. 106: 5057. Bibcode:2001JGR...106.5057M. doi:10.1029/2000JE001328. 
  216. ^ Chevrier, V.; et al. (2006). "Iron weathering products in a CO2+(H2O or H2O2) atmosphere: Implications for weathering processes on the surface of Mars". Geochimica et Cosmochimica Acta. 70: 4295–4317. Bibcode:2006GeCoA..70.4295C. doi:10.1016/j.gca.2006.06.1368. 
  217. ^ Bibring, J-P.; et al. (2006). "Global mineralogical and aqueous mars history derived from OMEGA/Mars Express data". Science. 312: 400–4. doi:10.1126/science.1122659. PMID 16627738. 
  218. ^ McEwen, A. S.; et al. (2007). "A Closer Look at Water-Related Geologic Activity on Mars". Science. 317: 1706–1709. doi:10.1126/science.1143987. PMID 17885125. 
  219. ^ Smith, Isaac B.; Putzig, Nathaniel E.; Holt, John W.; Phillips, Roger J. (27 May 2016). "An ice age recorded in the polar deposits of Mars". Science. 352 (6289): 1075–1078. doi:10.1126/science.aad6968. Retrieved 2016-05-27. 
  220. ^ a b c "Mars may be emerging from an ice age". ScienceDaily. MLA NASA/Jet Propulsion Laboratory. December 18, 2003. 
  221. ^ Mustard, J.; et al. (2001). "Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice". Nature. 412 (6845): 411–4. doi:10.1038/35086515. PMID 11473309. 
  222. ^ Kreslavsky, M.; Head, J. (2002). "Mars: Nature and evolution of young latitude-dependent water-ice-rich mantle" (PDF). Geophysical Research Letters. 29 (15): 14–1–14–4. Bibcode:2002GeoRL..29o..14K. doi:10.1029/2002GL015392. 
  223. ^ Shean, David E. (2005). "Origin and evolution of a cold-based tropical mountain glacier on Mars: The Pavonis Mons fan-shaped deposit". Journal of Geophysical Research. 110. Bibcode:2005JGRE..11005001S. doi:10.1029/2004JE002360. 
  224. ^ Forget, F.; et al. (2006). "Formation of Glaciers on Mars by Atmospheric Precipitation at High Obliquity". Science. 311 (5759): 368–71. Bibcode:2006Sci...311..368F. doi:10.1126/science.1120335. PMID 16424337. 
  225. ^ Dickson, James L.; Head, James W.; Marchant, David R. (2008). "Late Amazonian glaciation at the dichotomy boundary on Mars: Evidence for glacial thickness maxima and multiple glacial phases". Geology. 36 (5): 411–4. doi:10.1130/G24382A.1. 
  226. ^ a b Heldmann, Jennifer L.; et al. (May 7, 2005). "Formation of Martian gullies by the action of liquid water flowing under current Martian environmental conditions" (PDF). Journal of Geophysical Research. 110: Eo5004. Bibcode:2005JGRE..11005004H. doi:10.1029/2004JE002261.  'conditions such as now occur on Mars, outside of the temperature-pressure stability regime of liquid water' … 'Liquid water is typically stable at the lowest elevations and at low latitudes on the planet, because the atmospheric pressure is greater than the vapor pressure of water and surface temperatures in equatorial regions can reach 220 K (−53 °C; −64 °F) for parts of the day.
  227. ^ "Mars Gullies May Have Been Formed By Flowing Liquid Brine". Sciencedaily.com. February 15, 2009. 
  228. ^ a b Malin, Michael C.; Edgett, Kenneth S.; Posiolova, Liliya V.; McColley, Shawn M.; Dobrea, Eldar Z. Noe (December 8, 2006). "Present-Day Impact Cratering Rate and Contemporary Gully Activity on Mars". Science. 314 (5805): 1573–1577. Bibcode:2006Sci...314.1573M. doi:10.1126/science.1135156. PMID 17158321. Retrieved September 3, 2009. 
  229. ^ a b Head, JW; Marchant, DR; Kreslavsky, MA (2008). "Formation of gullies on Mars: Link to recent climate history and insolation microenvironments implicate surface water flow origin". PNAS. 105 (36): 13258–63. Bibcode:2008PNAS..10513258H. doi:10.1073/pnas.0803760105. PMC 2734344Freely accessible. PMID 18725636. 
  230. ^ Henderson, Mark (December 7, 2006). "Water has been flowing on Mars within past five years, Nasa says". The Times. UK. 
  231. ^ "Mars photo evidence shows recently running water.". The Christian Science Monitor. Retrieved March 17, 2007. 
  232. ^ Malin, Michael C.; Edgett, Kenneth S. (2000). "Evidence for Recent Groundwater Seepage and Surface Runoff on Mars". Science. 288 (5475): 2330–2335. Bibcode:2000Sci...288.2330M. doi:10.1126/science.288.5475.2330. PMID 10875910. 
  233. ^ Kolb, K.; Pelletier, Jon D.; McEwen, Alfred S. (2010). "Modeling the formation of bright slope deposits associated with gullies in Hale Crater, Mars: Implications for recent liquid water". Icarus. 205: 113–137. Bibcode:2010Icar..205..113K. doi:10.1016/j.icarus.2009.09.009. 
  234. ^ Hoffman, Nick (2002). "Active polar gullies on Mars and the role of carbon dioxide". Astrobiology. 2 (3): 313–323. doi:10.1089/153110702762027899. PMID 12530241. 
  235. ^ Musselwhite, Donald S.; Swindle, Timothy D.; Lunine, Jonathan I. (2001). "Liquid CO2 breakout and the formation of recent small gullies on Mars". Geophysical Research Letters. 28 (7): 1283–1285. Bibcode:2001GeoRL..28.1283M. doi:10.1029/2000gl012496. 
  236. ^ McEwen, Alfred. S.; Ojha, Lujendra; Dundas, Colin M. (June 17, 2011). "Seasonal Flows on Warm Martian Slopes". Science. American Association for the Advancement of Science. 333 (6043): 740–743. Bibcode:2011Sci...333..740M. doi:10.1126/science.1204816. ISSN 0036-8075. PMID 21817049. 
  237. ^ "Nepali Scientist Lujendra Ojha spots possible water on Mars". Nepali Blogger. August 6, 2011. 
