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Atmosphere of Mars

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Further information: Climate of Mars
Atmosphere of Mars
Mars
Image of Mars and its thin atmosphere, photographed by Emirates Mars Mission
General information[2]
Average surface pressure610 Pa (0.088 psi; 4.6 mmHg; 0.0060 atm)
Mass2.5x1016 kg[1]
Composition[3][4]
Carbon dioxide95%
Nitrogen2.8%
Argon2%
Oxygen0.174%
Carbon monoxide0.0747%
Water vapor0.03% (variable)

The atmosphere of Mars is the layer of gases surrounding Mars. It is primarily composed of carbon dioxide (95%), molecular nitrogen (2.85%), and argon (2%).[3] It also contains trace levels of water vapor, oxygen, carbon monoxide, hydrogen, and noble gases.[3][5][2] The atmosphere of Mars is much thinner and colder than Earth's having a max density 20g/m3 (about 2% of Earth’s value) with a temperature generally below zero down to -60 Celsius. The average surface pressure is about 610 pascals (0.088 psi) which is 0.6% of the Earth's value.[2]

The currently thin Martian atmosphere prohibits the existence of liquid water on the surface of Mars, but many studies suggest that the Martian atmosphere was much thicker in the past.[4] The higher density during spring and fall is reduced by 25% during the winter when carbon dioxide partly freezes at the pole caps.[6] The highest atmospheric density on Mars is equal to the density found 35 km (22 mi) above the Earth's surface and is ≈0.020 kg/m3.[7] The atmosphere of Mars has been losing mass to space since the planet's core slowed down, and the leakage of gases still continues today.[4][8][9]

The atmosphere of Mars is colder than Earth’s owing to the larger distance from the Sun, receiving less solar energy and has a lower effective temperature, which is about 210 K (−63 °C; −82 °F).[2] The average surface emission temperature of Mars is just 215 K (−58 °C; −73 °F), which is comparable to inland Antarctica.[2][4] Although Mars' atmosphere consists primarily of carbon dioxide, the greenhouse effect in the Martian atmosphere is much weaker than Earth's: 5 °C (9.0 °F) on Mars, versus 33 °C (59 °F) on Earth due to the much lower density of carbon dioxide, leading to less greenhouse warming.[2][4] The daily range of temperature in the lower atmosphere presents ample variation due to the low thermal inertia; it can range from −75 °C (−103 °F) to near 0 °C (32 °F) near the surface in some regions.[2][4][10] The temperature of the upper part of the Martian atmosphere is also significantly lower than Earth's because of the absence of stratospheric ozone and the radiative cooling effect of carbon dioxide at higher altitudes.[4]

Dust devils and dust storms are prevalent on Mars, which are sometimes observable by telescopes from Earth,[11] and in 2018 even with the naked eye as a change in colour and brightness of the planet.[12] Planet-encircling dust storms (global dust storms) occur on average every 5.5 Earth years (every 3 Martian years) on Mars[4][11] and can threaten the operation of Mars rovers.[13] However, the mechanism responsible for the development of large dust storms is still not well understood.[14][15] It has been suggested to be loosely related to gravitational influence of both moons, somewhat similar to the creation of tides on Earth.

The Martian atmosphere is an oxidized atmosphere. The photochemical reactions in the atmosphere tend to oxidize the organic species and turn them into carbon dioxide or carbon monoxide.[4] Although the most sensitive methane probe on the recently launched ExoMars Trace Gas Orbiter failed to find methane in the atmosphere over the whole of Mars,[16][17][18] several previous missions and ground-based telescopes detected unexpected levels of methane in the Martian atmosphere, which may even be a biosignature for life on Mars.[19][20][21] However, the interpretation of the measurements is still highly controversial and lacks a scientific consensus.[21][22]

Atmospheric evolution

[edit]
See also: Atmospheric escape and Water on Mars

The mass and composition of the Martian atmosphere are thought to have changed over the course of the planet's lifetime. A thicker, warmer and wetter atmosphere is required to explain several apparent features in the earlier history of Mars, such as the existence of liquid water bodies. Observations of the Martian upper atmosphere, measurements of isotopic composition and analyses of Martian meteorites, provide evidence of the long-term changes of the atmosphere and constraints for the relative importance of different processes.

Atmosphere in the early history

[edit]
Isotopic ratio of different species in Martian and Earth's atmosphere
Isotopic ratio Mars Earth Mars / Earth
D / H (in H2O) 9.3 ± 1.7 10−4[23][4] 1.56 10−4[24] ~6
12C / 13C 85.1 ± 0.3[23][4] 89.9[25] 0.95
14N / 15N 173 ± 9[23][26][4] 272[24] 0.64
16O / 18O 476 ± 4.0[23][4] 499[25] 0.95
36Ar / 38Ar 4.2 ± 0.1[27] 5.305 ± 0.008[28] 0.79
40Ar / 36Ar 1900 ± 300[29] 298.56 ± 0.31[28] ~6
C / 84Kr (4.4–6) × 106[30][4] 4 × 107[30][4] ~0.1
129Xe / 132Xe 2.5221 ± 0.0063[31] 0.97[citation needed] ~2.5

In general, the gases found on modern Mars are depleted in lighter stable isotopes, indicating the Martian atmosphere has changed by some mass-selected processes over its history. Scientists often rely on these measurements of isotope composition to reconstruct conditions of the Martian atmosphere in the past.[32][33][34]

While Mars and Earth have similar 12C / 13C and 16O / 18O ratios, 14N is much more depleted in the Martian atmosphere. It is thought that the photochemical escape processes are responsible for the isotopic fractionation and has caused a significant loss of nitrogen on geological timescales.[4] Estimates suggest that the initial partial pressure of N2 may have been up to 30 hPa.[35][36]

Hydrodynamic escape in the early history of Mars may explain the isotopic fractionation of argon and xenon. On modern Mars, the atmosphere is not leaking these two noble gases to outer space owing to their heavier mass. However, the higher abundance of hydrogen in the Martian atmosphere and the high fluxes of extreme UV from the young Sun, together could have driven a hydrodynamic outflow and dragged away these heavy gases.[37][38][4] Hydrodynamic escape also contributed to the loss of carbon, and models suggest that it is possible to lose 1,000 hPa (1 bar) of CO2 by hydrodynamic escape in one to ten million years under much stronger solar extreme UV on Mars.[39] Meanwhile, more recent observations made by the MAVEN orbiter suggested that sputtering escape is very important for the escape of heavy gases on the nightside of Mars and could have contributed to 65% loss of argon in the history of Mars.[40][41][33]

The Martian atmosphere is particularly prone to impact erosion owing to the low escape velocity of Mars. An early computer model suggested that Mars could have lost 99% of its initial atmosphere by the end of late heavy bombardment period based on a hypothetical bombardment flux estimated from lunar crater density.[42] In terms of relative abundance of carbon, the C / 84Kr ratio on Mars is only 10% of that on Earth and Venus. Assuming the three rocky planets have the same initial volatile inventory, then this low C / 84Kr ratio implies the mass of CO2 in the early Martian atmosphere should have been ten times higher than the present value.[43] The huge enrichment of radiogenic 40Ar over primordial 36Ar is also consistent with the impact erosion theory.[4]

One of the ways to estimate the amount of water lost by hydrogen escape in the upper atmosphere is to examine the enrichment of deuterium over hydrogen. Isotope-based studies estimate that 12 m to over 30 m global equivalent layer of water has been lost to space via hydrogen escape in Mars' history.[44] It is noted that atmospheric-escape-based approach only provides the lower limit for the estimated early water inventory.[4]

To explain the coexistence of liquid water and faint young Sun during early Mars' history, a much stronger greenhouse effect must have occurred in the Martian atmosphere to warm the surface up above freezing point of water. Carl Sagan first proposed that a 1 bar H2 atmosphere can produce enough warming for Mars.[45] The hydrogen can be produced by the vigorous outgassing from a highly reduced early Martian mantle and the presence of CO2 and water vapor can lower the required abundance of H2 to generate such a greenhouse effect.[46] Nevertheless, photochemical modeling showed that maintaining an atmosphere with this high level of H2 is difficult.[47] SO2 has also been one of the proposed effective greenhouse gases in the early history of Mars.[48][49][50] However, other studies suggested that high solubility of SO2, efficient formation of H2SO4 aerosol and surface deposition prohibit the long-term build-up of SO2 in the Martian atmosphere, and hence reduce the potential warming effect of SO2.[4]

Atmospheric escape on modern Mars

[edit]

Despite the lower gravity, Jeans escape is not efficient in the modern Martian atmosphere due to the relatively low temperature at the exobase (≈200 K at 200 km altitude). It can only explain the escape of hydrogen from Mars. Other non-thermal processes are needed to explain the observed escape of oxygen, carbon and nitrogen.

Hydrogen escape

[edit]

Molecular hydrogen (H2) is produced from the dissociation of H2O or other hydrogen-containing compounds in the lower atmosphere and diffuses to the exosphere. The exospheric H2 then decomposes into hydrogen atoms, and the atoms that have sufficient thermal energy can escape from the gravitation of Mars (Jeans escape). The escape of atomic hydrogen is evident from the UV spectrometers on different orbiters.[51][52] While most studies suggested that the escape of hydrogen is close to diffusion-limited on Mars,[53][54] more recent studies suggest that the escape rate is modulated by dust storms and has a large seasonality.[55][56][57] The estimated escape flux of hydrogen range from 107 cm−2 s−1 to 109 cm−2 s−1.[56]

Carbon escape

[edit]

Photochemistry of CO2 and CO in ionosphere can produce CO2+ and CO+ ions, respectively:

CO2 + hν ⟶ CO+2 + e−
CO + hν ⟶ CO+ + e−

An ion and an electron can recombine and produce electronic-neutral products. The products gain extra kinetic energy due to the Coulomb attraction between ions and electrons. This process is called dissociative recombination. Dissociative recombination can produce carbon atoms that travel faster than the escape velocity of Mars, and those moving upward can then escape the Martian atmosphere:

CO+ + e− ⟶ C + O
CO+2 + e− ⟶ C + O2

UV photolysis of carbon monoxide is another crucial mechanism for the carbon escape on Mars:[58]

CO + hν (λ < 116  nm) ⟶ C + O.

Other potentially important mechanisms include the sputtering escape of CO2 and collision of carbon with fast oxygen atoms.[4] The estimated overall escape flux is about 0.6 × 107 cm−2 s−1 to 2.2 × 107 cm−2 s−1 and depends heavily on solar activity.[59][4]

Nitrogen escape

[edit]

Like carbon, dissociative recombination of N2+ is important for the nitrogen escape on Mars.[60][61] In addition, other photochemical escape mechanism also play an important role:[60][62]

N2 + hν ⟶ N+ + N + e−
N2 + e− ⟶ N+ + N + 2e−

Nitrogen escape rate is very sensitive to the mass of the atom and solar activity. The overall estimated escape rate of 14N is 4.8 × 105 cm−2 s−1.[60]

Oxygen escape

[edit]

Dissociative recombination of CO2+ and O2+ (produced from CO2+ reaction as well) can generate the oxygen atoms that travel fast enough to escape:

CO+2 + e− ⟶ CO + O
CO+2 + O ⟶ O+2 + CO
O+2 + e− ⟶ O + O

However, the observations showed that there are not enough fast oxygen atoms the Martian exosphere as predicted by the dissociative recombination mechanism.[63][41] Model estimations of oxygen escape rate suggested it can be over 10 times lower than the hydrogen escape rate.[59][64] Ion pick and sputtering have been suggested as the alternative mechanisms for the oxygen escape, but this model suggests that they are less important than dissociative recombination at present.[65]

Mars's escaping atmosphere—carbon, oxygen, hydrogen—measured by MAVEN's UV spectrograph).[66]

Ionospheric escape

[edit]

The interaction of the solar wind and the interplanetary magnetic field with the Martian conductive ionosphere induces electrodynamic currents, that have been mapped and studied in detail, using MAVEN.[67] These currents can drive the ionospheric species to high altitudes, where the solar wind is able to sweep them away from the planet, resulting to global scale ion outflows. They are however not sufficient to explain the atmospheric and ionospheric losses of Mars over its lifetime.[68]

Current chemical composition

[edit]

Carbon dioxide

[edit]
See also: Martian polar ice caps

CO2 is the main component of the Martian atmosphere. It has a mean volume (molar) ratio of 94.9%.[3] In winter polar regions, the surface temperature can be lower than the frost point of CO2. CO2 gas in the atmosphere can condense on the surface to form 1–2 m thick solid dry ice.[4] In summer, the polar dry ice cap can undergo sublimation and release the CO2 back to the atmosphere. As a result, significant annual variability in atmospheric pressure (≈25%) and atmospheric composition can be observed on Mars.[69] The condensation process can be approximated by the Clausius–Clapeyron relation for CO2.[70][4]

There also exists the potential for adsorption of CO2 into and out of the regolith to contribute to the annual atmospheric variability. Although the sublimation and deposition of CO2 ice in the polar caps is the driving force behind seasonal cycles, other processes such as dust storms, atmospheric tides, and transient eddies also play a role.[71][72][73][74][75] Understanding each of these more minor processes and how they contribute to the overall atmospheric cycle will give a clearer picture as to how the Martian atmosphere works as a whole. It has been suggested that the regolith on Mars has high internal surface area, implying that it might have a relatively high capacity for the storage of adsorbed gas.[76] Since adsorption works through the adhesion of a film of molecules onto a surface, the amount of surface area for any given volume of material is the main contributor for how much adsorption can occur. A solid block of material, for example, would have no internal surface area, but a porous material, like a sponge, would have high internal surface area. Given the loose, finely grained nature of the Martian regolith, there is the possibility of significant levels of CO2 adsorption into it from the atmosphere.[77] Adsorption from the atmosphere into the regolith has previously been proposed as an explanation for the observed cycles in the methane and water mixing ratios.[76][77][78][79] More research is needed to help determine if CO2 adsorption is occurring, and if so, the extent of its impact on the overall atmospheric cycle.

