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At least 1,261 records · Page 70
All sourcesNASA NTRSDOE OSTI
NASA NTRS1977

Melt immiscibility in Apollo 15 KREEP - Origin of Fe-rich mare basalts

Silicate liquid immiscibility (SLI) is investigated in terms of chemistry and occurrence in two KREEP-rich Apollo 15 basalts. The two samples have different cooling histories but the same composition. In the first sample, SLI occurred at the time of 58% crystallization. In the second sample, SLI occurred after 20% had crystallized. It is noted that SLI could be initiated as soon as plagioclase (out of a total composition which also included zircon, FeS, SiO2, whitlockite, and ilmenite) alone had crystallized. Attention is given to Fe-rich immiscible melts, and it is suggested that SLI may play an important role in the formation of the source regions of Fe-rich mare basalts. The analytical technique used for the assays was an energy dispersive analysis system with a resolution of 167 eV.

Hollister, L. S.↗
NASA NTRS1975

Shock-induced subsolidus reduction-decomposition of orthopyroxene and shock-induced melting in norite 78235

Lunar rock 78235 is a coarse-grained igneous rock which was chipped from the top of a boulder about 1/2 m in size at Station 8 at the base of the Sculptured Hills, Taurus-Littrow Valley. The rock is a shocked coarse-grained norite with a relict subophitic texture; it is composed of about equal proportions of chromian bronzite and anorthite. Evidence is presented for the shock history of the rock. It is concluded that 78235 is a deep-seated norite of cumulate origin which has been intensely shocked. Although it may be possible to account for the observed shock-induced features by invoking a single shock event, the evidence is best explained by a history which includes at least two discrete shock events. In the first identifiable shock event much of the plagioclase was transformed to maskelynite and the associated bronzite was deformed and acquired a mosaic structure. In a later shock event, localized melting of both plagioclase pyroxene occurred.

Sclar, C. B.↗
NASA NTRS1979

Crystal nucleation in glass-forming alloy and pure metal melts under containerless and vibrationless conditions

Crystal nucleation behavior in metallic alloys known to form glasses in melt quenching was characterized and from this characterization the possibility that massive amounts of certain alloys could be slow cooled to the glass state was assessed. Crystal nucleation behavior of pure liquid metals was examined experimentally, under containerless conditions, and theoretically.

Turnbull, D.↗
NASA NTRS1979

Melting of Io by tidal dissipation

The resonant structure of Io leads to forced eccentricities that are considerably larger than the free values. Although still modest by all standards, these forced eccentricities coupled with the enormous tides induced by Jupiter lead to magnitudes of tidal dissipation that are large enough to completely dominate the thermal history of Io. In the present paper, the forced eccentricities are calculated and then substituted into an expression for the total tidal dissipation. The results point to the possibility that the dissipation of tidal energy in Io may have melted a major fraction of Io's mass.

Peale, S. J.↗
NASA NTRS1978

Clast assemblages of possible deep-seated /77517/ and immiscible-melt /77538/ origins in Apollo 17 breccias

Breccia samples 77517 and 77538 are composed of abundant mineral and lithic clasts set in porous, poorly sintered matrices. Clast assemblages in the two rocks are of contrasting composition and origin. Breccia 77517 has Mg-rich olivine and pyroxene and calcic plagioclase clasts, indicating limited, almost exclusively ANT-suite parentage. A significant feature is the presence of an assemblage (aluminous enstatite, forsterite, anorthite, aluminous spinel) corresponding to spinel cataclasite, a rock type of deep-seated (about 60 km) crustal origin. Breccia 77538 contains Fe-rich pyroxene and rather sodic plagioclase clasts, indicative of predominantly KREEP and/or mare derivation. An important feature is the occurrence of high-K and high-Fe lithic clasts whose compositions resemble those of immiscible-melts produced during late-stage magmatic crystallization, and which probably originated via silicate liquid immiscibility in a KREEP or mare basalt magma. Both rocks contain numerous fine-grained breccia clasts which represent material that has been modified by impact processes at or very near the moon's surface.

Warner, R. D.↗
NASA NTRS1978

Provenance of metal and melt rock textures in the Malvern howardite

Malvern has been recognized as a breccia containing crystal clasts, clasts of parent rock types, and clasts of impact origin. The matrix consists primarily of small angular crystal fragments of pyroxene and plagioclase. Contrary to achondrites, the Malvern clasts of primary rocks and crystals are virtually devoid of metal, and the matrix contains no metal or primary achondrite composition. The melt rocks contain metal of meteoritic composition, which is also present in the matrix of Malvern.

