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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 37 records · Page 2
All sourcesNASA NTRSDOE OSTI
NASA NTRS1980

Thermal conduction in a composite circular cylinder - A new technique for thermal conductivity measurements of lunar core samples

A technique is described for the measurement of the thermal conductivity of lunar core samples. According to their technique, the core sample is heated radiatively from the outside at a known rate, the temperature is measured at the surface of the core-tube, and the thermal conductivity of the sample is determined by comparing the measured temperature with the theory. The corresponding problems for a composite slab or sphere were solved and the solutions are presented for possible future application to the thermal conductivity measurements. The experimental apparatus construction and procedure are examined as well as the number of precautions taken to preserve the sample from disturbances and to improve the measurement results.

Horal, K.↗
NASA NTRS1983

An upper bound on the radius of a highly electrically conducting lunar core

Parker's (1980) nonlinear inverse theory for the electromagnetic sounding problem is converted to a form suitable for analysis of lunar day-side transfer function data by: (1) transforming the solution in plane geometry to that in spherical geometry; and (2) transforming the theoretical lunar transfer function in the dipole limit to an apparent resistivity function. The theory is applied to the revised lunar transfer function data set of Hood et al. (1982), which extends in frequency from 10 to the -5th to 10 to the -3rd Hz. On the assumption that an iron-rich lunar core, whether molten or solid, can be represented by a perfect conductor at the minimum sampled frequency, an upper bound of 435 km on the maximum radius of such a core is calculated. This bound is somewhat larger than values of 360-375 km previously estimated from the same data set via forward model calculations because the prior work did not consider all possible mantle conductivity functions.

Hobbs, B. A.↗
NASA NTRS2010

Seismic Detection of the Layers of the Lunar Core

This slide presentation reviews the analysis of Apollo-era seismic data and indirect geophysical measurements (i.e., moment of inertia, lunar laser ranging and electromagnetic induction) and concludes that significant questions still remain. The Apollo deep moonquake seismograms using terrestrial array processing methods is analyzed to infer the structure of the lunar core. The results indicate the presence of a solid inner and fluid outer core.

Weber, Renee C.↗
NASA NTRS1980

Lunar core detection using two surface magnetometers at very low frequency

A method is described which allows the analysis of the dipole component of the lunar induction using only measurements of two surface magnetometers. This is possible because the very low frequency of the relevant signal components limits the lunar response to the dipole partial wave. Because only surface magnetometers are necessary the simultaneous measurements made by the Apollo 15 and 16 surface modules can be used. Thus, additional information concerning the lunar transfer function can be applied to the determination of the existence and size of a metallic lunar core.

Herbert, F.↗
NASA NTRS2015

Experiments on Lunar Core Composition: Phase Equilibrium Analysis of A Multi-Element (Fe-Ni-S-C) System

Previous geochemical and geophysical experiments have proposed the presence of a small, metallic lunar core, but its composition is still being investigated. Knowledge of core composition can have a significant effect on understanding the thermal history of the Moon, the conditions surrounding the liquid-solid or liquid-liquid field, and siderophile element partitioning between mantle and core. However, experiments on complex bulk core compositions are very limited. One limitation comes from numerous studies that have only considered two or three element systems such as Fe-S or Fe-C, which do not supply a comprehensive understanding for complex systems such as Fe-Ni-S-Si-C. Recent geophysical data suggests the presence of up to 6% lighter elements. Reassessments of Apollo seismological analyses and samples have also shown the need to acquire more data for a broader range of pressures, temperatures, and compositions. This study considers a complex multi-element system (Fe-Ni-S-C) for a relevant pressure and temperature range to the Moon's core conditions.

Go, B. M.↗
NASA NTRS1982

Measurements of the lunar induced magnetic moment in the geomagnetic tail - Evidence for a lunar core

Apollo 15 and 16 subsatellite fluxgate magnetometer data have been analyzed for all intervals in which the moon was in the lobes of the geomagnetic tail to obtain an improved estimate of the average magnitude of the induced dipole moment of the moon. The resulting set of estimates yields an induced magnetic moment of -4.23 x 10 to the 22nd Gauss-cu cm per Gauss of applied field, corresponding to a G-factor of -0.008 + or - 0.001. These measurements do not place strong constraints on the conductivity of the lunar core. The observed effects would be detected as long as the core conductivity was greater than about 10 mho/m. If the outer cool layers of the moon that are at temperatures below the effective Curie point contain little or no free iron, then these measurements are consistent with the presence of a conducting core whose radius is slightly larger than 400 km. If these outer layers of the moon contain significant amounts of free iron and hence exhibit the paramagnetism expected in such a situation the core size could be even greater.

