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NASA NTRS1985

Petrology of the Cangas de Onis and nulles regolith breccias Implications for parent body history

The present study of the Cangas de Onis and Nulles H chondrite regolith breccias indicates that the minerals in the matrices and equilibrated clasts have essentially the same compositional distributions, so that much of the material in the castic matrix would have to have been derived from the impact comminution of clats. The apparently exclusive occurrence of H6 clasts in Cangas de Onis, and H4 clasts in Nulles, suggests that, at the locations where these breccias formed, the regolith predominantly consisted of H6 and H4 material, respectively.

Williams, C. V.↗

NASA NTRS1986

Debris-cloud collisions: Accretion studies in the space station

The growth of planetesimals in the Solar system reflects the success of collisional aggregation over disruption. Recent experiments performed at the NASA-Ames Vertical Gun Range are discussed using the production of debris cloud impaction to model protoplanetary accretion. The impact experiment assessed the differences between clustered and single body impacts on particulate surfaces. The preliminary results would indicate that collisions between two debris clouds might produce aggregates, thereby increasing particle sizes, whereas a single particle impacting a particle results in disruption and comminution. Such an experiment could provide new insight for early planetary growth processes and for interpreting the record of this stage. The use of the microgravity environment of the Space Station to further the research is discussed.

Schultz, P. H.↗

NASA NTRS1986

Petrology and classification of the Garraf, Spain chondrite

Microscopic and electron microprobe studies indicate that the Garraf meteorite is a highly-recrystallized chondrite of petrologic type 6. Olivine (Fa24.7; PMD 1.1) and low-Ca pyroxene (Fs20.9; PMD 1.1) compositions indicate that it belongs to the L-group. Based on contents of noble gases, pervasive fracturing of silicates, common undulose extinction of olivine and plagioclase, and the lack of melt pockets and maskelynite, Garraf is placed into shock facies b. It is concluded that Garraf is a highly recrystallized L6b chondrite that, after recrystallization, was cataclased and comminuted by shock.

Keil, K.↗

NASA NTRS1986

How pristine are cometary nuclei?

The claim that comets are the best obtainable source of original solar nebula material is assessed. To fully interpret the cosmochemical record contained in the comet nuclei, modifications since their formation in the primordial solar nebula, 4.5 Gyr ago must be considered. Possible processes include: comminution and collisions during formation; heating by short-lived radionuclides; accretion of interstellar gases; erosion by interstellar dust; polymerization by galactic cosmic rays; and heating and thermal evolution when the comets return to the planetary region. Consideration of these processes has important implications for where and how a sample is obtained on the cometary nucleus, and how it is preserved during the return to Earth. The possible dynamical history of short-period comets is discussed.

Weissman, Paul R.↗

NASA NTRS1987

The lunar regolith - Chemistry and petrology of Luna 24 grain size fractions

Chemical data obtained by instrumental neutron activation analysis are reported for 30 elements in eight lunar soil size fractions from 370 to less than 2 microns, as well as petrology for five size fractions down to 40-10 microns in two Luna 24 soils. While the compositions of coarser fractions are similar to each other, they differ from the fractions smaller than 10 microns; these become increasingly feldspathic and enriched in large ion lithophile elements (LILE) with decreasing grain size. The high concentrations of the Ni, Au and Ir meteoritic indicator elements in these finer fractions are consistent with comminution by meteoritic impact. Size distributions, petrology and LILE patterns indicate that Luna 24 soils are less reworked than most lunar soils.

Laul, J. C.↗

NASA NTRS1987

Planetary science

The following types of experiments for a proposed Space Station Microgravity Particle Research Facility are described: (1) low velocity collisions between fragile particles; (2) low velocity collisions of ice particles; (3) plasma-dust interaction; and (4) aggregation of finely-comminuted geological materials. The required capabilities and desired hardware for the facility are detailed.

Marshall, John R.↗

NASA NTRS1988

Aeolian weathering of Venusian surface materials - Preliminary results from laboratory simulations

An attempt is made to duplicate the atmospheric temperature, pressure, and approximate gas composition of all surface elevations on Venus by means of a simulator environment in which particles are impacted against rock targets as a way of studying planetary aeolian processes. While particles are abraded even at the low impact velocities envisioned for Venus, the same particles do not generate basaltic rock abrasion for impact velocities lower than 1 m/sec; comminution debris is instead transferred onto rock surfaces to form an accretion layer. These phenomena are seen as functions of the greater than 660 K temperatures encountered.

Marshall, John R.↗

NASA NTRS1989

Thermoluminescence and the origin of the dark matrix of Fayetteville and similar meteorites

The paper presents measurements of the induced thermoluminescence properties and carbon contents of the dark matrix and light clasts of six regolith breccias. For all of the meteorites, the dark matrix has a lower mean thermoluminescence sensitivity than the light clasts; the extent of the difference depends on the meteorite. The data suggest the formation of the dark matrix by comminution of the light clasts with the addition of a component, perhaps CM-like chondrites, with thermoluminescence properties distinct from those of ordinary chondrites.

