bluuebunny/crossref_metadata_2025 huggingface dataset:
FRAGMENTATION OF THE SIKHOTE‐ALIN METEORITIC BODY
Authors: Krinov E. L.
Published: June 2012

Based on the results of the study of regmaglyptic relief of individual specimens of the Sighote‐Alin iron meteorite shower, three main stages of fragmentation have been established for a meteoritic body moving through the atmosphere with cosmic velocity. During the first stage, the fragmentation took place at a relatively high cosmic velocity, the fragments being subjected to a major aerodynamic influence. In the second stage, the velocity had decreased due to atmospheric resistance and the fragments were subjected to less drastic aerodynamic action in the regmaglyptic formation. During the third stage, fragments were further fragmented when their cosmic velocities had been almost completely absorbed and the new fracture surfaces were practically untouched by atmospheric influence. As a result of such a multistage fragmentation, the main scatter‐ellipse was over‐lapped by two secondary ellipses, thereby complicating the patterns of scattering of individual specimens of the meteorite shower, which turns out to contain a number of anomalies.
THE CANYONLANDS METEORITE
Authors: Lange David E. , Frost Kent , Sipiera Paul P. , Moore Carleton B.
Published: June 2012

The Canyonlands meteorite weighing 1,520 grams was found near the confluence of the Green and Colorado Rivers, Utah, near lat 38°11′N.; long 109°53′W. It is a shocked, brecciated H6 chondrite containing large black veins which do not differ in composition from the main chondritic mass. A black fusion crust remains on part of the meteorite.
MAGNETITE SPHERULES IN MIOCENE VERSUS RECENT SANDS OF NEW JERSEY
Authors: Puffer John H.
Published: June 2012

Spherules composed of magnetite were found throughout the state of New Jersey. Samples of coastal plain sands of Miocene age, beach sands, street sweepings, wind‐blown dust, river waters, and dust from the stack scrubber of a scrap iron foundry were carefully examined. Spherules were found in each of the samples representing recent environments and in ancient sediments sampled near the surface, but are absent from each of the wide variety of ancient sediments carefully sampled below about one meter. The spherule samples consistently contain 0.4–0.8 weight percent Mn but contain less than 0.1 weight percent Ni. It is concluded that virtually none of the spherules is of an extraterrestrial origin.
MAGNETISM IN METEORITES
Authors: Herndon J. M. , Rowe M. W.
Published: June 2012

We present here a somewhat simplified overview of the subject of magnetism in meteorites. A glossary of magnetism terminology is included, followed by discussion of the various techniques used for magnetism studies in meteorites. The generalized results from use of these techniques by workers in the field is described. A brief critical analysis is offered.
THE ELLA ISLAND, GREENLAND, CHONDRITE
Authors: Carman J. H. , McCormick G. R.
Published: June 2012

The Ella Island, Greenland, meteorite was found in August of 1971. Electron microprobe study of the meteorite revealed it to contain olivine, low‐calcium pyroxene, high‐calcium pyroxene, plagioclase, kamacite, taenite, chromian‐hercynite and troilite. On the basis of fayalite and ferrosilite content, poorly‐defined chondrules, absence of glass in chondrules, presence of well‐developed feldspar in the matrix and chondrules, and degree of recrystallization of the matrix, the Ella Island meteorite is classified as an L‐6 chondrite.
THE IJOPEGA CHONDRITE: A NEW H6 FALL
Authors: Jaques A.L. , Lowenstein P.L. , Green D.H. , Kiss E. , Nance W.B. , Taylor S.R. , Ware N.G.
Published: June 2012

The Ijopega (Papua New Guinea) meteorite is a new H6 group chondrite fall which contains olivine (Fa 19.9 mole %), bronzite (Fs 17.8 mole %), plagioclase (An 12.1 Or 6.3 Ab 81.6 mole %), diopside, kamacite, taenite, troilite, chromite and whitlockite. The meteorite is extensively recrystallized and brecciated, and shows evidence of moderate shock deformation. Examination of Fe2+ and Mg partitioning between ortho‐ and clinopyroxene indicates a high equilibration temperature (940° or 880 °C). Chemical analysis shows the meteorite to be rich in S, containing about twice the average H‐group abundance. Trace elements, including REE, are in accord with established H‐group chondrite abundances.
THERMAL DEFORMATION AND FRACTURING IN OLIVINE‐RICH SAMPLES
Authors: Levi F. A.
Published: June 2012

A study was made of the effect of low‐temperature thermal fatigue on the generation of regular and irregular fractures in olivine‐rich terrestrial rocks. The results appear to confirm the influence of thermal actions in the metamorphism of stony meteorites and lunar rocks.
A PETROGRAPHIC AND MINERAL CHEMISTRY STUDY OF THE WESTON, CONNECTICUT, CHONDRITE
Authors: Noonan Albert F. , Nelen Joseph A.
Published: June 2012

The Weston meteorite is a breccia containing mostly light‐colored equilibrated chondritic xenoliths and less abundant highly un‐equilibrated chondritic inclusions fixed in a dark grey host of chondrules, mineral and rock fragments. Many of the inclusions show evidence of shock. Unlike most xenolithic chondrites, the Weston host contains a large fraction of considerably more equilibrated silicates than is found in the unequilibrated inclusions, suggesting either that most host silicates retain the mineral chemistry of an equilibrated source indigenous to Weston, or represent a unique fraction which equilibrated separately, prior to final agglomeration. The host silicates are similar in composition to minerals in the common xenoliths, supporting the former possibility that host chondrules and mineral fragments are derived from the xenolithic material, probably by impact fragmentation and melting. Also mixed with Weston is a small but distinct carbonaceous component including the minerals fassaite, Fespinel, forsterite, magnetite and Ca‐Al‐rich inclusion which are normally associated with carbonaceous chondrites.
RARE GASES IN BANSUR, UDAIPUR AND MADHIPURA CHONDRITES
Authors: Gopalan K. , Rao M.N.
Published: June 2012

