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  • LUNAR AND PLANETARY EXPLORATION  (11)
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  • 1
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    Searching for neuKREEP: An EMP study of Apollo 11 Group A basalts (1993)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: The Apollo 11 and 17 landing sites are characterized by the presence of high-Ti basalts (TiO2 greater than 6 percent). The Group A basalts of Apollo 11 have elevated K compositions (greater than 2000 ppm); and are enriched in incompatible trace elements relative to the other types of high-Ti basalt found in the region. These unique basalts also are the youngest of all high-Ti basalts, with an age of 3.56 +/- 0.02 Ga. Recent modelling of the Apollo 11 Group A basalts by Jerde et al. has demonstrated that this unique variety of high-Ti basalt may have formed through fractionation of a liquid with the composition of the Apollo 11 orange glass, coupled with assimilation of evolved material (dubbed neuKREEP and having similarities to lunar quartz monzodiorite). Assimilation of this material would impart its REE signature on the liquid, resulting in the elevated REE abundances observed. Minerals such as whitlockite which contain a large portion of the REE budget can be expected to reflect the REE characteristics of the assimilant. To this end, an examination of the whitlockite present in the Apollo 11 Group A basalts was undertaken to search for evidence of the neuKREEP material assimilated.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 2: G-M; p 717-718
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  • 2
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    neoKREEP: A new lunar component at Apollo 17 (1992)
    In:  CASI
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    Publication Date: 2013-08-31
    Description: The Apollo 11 (Mare Tranquillitatis) and Apollo 17 (Mare Serenitatis) landing sites are important as the only sources of high-Ti basalt visited by the Apollo missions. The lunar high-Ti basalts (greater than 6 percent TiO2) have no volumetrically comparable analogs among terrestrial basalts and require the presence of ilmenite in the source region, probably representing cumulates produced late in the crystallization of the lunar magma ocean. Six principal groups of high-Ti basalts are described, three from each of the two sites.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Inst., Workshop on Geology of the Apollo 17 Landing Site; p 21-24
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  • 3
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    On the composition of neuKREEP: QMD contamination at Apollo 11? (1993)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: The Group A basalts of Apollo 11 differ in many respects from other high-Ti basalts of the region. Chemically, they are the only high-K (greater than 2000 ppm K) variety of high-Ti basalt and are enriched in incompatible trace elements relative to other basalts from both the Apollo 11 and Apollo 17 sites. In addition, Group A basalts are the youngest of all high-Ti basalts, with an age of 3.56 +/- 0.02 Ga. The cluster of compositions is consistent with the Apollo 11 Group A basalts representing a single flow. Papanastassiou et al. have also indicated the uniqueness of these basalts, based particularly on relatively young Rb-Sr model ages (3.8 - 3.9 Ga). A model for the formation of the Group A basalts was presented by Jerde et al., wherein the Apollo 17 orange volcanic glass is the parent liquid. Fractionation of this composition, coupled with the assimilation of incompatible-element-rich material, results in compositions akin to those of the Apollo 11 Group A basalt population. Orange glass of similar major-element composition is present at the Apollo 11 site as well, although complete trace element analyses are not available. New modelling results using the Apollo 11 orange glass major elements are grossly similar to those obtained using the Apollo 17 orange glass, indicating approximately 30 percent fractionation.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 2: G-M; p 719-720
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  • 4
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    Production of O2 on the Moon: A lab-top demonstration of ilmenite reduction with hydrogen (1993)
    In:  Other Sources
    Details
    Publication Date: 2019-01-25
    Description: Estimates of the costs of transporting materials from Earth to the Moon are around $25,000 per pound. Therefore, it is imperative that we learn to utilize the resources on the Moon to partially offset these 'astronomical' expenses. The production of oxygen on the Moon utilizing indigenous materials is crucial to the establishment and development of an autonomous lunar colony. Besides obvious biologic needs, this lunar liquid oxygen (LLOX) could result in tremendous cost savings on fuel for effective transportation systems, particularly with its export to low-Earth orbit. Over 20 different process concepts were proposed and evaluated for the production of oxygen from lunar materials. Simplicity, low energy, easily attainable feedstock, and low resupply mass are the keywords for the process(es) which will ultimately be selected for the initial production of oxygen on the Moon. One of these schemes, which has received considerable study to date, is the hydrogen reduction of ilmenite. In fact, Carbotek, Inc. (Houston, TX) patented an ilmenite, hydrogen-reduction technique involving a three-stage, fluidized-bed process for the production of LLOX. A lab-top demonstration unit of the basic concepts of this oxygen generation process that was constructed by our group at the University of Tennessee is explained. It utilizes many of the principles which must be addressed in designing an effective production plant for operation on the Moon.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 3: N-Z; p 1411-1412
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  • 5
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    Evaluation of lunar rocks and soils for resource utilization: Detailed image analysis of raw materials and beneficiated products (1993)
    In:  Other Sources
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    Publication Date: 2019-01-25