Haq, Munir↗

NASA NTRS1991

Apollo 14 glasses and the origin of lunar soils

Electron microprobe for comparison with soil glass data were used to analyze homogeneous and heterogeneous glass clasts in four Apollo 14 regolith breccias (14042, 14301, 14313, and 14315). Glass types in the Apollo 14 samples were found to be dominated by highland compositions, which include KREEP, LKFM and highland basalt varieties. Only 14042 has a highland glass population similar to those of local Apollo 14 soils. Breccia 14301 stands out in that it is enriched in KREEP glasses with high K2O content, which are similar in composition to Apollo 12 ropy glasses. Only 14042 could be made from local present-day soils. Some of the ancient soils did not undergo breccia formation and closure, and they evolved by meteorite impact processing, by mixing together in various proportions, and by changes made by the addition of lithic fragments and other components. It is suggested that the Apollo 14 soils are made from mixtures of comminuted regolith breccias. A likely age sequence is presented.

Wentworth, S. J.↗

NASA NTRS1991

Geochemistry of 2-4-mm particles from Apollo 14 soil (14161) and implications regarding igneous components and soil-forming processes

The present paper describes the compositional systematics of 381 particles analyzed from 14161, which was taken near the lunar module as part of the bulk sample. Attention is given to the distribution of lithologies, based on petrographic examination and compositions determined by INAA, and to implications of the compositions of polymict particles regarding igneous precursors and soil-forming processes. It was found that the most abundant particles are the impact-melt lithologies and regolith and fragmental breccias. The mean composition of the entire suite of 2-4-mm particles differs from that of the associated less-than-1-mm fines by having higher concentrations of incompatible trace elements and Na2O, and a lower concentration of CaO. There is a subset of regolith breccia particles and agglutinates in the 2-4-mm particles that have nearly identical compositions and Is/FeO similar to those of the less-than-1-mm fines. It is suggested that these particles are constructional products formed from the local regolith rather than comminuted fragments of ancient regolith breccias.

Jolliff, B. L.↗

NASA NTRS1991

Chemical studies of H chondrites. III - Regolith evolution of the Fayetteville chondrite parent

Radiochemical neutron concentration analysis was used to determine Ag, Au, Bi, Cd, Co, Cs, Ga, In, Rb, Sb, Se, Te, Tl, and Zn contents in consortium samples of solar gas and track-rich dark matrix. Data obtained confirmed that the matrix is chemically homogeneous. Most dark clasts had similar mean trace element concentrations as the matrix but were compositionally much more heterogeneous. It is concluded that material incorporated with soil and compacted to form the dark portion of Fayetteville included soil-melt, the odd C2M fragment, and dark and light clasts which escaped comminution.

Xiao, Xiaoyue↗

NASA NTRS1992

Lunar hydrogen and other volatiles

The occurrence of solar wind implanted volatiles in the lunar regolith may provide resources to support a lunar settlement and fusion energy on earth in the 21st century. These volatiles include H, He, N, and C which are enriched in the finest fraction of the moon's comminuted regolith. These volatiles may be extracted by heating the soil. At 700 C near quantitative release of hydrogen and helium will occur, and approximately 20-30 percent of the N and C will corelease. It is estimated that per tonne of He-3 extracted from the lunar regolith at this temperature that 6300 tonnes H, 700 tonnes N, and 1600 tonnes C (as CO and CO2) will be released.

Jordan, J. L.↗

NASA NTRS1992

Impactite and pseudotachylite from Roter Kamm Crater, Namibia

Pseudotachylite is known to occur in a variety of geologic settings including thrust belts (e.g., the Alps and the Himalayas) and impact craters such as Roter Kamm, Namibia. Controversy exists, however, as to whether pseudotachylite can be produced by shock brecciation as well as by tectonic frictional melting. Also open to debate is the question of whether pseudotachylites form by frictional fusion or by cataclasis. It was speculated that the pseudotachylite at Roter Kamm was formed by extensional settling and adjustment of basement blocks during 'late modification stage' of impact. The occurrence of pseudotachylite in association with rocks resembling quenched glass bombs and melt breccias in a relatively young crater of known impact origin offers a rare opportunity to compare features of these materials. Petrographic, x-ray diffraction, and electron microprobe analyses of the impactites and pseudotachylites are being employed to determine the modes of deformation and to assess the role of frictional melting and comminution of adjacent target rocks.

Degenhardt, J. J., Jr.↗

NASA NTRS1993

Simulation of possible regolith optical alteration effects on carbonaceous chondrite meteorites

As the spectral reflectance search continues for links between meteorites and their parent body asteroids, the effects of optical surface alteration processes need to be considered. We present the results of an experimental simulation of the melting and recrystallization that occurs to a carbonaceous chondrite meteorite regolith powder upon heating. As done for the ordinary chondrite meteorites, we show the effects of possible parent-body regolith alteration processes on reflectance spectra of carbonaceous chondrites (CC's). For this study, six CC's of different mineralogical classes were obtained from the Antarctic Meteorite Collection: two CM meteorites, two CO meteorites, one CK, and one CV. Each sample was ground with a ceramic mortar and pestle to powders with maximum grain sizes of 180 and 90 microns. The reflectance spectra of these powders were measured at RELAB (Brown University) from 0.3 to 2.5 microns. Following comminution, the 90 micron grain size was melted in a nitrogen controlled-atmosphere fusion furnace at an approximate temperature of 1700 C. The fused sample was immediately held above a flow of nitrogen at 0 C for quenching. Following melting and recrystallization, the samples were reground to powders, and the reflectance spectra were remeasured. The effects on spectral reflectance for a sample of the CM carbonaceous chondrite called Murchison are shown.

