11b. Cloud-Covered Venus
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Transcript of 11b. Cloud-Covered Venus
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11b. Cloud-Covered Venus• The Venusian atmosphere• Venus has slow retrograde rotation• Venus has a hot dense atmosphere• Volcanic eruptions form Venusian clouds• Climatic evolution on Venus• Venus shows no evidence of plate tectonics
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Venus Data (Table 11-2)
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Mercury-Venus-Mars Relative Sizes
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Venus Data: Numbers• Diameter: 12,104. km 0.949 . Earth• Mass: 4.9 . 1024 kg 0.815 . Earth• Density: 5.24 . water 0.953 . Earth• Orbit: 1.1 . 108 km 0.72 AU• Day: – 243.01 days – 243.01 . Earth• Year: 224.70 days 0.62 . Earth
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Venus Data: Special Features• Venus is the second planet from the Sun• Venus is the second largest terrestrial planet• Venus has many active volcanoes• Venus is almost a twin of the Earth except …
– Venus has ~ 93 times Earth’s atmosphere– Venus’ atmosphere is ~ 96% CO2– Venus is perpetually cloud covered– Venus’ average surface temperature is ~ 480°C
• Venus’ surface can be “seen” only with radar• Venus is very easy to observe from Earth
– Venus is seen as much as 47° away from the Sun– Venus goes through phases much like the Moon
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Venus Phases & Angular Diameters
http://www.spacestationinfo.com/images/venus-phase1.gif
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Relative Sizes of Terrestrial Planets
http://upload.wikimedia.org/wikipedia/commons/d/dd/4_Terrestrial_Planets_Size_Comp_True_Color.png
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Venus As Seen From Earth• Venus is outshone only by the Sun & Moon
– Venus is very close to the Sun• Venus is ~ 0.7 AU from the Sun
– Venus is very close to the Earth• Venus is ~ 0.3 AU from the Earth at inferior conjunction
– Venus is very large• Venus is ~ 95% the diameter of Earth
– Venus has an albedo of ~ 0.59• Venus is perpetually cloud-covered
• Venus has large elongations– The Venusian orbit is nearly circular
• Greatest eastern elongation is ~ 47°Evening
• Greatest western elongation is ~ 47°Morning
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Orbits of Venus & Earth
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Venus’s Greatest ElongationsEastern (Evening) Western (Morning)
27 March 2012 15 August 2012
1 November 2013
22 March 2014
6 June 2015 26 October 2015
12 January 2017 3 June 2017
17 August 2018
6 January 2019Venus Elongation Explorer
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Venus’s Atmosphere: A First Look• Venus is perpetually cloud-covered
– This makes Venus extremely bright– Cloud details are best seen with ultraviolet l’s– Surface details are only seen with radar l’s
• Earth-based imaging systems• Magellan orbital mission
• The Venusian atmosphere is extremely dense– About 93 times more than Earth
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Venus Seen In Ultraviolet Light
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Venus’s Slow Retrograde Rotation• Observational difficulties
– Perpetual cloud cover obscures the surface• Only seen in radar l’s
– Clouds encircle the planet in ~ 4 days• Best seen in ultraviolet l’s
• Successful observations– Doppler shift analyses in the early 1960’s
• Transmit one precise l• Receive a slightly spread out range of l’s
– One edge of Venus is moving toward Earth– One edge of Venus is moving away from Earth
– Results• Venus rotates on its axis in a retrograde direction
– Uranus & Pluto also exhibit retrograde axial rotation• Venus’s day is ~ 243 Earth days long
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Prograde & Retrograde Rotation
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Venus’s a Hot, Dense Atmosphere• Insolation [Incoming solar radiation]
– Venus averages ~ 0.72 AU from the Sun• 1 / 0.722 = 1 / 0.52 = ~ 1.93 > sunlight than Earth
– Venus would be hotter even w/Earth’s atmosphere• Venusian environment
– Intense sunlight evaporated Venus’s oceans– Volcanic gases directly enter Venus’s atmosphere
• Most of Earth’s volcanic gases dissolve in ocean water– CO2 is extremely common in volcanic eruptions
• CO2 is an excellent absorber of infrared [heat] radiation• An important comparison
– Venus: 96.5% CO2 increases temperature ~ 400°C
– Earth: 0.04% CO2 increases temperature ~ 36°C
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Volcanic Eruptions Produce Clouds• Atmospheric sulfur compounds
– Fractional amounts• Venus ~1.5 . 10–2 of all atmospheric
gases• Earth ~1.0 . 10–9 of all atmospheric
gases– Venus has ~ 93 times more atmosphere than Earth
• Venus’s air has ~ 1.35 109 x more sulfur than Earth’s air• Probable cause
– Like CO2, sulfur is common in volcanic eruptions• No oceans to absorb this sulfur
• Instances of increased Venusian sulfur levels– Late 1950’s Earth-based observations– Late 1970’s Pioneer Venus Orbiter
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Venusian Cloud Layers
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Venera 13 Images Venus’s Surface
Venusian rocks appear orange because of cloud colors.
