By Martin J. van Kranendonk, R. Hugh Smithies and Vickie C. Bennett (Eds.)
Earth's Oldest Rocks offers a complete evaluation of all features of early Earth, from planetary accretion via to improvement of protocratons with depleted lithospheric keels via c. 3.2 Ga, in a sequence of papers written by way of over 50 of the world's prime specialists. The publication is split into chapters on early Earth historical past, ten chapters at the geology of particular cratons, and chapters on early Earth analogues and the tectonic framework of early Earth. person contributions handle subject matters that diversity from planetary accretion, a overview of Earth meteorites, value and composition of Hadean protocrust, composition of Archaean mantle and deep crust, all elements of the geology of Paleoarchean cratons, composition of Archean oceans and hydrothermal environments, facts and geological settings of youth, early Earth analogues from Venus and New Zealand, and a tectonic framework for early Earth.
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Extra info for Earth's Oldest Rocks
35 Ga. Early Archean rocks have been reported at several localities in West Africa (Fig. 2-1). Although not precisely dated, blocks of early Archean rocks occur in the Leo Rise area, which is largely a region of Birimian juvenile crust. , 1997). , 2001). Evidence of early Archean rocks also comes from the Hoggar Massif in the Tuareg shield in southern Algeria, although dating is less precise. , 2003). SHRIMP zircon ages from orthogneisses of the Amsaga terrane in the Reguibat Rise in western Mauritania (Fig.
Probably the most surprising discovery has been that, although the secular decrease with time of radioactive heat production has been confirmed and further constrained, the geological record of rock associations, their geochemical signatures, and structural relationships has been found to be more similar to, rather than very different from, that of modern plate tectonic equivalents. Abundant data accumulated over several decades indicate that Archaean rocks worldwide occur in accretionary orogens that formed by subduction–accretion processes.
Where it was cold enough out in the disk, at about 5 AU, water condensed as ice, forming a “snow line” (Stevenson and Lunine, 1988). The resulting pile-up of ices and dust trapped at the “snow line” at 5 AU locally increased the density of the nebula. This density increase led to a rapid (105 year) runaway growth of large bodies (10–15 Earth-masses) of ice and dust. 2 Earth-mass) are surviving examples of these cores. At the same time, the gas (H and He) was also being dispersed by the stellar winds.
Earth's Oldest Rocks by Martin J. van Kranendonk, R. Hugh Smithies and Vickie C. Bennett (Eds.)