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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 217 records · Page 12
All sourcesNASA NTRSDOE OSTI
NASA NTRS1974

Study of radiation damage and structure of Luna 16 sample particles using high-resolution electron microscopes

Using an electron scanning microscope and a high voltage microscope, a study was made of the radiation damage and structure of micron sized grains and grains separated from the 200-mesh fraction of the L-16-19 surface material sample. Then the structural features were compared with those found by studying with the same techniques grains separated from 20 different samples of lunar dust taken from the Apollo 11, Apollo 12, Apollo 14, and Apollo 15 collections. The L-16-19 sample is similar to the most intensely irradiated samples returned to earth by Apollo craft.

Borg, J.↗
NASA NTRS1974

Light scattering indicatrices of lunar surface material returned by Luna 16 automatic station

Measurements are made of the indicatrix of scattering of lunar surface material with an indicatometer that has a spread of the illuminating beam of less than 0.5 deg and of the detected beam of about 1.5 deg. The results are compared with the indicatrices for the lunar mean obtained by terrestrial telescopic measurements. It is concluded that the main features of the reflection of light by the moon) (rapid rise in brightness with approach to the full moon) are accounted for by the microrelief caused principally by grains smaller than a millimeter.

Barabashov, N. P.↗
NASA NTRS1974

Photometric and polarimetric analysis of samples of lunar surface material returned by the Luna 16 automatic station

Polarimetric properties were determined for the L-16-19-1-116 samples, weighing 0.087 g. The measurements were made for five wavelengths between 3540 and 5850 AU. In addition, the normal albedo was determined for each of these wavelengths. The albedo for the measured sample was slightly lower than for the typical material of the dark lunar maria and in addition, there was a well developed branch of negative polarization, which resembles the branch obtained for carbonaceous chondrites crushed into powder, and the branch obtained for the powders of several terrestrial basaltic and ultrabasic rocks.

Dollfus, A.↗
NASA NTRS1974

Cathodoluminescence of regolith returned by Luna 16 automatic station

Observations of local variations in the intensity and spectral composition of the cathodoluminescence of lunar regolith are described. These variations are caused by structural features, by the kind and quantity of the material, and by the admixtures. In addition, cathodoluminescent emission is also associated with a change in the temperature of the lunar surface. Periodic diurnal illumination and darkening of the moon is responsible for a temperature gradient normal to the lines of longitude. These observations made of regolith, using a scanning electron microscope with an attachment for temperature variation, simulate the indicated thermal changes of the cathodoluminescent properties of lunar material.

Spivak, G. V.↗
NASA NTRS1974

Magnetic properties of lunar samples returned by Luna 16 automatic station

Results of measuring the specific magnetic susceptibility of regolith are presented. The data indicate that regolith samples from the Sea of Tranquillity and the Sea of Fertility are similar in order of magnitude of the specific magnetic susceptibility. Several stony meteorites of subgroup L have a similar value of this quantity. After comparison with artificial analogs, it can be concluded that the bulk content of ferromagnetic minerals in regolith samples is 3 to 4 percent.

Gorshkov, E. S.↗
NASA NTRS1974

Effect of lunar surface material on radiation damage in mice (investigation of biological action of lunar surface material returned to earth by Luna 16 automatic station)

The effect was studied of lunar surface material from the Sea of Fertility on the radiation reaction (damage) in mice caused by exposure to ionizing radiation. The material was administered to the organism in three ways -- aerogenically, through the esophagus, or peritoneally. It was shown that administering the lunar surface material did not appreciably affect the death of the animals and the reaction of the peripheral blood caused by the action of radiation. In mice which prior to irradiation had been administered inhalationally or peritoneally the lunar surface material, a lag in the increment of bodyweight was observed.

Antipov, V. V.↗
NASA NTRS1977

The Luna and Zond programs

These series have included flyby, lunar-orbiting, and soft-landing missions. A variety of experiments were carried out by these spacecraft including studies of magnetism, X-ray and gamma ray emissions, gravitational anomalies, and chemical composition. Soil samples, near- and farside photography (both color and black and white), and earth-cloud photography were also acquired.

Source record↗
NASA NTRS1990

Photoclinometric analysis of wrinkle ridges on Lunae Planum, Mars

Wrinkle ridges are common morphologic features on Mars. Both volcanic and tectonic mechanisms were suggested to explain their origin; recent work has focused on a compressional origin. Analysis of terrestrial analogs has greatly influenced and aided the understanding of wrinkle ridge formation. An important aspect necessary to intrepret structure is topography. Topographic profiles across ridges can provide important constraints for models of internal structure and analyzing deformation associated with ridges. Topographic maps of Mars are too coarse to resolve the topography of individual ridges; therefore, monoscopic photoclinometry was used to derive topographic profiles for the ridges. Profiles spaced a few kilometers apart were obtained for each ridge, the number depended on ridge length, morphology, and albedo variation. Photoclinometry relies on pixel brightness variations which results from topography, albedo, or both. Because of the albedo variations, photoclimometric profiles can not be extended across large distances, such as between adjacent ridges (about 20 to 80 km). However, the technique is applicable to shorter distances, such as the distance across typical ridges. Profiles were measured across the ridge and extended a few kilometers on either side, including all visible components of the ridge. The results of these measurements and the use of internal structure and topographic profile models for estimating the shortening due to folding and faulting are discussed.

