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The atmosphere of Mars is the layer of gases surrounding Mars. It is primarily composed of carbon dioxide (95%), molecular nitrogen (2.8%), and argon (2%). It also contains trace levels of water vapor, oxygen, carbon monoxide, hydrogen, and noble gases. The atmosphere of Mars is much thinner than Earth's. The average surface pressure is only about 610 pascals (0.088 psi) which is less than 1% of the Earth's value.
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.
The higher density during spring and fall is reduced by 25% during the
winter when carbon dioxide partly freezes at the pole caps.
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. 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.
The atmosphere of Mars is colder than Earth's. Owing to the
larger distance from the Sun, Mars receives less solar energy and has a
lower effective temperature, which is about 210 K (−63 °C; −82 °F). The average surface emission temperature of Mars is just 215 K (−58 °C; −73 °F), which is comparable to inland Antarctica. The weaker greenhouse effect in the Martian atmosphere (5 °C (9.0 °F), versus 33 °C (59 °F) on Earth) can be explained by the low abundance of other greenhouse gases.
The daily range of temperature in the lower atmosphere is huge 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. 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.
Dust devils and dust storms are prevalent on Mars, which are sometimes observable by telescopes from Earth, and in 2018 even with the naked eye as a change in colour and brightness of the planet. Planet-encircling dust storms (global dust storms) occur on average every 5.5 Earth years (every 3 Martian years) on Mars and can threaten the operation of Mars rovers. However, the mechanism responsible for the development of large dust storms is still not well understood. 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 oxidizing atmosphere.
The photochemical reactions in the atmosphere tend to oxidize the
organic species and turn them into carbon dioxide or carbon monoxide. 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,
several previous missions and ground-based telescope detected
unexpected levels of methane in the Martian atmosphere, which may even
be a biosignature for life on Mars. However, the interpretation of the measurements is still highly controversial and lacks a scientific consensus.
History of atmospheric observations
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. In 1809, French astronomer Honoré Flaugergues wrote about his observation of "yellow clouds" on Mars, which are likely to be dust storm events. 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." Spectroscopic observations in the 1860s and 1870s 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. In 1926, photographic observations by William Hammond Wright at the Lick Observatory allowed Donald Howard Menzel to discover quantitative evidence of Mars's atmosphere.
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, as well as carbon monoxide in 1969. 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. 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.
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).
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. 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 2022.
Current chemical composition
Carbon dioxide
CO2 is the main component of the Martian atmosphere. It has a mean volume ratio of 94.9%. 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. 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. The condensation process can be approximated by the Clausius–Clapeyron relation for CO2.
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.
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. 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:
- 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. 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.
Nitrogen
N2 is the second most abundant gas in the Martian atmosphere. It has a mean volume ratio of 2.6%. Various measurements showed that the Martian atmosphere is enriched in 15N. The enrichment of heavy isotopes of nitrogen is possibly caused by mass-selective escape processes.
Argon
Argon is the third most abundant gas in the Martian atmosphere. It has a mean volume ratio of 1.9%. 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. 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.
Oxygen and ozone
The estimated mean volume ratio of molecular oxygen (O2) in the Martian atmosphere is 0.174%. 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.
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.
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.
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.
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.
The actual reactions between ozone and odd hydrogen species may be
further complicated by the heterogeneous reactions that take place in
water-ice clouds.
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. 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.
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).
Water vapor
Water vapor is a trace gas in the Martian atmosphere and has huge spatial, diurnal and seasonal variability.
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. 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).
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.
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. 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.
Dust
Under sufficiently strong wind (> 30 ms−1), dust particles can be mobilized and lifted from the surface to the atmosphere. Some of the dust particles can be suspended in the atmosphere and travel by circulation before falling back to the ground.
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). The local abundance of dust varies greatly by seasons and years. During global dust events, Mars surface assets can observe optical depth that is over 4.
Surface measurements also showed the effective radius of dust particles
ranges from 0.6 μm to 2 μm and has considerable seasonality.
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).
Seasonal variations in oxygen and methane at
Gale craterMethane
As a volcanic and biogenic species, methane is of interest to geologists and astrobiologists.
However, methane is chemically unstable in an oxidizing atmosphere with
UV radiation. The lifetime of methane in the Martian atmosphere is
about 400 years.
The detection of methane in a planetary atmosphere may indicate the
presence of recent geological activities or living organisms.
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.
The source of methane on Mars and the explanation for the enormous
discrepancy in the observed methane concentrations are still under
active debate.
See also the section "detection of methane in the atmosphere" for more details.
Sulfur dioxide
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. No SO2 has been detected in the atmosphere, with a sensitivity upper limit set at 0.2 ppb. 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.
Other trace gases
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%.
Noble gases, other than helium and argon, are present at trace levels (≈10 -
0.01 ppmv) in the Martian atmosphere. The concentration of helium,
neon, krypton and xenon in the Martian atmosphere has been measured by
different missions.
The isotopic ratios of noble gases reveal information about the early
geological activities on Mars and the evolution of its atmosphere.
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. Photochemical modeling estimated that the mixing ratio of H2 in the lower atmosphere is about 15 ±5 ppmv.
