Computer Science
Scientific paper
Sep 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sosyr..33..363s&link_type=abstract
Solar System Research, vol. 33, p. 363 (1999)
Computer Science
Scientific paper
The tectonomagmatic evolution of the Moon resembles the Paleoproterozoic (cratonic) stage of the Earth's evolution. Analogs of the Earth's old (Archean) magmatism, which was dominated by tonalitic granitoids at a subordinate role of komatiite-basaltic magmatism, and analogs of Phanerozoic magmatism, which is related to the active plate boundaries, were not discovered on the Moon. The oldest (4.45-4.25 Ga ago) continental magmatism of the Moon is represented by magnesian-suite rocks, which intrude the pristine anorthosite crust. In terms of compositional, mineral, and isotope-geochemical features, these rocks resemble those of the Earth's Early Paleoproterozoic siliceous high-Mg series (SHMS), but differ in their somewhat higher reduced character of the melts. As in the Earth, they are associated with the KREEP series enriched in K, REE, and P (KREEP is the abbreviation for K+REE+P). The second stage (3.8-3.2 Ga ago) of the Moon's tectonomagmatic evolution produced abundant mare basalts, which fill the depressions of newly formed lunar mares. The basalts are grouped into two types: low- and high-Ti. The former resemble basalts of the Earth's mid-oceanic ridges, while the latter are similar to geochemically enriched terrestrial moderate-alkaline intraplate Fe-Ti picrites and basalts, whose large-scale development occurred 2.2-2.0 Ga ago. Judging from the mineral composition, the mare basalts were derived from reduced melts, unlike their Earth's counterparts. By analogy with the Earth, mare magmatism is related to the ascend of mantle plumes and the spreading of their heads, which resulted in the formation of large mare depressions with a considerably decreased crustal thickness. It is suggested that, by analogy with the Earth, two stages may be distinguished in the Moon's evolution: the formation of the iron core from the protoplanetary matter and the subsequent accumulation of chondrite material. However, because of the proximity to the Earth, which, due to its large weight, more effectively "exhausted" the volatiles (especially H2O) from the surrounding space, the Moon and especially its core were depleted in these components. Differences in the evolution of the tectonomagmatic processes in the Moon and Earth were apparently related to the different energetic abilities of these planets.
Bogatikov O. A.
Sharkov E. V.
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