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At least 109 records · Page 6
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NASA NTRS1972

Mineralogy, petrology, and chemistry of a Luna 16 basaltic fragment, sample B-1.

Petrological, mineralogical, and chemical investigations of the B-1 Luna 16 sample have revealed that the sample is a fine-grained ophitic basalt which is distinguished from the Apollo samples by containing a single pyroxene, an ilmenite content intermediate to that of the Apollo samples, and subequal amounts of pyroxene and plagioclase. It is also distinguished by a high Sr content and a high K/U value.

Albee, A. L.↗
NASA NTRS1972

Rb-Sr age of a Luna 16 basalt and the model age of lunar soils.

An internal isochron was determined on a small basalt fragment (sample B-1) returned from the Luna 16 mission, which yields an age of 3.42 plus or minus 0.8 b.y. and a low initial Sr87/Sr86 value. A comparison is made of the data from four lunar missions to mare sites which shows that the last period of major flooding of the mare basins is confined to a narrow time interval of only 0.55 b.y. The direct evidence of major lunar magmatic activity appears to be confined to the interval from 3.1 to 4.0 b.y. The Sr87/Sr86 values for all mare basalts are extremely primitive and lie in a rather narrow range. A diagram is given for initial Sr87/Sr86 as a function of time for all lunar rocks.

Papanastassiou, D. A.↗
NASA NTRS1972

Neutron capture on Gd and Sm in the Luna 16, G-2 soil.

Measurement of the Gd and Sm isotopic compositions in the Luna 16, G-2 soil, a sample which has the largest low energy neutron fluence yet observed in a lunar sample. The ratio of the number of neutrons captured per atom by Sm-149 to Gd-157 is 0.76, which is distinct from the value of 0.86 observed at the Apollo 11, 12, and 14 sites. This indicates a softer neutron energy spectrum at the Sea of Plenty.

Russ, G. P.↗
NASA NTRS1972

Inert gases in twelve particles and one 'dust' sample from Luna 16.

The inert gases were measured mass-spectrometrically in 12 fragments and one dust sample from Luna 16. The fragments were classified petrologically by microscopic inspection. The major petrologic types were breccias and basalts. The He-4/Ne-20 ratio of the breccias (average 49) was systematically smaller than that of the basalts (average 78), probably because of He-Ne fractionation during or after the formation of the breccias. We suggest that the He-4/Ne-20 ratios of bulk fines in general may reflect the proportions of basaltic and breccia (plus cindery glasses) fragments in the fines. Exposure ages of four fragments are several hundred million years. The Ar-40/Ar-36 slopes of breccias and basalts are identical: 0.65.

Heymann, D.↗
NASA NTRS1972

Fossil track and thermoluminescence studies of Luna 16 material.

Measurements of track densities and thermoluminescence have been made on two 5-mg samples (feldspar crystals) from the Luna 16 core tube. The distribution of track densities is shown graphically and is similar to that observed in heavily irradiated Apollo samples. Results of thermoluminescence measurements are plotted and also compared with similar measurements of Apollo samples.

Walker, R.↗
NASA NTRS1972

Rare earths and other trace elements in Luna 16 soil.

An analysis has been made of four small samples of material brought to earth by the Luna 16 mission, with the aim to determine rare earths and other trace elements in these samples. The analytical results are tabulated, and the rare earth abundances are compared with the average for chondrites. A comparison is also made with the results of similar analyses of Apollo samples.

Helmke, P. A.↗
NASA NTRS1972

Meteoritic and non-meteoritic trace elements in Luna 16 samples.

Two Luna 16 soils have been analyzed for Ag, Au, Bi, Br, Cd, Co, Cs, Cu, Ga, Ge, In, Ur, Ni, Rb, Re, Sb, Se, Te, Tl, and Zn. A meteoritic component similar to that in Apollo 11 and 12 soils seems to be present, corresponding to about 1.5 to 2% Cl chondrites or equivalent. It probably consists largely of micrometeorites. Three elements show strong enrichments compared to Apollo 11 and 12 soils: Cd (5 x to 200 x), Ag (5 x to 10 x), and Bi (3 x). Presumably these elements were brought in by Cd-Ag-Bi rich material, similar to that in Unit VI of Apollo core 12028.

Laul, J. C.↗
NASA NTRS1972

Oxygen isotope composition of the Luna 16 soil.

The results of the 0-18/0-16 analysis of the available 16-mg sample of Luna 16 soil are presented and compared with oxygen-isotope compositions of several Apollo soils. The analytical techniques were the same as those of Onuma et al. (1970) applied to the Apollo samples. It is found that the soil from Mare Fecunditatis is indistinguishable in oxygen isotopic composition from the soils of Mare Tranquillitatis and the Fra Mauro region.

Clayton, R. N.↗
NASA NTRS1972

Major element composition of Luna 20 glasses.

Ten per cent of the 50 to 150-micron size fraction of Luna 20 soil is glass. A random suite of 270 of these glasses has been analyzed by electron microprobe techniques. The major glass type forms a strong cluster around a mean value corresponding to Highland basalt (anorthositic gabbro) with 70% normative feldspar. Minor glass groups have the compositions of mare basalts and of low-K Fra Mauro type basalts. The glass data indicate that Highland basalt is the major rock type in the highlands north of Mare Fecunditatis.

Warner, J.↗
NASA NTRS1972

Rb-Sr systematics of Luna 20 and Apollo 16 samples.