  238. ^ "NASA Spacecraft Data Suggest Water Flowing on Mars". NASA. August 4, 2011. 
  239. ^ McEwen, Alfred; Lujendra, Ojha; Dundas, Colin; Mattson, Sarah; Bryne, S; Wray, J; Cull, Selby; Murchie, Scott; Thomas, Nicholas; Gulick, Virginia (5 August 2011). "Seasonal Flows On Warm Martian Slopes.". Science. 333 (6043): 743–743. doi:10.1126/science.1204816. PMID 21817049. Retrieved 28 September 2015. 
  240. ^ Drake, Nadia; 28, National Geographic PUBLISHED September. "NASA Finds 'Definitive' Liquid Water on Mars". National Geographic News. Retrieved 2015-09-30. 
  241. ^ Moskowitz, Clara. "Water Flows on Mars Today, NASA Announces". Retrieved 2015-09-30. 
  242. ^ "NASA News Conference: Evidence of Liquid Water on Today's Mars". NASA. 28 September 2015. 
  243. ^ "NASA Confirms Evidence That Liquid Water Flows on Today's Mars". Retrieved 2015-09-30. 
  244. ^ Gronstal, Aaron L. (Jul 3, 2014). "Liquid Water from Ice and Salt on Mars". 
  245. ^ Moore, Nicole Casal (Jul 2, 2014). "Martian salts must touch ice to make liquid water, study shows". 
  246. ^ Gronstal, Aaron (July 3, 2014). "Liquid Water From Ice and Salt on Mars". Astrobiology Magazine (NASA). 
  247. ^ list of Honors and Accomplishments on the University of Michigan page about Nilton Renno.
  248. ^ ‘Swimming pool for bacteria’: There could be life on Mars today - new study - RT News
  249. ^ 'Is there life on Mars?': Water can and does exist on the planet says new research - the Independent
  250. ^ Martian salts must touch ice to make liquid water, study shows - Michigan News (the research was by a team of researchers at the University of Michigan)
  251. ^ "Based on the results of our experiment, we expect this soft ice that can liquify perhaps a few days per year, perhaps a few hours a day, almost anywhere on Mars. --- This is a small amount of liquid water. But for a bacteria, that would be a huge swimming pool ... So, a small amount of water is enough for you to be able to create conditions for Mars to be habitable today. And we believe this is possible in the shallow subsurface, and even the surface of the Mars polar region for a few hours per day during the spring.'"
    (transcript from 2 minutes into the video onwards, from Nilton Renno video (youtube)
  252. ^ a b Fischer, Erik; Martínez, Germán M.; Elliott, Harvey M.; Rennó, Nilton O. (2014). "Experimental evidence for the formation of liquid saline water on Mars". Geophysical Research Letters: n/a–n/a. doi:10.1002/2014GL060302. ISSN 0094-8276. 
  253. ^ a b Cite error: The named reference Mart.C3.ADnezRenno2013 was invoked but never defined (see the help page).
  254. ^ Martian salt streaks 'painted by liquid water' - BBC News
  255. ^ Amos, Jonathan. "Martian salt streaks 'painted by liquid water'". BBC Science. 
  256. ^ a b Staff (28 September 2015). "Video Highlight - NASA News Conference - Evidence of Liquid Water on Today's Mars". NASA. Retrieved 30 September 2015.  Cite error: Invalid <ref> tag; name "NASA-20150928b" defined multiple times with different content (see the help page).
  257. ^ a b Staff (28 September 2015). "Video Complete - NASA News Conference - Water Flowing on Present-Day Mars m". NASA. Retrieved 30 September 2015.  Cite error: Invalid <ref> tag; name "NASA-20150928a" defined multiple times with different content (see the help page).
  258. ^ a b c d Rummel, John D.; Beaty, David W.; Jones, Melissa A.; Bakermans, Corien; Barlow, Nadine G.; Boston, Penelope J.; Chevrier, Vincent F.; Clark, Benton C.; de Vera, Jean-Pierre P.; Gough, Raina V.; Hallsworth, John E.; Head, James W.; Hipkin, Victoria J.; Kieft, Thomas L.; McEwen, Alfred S.; Mellon, Michael T.; Mikucki, Jill A.; Nicholson, Wayne L.; Omelon, Christopher R.; Peterson, Ronald; Roden, Eric E.; Sherwood Lollar, Barbara; Tanaka, Kenneth L.; Viola, Donna; Wray, James J. (2014). "A New Analysis of Mars "Special Regions": Findings of the Second MEPAG Special Regions Science Analysis Group (SR-SAG2)" (PDF). Astrobiology. 14 (11): 887–968. doi:10.1089/ast.2014.1227. ISSN 1531-1074.  Cite error: Invalid <ref> tag; name "RummelBeaty2014" defined multiple times with different content (see the help page).
  259. ^ Surviving the conditions on Mars DLR, 26 April 2012
  260. ^ Jean-Pierre de Vera Lichens as survivors in space and on Mars Fungal Ecology Volume 5, Issue 4, August 2012, Pages 472–479
  261. ^ R. de la Torre Noetzel, F.J. Sanchez Inigo, E. Rabbow, G. Horneck, J. P. de Vera, L.G. Sancho Survival of lichens to simulated Mars conditions
  262. ^ F.J. Sáncheza, E. Mateo-Martíb, J. Raggioc, J. Meeßend, J. Martínez-Fríasb, L.Ga. Sanchoc, S. Ottd, R. de la Torrea The resistance of the lichen Circinaria gyrosa (nom. provis.) towards simulated Mars conditions—a model test for the survival capacity of an eukaryotic extremophile Planetary and Space Science Volume 72, Issue 1, November 2012, Pages 102–110
  263. ^ Cite error: The named reference BilliViaggiu2011 was invoked but never defined (see the help page).
  264. ^ Pigmentation as a survival strategy for ancient and modern photosynthetic microbes under high ultraviolet stress on planetary surfaces D.D. Wynn-Williams, H.G.M. Edwards, E.M. Newton and J.M. Holder, International Journal of Astrobiology 12/2001; 1(01):39 - 49. DOI: 10.1017/S1473550402001039
  265. ^ de Vera, Jean-Pierre; Schulze-Makuch, Dirk; Khan, Afshin; Lorek, Andreas; Koncz, Alexander; Möhlmann, Diedrich; Spohn, Tilman (2014). "Adaptation of an Antarctic lichen to Martian niche conditions can occur within 34 days" (PDF). Planetary and Space Science. 98: 182–190. doi:10.1016/j.pss.2013.07.014. ISSN 0032-0633. 
