Lunar polymict breccia 14321: a petrographic study

Seven petrographic thin sections of lunar rock sample 14321, ‘Big Bertha’, have been examined. It is a complex rock incorporating diverse lithic and single crystal fragments and represents a sampling of the heterogeneous Fra Mauro formation, considered by the writers to be lithified debris from the Imbrium impact event. Electron probe microanalysis and microscopic study of textures reveal the assembly history of this breccia which in turn allows some interpretation of the nature of the pre-Imbrium crust and the effect of the Imbrium impact and the subsequent transportation to the Apollo 14 site. The present-day polymict breccia 14321 is composed of basaltic clasts originating from the fragmentation of a single or closely related set of lava cooling units, a set of fragmental clasts designated as microbreccia 3 (themselves polymict microbreccias), and a light colored matrix which formed rock 14321 by cementing the two major groups of clasts. The light colored matrix material is derived from the fragmentation and mutual abrasion of the basalt and microbreccia 3. On the basis of consistent textural relations two older sets of microbreccias have been identified within microbreccia 3. Microbreccia 1 clasts are well-rounded, relatively light colored, and noritic. They are always completely enclosed within microbreccia 3, most often forming the central cores of rounded accretionary lapilli structures which we have designated as microbreccia 2. Microbreccias 1, 2, 3, and macrobreccia 14321 represent a chronological series of fragmentation and lithification events. Each of these events involved some thermal and/or shock metamorphism as evidenced by mineralogical and textural criteria, and the chronological order of formation of the breccias also corresponds to a decreasing intensity of associated thermal effects. The petrology and mineralogy of 14321 are described in detail in this paper. A more general interpretation of the combined petrographic and chemical data is given in Duncanet al. (1975a).     

The life and times of Big Bertha: lunar breccia 14321

The lithic units of polymict breccia 14321 (Big Bertha) have been grouped according to composition, texture, degree of metamorphism, and additional criteria based on a systematic study of the interrelationships of all clast-matrix pairs. From this information it has been possible to reconstruct the assembly and metamorphic history of this breccia. The earliest formed fragmental component of 14321 (microbreccia-1) is dominated by KREEP-rich norite, extruded and subsequently brecciated and lithified in an ejecta blanket at approximately 1000°C in the general region of Mare Imbrium after the Serenitatis impact but prior to the Imbrium impact. This early microbreccia component and lesser amounts of mare-type basalt, microgranite, rhyolite glass, anorthosite and olivine microbreccia were assembled at the Apollo 14 site as part of the Fra Mauro ejecta blanket from the Imbrium impact. The resulting microbreccia-3 incorporates all the lithic types above and accretionary lapilli structures (microbreccia-2) in a dark matrix annealed at approximately 700°C. A later impact on the Fra Mauro excavated and mutually abraded microbreccia-3 and a local, 14321-type, basalt which were assembled into polymict breccia 14321. Final placement of 14321 at its sampling location was accomplished during the minor Cone Crater impact event.     

Formation of the Bencubbin polymict meteoritic breccia

The Bencubbin meteorite is a polymict breccia consisting of a host fraction of ~60% metal and ~40% ferromagnesian silicates and a selection of carbonaceous, ordinary and ‘enstatite’ chondritic clasts. Concentrations of 27 elements were determined by neutron activation in replicate samples of the host silicates and the ordinary and carbonaceous chondritic clasts; 12 elements were determined in the host metal. Compositional data for the ordinary chondrite clast indicate a classification of LL4 ± 1. Refractory element data for the carbonaceous chondrite clast indicate that it belongs to the CI-CM-CO clan; its volatile element abundances are intermediate between those of CM and CO chondrites. Abundances of nonvolatile elements in the silicate host are similar to those in the carbonaceous chondrite clast and in CM chondrites; the rare earths are unfractionated. We conclude that it is not achondritic as previously designated, but chondritic and that it is probably related to the CI-CM-CO clan; its volatile abundances are lower than those in CO chondrites. Oxygen isotope data are consistent with these classifications. Host metal in Bencubbin and in the closely related Weatherford meteorite has low abundances of moderately volatile siderophiles; among iron meteorite groups its nearest relative is group IIIF.We suggest that Bencubbin and Weatherford formed as a result of an impact event on a carbonaceous chondrite regolith. The impact generated an ‘instant magma’ that trapped and surrounded regolithic clasts to form the polymict breccia. The parent of this ‘magma’ was probably the regolith itself, perhaps mainly consisting of the so-called ‘enstatite’ chondrite materials. Accretion of such a variety of materials to a small parent body was probably only possible in the asteroid belt.     

