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〕 * }} | surface_area = | volume = | mass = | density = | surface_grav = | temperatures = yes | temp_name1 = Kelvin | mean_temp_1 = 737 K | temp_name2 = Celsius | mean_temp_2 = 462 °C | mean_name3 = Fahrenheit | mean_temp_3 = | surface_pressure = 92 bar (9.2 MPa) }} NASA's Magellan spacecraft mission discovered that Venus has a geologically young surface with a relatively uniform age of 500±200 Ma (million years). The age of Venus was revealed by the observation of over 900 impact craters on the surface of the planet. These impact craters are nearly uniformly distributed over the surface of Venus and less than 10% have been modified by plains of volcanism or deformation. These observations indicate that a catastrophic resurfacing event took place on Venus around 500 Ma, and was followed by a dramatic decline in resurfacing rate. The radar images from the Magellan missions revealed that the terrestrial style of plate tectonics is not active on Venus and the surface appears to be immobile at the present time. Despite these surface observations, there are numerous surface features that indicate an actively convecting interior. The Soviet Venera landings revealed that the surface of Venus is essentially basaltic in composition based on geochemical measurements and morphology of volcanic flows. The surface of Venus is dominated by patterns of basaltic volcanism, and by compressional and extensional tectonic deformation, such as the highly deformed tessserae terrain and the pancake like volcano-tectonic features known as coronae. The planet's surface can be broadly characterized by its low lying plains, which cover about 80% of the surface, 'continental' plateaus and volcanic swells. There is also an abundance of small and large shield volcanoes distributed over the planet's surface. Based on its surface features, it appears that Venus is tectonically and convectively alive but has a lithosphere that is static. ==Resurfacing hypotheses== The global distribution of impact craters that was discovered by the Magellan mission to Venus has led to numerous theories on Venusian resurfacing. Phillips et al. (1992) developed two conceptual end-member resurfacing models that describe the distribution of impact craters. The first end-member model suggests that a spatially random distribution of craters can be maintained by having short duration resurfacing events of large spatial area that occur in random locations with long intervening time intervals. A special case of this end-member would be global resurfacing events; for this case we would be unable to tell from the current surface whether the last global event was part of a recurring cycle or a singular event in the planet's history. The other end-member is that resurfacing events that wipe out craters are of small spatial area, randomly distributed and frequently occurring. This is effectively a uniformitarian hypothesis as it assumes that geologic activity is occurring everywhere at similar rates. Global events that periodically resurface nearly the entire planet will leave a crater-free surface: craters then occur and aren't subsequently modified until the next global event. Resurfacing events occurring frequently everywhere will produce a surface with many craters in the process of being resurfaced.〔 Thus, the end-members can be distinguished by observing the extent to which the craters have experienced some degree of tectonic deformation or volcanic flooding. Initial surveys of the crater population suggested that only a few percent of the craters were heavily deformed or embayed by subsequent volcanism, thus favoring the "catastrophic resurfacing" end member.〔 A number of geophysical models were proposed to generate a global catastrophy, including *episodic plate tectonics proposed by Turcotte (1993) *a transition from mobile lid to stagnant lid convection proposed by Solomatov and Moresi (1996) * and a rapid transition from a thin to thick lithosphere proposed by Reese et al. (2007) The portion of the planet with large rift zones and superposed volcanoes was found to correlate with a low crater density and an unusual number of heavily deformed and obviously embayed craters.〔 The tessera regions of the planet seem to have a slightly higher than normal percentage of craters, but a few of these craters appear to be heavily deformed. These observations, combined with global geologic mapping activities, lead to scenarios of geologic surface evolution that paralleled the catastrophic geophysical models.〔 The general vision is that the tessera regions are old and date to a past time of more intense surface deformation; in rapid succession the tessera ceased deforming and volcanism flooded the low-lying areas; currently geologic activity is concentrated along the planet's rift zones. 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「Geodynamics of Venus」の詳細全文を読む スポンサード リンク
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