Russell, C. T.↗
NASA NTRS2001

Influence of a Fluid Lunar Core on the Moons Orientation

Oblateness of and dissipation at the lunar liquid-core/solid-mantle boundary affects the precession of core and mantle. Analysis of Lunar Laser ranges gives a weak detection of oblateness and a strong determination of dissipation. Additional information is contained in the original extended abstract.

Williams, J. G.↗
NASA NTRS1974

Preservation of lunar core samples - Preparation and interpretation of three-dimensional stratigraphic sections

Preservation and analysis of core samples collected from the lunar regolith are discussed. The objectives of core sampling are described together with the core-sampling equipment used in the Apollo program. The effects of disaggregation in core samples are summarized, and ways to preserve the stratigraphy in these samples are reviewed, particularly partial impregnation of samples with polybutyl methacrylate. It is shown that stratigraphic sections preserved in this way reveal individual fragments of the regolith in their original positions, primary and secondary depositional structures related to lunar processes, and the nature and extent of deformations caused by sampling equipment. It is concluded that since the core sedimentary structures indicate complex three-dimensional variations in the regolith, quantitative models of regolith evolution must allow for distinctive local histories as well as irregular reworking and deposition events due to impact processes.

Fryxell, R.↗
NASA NTRSDate not supplied

From Apollo to Artemis: Opening and Processing Lunar Core 73002 for the ANGSA Program

The Apollo mission returned 382 kg of lunar material comprising rock, soil and core samples. Some of these samples were intentionally set aside after their return from the Moon for future study, including samples sealed on the lunar surface, frozen samples and samples stored under Helium. The Apollo Next Generation Sample Analysis (ANGSA) program was established to study thesesamples, in part to help bridge the gap between Apollo and the next generation of lunar science and exploration.Apollo 17 double drive tube core sample 73001/73002 was collected about 50 meters east of Lara Crater from a landslide deposit originating from South Massif. After separating the two halves, the lower drive tube 73001 was immediately sealed in a special vacuum container. Both drive tubes were then placed in an Apollo Lunar Sample Return Container (ALSRC) and returned to Earth under vacuum. Total sample weight and length of 73001/73002 is 1263.0 g and up to 60 cm, with the upper drive 73002 containing 429.7 g and 23 cm of material ( which was then compressed to 18.5 cm during extrusion in the lab). We will present the meticulous methods involved in preparing for, opening and processing lunar core 73002, the upper half of the double drive tube. This includes searching and locating procedures and tools, practicing assembly and extrusion in a mock-up, and finally opening and dissecting the core sample 73002. Challenges (both expected and unexpected) encountered along the way and lessons learned during this project will help pave the way towards improving future lunar sample return missions and advancing insight into the Moon’s history

C. H. Krysher↗
NASA NTRS1992

Origin of the moon and lunar core formation

In a recent version of the giant impact hypothesis by O'Neill, the initial abundances of the siderophile elements in the lunar mantle were established not only by combining impactor material and proto-Earth material, but also by adding a late reduced veneer. O'Neal also appealed to the possible volatilities of some elements (Mo and W) under conditions of lunar accretion, and required the segregation of a small Ni-rich metallic core. An attempt to more rigorously model lunar core formation in the O'Neill scenario is made by correlating degree of partial melting to temperature and extrapolating the 1260 C partition coefficients to the appropriate temperatures along a constant redox buffer.

Hillgren, Valerie J.↗
NASA NTRS2004

Lunar Core and Tides

Variations in rotation and orientation of the Moon are sensitive to solid-body tidal dissipation, dissipation due to relative motion at the fluid-core/solid-mantle boundary, and tidal Love number k2 [1,2]. There is weaker sensitivity to flattening of the core-mantle boundary (CMB) [2,3,4] and fluid core moment of inertia [1]. Accurate Lunar Laser Ranging (LLR) measurements of the distance from observatories on the Earth to four retroreflector arrays on the Moon are sensitive to lunar rotation and orientation variations and tidal displacements. Past solutions using the LLR data have given results for dissipation due to solid-body tides and fluid core [1] plus Love number [1-5]. Detection of CMB flattening, which in the past has been marginal but improving [3,4,5], now seems significant. Direct detection of the core moment has not yet been achieved.

Williams, J. G.↗
NASA NTRS1976

Magnetic evidence concerning a lunar core

Two different methods were used to determine the lunar electromagnetic response: (1) comparison of Apollo 12 and Explorer 35 magnetometer data; and (2) observation of the dipole field configuration by orbiting Apollo 15 and 16 subsatellites. The methods give significantly different results. The subsatellite observations require the existence of a core, while the Apollo 12 and Explorer magnetometer measurements allow, but do not require, the existence of a core. Despite this, an upper limit of 580 km has been computed for the radius of the core.