Rock 14318: A polymict lunar breccia with chondritic texture

Rock 14318 is a complex microbreccia consisting of lithic fragments, chondrules, glass spherules, and glass and mineral fragments that are embedded into a fine-grained, partly glassy matrix. Rock fragmenta, chondrules, and glasses are tightly welded to the matrix and partly recrystallized, indicating a relatively high-temperature agglomeration history. Few lithic fragments have igneous textures; most are miorobreccias that have suffered various degrees of recrystallization before they were embedded into rock 14318. Compositions of lithic fragments, glasses and chondrules, in terms of compositional rock and rock suite equivalents, represent members of the ANT (anorthositic-noritic-troctolite) suite; the alkalic high-alumina basalt (KREEP) group; high-alkali quartz basalt; basalt; and dunite. The polymict nature of many lithic fragments suggests that rook 14318 require at least two, and probably more, impact episodes for its formation. Final agglomeration took place while part of the material was hot, as is indicated by the welded texture, suggesting that the final impact event was a large one, producing a fiery cloud similar to a nuée ardente. The close similarity in texture of lunar rock 14318 to certain polymict-brecciated meteorites such as Siena suggests that meteorites of this type were also formed by complex and successive impact events on the surface of the meteorite parent body, rather than during agglomeration of the parent body.     

The Nilpena ureilite,an unusual polymict breccia: implications for origin

Nilpena (173 g), a new ureilite find from the Parachilna area of South Australia, is an unusual polymict breccia containing polymineralic aggregates, mineral fragments and achondritic and chondritic lithic enclaves in a dark, C-rich matrix. The polymineralic aggregates consist of equigranular-textured olivine Fa₂₀ and pigeonite En₇₅Wo₉FS₁₆, and exhibit evidence of shock in the form of undulose extinction and kink-banding. Monomineralic fragments consist of olivine Fa_19–24 (with highly forsteritic rims up to Fa₃) and pigeonite, and appear to be derived by brecciation of the polymineralic aggregates. The enclave material consists of lithic granular olivine fragments, porphyritic enstatite fragments (either enstatite chondrite or aubrite), olivine-clinobronzite fragments resembling an H3 chondrite, and eucritelike lithic fragments composed of plagioclase An₉₈, salitic clinopyroxene Wo_48.5En_31.4Fs_20.1 and olivine Fa_49–53. The matrix contains kamacite (generally rich in P), schreibersite and troilite. The texture of Nilpena suggests formation by disruption of a olivine-pigeonite granular aggregate while the presence of the diverse chondritic and achondritic enclave material suggests an origin as a surface or near-surface breccia.Like other ureilites Nilpena is strongly differentiated with respect to cosmic abundances but is significantly enriched in Ba and LREE. A lack of correlation of lithophile elements with $\text{Fe}\text{(Fe + Mg)}$ ratio among ureilites suggests that the differentiation was not caused by varying degrees of partial melting of a homogeneous source. A cumulate origin therefore seems more plausible.     

Lunar rock-rain: Diverse silicate impact-vapor condensates in an Apollo-14 regolith breccia

