Earth's crustal evolution
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Crustal evolution regards the formation, existence, destruction and eventual renewal of the rocky crust found on the surface of the Earth.
Evolution on this scale can take place through the unique composition of Earth's crust in comparison to other terrestrial planets. Mars, Venus, Mercury and other planetary bodies possess compositionally uniform crusts unlike that of the Earth where both oceanic and continental plates make up the overall outermost shell.
In particular, crustal evolution represents the growth and destruction rates of both types of crust.
Early crust
Mechanism
The proto-earth was entirely molten due to high temperatures created and maintained by compression of the early atmosphere, rapid axial rotation and regular impacts with neighbouring planetesimals[1]. However, over time Earth began to cool as the frequency of planetary accretion slowed and heat stored within the magma ocean is lost to space through radiation. Once cool enough the peridotite magma began to crystallise
Types of crust
Crustal dichotomy
Impact cratering
Lifespan
Relative ages
Destruction
References
- ^ Erickson, Jon (2002). Historical Geology: Understanding Our Planet's Past. New York: Infobase Publishing. pp. 6–7. ISBN 1438109644.