Clark, Beth E.↗

NASA NTRS1993

Deposition of impact-generated vapors in the lunar regolith

The composition and structure of the finest grain sizes in lunar soils are strongly influenced by impact-associated processes such as comminution, melting, and vaporization. These factors in turn exert a strong influence on the optical properties of the materials. The literature regarding the fractionations that accompany the evaporation of silicate materials during impacts is reviewed, the evidence for vapor deposits in the lunar samples is considered, our own efforts to characterize vapor deposits in lunar soils using electron microscopy is described, and the implications of vapor deposits on the optical properties of the lunar fines are discussed.

Keller, Lindsay P.↗

NASA NTRS1993

The state of Fe in the lunar regolith and its relationship to the spectral reflectance properties of the moon

Space weathering may have altered the surfaces of airless bodies such as asteroids and the moon, and effectively shock-darkened their surfaces, resulting in much lower reflectance and shallower absorption bands compared to those of simple, comminuted, and powdered rocks produced in the laboratory. Studies of lunar samples from the Apollo missions have led to the suggestion that these reflection properties are inherent to the fine-grained regolith which has recorded a wide variety of shock-metamorphic effects. In particular, the lunar soil (i.e., that part of the regolith with grain sizes below 1 mm) contains native Fe in quantities above those present in the rocks from which the soil was formed. The origin and nature of the native Fe in the soil is addressed, and speculations concerning its effects upon the soil's optical properties are presented. Portions of this discussion draw heavily from earlier papers by our research group.

Taylor, Lawrence A.↗

NASA NTRS1991

Analysis of regional deformation and strain accumulation data adjacent to the San Andreas fault

A new approach to the understanding of crustal deformation was developed under this grant. This approach combined aspects of fractals, chaos, and self-organized criticality to provide a comprehensive theory for deformation on distributed faults. It is hypothesized that crustal deformation is an example of comminution: Deformation takes place on a fractal distribution of faults resulting in a fractal distribution of seismicity. Our primary effort under this grant was devoted to developing an understanding of distributed deformation in the continental crust. An initial effort was carried out on the fractal clustering of earthquakes in time. It was shown that earthquakes do not obey random Poisson statistics, but can be approximated in many cases by coupled, scale-invariant fractal statistics. We applied our approach to the statistics of earthquakes in the New Hebrides region of the southwest Pacific because of the very high level of seismicity there. This work was written up and published in the Bulletin of the Seismological Society of America. This approach was also applied to the statistics of the seismicity on the San Andreas fault system.

Turcotte, Donald L.↗

NASA NTRS1997

Description and Analysis of Core Samples: The Lunar Experience

Although no samples yet have been returned from a comet, extensive experience from sampling another solar system body, the Moon, does exist. While, in overall structure, composition, and physical properties the Moon bears little resemblance to what is expected for a comet, sampling the Moon has provided some basic lessons in how to do things which may be equally applicable to cometary samples. In particular, an extensive series of core samples has been taken on the Moon, and coring is the best way to sample a comet in three dimensions. Data from cores taken at 24 Apollo collection stations and 3 Luna sites have been used to provide insight into the evolution of the lunar regolith. It is now well understood that this regolith is very complex and reflects gardening (stirring of grains by micrometeorites), erosion (from impacts and solar wind sputtering), maturation (exposure on the bare lunar surface to solar winds ions and micrometeorite impacts) and comminution of coarse grains into finer grains, blanket deposition of coarse-grained layers, and other processes. All of these processes have been documented in cores. While a cometary regolith should not be expected to parallel in detail the lunar regolith, it is possible that the upper part of a cometary regolith may include textural, mineralogical, and chemical features which reflect the original accretion of the comet, including a form of gardening. Differences in relative velocities and gravitational attraction no doubt made this accretionary gardening qualitatively much different than the lunar version. Furthermore, at least some comets, depending on their orbits, have been subjected to impacts of the uppermost surface by small projectiles at some time in their history. Consequently, a more recent post-accretional gardening may have occurred. Finally, for comets which approach the sun, large scale erosion may have occurred driven by gas loss. The uppermost material of these comets may reflect some of the features of this erosional process, such as crust formation, and variations with depth might be expected. Overall, the upper few meters of a comet may be as complex in their own way as the upper few meters of the lunar regolith have proven to be, and by analogy, detailed studies of core samples containing this depth information will be needed to understand these processes and the details of the accretional history and the subsequent alteration history of comets.

McKay, David S.↗