Apollo 14 regolith breccia 14076, long known to be uniquely endowed with high-alumina, silica-poor (HASP) material of evaporation-residue origin, has been found to contain a diverse suite of complementary condensates, dubbed GASP (gas-associated spheroidal precipitates). GASP occurs in two forms: as glassy or extremely fine grained quenched-melt spheroids, mostly less than 5 μm across; and as quenched textured clasts up to 200 μm across. In two of the clasts, origin by aggregation of spheroidal GASP is confirmed by the presence of relict spheroids. GASP is distinctively depleted in the same refractory major oxides that are characteristically enriched in HASP: Al₂O₃ and CaO. Among the larger GASP spheroids, Al₂O₃ is seldom >1 wt%; among the clasts, excluding two instances of apparent contamination by Na- and K-rich substrate-derived melt, bulk Al₂O₃ averages 0.3 wt%. Depletion of Al₂O₃ and CaO is also manifested by pyroxene compositions in some clasts; e.g., in the largest clast, En₈₂Wo_0.45 with 0.07 wt% Al₂O₃. Although GASP bulk compositions are nearly pure SiO₂ + MgO + FeO, they are nonetheless highly diverse. Spheroid compositions range in mg from 7 to 84 mol%, and in FeO/SiO₂ (weight ratio) from 0.002 to 0.67. Bulk compositions and textures of many GASP spheroids suggest that liquid immiscibility occurred prior to quenching; implying that these materials were, some time after condensation, at temperatures of ∼1680 °C. Textural evidence for immiscibility includes lobate boundaries between silicic and mafic domains, and a general tendency for quenched mafic silicates to be concentrated into a few limited patches rather than evenly dispersed. The parent melt of the largest clast’s pyroxene is inferred to have formed as a partial melt within the parent aggregation of GASP matter, compositionally near the pyroxene + cristobalite + melt eutectic and thus at ∼1500 °C. A few GASP spheroids show possible signs of in-flight collision-coalescence, but aggregation of the much larger clasts probably took place in mushy puddles on the lunar surface. Little mixing took place between these GASP puddles and the related HASP, probably because GASP condensation did not commence until after an intermediate stage during which, while neither net evaporation nor net condensation took place, expansion of the vapor cloud carried the eventual GASP matter well apart from the HASP. Considering the characteristic length-scale of lunar regolith mixing, the concentration of both GASP and HASP into this single unique regolith sample (14076) is most consistent with a parent crater size (diameter) of 10-100 km. I speculate that the 14076 regolith may have been unusually situated, almost directly uprange from an unusually oblique large impact. Mercurian analogs of the 14076 impact condensates may have significant implications for remote sensing.     

The Almahata Sitta polymict breccia and the late accretion of asteroid 2008 TC3

On October 7, 2008, a small asteroid named 2008 TC₃ was detected in space about 19 h prior to its impact on Earth. Numerous world-wide observations of the object while still in space allowed a very precise determination of its impact area: the Nubian Desert of northern Sudan, Africa. The asteroid had a pre-atmospheric diameter of ∼4 m; its weight is reported with values between ∼8 and 83 t, and the bulk density with ∼2–3 g/cm³, translating into a bulk porosity in the range of ∼20–50%. Several dedicated field campaigns in the predicted strewn field resulted in the recovery of more than 700 (monolithological) meteorite fragments with a total weight of ∼10.5 kg. These meteorites were collectively named “Almahata Sitta”, after the nearby train station 6, and initially classified as an anomalous polymict ureilite. Further work, however, showed that Almahata Sitta is not only a ureilite but a complex polymict breccia containing chemically and texturally highly variable meteorite fragments, including different ureilites, a ureilite-related andesite, metal-sulfide assemblages related to ureilites, and various chondrite classes (enstatite, ordinary, carbonaceous, Rumuruti-like). It was shown that that chondrites and ureilites derive from one parent body, i.e., asteroid 2008 TC₃, making this object, in combination with the remotely sensed physical parameters, a loosely aggregated, rubble-pile-like object. Detailed examinations have been conducted and mineral-chemical data for 110 samples have been collected, but more work on the remaining samples is mandatory.     

The Antarctic achondrite ALHA 76005: a polymict eucrite

ALHA 76005 is a basaltic achondrite containing few. if any, orthopyroxenes. Its bulk major and trace element composition is like that of a non-cumulate eucrite, and unlike that of a howardite. It contains a variety of igneous clasts which differ in their textures, pyroxene/plagioclase ratios and pyroxene and plagioclase compositions. One clast, No. 4, was found to have the REE pattern of a cumulate eucrite and an oxygen isotopic composition different from that of the bulk meteorite. Both the chemical and oxygen isotopic composition of clast No. 4 suggest that it was derived from a source different from its host. These observations lead to the conclusion that ALHA 76005 is a polymict eucrite.     

Sampling variation of principal components

The convenience of reducing the dimension of a data matrix by principal component analysis invites substantive interpretation of the coefficients of the components. To test the consistency of component coefficients, 10 samples of approximately 25, 50, 100, and 200 items each were randomly drawn, with replacement, from a source sample consisting of 2086 subalkaline asalt analyses. From each sample principal components were calculated using 9 major oxides as variables. Although the eigenvalues are remarkably consistent, both across and within sample size groups, the coefficients of the eigenvectors are subject to considerable sample variance. It is sometimes assumed that the coefficients of the components calculated from small samples are well enough known to be used in detailed petrological interpretation. Our results indicate that the validity of this assumption should be tested in each specific research even when rather large samples are used. The testing procedure used here is suitable of a sufficiently large reservoir of sample items is available; in the absence of such a reservoir complete simulation could be used.     

