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The downwelling over the nightside causes adiabatic heating of the air, which forms a warm layer in the nightside mesosphere at the altitudes 90–120 km. [3] [2] The temperature of this layer—230 K (−43 °C)—is far higher than the typical temperature found in the nightside thermosphere—100 K (−173 °C). [2]
[90] [91] This makes the Venusian surface hotter than Mercury's, which has a minimum surface temperature of 53 K (−220 °C; −364 °F) and maximum surface temperature of 700 K (427 °C; 801 °F), [92] [93] even though Venus is nearly twice Mercury's distance from the Sun and thus receives only around a quarter of Mercury's solar irradiance ...
If these surface minerals were fully converted and saturated, then the atmospheric pressure would decline and the planet would cool somewhat. One of the possible end states modelled by Bullock and Grinspoon was an atmosphere of 43 bars (42 atm; 620 psi) and a surface temperature of 400 K (127 °C; 260 °F).
Land surface temperature anomalies for a given month compared to the long-term average temperature of that month between 2000-2008. [ 7 ] Sea surface temperature anomalies for a given month compared to the long-term average temperature of that month from 1985 through 1997.
Temperature (K) Mass Notes HIP 78530 b: 2,700 ± 100 [29] 23 M J [29] Likely a brown dwarf. GQ Lupi b: 2,650 ± 100 [30] 20 M J [30] [30] Likely a brown dwarf. CT Chamaelontis b: 2,600 ± 250 [31] 17 M J [31] Likely a brown dwarf. DH Tauri b 2,400 ± 100 [32] 11 M J [32] The following well-known planets are listed for the purpose of comparison ...
During the mapping cycle 1 (left-looking) radar surface mapping on Venus (September 15, 1990 to May 15, 1991), around 70% of the Venusian surface was mapped by synthetic aperture radar. In cycle 2 (right-looking), 54.5% of the surface was mapped, mainly the south pole regions and gaps from cycle 1 during May 15, 1991 to January 14, 1992.
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.
It is sometimes called Earth's "sister planet" due to their similar size, gravity, and bulk composition (Venus is both the closest planet to Earth and the planet closest in size to Earth). The surface of Venus is covered by a dense atmosphere and presents clear evidence of former violent volcanic activity.