We have analysed three Indian meteorites — Bansur, Udaipur and Madhipura — for the elemental and isotopic composition of Ne, Ar, Kr and Xe and determined their radiation and gas‐retention ages. It is found that Udaipur belongs to the group of unequilibrated ordinary chondrites and Madhipura probably belongs to the group of shocked hypersthene chondrites.
THREE SYNTHETIC LUNAR GLASSES*
Authors: Minkin J.A. , Chao E.C.T. , Christian R.P. , Harris E.E. , Norton D.R.
Published: June 2012

Glasses have been synthesized that have the approximate compositions of lunar rocks 61156, 68415, and 77135, respectively. The glasses have been analyzed by conventional analytical and electron microprobe techniques and have been found to be highly homogeneous. They have been used successfully as electron microprobe standards and for experimental studies of crystallization and solar‐wind implantation. Small amounts of these materials can be provided to investigators who would find them useful.
THE COMPOSITION OF THE CHASSIGNY METEORITE
Authors: Mason Brian , Nelon J.A. , Muir P. , Taylor S.R
Published: June 2012

Spark source mass spectrometric analysis of the Chassigny meteorite has given the following data (in ppm): Rb 0.4, Sr 7.2, Y 0.64, Zr 1.5, Nb 0.32, Ba 7.1, La 0.39, Ce 1.12, Pr 0.13, Nd 0.54, Sm 0.11, Eu 0.038, Gd 0.11, Tb 0.02, Dy 0.12, Ho 0.03, Er 0.09, Yb 0.10, Pb 1.0, Th 0.057, U 0.021. These data, in conjunction with major element composition and mineralogical and textural features, indicate that this meteorite is an olivinerich cumulate, possibly genetically related to the nakhlites.
BRAZILIAN METEORITES: THE MAFRA, SANTA CATARINA STATE, CHONDRITE
Authors: Levi‐Donati G. R. , Shima Masako , Sighinolfi G. P.
Published: June 2012

A chemical analysis and a mineralogical inspection have been performed on about 50 g of the Mafra, Santa Catarina State, Brazil, meteorite. The stone is an H‐4 chondrite. It shows some ambiguous characteristics concerning the iron distribution, which are discussed.
AN EXAMPLE OF A THERMALLY METAMORPHOSED AGGLUTINATE
Authors: Basu Abhijit
Published: June 2012

A single fragment from an Apollo 16 soil appears to be a soil agglutinate that has experienced thermal metamorphism. Its texture is similar to that observed in many of the samples of recrystallized polymict breccias collected in the lunar highlands. Debris blankets, consisting largely of mineral and lithic clasts and derived from highland bedrock by major impacts, are less likely than agglutinate‐rich soil from the highland megaregolith to be the progenitor of this class of recrystallized rocks.
EXPERIMENTS ON THE STABILITY OF FeOOH ON THE SURFACE OF THE MOON
Authors: Taylor Lawrence A. , Burton Jacqueline C.
Published: June 2012

The FeOOH phase in Apollo 16 rocks is akaganéite. Other polymorphs of FeOOH, i.e. geothite and lepidocrocite, may exist but have not been identified by X‐ray diffraction. Experiments performed during this study using akaganéite, geothite, and lepidocrocite placed at 135°C and under a pumping vacuum of 10−2 torr, demonstrate that these forms of FeOOH are not stable on the surface of the Moon, where daytime temperatures are about 140°C and pressures are about 10−7 torr. The effect of the vacuum is to strip off the water, and the temperature speeds up this dehydration process. These data lend support to the contention of Taylor et al. (1973) that the FeOOH in lunar rocks formed by the oxyhydration of lawrencite, FeCl2, due to contamination by terrestrial water vapor.
THE DEL RIO ATAXITE, TEXAS
Authors: Henderson Edward P. , King Elbert A.
Published: June 2012

Del Rio is a new ataxite from Texas that is not related to either Monahans or Nordheim, the only previously known ataxites from Texas. Del Rio has a nickel content of approximately 12.9 weight percent, apparently has been shocked prior to its fall, and contains minor inclusions of daubreelite, schreibersite and troilite.
PETROGRAPHY AND CHEMISTRY OF THE FAUCETT METEORITE, BUCHANAN COUNTY, MISSOURI
Authors: King Elbert A. , Jarosewich Eugene , Brookins Douglas G.
Published: June 2012

Nine, possibly ten, stones from northwestern Missouri are known as the Faucett meteorite. These stones are finds, but may be fragments of a large fireball seen in the area in 1907. The meteorite is an olivine‐bronzite chondrite (H4) containing approximately 31% chondrules and 69% matrix. Modal analysis gives: olivine 43%, orthopyroxene 28.3%, oligoclase 5.9%, glass 1.2%, metallic grains (both nickel‐iron and troilite) 19.7%, other minerals and unidentified grains 2.0%. The chemical analysis is typical of modern analyses of H‐group chondrites with a total iron value of 26.59 weight percent.
SKETCHES IN THE HISTORY OF METEORITICS 2: THE EARLY CHEMICAL AND MINERALOGICAL WORK
Authors: Sears D.W , Sears H.
Published: June 2012

The chemical and mineralogical work on meteorites over the period 1800 to 1840 is reviewed. The number of elements known to be present in meteorites rose from six to 19. Chemical techniques advanced rapidly so that by 1815 the procedure was essentially that of modern wet chemical analysts: removal of the magnetic material, dissolution of the acid‐soluble portion and fusion of the remainder with alkali. After Bournon's work in 1802 much mineralogical progress was made during the 1820's, notably by G. Rose. Berzelius made important contributions by his own analyses and synthesis of the work of others. By 1840 ordinary chondrites, carbonaceous chondrites, plagioclase‐pyroxene achondrites, Chassigny, pallasites and octahedrites could all be distinguished
THE KRAMER CREEK, COLORADO METEORITE: A NEW L4 CHONDRITE
Authors: Gibson Everett K. , Lange David E. , Keil Klaus , Schmidt Terry E. , Rhodes J. Michael
Published: June 2012

