Mars
With a gravitational force just one-third of that on Earth, Mars has only been able to retain a very thin, tenuous atmosphere consisting of 95% carbon dioxide. Atmospheric pressure is highly variable and 170 times weaker than on Earth.
With little heat from the Sun and no significant greenhouse effect, temperatures at the equator vary between –100°C and 0°C.
Most of the changes to Mars’ surface are caused by the winds that sweep across its dry landscape, raising clouds of ochre dust and turning the atmosphere a reddish brown. Violent storms periodically hurl these dust clouds 50 kilometres into the air, totally blocking out the sky.
Mars’ southern ice cap, seen by the Mars Global Surveyor probe. Taken in summer, this photograph shows the ice cap at its narrowest, spanning 430 kilometres.
At the poles, permanent ice caps of frozen water and carbon dioxide (dry ice) advance and recede with the changing seasons, while the rest of the planet is strewn with rocks and dust. Covered with countless meteor craters in its southern hemisphere and with volcanic plains in its northern hemisphere, the surface of Mars has been gouged out by giant canyons that extend from west to east. Its internal structure resembles that of other terrestrial planets, comprising a crust, mantle and core.
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Last updated: May 2003
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More information
Solar System exploration, NASA website
Mars Fact Sheet, National Space Science Data Center (NASA)
Mars exploation, NSSDC (NASA)
Philippe Labrot's website
Planetary photojournal - NASA website
CNES Youth/Education site
Educnet: new information and communication technologies in teaching






