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Mars CO2 Ice Polar Caps

  • François Forget
Part of the Astrophysics and Space Science Library book series (ASSL, volume 227)

Abstract

The Martian Polar caps have been observed for more than two centuries by terrestrial observers. Following the first observations by J. Cassini and C. Huygens, Herschel (1784) first described their seasonal characteristics. From Earth, they appear like white bright features waxing and waning over a Mars year. Because of the 25.1° inclination of Mars’equator to its orbit plane, the seasons on Mars are much like their terrestrial counterparts. By analogy with the Earth, most observers assumed that the Martian polar caps were composed of water frost, until the first space probes to Mars. Following the Mariner 4 mission in 1965, Leighton and Murray (1966) used a simple thermal model to reveal the processes which control the Martian seasonal polar caps: during the fall and winter seasons at high latitudes, the local surface and atmospheric temperatures become cold enough to reach the frost point of CO2, the major constituent of the thin Martian atmosphere. CO2 condenses and forms CO2 ice deposits on the surface. During the spring and summer seasons in a given hemisphere, the seasonal CO2 cap sublimates back into the atmosphere. Spectroscopic observations later confirmed the CO2 composition (Herr and Pimentel, 1969; Larson and Fink, 1972).

Keywords

Dust Storm Polar Night Sublimation Rate Martian Climate Global Dust Storm 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer Science+Business Media Dordrecht 1998

Authors and Affiliations

  • François Forget
    • 1
  1. 1.Laboratoire de Météorologie Dynamique du CNRSUniversité Paris 6Paris Cedex 05France

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