  266. ^ Cite error: The named reference DLRLichenHabitable was invoked but never defined (see the help page).
  267. ^ A Salty, Martian Meteorite Offers Clues to Habitability By Elizabeth Howell - Astrobiology Magazine (NASA) Aug 28, 2014
  268. ^ Cite error: The named reference Osanasaltpillars was invoked but never defined (see the help page).
  269. ^ "Some species (Haloferax mediterranei, Haloferax denitrificans, Haloferax gibbonsii, Haloarcula marismortui, Haloarcula vallismortis) could use perchlorate as an electron acceptor for anaerobic growth. Although perchlorate is highly oxidizing, its presence at a concentration of 0.2 M for up to 2 weeks did not negatively affect the ability of a yeast extract-based medium to support growth of the archaeon Halobacterium salinarum. These findings show that presence of perchlorate among the salts on Mars does not preclude the possibility of halophilic life. If indeed the liquid brines that may exist on Mars are inhabited by salt-requiring or salt-tolerant microorganisms similar to the halophiles on Earth, presence of perchlorate may even be stimulatory when it can serve as an electron acceptor for respiratory activity in the anaerobic Martian environment."Perchlorate and halophilic prokaryotes: implications for possible halophilic life on Mars Oren A1, Elevi Bardavid R, Mana L.. Water Sci Technol. 2009;60(7):1745-56. doi: 10.2166/wst.2009.635.
  270. ^ Cite error: The named reference Rincon was invoked but never defined (see the help page).
  271. ^ D. Schulze-Makuch, J.M. Houtkooper. "A Perchlorate Strategy for Extreme Xerophilic Life on Mars?" (PDF). European Planetary Science Congress 2010. 
  272. ^ Matson, John (February 6, 2013). "The New Way to Look for Mars Life: Follow the Salt". Scientific American. 
  273. ^ "Depending on the local solar constant, grain emissivity and thermal conductivity of ice, ice surrounding the dust grain melt for up to few hours a day during the warmest days of summer. For example, for solar constant 350 W/m2, emissivity 0.80, grain size 2 um, and thermal conductivity 0.4 W/mK melting lasts for ~300 minutes and result in melting of 6 mm of ice." ICE MELTING BY RADIANTLY HEATED DUST GRAINS ON THE MARTIAN NORTHERN POLE A. Losiak, L. Czechowski and M.A. Velbel, 77th Annual Meteoritical Society Meeting (2014)
  274. ^ Watery niche may foster life on Mars "According to Möhlmann, the heat from sunlight penetrating into ice or snow should get absorbed by any embedded dust grains, warming the dust and the surrounding ice. This heat mostly gets trapped because ice absorbs infrared radiation." (subscription required)
  275. ^ Tudor Vieru (2009-12-07). "Greenhouse Effect on Mars May Be Allowing for Life". News.softpedia.com. Retrieved 2011-08-20. 
  276. ^ Möhlmann, Diedrich T.F. (2010). "Temporary liquid water in upper snow/ice sub-surfaces on Mars?". Icarus. 207 (1): 140–148. doi:10.1016/j.icarus.2009.11.013. ISSN 0019-1035. 
  277. ^ Nl, K., and T. SAND. "Melting, runoff and the formation of frozen lakes in a mixed snow and blue-ice field in Dronning Maud Land, Antarctica.", J ournal oJ Glaciology, T'ol. 42, .\"0.141, 1996
  278. ^ Möhlmann, Diedrich T.F. (2010). "Temporary liquid water in upper snow/ice sub-surfaces on Mars?". Icarus. 207 (1): 140–148. doi:10.1016/j.icarus.2009.11.013. ISSN 0019-1035.  "The results described above make bare and optically transparent ice fields on Mars, analogous to terrestrial porous ‘‘blue-ice fields” of frozen snow with bluish meltwater at depths around 10 cm and more (cf. Liston and Winther, 2005), to be candidate sites where sub-surface melting might be possible. The thickness of the ice at these sites with translucent ice must be of several cenyimetres at least. The question is yet open as to whether bare and translucent water ice can have evolved or can also presently form on Mars, but there are also no indications which would rule out this possibility. Another open problem is whether the low thermal conductivity, which is necessary to avoid effective internal thermal losses (by heat conduction towards the cold surface) and to reach for A = 0.8 the range of temperatures around the melting point temperature, can be representative for snow/ice on Mars with yet nearly completely unknown physical properties."
  279. ^ Defrosting Defrosting of Richardson Dunes - HiRise data - gives the coordinates of the dune field with the Flow Like Features
  280. ^ Cite error: The named reference Kereszturi2008 was invoked but never defined (see the help page).
  281. ^ Jepsen, Steven M.; Priscu, John C.; Grimm, Robert E.; Bullock, Mark A. (2007). "The Potential for Lithoautotrophic Life on Mars: Application to Shallow Interfacial Water Environments" (PDF). Astrobiology. 7 (2): 342–354. doi:10.1089/ast.2007.0124. ISSN 1531-1074. 
  282. ^ Cite error: The named reference PriceSowers2004 was invoked but never defined (see the help page).
  283. ^ Kereszturi, Akos; Rivera-Valentin, Edgard G. (2012). "Locations of thin liquid water layers on present-day Mars" (PDF). Icarus. 221 (1): 289–295. doi:10.1016/j.icarus.2012.08.004. ISSN 0019-1035. 
  284. ^ HABITABILITY OF TRANGRESSING MARS DUNES. M Fisk, R Popa, N. Bridges, N. Renno, M. Mischna, J. Moores, R. Wiens, 44th Lunar and Planetary Science Conference (2013)
  285. ^ Starting conditions for hydrothermal systems underneath Martian craters: Hydrocode modeling Pierazzo, E., Artemieva, N.A., and Ivanov, B.A., 2005, from Large Meteorite Impacts III, Issue 384, p 444 edited by Thomas Kenkmann, Friedrich Hörz, Alexander Deutsch Geological Society of America, 1 Jan 2005 (pdf, earlier version with colour graphics)
  286. ^ "Impact melt and uplifted basement heat sources in craters >50 km in diameter should be sufficient to drive substantial hydrothermal activity and keep crater lakes from freezing for thousands of years, even under cold climatic conditions" Location and Sampling of Aqueous and Hydrothermal Deposits in Martian Impact Craters Horton E. Newsom, Justin J. Hagerty, and Ivan E. Thorsos. Astrobiology. March 2001, 1(1): 71-88. doi:10.1089/153110701750137459.]