The Kramer Creek, Colorado, chondrite was found in 1966 and identified as a meteorite in 1972. Bulk chemical analysis, particularly the total iron content (20.36%) and the ratio of Fetotal/SiO2 (0.52), as well as the compositions of olivine (Fa21.7) and orthopyroxene (Fs18.3) place the meteorite into the L‐group of chondrites. The well‐defined chondritic texture of the meteorite, the presence of igneous glass in the chondrules and of low‐Ca clinopyroxene, as well as the slight variations in FeO contents of olivine (2.4% MD) and orthopyroxene (5.6% MD) indicate that the chondrite belongs to the type 4 petrologic class.
LITHIC CLASTS IN THE SUPUHEE CHONDRITE
Authors: Leitch Catherine A. , Grossman Lawrence
Published: June 2012

Supuhee is a shocked and brecciated H6 chondrite containing foreign lithic clasts. Three such clasts were analysed with the electron microprobe in an attempt to locate “mysterite,” a volatile‐rich material postulated to be present in Supuhee. Clast 1 bears chemical and mineralogical similarities to C1 and C2 chondrites, but its total volatile content, <9.4%, is lower than that of either of these types. The composition of Clast 2 suggests its derivation from H‐group chondrite material via loss of metal and sulfide. The third clast is apparently a unique meteorite type bearing compositional similarities to both ordinary and enstatite chondrites. The occurrence of these clasts in a highly recrystallized host is evidence for their incorporation after metamorphism. The presence of Clast 1, coupled with this time sequence, indicates that conditions were favorable for the formation, incorporation and preservation of volatile‐rich materials such as mysterite
NOBLE GASES IN THE UNIQUE CHONDRITE, KAKANGARI
Authors: Srinivasan B. , Anders Edward
Published: June 2012

The Kakangari chondrite has a cosmic‐ray exposure age of 5.4 m.y. and a K‐Ar age near 4 g.y. Its high cosmogenic 3He/21Ne ratio of 7.5 indicates a small preatmospheric mass. The He and Ne are largely of solar‐wind origin, presumably implanted during exposure in the regolith of its parent body. The heavy gases Ar, Kr, Xe are largely of planetary origin. Taken together, the low 129Xe/132Xe (1.07), low 36Ar/132Xe (225), and high 132Xe content (45 × 10−10 cc STP/g) are more similar to the values for unequilibrated ordinary chondrites or even C1, C2 chondrites than to enstatite chondrites, and suggest that Kakangari has the same gas‐bearing mineral assemblage as the former, in spite of its high degree of reduction (Fa4.9).
FOUR NEW IRON METEORITE FINDS
Authors: Scott Edward R.D. , Wasson John T. , Bild Richard W.
Published: June 2012

Four new irons are described; Buenaventura (IIIB) from Chihuahua, Mexico: mass 114 kg; Denver City (anomalous) from Texas, USA: mass 26.1 kg; Kinsella (IIIB) from Alberta, Canada: mass 3.7 kg; and Tacoma (IA) from Washington, USA: mass 17 g. Denver City is unique, i.e., not related to any other known iron. Tacoma is the smallest iron meteorite recorded. All were purchased for the UCLA collection following a publicity drive for new meteorites
ALUMINUM‐26 AS A PLANETOID HEAT SOURCE IN THE EARLY SOLAR SYSTEM
Authors: Herndon J.M. , Herndon M.A.
Published: June 2012

The results of thermal model calculations which assume 26Al as a heat source are presented. The relation between 26Al content, the maximum central temperature obtained, and the time interval after formation until central cooling commences is elucidated. Because of the heating times required, these results constrain maximum permissible planetoid dimensions more severely than do previous calculations which assume a high initial temperature.
CHEMICAL ALTERATIONS OF THE HOLBROOK CHONDRITE RESULTING FROM TERRESTRIAL WEATHERING
Authors: Gibson Everett K. , Bogard Donald D.
Published: June 2012

The effects of chemical weathering on the Holbrook, Arizona chondrite were studied via major, minor, and trace element analysis along with noble gas measurements. Three samples of Holbrook were studied: a fresh specimen which fell in 1912, a specimen collected in 1931 and a specimen collected in 1968. The weathering of the meteorite produced changes in the Fe and Mg concentrations. The amount of metallic iron decreases with increasing degree of weathering. The MgO content decreases and the total iron content increases slightly with increasing weathering of the specimen, but these concentration differences are not necessarily due to weathering. Elemental concentrations for Ti, Ca, Al, P, Mn, Ni and Cr did not change significantly during weathering. Sodium may have been lost during weathering, whereas K showed a slight enrichment in abundance with terrestrial age. Trace elements C, Rb and Sr increased at least two‐fold during weathering of the meteorite. Abundances of the radiogenic and cosmogenic noble gases decreased with increasing terrestrial age. Concentration ratios of certain cosmogenic noble gas nuclides which are commonly used as indicators of gas loss and shielding in chondrites show unpredictable behavior in the weathered chondrite.
ESTIMATION DE LA POROSITE DE QUELQUES CHONDRITES PAR ANALYSE D'IMAGES DE LEURS SECTIONS POLIES
Authors: Michel‐Lévy M. Christophe
Published: June 2012

An eventual correlation between petrologic type and porosity can only be found if measurements are made on unshocked or slightly shocked chondrites. The main advantage of the method (described earlier in this journal) is that it offers the possibility of correlating on a very small scale porosity with structural and petrographical features along with punctual chemical and isotopic data. Moreover, the method is relatively unpolluting and non destructive, and requires very small amounts of matter. Porosity measurements have been carried out on polished thin section of five H chondrites, after sample impregnation with a fluorescent resin. The microscope images were analysed with a Quantimet. Two types of information have been derived. First, the macroporosity of the material ranges up to 13% in Sena (H5) but falls to 4% in samples that have undergone slight shock or compression. Second, approximately 25% by volume of the stones consist of zones of great permeability which were fissured or filled with loose debris. This has been observed in all cases but the well‐recrystallised Kernouve (H6) stone. Additional measurements are required to correlate petrology and porosity on a statistically significant basis.
GRAIN SIZE AND PETROGRAPHY OF C2 AND C3 CARBONACEOUS CHONDRITES
Authors: King Trude V.V. , King Elbert A.
Published: June 2012