Comparison of the abundance of carbon dioxide, nitrogen, and argon in the atmospheres of Earth, Venus, and Mars

Despite the high concentration of CO2 in the Martian atmosphere, the greenhouse effect is relatively weak on Mars (about 5 °C) because of the low concentration of water vapor and low atmospheric pressure. While water vapor in Earth's atmosphere has the largest contribution to greenhouse effect on modern Earth, it is present in only very low concentration in the Martian atmosphere. Moreover, under low atmospheric pressure, greenhouse gases cannot absorb infrared radiation effectively because the pressure-broadening effect is weak.[80][81]

In the presence of solar UV radiation (hν, photons with wavelength shorter than 225 nm), CO2 in the Martian atmosphere can be photolyzed via the following reaction:

CO2 + hν (λ < 225 nm) ⟶ CO + O.

If there is no chemical production of CO2, all the CO2 in the current Martian atmosphere would be removed by photolysis in about 3,500 years.[4] The hydroxyl radicals (OH) produced from the photolysis of water vapor, together with the other odd hydrogen species (e.g. H, HO2), can convert carbon monoxide (CO) back to CO2. The reaction cycle can be described as:[82][83]

CO + OH ⟶ CO2 + H
H + O2 + M ⟶ HO2 + M
HO2 + O ⟶ OH + O2
Net: CO + O ⟶ CO2

Mixing also plays a role in regenerating CO2 by bringing the O, CO, and O2 in the upper atmosphere downward.[4] The balance between photolysis and redox production keeps the average concentration of CO2 stable in the modern Martian atmosphere.

CO2 ice clouds can form in winter polar regions and at very high altitudes (>50 km) in tropical regions, where the air temperature is lower than the frost point of CO2.[2][84][85]

Nitrogen

[edit]

N2 is the second most abundant gas in the Martian atmosphere. It has a mean volume ratio of 2.6%.[3] Various measurements showed that the Martian atmosphere is enriched in 15N.[86][35] The enrichment of heavy isotopes of nitrogen is possibly caused by mass-selective escape processes.[87]

Argon isotope ratios are a signature of atmospheric loss on Mars.[88][89]

Argon

[edit]

Argon is the third most abundant gas in the Martian atmosphere. It has a mean volume ratio of 1.9%.[3] In terms of stable isotopes, Mars is enriched in 38Ar relative to 36Ar, which can be attributed to hydrodynamic escape.

One of Argon's isotopes, 40Ar, is produced from the radioactive decay of 40K. In contrast, 36Ar is primordial: It was present in the atmosphere after the formation of Mars. Observations indicate that Mars is enriched in 40Ar relative to 36Ar, which cannot be attributed to mass-selective loss processes.[29] A possible explanation for the enrichment is that a significant amount of primordial atmosphere, including 36Ar, was lost by impact erosion in the early history of Mars, while 40Ar was emitted to the atmosphere after the impact.[29][4]

Seasonal variations of oxygen at Gale crater

Oxygen and ozone

[edit]

The estimated mean volume ratio of molecular oxygen (O2) in the Martian atmosphere is 0.174%.[3] It is one of the products of the photolysis of CO2, water vapor, and ozone (O3). It can react with atomic oxygen (O) to re-form ozone (O3). In 2010, the Herschel Space Observatory detected molecular oxygen in the Martian atmosphere.[90]

Atomic oxygen is produced by photolysis of CO2 in the upper atmosphere and can escape the atmosphere via dissociative recombination or ion pickup. In early 2016, Stratospheric Observatory for Infrared Astronomy (SOFIA) detected atomic oxygen in the atmosphere of Mars, which has not been found since the Viking and Mariner mission in the 1970s.[91]

In 2019, NASA scientists working on the Curiosity rover mission, who have been taking measurements of the gas, discovered that the amount of oxygen in the Martian atmosphere rose by 30% in spring and summer.[92]

Similar to stratospheric ozone in Earth's atmosphere, the ozone present in the Martian atmosphere can be destroyed by catalytic cycles involving odd hydrogen species:

H + O3 ⟶ OH + O2
O + OH ⟶ H + O2
Net: O + O3 ⟶  2O2

Since water is an important source of these odd hydrogen species, higher abundance of ozone is usually observed in the regions with lower water vapor content.[93] Measurements showed that the total column of ozone can reach 2–30 μm-atm around the poles in winter and spring, where the air is cold and has low water saturation ratio.[94] The actual reactions between ozone and odd hydrogen species may be further complicated by the heterogeneous reactions that take place in water-ice clouds.[95]

It is thought that the vertical distribution and seasonality of ozone in the Martian atmosphere is driven by the complex interactions between chemistry and transport of oxygen-rich air from sunlit latitudes to the poles.[96][97] The UV/IR spectrometer on Mars Express (SPICAM) has shown the presence of two distinct ozone layers at low-to-mid latitudes. These comprise a persistent, near-surface layer below an altitude of 30 km (19 mi), a separate layer that is only present in northern spring and summer with an altitude varying from 30 to 60 km, and another separate layer that exists 40–60 km above the southern pole in winter, with no counterpart above the Mars's north pole.[98] This third ozone layer shows an abrupt decrease in elevation between 75 and 50 degrees south. SPICAM detected a gradual increase in ozone concentration at 50 km (31 mi) until midwinter, after which it slowly decreased to very low concentrations, with no layer detectable above 35 km (22 mi).[96]

Water vapor

[edit]
See also: Water on Mars and Martian polar ice caps
Clouds captured by NASA's Curiosity rover

Water vapor is a trace gas in the Martian atmosphere and has huge spatial, diurnal and seasonal variability.[99][100] Measurements made by Viking orbiter in the late 1970s suggested that the entire global total mass of water vapor is equivalent to about 1 to 2 km3 of ice.[101] More recent measurements by Mars Express orbiter showed that the globally annually-averaged column abundance of water vapor is about 10–20 precipitable microns (pr. μm).[102][103] Maximum abundance of water vapor (50-70 pr. μm) is found in the northern polar regions in early summer due to the sublimation of water ice in the polar cap.[102]

Unlike in Earth's atmosphere, liquid-water clouds cannot exist in the Martian atmosphere; this is because of the low atmospheric pressure. Cirrus-like water-ice clouds have been observed by the cameras on Opportunity rover and Phoenix lander.[104][105] Measurements made by the Phoenix lander showed that water-ice clouds can form at the top of the planetary boundary layer at night and precipitate back to the surface as ice crystals in the northern polar region.[100][106]

Precipitated water ice covering the Martian plain Utopia Planitia, the water ice precipitated by adhering to dry ice (observed by the Viking 2 lander)

Methane

[edit]
Main article: Methane on Mars

As a volcanic and biogenic species, methane is of interest to geologists and astrobiologists.[21] However, methane is chemically unstable in an oxidizing atmosphere with UV radiation. The lifetime of methane in the Martian atmosphere is about 400 years.[107] The detection of methane in a planetary atmosphere may indicate the presence of recent geological activities or living organisms.[21][108][109][107] Since 2004, trace amounts of methane (range from 60 ppb to under detection limit (< 0.05 ppb)) have been reported in various missions and observational studies.[110][111][112][113][114][115][116][117][118][16] The source of methane on Mars and the explanation for the enormous discrepancy in the observed methane concentrations are still under active debate.[22][21][107]

See also the section "detection of methane" for more details.

Sulfur dioxide

[edit]

Sulfur dioxide (SO2) in the atmosphere would be an indicator of current volcanic activity. It has become especially interesting due to the long-standing controversy of methane on Mars. If volcanoes have been active in recent Martian history, it would be expected to find SO2 together with methane in the current Martian atmosphere.[119][120] No SO2 has been detected in the atmosphere, with a sensitivity upper limit set at 0.2 ppb.[121][122] However, a team led by scientists at NASA Goddard Space Flight Center reported detection of SO2 in Rocknest soil samples analyzed by the Curiosity rover in March 2013.[123]

Other trace gases

[edit]

Carbon monoxide (CO) is produced by the photolysis of CO2 and quickly reacts with the oxidants in the Martian atmosphere to re-form CO2. The estimated mean volume ratio of CO in the Martian atmosphere is 0.0747%.[3]

Noble gases, other than helium and argon, are present at trace levels (neon at 2.5 ppmv, krypton at 0.3 ppmv and xenon at 0.08 ppmv[5]) in the Martian atmosphere. The concentration of helium, neon, krypton and xenon in the Martian atmosphere has been measured by different missions.[124][125][126][31] The isotopic ratios of noble gases reveal information about the early geological activities on Mars and the evolution of its atmosphere.[124][31][127]

Molecular hydrogen (H2) is produced by the reaction between odd hydrogen species in the middle atmosphere. It can be delivered to the upper atmosphere by mixing or diffusion, decompose to atomic hydrogen (H) by solar radiation and escape the Martian atmosphere.[128] Photochemical modeling estimated that the mixing ratio of H2 in the lower atmosphere is about 15 ±5 ppmv.[128]

Vertical structure

[edit]
The vertical structure of the atmosphere of Mars overlying with temperature profiles retrieved from the entry probes of Mars landers. Data source: NASA Planetary Data System

The vertical temperature structure of the Martian atmosphere differs from Earth's atmosphere in many ways. Information about the vertical structure is usually inferred by using the observations from thermal infrared soundings, radio occultation, aerobraking, landers' entry profiles.[129][130] Mars's atmosphere can be classified into three layers according to the average temperature profile:

  • Troposphere (≈0–40 km): The layer where most of the weather phenomena (e.g. convection and dust storms) take place. Its dynamics is heavily driven by the daytime surface heating and the amount of suspended dust. Mars has a higher scale height of 11.1 km than Earth (8.5 km) because of its weaker gravity.[5] The theoretical dry adiabatic lapse rate of Mars is 4.3 °C km−1,[131] but the measured average lapse rate is about 2.5 °C km−1 because the suspended dust particles absorb solar radiation and heat the air.[2] The planetary boundary layer can extend to over 10 km thick during the daytime.[2][132] The near-surface diurnal temperature range is huge (60 °C[131]) due to the low thermal inertia. Under dusty conditions, the suspended dust particles can reduce the surface diurnal temperature range to only 5 °C.[133] The temperature above 15 km is controlled by radiative processes instead of convection.[2] Mars is also a rare exception to the "0.1-bar tropopause" rule found in the other atmospheres in our solar system.[134]
  • Mesosphere (≈40–100 km): The layer that has the lowest temperature. CO2 in the mesosphere acts as a cooling agent by efficiently radiating heat into space. Stellar occultation observations show that the mesopause of Mars locates at about 100 km (around 0.01 to 0.001 Pa level) and has a temperature of 100–120 K.[135] The temperature can sometimes be lower than the frost point of CO2, and detections of CO2 ice clouds in the Martian mesosphere have been reported.[84][85]
  • Thermosphere (≈100–230 km): The layer is mainly controlled by extreme UV heating. The temperature of the Martian thermosphere increases with altitude and varies by season. The daytime temperature of the upper thermosphere ranges from 175 K (at aphelion) to 240 K (at perihelion) and can reach up to 390 K,[136][137] but it is still significantly lower than the temperature of Earth's thermosphere. The higher concentration of CO2 in the Martian thermosphere may explain part of the discrepancy because of the cooling effects of CO2 in high altitude. It is thought that auroral heating processes is not important in the Martian thermosphere because of the absence of a strong magnetic field in Mars, but the MAVEN orbiter has detected several aurora events.[138][139]

Mars does not have a persistent stratosphere due to the lack of shortwave-absorbing species in its middle atmosphere (e.g. stratospheric ozone in Earth's atmosphere and organic haze in Jupiter's atmosphere) for creating a temperature inversion.[140] However, a seasonal ozone layer and a strong temperature inversion in the middle atmosphere have been observed over the Martian south pole.[97][141] The altitude of the turbopause of Mars varies greatly from 60 to 140 km, and the variability is driven by the CO2 density in the lower thermosphere.[142] Mars also has a complicated ionosphere that interacts with the solar wind particles, extreme UV radiation and X-rays from Sun, and the magnetic field of its crust.[143][144] The exosphere of Mars starts at about 230 km and gradually merges with interplanetary space.[2]

The solar wind accelerates ions from Mars' upper atmosphere into space
(video (01:13); 5 November 2015)

Atmospheric dust and other dynamic features

[edit]

Atmospheric dust

[edit]
See also: mineral dust and Martian soil § Atmospheric dust

Under sufficiently strong wind (> 30 ms−1), dust particles can be mobilized and lifted from the surface to the atmosphere.[2][4] Some of the dust particles can be suspended in the atmosphere and travel by circulation before falling back to the ground.[14] Dust particles can attenuate solar radiation and interact with infrared radiation, which can lead to a significant radiative effect on Mars. Orbiter measurements suggest that the globally-averaged dust optical depth has a background level of 0.15 and peaks in the perihelion season (southern spring and summer).[145] The local abundance of dust varies greatly by seasons and years.[145][146] During global dust events, Mars surface assets can observe optical depth that is over 4.[147][148] Surface measurements also showed the effective radius of dust particles ranges from 0.6 μm to 2 μm and has considerable seasonality.[148][149][150]

Dust has an uneven vertical distribution on Mars. Apart from the planetary boundary layer, sounding data showed that there are other peaks of dust mixing ratio at the higher altitude (e.g. 15–30 km above the surface).[151][152][14]

Seasonal variations in oxygen and methane at Gale crater

Dust storms

[edit]
Further information: Climate of Mars § Dust storms, and Dust storms § On Mars
Difference of dust and water clouds: the orange cloud at the center of the image is a large dust cloud, the other white polar clouds are water clouds.
Detail of a Martian dust storm, as viewed from orbit
A 700 kilometer long dust storm front (marked by the red arrow) as viewed from orbit at different angles. The red circle of Martian terrain is just for orientation.
Mars without a dust storm in June 2001 (on left) and with a global dust storm in July 2001 (on right), as seen by Mars Global Surveyor