    Description: The rocks and soils of the Moon will be the raw materials for fuels and construction needs at a lunar base. This includes sources of materials for the generation of hydrogen, oxygen, metals, and other potential construction materials. For most of the bulk material needs, the regolith, and its less than 1 cm fraction, the soil, will suffice. But for specific mineral resources, it may be necessary to concentrate minerals from rocks or soils, and it is not always obvious which is the more appropriate feedstock. Besides an appreciation of site geology, the mineralogy and petrography of local rocks and soils is important for consideration of the resources which can provide feedstocks of ilmenite, glass, agglutinates, anorthite, etc. In such studies, it is very time-consuming and practically impossible to correlate particle counts (the traditional method of characterizing lunar soil petrography) with accurate modal analyses and with mineral associations in multi-mineralic grains. But x ray digital imaging, using x rays characteristic of each element, makes all this possible and much more (e.g., size and shape analysis). An application of beneficiation image analysis, in use in our lab (Oxford Instr. EDS and Cameca SX-50 EMP), was demonstrated to study mineral liberation from lunar rocks and soils. Results of x ray image analysis are presented.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 3: N-Z; p 1409-1410
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  • 6
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    Lunar meteorites - Siderophile element contents, and implications for the composition and origin of the moon (1989)
    In:  Other Sources
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    Publication Date: 2019-07-12
    Description: Data for 10 siderophile elements in all of the known lunar meteorites except for Y793274 are reported. Bulk compositional data for Ni, Ge, Cd, Re, Os, Ir, and Au were obtained from radiochemical neutron activation analysis (Warren et al., 1986). Data for Fe, Co, and Zn, and additional data for Ni, Ir, and Au were obtained by instrumental neutron activation analysis (Kallemeyn et al., 1988). Except for the case of Au in Y791197, there was good agreement between the results obtained by the two methods. The differences observed between the lunar-meteoritic regolith samples and central nearside highlands regolith samples are discussed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Earth and Planetary Science Letters (ISSN 0012-821X); 91; 3-4
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  • 7
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    Composition and origin of Nuevo Laredo Trend eucrites (1987)
    In:  Other Sources
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    Publication Date: 2019-07-12
    Description: The new bulk-rock analyses reported for the ALHA81001, Lakangaon and Nuevo Laredo eucritic meteorites indicate that the first of these resembles Ibitira in possessing lower Na concentrations than any other eucrite, while the other two are the lowest-Mg/Fe of all eucrites. The present data and those seen in the literature suggest that most of the ostensible Main Group eucrites actually belong to the Nuevo Laredo Trend, which is characterized by limited variations of incompatible element contents despite considerable variations in Mg/(Mg+Fe) ratio and V content.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Geochimica et Cosmochimica Acta (ISSN 0016-7037); 51; 713-725
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  • 8
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    Diverse eucritic pebbles in the Vaca Muerta mesosiderite (1987)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: Seven 5-cm basaltic pebbles from the Vaca Muerta mesosiderite were studied by neutron activation and electron microprobe analysis, and three additional pebbles were studied petrographically. The cumulate pebbles had low REE concentrations and high Eu/Sm ratios, indicating the absence of intercumulus liquid. Siderophile interelement ratios were similar to those found in Vaca Muerta metal except for anomalously low Ir concentrations. The presence of 20 percent impact-melt breccias among the pebbles and 35-40 percent melt breccias among the mesosiderite whole-rocks suggests that the mesosiderites were more extensively impact melted than the howardites. Three alternative models to explain this greater proportion of impact-melted material among the mesosiderites are proposed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Earth and Planetary Science Letters (ISSN 0012-821X); 84; 1 Ju
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  • 9
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    Pristine moon rocks - A 'large' felsite and a metal-rich ferroan anorthosite (1987)
    In:  Other Sources
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    Publication Date: 2019-07-12
    Description: Results of elemental analyses, performed either by instrumental neutron activation analysis (NAA) or radiochemical NAA, of 19 lunar rock samples obtained by the Apollo 15, 17, and 12 missions are presented. Two of the samples are most extraordinary: 'large' (1 g) felsite from Apollo 12 and a pristine ferroan anorthosite from Apollo 15. The felsite is mainly a graphic intergrowth of K-feldspar and a silica phase, with about 6 pct plagioclase and 1 pct each of ferroaugite, ilmenite, and fayalitic olivine. The Fe-metal content of ferroan anorthosite is 1.2 wt pct in the thin section studied (but, based on mass balance for Co and Ni, must have been lower in the chip used for bulk-rock analysis); the measured bulk-rock concentrations of siderophile elements Re, Os, and Ir are far higher than previously observed among pristine lunar anorthosites. These results underscore the uncertainty associated with any attempt to estimate the overall siderophile element contents of the moon's crust.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research (ISSN 0148-0227); 92; E303-E31
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  • 10
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    A potpourri of regolith breccias - 'New' samples from the Apollo 14, 16, and 17 landing sites (1987)
    In:  Other Sources
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    Publication Date: 2019-07-12
    Description: Compositional (by INAA) and petrographic studies were performed among the smaller rocks (not analyzed previously) from the Apollo 14, 16, and 17 sites as part of a search for regolith samples exotic to the small traverse areas associated with these missions. Of the 40 samples studied, 31 were regolith breccias. Among these, three of the Apollo 14 samples proved to be compositionally unique, particularly the 14315 sample, which is radically different from all other Apollo 14 regolith materials (lower Mg and Fe, far higher Al and far lower REE abundances), and is probably exotic to the Apollo 14 traverse area. Among 10 samples from Apollo 17, all but one proved to be typical Apollo 17 regolith breccia. However, the 72504,10 sample is more than 99 percent pure pyroclastic glass, compositionally identical to the Apollo 17 orange glass obtained at a location 4 km away, attesting to the widespread distribution of orange glass deposits.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research (ISSN 0148-0227); 92; E526-E53
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