  287. ^ Impact crater lakes on Mars, Horton E. Newsom, Gregory E. Brittelle, Charles A. Hibbitts, Laura J. Crossey, Albert M. Kudo, Journal of Geophysical Research: Planets (1991–2012) Volume 101, Issue E6, pages 14951–14955, 25 June 1996 DOI: 10.1029/96JE01139
  288. ^ Lakes on Mars (Google eBook), Nathalie A. Cabrol, Edmond A. Grin, Elsevier, 15 Sep 2010
  289. ^ A habitable environment on Martian volcano?, Kevin Stacey, News from Brown University, May 27, 2014, for the paper, see Volcano–ice interactions in the Arsia Mons tropical mountain glacier deposits, Kathleen E. Scanlona, James W. Heada, Lionel Wilsonb, David R. Marchant, Icarus Volume 237, 15 July 2014, Pages 315–339, doi:10.1016/j.icarus.2014.04.024
  290. ^ "Hunting for young lava flows". Geophysical Research Letters. Red Planet. June 1, 2011. Retrieved 4 October 2013. 
  291. ^ "Here we show that calderas on five major volcanoes on Mars have undergone repeated activation and resurfacing during the last 20 per cent of martian history, with phases of activity as young as two million years, suggesting that the volcanoes are potentially still active today. Glacial deposits at the base of the Olympus Mons escarpment show evidence for repeated phases of activity as recently as about four million years ago. Morphological evidence is found that snow and ice deposition on the Olympus construct at elevations of more than 7,000 metres led to episodes of glacial activity at this height. Even now, water ice protected by an insulating layer of dust may be present at high altitudes on Olympus Mons." Recent and episodic volcanic and glacial activity on Mars revealed by the High Resolution Stereo Camera G. Neukum1, R. Jaumann, H. Hoffmann, E. Hauber, J. W. Head, A. T. Basilevsky, B. A. Ivanov, S. C. Werner, S. van Gasselt, J. B. Murray, T. McCord & The HRSC Co-Investigator Team, Nature 432, 971-979 (23 December 2004) | doi:10.1038/nature03231; Received 3 September 2004; Accepted 30 November 2004
  292. ^ a b Cite error: The named reference phoenixisotope was invoked but never defined (see the help page).
  293. ^ Hunting for young lava flows Red Planet report, Posted on June 1, 2011 by rburnham
  294. ^ The Search For Volcanic Eruptions On Mars Reaches The Next Level, Elizabeth Howell - Feb 12, 2015, Astrobiology Magazine (NASA)
  295. ^ Cite error: The named reference icefumarolephotos was invoked but never defined (see the help page).
  296. ^ "Giant hollow towers of ice formed by steaming volcanic vents on Ross Island, Antarctica are providing clues about where to hunt for life on Mars." Martian Hot Spots Astrobiology Magazine (NASA) - Aug 7, 2003, Dr Nick Hoffman
  297. ^ Volcano-Ice Interaction as a Microbial Habitat on Earth and Mars, Claire R. Cousins and Ian A. Crawford, ASTROBIOLOGY Volume 11, Number 7, 2011, DOI: 10.1089/ast.2010.0550
  298. ^ The Ice Towers of Mt. Erebus as analogues of biological refuges on Mars ], N. Hoffman and P. R. Kyle, Sixth International Conference on Mars (2003)
  299. ^ Cite error: The named reference IceCaveMicrobes was invoked but never defined (see the help page).
  300. ^ Grin, E. A., N. A. Cabrol, and C. P. McKay. "The hypothesis of caves on Mars revisited through MGS data; Their potential as targets for the surveyor program." Workshop on Mars 2001: Integrated Science in Preparation for Sample Return and Human Exploration. Vol. 1. 1999.
  301. ^ Boston, Penelope J. "Location, location, location! Lava caves on Mars for habitat, resources, and the search for life." The Journal of Cosmology 12 (2010): 3957-3979.
  302. ^ NASA (December 19, 2014). "NASA, Planetary Scientists Find Meteoritic Evidence of Mars Water Reservoir". 
  303. ^ Usui, Tomohiro; Alexander, Conel M. O'D.; Wang, Jianhua; Simon, Justin I.; Jones, John H. (2015). "Meteoritic evidence for a previously unrecognized hydrogen reservoir on Mars" (PDF). Earth and Planetary Science Letters. 410: 140–151. doi:10.1016/j.epsl.2014.11.022. ISSN 0012-821X. 
  304. ^

    Error: No text given for quotation (or equals sign used in the actual argument to an unnamed parameter)

    , Lasue, Jeremie, et al. "Quantitative assessments of the martian hydrosphere." Space Science Reviews 174.1-4 (2013): 155-212.
  305. ^ a b Michalski, Joseph R., et al. "Groundwater activity on Mars and implications for a deep biosphere." Nature Geoscience 6.2 (2013): 133-138.
  306. ^

    "Aquifer Habitability Finally, deep aquifers below the cryosphere may have provided a hydraulic connection between various subpermafrost habitats. If Mars were ever inhabited, these hydraulic connections would likely have provided a means for biota to be transported from one habitable environment to another. An analogous system is fracture networks within or under permafrost in the terrestrial arctic. These systems harbor sulfatereducing microorganisms and other anaerobic taxa that can grow within the cold, saline conditions of the permafrost. Analogous conditions may exist within the Martian deep-subsurface where impact-generated fractures may have allowed both microorganisms and nutrients to migrate from one habitat to another—even ones arising from recent impacts and their associated hydrothermal environments, if habitats on Mars were inhabited and life existed on that planet "

    , Lasue, Jeremie, et al. "Quantitative assessments of the martian hydrosphere." Space Science Reviews 174.1-4 (2013): 155-212.
