Composition and Surface Pressure

Carbon dioxide constitutes 95.3 percent of the atmosphere by weight, nine times the quantity now in Earth's much more massive atmosphere. Much of Earth's carbon dioxide, however, is chemically locked in sedimentary rocks; the amount in the Martian atmosphere is less than a thousandth of the terrestrial total. The balance of the Martian atmosphere consists of molecular nitrogen, water vapour, and noble gases (argon, neon, krypton, and xenon). There are also trace amounts



percentage by weight

carbon dioxide (CO2)


molecular nitrogen (N2)


argon (Ar)


molecular oxygen (O2)


carbon monoxide (CO)


water vapour (H2O)


neon (Ne)


krypton (Kr)


xenon (Xe)


of gases that have been produced from the primary constituents by photochemical reactions, generally high in the atmosphere; these include molecular oxygen, carbon monoxide, nitric oxide, and small amounts of ozone.

The lower atmosphere supplies gas to the planet's ionosphere, where densities are low, temperatures are high, and components separate by diffusion according to their masses. Various constituents in the top of the atmosphere are lost to space, which affects the isotopic composition of the remaining gases. For example, because hydrogen is lost preferentially over its heavier isotope deuterium, Mars's atmosphere contains five times more deuterium than Earth's.

Although water is only a minor constituent of the Martian atmosphere (a few molecules per 10,000 at most), primarily because of low atmospheric and surface temperatures, it plays an important role in atmospheric chemistry and meteorology. The Martian atmosphere is effectively saturated with water vapour, yet there is no liquid water present on the surface. The temperature and pressure of the planet are so low that water molecules can exist only as ice or as vapour. Little water is exchanged daily with the surface despite the very cold nighttime surface temperatures.

Water vapour is mixed uniformly up to altitudes of 10-15 km (6-9 miles) and shows strong latitudinal gradients that depend on the season. The largest changes occur in the northern hemisphere. During

Seasonal water-ice ground frost on Mars, in a photograph taken by the Viking 2 lander at its high-latitude (48° N) landing site in Utopia Planitia on May 18,1979. NASA/JPL

summer in the north, the complete disappearance of the carbon dioxide cap leaves behind a water-ice cap. Sublimation of water from the residual cap results in a strong north-to-south concentration gradient of water vapour in the atmosphere. In the south, where a small carbon dioxide cap remains in summer and only a small amount of water ice has been detected, a strong water vapour gradient does not normally develop in the atmosphere.

The atmospheric water vapour is believed to be in contact with a much larger reservoir in the Martian soil.

Subsurface layers of ice are thought to be ubiquitous on Mars at latitudes poleward of 40°; the very low subsurface temperatures would prevent the ice from subliming. The 2001 Mars Odyssey spacecraft confirmed that ice is present within a metre of the surface at latitudes higher than 60°, and the Phoenix lander found ice below the surface at 68° N, but it is not known how deep the ice layer extends. In contrast, at low latitudes ice is unstable, and any ice present in the ground would tend to sublime into the atmosphere.

Isotopic measurements suggest that larger amounts of carbon dioxide, nitrogen, and argon were present in the atmosphere in the past and that Mars may have lost much of its inventory of volatile substances early in its history, either to space or to the ground (i.e., locked up chemically in rocks). Mars may once have had a much thicker atmosphere that was lost to the surface through chemical reactions, which formed carbonates, and to space through large asteroid impacts, which blew off atmospheric gases.

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