Local and regional dust storms are not rare on Mars.[14][2] Local storms have a size of about 103 km2 and occurrence of about 2000 events per Martian year, while regional storms of 106 km2 large are observed frequently in southern spring and summer.[2] Near the polar cap, dust storms sometimes can be generated by frontal activities and extra-tropical cyclones.[153][14]

Global dust storms (area > 106 km2 ) occur on average once every 3 Martian years.[4] Observations showed that larger dust storms are usually the result of merging smaller dust storms,[11][15] but the growth mechanism of the storm and the role of atmospheric feedbacks are still not well understood.[15][14] Although it is thought that Martian dust can be entrained into the atmosphere by processes similar to Earth's (e.g. saltation), the actual mechanisms are yet to be verified, and electrostatic or magnetic forces may also play in modulating dust emission.[14] Researchers reported that the largest single source of dust on Mars comes from the Medusae Fossae Formation.[154]

Main article: 2018 Mars global dust storm

On 1 June 2018, NASA scientists detected signs of a dust storm (see image) on Mars which resulted in the end of the solar-powered Opportunity rover's mission since the dust blocked the sunlight (see image) needed to operate. By 12 June, the storm was the most extensive recorded at the surface of the planet, and spanned an area about the size of North America and Russia combined (about a quarter of the planet). By 13 June, Opportunity rover began experiencing serious communication problems due to the dust storm.[155][156][157][158][159]

Mars dust storm – optical depth tau – May to September 2018
(Mars Climate Sounder; Mars Reconnaissance Orbiter)
(1:38; animation; 30 October 2018; file description)

Dust devils

[edit]
Main article: Martian dust devils
A small dust devil on Mars – viewed by the Curiosity rover – (August 9, 2020)

Dust devils are common on Mars.[160][14] Like their counterparts on Earth, dust devils form when the convective vortices driven by strong surface heating are loaded with dust particles.[161][162] Dust devils on Mars usually have a diameter of tens of meters and height of several kilometers, which are much taller than the ones observed on Earth.[2][162] Study of dust devils' tracks showed that most of Martian dust devils occur at around 60°N and 60°S in spring and summer.[160] They lift about 2.3 × 1011 kg of dust from land surface to atmosphere annually, which is comparable to the contribution from local and regional dust storms.[160]

Wind modification of the surface

[edit]

On Mars, the near-surface wind is not only emitting dust but also modifying the geomorphology of Mars over long time scales. Although it was thought that the atmosphere of Mars is too thin for mobilizing the sandy features, observations made by HiRSE showed that the migration of dunes is not rare on Mars.[163][164][165] The global average migration rate of dunes (2 – 120 m tall) is about 0.5 meter per year.[165] Atmospheric circulation models suggested repeated cycles of wind erosion and dust deposition can lead, possibly, to a net transport of soil materials from the lowlands to the uplands on geological timescales.[4]

Movement of sandy features in Nili Patera dune field on Mars detected by HiRISE. Photo credit: NASA/JPL Caltech/U. Arizona/JHU-APL

Thermal tides

[edit]
See also: Atmospheric tide

Solar heating on the day side and radiative cooling on the night side of a planet can induce pressure difference.[166] Thermal tides, which are the wind circulation and waves driven by such a daily-varying pressure field, can explain a lot of variability of the Martian atmosphere.[167] Compared to Earth's atmosphere, thermal tides have a larger influence on the Martian atmosphere because of the stronger diurnal temperature contrast.[168] The surface pressure measured by Mars rovers showed clear signals of thermal tides, although the variation also depends on the shape of the planet's surface and the amount of suspended dust in the atmosphere.[169] The atmospheric waves can also travel vertically and affect the temperature and water-ice content in the middle atmosphere of Mars.[167]

Orographic clouds

[edit]
See also: Orographic lift § Associated clouds
Water-ice clouds formed in the vicinity of the Arsia Mons volcano. The image was taken on 21 September 2018, but similar cloud formation events had been observed in the same site before. Photo credit: ESA/DLR/FU Berlin

On Earth, mountain ranges sometimes force an air mass to rise and cool down. As a result, water vapor becomes saturated and clouds are formed during the lifting process.[170] On Mars, orbiters have observed a seasonally recurrent formation of huge water-ice clouds around the downwind side of the 20 km-high volcanoes Arsia Mons, which is likely caused by the same mechanism.[171][172]

Acoustic environment

[edit]
Mars sounds (Perseverance) (video; 1:29; 1 April 2022)

In April 2022, scientists reported, for the first time, studies of sound waves on Mars. These studies were based on measurements by instruments on the Perseverance rover. The scientists found that the speed of sound is slower in the thin Martian atmosphere than on Earth. The speed of sound on Mars, within the audible bandwidth between 20 Hz – 20 kHz, varies depending on pitch, seemingly due to the low pressure and thermal turbulence of Martian surface air; and, as a result of these conditions, sound is much quieter, and live music would be more variable, than on Earth.[173][174][175]

Unexplained phenomena

[edit]

Detection of methane

[edit]
Main article: Methane on Mars

Methane (CH4) is chemically unstable in the current oxidizing atmosphere of Mars. It would quickly break down due to ultraviolet radiation from the Sun and chemical reactions with other gases. Therefore, a persistent presence of methane in the atmosphere may imply the existence of a source to continually replenish the gas.

The ESA-Roscomos Trace Gas Orbiter, which has made the most sensitive measurements of methane in Mars' atmosphere with over 100 global soundings, has found no methane to a detection limit of 0.05 parts per billion (ppb).[16][17][18] However, there have been other reports of detection of methane by ground-based telescopes and Curiosity rover. Trace amounts of methane, at the level of several ppb, were first reported in Mars's atmosphere by a team at the NASA Goddard Space Flight Center in 2003.[176][177] Large differences in the abundances were measured between observations taken in 2003 and 2006, which suggested that the methane was locally concentrated and probably seasonal.[178]

In 2014, NASA reported that the Curiosity rover detected a tenfold increase ('spike') in methane in the atmosphere around it in late 2013 and early 2014. Four measurements taken over two months in this period averaged 7.2 ppb, implying that Mars is episodically producing or releasing methane from an unknown source.[116] Before and after that, readings averaged around one-tenth that level.[179][180][116] On 7 June 2018, NASA announced a cyclical seasonal variation in the background level of atmospheric methane.[181][20][182]

Curiosity detected a cyclical seasonal variation in atmospheric methane.

The principal candidates for the origin of Mars' methane include non-biological processes such as water-rock reactions, radiolysis of water, and pyrite formation, all of which produce H2 that could then generate methane and other hydrocarbons via Fischer–Tropsch synthesis with CO and CO2.[183] It has also been shown that methane could be produced by a process involving water, carbon dioxide, and the mineral olivine, which is known to be common on Mars.[184] Living microorganisms, such as methanogens, are another possible source, but no evidence for the presence of such organisms has been found on Mars.[185][186][111] There are some suspicions about the detection of methane, which suggests that it may instead be caused by the undocumented terrestrial contamination from the rovers or a misinterpretation of measurement raw data.[22][187]

Lightning events

[edit]

In 2009, an Earth-based observational study reported detection of large-scale electric discharge events on Mars and proposed that they are related to lightning discharge in Martian dust storms.[188] However, later observation studies showed that the result is not reproducible using the radar receiver on Mars Express and the Earth-based Allen Telescope Array.[189][190][191] A laboratory study showed that the air pressure on Mars is not favorable for charging the dust grains, and thus it is difficult to generate lightning in Martian atmosphere.[192][191]

Super-rotating jet over the equator

[edit]

Super-rotation refers to the phenomenon that atmospheric mass has a higher angular velocity than the surface of the planet at the equator, which in principle cannot be driven by inviscid axisymmetric circulations.[193][194] Assimilated data and general circulation model (GCM) simulation suggest that super-rotating jet can be found in Martian atmosphere during global dust storms, but it is much weaker than the ones observed on slow-rotating planets like Venus and Titan.[153] GCM experiments showed that the thermal tides can play a role in inducing the super-rotating jet.[195] Nevertheless, modeling super-rotation still remains as a challenging topic for planetary scientists.[194]

History of atmospheric observations

[edit]
Main article: History of Mars observation

In 1784, German-born British astronomer William Herschel published an article about his observations of the Martian atmosphere in Philosophical Transactions and noted the occasional movement of a brighter region on Mars, which he attributed to clouds and vapors.[168][196] In 1809, French astronomer Honoré Flaugergues wrote about his observation of "yellow clouds" on Mars, which are likely to be dust storm events.[168] In 1864, William Rutter Dawes observed that "the ruddy tint of the planet does not arise from any peculiarity of its atmosphere; it seems to be fully proved by the fact that the redness is always deepest near the centre, where the atmosphere is thinnest."[197] Spectroscopic observations in the 1860s and 1870s[198] led many to think the atmosphere of Mars is similar to Earth's. In 1894, though, spectral analysis and other qualitative observations by William Wallace Campbell suggested Mars resembles the Moon, which has no appreciable atmosphere, in many respects.[198] In 1926, photographic observations by William Hammond Wright at the Lick Observatory allowed Donald Howard Menzel to discover quantitative evidence of Mars's atmosphere.[199][200]

With an enhanced understanding of optical properties of atmospheric gases and advancement in spectrometer technology, scientists started to measure the composition of the Martian atmosphere in the mid-20th century. Lewis David Kaplan and his team detected the signals of water vapor and carbon dioxide in the spectrogram of Mars in 1964,[201] as well as carbon monoxide in 1969.[202] In 1965, the measurements made during Mariner 4's flyby confirmed that the Martian atmosphere is constituted mostly of carbon dioxide, and the surface pressure is about 400 to 700 Pa.[203] After the composition of the Martian atmosphere was known, astrobiological research began on Earth to determine the viability of life on Mars. Containers that simulated environmental conditions on Mars, called "Mars jars", were developed for this purpose.[204]

In 1976, two landers of the Viking program provided the first ever in-situ measurements of the composition of the Martian atmosphere. Another objective of the mission included investigations for evidence of past or present life on Mars (see Viking lander biological experiments).[205] Since then, many orbiters and landers have been sent to Mars to measure different properties of the Martian atmosphere, such as concentration of trace gases and isotopic ratios. In addition, telescopic observations and analysis of Martian meteorites provide independent sources of information to verify the findings. The imageries and measurements made by these spacecraft greatly improve our understanding of the atmospheric processes outside Earth. The rover Curiosity and the lander InSight are still operating on the surface of Mars to carry out experiments and report the local daily weather.[206][207] The rover Perseverance and helicopter Ingenuity, which formed the Mars 2020 program, landed in February 2021. The rover Rosalind Franklin is scheduled to launch in 2028.

Potential for use by humans

[edit]
Main articles: In-situ resource utilization, Terraforming of Mars, and Colonization of Mars

The atmosphere of Mars is a resource of known composition available at any landing site on Mars. It has been proposed that human exploration of Mars could use carbon dioxide (CO2) from the Martian atmosphere to make methane (CH4) and use it as rocket fuel for the return mission. Mission studies that propose using the atmosphere in this way include the Mars Direct proposal of Robert Zubrin and the NASA Design Reference Mission study. Two major chemical pathways for use of the carbon dioxide are the Sabatier reaction, converting atmospheric carbon dioxide along with additional hydrogen (H2) to produce methane (CH4) and oxygen (O2), and electrolysis, using a zirconia solid oxide electrolyte to split the carbon dioxide into oxygen (O2) and carbon monoxide (CO).[208]

In 2021, the NASA rover Perseverance was able to make oxygen on Mars. The process is complex and takes a lot of time to produce a small amount of oxygen.[209]

[edit]
Martian sky with clouds at sunset, viewed by InSight
Polar ice cap with the depth of the atmosphere, as well as a large orographic cloud visible at the horizon over Olympus Mons
Martian atmosphere with cloud cover over Solis Planum
Cloud cover over Tempe Terra
Cloud cover over Charitum Montes
Martian sunset by Spirit rover at Gusev crater (May, 2005).
Martian sunset by Pathfinder at Ares Vallis (July, 1997).