Vertical structure
The
vertical structure of the atmosphere of Mars overlaying 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. 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. The theoretical dry adiabatic lapse rate of Mars is 4.3 °C km−1, 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. The planetary boundary layer can extend to over 10 km thick during the daytime. The near-surface diurnal temperature range is huge (60 °C)
due to the low thermal inertia. Under dusty conditions, the suspended
dust particles can reduce the surface diurnal temperature range to only
5 °C. The temperature above 15 km is controlled by radiative processes instead of convection. Mars is also a rare exception to the "0.1-bar tropopause" rule found in the other atmospheres in solar system.
- 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. 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.
- 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, 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.
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.
However, a seasonal ozone layer and a strong temperature inversion in
the middle atmosphere have been observed over the Martian south pole. 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.
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. The exosphere of Mars starts at about 230 km and gradually merges with interplanetary space.
Dust and other dynamic features
Dust devils
Dust devils are common on Mars.
Like their counterparts on Earth, dust devils form when the convective
vortices driven by strong surface heating are loaded with dust
particles.
Dust devils on Mars usually have a diameter of tens of meter and height
of several kilometers, which are much taller than the ones observed on
Earth. Study of dust devils' tracks showed that most of Martian dust devils occur at around 60°N and 60°S in spring and summer. 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.
Dust storms
Local and regional dust storms are not rare on Mars. 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. Near the polar cap, dust storms sometimes can be generated by frontal activities and extratropical cyclones.
Global dust storms (area > 106 km2 ) occur on average once every 3 Martian years. Observations showed that larger dust storms are usually the result of merging smaller dust storms, but the growth mechanism of the storm and the role of atmospheric feedbacks are still not well understood. 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. Researchers reported that the largest single source of dust on Mars comes from the Medusae Fossae Formation.
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.
Thermal tides
Solar heating on the day side and radiative cooling on the night side of a planet can induce pressure difference.
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.
Compared to Earth's atmosphere, thermal tides have a larger influence
on the Martian atmosphere because of the stronger diurnal temperature
contrast.
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.
The atmospheric waves can also travel vertically and affect the
temperature and water-ice content in the middle atmosphere of Mars.
Orographic 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.
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.
Wind modification of the surface
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. The global average migration rate of dunes (2 – 120 m tall) is about 0.5 meter per year.
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.
Movement of sandy features in
Nili Patera dune field on Mars detected by HiRISE. Photo credit: NASA/JPL Caltech/U. Arizona/JHU-APL
Acoustic environment
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 Martian atmosphere, 100 times thinner than the terrestrial atmosphere, than the atmosphere 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 unique Martian conditions, sound
is much quieter, and live music would be more variable, than on Earth.
Atmospheric evolution
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
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 ‰
|
1.56 ‰
|
~6
|
| 12C / 13C
|
85.1 ± 0.3
|
89.9
|
0.95
|
| 14N / 15N
|
173 ± 9
|
272
|
0.64
|
| 16O / 18O
|
476 ± 4.0
|
499
|
0.95
|
| 36Ar / 38Ar
|
4.2 ± 0.1
|
5.305 ± 0.008
|
0.79
|
| 40Ar / 36Ar
|
1900 ± 300
|
298.56 ± 0.31
|
~6
|
| C / 84Kr
|
(4.4–6) × 106
|
4 × 107
|
~0.1
|
| 129Xe / 132Xe
|
2.5221 ± 0.0063
|
0.97
|
~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.
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. Estimates suggest that the initial partial pressure of N2 may have been up to 30 hPa.
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.
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. 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.
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. 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. The huge enrichment of radiogenic 40Ar over primordial 36Ar is also consistent with the impact erosion theory.
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. It is noted that atmospheric-escape-based approach only provides the lower limit for the estimated early water inventory.
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. 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. Nevertheless, photochemical modeling showed that maintaining an atmosphere with this high level of H2 is difficult. SO2 has also been one of the proposed effective greenhouse gases in the early history of Mars. 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.
Atmospheric escape on modern Mars
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
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. While most studies suggested that the escape of hydrogen is close to diffusion-limited on Mars, more recent studies suggest that the escape rate is modulated by dust storms and has a large seasonality. The estimated escape flux of hydrogen range from 107 cm−2 s−1 to 109 cm−2 s−1.
Carbon escape
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:
- 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. 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.
Nitrogen escape
Like carbon, dissociative recombination of N2+ is important for the nitrogen escape on Mars. In addition, other photochemical escape mechanism also play an important role:
- 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.
Oxygen escape
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. Model estimations of oxygen escape rate suggested it can be over 10 times lower than the hydrogen escape rate.
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.
Unexplained phenomena
Detection of methane
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).
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. 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.
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. Before and after that, readings averaged around one-tenth that level. On 7 June 2018, NASA announced a cyclical seasonal variation in the background level of atmospheric methane.
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. 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. Living microorganisms, such as methanogens, are another possible source, but no evidence for the presence of such organisms has been found on Mars. 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.
Lightning events
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. 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.
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.
Super-rotating jet over the equator
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.
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. GCM experiments showed that the thermal tides can play a role in inducing the super-rotating jet. Nevertheless, modeling super-rotation still remains as a challenging topic for planetary scientists.
Potential for use by humans
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).
In 2021, however, the NASA spaceship 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.
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