bluuebunny/crossref_metadata_2025 huggingface dataset:
The Orbits of Three Stone‐Dropping Meteors: Tilden, Paragould, and Archie*
Authors: Wylie C. C.
Published: June 2012

The elements of the orbits of the bodies that dropped stony meteorites (aerolites) at Tilden, Illinois, in 1927; at Paragould, Arkansas, in 1930; and at Archie, Missouri, in 1932, are presented and briefly discussed. All 3 orbits were direct, with moderate eccentricities and inclinations, not unlike those of some of the asteroids.
The Energy of the Podkamennaya Tunguska, Siberia, Meteoritic Fall (±1019,609)
Authors: La Paz Lincoln
Published: June 2012

This note points out that, in case F. J. W. Whipple's estimate of the energy expended by the Podkamennaya Tunguska, Siberia, meteorite on the atmosphere is accepted, the mass of this meteorite, assumed to be terrene in composition, must have been of the order of 107 metric tons, if its velocity was 10 km./sec., and of the order of 105 metric tons, even if its velocity was 100 km./sec. The enormity of these terrene masses, coupled with the failure of exhaustive search to recover any fragment whatever of this fall, is held to support the hypothesis that the Podkamennaya Tunguska meteorite was contraterrene in nature.
The Non‐circularity of the Canyon Diablo, Arizona, Meteorite Crater*
Authors: Zimmerman Walter W.
Published: June 2012

In an attempt to obtain photographic evidence relative to the existence or non‐existence of “rays” in connection with the Canyon Diablo, Arizona, Meteorite Crater, aerial photographs were secured, which showed the Crater to be distinctly non‐circular in outline.
A New Glass of Possibly Extraterrestrial Origin*
Authors: Cross Frank C.
Published: June 2012

This paper records the discovery, in Val Verde County, on the Rio Grande in Texas, of 350 remarkably symmetrical specimens of natural glass resembling certain forms of tektites—particularly australites. The distribution of the specimens in a small elliptical area far removed from any evidence of volcanic action, as well as certain features of the specimens themselves, suggests for them a possibly extraterrestrial origin, tho they exhibit certain features which set them definitely apart from other specimens ordinarily accepted as belonging in the category of tektites.
The Valverdites: A Weathered Obsidian Form Superficially Resembling Certain Tektites*
Authors: La Paz Lincoln
Published: June 2012

This paper is devoted to a critical study of the natural glasses recently found in Val Verde County, Texas. On the basis of the behavior of these so‐called valverdites under the blowpipe flame; of their low densities and indices of refraction; of the crystallites and megascopic crystals contained in them; and of their other peculiarities, the conclusion is reached that they are not tektites, but are weathered pebbles of obsidian.
The Reported Crater‐Producing Meteoritic Fall of 1947 February 12 in Eastern Siberia
Authors: La Paz Lincoln
Published: June 2012

In recent issues of these Contributions, certain Russian news releases concerning the fall of crater‐producing meteorites in the Ussuri Taiga in eastern Siberia, on 1947 February 12, are quoted or abstracted. It is the purpose of this paper to record other Russian news items concerning this fall, and to point out the existence of internal inconsistencies in all such news reports; also surprising discrepancies, on the one hand, between them and the information on the Ussuri fall published by Russian meteoriticists, and, on the other hand, between them and the numerous concordant reports relating to the great Podkamennaya Tunguska, Siberia (± 1019,609), fall of 1908 June 30. A summary of the information on the Ussuri fall given in recent important papers by E. L. Krinov is presented, and attention is called to a program for the translation of Russian papers, such as Krinov's, on meteoritics, initiated in 1934–35 at the Ohio State University, by Dr. A. G. Wiens and the writer, and now resumed at the Institute of Meteoritics of the University of New Mexico by the writer, in cooperation with Dr. Alexander W. Boldyreff.
A Second Note on the Exclusively Meteoritic Minerals
Authors: Neuerburg George J.
Published: June 2012

Troilite, which has been contended recently to be exclusively meteoritic, has one well‐authenticated terrestrial occurrence. The identification of terrestrial clinoenstatite and clinohypersthene is subject to considerable doubt; it is therefore suggested that these minerals should be included in the list of exclusively meteoritic minerals. It is suggested further that taenite is properly excluded from this list. The revised list contains clinoenstatite (?), clinohypersthene (?), daubréelite, kosmochlor, merrillite (?), oldhamite, osbornite, phosphorus, schreibersite, and weinbergerite.
Azimuth Determinations in Meteoritics by Means of Time Readings*
Authors: La Paz Lincoln
Published: June 2012