See also

[edit]

References

[edit]
  1. ^ "Mars Fact Sheet". NASA. Archived from the original on 23 August 2021. Retrieved 2 December 2020.
  2. ^ a b c d e f g h i j k l m n o p Haberle, R. M. (1 January 2015), "SOLAR SYSTEM/SUN, ATMOSPHERES, EVOLUTION OF ATMOSPHERES | Planetary Atmospheres: Mars", in North, Gerald R.; Pyle, John; Zhang, Fuqing (eds.), Encyclopedia of Atmospheric Sciences (Second Edition), Academic Press, pp. 168–177, doi:10.1016/b978-0-12-382225-3.00312-1, ISBN 9780123822253
  3. ^ a b c d e f g h Franz, Heather B.; Trainer, Melissa G.; Malespin, Charles A.; Mahaffy, Paul R.; Atreya, Sushil K.; Becker, Richard H.; Benna, Mehdi; Conrad, Pamela G.; Eigenbrode, Jennifer L. (1 April 2017). "Initial SAM calibration gas experiments on Mars: Quadrupole mass spectrometer results and implications". Planetary and Space Science. 138: 44–54. Bibcode:2017P&SS..138...44F. doi:10.1016/j.pss.2017.01.014. ISSN 0032-0633.
  4. ^ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad Catling, David C. (2017). Atmospheric evolution on inhabited and lifeless worlds. Kasting, James F. Cambridge: Cambridge University Press. Bibcode:2017aeil.book.....C. ISBN 9780521844123. OCLC 956434982.
  5. ^ a b c "Mars Fact Sheet". nssdc.gsfc.nasa.gov. Archived from the original on 23 August 2021. Retrieved 13 June 2019.
  6. ^ "Weather, Weather, Everywhere?". Solar System Exploration. Archived from the original on 14 April 2009. Retrieved 21 September 2021.
  7. ^ "Mars Fact Sheet". Archived from the original on 23 August 2021. Retrieved 17 January 2018.
  8. ^ Jakosky, B. M.; Brain, D.; Chaffin, M.; Curry, S.; Deighan, J.; Grebowsky, J.; Halekas, J.; Leblanc, F.; Lillis, R. (15 November 2018). "Loss of the Martian atmosphere to space: Present-day loss rates determined from MAVEN observations and integrated loss through time". Icarus. 315: 146–157. Bibcode:2018Icar..315..146J. doi:10.1016/j.icarus.2018.05.030. ISSN 0019-1035. S2CID 125410604.
  9. ^ mars.nasa.gov. "NASA's MAVEN Reveals Most of Mars' Atmosphere Was Lost to Space". NASA's Mars Exploration Program. Archived from the original on 17 August 2020. Retrieved 11 June 2019.
  10. ^ "Temperature extremes on Mars". phys.org. Archived from the original on 2 December 2020. Retrieved 13 June 2019.
  11. ^ a b c Hille, Karl (18 September 2015). "The Fact and Fiction of Martian Dust Storms". NASA. Archived from the original on 2 March 2016. Retrieved 11 June 2019.
  12. ^ https://skyandtelescope.org/astronomy-news/is-the-mars-opposition-already-over/[Normally reddish-orange or even pink, Mars now glows pumpkin-orange. Even my eyes can see the difference. ALPO assistant coordinator Richard Schmude has also noted an increase in brightness of ≈0.2 magnitude concurrent with the color change.]
  13. ^ Greicius, Tony (8 June 2018). "Opportunity Hunkers Down During Dust Storm". NASA. Archived from the original on 30 November 2020. Retrieved 13 June 2019.
  14. ^ a b c d e f g h Kok, Jasper F; Parteli, Eric J R; Michaels, Timothy I; Karam, Diana Bou (14 September 2012). "The physics of wind-blown sand and dust". Reports on Progress in Physics. 75 (10): 106901. arXiv:1201.4353. Bibcode:2012RPPh...75j6901K. doi:10.1088/0034-4885/75/10/106901. ISSN 0034-4885. PMID 22982806. S2CID 206021236.
  15. ^ a b c Toigo, Anthony D.; Richardson, Mark I.; Wang, Huiqun; Guzewich, Scott D.; Newman, Claire E. (1 March 2018). "The cascade from local to global dust storms on Mars: Temporal and spatial thresholds on thermal and dynamical feedback". Icarus. 302: 514–536. Bibcode:2018Icar..302..514T. doi:10.1016/j.icarus.2017.11.032. ISSN 0019-1035.
  16. ^ a b c Vago, Jorge L.; Svedhem, Håkan; Zelenyi, Lev; Etiope, Giuseppe; Wilson, Colin F.; López-Moreno, Jose-Juan; Bellucci, Giancarlo; Patel, Manish R.; Neefs, Eddy (April 2019). "No detection of methane on Mars from early ExoMars Trace Gas Orbiter observations" (PDF). Nature. 568 (7753): 517–520. Bibcode:2019Natur.568..517K. doi:10.1038/s41586-019-1096-4. ISSN 1476-4687. PMID 30971829. S2CID 106411228. Archived (PDF) from the original on 27 September 2020. Retrieved 24 November 2019.
  17. ^ a b esa. "First results from the ExoMars Trace Gas Orbiter". European Space Agency. Archived from the original on 13 October 2019. Retrieved 12 June 2019.
  18. ^ a b Weule, Genelle (11 April 2019). "Mars methane mystery thickens as newest probe fails to find the gas". ABC News. Archived from the original on 7 November 2020. Retrieved 27 June 2019.
  19. ^ Formisano, Vittorio; Atreya, Sushil; Encrenaz, Thérèse; Ignatiev, Nikolai; Giuranna, Marco (3 December 2004). "Detection of Methane in the Atmosphere of Mars". Science. 306 (5702): 1758–1761. Bibcode:2004Sci...306.1758F. doi:10.1126/science.1101732. ISSN 0036-8075. PMID 15514118. S2CID 13533388.
  20. ^ a b Webster, Christopher R.; et al. (8 June 2018). "Background levels of methane in Mars' atmosphere show strong seasonal variations". Science. 360 (6393): 1093–1096. Bibcode:2018Sci...360.1093W. doi:10.1126/science.aaq0131. PMID 29880682.
  21. ^ a b c d e Yung, Yuk L.; Chen, Pin; Nealson, Kenneth; Atreya, Sushil; Beckett, Patrick; Blank, Jennifer G.; Ehlmann, Bethany; Eiler, John; Etiope, Giuseppe (19 September 2018). "Methane on Mars and Habitability: Challenges and Responses". Astrobiology. 18 (10): 1221–1242. Bibcode:2018AsBio..18.1221Y. doi:10.1089/ast.2018.1917. ISSN 1531-1074. PMC 6205098. PMID 30234380.
  22. ^ a b c Zahnle, Kevin; Freedman, Richard S.; Catling, David C. (1 April 2011). "Is there methane on Mars?". Icarus. 212 (2): 493–503. Bibcode:2011Icar..212..493Z. doi:10.1016/j.icarus.2010.11.027. ISSN 0019-1035. Archived from the original on 1 October 2020. Retrieved 4 July 2019.
  23. ^ a b c d Mahaffy, P.R.; Conrad, P.G.; MSL Science Team (1 February 2015). "Volatile and Isotopic Imprints of Ancient Mars". Elements. 11 (1): 51–56. Bibcode:2015Eleme..11...51M. doi:10.2113/gselements.11.1.51. ISSN 1811-5209.
  24. ^ a b Marty, Bernard (1 January 2012). "The origins and concentrations of water, carbon, nitrogen and noble gases on Earth". Earth and Planetary Science Letters. 313–314: 56–66. arXiv:1405.6336. Bibcode:2012E&PSL.313...56M. doi:10.1016/j.epsl.2011.10.040. ISSN 0012-821X. S2CID 41366698.
  25. ^ a b Henderson, Paul (2009). The Cambridge Handbook of Earth Science Data. Henderson, Gideon. Cambridge, UK: Cambridge University Press. ISBN 9780511580925. OCLC 435778559.
  26. ^ Wong, Michael H.; Atreya, Sushil K.; Mahaffy, Paul N.; Franz, Heather B.; Malespin, Charles; Trainer, Melissa G.; Stern, Jennifer C.; Conrad, Pamela G.; Manning, Heidi L.K. (16 December 2013). "Isotopes of nitrogen on Mars: Atmospheric measurements by Curiosity's mass spectrometer". Geophysical Research Letters. Mars atmospheric nitrogen isotopes. 40 (23): 6033–6037. Bibcode:2013GeoRL..40.6033W. doi:10.1002/2013GL057840. PMC 4459194. PMID 26074632.
  27. ^ Atreya, Sushil K.; Trainer, Melissa G.; Franz, Heather B.; Wong, Michael H.; Manning, Heidi L.K.; Malespin, Charles A.; Mahaffy, Paul R.; Conrad, Pamela G.; Brunner, Anna E. (2013). "Primordial argon isotope fractionation in the atmosphere of Mars measured by the SAM instrument on Curiosity and implications for atmospheric loss". Geophysical Research Letters. 40 (21): 5605–5609. Bibcode:2013GeoRL..40.5605A. doi:10.1002/2013GL057763. ISSN 1944-8007. PMC 4373143. PMID 25821261.
  28. ^ a b Lee, Jee-Yon; Marti, Kurt; Severinghaus, Jeffrey P.; Kawamura, Kenji; Yoo, Hee-Soo; Lee, Jin Bok; Kim, Jin Seog (1 September 2006). "A redetermination of the isotopic abundances of atmospheric Ar". Geochimica et Cosmochimica Acta. 70 (17): 4507–4512. Bibcode:2006GeCoA..70.4507L. doi:10.1016/j.gca.2006.06.1563. ISSN 0016-7037.
  29. ^ a b c Mahaffy, P.R.; Webster, C.R.; Atreya, S.K.; Franz, H.; Wong, M.; Conrad, P.G.; Harpold, D.; Jones, J.J.; Leshin, L.A. (19 July 2013). "Abundance and isotopic composition of gases in the Martian atmosphere from the Curiosity rover". Science. 341 (6143): 263–266. Bibcode:2013Sci...341..263M. doi:10.1126/science.1237966. ISSN 0036-8075. PMID 23869014. S2CID 206548973.
  30. ^ a b Pepin, Robert O. (1 July 1991). "On the origin and early evolution of terrestrial planet atmospheres and meteoritic volatiles". Icarus. 92 (1): 2–79. Bibcode:1991Icar...92....2P. doi:10.1016/0019-1035(91)90036-S. ISSN 0019-1035.
  31. ^ a b c Conrad, P. G.; Malespin, C. A.; Franz, H. B.; Pepin, R. O.; Trainer, M. G.; Schwenzer, S. P.; Atreya, S. K.; Freissinet, C.; Jones, J. H. (15 November 2016). "In situ measurement of atmospheric krypton and xenon on Mars with Mars Science Laboratory" (PDF). Earth and Planetary Science Letters. 454: 1–9. Bibcode:2016E&PSL.454....1C. doi:10.1016/j.epsl.2016.08.028. ISSN 0012-821X. OSTI 1417813. Archived (PDF) from the original on 19 July 2018. Retrieved 4 July 2019.
  32. ^ "Curiosity Sniffs Out History of Martian Atmosphere". NASA/JPL. Archived from the original on 28 July 2020. Retrieved 11 June 2019.
  33. ^ a b mars.nasa.gov. "NASA's MAVEN reveals most of Mars' atmosphere was lost to space". NASA's Mars Exploration Program. Archived from the original on 17 August 2020. Retrieved 11 June 2019.
  34. ^ Catling, David C.; Zahnle, Kevin J. (May 2009). "The planetary air leak" (PDF). Scientific American. p. 26. Archived (PDF) from the original on 26 October 2020. Retrieved 10 June 2019.
  35. ^ a b Avice, G.; Bekaert, D.V.; Chennaoui Aoudjehane, H.; Marty, B. (9 February 2018). "Noble gases and nitrogen in Tissint reveal the composition of the Mars atmosphere". Geochemical Perspectives Letters. 6: 11–16. doi:10.7185/geochemlet.1802.
  36. ^ McElroy, Michael B.; Yung, Yuk Ling; Nier, Alfred O. (1 October 1976). "Isotopic Composition of Nitrogen: Implications for the Past History of Mars' Atmosphere". Science. 194 (4260): 70–72. Bibcode:1976Sci...194...70M. doi:10.1126/science.194.4260.70. PMID 17793081. S2CID 34066697.
  37. ^ Hunten, Donald M.; Pepin, Robert O.; Walker, James C.G. (1 March 1987). "Mass fractionation in hydrodynamic escape". Icarus. 69 (3): 532–549. Bibcode:1987Icar...69..532H. doi:10.1016/0019-1035(87)90022-4. hdl:2027.42/26796. ISSN 0019-1035.
  38. ^ Hans Keppler; Shcheka, Svyatoslav S. (October 2012). "The origin of the terrestrial noble-gas signature". Nature. 490 (7421): 531–534. Bibcode:2012Natur.490..531S. doi:10.1038/nature11506. ISSN 1476-4687. PMID 23051754. S2CID 205230813.
  39. ^ Tian, Feng; Kasting, James F.; Solomon, Stanley C. (2009). "Thermal escape of carbon from the early Martian atmosphere". Geophysical Research Letters. 36 (2): n/a. Bibcode:2009GeoRL..36.2205T. doi:10.1029/2008GL036513. ISSN 1944-8007. S2CID 129208608.
  40. ^ Jakosky, B.M.; Slipski, M.; Benna, M.; Mahaffy, P.; Elrod, M.; Yelle, R.; Stone, S.; Alsaeed, N. (31 March 2017). "Mars' atmospheric history derived from upper-atmosphere measurements of 38Ar / 36Ar". Science. 355 (6332): 1408–1410. Bibcode:2017Sci...355.1408J. doi:10.1126/science.aai7721. ISSN 0036-8075. PMID 28360326.
  41. ^ a b Leblanc, F.; Martinez, A.; Chaufray, J. Y.; Modolo, R.; Hara, T.; Luhmann, J.; Lillis, R.; Curry, S.; McFadden, J. (2018). "On Mars's Atmospheric Sputtering After MAVEN's First Martian Year of Measurements" (PDF). Geophysical Research Letters. 45 (10): 4685–4691. Bibcode:2018GeoRL..45.4685L. doi:10.1002/2018GL077199. ISSN 1944-8007. S2CID 134561764.