Geochemistry of a chert breccia

A complex history of diagenetic interactions between a siliceous sediment, seawater and fresh water is revealed by intraformational chert breccias. Chert breccias were formed in the Campanian Mishash Formation in Israel, by “practically contemporaneous” fracturing of lithified cherty layers followed by silicification and lithification of the matrix. Pairs of fragments and matrix were compared with respect to their chemical (Ca, Sr, Na, K, Mg, Li, B, SO₄, Ba) and isotopic (δ¹⁸O, δD, δ¹¹B) composition. δ¹¹B was analyzed by ion-probe and includes a profile across a fragment-matrix contact. The epicontinental cherts of the Mishash Fm. are enriched by a factor of 10 to 50 in all elements other than O and Si in comparison with Deep-Sea cherts. All results are compatible with the proposition that the lithification of the matrix occurred in contact with fresh-water, as opposed to seawater in which the fragments, as well as most of the Mishash sediments were formed. The strongest evidence for this difference is in the higher concentration of B in the fragments (27-70 ppm vs. 11-21ppm in the matrix) and higher δ¹⁸O (29 to 35‰ vs. 21 to 33‰). δD is a less efficient discriminator, though compatible with fresher water diagenesis of the matrix: −115‰ to −76‰ for hydrogen in the chert of the fragments, compared to −141 to −85‰ for the matrix. δ¹¹B in the matrix shows some of the lowest values recorded in sediments (δ¹¹B = −33‰), but varies strongly, suggesting that the source of boron in the matrix is a mixture of a freshwater and a marine component. Both seawater and the freshwater that has equilibrated with the cherts underwent varying degrees of evaporation. Ca, Sr and SO₄ are carried by apatite, trapped as detritus in the matrix. The concentration of lithium in the matrix is high (11-16 ppm), whereas in the adjacent fragments it is mostly only within 1-2 ppm. Li probably enters the matrix from the interstitial solution, during the opal → quartz transformation. The second, prolonged, transformation takes place in a (freshwater) flow-through, open system. This allows a much larger mass of Li to be scavenged by the transforming silica despite its low concentration in freshwater.     

滇西北兰坪金顶超大型矿床研究新进展:侵位角砾岩的发现及其地质意义

兰坪金顶超大刚型床各种角砾岩和角砾岩型矿体十分发育，通过对角砾岩型矿体形态、产状、与围岩接触关系和角砾岩自身结构特点的研究，作者首次发现并提出灰岩角砾岩型矿体是一种侵位角砾岩。其形成机制类似于现代泥火山。     

A case study on geochemical anomaly identification through principal components analysis supplementary projection

Based on a case study in which a single geochemical anomaly was located in the vicinity of an abandoned mine in Central Portugal, a recursive methodology for anomaly/background separation was developed. This methodology relies on the supplementary projection of each of the samples taken from a subset of ‘anomaly candidates’ onto the axes provided by Principal Components Analysis of the background subset. The concept of ‘anomaly intensity’, defined by the average of the distances from the original to the supplementary projections, is the basis for final anomaly identification.     

A mineralogical and geochemical study of polymict eucrite discovered in Sahara of southwest Algeria

NWA2268 is a polymict eucrite discovered in the Sahara, at southwest Algeria, close to the region of Tindouf. This meteorite weighs 65 g and presents a thin black fusion crust. The rock is fine- to medium-grained breccia and contains mineral fragments of plagioclases, pyroxenes, spinel, olivine and silica. The rock contains some basaltic fragments with sub-ophitic or cumulative textures, constituted by plagioclases and exsolved pigeonite. Pyroxferroite grains are present and locally destabilised in an association of hedenbergite, fayalite and silica. It also presents unequilibrated eucritic clast with heterogeneous pyroxenes and plagioclases compositions. Pyroxenes in the all of the other clasts have equilibrated composition, with exolved pigeonites with augite lamellaes. This polymict eucrite contains also partially devitrified glass that represents impact melts linked to impact event. None recrystallization of this glass confirms a lack of post-brecciation metamorphism. Diogenitic fragments are less abundant than 10 %. The oxygen isotopic composition of NWA2268 is Δ¹⁷O (?0.43). This meteorite is interpreted as belonging to the HED group attributed to the 4-Vesta asteroid.     

