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This map shows a portion of the surface of Mars.
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Image from: NASA

Martian Global Geography

The surface of Mars consists of highlands and lowlands. The highlands are in the southern hemisphere (the bottom of the figure), and the lowlands are in the northern hemisphere of Mars (top of the figure). The lowlands contain the Tharsis Ridge, where many of the largest volcanoes of Mars are located. Next to the Tharsis Ridge is Valles Marineris, a very long canyon of Mars. The high resolution topographic map, which can be viewed by clicking on the image to the left, shows these regions in better detail. Measurements returned by Mars Global surveyor demonstrate the severe height difference between these two regions of Mars.

The highlands have tons of craters. They are the oldest portion of Mars. The lowlands are younger and so do not contain as many craters as the highlands.

Not seen clearly in this image are the Martian polar caps. Besides ice, the southern polar region of Mars contains other interesting geologic features such as layered terrain and giant sanddunes. This region was suppose to be explored by the Mars '98 mission.

Last modified April 27, 2001 by Jennifer Bergman.

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Windows to the Universe, a project of the National Earth Science Teachers Association, is sponsored in part is sponsored in part through grants from federal agencies (NASA and NOAA), and partnerships with affiliated organizations, including the American Geophysical Union, the Howard Hughes Medical Institute, the Earth System Information Partnership, the American Meteorological Society, the National Center for Science Education, and TERC. The American Geophysical Union and the American Geosciences Institute are Windows to the Universe Founding Partners. NESTA welcomes new Institutional Affiliates in support of our ongoing programs, as well as collaborations on new projects. Contact NESTA for more information. NASA ESIP NCSE HHMI AGU AGI AMS NOAA