Hewins, R. H.↗
NASA NTRS1978

Residual glasses and melt inclusions in basalts from DSDP Legs 45 and 46 - Evidence for magma mixing

Microprobe analyses of natural glasses in basalts recovered by Legs 45 and 46 of the Deep Sea Drilling Project are reported and interpreted in the context of other geochemical, petrographic and experimental data on the same rocks (Rhodes et al., 1978). Residual glass compositions in the moderately evolved aphyritic and abundantly phyric basalts within each site indicate that none of the units is related to any other or to a common parent by simple fractional crystallization. The compositional trends, extensive disequilibrium textures in the plagioclase phenocrysts and the presence in evolved lavas of refractory plagioclase and olivine phenocrysts bearing primitive melt inclusions provide evidence that magma mixing had a major role in the genesis of the Leg 45 and 46 basalts. The magma parental to these basalts was most likely characterized by high Mg/(Mg + Fe/+2/), CaO/Al2O3, CaO/Na2O and low lithophile concentrations. A mixing model involving incremental enrichment of magmaphile elements by repeated episodes of mixing of relatively primitive and moderately evolved magmas, followed by a small amount of fractionation is consistent with the characteristics of the basalts studied.

Dungan, M. A.↗
NASA NTRS1980

Low-cost solar array project task 1: Silicon material. Gaseous melt replenishment system

The operation of a silicon production technique was demonstrated. The essentials of the method comprise chemical vapor deposition of silicon, by hydrogen reduction of chlorosilanes, on the inside of a quartz reaction vessel having large internal surface area. The system was designed to allow successive deposition-melting cycles, with silicon removal being accomplished by discharging the molten silicon. The liquid product would be suitable for transfer to a crystal growth process, casting into solid form, or production of shots. A scaled-down prototype reactor demonstrated single pass conversion efficiency of 20 percent and deposition rates and energy consumption better than conventional Siemens reactors, via deposition rates of 365 microns/hr. and electrical consumption of 35 Kwhr/kg of silicon produced.

Jewett, D. N.↗
NASA NTRS1980

The distribution of temperature maxima for micrometeorites decelerated in the earth's atmosphere without melting

A simple model for the statistics of heating of micrometeorites decelerated in the earth's atmosphere without melting predicts that for 10 micron particles with thermal emissivity near 1, roughly half of those with density 1 g/cc are heated above 550 C, while half of those with density 3 g/cc are heated above 800 C. In the study of stratosphere collected interplanetary dust, the model can be helpful in identifying petrographic thermometers of the atmospheric entry process, and in understanding the most recent history of this new class of extraterrestrial material available in the laboratory.

Fraundorf, P.↗
NASA NTRS1980

Luna 24 ferrobasalt as a low-Mg primary melt

The fractional crystallization model for the petrogenesis of the Luna-24 very-low-titanium ferrobasalt is critically evaluated. Arguments are presented that show there is no real evidence favoring either surface of shallow subsurface differentiation of an Mg-rich primary magma; instead there is ample evidence suggesting such is not the case. It is therefore concluded that surface or near-surface fractionation of olivine from a primary vitrophyre/green glass magma did not produce the ferrobasalt composition. The ferrobasalt did not exist as a residual liquid within a differentiated flow, but rather was extruded as a melt in its own right.

Norman, M.↗
NASA NTRS1980

Elemental abundances in chondrules from unequilibrated chondrites Evidence for chondrule origin by melting of pre-existing materials

Bulk abundances of Na, Mg, Al, Ca, Sc, V, Cr, Ir, and Au were analyzed by neutron activation of chondrules separated from unequilibrated H, L, and LL chondrites and correlated with petrographic properties. The geometric mean composition of the whole-rock chondrule suites are almost indistinguishable from each other for many elements; chondrules are enriched in lithophile and depleted in siderophile elements in a pattern consistent with chondrule formation by melting of preexistent materials. The porphyritic chondrules are more enriched in refractory and siderophile elements as compared with the nonporphyrytic chondrules, indicating that these two chondrule groups may have formed from different precursors.

Gooding, J. L.↗
NASA NTRS1980

Melt density and the average composition of basalt

Densities of residual liquids produced by low pressure fractionation of olivine-rich melts pass through a minimum when pyroxene and plagioclase joint the crystallization sequence. The observation that erupted basalt compositions cluster around the degree of fractionation from picritic liquids corresponding to the density minimum in the liquid line of descent may thus suggest that the earth's crust imposes a density fiber on the liquids that pass through it, favoring the eruption of the light liquids at the density minimum over the eruption of denser more fractionated and less fractionated liquids.

