1 / 36

History of Venus

History of Venus. In this lecture. Venus today Comparison to Earth Venusian atmosphere Water and magnetic fields Geologic record Volcanic resurfacing Tectonic features The lack of craters Putting events in order Resurfacing models.

hogan
Download Presentation

History of Venus

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. History of Venus

  2. In this lecture • Venus today • Comparison to Earth • Venusian atmosphere • Water and magnetic fields • Geologic record • Volcanic resurfacing • Tectonic features • The lack of craters • Putting events in order • Resurfacing models Surface history of Venus is only available from ~1.0 Ga onward (not dissimilar to Earth) …as opposed to… Surface activity on the Moon and Mercury mostly died off about 3 Ga Surface activity and history of Mars spans its entire existence

  3. Comparisons to Earth • 81.5% of the mass of the Earth • Slightly higher mean density (5230 kg m-3) • Formed in a similar location – 0.72 AU • Implies a similar bulk composition Venus Earth

  4. Atmosphere of Venus • Massive CO2 atmosphere with intense greenhouse effect • 93 bars,740 K at mean surface elevation • Altitude variations 45-110 bars, 650-755 K • No day/night or equator/pole temperature variations • 3 distinct cloud-decks • Composed of sulfuric acid droplets • Produced by photo-oxidation of SO2 • Effective scavenger of water vapor • Layers differ in particle size • Very reflective (albedo 70%) keeps surface much cooler than it would otherwise be • 100 ms-1 east-west at altitude of 65 km • Drives cloud layer around planet in ~4 days • Reasons for super-rotating atmosphere are unknown • True surface (243 day - retrograde) rotation period found with terrestrial radar.

  5. Topography • Earth has obvious topography dichotomy • High continents • Low ocean floors • Venus has a unimodal hypsogram • No spreading centers • No Subduction zones • No plate tectonics • How is this topography supported??

  6. What went wrong? • Earth and Venus should be the same… • Venus absorbs roughly the same amount of sunlight as the Earth. • Venus has roughly the same amount of carbon as the Earth • …but… • Venus has no plate tectonics • Earth’s carbon get recycled through the crust • Venusian carbon accumulates in atmosphere – regulated by ‘Urey reaction’? CaCO3 + SiO2 = CaSiO3 + CO2 (calcite) + (silica) = (wollastonite) log10PCO2 = 7.797 – 4456/T Equilibrium gives 92 bars at 742 K All these differences can be traced back to the lack of water on Venus

  7. Why didn’t this happen on the Earth ? • Earth has water that rains • Rain dissolves CO2 from the atmosphere • Forms carbonic acid • This acidified rainwater weathers away rocks • Washes into the ocean and forms carbonate rocks • Carbonate rocks eventually recycled by plate tectonics • The rock-cycle keeps all this in balance • Sometimes this gets out of sync e.g. snowball Earth – stops weathering

  8. Venus started with plenty of water • Temperatures were just a little too high to allow rainfall • Atmospheric CO2 didn’t dissolve and form carbonate rocks • Venus and Earth have the same amount of CO2 • Earth’s CO2 is locked up in carbonate rocks • Venus’s CO2 is still all in the atmosphere • Same for sulfur compounds produced by volcanoes • SO2 (sulfur dioxide) on Earth dissolves in the oceans • SO2 on Venus stays in the atmosphere and forms clouds of sulfuric acid

  9. What happened to the water? • Water & CO2 build up in the atmosphere • A very massive atmosphere • A very hot surface • No Magnetic field • Slow spin • Large early impact? • Solar Tides? • Little core convection • Hot surface & thick lithosphere keep core hot • Water disassociated by sunlight • H can thermally escape • Solar wind impinges directly on Venusian ionosphere • Ions can be easily stripped away • Deuterium to Hydrogen ratio: 0.024 • 150 times that of Earth • Indicates significant loss of hydrogen • Sun was 30% fainter in early solar system • Venus may once have been more Earth-like Venus Earth

  10. Landers • Only glimpse of the surface • Soviets had 4 successful Venera landings on Venus • Onboard experiments found basaltic surface • Dark surface, albedo of 3-10% • Surface winds of ~ 0.3-1.0 m/s • Surface temperatures of 740 K • Landers lasted 45-60 minutes Venera 14 – 13 S, 310 E – March 1982

  11. Spherical images can be unwraped into a low-res perspective view • Smooth-ish basaltic rock – low viscosity magmas Venera 13 Baltis Vallis – 6800 km Venera 9 – A Blockier Appearance

