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Venus surface, fairly flat but varied terrain

Planet Venus surface facts obtained by radar

Most of the topographical information about Venus’ surface was obtained by the Soviet missions Venera 15 and 16 and by the American space probes Pioneer et Magellan during the period 1978 to 1994. Our knowledge concerns about 98% of the surface.

The only way to penetrate Venus’ cloud layer is with radar, bouncing it back off the surface from an orbiting probe or even from the Earth. In fact, many images were obtained in the middle of the 70s with the giant antenna at Arecibo in Porto Rico giving a resolution of 12 cm.

The radar surveys indicate a varied terrain with:

  • mountains
  • plains
  • high plateaus
  • volcanoes
  • crest
  • impact craters

Venus surface color

The planet’s surface seems to be orange which could be due to oxidation identical to that seen on Mars.

Young and flat landscape

The age of the crust has been evaluated at 500 million years, which is young in the history of the solar system. Lunar continents are over 4 billion years old. The dating is done by counting the number of craters and the orbit of the planet. More craters mean an older surface. Venus reveals about 1000 impact craters.

As there are no oceans on Venus there is also no ‘sea-level’ reference. Planetologists have taken the average planetary radius as a reference. This is 6051.84 km.

Globally, Venus is a fairly flat terrain; about 60% of the surface doesn’t rise more than 500m above the average level. Altitude variations are weak, about 2 to 3 km, except for a few mountainous regions. The ‘continents’ rise about 10 km, compared to a difference of 25km on Mars and of 20km on Earth.

Surface spread on Mars Venus Earth
Spread of surface on Mars, Earth and Venus. On Earth, variations group around 2 distinct base levels: the raised continents and the ocean floor. Venus is particularly flat: about 60% of the terrain is at less than 500 m from the average level, fixed at 6051.84 km. Only a few structures are higher. In comparison, Mars surface structures are spread over a wider interval of levels but do not show, as for the Earth, a double peaked distribution. (Credit: 2003, Professor Kenneth R. Lang, Tufts University)

False colour image obtained from radar data from the orbiter Pioneer-Venus. Colours indicate the altitude – red being the highest and blue being the lowest. A few geographical markers are named: in the north-west, the Ishtar Terraand Lakshmi Planum plateaus culminate in Mount Maxwell; south of the equator the Aphrodite Terra plateau, with Maat Mons at its eastern tip; in the south east Alpha Regio and to the west Beta Regio; in light blue we see the vast plains of Venus and in dark blue the deepest depressions. (Credit: NASA/JPL)