  42. ^ Vickery, A.M.; Melosh, H.J. (April 1989). "Impact erosion of the primordial atmosphere of Mars". Nature. 338 (6215): 487–489. Bibcode:1989Natur.338..487M. doi:10.1038/338487a0. ISSN 1476-4687. PMID 11536608. S2CID 4285528.
  43. ^ Owen, Tobias; Bar-Nun, Akiva (1 August 1995). "Comets, impacts, and atmospheres". Icarus. 116 (2): 215–226. Bibcode:1995Icar..116..215O. doi:10.1006/icar.1995.1122. ISSN 0019-1035. PMID 11539473.
  44. ^ Krasnopolsky, Vladimir A. (2002). "Mars' upper atmosphere and ionosphere at low, medium, and high solar activities: Implications for evolution of water". Journal of Geophysical Research: Planets. 107 (E12): 11‑1–11‑11. Bibcode:2002JGRE..107.5128K. doi:10.1029/2001JE001809. ISSN 2156-2202.
  45. ^ Sagan, Carl (September 1977). "Reducing greenhouses and the temperature history of Earth and Mars". Nature. 269 (5625): 224–226. Bibcode:1977Natur.269..224S. doi:10.1038/269224a0. ISSN 1476-4687. S2CID 4216277.
  46. ^ Kasting, James F.; Freedman, Richard; Robinson, Tyler D.; Zugger, Michael E.; Kopparapu, Ravi; Ramirez, Ramses M. (January 2014). "Warming early Mars with CO2 and H2". Nature Geoscience. 7 (1): 59–63. arXiv:1405.6701. Bibcode:2014NatGe...7...59R. doi:10.1038/ngeo2000. ISSN 1752-0908. S2CID 118520121.
  47. ^ Batalha, Natasha; Domagal-Goldman, Shawn D.; Ramirez, Ramses; Kasting, James F. (15 September 2015). "Testing the early Mars H2–CO2 greenhouse hypothesis with a 1-D photochemical model". Icarus. 258: 337–349. arXiv:1507.02569. Bibcode:2015Icar..258..337B. doi:10.1016/j.icarus.2015.06.016. ISSN 0019-1035. S2CID 118359789.
  48. ^ Johnson, Sarah Stewart; Mischna, Michael A.; Grove, Timothy L.; Zuber, Maria T. (8 August 2008). "Sulfur-induced greenhouse warming on early Mars". Journal of Geophysical Research. 113 (E8): E08005. Bibcode:2008JGRE..113.8005J. doi:10.1029/2007JE002962. ISSN 0148-0227. S2CID 7525497.
  49. ^ Schrag, Daniel P.; Zuber, Maria T.; Halevy, Itay (21 December 2007). "A sulfur dioxide climate feedback on early Mars". Science. 318 (5858): 1903–1907. Bibcode:2007Sci...318.1903H. doi:10.1126/science.1147039. ISSN 0036-8075. PMID 18096802. S2CID 7246517.
  50. ^ "Sulfur dioxide may have helped maintain a warm early Mars". phys.org. Archived from the original on 8 June 2019. Retrieved 8 June 2019.
  51. ^ Anderson, Donald E. (1974). "Mariner 6, 7, and 9 Ultraviolet Spectrometer Experiment: Analysis of hydrogen Lyman alpha data". Journal of Geophysical Research. 79 (10): 1513–1518. Bibcode:1974JGR....79.1513A. doi:10.1029/JA079i010p01513. ISSN 2156-2202.
  52. ^ Chaufray, J.Y.; Bertaux, J.L.; Leblanc, F.; Quémerais, E. (June 2008). "Observation of the hydrogen corona with SPICAM on Mars Express". Icarus. 195 (2): 598–613. Bibcode:2008Icar..195..598C. doi:10.1016/j.icarus.2008.01.009.
  53. ^ Hunten, Donald M. (November 1973). "The Escape of Light Gases from Planetary Atmospheres". Journal of the Atmospheric Sciences. 30 (8): 1481–1494. Bibcode:1973JAtS...30.1481H. doi:10.1175/1520-0469(1973)030<1481:TEOLGF>2.0.CO;2. ISSN 0022-4928.
  54. ^ Zahnle, Kevin; Haberle, Robert M.; Catling, David C.; Kasting, James F. (2008). "Photochemical instability of the ancient Martian atmosphere". Journal of Geophysical Research: Planets. 113 (E11): E11004. Bibcode:2008JGRE..11311004Z. doi:10.1029/2008JE003160. ISSN 2156-2202. S2CID 2199349.
  55. ^ Bhattacharyya, D.; Clarke, J. T.; Chaufray, J. Y.; Mayyasi, M.; Bertaux, J. L.; Chaffin, M. S.; Schneider, N. M.; Villanueva, G. L. (2017). "Seasonal Changes in Hydrogen Escape From Mars Through Analysis of HST Observations of the Martian Exosphere Near Perihelion" (PDF). Journal of Geophysical Research: Space Physics. 122 (11): 11, 756–11, 764. Bibcode:2017JGRA..12211756B. doi:10.1002/2017JA024572. ISSN 2169-9402. S2CID 119084288. Archived (PDF) from the original on 5 November 2020. Retrieved 6 January 2021.
  56. ^ a b Schofield, John T.; Shirley, James H.; Piqueux, Sylvain; McCleese, Daniel J.; Paul O. Hayne; Kass, David M.; Halekas, Jasper S.; Chaffin, Michael S.; Kleinböhl, Armin (February 2018). "Hydrogen escape from Mars enhanced by deep convection in dust storms". Nature Astronomy. 2 (2): 126–132. Bibcode:2018NatAs...2..126H. doi:10.1038/s41550-017-0353-4. ISSN 2397-3366. S2CID 134961099.
  57. ^ Shekhtman, Svetlana (29 April 2019). "How Global Dust Storms Affect Martian Water, Winds, and Climate". NASA. Archived from the original on 17 June 2019. Retrieved 10 June 2019.
  58. ^ Nagy, Andrew F.; Liemohn, Michael W.; Fox, J. L.; Kim, Jhoon (2001). "Hot carbon densities in the exosphere of Mars". Journal of Geophysical Research: Space Physics. 106 (A10): 21565–21568. Bibcode:2001JGR...10621565N. doi:10.1029/2001JA000007. ISSN 2156-2202. Archived from the original on 28 July 2020. Retrieved 24 November 2019.
  59. ^ a b Gröller, H.; Lichtenegger, H.; Lammer, H.; Shematovich, V. I. (1 August 2014). "Hot oxygen and carbon escape from the martian atmosphere". Planetary and Space Science. Planetary evolution and life. 98: 93–105. arXiv:1911.01107. Bibcode:2014P&SS...98...93G. doi:10.1016/j.pss.2014.01.007. ISSN 0032-0633. S2CID 122599784.
  60. ^ a b c Fox, J. L. (1993). "The production and escape of nitrogen atoms on Mars". Journal of Geophysical Research: Planets. 98 (E2): 3297–3310. Bibcode:1993JGR....98.3297F. doi:10.1029/92JE02289. ISSN 2156-2202. Archived from the original on 21 July 2018. Retrieved 24 June 2019.
  61. ^ Mandt, Kathleen; Mousis, Olivier; Chassefière, Eric (July 2015). "Comparative planetology of the history of nitrogen isotopes in the atmospheres of Titan and Mars". Icarus. 254: 259–261. Bibcode:2015Icar..254..259M. doi:10.1016/j.icarus.2015.03.025. PMC 6527424. PMID 31118538.
  62. ^ Fox, J.L. (December 2007). "Comment on the papers "Production of hot nitrogen atoms in the martian thermosphere" by F. Bakalian and "Monte Carlo computations of the escape of atomic nitrogen from Mars" by F. Bakalian and R.E. Hartle". Icarus. 192 (1): 296–301. Bibcode:2007Icar..192..296F. doi:10.1016/j.icarus.2007.05.022.
  63. ^ Feldman, Paul D.; Steffl, Andrew J.; Parker, Joel Wm.; A'Hearn, Michael F.; Bertaux, Jean-Loup; Alan Stern, S.; Weaver, Harold A.; Slater, David C.; Versteeg, Maarten (1 August 2011). "Rosetta-Alice observations of exospheric hydrogen and oxygen on Mars". Icarus. 214 (2): 394–399. arXiv:1106.3926. Bibcode:2011Icar..214..394F. doi:10.1016/j.icarus.2011.06.013. ISSN 0019-1035. S2CID 118646223.
  64. ^ Lammer, H.; Lichtenegger, H.I.M.; Kolb, C.; Ribas, I.; Guinan, E.F.; Abart, R.; Bauer, S.J. (September 2003). "Loss of water from Mars". Icarus. 165 (1): 9–25. doi:10.1016/S0019-1035(03)00170-2.
  65. ^ Valeille, Arnaud; Bougher, Stephen W.; Tenishev, Valeriy; Combi, Michael R.; Nagy, Andrew F. (1 March 2010). "Water loss and evolution of the upper atmosphere and exosphere over martian history". Icarus. Solar Wind Interactions with Mars. 206 (1): 28–39. Bibcode:2010Icar..206...28V. doi:10.1016/j.icarus.2009.04.036. ISSN 0019-1035.
  66. ^ Jones, Nancy; Steigerwald, Bill; Brown, Dwayne; Webster, Guy (14 October 2014). "NASA Mission Provides Its First Look at Martian Upper Atmosphere". NASA. Archived from the original on 19 October 2014. Retrieved 15 October 2014.
  67. ^ Ramstad, Robin; Brain, David A.; Dong, Yaxue; Espley, Jared; Halekas, Jasper; Jakosky, Bruce (October 2020). "The global current systems of the Martian induced magnetosphere". Nature Astronomy. 4 (10): 979–985. doi:10.1038/s41550-020-1099-y. ISSN 2397-3366.
  68. ^ Ramstad, Robin; Barabash, Stas; Futaana, Yoshifumi; Nilsson, Hans; Holmström, Mats (November 2018). "Ion Escape From Mars Through Time: An Extrapolation of Atmospheric Loss Based on 10 Years of Mars Express Measurements". Journal of Geophysical Research: Planets. 123 (11): 3051–3060. doi:10.1029/2018JE005727. ISSN 2169-9097.
  69. ^ "Seasons on Mars". www.msss.com. Archived from the original on 3 November 2020. Retrieved 7 June 2019.
  70. ^ Soto, Alejandro; Mischna, Michael; Schneider, Tapio; Lee, Christopher; Richardson, Mark (1 April 2015). "Martian atmospheric collapse: Idealized GCM studies" (PDF). Icarus. 250: 553–569. Bibcode:2015Icar..250..553S. doi:10.1016/j.icarus.2014.11.028. ISSN 0019-1035. Archived (PDF) from the original on 15 August 2017. Retrieved 30 August 2020.
  71. ^ Hess, Seymour L.; Henry, Robert M.; Tillman, James E. (1979). "The seasonal variation of atmospheric pressure on Mars as affected by the south polar cap". Journal of Geophysical Research. 84 (B6): 2923. Bibcode:1979JGR....84.2923H. doi:10.1029/JB084iB06p02923. ISSN 0148-0227.
  72. ^ Hess, S. L.; Ryan, J. A.; Tillman, J. E.; Henry, R. M.; Leovy, C. B. (March 1980). "The annual cycle of pressure on Mars measured by Viking Landers 1 and 2". Geophysical Research Letters. 7 (3): 197–200. Bibcode:1980GeoRL...7..197H. doi:10.1029/GL007i003p00197.
  73. ^ Ordonez-Etxeberria, Iñaki; Hueso, Ricardo; Sánchez-Lavega, Agustín; Millour, Ehouarn; Forget, Francois (January 2019). "Meteorological pressure at Gale crater from a comparison of REMS/MSL data and MCD modelling: Effect of dust storms". Icarus. 317: 591–609. Bibcode:2019Icar..317..591O. doi:10.1016/j.icarus.2018.09.003. S2CID 125851495.
  74. ^ Guzewich, Scott D.; Newman, C.E.; de la Torre Juárez, M.; Wilson, R.J.; Lemmon, M.; Smith, M.D.; Kahanpää, H.; Harri, A.-M. (April 2016). "Atmospheric tides in Gale Crater, Mars". Icarus. 268: 37–49. Bibcode:2016Icar..268...37G. doi:10.1016/j.icarus.2015.12.028.
  75. ^ Haberle, Robert M.; Juárez, Manuel de la Torre; Kahre, Melinda A.; Kass, David M.; Barnes, Jeffrey R.; Hollingsworth, Jeffery L.; Harri, Ari-Matti; Kahanpää, Henrik (June 2018). "Detection of Northern Hemisphere transient eddies at Gale Crater Mars". Icarus. 307: 150–160. Bibcode:2018Icar..307..150H. doi:10.1016/j.icarus.2018.02.013. S2CID 92991001.
  76. ^ a b Fanale, F. P.; Cannon, W. A. (April 1971). "Adsorption on the Martian Regolith". Nature. 230 (5295): 502–504. Bibcode:1971Natur.230..502F. doi:10.1038/230502a0. ISSN 0028-0836. S2CID 4263086.
  77. ^ a b Zent, Aaron P.; Quinn, Richard C. (1995). "Simultaneous adsorption of CO 2 and H 2 O under Mars-like conditions and application to the evolution of the Martian climate". Journal of Geophysical Research. 100 (E3): 5341. Bibcode:1995JGR...100.5341Z. doi:10.1029/94JE01899. hdl:2060/19940030969. ISSN 0148-0227. S2CID 129616949.
  78. ^ Moores, John E.; Gough, Raina V.; Martinez, German M.; Meslin, Pierre-Yves; Smith, Christina L.; Atreya, Sushil K.; Mahaffy, Paul R.; Newman, Claire E.; Webster, Christopher R. (May 2019). "Methane seasonal cycle at Gale Crater on Mars consistent with regolith adsorption and diffusion". Nature Geoscience. 12 (5): 321–325. Bibcode:2019NatGe..12..321M. doi:10.1038/s41561-019-0313-y. ISSN 1752-0894. S2CID 135136911.
  79. ^ Meslin, P.-Y.; Gough, R.; Lefèvre, F.; Forget, F. (February 2011). "Little variability of methane on Mars induced by adsorption in the regolith". Planetary and Space Science. 59 (2–3): 247–258. Bibcode:2011P&SS...59..247M. doi:10.1016/j.pss.2010.09.022.
  80. ^ "Greenhouse effects ... also on other planets". European Space Agency. Archived from the original on 29 September 2019. Retrieved 7 June 2019.
