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Tectonics and evolution of venus.

R J Phillips, W M Kaula, G E McGill

    Science (New York, N.Y.)
    |May 22, 1981
    PubMed
    Summary
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    Venus tectonics lack Earth-like features such as ocean rises. Its ancient crust and high temperatures likely halted plate tectonics over a billion years ago, with highlands supported by hotspots.

    Area of Science:

    • Planetary Science
    • Geology
    • Geophysics

    Background:

    • Venus exhibits unique global tectonics distinct from Earth's.
    • Surface features include rolling terrain and limited highlands, with gravity positively correlated to topography.
    • An ancient crust and high surface temperatures impede subduction on Venus.

    Purpose of the Study:

    • To analyze the distinctive tectonic processes of Venus.
    • To understand the support mechanisms for Venusian highlands.
    • To investigate the cessation of plate tectonics on Venus.

    Main Methods:

    • Analysis of surface topography and gravity data.
    • Geological modeling of crustal support and thermal regimes.
    • Comparison of Venusian tectonics with terrestrial models.

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    Main Results:

    • Venus lacks Earth-like oceanic ridges; highlands are compensated at ~100 km depth.
    • Gravity and topography show a positive correlation across all wavelengths.
    • Evidence suggests water destabilization and cessation of plate tectonics over 1 billion years ago.

    Conclusions:

    • Venusian highlands are actively supported, likely by mantle plumes or hotspots.
    • The planet's tectonic style is ancient and influenced by its high surface temperature.
    • The absence of Earth-like plate tectonics is linked to the loss of surface water and thermal conditions.