Engineering topics

Housley, R. M.

Publications and source records attributed to Housley, R. M..

At least 19 records

NASA NTRS1992

Mapping the Moon in Soft x Rays: Promises and Challenges

Recent ROSAT images reported by Schmitt et el. show that the sunlit part of the Moon is a significant source of very soft x rays. Stimulated by these observations, Edwards et al. have made an analysis of the response of the Moon to the solar soft x ray and EUV spectrum. They argue that much of the observed emission is in the form of discrete fluorescence lines in the energy range 25 to 100 eV, and that these lines are generally much stronger than the adjacent directly scattered solar background. On this basis they suggest that soft x ray fluorescence can be used to remotely obtain high-precision elemental maps of the lunar surface. Edwards et al. have continued to develop this idea and have suggested a system using soft x ray telescopes in lunar orbit, which could also obtain very good spatial resolution. This combination could be extremely valuable in furthering our understanding of lunar chemistry and potential resource distributions. High spatial resolution combined with the thin surface layer from which these soft x rays arise suggests the exciting possibility that x ray telescopes could map lunar volcanic volatiles from orbit.

Housley, R. M.↗

NASA NTRS1990

Chemical removal of contaminants from thin film Bi4Sr3Ca3Cu4O(16 + x) surfaces

A solution of Br in absolute ethanol, previously shown to be effective in removing nonsuperconducting species from Y-Ba-Cu-O thin film surfaces, is shown also to be effective in treating Bi-Sr-Ca-Cu-O thin film surfaces. X-ray photoelectron spectra obtained after etching are consistent with previously reported results obtained from samples cleaved or scraped in vacuum.

Vasquez, R. P.↗

NASA NTRS1989

Ceramic problems/challenges in high temperature oxide superconductors - Hysteretic force measurements as a new analysis tool

A technique is presented for analyzing high-temperature oxide superconductors using hysteretic magnetic force/distance measurements. Emphasis is placed on developing low weight, highly robust superconducting materials for space applications. Bi-Ca-Sr-Cu superconductors are prepared and characterized by standard techniques. It is found that standard techniques such as XRD, SEM, and TEM are insufficient to completely characterize superconductors. The magnetic properties of the superconductors are studied with the new technique, based on measuring the force between a magnet and the superconductor as a function of their separation.

Morgan, P. E. D.↗

NASA NTRS1988

Syntactic intergrowth problems with BCSCO and fabrication difficulties therefrom

EDXS performed on isolated particles of the Bi-Ca-Sr-Cu-O high-temperature ceramic superconductor has verified the presence of significant elemental exchange between the Ca and Sr, and, to a lesser extent, between Cu and Bi. Two primary preparations, identified as primarily 24.4 A and 30.6 A, respectively, are identified. The Cu:Bi ratio in the 30.6 A material is approximately 1:1 for most particles, although only a few particles of the nominally 24.4 A material have the expected 1:2 ratio. No unequivocal assignment of atomic composition to the predominantly 24.4 A or 30.6 A appears possible, if major syntactic problems are present.

Morgan, P. E. D.↗

NASA NTRS1986

Gallium-bearing sphalerite in a metal-sulfide nodule of the Qingzhen (EH3) chondrite

The composition and possible history of the Qingshen (EH3) chondrite is presented. The chondrite contains a population of spheroidal metal-sulfide nodules, which display textural evidence of reheating and melting. Evidence of metal sulfuration is also present, suggesting replacement of metal by sulfide during melting. This process has led to the nucleation of perryite along metal-sulfide interfaces. The Ga-bearing sphalerite that was found may have formed by injection of molten sulfide droplets into the metal followed by subsolidus diffusion of Ga from the metal into the sulfide. The latter may occur because of Ga supersaturation in the metal during progressive sulfuration and its decreased affinity for the metal phase during cooling below the taenite-kamacite transition point.

Rambaldi, E. R.↗

NASA NTRS1986

Roedderite in the Qingzhen (EH3) chondrite

The rare mineral roedderite, (Na1.09 K0.89 Ca0.02)2.00 (Mg4.71 Fe0.27)4.98 (Si11.80 Al0.09)11.89 O30 has been found in accessory amounts in the highly unequilibrated enstatite chondrite, Qingzhen. It occurs in association with minor amounts of albite and SiO2 as inclusions within the metal or sulfide phases of metal-sulfide assemblages. The roedderite crystals are connected through oxide and silicate veins to the surrounding matrix. The presence of glass coated vesicles on the surface of the assemblages strongly suggests that roedderite originated in the presence of a fluid phase, presumably during post-accretional planetary processes.

