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The surface of Venus is comparatively flat. When 93% of the topography was mapped by Pioneer Venus Orbiter, scientists found that the total distance from the lowest point to the highest point on the entire surface was about 13 kilometres (8.1 mi), about the same as the vertical distance between the Earth's ocean floor and the higher summits of the Himalayas.
The mesosphere of Venus can be divided into two layers: the lower one between 62 and 73 km [43] and the upper one between 73 and 95 km. [28] In the first layer the temperature is nearly constant at 230 K (−43 °C). This layer coincides with the upper cloud deck.
Conditions perhaps favourable for life on Venus have been identified at its cloud layers. Venus may have had liquid surface water early in its history with a habitable environment, [24] [25] before a runaway greenhouse effect evaporated any water and turned Venus into its present state. [26] [27] [28] The rotation of Venus has been slowed and ...
The surface of Venus is dominated by geologic features that include volcanoes, large impact craters, and aeolian erosion and sedimentation landforms. Venus has a topography reflecting its single, strong crustal plate, with a unimodal elevation distribution (over 90% of the surface lies within an elevation of -1.0 and 2.5 km) [1] that preserves geologic structures for long periods of time.
The story appears to have been different on Mars, the fourth planet from the sun. Surface features on Mars indicate it had an ocean of liquid water billions of years ago. No such features have ...
Much of Venus' surface appears to have been shaped by volcanic activity. Overall, Venus has several times as many volcanoes as Earth, and it possesses some 167 giant volcanoes that are over 100 kilometres (62 mi) across. The only volcanic complex of this size on Earth is the Big Island of Hawaii. However, this is not because Venus is more ...
Different missions have mapped different cartographic quadrangles of the surface of Venus. They applied different mapping schemes and came up with different classifications of Venusian units. Here is a table comparing the different mapping scheme and unit identification by the Magellan science team (1994), [ 11 ] Vicki L. Hansen (2005) [ 12 ...
No secondary characteristics have been observed around exoplanets. The sub-brown dwarf Cha 110913−773444, which has been described as a rogue planet, is believed to be orbited by a tiny protoplanetary disc, [150] and the sub-brown dwarf OTS 44 was shown to be surrounded by a substantial protoplanetary disk of at least 10 Earth masses. [151]