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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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NASA NTRS1972

Moon - Possible nature of the body that produced the Imbrian Basin, from the composition of Apollo 14 samples.

Soils from the Apollo 14 site contain nearly three times as much meteoritic material as soils from the Apollo 11, Apollo 12, and Luna 16 sites. Part of this material consists of the ubiquitous micrometeorite component, of primitive (carbonaceous-chondrite-like) composition. The remainder, seen most conspicuously in coarse glass and norite fragments, has a decidedly fractionated composition, with volatile elements less than one-tenth as abundant as siderophiles. This material seems to be debris of the Cyprus-sized planetesimal that produced the Imbrian Basin. Compositionally this planetesimal has no exact counterpart among known meteorite classes, though group IVA irons come close. It also resembles the initial composition of the earth as postulated by the two-component model. Apparently the Imbrian planetesimal was an earth satellite swept up by the moon during tidal recession or capture, or an asteroid deflected by Mars into terrestrial space.

Ganapathy, R.↗
NASA NTRS1971

Lunar surface temperatures from Apollo 12.

The diurnal variation of temperatures in the lunar surface layer is calculated using the measured properties of the Apollo 12 samples. The results are compared with similar calculations made using data from the Apollo 11 samples and with previous infrared temperature measurements. Comparisons are also made with prior calculations which used assumed properties. These are based on an effective value of the thermal parameter (gamma) of 1034 which is obtained from integrated average values of the specific heat and thermal conductivity of the Apollo 12 fines.

Cremers, C. J.↗
NASA NTRS1971

Petrology of Apollo 11 sample 10071 - A differentiated mini-igneous complex.

Sample 10071,33 is a thin section of Apollo 11 ferrobasalt showing an unusual dual texture. The major portion of the sample is very similar to other fine grained Apollo 11 basalts, but the thin section also includes materials with a distinct variolitic texture. The two areas are separated by a sharp boundary and the mineralogy and composition of the two textural types are quite distinct. The mineralogy and chemistry of the variolitic portion show it to be the product of rapid cooling of a liquid, intermediate between the typical Apollo 11 ferrobasalt and the associated Si and K-rich mesostasis. This liquid is the result of fractional crystallization of a magma of composition closely corresponding to the major portion of the 10071 system, followed by crystal-liquid separation. The sample provides strong and direct evidence for igneous differentiation on the lunar surface.

Drake, M. J.↗
NASA NTRS1971

Age of an Apollo 15 mare basalt - Lunar crust and mantle evolution.

An internal Rb-Sr isochron for the large basalt boulder 15555 returned from the edge of Hadley rille by the Apollo 15 mission yields an age 3.32 (plus or minus 0.06) b.y. and an initial Sr-88/Sr-86, I = 0.69934 plus or minus 5. This age and I value fall well within the range obtained for the Apollo 12 basalts from the Ocean of Storms and may indicate that extensive lava flows occurred at 3.3 b.y. over widespread areas of the moon. The Sr composition of the anorthosite 15415 is as low as that of plagioclase extracted from the Apollo 11 low K rocks. The initial Sr composition of 15415 for an assumed age of 3.3 to 4.6 b.y. is extremely primitive and provides further evidence for an extremely short formation interval of a nonchondritic moon with respect to an origin in time defined by BABI.

Wasserburg, G. J.↗
NASA NTRS1972

Thermal property measurements on lunar material returned by Apollo 11 and 12 missions.

Measurement of thermal diffusivity on Apollo 11 type A and type C samples in the temperature range between 150 and 440 K under atmospheric pressure. Thermal diffusivity of type C material is lower and less temperature-dependent than type A material. Both types of samples exhibit lower thermal diffusivities than nonporous terrestrial basalt. The rate of heat generation of Apollo 11 and 12 samples was calculated from the concentrations of radioactive elements: potassium, thorium, and uranium. Apollo 11 crystalline rocks show an average rate of heat generation which is not significantly different from terrestrial basalt. The Th/U ratio does not differ greatly from chondritic and terrestrial averages.

Horai, K.-I.↗
NASA NTRS1972

Apollo 15 orbital science summary.

