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• W2156827195 abstract "Abstract The theory that tektites are of lunar origin has frequently been criticized on the grounds that rocks of this chemical composition could not have been formed on the Moon. The purpose of this paper is to show that tektites may have been derived from silicic igneous rocks, specifically rhyolitic tuffs, forming the upper layers of the maria. The essentially igneous nature of tektites is indicated by their bulk composition, their restricted compositional range, and the high probability that they have not been derived from sedimentary rocks by random processes such as meteoritic impact. The differences between tektites and normal igneous rocks probably reflect their formation by extremely high temperature fusion of previously solid igneous rock. It is shown that if the Moon originally had a chondritic composition, the fusion curve of the lunar material should intersect the thermal gradients computed by G. J. F. MacDonald at the present time at 400 to 500 km depth, depending on the slope of the fusion curve, even if the Moon had originally been at 0°C. Additional heat sources such as the kinetic energy of accretion and capture-induced internal friction would probably have raised the temperature well above the “cold” Moon gradient. Magmas generated by partial fusion of the assumed chondritic material should be basaltic. It is proposed that the maria are the lunar equivalents of terrestrial lopoliths such as the Bushveld and Sudbury complexes, which are large basins filled mainly with basaltic rock overlain by tuffs, rhyolites, and granophyres. Tektites may have been derived from these silicic rocks by some process involving meteoritic impact." @default.
• W2156827195 created "2016-06-24" @default.
• W2156827195 creator A5044328921 @default.
• W2156827195 date "1963-01-01" @default.
• W2156827195 modified "2023-09-26" @default.
• W2156827195 title "The relation of tektites to lunar igneous activity" @default.
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• W2156827195 doi "https://doi.org/10.1016/0019-1035(63)90006-x" @default.
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