Grain size frequency distributions of the ≥ 0.1 mm size fractions have been measured for 19 C2 and C3 carbonaceous chondrites (7 CM2, 5 CO3, 6 CV3 and 1 CV2). The grain size frequency distribution curves and summary statistics are remarkably similar for the CM2 and CO3 meteorites, with ranges of median grain size from 2.36φ to 2.67φ and graphic mean grain size from 2.20φ to 2.59φ. The CV3 specimens are distinctly coarser than the CM2 and CO3 meteorites and have a wider range of grain size summary statistics. The grain size frequency data for fluid drop chondrules and for lithic chondrules show approximately the same size frequency characteristics as the more abundant particles in each of the petrologic subgroups. If the chondrules and other particles were produced by different mechanisms or in different environments, an extremely effective size sorting process is required to produce the observed grain size frequency distributions. Alternatively, most of the particles and the observed grain size frequency distributions might have been produced by small impacts into an immature, accretionary regolith. The strong similarity between the grain sizes of the CM2 and CO3 meteorites, together with previously recognized chemical similarities, suggest a genetic relationship between the two petrologic subgroups. The grain size frequency distributions of chondrules and other particles in CM2 and CO3 meteorites are different from those found previously in ordinary chondrites
INFRARED (JHK) PHOTOMETRY OF METEORITES AND ASTEROIDS
Authors: Leake Martha , Gradie Jonathan , Morrison David
Published: June 2012

We present JHK colors observed for ten asteroids and synthesized JHK colors for seven meteorite groups, samples of iron and nickel metal, pyroxene, olivine, feldspar, a lunar anorthite and some terrestrial mineral samples. Pronounced differences are apparent between the chondritic and achondritic meteorite classes; the chondritic classes show less subdued trends in J‐H color which reflect their metamorphic grade

We find small but significant differences between the JHK colors of the predominant C and S classes of asteroids. All JHK colors of asteroids observed here fall within the limited domain defined by the various chondritic and iron‐rich meteorites but are strikingly different from those of most achondritic meteorites
VEIN FORMATION IN THE C1 CARBONACEOUS CHONDRITES
Authors: Richardson Steven M.
Published: June 2012

Veins in the C1 chondrites Orgueil, Alais, and Ivuna have been deposited during an extended period of impact brecciation and leaching. At least three generations of mineralization, dominated successively by carbonates, calcium sulfate, and magnesium sulfate, can be recognized. Vein minerals are derived locally by closed‐system reactions between matrix phyllosilicates and an aqueous fluid, with the result that few, if any, primitive mineral phases still exist in the C1s
SIX METEORITES FROM KANSAS: PETROGRAPHIC OBSERVATIONS AND RARE GASES
Authors: King Elbert A. , Herzog G.F.
Published: June 2012

Electron microprobe analyses and petrographic observations demonstrate that Almelo Township (L6), Beeler (LL6), Kalvesta (H4), Phillips County (L6), and Yocemento (L5) are typical ordinary chondrites. Selden has abnormally iron‐rich silicates and nickel‐rich metal, and it may have been a lower petrologic type that has been shocked to an LL5. Shielding corrected exposure ages range from 0.80 m.y. (Kalvesta) to 47.0 m.y. (Yocemento).
A CHEMICAL STUDY OF THE IMPACT GLASSES AND BASAL TS FROM LONAR CRATER, INDIA
Authors: Stroube W.B. , Garg A.N. , Ali M.Z. , Ehmann W.D.
Published: June 2012

Twenty‐nine elements have been determined by INAA in two impact glasses and four basalts from Lonar Crater, India. The glasses are remarkably similar to the underlying core basalt samples in major, minor and trace element abundances. This suggests that impact‐induced chemical fractionation during formation of the glasses from basalt is minimal for many of the principal rock and mineral‐forming elements. It should be recognized that many of the most volatile trace elements were not determined in this study. Differences in the volatile trace element contents of the glasses and basalts due to either impact‐induced fractionation, or incorporation of material from a volatile‐rich impacting body, can not yet be excluded.
XENON, OSMIUM, AND LEAD FORMED IN O‐SHELLS AND C‐SHELLS OF MASSIVE STARS
Authors: Heymann Dieter , Dziczkaniec Marlene
Published: June 2012

In this paper we show that the explosive products from O‐shells of massive stars which contain 124Xe with large overproduction factors do not contain any of the naturally occurring isotopes of Os and Pb. We show further that the explosive products from C‐shells (explosive carbon burning) do contain Os and Pb along with Xe which is strongly enriched in r‐Xe of anomalous isotopic composition. The composition of Os in this matter is probably s‐like rather than r‐like. Pb in this matter is enriched in 208Pb. The results and arguments of this paper have implications for studies of isotopic compositions of Xe, Os, and Pb in residues of the Allende and other carbonaceous chondrites.
A PROCESS OF STELLAR NUCLEOSYNTHESIS WHICH MIMICKS MASS FRACTIONATION IN P‐XENON
Authors: Heymann Dieter , Dziczkaniec Marlene
Published: June 2012