  307. ^ Donald M. Hassler, Cary Zeitlin, Robert F. Wimmer-Schweingruber, Bent Ehresmann, Scot Rafkin, Jennifer L. Eigenbrode, David E. Brinza, Gerald Weigle, Stephan Böttcher, Eckart Böhm, Soenke Burmeister, Jingnan Guo, Jan Köhler, Cesar Martin, Guenther Reitz, Francis A. Cucinotta, Myung-Hee Kim, David Grinspoon, Mark A. Bullock, Arik Posner, Javier Gómez-Elvira, Ashwin Vasavada, and John P. Grotzinger, and the MSL Science Team (12 November 2013). "Mars' Surface Radiation Environment Measured with the Mars Science Laboratory's Curiosity Rover" (PDF). Science: 7. 
  308. ^ Donald M. Hassler, Cary Zeitlin, Robert F. Wimmer-Schweingruber, Bent Ehresmann, Scot Rafkin, Jennifer L. Eigenbrode, David E. Brinza, Gerald Weigle, Stephan Böttcher, Eckart Böhm, Soenke Burmeister, Jingnan Guo, Jan Köhler, Cesar Martin, Guenther Reitz, Francis A. Cucinotta, Myung-Hee Kim, David Grinspoon, Mark A. Bullock, Arik Posner, Javier Gómez-Elvira, Ashwin Vasavada, and John P. Grotzinger, and the MSL Science Team (12 November 2013). "Mars' Surface Radiation Environment Measured with the Mars Science Laboratory's Curiosity Rover" (PDF). Science: 8. 
  309. ^ Joanna Carver and Victoria Jaggard (21 November 2012). "Mars is safe from radiation – but the trip there isn't". New Scientist. 
  310. ^ Minkel, JR (August 5, 2008). "NASA Says Perchlorate Does Not Rule Out Life on Mars - Unexpected chemical in Martian soil is a food source for some Earthly microbes". Scientific American. 
  311. ^ CHANG, KENNETH (October 5, 2015). "Mars Is Pretty Clean. Her Job at NASA Is to Keep It That Way". 
  312. ^ "Warm-Season Flows on Slope in Newton Crater". NASA Press Release. 
  313. ^ Amos, Jonathan. "Martian salt streaks 'painted by liquid water'". BBC Science. 
  314. ^ "Mars Reconnaissance Orbiter Telecommunications" (PDF). JPL. September 2006. 
  315. ^ "Mars Exploration: Missions". Marsprogram.jpl.nasa.gov. Retrieved December 19, 2010. 
  316. ^ "Viking Orbiter Views of Mars". History.nasa.gov. Retrieved December 19, 2010. 
  317. ^ "ch5". NASA History. NASA. Retrieved December 19, 2010. 
  318. ^ "Craters". NASA. Retrieved December 19, 2010. 
  319. ^ Morton, O. (2002). Mapping Mars. Picador, NY. 
  320. ^ Arvidson, R; Gooding, James L.; Moore, Henry J. (1989). "The Martian surface as Imaged, Sampled, and Analyzed by the Viking Landers". Review of Geophysics. 27: 39–60. Bibcode:1989RvGeo..27...39A. doi:10.1029/RG027i001p00039. 
  321. ^ Clark, B.; Baird, AK; Rose Jr., HJ; Toulmin P, 3rd; Keil, K; Castro, AJ; Kelliher, WC; Rowe, CD; Evans, PH (1976). "Inorganic Analysis of Martian Samples at the Viking Landing Sites". Science. 194 (4271): 1283–1288. Bibcode:1976Sci...194.1283C. doi:10.1126/science.194.4271.1283. PMID 17797084. 
  322. ^ Hoefen, T.M.; et al. (2003). "Discovery of Olivine in the Nili Fossae Region of Mars". Science. 302 (5645): 627–630. Bibcode:2003Sci...302..627H. doi:10.1126/science.1089647. PMID 14576430. 
  323. ^ Hoefen, T.; Clark, RN; Bandfield, JL; Smith, MD; Pearl, JC; Christensen, PR (2003). "Discovery of Olivine in the Nili Fossae Region of Mars". Science. 302 (5645): 627–630. Bibcode:2003Sci...302..627H. doi:10.1126/science.1089647. PMID 14576430. 
  324. ^ Malin, Michael C.; Edgett, Kenneth S. (2001). "Mars Global Surveyor Mars Orbiter Camera: Interplanetary cruise through primary mission". Journal of Geophysical Research. 106 (E10): 23429–23570. Bibcode:2001JGR...10623429M. doi:10.1029/2000JE001455. 
  325. ^ "Atmospheric and Meteorological Properties". NASA. 
  326. ^ a b Golombek, M. P.; Cook, R. A.; Economou, T.; Folkner, W. M.; Haldemann, A. F. C.; Kallemeyn, P. H.; Knudsen, J. M.; Manning, R. M.; Moore, H. J.; Parker, T. J.; Rieder, R.; Schofield, J. T.; Smith, P. H.; Vaughan, R. M. (1997). "Overview of the Mars Pathfinder Mission and Assessment of Landing Site Predictions". Science. 278 (5344): 1743–1748. Bibcode:1997Sci...278.1743G. doi:10.1126/science.278.5344.1743. PMID 9388167. 
  327. ^ Murche, S.; Mustard, John; Bishop, Janice; Head, James; Pieters, Carle; Erard, Stephane (1993). "Spatial Variations in the Spectral Properties of Bright Regions on Mars". Icarus. 105 (2): 454–468. Bibcode:1993Icar..105..454M. doi:10.1006/icar.1993.1141. 
  328. ^ "Home Page for Bell (1996) Geochemical Society paper". Marswatch.tn.cornell.edu. Retrieved December 19, 2010. 
  329. ^ Feldman, W. C.; Boynton, W. V.; Tokar, R. L.; Prettyman, T. H.; Gasnault, O.; Squyres, S. W.; Elphic, R. C.; Lawrence, D. J.; Lawson, S. L.; Maurice, S.; McKinney, G. W.; Moore, K. R.; Reedy, R. C. (2002). "Global Distribution of Neutrons from Mars: Results from Mars Odyssey". Science. 297 (5578): 75–78. Bibcode:2002Sci...297...75F. doi:10.1126/science.1073541. PMID 12040088. 
