bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Total Known Weight of the Cape York, Greenland, Sideritic Fall (ECN =+0650,760:)*
Authors: Leonard Frederick C. 
Published: June 2012

ABSTRACTThe total known weight of the Cape York, Greenland, sideritic fall, which includes 4 recovered individuals—“Ahnighito,” the Savik iron, “the Woman,” and “the Dog”—appears, in the light of the best available information, to be approximately 66 metric tons.The Savik iron (weight = 3402 kg.) and the Furnas County member (weight = 1073 kg.) of the Norton County, Kansas‐Furnas County, Nebraska; achondritic shower of 1948 February 18 raise to 68 the total number of known individual meteorites weighing 400 kg. or more.The largest recovered member of the Canyon Diablo, Arizona, sideritic fall (weight = 639 kg.) has recently been placed on permanent display in the new museum building on the north rim of the Barringer Meteorite Crater.
Injuries from Falling Meteorites
Authors: La Paz Lincoln 
Published: June 2012

ABSTRACTIn the first section of this paper, historical evidence concerning injuries occasioned by falling meteorites, including the recent Aba, Japan, incident described by I. Yamamoto and S. Murayama in the preceding notes is presented. In the second section, the possibility of injury from meteoritic falls is critically examined from the viewpoint of the theory of probability. It is found that the probability of a hit on the Human Target‐Area (HTA) of Europe (or of America) during any century between 1600 a.d. and 2200 a.d. is very small. There are, however, about 316 chances out of 1000 that at least one meteorite will strike in the world's HTA during the 20th century. Furthermore, there is very nearly a 50–50 chance for at least one meteorite to hit in the same HTA during the 3 centuries from 1700 to 2000 a.d. Finally, the odds are 99 to 1 that in at least one of the centuries between 2100 and 3300 a.d. at least one meteorite will hit in the world's HTA.
A Re‐examination of the Crater near Crestone, Colorado*
Authors: MARVIN URSULA B. , MARVIN T. C. 
Published: June 2012

Abstract The Crestone Crater is an elliptical bowl measuring 355 feet by 246 feet with a mean depth of 23 feet. It lies in unconsolidated sand on the surface of an alluvial fan at the base of the Sangre de Cristo Mountain Range in the San Luis Valley, Colorado (37° 54′ N, 105° 39′ W). Aerial photographs show the crater as a striking feature in its setting on a gently undulating terrain.We examined the site in August 1963 to appraise the possibility that it was formed by meteorite or comet impact. The crater and its vicinity were mapped at two‐foot contour intervals, and two lines of auger‐hole samples, eight feet deep, were collected across the crater.Sand from the rim and floor is similar in grain size and composition to that several miles to the north and south. It is barren of meteoritic debris, nickel‐iron spherules, rock flour, and impact glass.The crater is less than half as deep relative to its diameter as known meteorite explosion craters. Furthermore, topographic profiles indicate that the crater does not form a depression in the land surface. The crater rim is a positive feature enclosing a basin that has a floor approximately level with the surface of the alluvial fan on which it lies.In the absence of any mineralogic or topographic evidence of impact or explosion, we conclude that this landform is not meteoritic or cometary in origin.
Hollow Australite Button with Flange, Hordern Vale, Otway Peninsula, Western Victoria
Authors: BAKER GEORGE 
Published: June 2012

Abstract A relatively thin walled hollow australite button recently discovered in an unbroken condition on the surface of a shallow sand pit in the Otway Ranges, Victoria, contains a double internal cavity with a total calculated volume of approximately four cubic centimeters. A little over half of a well developed circumferential flange is still attached to the hollow core of the specimen, the missing portion having been removed by terrestrial erosion. The front surface reveals a well preserved aerodynamic sculpture pattern such that the orientation of the specimen during hypersonic atmospheric transit can be accurately determined to show its aerodynamically stable flight position.Such double bubbles are unique among Australian tektites, whether in the fractured or well preserved state, and it is equally as uncommon to find an unbroken hollow australite core with remnants of still attached circumferential flange.
MINERALOGICAL RELATIONSHIPS IN SEYMOUR, A COARSE OCTAHEDRITE
Authors: Drake John C. 
Published: June 2012

Seymour is a coarse octahedrite weighing 24.5 kg. It contains two types of troilite‐graphite nodules (massive graphite nodules with irregular troilite rims, and troilite nodules with irregular, partial or total, rims of graphite); four morphologically distinct types of phosphide (lamellar, swathing, grain boundary, and rhabdite); and three types of cohenite (lamellar, swathing, and inclusions in kamacite).It is believed that lamellar and swathing schreibersite crystallized from taenite at approximately 900°C. This was followed by the crystallization of kamacite, then the development of cohenite, and finally a second period of phosphide nucleation giving rise to grain boundary schreibersite and rhabdite. Compositional data indicates that grain boundary schreibersite and rhabdite grew simultaneously.
AN EQUATION FOR THE DETERMINATION OF IRON‐METEORITE COOLING RATES
Authors: Wasson John T. 
Published: June 2012

