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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 559 records · Page 31
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NASA NTRS1972

Trace elements in Apollo 15 samples - Implications for meteorite influx and volatile depletion on the moon

Five Apollo 15 soils and four rocks were examined by neutron activation analysis for 18 volatile and siderophile elements. The results obtained are initially interpreted in terms of local geologic problems at the Apollo 15 site. Implications bearing on the meteorite influx and volatile element depletion on the moon are then examined. Elbow Crater soil 15081, collected 65 m from the rim, contains a meteoritic component equivalent to 1.72% Cl material, similar to that at other lunar sites. Other soils are lower owing to dilution by fresh bedrock or talus from the Apennine Front. The moon-earth difference in volatile elements is discussed from the viewpoint of a difference in the efficiency of accretion from the solar nebula.

Morgan, J. W.↗
NASA NTRS1974

Geophysical data and the interior of the moon

Geophysical data and physical properties of the lunar interior are considered, giving attention to density, gravity field, viscosity, the strength of lunar materials, electrical conductivity, and magnetic properties. Seismic data and structure of the lunar interior are discussed, taking into account moonquakes and lunar tectonism, the velocity structure, and the compositional implications of the velocity structure. Questions regarding the thermal state and the evolution of the moon are also explored. The data and the models presented characterize the moon as a differentiated body which evolved relatively early in its history.

Toksoz, M. N.↗
NASA NTRS1974

Spatial distribution of polarization over the disks of Venus, Jupiter, Saturn, and the moon

The method of photographic subtraction, which superposes positive and negative photographs taken with the analyzer rotated through 90 deg, is used to analyze polarization photographs of Venus, Jupiter, Saturn, and the moon. For Venus, near 90 deg phase angle, variation in polarization in ultraviolet light appears to correspond generally with the position of the cloud markings. The northern hemisphere of Saturn shows higher polarization in blue light than does the rest of the planet. The polarization of the moon is shown to deviate significantly from Umov's law for reciprocity of polarization and reflectivity in certain regions.

Fountain, J. W.↗
NASA NTRS1974

Mie scattering of the interplanetary magnetic field by the whole moon

Based on the results of the Apollo magnetometer experiments, it is shown that the wavelength spectrum of the fluctuations of the interplanetary magnetic field includes scales consistent with the radius of the moon. Quadrupole and possibly octupole magnetic multipoles are found in the data and indicate that the moon is excited in several modes.

Sonett, C. P.↗
NASA NTRS1974

The evolution of the moon

The thermal evolution of the moon as it can be defined by the available data and theoretical calculations is discussed. A wide assortment of geological, geochemical and geophysical data constrain both the present-day temperatures and the thermal history of the lunar interior. On the basis of these data, the moon is characterized as a differentiated body with a crust, a 1000-km-thick solid mantle (lithosphere) and an interior region (core) which may be partially molten. The presence of a crust indicates extensive melting and differentiation early in the lunar history. The ages of lunar samples define the chronology of igneous activity on the lunar surface. This covers a time span of about 1.5 billion years, from the origin to about 3.16 billion years ago. Most theoretical models require extensive melting early in the lunar history, and the outward differentiation of radioactive heat sources.

Toksoz, M. N.↗
NASA NTRS1974

Mapping of the moon: Past and present

The present work provides an outline of the history of the efforts to map the topography of the surface of the moon, from the days of pre-telescopic astronomy to the present. The first part of the book covers the time span from 1600 to 1960 and reproduces numerous examples of this early, earth-based selenographic work. The manned lunar missions in the 1960's revolutionized the science of lunar mapping with their high-resolution, close-range photography of the moon. In 1959, a comprehensive lunar mapping program was initiated by two DOD mapping agencies - the U.S. Air Force Aeronautical Chart and Information Center (ACIC) and the U.S. Army Map Service (AMS). In the course of this program, the cause of lunar mapping enlisted for the first time the services of professional cartographers; the outcome of their efforts speedily relegated all previous work into absolescence. The methods and results of this work are described, and the underlying principles of physical selenodesy are set forth, including the definition of lunar coordinates and the methods for a determination of three-dimensional coordinates of lunar features. A section is included on lunar mapping in the U.S.S.R.