The combination of the O‐shell theory of Heymann and Dziczkaniec and the supernova theory of Woosley and Howard clearly identifies the astrophysical sites for the formation of the anomalous light Xe component in carbonaceous chondrites. These sites are the O‐ and Ne‐shells, and possibly C‐shell of a massive star. Most of the 124Xe and 126Xe are formed in the O‐shell during hydrostatic core silicon‐burning, when a seed of heavy nuclei is exposed to an effective temperature near T9 = 2.0. 128Xe is formed via 128Ba in the O‐shell, but the amounts appear too small to satisfy the deduced 128Xe/124Xe and 128Xe/126Xe yield ratios from the chondrites. However, substantial amounts of 128Xe can be formed in the adjacent Ne‐ and C‐shells during the explosion. The formation of 128Ba in the O‐shell would increase if the (γ, α) photodisintegration rate in 128Ba is actually smaller than calculated by Woosley and Howard. Lewis et al. have proposed that the anomalous light Xe component is mass‐fractionated normal Xe. It is in this sense that the process of stellar nucleosynthesis of the present paper mimicks mass‐fractionation.
CHEMICAL COMPOSITION AND CLASSIFICATION OF 19 YAMATO METEORITES
Authors: Jochum K.P. , Grais K.I. , Hintenberger H.
Published: June 2012

The elements Na, Mg, Al, Si, S, K, Ca, (V), Cr, Mn, Fe, Co and Ni have been determined in 19 Yamato meteorites by spark source mass spectrometry. For comparison the chondrites Allan Hills 7603, Mt Baldr (b) and Holbrook and the achondrites Johnstown, Pasamonte and Stannern also have been analyzed by the same method. By virtue of their chemical composition the Yamato meteorites 74002 and 74144 prove to be ordinary chondrites of type L; 74001, 74103, 74155 and 74156 are ordinary chondrites of type H; 74662 is a carbonaceous chondrite; Yamato 74010, 74011, 74016, 74037, 74097, 74125 and 74136 are diogenites; Yamato 7308(1) is a howardite; and Yamato 74450 is a eucrite. This agrees with earlier classifications based on petrological and mineralogical arguments (Nagata, 1978; Motylewski, 1978). For the chondrites Yamato 74002, 74106, 74144 and the diogenite 74125, however, no previous classifications could be found in the literature.

In a Mg‐Al diagram the eucrites, the howardites, the diogenites and the ureilites fall into characteristic fields. This enabled not only the classification of the Yamato achondrites investigated in this paper but also confirmed the previous identification of Yamato 74123 as a ureilite (Hintenberger et al., 1978).

A very high chromium content is characteristic of some Yamato diogenites, especially Yamato 74037 (3.4%). Chromium and vanadium are positively correlated in the achondrites investigated.
NEW LIGHT ON THE ORIGIN OF THE HOLY BLACK STONE OF THE KA'BA
Authors: Thomsen Elsebeth
Published: June 2012

At various times the Black Stone of the Ka'ba has been considered to be lava, basalt, a meteorite and lately an agate. This paper discusses the possibility that it may consist of impactite glass, derived from the meteoritic craters of Al‐Hadidah, called Wabar.
DEFORMATION MECHANISMS IN MILDLY SHOCKED CHONDRITIC DIOPSIDE
Authors: Ashworth J.R.
Published: June 2012

In several ordinary chondrites showing slight shock deformation, the shock effects in diopsidic pyroxene have been characterized, using transmission electron microscopy. Narrow twin lamellae, and slip planes, in (100) orientation are abundant. These are comparable with the effects of experimental deformation at low strain‐rates. The absence of (001) twinning indicates different conditions from those in shock experiments and in many natural shock events. Predominance of the (100) features is thought to indicate a particularly mild type of shock, in which the stresses generated within a crystal are low.
IMPACT AND IMPACT‐LIKE STRUCTURES IN ALGERIA PART I FOUR BOWL‐SHAPED DEPRESSIONS
Authors: Lambert Philippe , McHone John F. , Dietz Robert S. , Houfani Messaoud
Published: June 2012

From orbital, aviation and geologic documents, four circular depressions on the Sahara sedimentary platform were selected for field investigation because of their possible impact origin. Our results can be summarized as follows: Amguid Crater (26° 05′N; 004° 23.5′E; 450 m diameter, 30 m deep) is perfectly circular, with a steep wall, a raised rim and an ejecta blanket. The strata are uplifted, outward dipping, dislocated and locally overturned at the rim crest. Large blocks are scattered around the rim. There is petrological evidence of shock by planar elements in quartz. Amguid is a well preserved impact crater probably no older than 100,000 years. Talemzane (33° 19′N; 004° 02′E; 1.7 km diameter, 70 m deep) is also perfectly circular and displays a raised rim. The strata are uplifted, outward dipping, and locally highly fractured. Numerous breccia veins are clearly exposed in the crater wall. Consolidated ejected debris form a continuous blanket more than 500 m outward from the rim. Reworked mixed breccias are exposed at the base of the crater wall. Planar elements are observed in quartz clasts in the mixed breccia. Talemzane is an impact crater on the order of 0.5 to 3 million years old. El Mouilah (33° 51′N; 002° 03′E; 4.5 km diameter, 130 m deep) is almost perfectly circular, the walls are steep and there is a central dome. In spite of a promising morphology, there is no field evidence of impact. El Mouilah is possibly a recent collapse structure due to dissolution in the thick underlying limestone and gypsum formations or purely erosional in origin. Aflou (34° 00′N; 002° 03′E) is not circular (3 × 5 km) but was selected because it appears in the literature as a probable impact crater, the main argument being the existence of fused materials in the center (Marks et al., 1972). We found no evidence of impact, but several occurrences of igneous rocks along an E‐W direction suggest a structurally controlled volcanic activity. A volcanic activity is also supported by the existence of a local magnetic anomaly centered on the depression. Aflou is neither an impact structure nor a crater. Located on a probable structural dome, at the intersection of several structural trends, the formation of the depression can be due to erosion and/or dissolution in the thick underlying limestone and gypsum formations.
PAPUANITES: PSEUDO‐TEKTITES FROM NEW GUINEA
Authors: Visker Derk A. , Ehmann W.D. , Young R.C.
Published: June 2012

