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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

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At least 361 records · Page 20
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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

Chemistry and thermal history of metal particles in Luna 20 soils.

Individual metal particles from Luna 20 thin sections 521, 513 and 514 as well as several small metallic inclusions in silicate particles from Luna 20 thin sections 501 and 502 were examined using optical microscopy and the electron microprobe. All the metallic particles and inclusions analyzed are of meteoritic Co-Ni content as are most of the metallic particles from the Fra Mauro and the Apollo 16 highlands sites. It is proposed that most of the metal at these 3 sites had its origin in the meteoritic projectiles that bombarded and accumulated in the early lunar crust. It is apparent that the metallic particles and some of the metallic inclusions in the Luna 20 soil have been subjected to reheating on the moon and this process has removed any evidence of the original meteoritic microstructure of the metal.

Goldstein, J. I.↗
NASA NTRS1972

Mach 1 oxidation of thoriated nickel chromium at 1204 C /2200 F/.

Electropolished and ground samples of TD-NiCr were exposed to a 1-atm, Mach 1 gas stream at 1204 C for times up to 50 hr. The samples were subjected to both cyclic and isothermal exposure. Weight change, metal loss, X-ray diffraction, metallographic, and electron microprobe analyses were performed. Neither surface preparation nor cyclic-against-isothermal-exposure conditions had a strong effect on the oxidation behavior of the alloy. Initially, a Cr2O3 layer was formed whose volatilization resulted in a very rapid loss of metal - more than 40 microns in the first hour. At about 1 hr, the Cr2O3 layer broke down and NiO began to cover the surface. By 5 hr, the NiO had covered the surface and the rate of loss slowed. The rate-controlling step was diffusion of Cr through NiO.

Lowell, C. E.↗
NASA NTRS1973

VLS /vapor-liquid-solid/ - Newly discovered growth mechanism on the lunar surface.

A probable vapor-liquid-solid (VLS) type of growth has been discovered for the first time in nature on the surface of lunar rock 15015. Scanning electron microprobe and energy dispersive x-ray data indicate that the growth occurs as metallic iron stalks from about 0.015 to 0.15 micrometer in diameter, with bulbous tips consisting of a mixture of iron and sulfur and measuring from about 0.03 to 0.2 micrometer in diameter. The stalk length is two to ten times the bulb diameter.

Carter, J. L.↗
NASA NTRS1973

Role of Hf and Zr in the hydrogen embrittlement of Ta and Cb alloys

The hydrogen embrittlement of aged T-111 and similar Ta and Cb alloys is characterized and the mechanisms believed responsible for the increased sensitivity of T-111 to low temperature hydrogen embrittlement after aging for 1000 hours or longer near 1040 C are described. A total of eight Ta base alloys and two Cb base alloys were investigated. The effects of pre-age annealing temperature, aging time, temperature and environment, and alloy composition on the susceptibility to hydrogen embrittlement were investigated. The primary method of determining the effects of these variables on the ductility of T-111 was by bend testing at 25 and -196 C. Fractured specimens were examined by the scanning electron microscope, electron microprobe, metallography and X-ray diffration.

Stephens, J. R.↗
NASA NTRS1972

Disproportionation of Fe2SiO4 to 2FeO plus SiO2 at pressures up to 250kbar and temperatures up to 3000 C

A sample of Fe2SiO4 (spinel) at approximately 250 kbar in a diamond anvil press was heated to approximately 3000 C for a duration of some ms using a focused light beam from a pulsed ruby laser. After quenching and unloading, X-ray diffraction patterns indicated that the portion of the sample that had been heated contained wustite and stishovite. A sample of Fe2SiO4 (fayalite) at approximately 200 kbar in a diamond anvil press has been heated to 800 C for 20 min in a furnace. After quenching and unloading, the sample was found to have concentric zones with the fayalite phase at the lowest pressure, the spinel phase at the intermediate pressure, and a dark region at the center where the pressure was highest. An X-ray diffraction pattern of the dark central region indicated the presence of wustite. A microprobe analysis of a sample produced by a similar procedure indicated that SiO2 is apparently evolved along with wustite but is not sufficiently crystalline to be detected by X-ray diffraction.