The inability of untrained observers accurately to measure and report, e.g., the azimuth (bearing) of the point of disappearance, L, of a fireball is universally acknowledged. Even several weeks after the occurrence of a spectacular fireball, however, such observers are able to remember and to point out with some accuracy the position that L occupied in the sky. In this paper, advantage is taken of the layman's ability to recall and to sight at points in the sky like L, in order to develop a method by means of which the azimuth of a point, P, on the apparent path of a meteorite thru the atmosphere can be calculated, provided the observer simply reads and records a single watch‐time, T, on some sunny day subsequent to the fall. This time, T, is the instant when the true Sun either has the same azimuth as P or differs from P in azimuth by 180°.
The Effect of Cosmic Rays on Meteorites
Authors: Stücklen Hildegard
Published: June 2012

Abstract

An investigation has been made into the effect upon meteorites in space of the primary rays in the exceedingly strong cosmic radiation that falls upon these bodies before they penetrate the Earth's atmosphere. Specimens of meteorites with terrestrial ages (i.e., intervals since time of fall) ranging from 9 months to 457 years were studied by means of the nuclear‐emulsion‐plate technique.

The oldest meteorite studied (Ensisheim, Alsace, France) was found to be inactive, and the next oldest (Pitts, Georgia) was only very slightly active. On the other hand, the relatively young Walters, Oklahoma, meteorite showed considerable activity, and a metallic inclusion and one piece of crust from the very recent Norton‐Furnas Counties, Kansas‐Nebraska, achondritic fall of 1948 February 18 were very active indeed. Another piece of Norton crust showed only slight activity, and two other fragments of this achondrite were inactive.

Examination of the nuclear “stars” recorded on the emulsion plates shows that the activity observed in the specimens studied is an induced one and cannot be attributed to the low content of natural radioactive elements present in the meteorites. Tentative explanations of this induced activity are advanced in the paper.
A Preliminary Report on Indian Ruins Discovered Near the Crest of the Barringer Meteorite Crater, Arizona*
Authors: La Paz Lincoln
Published: June 2012

Abstract

References to the superstitious fear with which the Barringer Meteorite Crater, near Canyon Diablo, Arizona, was regarded by the native dwellers of the Southwest, and to their avoidance of the Crater site, are abundant in the literature of meteoritics. Discovery of points and other artifacts on the flanks of the Crater by the Ohio State University Meteorite Expedition of 1939 first cast doubt on the validity of legendary scare‐stories concerning the Indians, and this doubt was intensified by the discovery, in 1948–49, of remarkable arrowheads and pottery‐shards, well up on the rim of the Crater, by Mr. Theodore E. Johnson, the Custodian of the Crater. In an effort to settle the question of possible Indian occupancy of the rim, archeological investigations were carried on by the Institute of Meteoritics at the Crater in the summer of 1950. As a result, not only were many points and other artifacts collected, but also Indian ruins, constructed from blocks of the Coconino sandstone occurring in the Crater rim, were discovered. One of these ruins, situated only 250 feet below the crest of the Crater rim, was completely excavated by Institute personnel, and is believed to date from a.d. 1300, at the latest.
Synthetic Schreibersite*
Authors: Buddhue John Davis
Published: June 2012

Abstract

A simple preparation of 2 synthetic nickel‐iron phosphides is described. One has the physical properties and chemical composition of schreibersite. The other is non‐magnetic, is almost insoluble in acids, and has an analysis similar to 3 anomalous analyses of phosphide from the Canyon Diablo, Arizona, siderites.
Some Observations on High‐Speed Impact*
Authors: Rinehart John S.
Published: June 2012

Abstract

This paper summarizes many of the experimental data that exist on phenomena associated with the impact of high‐velocity particles; specifically, it discusses the impact of 20,000 ft./sec. particles produced by shaped charges, and the mechanics and energetics of crater formation. The probable mass of the meteorite that formed the Barringer Meteorite Crater of Arizona is calculated and found to be about 12,500 ordinary tons.

The principal conclusions drawn from the data are that (a) probably only a small fraction of the total mass of a meteorite is vaporized on impact; (b) a meteorite may or may not shatter on impact; (c) the volume of the crater fixes rather closely the striking energy of the meteorite; and (d) there is some likelihood that high‐velocity meteorites do not imbed themselves in the craters that they form.
The La Lande, New Mexico, Chondrite (ECN =+1041,344)*
Authors: Beck Carl W. , Stevenson Ralph G. , La Paz Lincoln
Published: June 2012

Abstract

In this paper are given details concerning a chondritic meteorite found in 1933 near the La Lande post office in De Baca County, New Mexico. Macroscopic and microscopic mineralogical examinations and chemical analyses are given. The meteorite is composed chiefly of olivine and enstatite (variety, hypersthene), lesser amounts of a dispersed metallic phase, and small percentages of enstatite‐clinoenstatite intergrowths and secondary hematite. On the basis of this investigation, the La Lande meteorite is classified as a hypersthene‐olivine chondrite (Chy). Evidence is presented to indicate that the La Lande aerolite may not be a distinct fall, but may be simply a member of the widely scattered Melrose, Curry County, New Mexico, shower. Three (3) figures and 2 tables are given.
The Odessa, Texas, Siderite (ECN =+ 1025,318)*
Authors: Beck Carl W. , La Paz Lincoln
Published: June 2012