Spherical translucent green glasses found in New Guinea for many years have the external appearance of stream abraded tektites, but are chemically distinct from known tektite groups. Their chemical composition is most similar to artificial glasses. If these objects are the source of reports of tektites occurring in New Guinea, the existence of New Guinea tektites must now be discounted.
RELATIVE ABUNDANCES OF CHONDRULE PRIMARY TEXTURAL TYPES IN ORDINARY CHONDRITES AND THEIR BEARING ON CONDITIONS OF CHONDRULE FORMATION
Authors: Gooding James L. , Keil Klaus
Published: June 2012

A petrographic survey of > 1600 chondrules in thin‐sections of 12 different mildly to highly unequilibrated H‐, L‐, and LL‐chondrites, as well as morphological and textural study of 141 whole chondrules separated from 11 of the same chondrites, was used to determine the relative abundances of definable chondrule primary textural types. Percentage abundances of various chondrule types are remarkably similar in all chondrites studied and are ∼ 47–52 porphyritic olivine‐pyroxene (POP), 15–27 porphyritic olivine (PO), 9–11 porphyritic pyroxene (PP), 3–4 barred olivine (BO), 7–9 radial pyroxene (RP), 2–5 granular olivine‐pyroxene (GOP), 3–5 cryptocrystalline (C), and ≤ 1 metallic (M). Neither chondrule size nor shape is strongly correlated with textural type. Compound and cratered chondrules, which are interpreted as products of collisions between plastic chondrules, comprise ∼ 2–28% of nonporphyritic (RP, GOP, C) but only ∼ 2–9% of porphyritic (POP, PO, PP, BO) chondrules, leading to a model‐dependent implication that nonporphyritic chondrules evolved at number densities (chondrules per unit volume of space) which were 102 to 104 times greater than those which prevailed during porphyritic chondrule formation (total range of ∼ 1 to ∼ 106 m−3). Distinctive “rims” of fine‐grained sulfides and/or silicates occur on both porphyritic and nonporphyritic types and appear to post‐date chondrule formation. Apparently, either the same process(es) contributed chondrules to all unequilibrated ordinary chondrites or, if genetically different, the various chondrule types were well mixed before incorporation into chondrites. Melting of pre‐existing materials is the mechanism favored for chondrule formation.
VUGS IN ORDINARY CHONDRITES
Authors: Olsen Edward
Published: June 2012

Large vugs occur in the ordinary chondrite, Farmington. They contain the same phases present in the body of the meteorite, either as vug wall lining or as crystals attached to linings. The morphologies of these phases indicate a history of melting and vapor deposition. These vugs are compared with vugs in the ordinary chondrites, Orvinio and Tadjera, and with published reports of vugs in Rose City and Shaw. It is concluded that although shock events may not cause heating above the liquidus for the body of the meteorite, local pockets of melting and vapor formation do occur due to inhomogenieties in the shock wave pattern. Vugs represent such pockets. Vug formation, as a consequence of shock processing, is widespread among ordinary chondrites and shows no correlation with the average temperature of shock heating, subsequent average cooling rate (as indicated by metallurgical criteria), or blackening of body color.
GRIER(b), A “MONOMICT,” BRECCIATED CHONDRITE
Authors: Fredriksson K. , Reid C.G.R. , Fredriksson B.J.
Published: June 2012

The Grier(b), New Mexico meteorite, a single mass of 929.4 grams, was found in 1969. This brecciated chondrite can be classified as an L‐group from the bulk chemical analysis, ∼ 8 wt % metal with an estimated total iron content of 25 wt %, and the constant olivine (Fa25.5) and orthopyroxene (Fs23) compositions. The main portion of the meteorite fits the criteria for an L5 (grey to intermediate hypersthene) chondrite. A conspicuous, large (several cm3) dense fragment, texturally an L6–7 chondrite, contains practically no metal or chondrules. However, there is little variation in the bulk silicate and individual phase compositions between the fragment and the matrix. In spite of this, it seems unlikely that the fragment was created in situ because metal and sulfide are not found in the fragment‐matrix contact zone; thus the formation of olivines and pyroxenes in both parts, as well as the “draining” of metal from the fragment, occurred prior to accretion with little, if any, subsequent thermal metamorphism.
IRGHIZITES AND ZHAMANSHINITES: ZHAMANSHIN CRATER, USSR
Authors: Bouşka V.I. , Povondra P. , Florenskij P.V. , Řanda Z.
Published: June 2012

Two irghizites, three zhamanshinites and one sample each of lechatelierite, vein‐quartz, Palaeogene silty clay and Palaeogene quartzite were analyzed using neutron activation analysis. A silicate analysis of the Palaeogene silty clay has also been performed, as well as an incomplete analysis of the Palaeogene quartzite from the Zhamanshin impact crater. The REE abundances of irghizites resemble those of sedimentary rocks. On the Köhler and Raaz diagram all projection points of irghizites lie inside the field of tektites, and indicate that they were derived from terrestrial sedimentary rocks. The Zhamanshin impact glasses may be divided into three types: (a) silica‐rich zhamanshinites (x̄SiO2 = 73.89%), (b) zhamanshinites (x̄SiO2 = 54.34%), and (c) silica‐poor zhamanshinites (x̄SiO2 = 39.64%). These are also characterized by varying proportions of alkalis and Al. Mn and Ca contents. Irghizites and silica‐rich zhamanshinites display a depletion of Eu. Zhamanshinites do not show this Eu depletion. Partial melting is assumed to be an important process in the origin of zhamanshinites.
IMPACT AND IMPACT‐LIKE STRUCTURES IN ALGERIA PART II MULTI‐RINGED STRUCTURES
Authors: Lambert P. , McHone J.F. , Dietz R.S. , Briedj M. , Djender M.
Published: June 2012