Rambaldi, E. R.↗

NASA NTRS1986

Lunar sample analysis

A wide variety of lunar sample and meteorite studies were performed. Abstracts of the most recent reports are also attached. Experimental techniques employed have included scanning electron microscopy, transmission electron microscopy, Mossbauer spectroscopy, atomic absorption analysis and a variety of simulation studies.

Housley, R. M.↗

NASA NTRS1985

Lunar sample analysis

Recent results on the antarctic meteorite ALPHA 77003 which contribute to understanding the alteration processes which produced matrix in unequilibrated chondrites are presented. Also included are additional scanning electron microscope results confirming that the matrix in Allende was formed by in situ alteration.

Housley, R. M.↗

NASA NTRS1984

Occurrence of oxidized components in Qingzhen enstatite chondrite

It is shown that the most unequilibrated enstatite chondrite, Qingzhen, contains a population of enstatite grains which appear to have formed under more oxidizing nebular conditions than the bulk of the meteorite, which is highly reduced. These grains are black in transmitted light because of the presence of micron-sized inclusions of Ni-poor, Cr-rich metal, and occur either isolated within the matrix or in chondrule interiors. The textural occurrence of these grains argues against their having been introduced during collision of Qingzhen with an oxidized meteorite. Most likely, they originated in the same general nebular neighborhood of the reduced bulk Qingzhen material and were subsequently transported into the reducing environment either before or during the process of chondrule formation. The discovery of this once-oxidized material in Qingzhen posed significant constraints on existing models of formation of reduced matter in the solar system.

Rambaldi, E. R.↗

NASA NTRS1984

The chemistry of micrometeoroids (A0187-1)

The prime objective of this experiment is to obtain chemical analyses of a statistically significant number of micrometeoroids. These data will then be compared with the chemical composition of meteorites. Secondary objectives of the experiment relate to density, shape, mass frequency, and absolute flux of micrometeorids as deduced from detailed crater geometrics (depth) diameter, and plane shape, and number of total events observed.

Hoerz, F.↗

NASA NTRS1984

Lunar sample analysis

Results are presented from an extensive series of new high resolution scanning electron microscope studies of the very primative group of meteorites known as unequilibrated chondrites. These include quantitative analyses of micrometer sized phases and interpretation in terms of relevant phase equilibria. Several new meteorite minerals including high chromium metal, have been discovered.

Housley, R. M.↗

NASA NTRS1983

Evidence for relict grains in chondrules of Qingzhen, an E3 type enstatite chondrite

Petrographic and chemical studies of the Qingzhen chondrite strongly suggest that it is the most highly unequilibrated (type 3) enstatite chondrite recognized so far. Qingzhen contains abundant, well-defined chondrules, some of which were incompletely molten during the chondrule formation process. The relict olivine grains within these chondrules contain dusty inclusions of almost pure metallic Fe, which appear to be the in situ reduction product of the fayalitic component of the olivine. The reduction process presumably took place at the time of chondrule formation and the chondrule precursor material must have been more oxidized than average enstatilite chondrite material. It is believed that this oxidized material may have formed at the enstatite chondrite formation location in the solar nebula, provided fluctuations in the degree of oxidation of the nebular gas existed at such locations. Reheating of this material under more reducing conditions would lead to the observed reduction of the olivine. Igneous olivines within chondrules always contain detectable amounts of CaO, while relict olivines are essentially CaO-free. This seems to suggest thatg the relict olivines did not originate during a previous igenous process of chondrule formation and might represent condensation products from the early solar nebula.

Rambaldi, E. R.↗

NASA NTRS1983

Lunar sample analysis

The evolution of the lunar regolith under solar wind and micrometeorite bombardment is discussed as well as the size distribution of ultrafine iron in lunar soil. The most important characteristics of complex graphite, sulfide, arsenide, palladium, and platinum mineralization in a pegmatoid pyroxenite of the Stillwater Complex in Montana are examined. Oblique reflected light micrographs and backscattered electron SEM images of the graphite associations are included.