Goldstein, B. E.↗
NASA NTRS2020

Adventures in Lunar Core Processing: Timeline of and Preparation for Opening of Core Sample 73002 for the ANGSA Program

The Apollo mission returned 382 kg of rocks, soil and core samples, which have helped to advance our knowledge of lunar science. Studies of these lunar samples are crucial for our understanding of the Moon’s geological evolution. Here, we present the meticulous process that involves preparing for, and ultimately opening, the unopened Apollo 17 drive tube: 73002,0, so that the next generation of lunar scientists can further our insight into the Moon’s history.

Krysher, C. H.↗
NASA NTRS1976

Ferromagnetic resonance studies of lunar core stratigraphy

We first review the evidence which links the characteristic ferromagnetic resonance observed in lunar fines samples with agglutinatic glass produced primarily by micrometeorite impacts and present new results on Apollo 15, 16, and 17 breccias which support this link by showing that only regolith breccias contribute significantly to the characteristic FMR intensity. We then provide a calibration of the amount of Fe metal in the form of uniformly magnetized spheres required to give our observed FMR intensities and discuss the theoretical magnetic behavior to be expected of Fe spheres as a function of size. Finally, we present FMR results on samples from every 5 mm interval in the core segments 60003, 60009, and 70009. These results lead us to suggest: (1) that secondary mixing may generally be extensive during regolith deposition so that buried regolith surfaces are hard to recognize or define; and (2) that local grinding of rocks and pebbles during deposition may lead to short scale fluctuations in grain size, composition, and apparent exposure age of samples.

Housley, R. M.↗
NASA NTRS1977

Chemical characterization of lunar core 60010

Twenty-eight major, minor, and trace-element abundances have been determined in nine fines fractions of core 60010 by instrumental thermal and 14 MeV neutron activation analysis. With the exception of the elements Fe, Co, and Ni, core section 60010 exhibits a much more uniform composition than the lower section (60009) of the double drive tube collected at the Apollo 16 LM site. The siderophilic meteorite indicator elements Fe, Co, and Ni are significantly enriched in subsample 40, which is located 3.0-4.5 cm below the lunar surface, and are highly variable throughout the 60010 core section. Microscopic examination of subsample 40 revealed the presence of numerous metallic fragments including an approximately 1-mm metal fragment exhibiting only Fe, Co, Ni, and Ir gamma-ray peaks and having a composition typical of a coarse octahedrite. Composition profiles of 60010 exhibit small variations in lithophilic element abundances which can be related to most of the seven stratigraphic units of Duke and Nagle (1976). Although the basal portion of 60010 has been described as texturally similar to the upper unit of 60009, the present chemical studies show a marked compositional difference at this interface.

Ali, M. Z.↗
NASA NTRS1977

Remanent magnetization stratigraphy of lunar cores

Depth dependent fluctuations have been observed in the natural remanent magnetizations (NRM) of drive cores and drill strings from Apollo 16 and 17 missions. Partial demagnetization of unstable secondary magnetizations and identification of characteristic error signals from a core which is known to have been recently disturbed allow us to identify and isolate the stable NRM stratigraphy in double drive core 60010/60009 and drill strings 60002-60004. The observed magnetization fluctuations persist after normalization to take into account depth dependent variations in the carriers of stable NRM. We tentatively ascribe the stable NRM stratigraphy to instantaneous records of past magnetic fields at the lunar surface and suggest that the stable NRM stratigraphy technique could develop as a new relative time-stratigraphic tool, to be used with other physical measurements such as relative intensity of ferromagnetic resonance and charged particle track density to study the evolution of the lunar regolith.

Banerjee, S. K.↗
NASA NTRS1976

Chemical characterization of lunar core 60009

A total of 27 major, minor and trace element abundances in 27 fine fractions (smaller than 1 mm) of core 60009 were determined by instrumental neutron activation analysis. The core was divided into five chemically defined stratigraphic units. Unit 1, 0.5 to 11.5 cm, is characterized by low Ca and Al abundances which increase towards the base of the unit and high ferromagnesian element abundances. Unit 2, 11.5 to 19.8 cm, has higher abundances of Ca and Al and lower abundances of ferromagnesian elements than unit 1 and is much more uniform. Unit 3, 19.8 to 25.7 cm is very similar to unit 1 and may have been derived from the same source region. Unit 4, 25.7 to 29.6 cm, has the highest Ca and Al abundances of all the units defined and the lowest abundances of ferromagnesian elements. The ferromagnesian elements generally decrease in abundance towards the base of the unit. This unit exhibits a positive Eu anomaly. Unit 5, 29.6 to 31.5 cm, has the lowest Ca and Al abundances and highest ferromagnesian abundances of all the units. The unit boundaries correspond well with major unit boundaries characterized by Duke and Nagle (1974) on the basis of textural parameters, structure, composition and thickness of layers.

Ali, M. Z.↗