  330. ^ Mitrofanov, I.; Anfimov, D.; Kozyrev, A.; Litvak, M.; Sanin, A.; Tret'yakov, V.; Krylov, A.; Shvetsov, V.; Boynton, W.; Shinohara, C.; Hamara, D.; Saunders, R. S. (2002). "Maps of Subsurface Hydrogen from the High Energy Neutron Detector, Mars Odyssey". Science. 297 (5578): 78–81. Bibcode:2002Sci...297...78M. doi:10.1126/science.1073616. PMID 12040089. 
  331. ^ Boynton, W. V.; Feldman, W. C.; Squyres, S. W.; Prettyman, T. H.; Brückner, J.; Evans, L. G.; Reedy, R. C.; Starr, R.; Arnold, J. R.; Drake, D. M.; Englert, P. A. J.; Metzger, A. E.; Mitrofanov, Igor; Trombka, J. I.; d'Uston, C.; Wänke, H.; Gasnault, O.; Hamara, D. K.; Janes, D. M.; Marcialis, R. L.; Maurice, S.; Mikheeva, I.; Taylor, G. J.; Tokar, R.; Shinohara, C. (2002). "Distribution of Hydrogen in the Near Surface of Mars: Evidence for Subsurface Ice Deposits". Science. 297 (5578): 81–85. Bibcode:2002Sci...297...81B. doi:10.1126/science.1073722. PMID 12040090. 
  332. ^ "Dao Vallis". Mars Odyssey Mission. THEMIS. August 7, 2002. Retrieved December 19, 2010. 
  333. ^ a b Smith, P. H.; Tamppari, L.; Arvidson, R. E.; Bass, D.; Blaney, D.; Boynton, W.; Carswell, A.; Catling, D.; Clark, B.; Duck, T.; DeJong, E.; Fisher, D.; Goetz, W.; Gunnlaugsson, P.; Hecht, M.; Hipkin, V.; Hoffman, J.; Hviid, S.; Keller, H.; Kounaves, S.; Lange, C. F.; Lemmon, M.; Madsen, M.; Malin, M.; Markiewicz, W.; Marshall, J.; McKay, C.; Mellon, M.; Michelangeli, D.; et al. (2008). "Introduction to special section on the phoenix mission: Landing site characterization experiments, mission overviews, and expected science". J. Geophysical Research. 113: E00A18. Bibcode:2008JGRE..113.0A18S. doi:10.1029/2008JE003083. 
  334. ^ "NASA Data Shed New Light About Water and Volcanoes on Mars". NASA. September 9, 2010. Retrieved March 21, 2014. 
  335. ^ Mellon, M.; Jakosky, B. (1993). "Geographic variations in the thermal and diffusive stability of ground ice on Mars". J. Geographical Research. 98: 3345–3364. Bibcode:1993JGR....98.3345M. doi:10.1029/92JE02355. 
  336. ^ "Confirmation of Water on Mars". Nasa.gov. June 20, 2008. 
  337. ^ a b "The Dirt on Mars Lander Soil Findings". SPACE.com. Retrieved December 19, 2010. 
  338. ^ a b c Martínez, G. M. & Renno, N. O. (2013). "Water and brines on Mars: current evidence and implications for MSL". Space Science Reviews. 175 (1–4): 29–51. Bibcode:2013SSRv..175...29M. doi:10.1007/s11214-012-9956-3. 
  339. ^ Rennó, Nilton O.; Bos, Brent J.; Catling, David; Clark, Benton C.; Drube, Line; Fisher, David; Goetz, Walter; Hviid, Stubbe F.; Keller, Horst Uwe; Kok, Jasper F.; Kounaves, Samuel P.; Leer, Kristoffer; Lemmon, Mark; Madsen, Morten Bo; Markiewicz, Wojciech J.; Marshall, John; McKay, Christopher; Mehta, Manish; Smith, Miles; Zorzano, M. P.; Smith, Peter H.; Stoker, Carol; Young, Suzanne M. M. (2009). "Possible physical and thermodynamical evidence for liquid water at the Phoenix landing site". Journal of Geophysical Research. 114: E00E03. Bibcode:2009JGRE..114.0E03R. doi:10.1029/2009JE003362. 
  340. ^ Chang, Kenneth (March 16, 2009). "Blobs in Photos of Mars Lander Stir a Debate: Are They Water?". New York Times (online). 
  341. ^ "Liquid Saltwater Is Likely Present On Mars, New Analysis Shows". ScienceDaily. March 20, 2009. 
  342. ^ "Astrobiology Top 10: Too Salty to Freeze". Astrobio.net. Retrieved December 19, 2010. 
  343. ^ Hecht, M. H.; Kounaves, S. P.; Quinn, R. C.; West, S. J.; Young, S. M. M.; Ming, D. W.; Catling, D. C.; Clark, B. C.; Boynton, W. V.; Hoffman, J.; DeFlores, L. P.; Gospodinova, K.; Kapit, J.; Smith, P. H. (2009). "Detection of Perchlorate and the Soluble Chemistry of Martian Soil at the Phoenix Lander Site". Science. 325 (5936): 64–67. Bibcode:2009Sci...325...64H. doi:10.1126/science.1172466 (inactive 2017-01-15). PMID 19574385. 
  344. ^ Smith, P. H.; Tamppari, L. K.; Arvidson, R. E.; Bass, D.; Blaney, D.; Boynton, W. V.; Carswell, A.; Catling, D. C.; Clark, B. C.; Duck, T.; DeJong, E.; Fisher, D.; Goetz, W.; Gunnlaugsson, H. P.; Hecht, M. H.; Hipkin, V.; Hoffman, J.; Hviid, S. F.; Keller, H. U.; Kounaves, S. P.; Lange, C. F.; Lemmon, M. T.; Madsen, M. B.; Markiewicz, W. J.; Marshall, J.; McKay, C. P.; Mellon, M. T.; Ming, D. W.; Morris, R. V.; et al. (2009). "H2O at the Phoenix Landing Site". Science. 325 (5936): 58–61. Bibcode:2009Sci...325...58S. doi:10.1126/science.1172339 (inactive 2017-01-15). PMID 19574383. 