  81. ^ Yung, Yuk L.; Kirschvink, Joseph L.; Pahlevan, Kaveh; Li, King-Fai (16 June 2009). "Atmospheric pressure as a natural climate regulator for a terrestrial planet with a biosphere". Proceedings of the National Academy of Sciences. 106 (24): 9576–9579. Bibcode:2009PNAS..106.9576L. doi:10.1073/pnas.0809436106. ISSN 0027-8424. PMC 2701016. PMID 19487662.
  82. ^ McElroy, M.B.; Donahue, T.M. (15 September 1972). "Stability of the Martian atmosphere". Science. 177 (4053): 986–988. Bibcode:1972Sci...177..986M. doi:10.1126/science.177.4053.986. hdl:2060/19730010098. ISSN 0036-8075. PMID 17788809. S2CID 30958948.
  83. ^ Parkinson, T.D.; Hunten, D.M. (October 1972). "Spectroscopy and acronomy of O2 on Mars". Journal of the Atmospheric Sciences. 29 (7): 1380–1390. Bibcode:1972JAtS...29.1380P. doi:10.1175/1520-0469(1972)029<1380:SAAOOO>2.0.CO;2. ISSN 0022-4928.
  84. ^ a b Stevens, M.H.; Siskind, D.E.; Evans, J.S.; Jain, S.K.; Schneider, N.M.; Deighan, J.; Stewart, A.I.F.; Crismani, M.; Stiepen, A. (28 May 2017). "Martian mesospheric cloud observations by IUVS on MAVEN: Thermal tides coupled to the upper atmosphere: IUVS Martian Mesospheric Clouds". Geophysical Research Letters. 44 (10): 4709–4715. doi:10.1002/2017GL072717. hdl:10150/624978. S2CID 13748950.
  85. ^ a b González-Galindo, Francisco; Määttänen, Anni; Forget, François; Spiga, Aymeric (1 November 2011). "The martian mesosphere as revealed by CO2 cloud observations and general circulation modeling". Icarus. 216 (1): 10–22. Bibcode:2011Icar..216...10G. doi:10.1016/j.icarus.2011.08.006. ISSN 0019-1035.
  86. ^ Stevens, M.H.; Evans, J.S.; Schneider, N.M.; Stewart, A.I.F.; Deighan, J.; Jain, S.K.; Crismani, M.; Stiepen, A.; Chaffin, M.S.; McClintock, W.E.; Holsclaw, G.M.; Lefèvre, F.; Lo, D.Y.; Clarke, J.T.; Montmessin, F.; Bougher, S.W.; Jakosky, B.M. (2015). "New observations of molecular nitrogen in the Martian upper atmosphere by IUVS on MAVEN". Geophysical Research Letters. 42 (21): 9050–9056. Bibcode:2015GeoRL..42.9050S. doi:10.1002/2015GL065319.
  87. ^ Mandt, Kathleen; Mousis, Olivier; Chassefière, Eric (1 July 2015). "Comparative planetology of the history of nitrogen isotopes in the atmospheres of Titan and Mars". Icarus. 254: 259–261. Bibcode:2015Icar..254..259M. doi:10.1016/j.icarus.2015.03.025. PMC 6527424. PMID 31118538.
  88. ^ Webster, Guy (8 April 2013). "Remaining Martian atmosphere still dynamic" (Press release). NASA. Archived from the original on 26 July 2020. Retrieved 12 June 2019.
  89. ^ Wall, Mike (8 April 2013). "Most of Mars' atmosphere is lost in space". Space.com. Archived from the original on 30 January 2016. Retrieved 9 April 2013.
  90. ^ Hartogh, P.; Jarchow, C.; Lellouch, E.; de Val-Borro, M.; Rengel, M.; Moreno, R.; et al. (2010). "Herschel / HIFI observations of Mars: First detection of O2 at sub-millimetre wavelengths and upper limits on HCL and H2O2". Astronomy and Astrophysics. 521: L49. arXiv:1007.1301. Bibcode:2010A&A...521L..49H. doi:10.1051/0004-6361/201015160. S2CID 119271891. Archived from the original on 7 February 2019. Retrieved 6 February 2019.
  91. ^ "Flying Observatory Detects Atomic Oxygen in Martian Atmosphere – NASA". 6 May 2016. Archived from the original on 8 November 2020. Retrieved 18 March 2017.
  92. ^ "Nasa probes oxygen mystery on Mars". BBC News. 14 November 2019. Archived from the original on 17 January 2020. Retrieved 15 November 2019.
  93. ^ Krasnopolsky, Vladimir A. (1 November 2006). "Photochemistry of the martian atmosphere: Seasonal, latitudinal, and diurnal variations". Icarus. 185 (1): 153–170. Bibcode:2006Icar..185..153K. doi:10.1016/j.icarus.2006.06.003. ISSN 0019-1035.
  94. ^ Perrier, S.; Bertaux, J.L.; Lefèvre, F.; Lebonnois, S.; Korablev, O.; Fedorova, A.; Montmessin, F. (2006). "Global distribution of total ozone on Mars from SPICAM/MEX UV measurements". Journal of Geophysical Research. Planets. 111 (E9): E09S06. Bibcode:2006JGRE..111.9S06P. doi:10.1029/2006JE002681. ISSN 2156-2202.
  95. ^ Perrier, Séverine; Montmessin, Franck; Lebonnois, Sébastien; Forget, François; Fast, Kelly; Encrenaz, Thérèse; et al. (August 2008). "Heterogeneous chemistry in the atmosphere of Mars". Nature. 454 (7207): 971–975. Bibcode:2008Natur.454..971L. doi:10.1038/nature07116. ISSN 1476-4687. PMID 18719584. S2CID 205214046.
  96. ^ a b Franck Lefèvre; Montmessin, Franck (November 2013). "Transport-driven formation of a polar ozone layer on Mars". Nature Geoscience. 6 (11): 930–933. Bibcode:2013NatGe...6..930M. doi:10.1038/ngeo1957. ISSN 1752-0908.
  97. ^ a b "A seasonal ozone layer over the Martian south pole". sci.esa.int. Mars Express. European Space Agency. Archived from the original on 3 June 2019. Retrieved 3 June 2019.
  98. ^ Lebonnois, Sébastien; Quémerais, Eric; Montmessin, Franck; Lefèvre, Franck; Perrier, Séverine; Bertaux, Jean-Loup; Forget, François (2006). "Vertical distribution of ozone on Mars as measured by SPICAM/Mars Express using stellar occultations" (PDF). Journal of Geophysical Research. Planets. 111 (E9): E09S05. Bibcode:2006JGRE..111.9S05L. doi:10.1029/2005JE002643. ISSN 2156-2202. S2CID 55162288. Archived (PDF) from the original on 8 November 2020. Retrieved 30 August 2020.
  99. ^ Titov, D.V. (1 January 2002). "Water vapour in the atmosphere of Mars". Advances in Space Research. 29 (2): 183–191. Bibcode:2002AdSpR..29..183T. doi:10.1016/S0273-1177(01)00568-3. ISSN 0273-1177.
  100. ^ a b Whiteway, J.A.; Komguem, L.; Dickinson, C.; Cook, C.; Illnicki, M.; Seabrook, J.; Popovici, V.; Duck, T. J.; Davy, R. (3 July 2009). "Mars Water-Ice Clouds and Precipitation". Science. 325 (5936): 68–70. Bibcode:2009Sci...325...68W. doi:10.1126/science.1172344. ISSN 0036-8075. PMID 19574386. S2CID 206519222.
  101. ^ Jakosky, Bruce M.; Farmer, Crofton B. (1982). "The seasonal and global behavior of water vapor in the Mars atmosphere: Complete global results of the Viking Atmospheric Water Detector Experiment". Journal of Geophysical Research. Solid Earth. 87 (B4): 2999–3019. Bibcode:1982JGR....87.2999J. doi:10.1029/JB087iB04p02999. ISSN 2156-2202.
  102. ^ a b Trokhimovskiy, Alexander; Fedorova, Anna; Korablev, Oleg; Montmessin, Franck; Bertaux, Jean-Loup; Rodin, Alexander; Smith, Michael D. (1 May 2015). "Mars' water vapor mapping by the SPICAM IR spectrometer: Five martian years of observations". Icarus. Dynamic Mars. 251: 50–64. Bibcode:2015Icar..251...50T. doi:10.1016/j.icarus.2014.10.007. ISSN 0019-1035.
  103. ^ "Scientists 'map' water vapor in Martian atmosphere". ScienceDaily. Archived from the original on 8 June 2019. Retrieved 8 June 2019.
  104. ^ mars.nasa.gov. "Mars Exploration Rover". Jet Propulsion Laboratory. mars.nasa.gov. NASA. Archived from the original on 8 August 2012. Retrieved 8 June 2019.
  105. ^ Ice Clouds in Martian Arctic. www.nasa.gov (accelerated movie). NASA. Archived from the original on 3 January 2019. Retrieved 8 June 2019.
  106. ^ Montmessin, Franck; Forget, François; Millour, Ehouarn; Navarro, Thomas; Madeleine, Jean-Baptiste; Hinson, David P.; Spiga, Aymeric (September 2017). "Snow precipitation on Mars driven by cloud-induced night-time convection". Nature Geoscience. 10 (9): 652–657. Bibcode:2017NatGe..10..652S. doi:10.1038/ngeo3008. ISSN 1752-0908. S2CID 135198120.
  107. ^ a b c esa. "The methane mystery". European Space Agency. Archived from the original on 2 June 2019. Retrieved 7 June 2019.
  108. ^ Potter, Sean (7 June 2018). "NASA Finds Ancient Organic Material, Mysterious Methane on Mars". NASA. Archived from the original on 8 June 2019. Retrieved 6 June 2019.
  109. ^ Witze, Alexandra (25 October 2018). "Mars scientists edge closer to solving methane mystery". Nature. 563 (7729): 18–19. Bibcode:2018Natur.563...18W. doi:10.1038/d41586-018-07177-4. PMID 30377322.
  110. ^ Formisano, Vittorio; Atreya, Sushil; Encrenaz, Thérèse; Ignatiev, Nikolai; Giuranna, Marco (3 December 2004). "Detection of Methane in the Atmosphere of Mars". Science. 306 (5702): 1758–1761. Bibcode:2004Sci...306.1758F. doi:10.1126/science.1101732. ISSN 0036-8075. PMID 15514118. S2CID 13533388.
  111. ^ a b Krasnopolsky, Vladimir A.; Maillard, Jean Pierre; Owen, Tobias C. (December 2004). "Detection of methane in the martian atmosphere: evidence for life?". Icarus. 172 (2): 537–547. Bibcode:2004Icar..172..537K. doi:10.1016/j.icarus.2004.07.004.
  112. ^ Geminale, A.; Formisano, V.; Giuranna, M. (July 2008). "Methane in Martian atmosphere: Average spatial, diurnal, and seasonal behaviour". Planetary and Space Science. 56 (9): 1194–1203. Bibcode:2008P&SS...56.1194G. doi:10.1016/j.pss.2008.03.004.
  113. ^ Mumma, M.J.; Villanueva, G.L.; Novak, R.E.; Hewagama, T.; Bonev, B.P.; DiSanti, M.A.; Mandell, A.M.; Smith, M.D. (20 February 2009). "Strong Release of Methane on Mars in Northern Summer 2003". Science. 323 (5917): 1041–1045. Bibcode:2009Sci...323.1041M. doi:10.1126/science.1165243. ISSN 0036-8075. PMID 19150811. S2CID 25083438.
  114. ^ Fonti, S.; Marzo, G.A. (March 2010). "Mapping the methane on Mars". Astronomy and Astrophysics. 512: A51. Bibcode:2010A&A...512A..51F. doi:10.1051/0004-6361/200913178. ISSN 0004-6361.
  115. ^ Geminale, A.; Formisano, V.; Sindoni, G. (1 February 2011). "Mapping methane in Martian atmosphere with PFS-MEX data". Planetary and Space Science. Methane on Mars: Current Observations, Interpretation and Future Plans. 59 (2): 137–148. Bibcode:2011P&SS...59..137G. doi:10.1016/j.pss.2010.07.011. ISSN 0032-0633.
  116. ^ a b c Webster, C. R.; Mahaffy, P. R.; Atreya, S. K.; Flesch, G. J.; Mischna, M. A.; Meslin, P.-Y.; Farley, K. A.; Conrad, P. G.; Christensen, L. E. (23 January 2015). "Mars methane detection and variability at Gale crater" (PDF). Science. 347 (6220): 415–417. Bibcode:2015Sci...347..415W. doi:10.1126/science.1261713. ISSN 0036-8075. PMID 25515120. S2CID 20304810. Archived (PDF) from the original on 22 July 2018. Retrieved 24 June 2019.
  117. ^ Vasavada, Ashwin R.; Zurek, Richard W.; Sander, Stanley P.; Crisp, Joy; Lemmon, Mark; Hassler, Donald M.; Genzer, Maria; Harri, Ari-Matti; Smith, Michael D. (8 June 2018). "Background levels of methane in Mars' atmosphere show strong seasonal variations". Science. 360 (6393): 1093–1096. Bibcode:2018Sci...360.1093W. doi:10.1126/science.aaq0131. ISSN 0036-8075. PMID 29880682.
  118. ^ Amoroso, Marilena; Merritt, Donald; Parra, Julia Marín-Yaseli de la; Cardesín-Moinelo, Alejandro; Aoki, Shohei; Wolkenberg, Paulina; Alessandro Aronica; Formisano, Vittorio; Oehler, Dorothy (May 2019). "Independent confirmation of a methane spike on Mars and a source region east of Gale Crater". Nature Geoscience. 12 (5): 326–332. Bibcode:2019NatGe..12..326G. doi:10.1038/s41561-019-0331-9. ISSN 1752-0908. S2CID 134110253.
  119. ^ Krasnopolsky, Vladimir A. (15 November 2005). "A sensitive search for SO2 in the martian atmosphere: Implications for seepage and origin of methane". Icarus. Jovian Magnetospheric Environment Science. 178 (2): 487–492. Bibcode:2005Icar..178..487K. doi:10.1016/j.icarus.2005.05.006. ISSN 0019-1035.
  120. ^ Hecht, Jeff. "Volcanoes ruled out for Martian methane". www.newscientist.com. Archived from the original on 8 June 2019. Retrieved 8 June 2019.
  121. ^ Krasnopolsky, Vladimir A (2012). "Search for methane and upper limits to ethane and SO2 on Mars". Icarus. 217 (1): 144–152. Bibcode:2012Icar..217..144K. doi:10.1016/j.icarus.2011.10.019.
