Search results
Results from the WOW.Com Content Network
Its peak is the highest point on Venus, 11 km (7 mi) above the Venusian average surface elevation. [40] The southern continent is called Aphrodite Terra, after the Greek mythological goddess of love, and is the larger of the two highland regions at roughly the size of South America. A network of fractures and faults covers much of this area. [41]
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.
This is equal to the entire crust of Venus down to a depth of about 21.4 kilometers. Another study [21] concluded that under optimal conditions, on average, 1 cubic meter of basalt rock can sequester 260 kg of carbon dioxide. Venus's crust appears to be 70 kilometres (43 mi) thick and the planet is dominated by volcanic features.
The troposphere on Venus contains 99% of the atmosphere by mass. 90% of the atmosphere of Venus is within 28 km (17.5 mi) of the surface; by comparison, 90% of the atmosphere of Earth is within 16 km (10 mi) of the surface. At a height of 50 km (31 mi) the atmospheric pressure is approximately equal to that at the surface of Earth. [34]
This approximate conjunction is not precise enough to produce a triplet, as Venus arrives 22 hours earlier each time. The last transit not to be part of a pair was in 1396 (the planet passed slightly above the disc of the Sun in 1388); [ 33 ] the next one will be in 3089.
[1] [2] The low eccentricity and comparatively small size of its orbit give Venus the least range in distance between perihelion and aphelion of the planets: 1.46 million km. The planet orbits the Sun once every 225 days [3] and travels 4.54 au (679,000,000 km; 422,000,000 mi) in doing so, [4] giving an average orbital speed of 35 km/s (78,000 ...
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 moons of the trans-Neptunian objects (other than Charon) have not been included, because they appear to follow the normal situation for TNOs rather than the moons of Saturn and Uranus, and become solid at a larger size (900–1000 km diameter, rather than 400 km as for the moons of Saturn and Uranus).