1. 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

2. Venus Data (Table 12-1)

3. Venus Data: Numbers Diameter:12,104.km0.949. Earth Mass:4.9. 10 24 kg0.815. Earth Density:5.24. water0.953. Earth Orbit:1.1. 10 8 km0.72 AU Day:– 243.01 days– 243.01. Earth Year:224.70 days0.62. Earth

4. 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% CO 2 –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

5. Venus Phases & Angular Diameters http://www.spacestationinfo.com/images/venus-phase1.gif

6. Relative Sizes of Terrestrial Planets http://upload.wikimedia.org/wikipedia/commons/d/dd/4_Terrestrial_Planets_Size_Comp_True_Color.png

7. 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 Greatesteasternelongation is ~ 47°Evening Greatestwesternelongation is ~ 47°Morning

8. Orbits of Venus & Earth

9. Venus’s Greatest Elongations Eastern (Evening)Western (Morning) 1 November 201322 March 2014 6 June 201526 October 2015 12 January 20173 June 2017 17 August 20186 January 2019 24 March 202013 August 2020

10. Venus’s Atmosphere: A First Look Venus is perpetually cloud-covered –This makes Venus extremely bright –Clouddetails are best seen withultraviolet ’s –Surfacedetails are only seen withradar ’s Earth-basedimaging systems Magellanorbital mission The Venusian atmosphere is extremely dense –About 93 times more than Earth

11. Venus Seen In Ultraviolet Light

12. Venus’s Slow Retrograde Rotation Observational difficulties –Perpetual cloud cover obscures the surface Surface can be seen only using radar ’s –Clouds encircle the planet in ~ 4 days Best seen in UV ’s Successful observations –Doppler shift analyses in the early 1960’s Transmit one precise Receive a slightly spread out range of ’s –One edge of Venus is movingtowardEarth –One edge of Venus is movingaway fromEarth –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

13. Prograde & Retrograde Rotation

14. Venus’s a Hot, Dense Atmosphere Insolation[Incoming solar radiation] –Venus averages ~ 0.72 AU from the Sun 1 / 0.72 2 = 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 –CO 2 is extremely common in volcanic eruptions CO 2 is an excellent absorber of infrared [heat] radiation An important comparison –Venus:96.5% CO 2 increases temperature ~ 400°C –Earth:0.04% CO 2 increases temperature ~ 36°C

15. 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 10 9 x more sulfur than Earth’s air Probable cause –Like CO 2, sulfur is common in volcanic eruptions No oceans to absorb this sulfur Instances of increased Venusian sulfur levels –Late 1950’sEarth-based observations –Late 1970’sPioneer Venus Orbiter

16. Venusian Cloud Layers

17. 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

18. Venusian Atmospheric Circulation

19. Venusian Climatic Evolution Proto-atmospheres –Venus & Earth were probably remarkably similar Countless volcanic eruptions provided H 2 O, CO 2 & SO 2 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

20. 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

21. Volcanoes On Venus & Earth VenusEarth 0% oceans~ 70% oceans Gas enters atmosphereGas absorbed by oceans High CO 2 & SO 2 concentrationsLow CO 2 & SO 2 concentrations Yellow skyBlue sky

22. Venus: A Mercator Projection

23. Venus: A Global Perspective

24. Volcanic Activity On Venus & Earth

25. Aine Corona With Pancake Domes

26. Solar System’s Longest Channel

27. Theia Mons (Earth Radar Image)

28. Maat Mons (Vertical Exag. = 22.5)

29. 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

30. 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 CO 2 & SO 2 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