In this paper, summary results of the Apollo 15 orbital science payload are given, and some quick-look results of Apollo 16 are discussed. Geochemical instruments, consisting of gamma-ray, X-ray, and alpha particle spectrometers, have provided a chemical map of the lunar surface flown over by Apollo 15. The Laser Altimeter and frontside gravity data have shown some unexpected results with regard to the lunar shape, and provided new basis for understanding lunar mascons. A magnetometer, aboard the small subsatellite, has located magnetic anomalies principally on the lunar farside, and has shown that the small lunar magnetic field is smoother on the frontside than on the back. The mass spectrometer, in orbit aboard the Command and Service Modules, has measured unexpectedly large populations of molecules at orbital altitude (110 km), mostly due to spacecraft contamination. Two major camera systems have provided the first systematic metric quality photography and concurrent high resolution stereo coverage of the lunar surface.

Esenwein, G. F.↗
NASA NTRS1972

Spectral reflectance and emittance of Apollo 11 and 12 lunar material.

The thermal radiation properties of Apollo 11 and 12 fines (soils) are reviewed and presented as a function of wavelength, angle of illumination, and bulk density. The spectral directional reflectance is presented for wavelengths from 0.6 to 2 microns and for angles of illumination of 10, 20, 30, 45, and 60 deg. The normal emittance is presented for wavelengths from 2.5 to 14.5 microns. The solar albedo and total normal emittance as a function of temperature were calculated from the spectral values. The solar albedo for Apollo 11 fines is 0.099 whereas for Apollo 12 fines is approximately 0.119 for angles of illumination of 10 deg and a density of 1600 kg cu m.

Birkebak, R. C.↗
NASA NTRS1972

Study of the detail content of Apollo orbital photography

The results achieved during a study of the Detail Content of Apollo Orbital Photography are reported. The effect of residual motion smear or image reproduction processes upon the detail content of lunar surface imagery obtained from the orbiting command module are assessed. Data and conclusions obtained from the Apollo 8, 12, 14 and 15 missions are included. For the Apollo 8, 12 and 14 missions, the bracket-mounted Hasselblad camera had no mechanism internal to the camera for motion compensation. If the motion of the command module were left totally uncompensated, these photographs would exhibit a ground smear varying from 12 to 27 meters depending upon the focal length of the lens and the exposure time. During the photographic sequences motion compensation was attempted by firing the attitude control system of the spacecraft at a rate to compensate for the motion relative to the lunar surface. The residual smear occurring in selected frames of imagery was assessed using edge analyses methods to obtain and achieved modulation transfer function (MTF) which was compared to a baseline MTF.

Kinzly, R. E.↗
NASA NTRS1972

Gas analysis of Apollo 12, 14, and 15 samples by laser-probe mass spectrometry

Solar wind gases, cosmogenic gases from high energy spallation reactions from soxmic rays, and radiogenic gases from decay of radioactive potassium and from uranium and thorium isotopes were analyzed in lunar materials. Details are presented on two aspects of the studies: (1) The spatial distribution of Ar-40/Ar-38 ages in lunar breccia 14301 was determined. The ages of clasts within this breccia are 3.68 + or - 0.09 and 2.9 + or - 0.3 x 10 to the 9th power years. Parentless radiogenic Ar-40 exists within the fine-grained matrix. (2) The distribution of helium, neon, and argon isotopes within Apollo 15 samples results primarily from fractionated solar wind gases, accompanied by small quantities of cosmogenic gases. Comparison of this Apollo 15 data with Kapoeta and Fayetteville meteorite and Apollo 12 and 14 data indicates that solar wind implantation followed by fractionation of the gases was primarily responsible for incorporation of original gas phase within solid bodies of the solar system.

Imegrue, G. H.↗
NASA NTRS1972

Electrophoresis demonstration on Apollo 16

Free fluid electrophoresis, a process used to separate particulate species according to surface charge, size, or shape was suggested as a promising technique to utilize the near zero gravity condition of space. Fluid electrophoresis on earth is disturbed by gravity-induced thermal convection and sedimentation. An apparatus was developed to demonstrate the principle and possible problems of electrophoresis on Apollo 14 and the separation boundary between red and blue dye was photographed in space. The basic operating elements of the Apollo 14 unit were used for a second flight demonstration on Apollo 16. Polystyrene latex particles of two different sizes were used to simulate the electrophoresis of large biological particles. The particle bands in space were extremely stable compared to ground operation because convection in the fluid was negligible. Electrophoresis of the polystyrene latex particle groups according to size was accomplished although electro-osmosis in the flight apparatus prevented the clear separation of two particle bands.