  345. ^ Whiteway, J. A.; Komguem, L.; Dickinson, C.; Cook, C.; Illnicki, M.; Seabrook, J.; Popovici, V.; Duck, T. J.; Davy, R.; Taylor, P. A.; Pathak, J.; Fisher, D.; Carswell, A. I.; Daly, M.; Hipkin, V.; Zent, A. P.; Hecht, M. H.; Wood, S. E.; Tamppari, L. K.; Renno, N.; Moores, J. E.; Lemmon, M. T.; Daerden, F.; Smith, P. H. (2009). "Mars Water-Ice Clouds and Precipitation". Science. 325 (5936): 68–70. Bibcode:2009Sci...325...68W. doi:10.1126/science.1172344 (inactive 2017-01-15). PMID 19574386. 
  346. ^ "CSA – News Release". Asc-csa.gc.ca. July 2, 2009. 
  347. ^ "Mars Exploration Rover Mission: Press Releases". Marsrovers.jpl.nasa.gov. March 5, 2004. 
  348. ^ "NASA – Mars Rover Spirit Unearths Surprise Evidence of Wetter Past". NASA. May 21, 2007. 
  349. ^ Bertster, Guy (December 10, 2007). "Mars Rover Investigates Signs of Steamy Martian Past". Press Release. Jet Propulsion Laboratory, Pasadena, California. 
  350. ^ Klingelhofer, G.; et al. (2005). "volume XXXVI". Lunar Planet. Sci. (abstr.): 2349. 
  351. ^ Schroder, C.; et al. (2005). "Journal of Geophysical Research" (abstr.). 7. European Geosciences Union, General Assembly: 10254. 
  352. ^ Morris, S.; et al. (2006). "Mössbauer mineralogy of rock, soil, and dust at Gusev crater, Mars: Spirit's journal through weakly altered olivine basalt on the plains and pervasively altered basalt in the Columbia Hills". J. Geophys. Res. 111: n/a. Bibcode:2006JGRE..111.2S13M. doi:10.1029/2005je002584. 
  353. ^ Ming, D.; Mittlefehldt, D. W.; Morris, R. V.; Golden, D. C.; Gellert, R.; Yen, A.; Clark, B. C.; Squyres, S. W.; Farrand, W. H.; Ruff, S. W.; Arvidson, R. E.; Klingelhöfer, G.; McSween, H. Y.; Rodionov, D. S.; Schröder, C.; De Souza, P. A.; Wang, A. (2006). "Geochemical and mineralogical indicators for aqueous processes in the Columbia Hills of Gusev crater, Mars". J. Geophys. Res. 111: E02S12. Bibcode:2006JGRE..111.2S12M. doi:10.1029/2005JE002560. 
  354. ^ Bell, J, ed. (2008). "The Martian Surface". Cambridge University Press. ISBN 978-0-521-86698-9. 
  355. ^ Morris, R. V.; Ruff, S. W.; Gellert, R.; Ming, D. W.; Arvidson, R. E.; Clark, B. C.; Golden, D. C.; Siebach, K.; Klingelhofer, G.; Schroder, C.; Fleischer, I.; Yen, A. S.; Squyres, S. W. (June 4, 2010). "Outcrop of long-sought rare rock on Mars found". Science. Sciencedaily.com. 329 (5990): 421–424. Bibcode:2010Sci...329..421M. doi:10.1126/science.1189667. PMID 20522738. 
  356. ^ Morris, Richard V.; Ruff, Steven W.; Gellert, Ralf; Ming, Douglas W.; Arvidson, Raymond E.; Clark, Benton C.; Golden, D. C.; Siebach, Kirsten; et al. (June 3, 2010). "Identification of Carbonate-Rich Outcrops on Mars by the Spirit Rover". Science. 329 (5990): 421–424. Bibcode:2010Sci...329..421M. doi:10.1126/science.1189667. PMID 20522738. 
  357. ^ "Opportunity Rover Finds Strong Evidence Meridiani Planum Was Wet". Retrieved July 8, 2006. 
  358. ^ Harwood, William (January 25, 2013). "Opportunity rover moves into 10th year of Mars operations". Space Flight Now. 
  359. ^ Benison, KC; Laclair, DA (2003). "Modern and ancient extremely acid saline deposits: terrestrial analogs for martian environments?". Astrobiology. 3 (3): 609–618. Bibcode:2003AsBio...3..609B. doi:10.1089/153110703322610690. PMID 14678669. 
  360. ^ Benison, K; Bowen, B (2006). "Acid saline lake systems give clues about past environments and the search for life on Mars". Icarus. 183 (1): 225–229. Bibcode:2006Icar..183..225B. doi:10.1016/j.icarus.2006.02.018. 
  361. ^ Osterloo, MM; Hamilton, VE; Bandfield, JL; Glotch, TD; Baldridge, AM; Christensen, PR; Tornabene, LL; Anderson, FS (2008). "Chloride-Bearing Materials in the Southern Highlands of Mars". Science. 319 (5870): 1651–1654. Bibcode:2008Sci...319.1651O. doi:10.1126/science.1150690. PMID 18356522. 
  362. ^ Grotzinger, J.; Milliken, R., eds. (2012). "Sedimentary Geology of Mars". SEPM. 
  363. ^ "HiRISE – High Resolution Imaging Science Experiment". HiriUniversity of Arizona. Retrieved December 19, 2010. 
  364. ^ "Target Zone: Nilosyrtis? | Mars Odyssey Mission THEMIS". Themis.asu.edu. Retrieved December 19, 2010. 
  365. ^ Mellon, M. T.; Jakosky, B. M.; Postawko, S. E. (1997). "The persistence of equatorial ground ice on Mars". J. Geophys. Res. onlinelibrary.wiley.com. 102(E8): 19357–19369. Bibcode:1997JGR...10219357M. doi:10.1029/97JE01346. 
  366. ^ Arfstrom, John D. (2012). "A Conceptual Model of Equatorial Ice Sheets on Mars. J" (PDF). Comparative Climatology of Terrestrial Planets. Lunar and Planetary Institute. 
  367. ^ Byrne, Shane; Dundas, Colin M.; Kennedy, Megan R.; Mellon, Michael T.; McEwen, Alfred S.; Cull, Selby C.; Daubar, Ingrid J.; Shean, David E.; Seelos, Kimberly D.; Murchie, Scott L.; Cantor, Bruce A.; Arvidson, Raymond E.; Edgett, Kenneth S.; Reufer, Andreas; Thomas, Nicolas; Harrison, Tanya N.; Posiolova, Liliya V.; Seelos, Frank P. (2009). "Distribution of mid-latitude ground ice on Mars from new impact craters". Science. 325 (5948): 1674–1676. Bibcode:2009Sci...325.1674B. doi:10.1126/science.1175307. PMID 19779195. 