While Part I was devoted to the study of bowl‐shaped depressions in Algeria, the present article focuses on multi‐ringed structures of possible impact origin on the Algerian Sahara platform. Four structures were selected from orbital, aviation and geologic documents but only three were visited. TIN BIDER (27°36′N; 005°07′E) is a concentric multiple ring structure at least 6 km in diameter. Upper‐Cretaceous sedimentary beds outside the structure dip inward a few degrees at the periphery and become extremely folded nearer the center, yet a general circular symmetry is always retained. A clearly exposed contact between upper deformed beds and underlying on‐deformed beds is remarkably flat, dipping less than 10° inward. The upper beds display strong centrifugal folding. In the center of the structure Lower‐Cretaceous sandstones about 0.5 km above their normal stratigraphic position are exposed. Although no shatter cones, intensive brecciation, or fracturing were observed, there is definite petrographic evidence of shock metamorphism (planar elements) in the quartz grains of the central sandstones. Tin Bider is a probable impact structure. It is the only astrobleme known with such prominent ductile deformations, a characteristic which may be due to the nature of the target materials. Detailed studies are now required to understand the mechanism of deformation of this multi‐ringed structure. Its formation may be early Tertiary in age. FOUM TEGUENTOUR (26°14.5′N; 002°25′E) is an 8 km diameter bull's eye ring pattern. Although the high circularity and the morphology are consistent with an impact origin, the prominence of ductile deformation, the nature of the formations (clay‐gypsum with sandstone intercalcations), the type of folds, the relationships between the structure and a surrounding plateau, and the lack of any evidence of shock effects better support a diapiric origin. MAZOULA (28°24′N; 007°49′E) is an 800 m diameter multi‐ring feature with a 300 m wide anticlinal dome which rises some 30–35 m above the surrounding horizontal strata. The dome is capped by a flat‐lying massive carbonate layer dipping on the flanks in accordance to the surface topography. There are no special disturbances, no fractures or breccias. Mazoula is not impact in origin but may be a Cretaceous rudistid reef and/or a salt diapir.
TIERRA BLANCA: AN UNUSUAL ACHONDRITE FROM WEST TEXAS
Authors: King Elbert A. , Jarosewich Eugene , Daugherty F.W.
Published: June 2012

Tierra Blanca is an achondrite (sensu stricto) composed chiefly of orthopyroxene, olivine, plagioclase and clinopyroxene. The mineralogy, major element chemistry and texture are similar to Winona and also Mt. Morris, Acapulco and Antarctic meteorite ALHA 77081 to some degree. The designation of this group as “Winonaites,” as suggested by Prinz et al. (1980), seems justified and useful.
TWO NEW IRON METEORITES FROM WESTERN AUSTRALIA
Authors: De Laeter J.R.
Published: June 2012

Two new iron meteorites from Western Australia are described: Cosmo Newberry — a 2.156 kg meteorite of unusual spiky shape, and Gnowangerup — a 33.6 kg pear‐shaped meteorite. X‐ray fluorescence spectrometry shows that Cosmo Newberry can be classified in Group IIA, whilst Gnowangerup is a member of Group IIIAB. Neither iron can be associated with any other Western Australian meteorite.
THE MANEGAON DIOGENITE
Authors: Fredriksson K.
Published: June 2012

A new analysis of the Manegaon hypersthene achondrite is presented and compared with the other eight known falls of this class.
CANADIAN ARCTIC METEORITE SEARCH: 1981
Authors: Robertson P.B. , Coleman L.C. , Olsen E.J. , Kissin S.A.
Published: June 2012

The recovery of several thousand meteorite fragments from Antarctica has led to speculation that accumulations may occur on the Earth's other major ice caps. Meteorites falling over the past 80,000 years on the Devon Island ice cap in the Canadian Arctic may be exposed at the surface near the ice cap margin. From the terrestrial meteorite flux, ice movement rates, and fragmentation factors it is calculated that 12,560 samples of 150 g mass are potentially concentrated in a 65 km2 zone along the northwest margin. A search of this region on foot and by helicopter in July, 1981, failed to recover any specimens. Although metre‐sized gneissic boulders, plucked from the underlying Precambrian basement, were concentrated in this zone it is postulated that the unseasonal 30 cm snow cover on the ice prohibited the recognition of possible meteorite specimens, which may average only 5 cm in diameter.
BRECCIATED MUONG NONG‐TYPE TEKTITES
Authors: Futrell Darryl S. , Fredriksson Kurt
Published: June 2012

Welded breccias and faults in Muong Nong‐type indochinite tektites from Thailand are illustrated. Electron probe analyses of these tektites show somewhat higher Al and alkalies in light‐colored layers, and somewhat higher Si and Ca in dark‐colored layers.
SUMMARY OF SEVERAL RECENT CHONDRITE FINDS FROM THE TEXAS PANHANDLE
Authors: Sipiera Paul S. , Olsen Edward J. , Eatough Dorothy L. , Dod Bruce D.
Published: June 2012

Eleven recent chondrite finds from the Texas Panhandle have been examined and classified according to mineralogical and petrological criteria: five H's, five L's, and one LL chondrite. Five are distinct from nearby finds, while three remain ambiguous and three are related to previously reported chondrites. In addition, data are provided to classify the Muleshoe, Silverton, and Vigo Park chondrites, all of which were previously undescribed in the literature.
DESCRIPTION, CHEMICAL COMPOSITION AND NOBLE GASES OF THE CHONDRITE NOGATA
Authors: Shima Masako , Murayama Sadao , Okada Akihiko , Yabuki Hideo , Takaoka Nobuo
Published: June 2012

An ordinary chondrite weighing 472 g kept in the Shinto shrine, Suga Jinja, Nogata‐shi, Fukuoka‐ken, Japan, as treasure, was said to have fallen in the precinct of the shrine, approximately 130°45.0′E. and 33°43.5′N., on May 19, 861 A.D. The date of fall was confirmed by old literature, as well as written script on, and 14C age determination of, the lid of the wooden box in which it has been stored.

The chondrite was named Nogata after the present name of the place of fall.

Although the Fe content of Nogata is a little too low, the bulk chemical composition, comparison of the norm with average H‐, L‐ and LL‐group chondrites, the relation of Femetal/Ni versus Femetal/Fetotal, and molar composition of olivine and orthopyroxene indicate that Nogata is an L‐group chondrite.