Snyder, R. S.↗
NASA NTRS1973

Apollo experience report: Protection against radiation

Radiation protection problems on earth and in space are discussed. Flight through the Van Allen belts and into space beyond the geomagnetic shielding was recognized as hazardous before the advent of manned space flight. Specialized dosimetry systems were developed for use on the Apollo spacecraft, and systems for solar-particle-event warning and dose projection were devised. Radiation sources of manmade origin on board the Apollo spacecraft present additional problems. Methods applied to evaluate and control or avoid the various Apollo radiation hazards are discussed.

English, R. A.↗
NASA NTRS1972

Topographic mapping of the Apollo 16 landing site

The techniques are described for obtaining high resolution photographs from the Apollo 14 lunar orbiter for topographic mapping of the Descartes landing site for use in planning Apollo 16. The Apollo 16 spacecraft landed approximately 250 m from the selected target point, and few topographic surprises were encountered.

Hill, R. O.↗
NASA NTRS1972

Orientale Basin deposits (Riccioli area) in Apollo 16 earthshine photography, part E

Interpretations of photography of Orientale Basin deposits obtained under earthshine illumination conditions during the Apollo 16 mission are presented. Although the quality of these photographs is less than that obtainable in sunshine, these regions are in the dark during Apollo missions because of the locations of the Apollo landing sites. Photography of these regions under different lighting geometry and from different viewpoints is therefore a useful addition to previous photographic data. Oblique photography was obtained of Riccioli Crater and adjacent areas, which lie northeast of the Orientale Basin.

Lloyd, D. D.↗
NASA NTRS1973

Apollo 17 Mission Report

Operational and engineering aspects of the Apollo 17 mission are outlined. The vehicle configuration was similar to those of Apollo 15 and 16. There were significant differences in the science payload for Apollo 17 and spacecraft hardware differences and experiment equipment are described. The mission achieved a landing in the Taurus-Littrow region of the moon and returned samples of the pre-Imbrium highlands and young craters.

MIssion Evaluation Team↗
NASA NTRS1973

Apollo 17 heat flow and convection experiments: Final data analyses results

A group of experiments called the Apollo 17 heat flow and convection (HFC) experiments was conducted, aboard the Apollo 17 spacecraft while in translunar coast on the way to the moon. These experiments together with the HFC experiments flown on Apollo 14 demonstrated and provided data on two types of low-g natural convection: cellular, surface tension-driven convection and convection in confined fluids caused by spacecraft and astronaut movements. Observed convection onset times show that surface tension-driven convection occurs at lower temperature gradients in low-g than in one-g environments. Data on heat flow in confined fluids show that spacecraft and astronaut movements can cause significant degrees of convection.

Bannister, T. C.↗
NASA NTRS1972

Sedimentology of clastic rocks returned from the moon by Apollo 15.

A petrographic study of eleven samples of clastic rock returned from the moon by Apollo 15 suggests that two lithologies are present. The distinction between the two lithologies is based on the glass content of the rock matrices and the morphology of the detrital particles. Group I rocks have abundant, glass-rich, porous matrices and glass particles with morphologies comparable to those of glass particles in the lunar soil. The group I rocks were probably formed by welding or sintering of surficial soil deposits by impact-generated base surges of limited extent. Group II rocks have an essentially mineralic matrix and have an abundance of rounded mineral grains. Sample 15455 is the only Apollo 15 sample assigned to this group. In its general textural features, sample 15455 is comparable with the group II rocks from the Fra Mauro Formation at the Apollo 14 site. Textural features such as shock modification and rounding of mineral grains suggest that this sample is the product of a large-scale impact-generated base surge which possibly resulted from the Imbrian event.

Lindsay, J. F.↗
NASA NTRS1972

Introductory remarks - The Apollo 14 mission.

Description of the Apollo 14 mission within the general context of the entire Apollo program. In the Apollo 14 mission, which ended successfully on Feb. 9, 1971, more time was spent on extravehicular activities than in previous missions. In addition, enlarged propellant tanks permitted a larger payload, and some 42 kilograms of samples were brought back.

Newell, H. E.↗
NASA NTRS1972

A quest for porphyrins in lunar soil - Samples from Apollo 11, 12 and 14.

Analyses for porphyrins in the lunar samples were carried out by extracting the lunar soils as received by organic solvents followed by analytical demetallation using methanesulfonic acid after which free-base porphyrins, if present, were recovered and demonstrably recomplexed with divalent cations. Samples from Apollo 11 showed the presence of fluorescent substances attributed to exhaust from the descent engine. One sample from Apollo 12 showed pigments resembling porphyrins. The Apollo 14 results were negative.

Hodgson, G. W.↗