  122. ^ Encrenaz, T.; Greathouse, T. K.; Richter, M. J.; Lacy, J. H.; Fouchet, T.; Bézard, B.; Lefèvre, F.; Forget, F.; Atreya, S. K. (2011). "A stringent upper limit to SO2 in the Martian atmosphere". Astronomy and Astrophysics. 530: 37. Bibcode:2011A&A...530A..37E. doi:10.1051/0004-6361/201116820.
  123. ^ McAdam, A. C.; Franz, H.; Archer, P. D.; Freissinet, C.; Sutter, B.; Glavin, D. P.; Eigenbrode, J. L.; Bower, H.; Stern, J.; Mahaffy, P. R.; Morris, R. V.; Ming, D. W.; Rampe, E.; Brunner, A. E.; Steele, A.; Navarro-González, R.; Bish, D. L.; Blake, D.; Wray, J.; Grotzinger, J.; MSL Science Team (2013). "Insights into the Sulfur Mineralogy of Martian Soil at Rocknest, Gale Crater, Enabled by Evolved Gas Analyses". 44th Lunar and Planetary Science Conference, held 18–22 March 2013 in The Woodlands, Texas. LPI Contribution No. 1719, p. 1751
  124. ^ a b Owen, T.; Biemann, K.; Rushneck, D. R.; Biller, J. E.; Howarth, D. W.; Lafleur, A. L. (17 December 1976). "The Atmosphere of Mars: Detection of Krypton and Xenon". Science. 194 (4271): 1293–1295. Bibcode:1976Sci...194.1293O. doi:10.1126/science.194.4271.1293. ISSN 0036-8075. PMID 17797086. S2CID 37362034.
  125. ^ Owen, Tobias; Biemann, K.; Rushneck, D. R.; Biller, J. E.; Howarth, D. W.; Lafleur, A. L. (1977). "The composition of the atmosphere at the surface of Mars". Journal of Geophysical Research. 82 (28): 4635–4639. Bibcode:1977JGR....82.4635O. doi:10.1029/JS082i028p04635. ISSN 2156-2202.
  126. ^ Krasnopolsky, Vladimir A.; Gladstone, G. Randall (1 August 2005). "Helium on Mars and Venus: EUVE observations and modeling". Icarus. 176 (2): 395–407. Bibcode:2005Icar..176..395K. doi:10.1016/j.icarus.2005.02.005. ISSN 0019-1035.
  127. ^ "Curiosity finds evidence of Mars crust contributing to atmosphere". JPL. NASA. Archived from the original on 9 March 2020. Retrieved 8 June 2019.
  128. ^ a b Krasnopolsky, V. A. (30 November 2001). "Detection of Molecular Hydrogen in the Atmosphere of Mars". Science. 294 (5548): 1914–1917. Bibcode:2001Sci...294.1914K. doi:10.1126/science.1065569. PMID 11729314. S2CID 25856765.
  129. ^ Smith, Michael D. (May 2008). "Spacecraft Observations of the Martian Atmosphere". Annual Review of Earth and Planetary Sciences. 36 (1): 191–219. Bibcode:2008AREPS..36..191S. doi:10.1146/annurev.earth.36.031207.124334. ISSN 0084-6597. S2CID 102489157.
  130. ^ Withers, Paul; Catling, D. C. (December 2010). "Observations of atmospheric tides on Mars at the season and latitude of the Phoenix atmospheric entry". Geophysical Research Letters. 37 (24): n/a. Bibcode:2010GeoRL..3724204W. doi:10.1029/2010GL045382. S2CID 26311417.
  131. ^ a b Leovy, Conway (July 2001). "Weather and climate on Mars". Nature. 412 (6843): 245–249. Bibcode:2001Natur.412..245L. doi:10.1038/35084192. ISSN 1476-4687. PMID 11449286. S2CID 4383943.
  132. ^ Petrosyan, A.; Galperin, B.; Larsen, S. E.; Lewis, S. R.; Määttänen, A.; Read, P. L.; Renno, N.; Rogberg, L. P. H. T.; Savijärvi, H. (17 September 2011). "The Martian Atmospheric Boundary Layer". Reviews of Geophysics. 49 (3): RG3005. Bibcode:2011RvGeo..49.3005P. doi:10.1029/2010RG000351. hdl:2027.42/94893. ISSN 8755-1209. S2CID 37493454.
  133. ^ Catling, David C. (13 April 2017). Atmospheric evolution on inhabited and lifeless worlds. Kasting, James F. Cambridge. Bibcode:2017aeil.book.....C. ISBN 9780521844123. OCLC 956434982.{{cite book}}: CS1 maint: location missing publisher (link)
  134. ^ Robinson, T. D.; Catling, D. C. (January 2014). "Common 0.1 bar tropopause in thick atmospheres set by pressure-dependent infrared transparency". Nature Geoscience. 7 (1): 12–15. arXiv:1312.6859. Bibcode:2014NatGe...7...12R. doi:10.1038/ngeo2020. ISSN 1752-0894. S2CID 73657868.
  135. ^ Forget, François; Montmessin, Franck; Bertaux, Jean-Loup; González-Galindo, Francisco; Lebonnois, Sébastien; Quémerais, Eric; Reberac, Aurélie; Dimarellis, Emmanuel; López-Valverde, Miguel A. (28 January 2009). "Density and temperatures of the upper Martian atmosphere measured by stellar occultations with Mars Express SPICAM" (PDF). Journal of Geophysical Research. 114 (E1): E01004. Bibcode:2009JGRE..114.1004F. doi:10.1029/2008JE003086. ISSN 0148-0227. S2CID 2660831. Archived (PDF) from the original on 3 May 2019. Retrieved 24 June 2019.
  136. ^ Bougher, S. W.; Pawlowski, D.; Bell, J. M.; Nelli, S.; McDunn, T.; Murphy, J. R.; Chizek, M.; Ridley, A. (February 2015). "Mars Global Ionosphere-Thermosphere Model: Solar cycle, seasonal, and diurnal variations of the Mars upper atmosphere: BOUGHER ET AL". Journal of Geophysical Research: Planets. 120 (2): 311–342. doi:10.1002/2014JE004715. hdl:2027.42/110830. S2CID 91178752.
  137. ^ Bougher, Stephen W.; Roeten, Kali J.; Olsen, Kirk; Mahaffy, Paul R.; Benna, Mehdi; Elrod, Meredith; Jain, Sonal K.; Schneider, Nicholas M.; Deighan, Justin (2017). "The structure and variability of Mars dayside thermosphere from MAVEN NGIMS and IUVS measurements: Seasonal and solar activity trends in scale heights and temperatures". Journal of Geophysical Research: Space Physics. 122 (1): 1296–1313. Bibcode:2017JGRA..122.1296B. doi:10.1002/2016JA023454. hdl:2027.42/136242. ISSN 2169-9402.
  138. ^ Zell, Holly (29 May 2015). "MAVEN Captures Aurora on Mars". NASA. Archived from the original on 31 July 2020. Retrieved 5 June 2019.
  139. ^ Greicius, Tony (28 September 2017). "NASA Missions See Effects at Mars From Large Solar Storm". NASA. Archived from the original on 8 June 2019. Retrieved 5 June 2019.
  140. ^ "Mars Education | Developing the Next Generation of Explorers". marsed.asu.edu. Archived from the original on 3 June 2019. Retrieved 3 June 2019.
  141. ^ McCleese, D. J.; Schofield, J. T.; Taylor, F. W.; Abdou, W. A.; Aharonson, O.; Banfield, D.; Calcutt, S. B.; Heavens, N. G.; Irwin, P. G. J. (November 2008). "Intense polar temperature inversion in the middle atmosphere on Mars". Nature Geoscience. 1 (11): 745–749. Bibcode:2008NatGe...1..745M. doi:10.1038/ngeo332. ISSN 1752-0894. S2CID 128907168.
  142. ^ Slipski, M.; Jakosky, B. M.; Benna, M.; Elrod, M.; Mahaffy, P.; Kass, D.; Stone, S.; Yelle, R. (2018). "Variability of Martian Turbopause Altitudes". Journal of Geophysical Research: Planets. 123 (11): 2939–2957. Bibcode:2018JGRE..123.2939S. doi:10.1029/2018JE005704. ISSN 2169-9100.
  143. ^ "Mars' ionosphere shaped by crustal magnetic fields". sci.esa.int. Archived from the original on 3 June 2019. Retrieved 3 June 2019.
  144. ^ "New views of the Martian ionosphere". sci.esa.int. Archived from the original on 11 November 2013. Retrieved 3 June 2019.
  145. ^ a b Smith, Michael D. (1 January 2004). "Interannual variability in TES atmospheric observations of Mars during 1999–2003". Icarus. Special Issue on DS1 / Comet Borrelly. 167 (1): 148–165. Bibcode:2004Icar..167..148S. doi:10.1016/j.icarus.2003.09.010. ISSN 0019-1035.
  146. ^ Montabone, L.; Forget, F.; Millour, E.; Wilson, R.J.; Lewis, S.R.; Cantor, B.; et al. (1 May 2015). "Eight-year climatology of dust optical depth on Mars". Icarus. Dynamic Mars. 251: 65–95. arXiv:1409.4841. Bibcode:2015Icar..251...65M. doi:10.1016/j.icarus.2014.12.034. ISSN 0019-1035. S2CID 118336315.
  147. ^ NASA/JPL-Caltech/TAMU. "Atmospheric opacity from Opportunity's point of view". NASA's Mars Exploration Program. Archived from the original on 9 June 2019. Retrieved 9 June 2019.
  148. ^ a b Lemmon, Mark T.; Wolff, Michael J.; Bell, James F.; Smith, Michael D.; Cantor, Bruce A.; Smith, Peter H. (1 May 2015). "Dust aerosol, clouds, and the atmospheric optical depth record over 5 Mars years of the Mars Exploration Rover mission". Icarus. Dynamic Mars. 251: 96–111. arXiv:1403.4234. Bibcode:2015Icar..251...96L. doi:10.1016/j.icarus.2014.03.029. ISSN 0019-1035. S2CID 5194550.
  149. ^ Chen-Chen, H.; Pérez-Hoyos, S.; Sánchez-Lavega, A. (1 February 2019). "Dust particle size and optical depth on Mars retrieved by the MSL navigation cameras". Icarus. 319: 43–57. arXiv:1905.01073. Bibcode:2019Icar..319...43C. doi:10.1016/j.icarus.2018.09.010. ISSN 0019-1035. S2CID 125311345.
  150. ^ Vicente-Retortillo, Álvaro; Martínez, Germán M.; Renno, Nilton O.; Lemmon, Mark T.; de la Torre-Juárez, Manuel (2017). "Determination of dust aerosol particle size at Gale Crater using REMS UVS and Mastcam measurements". Geophysical Research Letters. 44 (8): 3502–3508. Bibcode:2017GeoRL..44.3502V. doi:10.1002/2017GL072589. hdl:2027.42/137189. ISSN 1944-8007.
  151. ^ McCleese, D.J.; Heavens, N.G.; Schofield, J.T.; Abdou, W.A.; Bandfield, J.L.; Calcutt, S.B.; et al. (2010). "Structure and dynamics of the Martian lower and middle atmosphere as observed by the Mars Climate Sounder: Seasonal variations in zonal mean temperature, dust, and water ice aerosols" (PDF). Journal of Geophysical Research. Planets. 115 (E12): E12016. Bibcode:2010JGRE..11512016M. doi:10.1029/2010JE003677. ISSN 2156-2202. S2CID 215820851. Archived (PDF) from the original on 15 August 2017. Retrieved 24 June 2019.
  152. ^ Guzewich, Scott D.; Talaat, Elsayed R.; Toigo, Anthony D.; Waugh, Darryn W.; McConnochie, Timothy H. (2013). "High-altitude dust layers on Mars: Observations with the Thermal Emission Spectrometer". Journal of Geophysical Research. Planets. 118 (6): 1177–1194. Bibcode:2013JGRE..118.1177G. doi:10.1002/jgre.20076. ISSN 2169-9100.
  153. ^ a b Read, P L; Lewis, S R; Mulholland, D P (4 November 2015). "The physics of Martian weather and climate: a review" (PDF). Reports on Progress in Physics. 78 (12): 125901. Bibcode:2015RPPh...78l5901R. doi:10.1088/0034-4885/78/12/125901. ISSN 0034-4885. PMID 26534887. S2CID 20087052. Archived (PDF) from the original on 20 July 2018. Retrieved 24 June 2019.
  154. ^ Ojha, Lujendra; Lewis, Kevin; Karunatillake, Suniti; Schmidt, Mariek (20 July 2018). "The Medusae Fossae Formation as the single largest source of dust on Mars". Nature Communications. 9 (2867 (2018)): 2867. Bibcode:2018NatCo...9.2867O. doi:10.1038/s41467-018-05291-5. PMC 6054634. PMID 30030425.
  155. ^ Malik, Tariq (13 June 2018). "As Massive Storm Rages on Mars, Opportunity Rover Falls Silent – Dust clouds blotting out the sun could be the end of the solar-powered probe". Scientific American. Archived from the original on 13 June 2018. Retrieved 13 June 2018.
  156. ^ Wall, Mike (12 June 2018). "NASA's Curiosity Rover Is Tracking a Huge Dust Storm on Mars (Photo)". Space.com. Archived from the original on 21 December 2020. Retrieved 13 June 2018.
  157. ^ Good, Andrew; Brown, Dwayne; Wendell, JoAnna (12 June 2018). "NASA to Hold Media Teleconference on Martian Dust Storm, Mars Opportunity Rover". NASA. Archived from the original on 21 June 2018. Retrieved 12 June 2018.
  158. ^ Good, Andrew (13 June 2018). "NASA Encounters the Perfect Storm for Science". NASA. Archived from the original on 25 June 2018. Retrieved 14 June 2018.
  159. ^ NASA Staff (13 June 2018). "Mars Dust Storm News – Teleconference – audio (065:22)". NASA. Archived from the original on 13 June 2018. Retrieved 13 June 2018.
  160. ^ a b c Whelley, Patrick L.; Greeley, Ronald (2008). "The distribution of dust devil activity on Mars". Journal of Geophysical Research: Planets. 113 (E7): E07002. Bibcode:2008JGRE..113.7002W. doi:10.1029/2007JE002966. ISSN 2156-2202.
