Tectonics Terrestrial Planets2

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Information about Tectonics Terrestrial Planets2

Published on April 7, 2008

Author: Mahugani

Source: authorstream.com

What do we mean by “tectonics?”:  What do we mean by “tectonics?” Movement of a planet’s surface Movement = ??? What Drives Tectonics?:  What Drives Tectonics? What Drives Tectonics?:  What Drives Tectonics? Types of Movement:  Types of Movement Types of Movement:  Types of Movement Types of Movement:  Types of Movement Slide9:  Mercury Geologically inactive (3.7 Ga) Features resulting from compressive forces Slide10:  Venus Possibly geologically active Volcanoes = heat loss Lava flows (craters  young) Thick crust; convecting mantle Wrinkle ridges, extensional zones Slide11:  Alpha Regio Tesserae - highly deformed older terrain (< 1 Ga) More cratered Embayed by lava flows Slide12:  Maat Mons – 8 km high, Aphrodite Terra Region Slide13:  Mars Probably geologically active Volcanoes = heat loss Thick crust; convecting mantle Wrinkle ridges, extensional zones - BIG Slide14:  Olympus Mons 24 km high 550-600 km across Thick crust! Mars:  Mars dfldjfkdkfj Volcanoes on Mars:  Volcanoes on Mars http://volcano.und.nodak.edu/vwdocs/planet_volcano/mars/Overview.html Martian Volcanoes:  Martian Volcanoes Less gravitational pull; volcanoes larger before collapsing under own weight Hot spots and crust are stationary Slide18:  It’s still all about heat loss! Slide19:  Heat from Impacts, differentiation, radioactive decay Differentiation of layers Continued differentiation - volcanism, tectonism All are differentiated All have been cooling – unique signature Moon and Mercury – solid core; geologically inactive; conduction Mars and Venus – solid core; geologically active; convection in mantle Earth ….

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