The Goldstein‐Short graph for the determination of ironmeteorite cooling rates from kamacite bandwidths and Ni concentrations has been approximated by the equation:log CR = −2.040 log BW — 8.940 log Ni + 8.700where the cooling rate, CR, is in units of°K/m.y., the bandwidth, BW, in units of mm, and Ni concentration is in weight percent. The equation reproduces the Goldstein‐Short values to within ±7% within the Ni concentration range 7 to 14%, which includes most octahedrites. The discrepancy between the graphical or analytical cooling‐rate estimations and those estimated from microprobe data is a factor of 2.1 at 1σ.
ON THE POSSIBLE NUMBER AND MASS OF FRAGMENTS FROM PUŁTUSK METEORITE SHOWER, 1868
Authors: Lang Bruno , Kowalski Maciej 
Published: June 2012

The earlier efforts to approximate the total number and mass of fragments from Pułtusk meteorite shower 1868 have been found unsatisfactoryWith the use of the field data of Samsonowicz and the sorting equation after Frost, differential expressions approximating the mass and number of fragments are derived. These expressions numerically integrated over the elliptical strewnfield area lead to the estimates ∼ 1.8 times 105 and ∼ 2 times 106 g for the total number and mass of fragments respectively.The meaning of the obtained results is discussed.
CARBON AND NITROGEN ABUNDANCES IN SELECTED ACHONDRITES
Authors: Gibson Everett K. , Moore Carleton B. , Lewis Charles F. 
Published: June 2012

Total carbon and nitrogen contents are reported for four howardites, three enstatite achondrites and one hypersthene achondrite. The mean value for eucrites is 650 ppm C and howardites 1440 ppm C. The Haraiya eucrite has an anomalously high carbon contentThe nitrogen contents range between 24 and 66 ppm N. The mean N value for eucrites is 36 ppm N and for the howardites 51 ppm N.
MINERALOGY AND PETROLOGY OF THE YILMIA ENSTATITE CHONDRITE
Authors: Buseck Peter R. , Holdsworth Edward F. 
Published: June 2012

Yilmia, a new enstatite chondrite contains moderately well defined radiating and granular chondrules. The plagioclase to enstatite ratio is appreciably higher within than outside of the two granular chondrules in our microprobe sections. Osbornite was observed within the granular chondrules, but not in the rayed chondrules or surrounding matrixMajor phases include enstatite, plagioclase (Ab80 An16 Or4), silica, silicon‐rich kamacite and titanian troilite. Minor phases are many and varied: sinoite, silicon‐rich taenite, schreibersite, graphite, osbornite, oldhamite, “normal” and zincian daubreelite, ferroan alabandite and a new FeZnMn monosulfideThe new mineral (Fe.538 Zn.246 Mn.159 Mg.004 S) closely resembles albandite and could easily have been overlooked in other meteorites unless a microprobe was used. A new form of oldhamite was also found. Indarch oldhamite, analyzed for comparative purposes, consists of two similar but distinct species: Ca.96 Mn.005 Mg.04 Fe.01 S and Ca1.000 Mn.004 Mg.02 Fe.005 S. These have not been reported from other meteoritesBased on its mineralogy and texture this is a type II (E6) enstatite chondrite that is transitional toward the intermediate type (E5). It is unique in its mineralogical complexity, abundance of taenite, diversity of zincian minerals and monosulfides, and restriction of osbornite to certain chondrules
CALCIUM VARIATION IN OLIVINES OF THE MURCHISON AND VIGARANO METEORITES
Authors: Hutchison R. , Symes R.F. 
Published: June 2012

Olivine grains were analysed by microprobe for Si, Ca, Mg, and Fe. Distribution of Mg and Fe is similar to that already established for Type II and III carbonaceous chondrites. Calcium concentration varies by a factor of about 4 and seems to be independent of fayalite content: its range (about 0.1 − 0.45 weight percent) resembles that in the olivines of Murray (Fredriksson and Keil, 1964).Olivines of carbonaceous chondrites are the product of mechanical mixing of pre‐existing crystals (Van Schmus, 1969). More than one fractionation process is necessary to account for Ca variation superimposed on Mg:Fe fractionation observed in Murray, Murchison and Vigarano.
EVIDENCE FOR VAPOR FRACTIONATION IN THE ORIGIN OF CHONDRULES
Authors: Walter Louis S. , Dodd Robert T. 
Published: June 2012

