Engineering topics
Publications and source records attributed to Marvin, U. B..
The petrology of Luna 20 lithic fragments is described and compared to that of other highland sites. An identification of the major types of rocks that compose the lunar terrae is attempted, and their probable petrogenesis is discussed.
A total of 645 particles in the 1 to 2 mm size range has been classified in the Apollo 16 soil samples 60602,3, 61242,7, 66042,4, 67602,13, and 69942,13. Five major categories of lithic fragments recognized in these samples include (1) an anorthositic/noritic/troctolitic, or ANT suite, (2) light-matrix breccias, (3) poikiloblastic noritic/anorthositic fragments, (4) spinel-troctolites, and (5) feldspathic basalts. The petrography and phase chemistry of the lithic fragments are discussed along with results of the fragment census and the stratigraphy of the Apollo 16 site.
Nine petrographically distinct separates from Apollo 15 coarse soils were characterized by electron microprobe and analyzed by neutron activation analysis for Ag, Au, Bi, Br, Cd, Cs, Ge, In, Ir, Rb, Re, Sb, Se, Te, Tl, U, and Zn. Like some alkali-poor anorthosites from Apollo 16, 15102 anorthosite is low in meteoritic siderophiles but enriched in Tl, perhaps by volcanic processes. Norites from 15102 and troctolites from 15302 are lower in KREEP than are Apollo 12 or 14 norites. A possible progenitor of KREEP-rich norite breccias has been found: a mesostasis-rich basalt from 15272 high in KREEP-related elements, but very low in the siderophiles Ir, Re, Au, Sb, and Ge, and hence lacking the ancient meteoritic component that occurs in all lunar norites. At least two varieties of ancient meteoritic component are present in the soil separates from this site, consistent with the complex impact history of the Pre-Imbrian surface.
Review of the mineralogy and texture of the Haveroe and of some of the six other known ureilites, and assessment of the implications of their observed characteristics. In common with other ureilites, Haveroe shows mineralogical and textural evidence of preterrestrial shock. The olivines and metal grains have been recrystallized, the fabric includes angular voids, and graphite-rich areas are present that have been partially converted to diamonds with some indication of lonsdaleite. On the basis of such features, a subdivision of ureilites into particular types is proposed.
Some 2380 lithic and vitreous particles from levels A and G of the Luna 16 core-tube sample were classified. The relative proportions of particle types from each of the two layers are reported, and some petrological and mineralogical aspects of the lithic and vitreous components of the lunar regolith are discussed. Possible sources of the particles in the Luna 16 soil are examined.
Fragments of noritic breccias having a range of recrystallization textures and noritic basalts comprise about 80% of the 1 to 2 mm soil samples from Cone Crater (14142) and the bottom of the trench (14151). In five other samples, noritic fragments range in abundance from 42 to 56%. The remaining particles in each case are glasses, soil breccias, and glass-bonded aggregates; other crystalline rock types such as anorthosites constitute less than 1% of the soil. Noritic materials - i.e., Apollo 12 and 14 norites and ropy (KREEP) glass particles, can be divided into two broad groups on a chemical basis. The particles in one group have relatively high bulk TiO2 contents and high Fe/(Fe + Mg) ratios in their normative pyroxenes; the ropy glasses from Apollo 12 and 14 and a few Apollo 12 noritic rock fragments are in this category. Particles in the other class contain pyroxenes with a lower Fe/(Fe + Mg) and have a range of TiO2 contents; most noritic rock fragments from Apollo 12 and 14 are in this group. The ropy glasses may be from Copernicus or other rayed craters, but almost all the norites derive from the Fra Mauro formation or other noritic occurrences associated with Oceanus Procellarum.
An olivine-rich microbreccia with noritic affinities, collected on the Apollo 14 mission to Fra Mauro, is described and analyzed. A photomicrograph (by plain transmitted light) of the microbreccia is discussed. One of three distinct areas on the microbreccia is shown to be a dunite containing over 90% olivine. The other two are more gabbroic in composition, though most of the mineral clasts are olivine. The fine grained matrix material contains significant amounts of K2O and P2O5, suggesting a relation to norites.
A total number of 1858 lithic and vitreous fragments from the Luna 16 core-tube sample are classified. The fragments were taken from soil fractions ranging in size from 150 to 425 microns at levels A and G. No important differences are observed between the proportions of particle types in levels A and G, nor between the soils of Luna 16 and those from the Apollo 11 landing site in the nearby Mare Tranquillitatis.
Mineralogy and petrology of Apollo 12 lunar samples
Noritic and anorthositic rock fragment proportions and sources in Apollo 12 soil samples
Mineralogy and petrology of Apollo 11 lunar sample
Allende meteorite showing presence of Ca-Al-rich glasses associated with other crystalline phases
Apollo 11 lunar anorthosites properties and characteristics, discussing grain size, Na content, color, density, chemical composition and geomorphic effects
Feasibility of using ultrashort pulse laser ranging and independent clock radio interferometry distance measurement methods to test for existence of continental drift
Black magnetic spherules in Pleistocene and recent beach sands, investigating origin by electron microscopy
Iron-rich silicates significance in Mezo-Madaras chondrite
Crestone crater morphology indicates that it is not meteoritic or cometary in origin
Merrihueite, alkali-ferromagnesian silicate mineral occurring in Mezo-Madaras chondrite