Plescia, J. B.↗
NASA NTRS2009

Lunar Samples: Apollo Collection Tools, Curation Handling, Surveyor III and Soviet Luna Samples

The 6 Apollo missions that landed on the lunar surface returned 2196 samples comprised of 382 kg. The 58 samples weighing 21.5 kg collected on Apollo 11 expanded to 741 samples weighing 110.5 kg by the time of Apollo 17. The main goal on Apollo 11 was to obtain some material and return it safely to Earth. As we gained experience, the sampling tools and a more specific sampling strategy evolved. A summary of the sample types returned is shown in Table 1. By year 1989, some statistics on allocation by sample type were compiled [2]. The "scientific interest index" is based on the assumption that the more allocations per gram of sample, the higher the scientific interest. It is basically a reflection of the amount of diversity within a given sample type. Samples were also set aside for biohazard testing. The samples set aside and used for biohazard testing were represen-tative, as opposed to diverse. They tended to be larger and be comprised of less scientifically valuable mate-rial, such as dust and debris in the bottom of sample containers.

Allton, J.H.↗
NASA NTRS2009

Luna: What Did We Learn and What Should We Expect?

This presentation presents a look at the space program's background prior to lunar exploration and highlights the Apollo program and lessons learned from lunar exploration. The possibilities of exposures and difficulties attributed to lunar dust are described, including obscured vision, clogged equipment, coated surfaces, and inhalation, among others. A lunar dust simulant is proposed to support preliminary studies. Lunar dust is constantly activated by meteorite lunar dust, UV radiation and elements of solar wind - this active dust could produce reactive species. Methods of deactivation must be determined before new lunar missions, but first we must understand how to reactivate dust on Earth. Activation methods tested and described here include crushing/grinding or UV activation. Grinding time has a direct effect on amount of hydroxyl radicals produced upon addition of ground quartz to a solution. An increase in hydroxyl production was also seen for a lunar simulant with increased grinding.

Wallace, William T.↗
NASA NTRS1978

Experimental petrology of very low Ti /VLT/ basalts

Synthetic analogs of Luna 24 ferrobasalt and an Apollo 15 green glass were subjected to iron capsule experiments to test hypotheses concerning the generation of Luna 24 ferrobasalt. Results of the experiments indicated that the Luna 24 ferrobasalt may be generated by near-surface fractionation of a Luna 24 green glass parent. Evidence for the parent magma which differentiated at or near the Mare Crisium site to yield the Luna 24 ferrobasalt may be found in the Luna 24 green glass and lithic fragments of vitrophyres.

Grove, T. L.↗
NASA NTRS1977

The Lunar Orbiter program

The Luna and Zond series of unmanned U.S.S.R. spacecraft were designed to investigate the moon and its vicinity. Sixteen Luna spacecraft and, six Zond spacecraft have obtained lunar data. These series have included flyby, lunar-orbiting, and soft-landing missions. A variety of experiments were carried out by these spacecraft including studies of magnetism, X-ray and gamma emissions, gravitational anomalies, and chemical composition. Soil samples, near- and farside photography (both color and black and white), and earth-cloud photography were also acquired. Luna 17 and 23, carried automatic roving vehicles (Lunokhod 1 and 2) that traversed portions of the lunar surface. Lunokhod 1 roamed in Mare Imbrium near Sinus Iridum, and Lunokhod 2 roamed in the Crater Le Monnier at the eastern edge of Mare Serenitatis. The Luna 16, 20, and 24 missions soft-landed on the lunar surface, scooped up lunar material, and returned these samples to earth. The photographic samples received are in the form of paper prints. Some publications containing photographs are described.

Source record↗
NASA NTRS1978

Evidence for a high-magnesium subsurface basalt in Mare Crisium from orbital X-ray fluorescence data

Orbital X-ray fluorescence data taken by the Apollo 15 mission over Mare Crisium are analyzed in order to detect surface occurrences of the magnesium-rich materials found in the Luna 24 core sample. Apollo 15 data of the surface soils of the Luna 24 landing site, expressed as Al/Si and Mg/Si ratios, are found to be well correlated with the composition of the less than 74 micron fraction of the core sample. Orbital data indicate that most surface areas of the southern part of Mare Crisium have magnesium contents lower than or equal to that of the landing site, with the exception of areas in the vicinities of the post-mare craters Picard and Pierce and an area northeast of the Luna 24 site. The crater material is interpreted to be a magnesium-rich subsurface basalt excavated by crater formation, which may represent the material from which magnesium-rich Luna 24 samples, including olivine gabbro and olivine vitrophyre, were derived.

Andre, C. G.↗