The major‐element compositions of 47 individual Chainpur (LL‐3) chondrules were determined. There appears to be no correlation between Na and Al, in contrast with the correlation previously found in Bjurbole chondrules in which these elements are characteristically found in equal molar proportions. The correlation in Bjurbole chondrules is considered to be the effect of metamorphism.The compositional variations among Chainpur chondrules point to a fractionation which basically involved only silica. This can best be explained as being the result of vapor fractionation which took place during or after the formation of the chondrules. The degree of fractionation is not a function of the mass of the chondrule, a fact which places some restraints on heating mechanisms (e.g., radiant or shock heating) which might vary depending on the surface area/mass ratio.The ratio of Ca to Al in the individual chondrules is generally close to the value 1.08 which has been found to be characteristic of the chondrites in general.
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 gradeWe 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
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.
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 GUJARGAON METEORITE
Authors: Gupta P.R. Sen , Ram Kashi , Das A.K. , Paul S.R. , Guha B.K. , Nag D.K. 
Published: June 2012

The Gujargaon meteorite was observed to fall on a cotton field at Gujargaon in Dewas district, Madhya Pradesh, India, on the afternoon of the 4th of September, 1982. It is an oriented stone with a saucer‐shaped front and regmaglypted rear with surfaces of more than one generation, and is entirely covered by fusion crust.Gujargaon is an H5 chondrite with rare chondrules integrated with the matrix. Intense fracturing with fractures filled by glassy veins, and undulose extinction and deformation‐twin lamellae in troilite bear evidences of shock. Compared to average H‐group chondrites Gujargaon appears to have higher contents of SiO2and normative pyroxene.
MINERALOGY OF THE BOCAIUVA IRON METEORITE: A PRELIMINARY STUDY
Authors: Desnoyers C. , Michel‐Levy M. Christophe , Azevedo I.S. , Scorzelli R.B. , Danon J. , da Silva E. Galvão 
Published: June 2012

The Bocaiuva iron contains 10 to 15% by volume of silicate inclusions which are surrounded by kamacite (6.5 wt % Ni). The metal shows a Widmanstätten pattern in metal areas devoid of silicates; taenite evolved in plessite fields. The silicate inclusions occur as nodules, and as irregular or chain‐like aggregates in which olivine may be rounded or faceted. The magnesian silicates (forsterite, enstatite, diopside) are similar in composition to those of the group IAB irons, whereas the interstitial plagioclase is much more calcic (An 50) than that usually found. Iron sulfide occurs as pyrrhotite and contains 1–2 wt% Cu. Chromite and euhedral magnetite are accessory phases always associated with pyrrhotite. Some patches of pyrrhotite enclose rounded chromite and small plagioclase crystals displaying compositions different from those of the ground mass of the inclusions. Schreibersite shows a compositional variability.This preliminary study underlines the unusual nature of Ms iron and raises several questions concerning the genetic relations between silicates, sulfide and metal, and the thermal history of the whole material.
THE COLONY METEORITE AND VARIATIONS IN CO3 CHONDRITE PROPERTIES
Authors: Rubin Alan E. , James Janet A. , Keck Bradley D. , Weeks Karen S. , Sears Derek W.G. , Jarosewich Eugene 
Published: June 2012

The Colony meteorite is an accretionary breccia containing several millimeter‐to centimeter‐size chondritic clasts embedded in a chondritic host. Colony is one of the least equilibrated CO3 chondrites; it has an unrecrystallized texture and contains compositionally heterogeneous olivine and low‐Ca pyroxene, kamacite with low Ni and Co and high Cr, amoeboid inclusions with low FeO and MnO, a fine‐grained silicate matrix with very high FeO, and numerous small chondrules with clear pink glass. However, Colony differs from normal CO chondrites in several respects: Although Al, Sc, V, Cr, Ir, Fe, Au and Ga abundances are consistent with a CO chondrite classification, certain lithophiles (Mg and Mn), siderophiles (Ni and Co) and chalcophiles (Se and Zn) are depleted by factors of 10–40%. The shape of Colony's thermoluminescence (TL) glow curve is similar to that of Allan Hills A77307 (another unequilibrated chondrite with CO3 petrological characteristics) and different from those of normal CO chondrites. [ALHA77307 also resembles Colony in having low Mg, Mn, Ni and Co, compared to normal CO chondrites, but it possesses CO‐CV levels of Se and Zn and nearly CV levels of Cd.]Colony is badly weathered; it contains 22.7 wt.% Fe2O3 and 5.7 wt.% H2O. Recalculating the analysis on an H2O‐free basis with all Fe2O3, NiO and CoO converted to metal, yields an inferred original metallic Fe, Ni abundance of ∼ 19 wt.%. This is similar to that of Kainsaz (an unweathered CO3 fall), but much higher than that of all other CO3 chondrites (< 6.3 wt.%). Although it is possible that Colony and either ALHA77307 or Kainsaz constitute distinct CO3 chemical subgroups, the weathered nature of Colony and ALHA77307 preclude the drawing of firm conclusions. Nevertheless, it is clear that CO3 chondrites vary more in compositional and petrological properties than was previously recognized.
The Distribution and Significance of Evaporitic Weathering Products on Antarctic Meteorites
Authors: Velbel Michael Anthony 
Published: June 2012