Stolper, E.↗
NASA NTRS1982

The measurement of heats of solution of high melting metallic systems in an electromagnetic levitation field

A method was tested for measuring the enthalpies of mixing of liquid metallic alloying systems, involving the combination of two samples in the electromagnetic field of an induction coil. The heat of solution is calculated from the pyrometrically measured temperature effect, the heat capacity of the alloy, and the heat content of the added sample. The usefulness of the method was tested experimentally with iron-copper and niobium-silicon systems. This method should be especially applicable to high-melting alloys, for which conventional measurements have failed.

Frohberg, M. G.↗
NASA NTRS1981

Derivation of a heterogeneous lithic fragment in the Bovedy L-group chondrite from impact-melted porphyritic chondrules

Results are presented of petrographic, compositional and dating analyses of a light-colored lithic fragment in the L-group Bovedy meteorite that has a composition different from that of the host chondrite. Polished thin sections of the lithic fragment, host, and the fragment-host boundary were examined microscopically and analyzed by electron microprobe, metallic Ni-Fe, and instrumental neutron activation techniques; chips of the fragment were also used for Ar-39/Ar-40 dating and oxygen isotope analyses. The poikilitic textures, olivine, low-Ca pyroxene and kamacite composition and low Na2O, K2O and P2O5 contents of the fragment indicate that it represents a solidified, slightly fractionated impact melt formed from a source rich in porphyritic chondrules. A progressive increase on MgO content across the fragment is accounted for by the heterogeneous nucleation of MgO-rich phases. The Ar data indicate that the Bovedy lithic fragment and its host were partly degassed of radiogenic Ar less than 0.94 billion years ago, probably due to shock. The data are consistent with a cooling rate of about 5 C/million years through 500 C, which must have resulted from the burial of the assemblage beneath insulating material on the parent body at depths of at least several km.

Rubin, A. E.↗
NASA NTRS1983

Hot-Melt Adhesive Attachment System

Adhesive system is as effective on Earth as in space. Fiberglass cloth mounted in head assembly. When adhesive reaches melt temperature head is attached to metals composites, ceramics, and other materials. Once attached, head cooled rapidly for quick stick. Used to tether tools or attach temporary scaffolding to walls, buildings, or beams.

Fox, R. L.↗
NASA NTRS1982

Origin of SiC impurities in silicon crystals grown from the melt in vacuums

A main source of high carbon levels in silicon crystals grown from melt under reduced pressures and contained in silica crucibles supported by graphite retainer/susceptor was identified by thermodynamic analysis. The calculations were verified by experimental results and the carbon level is reduced by approximately 50% with the use of molybdenum retainers.

Schmid, F.↗
NASA NTRS1982

Siderophiles in the Brachina meteorite - Impact melting

Oxygen isotope ratios, siderophile abundances, and siderophile ratios for the Brachina meteorite (a chassignite) are compared with data reported for various chassignites, shergottites, nakhlites, pallasites, iron meteorites, chondrites, lunar low-Ti basalts, and terrestrial basalts. The results show that Brachina is different in origin from other shergottites, nakhlites, and chassignites. It is suggested that all the chassignites, shergottites, and nakhlites could have formed on Mars in an impact event about 180 million yr ago and that Brachina may have been ejected from Mars as a large tektitelike impact-melt blob consisting of Chassigny-like target material and a small amount of Eagle Station trio-like pallasite material.

Ryder, G.↗
NASA NTRS1983

Supercooling and structure of levitation melted Fe-Ni alloys

A study has been made of the effect of supercooling, quenching rate, growth inhibitors, and grain refiners on the structure of levitation-melted Fe- 25 pct Ni alloys. A combination of three morphologies, dendritic, spherical, and mixed dendritic and spherical, is observed in samples superheated or supercooled by less than 175 K. At larger supercooling, however, only the spherical morphology is observed. The grain size and the grain boundary shape are found to be strongly dependent on the subgrain morphology but not on the quenching temperature. Considerable grain growth is evident in samples with spherical and mixed morphologies but not in the dendriitic samples. The average cooling rates during solidification and the heat transfer coefficients at the metal-quenching medium boundary are calculated. For samples solidified in water, molten lead, and ceramic molds, the heat transfer coefficients are 0.41, 0.52, and 0.15 w/sq cm, respectively.

Abbaschian, G. J.↗