Bassett, W. A.↗
NASA NTRS1973

On the manganese content of cosmic flakes from deep-sea sediments

Cosmic flakes belong to the category of cosmic microparticles. They occur together with cosmic spherules in sediments. These flakes appear to represent ablation products of iron meteorites burnt away during the passage of a meteorite through the atmosphere by friction against air molecules. Microprobe analyses of flakes from deep sea deposits proved the particles to consist of magnetite which in most cases had been altered into maghemite in the outer zones. This is in agreement with the assumption that they represent fragments of fusion crust of iron meteorites. Most of the flakes, however, contained a small percentage of manganese. This element is not a common constituent of iron meteorites. An attempt is made to explain the presence of manganese in flakes and its absence in cosmic spherules.

Utech, K.↗
NASA NTRS1974

Petrographic and crystallographic study of silicate minerals in lunar rocks

Optical U-stage measurements, chemical microprobe data, and X-ray procession photographs of a bytownite twin group from rock 12032,44 are compared. Sharp but weak b and no c-reflections were observed for this An89 bytownite indicating a partly disordered structure. Euler angles, used to characterize the orientation of the optical indicatrix, compare better with values for plutonic than for volcanic plagioclase. This indicates that structural and optical properties cannot be directly correlated.

Carmichael, I. S. E.↗
NASA NTRS1974

Interdiffusion behavior of tungsten or rhenium and group 5 and 6 elements and alloys of the periodic table, part 1

Arc cast W, CVD W, CVD Re, and powder metallurgy Re materials were hot isostatically pressure welded to ten different refractory metals and alloys (Cb, Cb-1Zr, Ta, Ta-10W, T-111, ASTAR-811C, W-25Re, Mo-50Re, W-30Re-20Mo, ect.) and thermally aged at 10 to the minus 8th power torr at 1200, 1500, 1630, 1800, and 2000 C for 100 to 2000 hours. Electron beam microprobe analysis was used to characterize the interdiffusion zone width of each couple system as a function of age time and temperature. Extrapolations of interdiffusion zone thickness to 10,000 hours were made. Classic interdiffusion analysis was performed for several of the systems by Boltzmann-Matano analysis. A method of inhibiting Kirkendall voids from forming during thermal ageing of dissimilar metal junctions was devised and experimentally demonstrated. An electron beam weld study of Cb-1Zr to Re and W-25Re demonstrated the limited acceptability of these welds.

Arcella, F. G.↗
NASA NTRS1973

Evaluation of ground characterization samples MCN-2 and MCN-3, section 1

A detailed metallurgical evaluation of two exothermically brazed nickel ground characterization samples was conducted. Samples MCN-2 and MCN-3 were among six samples that were brazed as part of a exothermic brazing experiment to obtain baseline data for use in determining the effect of weightlessness on: (1) the wetting and flow behavior of brazing filler metals; and (2) the metallurgical characteristics of the brazed joints. The samples were evaluated by metallographic examination and electron microprobe analysis.

Source record↗
NASA NTRS1973

Effects of diffusion on aluminum depletion and degradation of NiAl coatings

Experimental demonstration of the effects of diffusion on aluminum depletion and degradation in NiAl coatings on superalloys. Pack aluminized IN 100 and Mar-M200 were vacuum annealed at 1100 C to allow diffusion to proceed independently of oxidation. As-coated and as-diffused coatings were compared before and after cyclic furnace oxidation at 1100 C. The extent of degradation was judged by specific weight change, metallography, and electron microprobe analyses.

