Atmosphere of Mars Totally Explained

Everything about Atmosphere Of Mars totally explained

Carbon dioxide	95.32%
Nitrogen	2.7%
Argon	1.6%
Oxygen	0.13%
Carbon monoxide	0.07%
Water vapor	0.03%
Nitric oxide	0.013%
Neon	2.5 ppm
Krypton	300 ppb
Formaldehyde	130 ppb (External Link)
Xenon	80 ppb
Ozone	30 ppb
Methane	10.5 ppb

Mars, the fourth planet from the Sun, has a very different atmosphere from that of Earth. There has been much interest in studying its composition since the recent detection of a small amount of methane, which may signal life on Mars.
The atmosphere of Mars is relatively thin, and the atmospheric pressure on the surface varies from around 30 Pa (0.03 kPa) on Olympus Mons's peak to over 1155 Pa (1.155 kPa) in the depths of Hellas Planitia, with a mean surface level pressure of 600 Pa (0.6 kPa), compared to Earth's 101.3 kPa. However, the scale height of the atmosphere is about 11 km, somewhat higher than Earth's 6 km. The atmosphere on Mars consists of 95% carbon dioxide, 3% nitrogen, 1.6% argon, and contains traces of oxygen, water, and methane. The atmosphere is quite dusty, giving the Martian sky a color when seen from the surface; data from the Mars Exploration Rovers indicates the suspended dust particles are roughly 1.5 micrometres across.

Structure

Mars' atmosphere is composed of the following major divisions:

Lower Atmosphere: This is a warm region affected by heat from airborne dust and from the ground.

Middle Atmosphere: Mars has a jetstream which flows in this region.

Upper Atmosphere, or Thermosphere: This region has very high temperatures caused by heating from the Sun. Here, atmospheric gases start to separate from each other rather than forming the even mix found in the lower atmospheric layers.

Exosphere: 200 kilometers and higher. This region is where the last wisps of atmosphere merge into space. There is no hard boundary so it's very difficult to tell where the atmosphere ends.

Composition

Carbon dioxide

The main component of the atmosphere of Mars is carbon dioxide (CO₂). During the Martian winter the poles are in continual darkness and the surface gets so cold that as much as 25% of the atmospheric CO₂ condenses at the polar caps into solid CO₂ ice (dry ice). When the poles are again exposed to sunlight during the Martian summer, the CO₂ ice sublimes back into the atmosphere. This process leads to a significant annual variation in the atmospheric pressure and atmospheric composition around the Martian poles.

Argon

The atmosphere of Mars is considerably enriched with the noble gas argon in comparison to that atmosphere of the other planets within the solar system. Unlike carbon dioxide, the argon content of the atmosphere doesn't condense, and hence the total amount of argon in the Mars atmosphere is constant. However, the relative concentration at any given location can change as carbon dioxide moves in and out of the atmosphere. Recent satellite data shows an increase in atmospheric argon over the southern pole in autumn, which dissipates the following spring.

Water

Other aspects of the Martian atmosphere vary significantly. As carbon dioxide sublimes back into the atmosphere during the martian summer, enormous winds sweep off the poles at speeds approaching 250 mph (400 km/h). These seasonal actions transport large amounts of dust and water vapor giving rise to Earth-like frost and large cirrus clouds. These clouds of water-ice were photographed by the Opportunity rover in 2004.

Methane

Trace amounts of methane, at the level of several parts per billion, were first reported in Mars' atmosphere by a team at the NASA Goddard Space Flight Center in 2003. In March 2004 the Mars Express Orbiter and ground based observations from Canada-France-Hawaii Telescope also suggested the presence of methane in the Martian atmosphere, with a concentration of about 10 ppb by volume. The presence of methane on Mars is very intriguing, since as an unstable gas it indicates that there must be (or have been within the last few hundred years) a source of the gas on the planet. It is estimated that Mars must produce 150 ton/year of methane. Volcanic activity, comet impacts, and the existence of life in the form of microorganisms such as methanogens are among possible but as yet unproven sources. The methane appears to occur in patches, which suggests that it's being rapidly broken down before it has time to become uniformly distributed in the atmosphere, and so it's presumably also continually being released to the atmosphere. Plans are now being made to look for other companion gases that may suggest which sources are most likely; in the Earth's oceans biological methane production tends to be accompanied by ethane, while volcanic methane is accompanied by sulfur dioxide.
It was also recently shown that methane could be produced by a non-biological process involving water, carbon dioxide, and the mineral olivine, which is known to be common on Mars. The required conditions for this reaction (for example temperature and pressure) don't exist on the surface, but likely exist within the crust. To prove this process is occurring, serpentine, a mineral by-product of the process would be detected.
The ESA found that the concentrations of methane in the martian atmosphere wasn't even, but rather that it coincided with the presence of water vapor. In the upper atmosphere these two gasses are uniformly distributed, but near the surface they concentrate in three equatorial regions, namely Arabia Terra, Elysium Planitia, and Arcadia Memnonia. Planetary scientist David H. Grinspoon (Southwest Research Institute) feels that the coincidence of water vapor and methane increases the chance of a biological source, but cautions that it's uncertain how life could have survived so long on a planet as inhospitable as Mars.

Potential for utilization by humans

The atmosphere of Mars is a resource of known composition which is available at any landing site on Mars. For this reason, it has been proposed that human exploration of Mars could use carbon dioxide from Martian atmosphere as feedstock to manufacture rocket fuel to use for the return mission. Mission studies which 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 utilization of the carbon dioxide are the Sabatier reaction, converting atmospheric carbon dioxide along with additional hydrogen to produce methane and oxygen, and electrolysis, using a zirconia solid oxide electrolyte to split the carbon dioxide into oxygen and carbon monoxide.
However, if humans are to colonize Mars in the future, they'd likely need as many greenhouse gases as they can get in order to maintain a warm climate. So using the Martian atmosphere as a consumable resource with no intentions of replenishing it may be considered dubious. (see terraforming mars)

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