  12. Venera 14 Venera 10

  13. Venus rock composition • Sampled in only 7 locations by Soviet landers • Composition consistent with low-silica basalt • Exposed crust is <1 Gyr old though Venera 14

  14. Interpretation of Radar Data • Surface of Venus has been imaged by radar • Pioneer Venus (late 1970’s) • Venera 15 and 16 (1980’s) • Magellan (1992 – 1994) • Backscatter and altimetry • 98% coverage • Side-looking system • No shadows – observation at 0o phase • Light/Dark tones don’t correspond to albedo • Strong radar return from: • Terrain that has roughness on the scale of the radar wavelength • Large-scale slopes facing the spacecraft • High-altitude ‘shiny’ material • High return due to unusual dielectric constant

  15. Physiography • Surface dominated by volcanic material • Plenty of tectonics but no plate tectonics • Over 80% of Venus made up by • Volcanic plains - 70% of surface, low-lying • 9 Volcanic rises – Rift zones and major volcanoes, dynamically supported • 5 Crustal plateaus – Dominated by Tesserae, isostatically compensated • Unusual lack of impact craters • Very young surface 0.5 – 1.0 Gyr

  16. Low-lying Plains • Ridged plains • Smooth Plains • Highlands • Crustal Plateaus • Volcanic Rises

  17. Volcanism on Venus • Range of volcanic styles • Low viscosity plains volcanism  Shield volcanism  highly viscous features Sinuous rills: Baltis Vallis – 6800 km

  18. Some viscous flow features may exist… Pancake domes – Eistla region South Deadman Flow – Long valley, CA

  19. Shield plains • Usually only a few 100 km across • Fields of gentle sloping volcanic shields • Crossed by wrinkle ridges • Shields usually constructed from non-viscous lava • Some shields are steep implying more evolved lava • Venera 8 lander probably sampled one of these areas

  20. Volcanic Plains • Ridged plains – 70 % Venusian surface • Emplaced over a few 10’s Myr • Deformed with wrinkle ridges (compressional faults) • 1-2 km wide, 100-200 km long • High-yield, non-viscous eruptions of basalt • Gentle slopes and smooth surfaces • Long run-out flows 100-200 km • Chemical analysis – Venera 9, 10, 13 & Vega 1, 2 • Total volume of lavas close to 1-2 x 108 km3 • Contain sinuous channels • 2-5 km wide, 100’s km long • Baltis Vallis is 6800 km long, longest channel in the solar system • Thermal erosion by lava • Smooth plains cover 10-15% of Venusian surface • Superposed on ridged plains • Not deformed by wrinkle ridges • Consist of overlapping flows with lobate morphology Sinuous rills: Baltis Vallis – 6800 km

  21. Emplacement of plains material followed by widespread compression • Solomon et al. (and some other papers) describe a climate-volcanism-tectonism feedback mechanism • Resurfacing releases a lot of CO2 causing planet to warm up • Heating of surfaces causes thermal expansion resulting in compressive forces. • Explains pervasive wrinkle ridge formation on volcanic plains

  22. Coronae • Morphologic term • Quasi-circular raised feature • Annulus of concentric fractures and ridges • Radially orientated fractures in their interiors • 360 Coronae identified • Size ranges from 75 to 2000 Km • Interiors raised about 1km • Associated with large amounts of volcanism • Occurred in parallel with volcanic plains formation • Typical formation sequence: • Volcanism • Topographic uplift • Forming radial fractures • Withdrawal of magma • Topographic subsidence • Forming concentric fractures

  23. Highlands • Crustal Plateaus • Volcanic Rises • Low-lying Plains • Ridged plains • Smooth Plains

  24. Volcanic Rises • Nine major volcanic rises • 1000-2400km across • Containing: • Rift zones • Lava flows • Large volcanic edifaces • Associated gravity anomalies • Dynamically supported by a mantle plume • Young • Craters? • Partly uplifted old plains • Superposed features are young though • Usually dominated by: • Rifts • Large shield volcanoes • Coronae

  25. Rifts • Extensional stress from volcanic rise uplift

  26. Crustal Plateaus • Steep-sided, flat-topped, quasi-circular • Isostatically compensated • 1000-3000km across, raised by 0.5-4km • Dominated by Tesserae • Regions of complexly deformed material • Contain several episodes of both extension and compression. • Extremely rough (bright) at radar wavelength • Origin of Tesserae • Current thinking leans toward mantle plume origin • Upwelling mantle plume causes extension • Crust thickens • Partial collapse when plume disappears causes compression