Housley, R. M.↗

NASA NTRS1983

Sputtering of the gallium-indium eutectic alloy in the liquid phase

Watson and Haff (1980) have discussed a theory which is designed to explain quantitatively isotopic fractionation effects observed during sputtering of simple or complex targets. This theory is based on the assumption that most of the atoms sputtered from a surface originate in the top monolayer. The present investigation is mainly concerned with a direct experimental test of that assumption. The sputtering of both solid and liquid phases of gallium, indium, and the gallium-indium eutectic alloy is studied. Results obtained with the aid of ion scattering and Auger spectroscopy show that, in agreement with rough theoretical expectations, the surface monolayer of a gallium-indium alloy with 16.5 percent indium in bulk contains more than 94 percent indium, while the next layer can be only slightly enriched.

Dumke, M. F.↗

NASA NTRS1983

On the alteration of Allende chondrules and the formation of matrix

Recent SEM observations of the Allende chondrules and matrix are reported. Intergrowths of both Fe-rich olivine (with a composition near Fa50), and clinoenstatite (with a composition of about Fs2). All of the clinoenstatite was involved in associations along the outer margins, grain boundaries, and internal crack surfaces of the chondrule. Most of the chondrules also contain abundant opaque inclusions which must have been strongly altered and partially replaced before chondrule formation. It is suggested that the Fe-rich olivine formed from the clinoenstatite by a reaction of the type Fe + 1/202 + MgSiO3 to (Fe,Mg)2SiO4. It is argued that a variation of the small, internally-heated planetesimal provides the most plausible environment for the chemical reaction.

Housley, R. M.↗

NASA NTRS1982

Distribution and evolution of Zn, Cd, and Pb in Apollo 16 regolith samples and the average U-Pb ages of the parent rocks

The concentration of surface (low temperature site) and interior (high temperature site) Cd, Zn, and Pb in 13 Apollo 16 highland fines samples, pristine rock 65325, and mare fines sample 75081 were analyzed directly from the thermal release profiles obtained by flameless atomic absorption technique (FLAA). Cd and Zn in pristine ferroan anothosite 65325, anorthositic grains of the most mature fines 65701, and basaltic rock fragments of mare fines 75081 were almost all surface Cd and Zn indicating that most volatiles were deposited on the surfaces of vugs, vesicles and microcracks during the initial cooling process. A considerable amount of interior Cd and Zn was observed in agglutinates. This result suggests that high temperature site interior volatiles originate from entrapment during the lunar maturation processes. Interior Cd found in the most mature fines sample 65701 was only about 15% of the total Cd in the sample. Interior Pb present in Apollo 16 fines samples went up to 60%. From our Cd studies we can assume that this interior Pb in highland fines samples is largely due to the radiogenic decay which occurred after the redistribution of the volatiles took place. We obtained an average age of 4.0 b.y. for the parent rocks of Apollo 16 highland regolith from our interior Pb analyses.

Cirlin, E. H.↗

NASA NTRS1982

SEM, optical, and Moessbauer studies of submicrometer chromite in Allende

New scanning electron and optical microscope results are presented showing that sub-micrometer chromite is abundant along healed cracks and grain boundaries in Allende chondrule olivine. Some wider healed cracks also contain pentlandite and euhedral Ni3Fe grains. Also reported are Moessbauer measurements on Allende HF-HCl residues confirming a high Fe(+++)/Fe(++) ratio.

Housley, R. M.↗

NASA NTRS1980

Toward a model of grain surface exposure in planetary regoliths

The interpretation of solar wind implanted gas concentration versus particle size for lunar regolith samples is considered. In so doing, interparticle adhesive forces are considered explicitly and the simplest possible grain exposure law consistent with the existence of such forces is hypothesized. Namely, for particles small enough that these forces exceed the lunar gravitational force, any element of area has equal probability of being in the regolith surface regardless of the size of the grain on which it is situated. This law leads to the expectation that concentrations will depend inversely on mean grain radius for small grains and gradually become independent of radius for very large grains consistent with observations. Therefore, such a concentration dependence cannot by used to infer the presence of saturation losses.

Housley, R. M.↗