Statistics – Computation
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....1267s&link_type=abstract
EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #1267
Statistics
Computation
Scientific paper
At present the main ideas about origin and evolution of the solid planets of the Earth's group are mainly based on different physical and geochemical computations and estimates. Geological and petrological data are practically disregarded, however, they could be very useful for understanding of these processes. Comparative study of tectonic-magmatic development of the Earth and the Moon showed that there are essential similarity between evolution of the lunar magmatism and the Paleoproterozoic terrestrial magmatism (analogs of the terrestrial Archean type of activity with its granite-greenstone terranes and the Phanerozoic subduction-related situations were lacking on the Moon). Geological development of the both bodies became after solidification of their global oceans, which resulted in appearance on the Earth the primordial sialic crust and primordial anorthositic on the Moon. Geological data indicate that the further evolution of the bodies had occurred in two main stages with rather different character of its tectonomagmatic processes. On the Earth at the frontier 2.2-2.0 Ga mainly depleted mantle sources was changes for the mainly geochemical-enriched ones (with the advent of Fe-Ti picrites and basalts in global scale as well as high-Ti alkaline rocks) which was followed by changing of plume-tectonics to plate tectonics and appearance of ophiolites (in the Penrose Conference's sense). On the Moon such change occurred at the boundary 3.9-3.8 Ga when had formed large maria depressions with thinned crust and abundant basaltic volcanism including high-Ti varieties. Thus, in the both cases a new material sudden began to involve in the geological processes in the planets outer shells. From all of these, probably, follows that the both planetary bodies originally had heterogeneous structures and evolved under the same scenario: their gradually downward warming up to appearance of its liquid cores, accompanied by gradually cooling of their outer parts. Such warming is presumably linked with a wave of centripetal deformations into revolving bodies. It suggests that at the first stage of their development tectonomagmatic processes were linked with ascending of the mantle superplumes, which was formed into the depleted mantle. Appearance of the liquid cores initiated ascending of the geochemical-enriched superplumes of the second generation from the CMB; they reached more shallow levels and extension of their heads led to cardinal transformation of the planets outer shells.
Bogatikov O.
Sharkov Evgenii
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