  161. ^ Balme, Matt; Greeley, Ronald (2006). "Dust devils on Earth and Mars". Reviews of Geophysics. 44 (3): RG3003. Bibcode:2006RvGeo..44.3003B. doi:10.1029/2005RG000188. ISSN 1944-9208. S2CID 53391259.
  162. ^ a b "The Devils of Mars | Science Mission Directorate". science.nasa.gov. Archived from the original on 26 December 2018. Retrieved 11 June 2019.
  163. ^ Stolte, Daniel; Communications, University (22 May 2019). "On Mars, Sands Shift to a Different Drum". UANews. Archived from the original on 4 June 2019. Retrieved 11 June 2019.
  164. ^ "NASA – NASA Orbiter Catches Mars Sand Dunes in Motion". www.nasa.gov. Archived from the original on 26 July 2020. Retrieved 11 June 2019.
  165. ^ a b Urso, Anna C.; Fenton, Lori K.; Banks, Maria E.; Chojnacki, Matthew (1 May 2019). "Boundary condition controls on the high-sand-flux regions of Mars". Geology. 47 (5): 427–430. Bibcode:2019Geo....47..427C. doi:10.1130/G45793.1. ISSN 0091-7613. PMC 7241575. PMID 32440031.
  166. ^ "Thermal tide – AMS Glossary". glossary.ametsoc.org. Archived from the original on 26 July 2020. Retrieved 11 June 2019.
  167. ^ a b Lee, C.; Lawson, W. G.; Richardson, M. I.; Heavens, N. G.; Kleinböhl, A.; Banfield, D.; McCleese, D. J.; Zurek, R.; Kass, D. (2009). "Thermal tides in the Martian middle atmosphere as seen by the Mars Climate Sounder". Journal of Geophysical Research: Planets. 114 (E3): E03005. Bibcode:2009JGRE..114.3005L. doi:10.1029/2008JE003285. ISSN 2156-2202. PMC 5018996. PMID 27630378.
  168. ^ a b c Mars. Kieffer, Hugh H. Tucson: University of Arizona Press. 1992. ISBN 0816512574. OCLC 25713423.{{cite book}}: CS1 maint: others (link)
  169. ^ "NASA – Thermal Tides at Mars". www.nasa.gov. Archived from the original on 17 June 2019. Retrieved 11 June 2019.
  170. ^ "Orographic cloud – AMS Glossary". glossary.ametsoc.org. Archived from the original on 10 September 2019. Retrieved 11 June 2019.
  171. ^ esa. "Mars Express keeps an eye on curious cloud". European Space Agency. Archived from the original on 15 June 2019. Retrieved 11 June 2019.
  172. ^ rburnham. "Mars Express: Keeping an eye on a curious cloud | Red Planet Report". Archived from the original on 27 September 2019. Retrieved 11 June 2019.
  173. ^ Maurice, S (1 April 2022). "In situ recording of Mars soundscape". Nature. 605 (7911): 653–658. Bibcode:2022Natur.605..653M. doi:10.1038/s41586-022-04679-0. PMC 9132769. PMID 35364602. S2CID 247865804.
  174. ^ Agle, DC; Fox, Karen; Johnson, Alana; Brennan, Pat (1 April 2022). "What Sounds Captured by NASA's Perseverance Rover Reveal About Mars – A new study based on recordings made by the rover finds that the speed of sound is slower on the Red Planet than on Earth and that, mostly, a deep silence prevails". NASA. Retrieved 5 April 2022.
  175. ^ Ferreira, Becky (4 April 2022). "Sound on Mars Has a 'Unique' And Extremely Trippy Property, Recordings Reveal – Mars has two speeds of sound, which "may induce a unique listening experience on Mars with an early arrival of high-pitched sounds compared to bass". Vice. Retrieved 5 April 2022.
  176. ^ Mumma, M. J.; Novak, R. E.; DiSanti, M. A.; Bonev, B. P. (2003). "A Sensitive Search for Methane on Mars". Bulletin of the American Astronomical Society. 35: 937. Bibcode:2003DPS....35.1418M.
  177. ^ Naeye, Robert (28 September 2004). "Mars Methane Boosts Chances for Life". Sky & Telescope. Archived from the original on 20 December 2014. Retrieved 20 December 2014.
  178. ^ Hand, Eric (2018). "Mars methane rises and falls with the seasons". Science. 359 (6371): 16–17. Bibcode:2018Sci...359...16H. doi:10.1126/science.359.6371.16. PMID 29301992.
  179. ^ Webster, Guy; Neal-Jones, Nancy; Brown, Dwayne (16 December 2014). "NASA Rover Finds Active and Ancient Organic Chemistry on Mars". NASA. Archived from the original on 17 December 2014. Retrieved 16 December 2014.
  180. ^ Chang, Kenneth (16 December 2014). "'A Great Moment': Rover Finds Clue That Mars May Harbor Life". The New York Times. Archived from the original on 16 December 2014. Retrieved 16 December 2014.
  181. ^ Chang, Kenneth (7 June 2018). "Life on Mars? Rover's Latest Discovery Puts It 'On the Table' - The identification of organic molecules in rocks on the red planet does not necessarily point to life there, past or present, but does indicate that some of the building blocks were present". The New York Times. Archived from the original on 8 June 2018. Retrieved 8 June 2018.
  182. ^ Eigenbrode, Jennifer L.; et al. (8 June 2018). "Organic matter preserved in 3-billion-year-old mudstones at Gale crater, Mars". Science. 360 (6393): 1096–1101. Bibcode:2018Sci...360.1096E. doi:10.1126/science.aas9185. hdl:10044/1/60810. PMID 29880683.
  183. ^ Mumma, Michael; et al. (2010). "The Astrobiology of Mars: Methane and Other Candinate Biomarker Gases, and Related Interdisciplinary Studies on Earth and Mars" (PDF). Astrobiology Science Conference 2010. Astrophysics Data System. Greenbelt, MD: Goddard Space Flight Center. Archived (PDF) from the original on 25 October 2012. Retrieved 24 July 2010.
  184. ^ Oze, C.; Sharma, M. (2005). "Have olivine, will gas: Serpentinization and the abiogenic production of methane on Mars". Geophys. Res. Lett. 32 (10): L10203. Bibcode:2005GeoRL..3210203O. doi:10.1029/2005GL022691. S2CID 28981740.
  185. ^ Oze, Christopher; Jones, Camille; Goldsmith, Jonas I.; Rosenbauer, Robert J. (7 June 2012). "Differentiating biotic from abiotic methane genesis in hydrothermally active planetary surfaces". PNAS. 109 (25): 9750–9754. Bibcode:2012PNAS..109.9750O. doi:10.1073/pnas.1205223109. PMC 3382529. PMID 22679287.
  186. ^ Staff (25 June 2012). "Mars Life Could Leave Traces in Red Planet's Air: Study". Space.com. Archived from the original on 9 October 2019. Retrieved 27 June 2012.
  187. ^ Zahnle, Kevin; Catling, David (2019). "The paradox of Martian Methane" (PDF). Ninth International Conference on Mars 2019. LPI Contrib. No. 2089. Archived (PDF) from the original on 1 October 2021. Retrieved 27 June 2019.
  188. ^ Ruf, Christopher; Renno, Nilton O.; Kok, Jasper F.; Bandelier, Etienne; Sander, Michael J.; Gross, Steven; Skjerve, Lyle; Cantor, Bruce (2009). "Emission of non-thermal microwave radiation by a Martian dust storm". Geophysical Research Letters. 36 (13): L13202. Bibcode:2009GeoRL..3613202R. doi:10.1029/2009GL038715. hdl:2027.42/94934. ISSN 1944-8007. S2CID 14707525.
  189. ^ Gurnett, D. A.; Morgan, D. D.; Granroth, L. J.; Cantor, B. A.; Farrell, W. M.; Espley, J. R. (2010). "Non-detection of impulsive radio signals from lightning in Martian dust storms using the radar receiver on the Mars Express spacecraft". Geophysical Research Letters. 37 (17): n/a. Bibcode:2010GeoRL..3717802G. doi:10.1029/2010GL044368. ISSN 1944-8007. S2CID 134066523.
  190. ^ Anderson, Marin M.; Siemion, Andrew P. V.; Barott, William C.; Bower, Geoffrey C.; Delory, Gregory T.; Pater, Imke de; Werthimer, Dan (December 2011). "The Allen Telescope Array Search for Electrostatic Discharges on Mars". The Astrophysical Journal. 744 (1): 15. arXiv:1111.0685. doi:10.1088/0004-637X/744/1/15. ISSN 0004-637X. S2CID 118861678. Archived from the original on 27 April 2019. Retrieved 30 August 2020.
  191. ^ a b Choi, Charles; Q. (6 June 2019). "Why Mars Lightning Is Weak and Rare". Space.com. Archived from the original on 9 June 2019. Retrieved 7 June 2019.
  192. ^ Wurm, Gerhard; Schmidt, Lars; Steinpilz, Tobias; Boden, Lucia; Teiser, Jens (1 October 2019). "A challenge for Martian lightning: Limits of collisional charging at low pressure". Icarus. 331: 103–109. arXiv:1905.11138. Bibcode:2019Icar..331..103W. doi:10.1016/j.icarus.2019.05.004. ISSN 0019-1035. S2CID 166228217.
  193. ^ Laraia, Anne L.; Schneider, Tapio (30 July 2015). "Superrotation in Terrestrial Atmospheres" (PDF). Journal of the Atmospheric Sciences. 72 (11): 4281–4296. Bibcode:2015JAtS...72.4281L. doi:10.1175/JAS-D-15-0030.1. ISSN 0022-4928. S2CID 30893675. Archived (PDF) from the original on 23 July 2018. Retrieved 24 June 2019.
  194. ^ a b Read, Peter L.; Lebonnois, Sebastien (30 May 2018). "Superrotation on Venus, on Titan, and Elsewhere". Annual Review of Earth and Planetary Sciences. 46 (1): 175–202. Bibcode:2018AREPS..46..175R. doi:10.1146/annurev-earth-082517-010137. ISSN 0084-6597. S2CID 134203070.
  195. ^ Lewis, Stephen R.; Read, Peter L. (2003). "Equatorial jets in the dusty Martian atmosphere" (PDF). Journal of Geophysical Research: Planets. 108 (E4): 5034. Bibcode:2003JGRE..108.5034L. doi:10.1029/2002JE001933. ISSN 2156-2202. Archived (PDF) from the original on 26 July 2020. Retrieved 30 July 2019.
  196. ^ Herschel William (1 January 1784). "XIX. On the remarkable appearances at the polar regions of the planet Mars, and its spheroidical figure; with a few hints relating to its real diameter and atmosphere". Philosophical Transactions of the Royal Society of London. 74: 233–273. doi:10.1098/rstl.1784.0020. S2CID 186212257.
  197. ^ Dawes, W.R. (1865). "Physical Observations of Mars Near the Opposition in 1864". Astronomical Register. 3: 220.1. Bibcode:1865AReg....3..220D.
  198. ^ a b Campbell, W.W. (1894). "Concerning an Atmosphere on Mars". Publications of the Astronomical Society of the Pacific. 6 (38): 273. Bibcode:1894PASP....6..273C. doi:10.1086/120876.
  199. ^ Wright, W. H. (1925). "Photographs of Mars made with light of different colors". Lick Observatory Bulletin. 12: 48–61. Bibcode:1925LicOB..12...48W. doi:10.5479/ADS/bib/1925LicOB.12.48W.
  200. ^ Menzel, D. H. (1926). "The Atmosphere of Mars". Astrophysical Journal. 61: 48. Bibcode:1926ApJ....63...48M. doi:10.1086/142949.
  201. ^ Kaplan, Lewis D.; Münch, Guido; Spinrad, Hyron (January 1964). "An Analysis of the Spectrum of Mars". The Astrophysical Journal. 139: 1. Bibcode:1964ApJ...139....1K. doi:10.1086/147736. ISSN 0004-637X.
  202. ^ Kaplan, Lewis D.; Connes, J.; Connes, P. (September 1969). "Carbon Monoxide in the Martian Atmosphere". The Astrophysical Journal. 157: L187. Bibcode:1969ApJ...157L.187K. doi:10.1086/180416. ISSN 0004-637X.
  203. ^ "Mariner 4 Anniversary Marks 30 Years of Mars Exploration". NASA/JPL. Archived from the original on 28 July 2020. Retrieved 9 June 2019.
  204. ^ Scoles, Sarah (24 July 2020). "The Doctor From Nazi Germany and the Roots of the Hunt for Life on Mars". The New York Times. ISSN 0362-4331. Archived from the original on 25 November 2020. Retrieved 24 July 2020.
  205. ^ Kemppinen, O; Tillman, J.E; Schmidt, W; Harri, A.-M (2013). "New analysis software for Viking Lander meteorological data". Geoscientific Instrumentation, Methods and Data Systems. 2 (1): 61–69. Bibcode:2013GI......2...61K. doi:10.5194/gi-2-61-2013.
  206. ^ mars.nasa.gov. "Mars Weather at Elysium Planitia". NASA's InSight Mars Lander. Archived from the original on 1 December 2020. Retrieved 13 June 2019.
  207. ^ NASA, JPL. "Rover Environmental Monitoring Station (REMS) – NASA Mars Curiosity Rover". mars.nasa.gov. Archived from the original on 12 November 2020. Retrieved 13 June 2019.
  208. ^ "NASA Wants to Make Rocket Fuel From Martian Soil - ExtremeTech". www.extremetech.com. Archived from the original on 26 September 2020. Retrieved 23 September 2020.
  209. ^ "NASA's Perseverance rover produces oxygen on Mars in historic first — water could be next, scientists say". 22 April 2021.

Further reading

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