Smialek, J. L.↗
NASA NTRS1973

Polarized crystal-field spectra of micro particles of the moon

The instrumentation used in the investigation is considered, giving attention also to a block diagram of the apparatus used for measuring crystal-field spectra. The basic object of the studies was to identify the states of transition elements in lunar crystals in order to obtain information on the chemistry of their crystallization history. After spectral measurements were obtained, the crystals were analyzed for major and minor elements using the electron microprobe. Mineral spectra are considered, giving attention to pyroxene, olivine, plagioclase, and lunar glasses.

Mao, H. K.↗
NASA NTRS1974

Restudy of pyroxene-pyroxene equilibration temperature for ordinary chondrite meteorites

Experimental verification of the conclusions of Van Schmus and Koffman (1967) that the equilibration temperatures of ordinary chondrites are roughly the same regardless of classification, and that these temperatures range from 770 to 860 C. The higher average relative equilibrium temperatures found are attributed to improvements in microprobe techniques, and better standards and correction procedures introduced over the last six years. Agreement is expressed with their conclusion that ordinary chondrites embody equilibria achieved within the metamorphic temperature regime and not under igneous temperatures as postulated earlier by Craig (1964) and Mueller (1964).

Bunch, T. E.↗
NASA NTRS1973

Analysis of the ultrafine fraction of the Apollo 14 regolith

Analyses were obtained on more than 2400 randomly selected particles from the sub-37 micron (ultrafine) fraction of ten Apollo 14 regolith samples. The analyses were conducted with an energy dispersive electron microprobe system. The semiquantitative data were used to group the particles into ten categories. The pyroxene/plagioclase and olivine/plagioclase ratios are inconsistent with those ratios in the Apollo 14 breccias and rocks. The data suggest that fragmented basalts similar to Apollo 12 olivine basalts may have made significant contributions to the ultrafine fraction of the Fra Mauro regolith. Among a number of unusual particles encountered are brown, birefringent lath-shaped grains with 60 wt % SiO2 and 34 wt % FeO(FeSi2O5) and a glass with 20 to 25 wt % CaO, 0 to 8 wt % MgO, 40 to 45 wt % Al2O3 and approximately 30 wt % SiO2.

Finkelman, R. B.↗
NASA NTRS1973

Pyroxene poikiloblastic rocks from the lunar highlands

The results of detailed petrographic, X-ray, electron microprobe, ion probe, and Ar-40/Ar-39 age studies of pyroxene poikiloblastic breccias, an important lunar highlands lithology, are interpreted to indicate that high grade metamorphic recrystallization occurred over wide regions of the moon at about 4.0 G.y. This metamorphism was probably related to a period of high meteorite influx at that time. The temperatures achieved were highly variable but in some cases were sufficiently intense to cause varying degrees of partial melting of the precursor highlands breccias. A complete spectrum of metamorphic grades from only slight recrystallization to virtually complete melting would be expected in such a model. Such a spectrum is observed in the Apollo 16 rocks.

Bence, A. E.↗
NASA NTRS1973

Armalcolite and genetically associated opaque minerals in the lunar samples

A comprehensive electron microprobe study of armalcolite in samples from five Apollo sites (11-16), together with analytical data previously reported from Apollo 17 and Luna 20 show that three distinct compositional types of armacolite are present in the lunar samples. These types are classified as armalcolite, Cr-Zr-Ca-armalcolite and Zr-armalcolite. The Zr-free armalcolites are typical of high-Ti mare basalts whereas the Zr-rich armalcolites are typical of non-mare high alumina basalts. The latter armalcolites are in complete oxide intergrowths (baddeleyite, zirconolite, rutile, ilmenite, and chromite) and are in contrast to the Zr-free armalcolites which are commonly only associated with ilmenite. Subsolidus decomposition of armalcolite to an iron and Mg-rich rutile + ilmenite-geikielite, and the solid state formation of armalcolite from magnesium-ilmenite + niobian-rutile are described for the first time in the lunar samples.

Haggerty, S. E.↗