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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 19 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1988

Production of Be-10 in stony meteorites - Composition dependence

The relationship between the production rate of Be-10 in stony meteorites and its element composition was investigated by measuring the contents of Be-10 in 21 samples from 17 meteorites with known major-element composition, and comparing the experimental Be-10 values with those obtained by the regression analysis. The Be-10 production was modeled by the equation of Stauffer (1962). The measured Be-10 contents were found to range from 16 dpm/kg in the oxygen- and magnesium-poor eucrites and the Indarch meteorite to 28 dpm/kg in the oxygen- and magnesium-rich aubrites and the mineral separates from Bruderheim. Using the regression analyses and taking in account various corrections, an equation was obtained which reproduces the measured Be-10 content with an accuracy of about 10 percent.

Moniot, R. K.↗
NASA NTRS1994

The Twenty-Fifth Lunar and Planetary Science Conference. Part 1: A-G

Papers from the conference are presented, and the topics covered include the following: planetary geology, meteorites, planetary composition, meteoritic composition, planetary craters, lunar craters, meteorite craters, petrology, petrography, volcanology, planetary crusts, geochronology, geomorphism, mineralogy, lithology, planetary atmospheres, impact melts, volcanoes, planetary evolution, tectonics, planetary mapping, asteroids, comets, lunar soil, lunar rocks, lunar geology, metamorphism, chemical composition, meteorite craters, and planetary mantles.

Source record↗
NASA NTRS1993

Twenty-Fourth Lunar and Planetary Science Conference. Part 3: N-Z

Papers from the conference are presented, and the topics covered include the following: planetary geology, meteorites, planetary composition, meteoritic composition, planetary craters, lunar craters, meteorite craters, petrology, petrography, volcanology, planetary crusts, geochronology, geomorphism, mineralogy, lithology, planetary atmospheres, impact melts, K-T Boundary Layer, volcanoes, planetary evolution, tectonics, planetary mapping, asteroids, comets, lunar soil, lunar rocks, lunar geology, metamorphism, chemical composition, meteorite craters, planetary mantles, and space exploration.

Source record↗
NASA NTRS2002

Element-Element Correlations Among Martian Meteorite Bulk Compositions: Peculiarities Explained(?) By Mixing, with Implications for the Composition of Mars

Correlations of elements abundances among the Martian meteorites have been used to infer the bulk composition of the Martian mantle, and thence the broad petrogenesis of the planet. It has been assumed that the correlations represent igneous fractionations. However, the correlations are also consistent with mixing, broadly similar to that inferred from radio-isotope data. If the correlations represent mixing of geochemical components, it is not clear that they represent Mars' mantle or bulk composition.

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NASA NTRS1993

The carbon components in SNC meteorites of feldspathic harzburgite composition

Two meteorites collected in Antarctica, ALH A77005 and LEW 88516, have characteristics which link them to the shergottite group of SNC meteorites. Essentially, ALH A77005 and LEW 88516 are feldspathic harzburgites, being comprised of roughly equal quantities of olivine and pyroxene, with an additional few percent of feldspar which has subsequently been converted to maskelynite by shock. The meteorites represent samples of a cumulate rock which is itself composed of two different lithologies: in one, large pyroxenes poikilitically enclose olivine crystals, while the other consists of interstitial areas made up of pyroxene, olivine, maskelynite, whitlockite, troilite, ilmenite and chlorapatite. It has been proposed that meteorites such as ALH A77005 (and LEW 88516) are relict samples of the source peridotite from which the other shergottites formed. As such it should be informative to study in detail the carbon components present within these samples, in order to make comparisons with data from other shergottites. Although not plutonic in origin, and therefore not sampling a truly deep source, analyses of ALH A77005 and LEW 88516 should assist with attempts to define the bulk carbon isotopic composition of Mars. This has been assessed previously through analyses of carbon of presumed magmatic origin in other SNC meteorites, but the carbon isotopic compositions obtained seem to be at variance with what might be expected. It is important to constrain the carbon isotopic composition of Mars as well as possible so that models of atmospheric evolution, based on carbon isotopic data, can yield the most reliable results.

Wright, I. P.↗
NASA NTRS2002

Element-Element Correlations Among Martian Meteorite Bulk Compositions: Peculiarities Explained(?) by Mixing, with Implications for the Composition of Mars

Most estimates of the chemical corn position of Mars' mantle and core derive from elementelement correlations bulk analyses of Martian meteorites [I-31. To use the correlations in this manner assumes implicitly that they reflect mineraVmelt fractionations (e.g., partial melting, fractional crystallization, accumulation) among a cogenetic suite of igneous rocks. However, similar correlations can zppear from mixing of chemical components, and need not imply that the components were cogenetic nor that they had an igneous origin. Several aspects of the elemental and isotopic chem istries of the Martian meteorites can be explained by mixing of geochemical components (mantle or crustal), e.g. [5,6]. Thus, it is worth asking whether mixing rektions might be seen in bulk chemical data, and (if so) whether the mixing components can be used to infer average planet or mantle compositions.

Treiman, A. H.↗
NASA NTRS1989

Interstellar SiC in the Murchison and Murray meteorites - Isotopic composition of Ne, Xe, Si, C, and N

Detailed ion-probe data are reported on Murchison and Murray C2 chondrites, along with noble-gas data on Murchison, with the purpose of characterizing the number and isotopic composition of independent SiC components and to link them to their stellar sources. Results show that coarse-grained and fine-grained SiC (totaling about 6-9 ppm of the two meteorites) contains record concentrations of two exotic components: Ne-E(H) (nearly monoisotopic Ne-22) and Se-S (enriched in isotopes 128, 130, and 132), respectively. The Ne-21 content was found to exceed up to 40-fold the content expected from the recent cosmic-ray irradiation, implying a presolar cosmic-ray exposure age of about 39 Ma. This age is much shorter that the predicted 500 Ma lifetime of refractory interstellar grains and implies either a selective interstellar destruction process for SiC, enhanced supernova activity in the protosolar neighborhood, or late outgassing of greater than 90 percent of the SiC.

Zinner, Ernst↗