Kopal, Z.↗
NASA NTRS1974

Methods of radar studies of the moon and the planets from spacecraft

Radar studies of the moon and planets from the earth have been valuable but limited in comparison to radar studies from spacecraft. Autonomous and non-autonomous methods of radar research from space satellites and probes are considered. Results of both the Luna and Surveyor series of lunar spacecraft are presented. It is concluded that use of radar in spacecraft allows valuable, high resolution measurement even near the limb and on the back side of the moon.

Krupenio, N. N.↗
NASA NTRS1974

Meteoritic material on the moon

Micrometeorites, ancient planetesimal debris from the early intense bombardment, and debris of recent, crater-forming projectiles are discussed and their amounts and compositions have been determined from trace element studies. The micrometeorite component is uniformly distrubuted over the entire lunar surface, but is seen most clearly in mare soils whereas, the ancient component is seen in highland breccias and soils. A few properties of the basin-forming objects are inferred from the trace element data. An attempt is made to reconstruct the bombardment history of the moon from the observation that only basin-forming objects fell on the moon after crustal differentiation. The apparent half-life of basin-forming bodies is close to the calculated value for earth-crossing planetesimals. It is shown that a gap in radiometric ages is expected between the Imbrium and Nectaris impacts, because all 7 basins formed in this interval lie on the farside or east limb.

Morgan, J. W.↗
NASA NTRS1974

Formation and composition of the moon

Many of the properties of the moon are discussed including the enrichment in Ca, Al, Ti, U, Th, Ba, Sr and the REE and the depletion in Fe, Rb, K, Na and other volatiles which could be understood if the moon represents a high temperature condensate from the solar nebula. Thermodynamic calculations show that Ca, Al and Ti rich compounds condense first in a cooling nebula. The initial high temperature mineralogy is gehlenite, spinel, perovskite, Ca-Al-rich pyroxenes and anorthite. Inclusions in Type III carbonaceous chondrites such as the Allende meteorite are composed primarily of these minerals and, in addition, are highly enriched in refractories such as REE relative to carbonaceous chondrites. These inclusions can yield basalt and anorthosite in the proportions required to eliminate the europium anomaly, leaving a residual spinel-melilite interior.

Anderson, D. L.↗
NASA NTRS1974

The evolution of the moon and the terrestrial planets

The thermal evolutions of the Moon, Mars, Venus and Mercury are calculated theoretically starting from cosmochemical condensation models. An assortment of geological, geochemical and geophysical data are used to constrain both the present day temperatures and the thermal histories of the planets' interiors. Such data imply that the planets were heated during or shortly after formation and that all the terrestrial planets started their differentiations early in their history. The moon, smallest in size, is characterized as a differentiated body with a crust, a thick solid mantle and an interior region which may be partially molten. Mars, intermediate in size, is assumed to have differentiated an Fe-FeS core. Venus is characterized as a planet not unlike the earth in many respects. Core formation has occurred probably during the first billion years after the formation. Mercury, which probably has a large core, may have a 500 km thick solid lithosphere and a partially molten core if it is assumed that some heat sources exist in the core.

Toksoez, M. N.↗
NASA NTRS1974

Evolution of the moon: The 1974 model

Investigations are reported of Apollo and Luna explorations which have brought about the understanding of the moon and its structure. It is shown that with this knowledge of the moon, a better understanding is presented of the earth's origin, structure and composition.

Schmitt, H. H.↗
NASA NTRS1975

Seismic effects from major basin formations on the moon and Mercury

Grooved and hilly terrains occur at the antipode of major basins on the moon (Imbrium, Orientale) and Mercury (Caloris). Such terrains may represent extensive landslides and surface disruption produced by impact-generated P-waves and antipodal convergence of surface waves. Order-of-magnitude calculations for an Imbrium-size impact on the moon indicate P-wave-induced surface displacements of 10 m at the basin antipode that would arrive prior to secondary ejecta. Comparable surface waves would arrive subsequent to secondary ejecta impacts beyond 1000 km and would increase in magnitude as they converge at the antipode. Other seismically induced surface features include: subdued, furrowed crater walls produced by landslides and concomitant secondary impacts; emplacement and leveling of light plains units owing to seismically induced 'fluidization' of slide material; and perhaps the production and enhancement of deep-seated fractures that led to the concentration of farside lunar maria in the Apollo-Ingenii region.

