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It is much denser and hotter than that of Earth; the temperature at the surface is 740 K (467 °C, 872 °F), and the pressure is 93 bar (1,350 psi), roughly the pressure found 900 m (3,000 ft) under water on Earth. The atmosphere of Venus supports decks of opaque clouds of sulfuric acid that cover the entire planet, preventing optical Earth ...
Studies have proven that Venus needed liquid water three billion years ago to be able to have such high concentrations of water-related minerals and gases on its surface and in its atmosphere today. However, such studies proved that the liquids would only have lasted up until 700 million to 750 million years ago, before eventually evaporating ...
Venus' atmosphere is about 90 times denser than Earth's and the surface temperature is at least 462 °C (864 °F), conditions which would prevent a standard electronic computer from operating for any significant period of time. [1]
Venus's atmosphere is composed of 96% carbon dioxide. Billions of years ago, when the Sun was 25 to 30% dimmer, Venus's surface temperature could have been much cooler, and its climate could have resembled current Earth's, complete with a hydrological cycle—before it experienced a runaway greenhouse effect. [44]
The current Venusian atmosphere has only ~200 mg/kg H 2 O(g) in its atmosphere and the pressure and temperature regime makes water unstable on its surface. Nevertheless, assuming that early Venus's H 2 O had a ratio between deuterium (heavy hydrogen, 2H) and hydrogen (1H) similar to Earth's Vienna Standard Mean Ocean Water of 1.6×10 −4, [7] the current D/H ratio in the Venusian atmosphere ...
Atmosphere of Venus in UV, by Pioneer Venus Orbiter in 1979. Venus' atmosphere is mostly composed of carbon dioxide. It contains minor amounts of nitrogen and other trace elements, including compounds based on hydrogen, nitrogen, sulphur, carbon, and oxygen. The atmosphere of Venus is much hotter and denser than that of Earth, though shallower.
These three changes are closely interrelated because Venus's extreme temperature is due to the high pressure of its dense atmosphere and the greenhouse effect. The most simple proposal is to "veil" the planet from the sun, thus dropping the temperature low enough to condense or solidify carbon dioxide which would then need to be removed or ...
Venera 4 (Russian: Венера-4, lit. 'Venus-4'), also designated 4V-1 No.310, was a probe in the Soviet Venera program for the exploration of Venus.The probe comprised a lander, designed to enter the Venusian atmosphere and parachute to the surface, and a carrier/flyby spacecraft, which carried the lander to Venus and served as a communications relay for it.