- Main article: Atmosphere of Mars
Mars lost its magnetosphere 4 billion years ago, so the solar wind interacts directly with the Martian ionosphere, keeping the atmosphere thinner than it would otherwise be by stripping away atoms from the outer layer. Both Mars Global Surveyor and Mars Express have detected these ionised atmospheric particles trailing off into space behind Mars. The atmosphere of Mars is now relatively thin. Atmospheric pressure on the surface varies from around 30 Pa (0.03 kPa) sound around 123.521825 dB on Olympus Mons to over 1,155 Pa, 155.193357 (1.155 kPa) in the depths of Hellas Planitia, with a mean surface level pressure of 600 Pa, 149.542425 (0.6 kPa). Mars's mean surface pressure equals the pressure found 35 km above the Earth's surface. This is less than 1% of the surface pressure on Earth (101.3 kPa and 194.091589 dB). The scale height of the atmosphere, about 11 km, is higher than Earth's (6 km) due to the lower gravity. Mars' gravity is only about 38% of the surface gravity on Earth.
The atmosphere on Mars consists of 95% carbon dioxide, 3% nitrogen, 1.6% argon, and contains traces of oxygen and water. The atmosphere is quite dusty, containing particulates about 1.5 µm in diameter which give the Martian sky a tawny color when seen from the surface.
Several researchers claim to have detected methane in the Martian atmosphere with a concentration of about 30 ppb by volume. Since methane is an unstable gas that is broken down by ultraviolet radiation, typically lasting about 340 years in the Martian atmosphere, its presence would indicate a current or recent source of the gas on the planet. Volcanic activity, cometary impacts, and the presence of methanogenic microbial life forms are among possible sources. It was recently pointed out that methane could also be produced by a non-biological process called serpentinization[b] involving water, carbon dioxide, and the mineral olivine, which is known to be common on Mars.
During a pole's winter, it lies in continuous darkness, chilling the surface and causing 25–30% of the atmosphere to condense out into thick slabs of CO2 ice (dry ice). When the poles are again exposed to sunlight, the frozen CO2 sublimes, creating enormous winds that sweep off the poles as fast as 400 km/h. These seasonal actions transport large amounts of dust and water vapor, giving rise to Earth-like frost and large cirrus clouds. Clouds of water-ice were photographed by the Opportunity rover in 2004.
- ↑ Philips, Tony (2001). "The Solar Wind at Mars". Science@NASA. Retrieved on 2006-10-08.
- ↑ R. Lundin, S. Barabash, H. Andersson, M. Holmström, A. Grigoriev, M. Yamauchi, J.-A. Sauvaud, A. Fedorov, E. Budnik, J.-J. Thocaven,2 D. Winningham, R. Frahm, J. Scherrer, J. Sharber, K. Asamura, H. Hayakawa, A. Coates, D. R. Linder, C. Curtis, K. C. Hsieh, B. R. Sandel, M. Grande, M. Carter, D. H. Reading, H. Koskinen, E. Kallio, P. Riihela, W. Schmidt, T. Säles, J. Kozyra, N. Krupp, J. Woch, J. Luhmann, S. McKenna-Lawler, R. Cerulli-Irelli, S. Orsini, M. Maggi, A. Mura, A. Milillo, E. Roelof, D. Williams, S. Livi, P. Brandt, P. Wurz, P. Bochsler (2004). "Solar Wind-Induced Atmospheric Erosion at Mars: First Results from ASPERA-3 on Mars Express". Science 305: 1933–1936. doi:10.1126/science.1101860. PMID 15448263.
- ↑ Cite error: Invalid
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- ↑ Lemmon; et al. (2004). "Atmospheric Imaging Results from Mars Rovers". Science 306: 1753–1756. doi:10.1126/science.1104474. PMID 15576613.
- ↑ V. Formisano, S. Atreya, T. Encrenaz, N. Ignatiev, M. Giuranna (2004). "Detection of Methane in the Atmosphere of Mars". Science 306: 1758–1761. doi:10.1126/science.1101732. PMID 15514118.
- ↑ "Mars Express confirms methane in the Martian atmosphere", ESA (March 30, 2004). Retrieved on 17 March 2006.
- ↑ Martin Baucom (2006). "Life on Mars?". American Scientist 94 (2): 119–120, http://www.americanscientist.org/template/AssetDetail/assetid/49613. Retrieved on 26 February 2007.
- ↑ C. Oze, M. Sharma (2005). "Have olivine, will gas: Serpentinization and the abiogenic production of methane on Mars". Geophys. Res. Lett. 32: L10203. doi:10.1029/2005GL022691.
- ↑ J. T. Mellon, W. C. Feldman, T. H. Prettyman (2003). "The presence and stability of ground ice in the southern hemisphere of Mars". Icarus 169 (2): 324–340. doi:10.1016/j.icarus.2003.10.022, http://adsabs.harvard.edu/abs/2004Icar..169..324M. Retrieved on 26 February 2007.
- ↑ "Mars Rovers Spot Water-Clue Mineral, Frost, Clouds", NASA (December 13, 2004). Retrieved on 17 March 2006.