Schultz, P. H.↗
NASA NTRS1974

The rotation of the moon

The present review attempts to give a comprehensible demonstration that the Cassini determination of the geometric laws describing the gross rotation of the moon relative to the precessing lunar orbit in terms of the mean orientation elements of the orbit (the Cassini motion) is an approximation to a dynamically consistent system. Traditional approaches to the derivation of the physical librations of the moon are presented, in addition to recent studies on flaws in the traditional theories. For future research, the advantages of an analytic theory will be required.

Mulholland, J. D.↗
NASA NTRS1974

Apollo 17 petrology and experimental determination of differentiation sequences in model moon compositions

Experimental studies of model moon compositions are discussed, taking into account questions related to the differentiation of the outer layer of the moon. Phase relations for a series of proposed lunar compositions have been determined and a petrographic and electron microprobe study was conducted on four Apollo 17 samples. Two of the samples consist of high-titanium mare basalts, one includes crushed anorthosite and gabbro, and another contains blue-gray breccia.

Hodges, F. N.↗
NASA NTRS1974

K and U systematics and average concentrations on the moon

The K-U, Th-U, and Th-Al systematics for lunar samples from the Apollo 11-17 missions and the Luna 16 and 20 missions are summarized. With few exceptions (granitic portion of 12013 and the Apollo 17 mare basalts) the Th/U ratio is 3.8 plus or minus 0.2. The K/U ratio for lunar samples is about 2600 and is distinctly different from the K/U ratio found in terrestrial samples and in the majority of meteorites. The K-U systematics are similar to the K-La, K-Sm, K-Ba, and K-Zr systematics, suggesting that the moon accreted approximately homogeneously. Based on a model the moon contains an average abundance of about 80 ppb U, about 200 ppm K, and about 7 times chondritic abundances for all the refractory elements such as Al, Ca, Ti, Zr, Ba, Sr, and REE. The Th-Al systematics of many lunar highland rocks are dominated by the presence of the rock-type KREEP.

Schonfeld, E.↗
NASA NTRS1974

Bulk compositions of the moon and earth, estimated from meteorites

The present work calculates the bulk compositions of the earth and moon, based on the assumption that these planets formed by the same processes as chondrites. In terms of the model presented, the earth contains 9.2% early condensate and 1.5% carbonaceous, volatile-rich silicate. For the moon these percentages are 30.1 and 0.04, respectively. When lunar and terrestrial basalt data are normalized to these model compositions, element abundance patterns based on the percentages (assuming that each component carried its cosmic complement of trace elements) demonstrate the essential identity of igneous processes on both celestial bodies.

Ganapathy, R.↗
NASA NTRS1974

Oxygen isotopic constraints on the composition of the moon

The mean oxygen isotopic composition of 5 Apollo 17 soils, one Apollo 17 breccia and one Apollo 12 soil is delta O-18 = 5.63 + or - .05 and delta O-17 = 3.8 + or - .2%. These values are within several tenths of a part permil of the composition of a large fraction of the lunar interior. High-temperature condensate aggregates from Allende and other C2 and C3 chondrites are vastly enriched in O-16 compared to this composition. The moon cannot be a mixture of ordinary chondrites and Allende inclusions, nor can it be derived from such a mixture by chemical fractionation processes. The moon's isotopic composition is consistent with a mixture of high- and low-temperature condensates but the refractory fraction would have to be free of the O-16-rich component so prevalent in the meteoritic aggregates, a fact which makes such models less attractive than they once seemed.

Grossman, L.↗
NASA NTRS1974

Episodic release of Ar-40 from the interior of the moon

Measurements of lunar atmosphere made by the mass spectrometer at the Apollo 17 landing site during the first 9 lunations of 1973 show an apparently cyclical variation of radiogenic Ar-40, with maximum to minimum abundance ratio of about 2. There seems to be a 6-7 month periodicity in the oscillation, but the limited data base makes a fixed oscillatory pattern uncertain. The significance of the variation of atmospheric argon lies in the implication that its source is episodic in nature, ranging in strength from about 1% of the total rate of production of Ar-40 in the moon to near zero. This requires a presently active mechanism for transient venting of gas from deep within the moon.

Hodges, R. R., Jr.↗