The same picture corrected to remove atmospheric colors.
1 March 1982
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Venusian Atmospheric Circulation
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Venusian Climatic Evolution• Proto-atmospheres
– Venus & Earth were probably remarkably similar• Countless volcanic eruptions provided H2O, CO2 & SO2
• Proto-Sun– Infant Sun produced only ~70% of today’s energy
• All stars gradually increase their energy output
• Climatic evolution– Infant Venus was cool enough to have liquid water
• Single-celled life forms may have evolved on Venus– Juvenile Venus became too hot to have oceans
• The same fate faces Earth in ~ 1 billion years
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Venus Shows No Plate Tectonics• Expected signs
– Globe-circling volcanic mountain chains– Extensive sets of transform faults– Extremely long subduction trenches
• Observed signs– No elongated volcanic mountain chains
• Substantial evidence of hot-spot volcanoes– No confirmed transform faults– No confirmed subduction trenches
• Probable cause– No oceans to affect subduction zone activity
• Venusian lithosphere is too hot & soft to sustain forces• Subducted water promotes lower temperature melting
• “Flake [Blob] tectonics”
Pancake domes
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Mantle Convection: Earth & Venus
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Volcanoes On Venus & Earth
VenusEarth0% oceans ~ 70% oceansGas enters atmosphere Gas absorbed by oceans
High CO2 & SO2 concentrations Low CO2 & SO2 concentrations
Yellow sky Blue sky
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Venus: A Mercator Projection
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Venus: A Global Perspective
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Venus: A 3-D Elevation Model
Magellan: Venus False-Color Terrain [HD]
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Volcanic Activity On Venus & Earth
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Aine Corona With Pancake Domes
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Solar System’s Longest Channel
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Theia Mons (Earth Radar Image)
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Maat Mons (Vertical Exag. = 22.5)
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Spacecraft Exploration of Venus• Russia
– Venera missions• 10 of 16 spacecraft successfully arrived at Venus• Venera 4 entered the atmosphere on 18 October 1967• Venera 7 soft-landed on 15 December 1970• Venera 12 operated ≥110 minutes on 21 December 1978
• United States– Voyager missions
• Primarily orbiters with low-resolution radar images– Magellan mission
• High-resolution radar images of almost the entire surface
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• Venus as seen from Earth– Very bright & excellent elongations– Distinct phases much like the Moon
• Perpetual cloud cover– Obscures the Venusian surface– Encircles the planet in only ~4 days– Radar needed to penetrate clouds
• Axial rotation– Retrograde, once in ~243 Earth days– Uranus & Pluto also retrograde
• The Venusian atmosphere– Basic properties
• Dominance of CO2 & SO2
• High temperature & pressure• Apparent lack of liquid water
– Evolution• Initially much like Earth’s atmosphere• Solar radiation increased ~30%
• No plate tectonics on Venus– None of the classic evidence– Absence of oceans probably the cause– Evidence of “blob” tectonics
• Abundant pancake domes• Spacecraft exploration of Venus
– Russia– United States
Important Concepts