  368. ^ "Water Ice Exposed in Mars Craters". SPACE.com. Retrieved December 19, 2010. 
  369. ^ Brown, Dwayne (October 30, 2012). "NASA Rover's First Soil Studies Help Fingerprint Martian Minerals". NASA. 
  370. ^ Brown, Dwayne; Webster, Guy; Neal-Jones, Nance (December 3, 2012). "NASA Mars Rover Fully Analyzes First Martian Soil Samples". NASA. 
  371. ^ Chang, Ken (December 3, 2012). "Mars Rover Discovery Revealed". New York Times. 
  372. ^ a b Webster, Guy; Brown, Dwayne (March 18, 2013). "Curiosity Mars Rover Sees Trend In Water Presence". NASA. 
  373. ^ Rincon, Paul (March 19, 2013). "Curiosity breaks rock to reveal dazzling white interior". BBC. 
  374. ^ Staff (March 20, 2013). "Red planet coughs up a white rock, and scientists freak out". MSN. 
  375. ^ Lieberman, Josh (September 26, 2013). "Mars Water Found: Curiosity Rover Uncovers 'Abundant, Easily Accessible' Water In Martian Soil". iSciencetimes. 
  376. ^ Leshin, L. A.; et al. (September 27, 2013). "Volatile, Isotope, and Organic Analysis of Martian Fines with the Mars Curiosity Rover". Science. 341 (6153): 1238937. doi:10.1126/science.1238937. PMID 24072926. 
  377. ^ a b Grotzinger, John (September 26, 2013). "Introduction To Special Issue: Analysis of Surface Materials by the Curiosity Mars Rover". Science. 341 (6153): 1475. Bibcode:2013Sci...341.1475G. doi:10.1126/science.1244258. 
  378. ^ Neal-Jones, Nancy; Zubritsky, Elizabeth; Webster, Guy; Martialay, Mary (September 26, 2013). "Curiosity's SAM Instrument Finds Water and More in Surface Sample". NASA. 
  379. ^ a b Webster, Guy; Brown, Dwayne (September 26, 2013). "Science Gains From Diverse Landing Area of Curiosity". NASA. 
  380. ^ a b Chang, Kenneth (October 1, 2013). "Hitting Pay Dirt on Mars". New York Times. 
  381. ^ a b Meslin, P.-Y.; et al. (September 26, 2013). "Soil Diversity and Hydration as Observed by ChemCam at Gale Crater, Mars". Science. 341 (6153): 1238670. doi:10.1126/science.1238670. 
  382. ^ Stolper, E.M.; Baker, M.B.; Newcombe, M.E.; Schmidt, M.E.; Treiman, A.H.; Cousin, A.; Dyar, M.D.; Fisk, M.R.; Gellert, R.; King, P.L.; Leshin, L.; Maurice, S.; McLennan, S.M.; Minitti, M.E.; Perrett, G.; Rowland, S.; Sautter, V.; Wiens, R.C.; MSL ScienceTeam (2013). "The Petrochemistry of Jake_M: A Martian Mugearite". Science. AAAS. 341 (6153): 1239463. doi:10.1126/science.1239463. Retrieved September 28, 2013. 
  383. ^ Webster, Guy; Neal-Jones, Nancy; Brown, Dwayne (December 16, 2014). "NASA Rover Finds Active and Ancient Organic Chemistry on Mars". NASA. Retrieved December 16, 2014. 
  384. ^ Chang, Kenneth (December 16, 2014). "'A Great Moment': Rover Finds Clue That Mars May Harbor Life". New York Times. Retrieved December 16, 2014. 
  385. ^ Mahaffy, P. R.; et al. (December 16, 2014). "Mars Atmosphere - The imprint of atmospheric evolution in the D/H of Hesperian clay minerals on Mars". Science. 347 (6220): 412–414. Bibcode:2015Sci...347..412M. doi:10.1126/science.1260291. Retrieved December 16, 2014. 
  386. ^ Rincon, Paul (April 13, 2015). "Evidence of liquid water found on Mars". BBC News. Retrieved April 15, 2015. 
  387. ^ Clavin, Whitney (October 8, 2015). "NASA's Curiosity Rover Team Confirms Ancient Lakes on Mars". NASA. Retrieved October 9, 2015. 
  388. ^ Grotzinger, J.P.; et al. (October 9, 2015). "Deposition, exhumation, and paleoclimate of an ancient lake deposit, Gale crater, Mars". Science. 350 (6257): aac7575. Bibcode:2015Sci...350.7575G. doi:10.1126/science.aac7575. Retrieved October 9, 2015. 


  • Boyce, Joseph, M. (2008). The Smithsonian Book of Mars; Konecky & Konecky: Old Saybrook, CT, ISBN 978-1-58834-074-0
  • Carr, Michael, H. (1996). Water on Mars; Oxford University Press: New York, ISBN 0-19-509938-9.
  • Carr, Michael, H. (2006). The Surface of Mars; Cambridge University Press: Cambridge, UK, ISBN 978-0-521-87201-0.
  • Hartmann, William, K. (2003). A Traveler’s Guide to Mars: The Mysterious Landscapes of the Red Planet; Workman: New York, ISBN 0-7611-2606-6.
  • Hanlon, Michael (2004). The Real Mars: Spirit, Opportunity, Mars Express and the Quest to Explore the Red Planet; Constable: London, ISBN 1-84119-637-1.
  • Kargel, Jeffrey, S. (2004). Mars: A Warmer Wetter Planet; Springer-Praxis: London, ISBN 1-85233-568-8.
  • Morton, Oliver (2003). Mapping Mars: Science, Imagination, and the Birth of a World; Picador: New York, ISBN 0-312-42261-X.
  • Sheehan, William (1996). The Planet Mars: A History of Observation and Discovery; University of Arizona Press: Tucson, AZ, ISBN 0-8165-1640-5.
  • Viking Orbiter Imaging Team (1980). Viking Orbiter Views of Mars, C.R. Spitzer, Ed.; NASA SP-441: Washington DC.

External links[edit]