For the soils of two lunar highland sites from which samples were returned by the Luna 20 probe and the Apollo 16 mission, Rb-Sr data are presented. For comparison, the results of some additional analyses of Apollo 15 soils are also given. All these soils indicate that an early lunar differentiation process occurred in the interval of 4.3-4.6 b.y. and resulted in the formation of a crust rich in K, Rb, U, and Th.

Papanastassiou, D. A.↗
NASA NTRS1973

Pb-207/Pb-206 ages of individual mineral phases in Luna 20 material by ion microprobe mass analysis.

Ion microprobe analyses of returned lunar material have helped to demonstrate that U, Th, and radiogenic Pb are concentrated in small accessory mineral phases. It is possible to measure the isotopic composition of this Pb and obtain a radiometric Pb-207/Pb-206 age for the mineral. The ages so derived compare favorably with crystallization ages determined by conventional methods. A grain mount (22003,2/6) of Luna 20 material was searched for such accessory mineral phases, and two were found. One of these phases give an age of 4.12 plus or minus 0.04 b.y. and the other an age of 4.42 plus or minus 0.11 b.y. Ages of minerals dated by the ion probe in Apollo samples 14310 and 15555 are given for comparison. Data on the upper limit for Pb concentration in the outermost surface layers of free lunar soil particles are also given.

Andersen, C. A.↗
NASA NTRS1973

Optical and chemical analysis of iron in Luna 20 plagioclase.

Review of analytical data on the iron content of Luna 20 anorthitic plagioclase, obtained by a highly sensitive technique for measuring polarized absorption related to crystal-field splittings and by automated electron microprobe analysis of oriented single crystals. The iron content is found to range from a few hundredths to a few tenths of a weight per cent from crystal to crystal. The optical and chemical properties of the iron appear to be caused by postcrystallization migration and exsolution. Postcrystallization effects may obscure evidence of the original oxidation state and iron concentration of these crystals.

Bell, P. M.↗
NASA NTRS1973

Oxide minerals in lithic fragments from Luna 20 fines.

One hundred seventy-six oxide mineral grains in the Luna 20 samples were analyzed by electron microprobe. Spinel is the most abundant oxide, occurring in troctolite fragments. Next most abundant is ilmenite, which occurs in all rock types except those containing spinel. Chromite also occurs in all rock types except those containing spinel. Minor amounts of ulvospinel, armalcolite, zirkelite, baddeleyite and an unidentified TiO2-rich phase were also found. Spinel grains are predominantly spinel-hercynite solid solutions, commonly with very minor chromite. The Fe/(Fe + Mg) ratio is generally lower than in spinel from Apollo 14 rocks. Chromites in non-mare rocks are similar to those from mare rocks. Ilmenite of mare origin is Mg-poor and Zr-rich compared to non-mare ilmenite; these elements may therefore be useful in determining the origin of ilmenite grains. Phase equilibria considerations suggest that spinel troctolite crystallized from a melt high in alumina; a likely candidate is the high-alumina basalt of Prinz et al. (1973).

Brett, R.↗
NASA NTRS1973

Petrology of fine-grained rock fragments and petrologic implications of single crystal from the Luna 20 soil.

Only fine-grained rocks are present in the Luna 20 samples, and coarser-grained rocks are represented by fragments of single crystals. A petrologic study has been made of 47 fine-grained crystalline rocks, microbreccias, and glassy aggregates. In addition, a total of 33 single crystals of pyroxene, plagioclase, olivine, and spinel, in the size range from 125 to 500 microns, have been examined using electron microprobe and single-crystal X-ray diffraction techniques. The most abundant fine-grained crystalline rocks in the samples examined are recrystallized anorthositic norite and anorthositic troctolite. Gabbroic rocks, anorthosite, and KREEP basalt are present but not common. Most of the single crystals of pyroxene and plagioclase could have been derived from coarser-grained noritic, troctolitic, and anorthositic rocks. However, three of the 14 pyroxene crystals, and two of the five olivine crystals have Fe/(Fe + Mg) contents greater than 0.45 and are believed to have been derived from mare basalts or related rocks.

Cameron, K. L.↗
NASA NTRS1973

Chemistry and surface morphology of soil particles from Luna 20 LRL sample 22003.

Optical and scanning electron microscopy, scanning electron microprobes and energy dispersion techniques were applied in an analysis of six siliceous glass spheres, five siliceous glass-bonded agglutinates and one breccia fragment from Luna 20 sample 22003. It is theorized that local meteor impact processes might have been responsible for the formation of most of the glass spheres and that the impacts of relatively high velocity particles might have been responsible for the craters observed on the surfaces of the spheres. The concentrations of iron spherules on the surfaces of the glass spheres were generally lower than in similar Apollo 11 and 12 glass spheres.

Carter, J. L.↗
NASA NTRS1973

Petrology of Luna 20 regolith from the lunar highlands.

The Luna 20 regolith sample contains crystalline lithic fragments of mare basalt, the anorthosite-norite-troctolite group, and feldspathic basalt. Discrete mineral fragments and mineral fragments in regolith breccias can generally be assigned, based on chemical criteria, to one or the other of the first two rock types. A complex history is indicated for the regolith fragments involving repeated metamorphism and melting of the highlands due to impact events. The glass fragments and the feldspathic basalts probably are the result of this melting and their composition may be representative of a large portion of the regolith at this site.

Crawford, M. L.↗