Abstract— The distribution of white evaporitic deposits differs among different meteorite compositional groups and weathering categories of Antarctic meteorites. Evaporites occur with unusual frequency on carbonaceous chondrites, and are especially common in carbonaceous chondrites of weathering categories A and B. Among achondrites, weathering categories A and A/B show the most examples of evaporite weathering. Unlike carbonaceous chondrites and achondrites, most evaporite‐bearing ordinary (H and L) chondrites are from rustier meteorites of weathering categories B and, to a lesser degree, B/C and C. LL chondrites are conspicuous by their complete lack of any evaporitic weathering product.Almost two‐thirds of all evaporite‐bearing meteorites belong to weathering categories A, A/B, and B. Where chemical data are available, surficial evaporite deposits are associated with elemental anomalies in meteorite interiors. Meteorites of weathering classes B, A/B, and even A may have experienced significant element redistribution and/or contamination as a result of terrestrial exposure. Evaporite formation during terrestrial weathering cannot be neglected in geochemical, cosmochemical, and mineralogical studies of Antarctic meteorites. A lower‐case “e” should be added to the weathering classification of evaporite‐bearing Antarctic meteorites, to inform meteorite scientists of the presence of evaporite deposits and their associated compositional effects.
Raman Spectra of Shocked Minerals 1: Olivine
Authors: Heymann D. , Cellucci T. A. 
Published: June 2012

Abstract— The Raman spectrum of olivine contained in a chip of the Twin Sisters Peak dunite shocked to 22.2 GPa is essentially identical to the spectrum of unshocked olivine in this rock. The Raman spectra of a powder of the rock shocked to 20.1 GPa and of chips shocked to 59.5 GPa and 60.7 GPa show strong and broad low‐frequency features with crests at 475 cm−1, 556 cm−1, and 572 cm−1, and strong as well as broad high‐frequency features near 1100 cm−1. We conclude that these features are most likely due to the formation of “olivine glass” with a considerable degree of three‐dimensional Si‐O‐Si linkage, having scattered domains of greatly variable grain size, internal structure, and, possibly, chemical composition. We cannot conclude with our results at hand whether olivine shocked to the highest pressures has not decomposed to very fine‐grained MgO plus an SiO2‐rich glass.We also conclude from our results that the structural changes are not likely to have formed in the laser beam of the measurement.
The Haughton Impact Structure, Devon Island, Canada: Setting and History of Investigations
Authors: Robertson P. Blyth 
Published: June 2012

Abstract— Although mapped initially as a piercement dome, subsequent discovery of shock metamorphism in clasts of an impact breccia, shatter cones in outcrops of uplifted target rocks and morphological and geophysical characteristics consistent with a complex crater, confirmed a meteorite impact origin for the Haughton structure, Devon Island.Results of three field investigations carried out prior to 1984 defined a complex crater, 20 km in diameter, formed in a lower Paleozoic sedimentary sequence overlying gneisses of the Precambrian basement. The distribution of allochthonous breccia overlying the disturbed target rocks and of the sediments deposited in the crater‐filling lake were mapped. A Miocene or possibly Holocene age for the crater was based on paleo‐flora and fauna assemblages from the lake sediments. Gravity and magnetic surveys revealed anomalies coincident with the crater, but not interpretable from surface lithologies.Some of the early investigations were of a reconnaissance nature and results and interpretation can only be considered preliminary. Other studies that were carried out in some detail, petrographic investigations in particular, require complementary work for a fuller understanding of their significance. As a result, in 1984 the HISS (Haughton Impact Structure Studies) group carried out a program of detailed geological mapping and sampling, and seismic, gravity, and magnetic surveys in an attempt to improve the definition of the surface and subsurface nature of Haughton, and to formulate a more complete understanding of its formation and subsequent history. Results of these various studies are presented in the eight succeeding papers of this volume.