Objective comparison of mass fragmentograms by principal components analysis: method and results

The multivariate statistical method of Principal Components Analysis is used to classify gas chromatographic-mass spectrometric data. The specific examples comprise sterane and triterpane regions of GC-MS analyses of branched/cyclic fractions. The statistical model provides an objective analogue to visual comparison and classification of mass fragmentograms. Sources of experimental error influencing the statistical results include insufficient sample size, short integration times, and peak skewing. The method successfully groups samples of oils, oil sand, and polluted beach sand according to geographic origin: beach sand groups with type of crude spilled; laboratory biodegraded and untreated Nigerian crudes group together. Applications of three-mode Principal Components Analysis can range from study of geologic processes acting on organic compounds to classification of unknown pollutants.     

An effect of closure on the structure of principal components

The principal components transformation generates, from any data array, a new set of variables—the scores of the components—characterized by a total variance exactly equal to that of the initial set. It is in this sense that the transformed variables are said to contain, preserve, or account for, the variance of the original set. The scores, however, are uncorrelated. In the course of the transformation, what becomes of the strong interdependence of variance and covariance so characteristic of closed arrays? The question seems to have attracted little attention; we are aware of no study of it in the earth sciences. Experimental work reported here shows quite clearly that the overall equivalence of variance and covariance imposed by closure, though absent from the component scores,may emerge in relations between the coefficientsof each of the lower-order components; if the raw data are complete rock analyses, the sum of all the covariances of the coefficients of such a component is negative, and is very nearly equal to the sum of all the variances in absolute value. (In all cases so far examined, the absolute value of the first sum is a little less than that of the second.) The principal components transformation provides an elegant escape from closure correlation if a petrographic problem can be restated entirely in terms of component scores, but not if a physical interpretation of the component vectors is required.     

Spatial orthogonality of the principal components computed from coregionalized variables

Within the frame of the linear model of coregionalization, this paper sets up equations relating the variogram matrix of the principal components extracted from the variance-covariance matrix to the diagonal variogram matrices of the regionalized factors. The spatial orthogonality of the principal components is investigated in three situations: the intrinsic correlation, two basic structures with independent nugget components, three basic structures with independent nugget components and uncorrelated subsets of variables. Two examples point out that the correlation between the principal components may be nonnegligible at short distances, especially if the correlation structure changes according to the spatial scale considered. For one of the two case studies, an orthogonal varimax rotation of the first principal components is found to greatly reduce the spatial correlation between some of them.     

基于微结构参数主成分的黄土湿陷性评价

黄土的湿陷性与其微观结构特征密切相关,它的微结构又受其应力状态和所处的含水状态影响。通过改变含水率与固结压力,对西安原状黄土进行了湿陷性试验,由此分析了不同含水率与固结压力条件下湿陷性的差异与联系,同时通过电镜扫描（SEM）获取了湿陷前、后黄土试样的微结构照片,进而获取了相应条件下的SEM照片的简单微结构参数。分析了湿陷前、后微结构参数的变化,探讨了简单微结构参数间相关关系,基于主成分分析法构建了合成微结构参数。研究表明：随着固结压力的增大,颗粒体所占比重越来越大,第1主成分近似线性增大,黄土湿陷系数与其累积主成分呈线性关系。根据这一重要认识,建立了主成分得分的湿陷系数计算方法,进而建立了黄土湿陷性评价方法。该研究对定量研究黄土湿陷性的微结构效应做了有益的探索。     

Lunar sample 14425: Not a lunar tektite

Energy-dispersive x-ray analysis of a polished section of lunar sample 14425 shows, in contradiction to a previous report, that it has a composition similar to Apollo 14 breccias, but not to high-magnesium microtektites. The glass is homogeneous, but the bead contains numerous metallic spherules up to 0.7 mm in diameter. The metal in the spherules is iron with up to 16 wt.% Ni and 9 wt.% P and small amounts of S and Si. The high phosphorus content indicates the presence of a fine-grained phosphide phase in the metal. All of the metallic spherules have an associated sulphide phase. The composition of the glass bead and the presence of numerous Ni-Fe spherules with an associated sulphide phase indicates that the bead was formed by impact melting of surficial deposits at the Apollo 14 site.     

Correlation,principal components,and the problem of multistate data

Problems of using discrete data in correlation and components analysis are discussed, and some guidelines are suggested.