By O. D. Rode, A. V. Ivanov, M. A. Nazarov, A. Cimbálníková, K. Jurek, V. Hejl, О. Д. à одэ, А. В. Иванов, М. А. Назаров, А. Цимбальникова, К. Юрек, В. Гейл (auth.)

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Extra resources for Atlas of Photomicrographs of the Surface Structures of Lunar Regolith Particles / АТЛАС МИКà ОФОТОГà АФИЙ ПОВЕà ХНОСТИ ЧАСТИЦ ЛУННОГО à ЕГОЛИТА

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54, 132). The degree of maturity of the spall zone rises with the crater diameter. It should be remarked that there is a wide spectrum of transitional crater forms showing features of both the low-velocity and high-velocity craters (Fig. 130). The regolith particles on the lunar surface are exposed continuously to impact effects. The impact energy controls the degree of alteration of the particle surfaces. The finest components of meteorites and solar wind ions constantly rework the particle forms.

No indications of the pyroclastic origin of regolith particles have been found. Metamorphism, (cataclasis and recrystallization), fragmentation and displacement of clastic material, agglomeration of fragments, melting, evaporation and condensation processes occur as a result of intensive meteoritic bombardment of the lunar surface and are reflected directly or indirectly in the morphology of lunar particles. Meteoritic bombardment gives rise not only to physical but also to chemical alterations of lunar rocks.

114, 146). Judging from their morphology, the hemispheres are halves of spherical particles rising above the surface of the host; the second half is embedded in the host particle. The character of their embedding suggests that they originated most likely as a result of liquation. However, they could also have formed by condensation at high-intensity impacts, or by reduction of lunar Fe-silicates by solar wind hydrogen, and subsequent growth of metallic products due to impact melting. Of interest are the crystals of minerals (iron and silicates - plagioclase, pyroxene, olivine) found in the cavities of magmatic rock fragments and breccias (Fig.

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