From the well recrystallized structure, extreme obliteration of the primary chondrule texture, homogeneous composition of olivine and orthopyroxene, absence of igneous glass and interstitial and well‐developed plagioclase, it should be classified as petrologic type 6.

Nogata appears lightly shocked, upper b or the border of b and c by Van Schmus and Ribbe's classification, whereas most L6 chondrites are more heavily shocked.

Nogata contains rather high amounts of both radiogenic and spallogenic light noble gases, and gives gas retention ages and cosmic‐ray‐exposure ages (e.g. 21Ne age) of 4.5 and 4.7 × 103 years and 4.00 × 107 years, respectively. From such results combined with the light shock effects of Nogata, it is concluded that metamorphism of this chondrite was completed just after the formation of the parent body in a very short interval, > 108 years, with subsequent quiescence.
THE ATLANTA ENSTATITE CHONDRITE BRECCIA
Authors: Rubin Alan E.
Published: June 2012

Atlanta is the fifth known brecciated enstatite chondrite. It contains a centimeter‐sized troilite‐rich clast, similar to those that occur in Blithfield. All of these clasts probably formed in the solar nebula under high pS2/pO2 conditions in a gas of non‐cosmic composition. The absence of ordinary or carbonaceous chondrite clasts in any of the enstatite chondrite breccias and absence of enstatite chondrite clasts or materials formed at high pS2/pO2 ratios in ordinary and carbonaceous chondrite breccias support the model that enstatite chondrites were formed at a location distant from those of the other chondritic groups.
LITHIUM IN STONE METEORITES AND STONY IRONS
Authors: Murty S.V.S. , Shukla P.N. , Goel P.S.
Published: June 2012

Lithium contents have been determined by neutron activation analysis in 54 meteorites distributed as: C (9), H (13), L (10), LL (3), E (2), achondrites (11), and stony irons (6). Among the undifferentiated meteorites Li contents range from 1 to 3 ppm. Li contents are higher in Ca‐rich achondrites and mesosiderites than in Ca‐poor achondrites and pallasites respectively. Among achondrites, Li correlates positively with Ca and Al and inversely with Mg. A minor Li‐rich phase might be associated with the plagioclase component of achondrites. In several meteorites Li concentration is determined in magnetic and nonmagnetic fractions, chondrules, and light and dark components (for the gas‐rich meteorites).
BRIANZA: AN EXAMPLE OF WRONGLY BELIEVED CHONDRITE
Authors: Levi‐Donati G.R. , Clarke Roy S.
Published: June 2012

The results obtained from the specimen labelled BRIANZA revealed that it is an artificial iron and not a chondritic meteorite, as previously supposed.
USTÍ NAD ORLICI: A NEW L6 CHONDRITE FROM CZECHOSLOVAKIA
Authors: Bukovanská M. , Jake***ŝ P. , Pernicka E. , El Goresy A.
Published: June 2012

Ustí nad Orlici (Kerhartice), a meteorite which fell on June 12, 1963 in Czechoslovakia, is classified as a L6 chondrite. Compositions of olivine (Fa 23.4), orthopyroxene (Fs 20, Wo 1.3), plagioclase (Ab85An10Or5) along with the bulk composition of the meteorite support this classification. Chromite compositions vary with grain size. Large chromites are higher in TiO2 and lower in Fe3 than small chromites. This may indicate that either these two chromites formed initially under different fO2 conditions, or that this difference resulted from different equilibration behaviors of both chromites as a function of grain size. The meteorite contains three distinct sulfide assemblages: 1) troilite‐pentlandite, 2) troilite, pentlandite‐cubanite‐chalcopyrite‐pyrrhotite‐mackinawite, 3) troilite‐tetrataenite‐(Fe, Cu, Ni)1***. 02S. These assemblages indicate equilibration down to temperatures close to 200 °C.
MINOR ELEMENTS IN MARJALAHTI OLIVINE
Authors: Ryder Graham
Published: June 2012

Precise microprobe determinations of minor elements in olivine from Marjalahti show averages of 0.067% CaO; 0.0211% Cr2O3; less than 0.0045% TiO2; 0.288% MnO; and 30 ppm Ni. The calcium is as high as in some terrestrial plutonic olivines (e.g. Stillwater) but lower than in terrestrial nodule (high‐temperature mantle?) olivines, consistent with very slow cooling to low temperatures. The chromium is discrepant with some earlier determinations, and possibly chromium is zoned in most pallasitic olivines. The Ti, Mn, and Ni data are consistent with previous determinations.
THE GRAYTON BEACH, FLORIDA METEORITE
Authors: Povenmire Harold
Published: June 2012

On October 30, 1983, two treasure hunters, Phillip W. Gibson, a government diver and former Apollo recovery team member, and John M. Green, M.D. were searching for Spanish armor in an ancient Indian midden, or trash site near Grayton Beach, Florida. Using metal detectors, they found an 11.3 kg heavy brown rock approximately one meter below the surface.
HIGH POSSIL AND STRATHMORE—A STUDY OF TWO L6 CHONDRITES
Authors: Bevan A.W.R. , Hutchison R. , Easton A.J. , Durant G.P. , Farrow C.M.
Published: June 2012

High Possil and Strathmore are the first (1804) and last (1917) meteorite falls, respectively, of the three recorded in Scotland. Olivine compositions and total Fe contents in High Possil (Fa25.2; 21.35 wt %) and Strathmore (Fa25.3; 20.6 wt %) confirm their classification as L‐group chondrites (Mason, 1963), and the presence of abundant plagioclase feldspar shows that both chondrites belong to petrologic type 6. Both chondrites display thermal and mechanical alteration attributable to moderate shock‐loading appropriate to facies c (High Possil) and c‐d (Strathmore) (Dodd and Jarosewich, 1979). Incipient shock‐melting of metal and troilite in both chondrites is the first described from Lc chondrites, and differences in the responses of metallic and silicate minerals to shock‐loading are discussed.