  27. Cratering • Almost 1000 impact craters on Venus • Very young surface • Mean age 750 Myr • 85% of the planets history is missing • All craters at >3 Km • Atmosphere stops smaller impacts • Craters 3-30 km in size have an irregular appearance • Craters >30 km in size appear sharp • Tesserae are the old features • 900 +/- 220 Ma • Volcanic plains have 2 units • Old plains 975 +/- 50 Ma • Young Plains 675 +/- 50 Ma • Volcanic rises have young features • Rifts and large isolated shields • Also contain older uplifted terrain

  28. Crater-less impacts • Impacting bodies can explode or be slowed in the atmosphere • Significant drag when the projectile encounters its own mass in atmospheric gas: • Where Ps is the surface gas pressure, g is gravity and ρi is projectile density • If impact speed is reduced below elastic wave speed then there’s no shockwave – projectile survives • Ram pressure from atmospheric shock • If Pram exceeds the yield strength then projectile fragments • If fragments drift apart enough then they develop their own shockfronts – fragments separate explosively • Weak bodies at high velocities (comets) are susceptible • Tunguska event on Earth • Crater-less ‘powder burns’ on venus • Crater clusters on Mars

  29. ‘Powder burns’ on Venus • Crater clusters on Mars • Atmospheric breakup allows clusters to form here • Screened out on Earth and Venus • No breakup on Moon or Mercury Mars Venus

  30. Distribution of craters • Appears completely random • Some plains units may be older • Simulations taking in account atmospheric screening give ages of 700-800 Myr • 26,000 impactors > 1011 kg to produce 940 craters • Atmosphere is very effective at blocking impacts

  31. Catastrophic resurfacing? • Low crater population • Catastrophic resurfacing • Continual resurfacing (like Earth) • Craters are indistinguishable from a random distribution • ~80% of craters are pristine • Others have superposed tectonics or volcanic material Heloise crater – 38 km Balch crater – 40 km

  32. Catastrophic resurfacing? • One timeline… • Tesserae form first • Most craters on them are removed by tectonics • Extensive Plains volcanism • Resurfaces most of the planet • Global compression creates ridged plains • Additional volcanism makes smooth plains • Back to extension • Volcanic rises • Rifts

  33. Not so catastrophic resurfacing? • One timeline… • Volcanic rises and plains form continuously • Focused mantle plumes for rises • Diffuse upwelling for plains volcanism • Volcanic rises evolve in Tesserae Transition to thick lithosphere ~700Ma • New volcanic rises can no longer evolve into tesserae • Lack of transitional features means this occurred quite fast • Extension allows for coronae and rifts • Plains volcanism shuts off

  34. The future for Venus • Can a thick lid break? • Lack of water is a problem • Thermal energy builds in the mantle • Transient subduction? • Happened in the past? Venusian Geological Periods

  35. Comparison to Earth • Almost the same mass and bulk composition • Only 2 Mars-masses apart (+/- 1 giant impact) • Probably the same water budget • Asthenosphere likely in early history • Basalt to eclogite transition is deeper on Venus (65 km) • This could inhibit the initiation of plate tectonics • Provides more time to outgas CO2 and initiate runaway greenhouse • Water outgassed and destroyed over geologic time

  36. Summary • Venus is like the Earth in a lot of ways • Size, density, composition, orbit …but… • A runaway greenhouse atmosphere has vaporized all the water • Lack of a magnetic field means that the water is easily removable • No water in the mantle means no plate-tectonics or carbon cycle • So the atmosphere had a profound effect on surface processes • Volcanic (low-viscosity basalt) plains dominate the surface • Lengthy sinuous rills • Ridged plains smooth plains, and shield plains • Pancake domes might indicate some silica-rich volcanism • 5 main crustal plateaus • Contain extensively fractured tesserae • High standing remnants, perhaps once supported by mantle plumes • 9 main volcanic rises • Currently supported by a mantle plume • Extension creates rifts • Coronae are interpreted as collapsed upwellings • Cratering record indicate a very young surface • Lack of degraded craters has been interpreted as a catastrophic resurfacing < 1Ga …OR… • …surface geology can also be interpreted in terms of more gradual processes • With a transition to a thick lithosphere within the past Gyr

More Related