9.5-Geology of Venus, 9.6-Geology of Earth
9.5-Geology of Venus, 9.6-Geology of Earth

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University of Toronto St. George
Astronomy & Astrophysics

9.5 Geology of Venus -surface is searing hot with brutal pressure -radius is only about 5% smaller than Earth -Radar mapping: a way to study its geological features through the bouncing of radio waves off the surface and using the reflections to create a 3-D images of the surface -has some impact craters but far less than Mercury, the Moon or Mars -the surface is about the same age everywhere -surface of Venus is about 750 million years old -no craters from the heavy bombardment remain -lacks small craters they burn up as they enter Venus thick atmosphere -volcanism is clearly important -abundant evidence of lava plains and many volcanic mountains -outgassing supplies sulfur dioxide to the atmosphere the clouds contain sulfuric acid -tectonic in origin -curst is quite contorted surface appears to be fractured in a regular pattern -other tectonic feature, coronae, point directly to mantle convection on Venus -probably formed by hot, rising plumes in the mantle (may also push lava up to surface) -lots of volcanoes around the coronae -lack erosion on Venus compared to Earth -far too hot for any type of rain or snow has virtually no wind or weather because of its slow rotation (once every 243 days) -lack of plate tectonics suggests -weaker mantle convection -lithosphere somehow resists fracturing -lack of plate tectonics because of its high surface temperature leading to loss of water and lithosphere thickening 9.6 Geology of Earth -remains volcanically and tectonically active -outgassing liquid because the temperatures are in range -erosio
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