Abstract

This paper presents certain historical facts relating to the discovery of meteorites in the neighborhood of the Odessa, Texas, Meteorite Crater; a discussion of the distribution and other characteristics of the meteoritic materials so far recovered by surface and subsurface search at that crater; a detailed mineralogical and metallographic study of the metallic phase of the meteorite; and chemical and radiochemical analyses of the sideritic material. The results of the investigation, insofar as they relate to the unaltered nickel‐iron, are consonant with the classification of Odessa as a coarse octahedrite (Og). Two (2) figures and 2 tables are given.
A Possible Meteorite Crater near Duckwater, Nye County, Nevada (ECN =+1157,387)
Authors: Rinehart John S. , Elvey C. T.
Published: June 2012

Abstract

A circular crater, known before 1936, near Duckwater, Nye County, Nevada (ECN = + 1157,387), some 225 feet in diameter and from 10 to 15 feet deep, which may be meteoritic in origin, is described. Altho extensive searches have been made, no meteoritic material has as yet been located in or near this crater.
A Reinvestigation of the Weaver Mountains, Arizona, Meteorite*
Authors: Henderson Edward P. , Perry Stuart H.
Published: June 2012

The Weaver Mountains, Arizona, meteorite has been reanalyzed. The new results confirm those of the previously reported analysis of this meteorite. The specific gravity first reported, 7.108, was found to be incorrect; this was redetermined and found to be 8.07. The Weaver Mountains meteorite has similar metallographic structures to the Babb's Mill, Tennessee, and the Shingle Springs, California, meteorites. These 3 meteorites are nickel‐rich ataxites, and the ground‐mass of each consists of imperfectly transformed γ‐α structures, in which occur small bodies of kamacite.
The “Josiah” and the “Joshua Bates” and the Meteoritic‐Dust Shower of November 14, 1856
Authors: Hoffleit Dorrit
Published: June 2012

Thru loose misquotations made some 25 years after the originally published facts in regard to the important shower of meteoritic dust that fell onto the ship Joshua Bates on November 14, 1856, the misconception has arisen that two such showers had been observed, the second in 1859. It is here shown that all of the references involved correspond to one and the same shower.
The Total Known Weight of the Cape York, Greenland, Sideritic Fall (ECN =+0650,760:)*
Authors: Leonard Frederick C.
Published: June 2012

The 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

In 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.
The Determination of the Co‐ordinates of a Meteor by Orthographic Projection*
Authors: Wylie Paul E.
Published: June 2012

A graphical method of solving the PZM or astronomical triangle is presented —one adapted particularly to observations of meteors.
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.
Shatter Cones at the Middlesboro Structure, Kentucky
Authors: DIETZ ROBERT S.
Published: June 2012

Abstract Shatter cones have been discovered in two residual boulders in the central uplift eye of the Middlesboro structure, Kentucky. This finding gives additional support to the interpretation of Englund and Roen (1962) that this is probably an astrobleme, i.e., an ancient meteorite impact scar.
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.
The Belle Plaine III Meteorite
Authors: GILLERMAN ELLIOT , HILL WALTER E.
Published: June 2012

Abstract The Belle Plaine III meteorite is one of three meteorites, all of about the same size, found within a 2 mile strip southeast of Belle Plaine, Kansas. The meteorite weighs 23.9 kg, and consists of about 28% metallic minerals and 72% silicates. Nickel‐iron, magnetite, hypersthene and olivene are the major constituents. The meteorite is an olivene‐hypersthene chondrite.
Lanai Meteorite Crater Apparently Myth
Authors: BARRINGER BRANDON
Published: June 2012

Abstract A survey by air and on the ground revealed no depression at the place supposedly called Ka‐imu‐hoku, Hawaiian for “The Star Oven”, on the island of Lanai. It had been reported as a “pit in the sand” or “the place where a meteor fell”. Reasons are given for believing the name was based on native observation of a nineteenth century fireball.
A Crater Formed by Gas Erosion of a Nuclear Explosion Vent
Authors: HANSEN SPENST M.
Published: June 2012

Abstract The PALANQUIN experiment was a 4.3 kiloton nuclear explosion detonated at a depth of 280 feet (85.3 m) in layered trachytic volcanic rocks at the Nevada Test Site. The resulting apparent crater had an unusual conical shape and dimensions of 119.1 feet (36.3 m) radius, and 78.8 feet (24.0 m) depth. The crater volume was 46,800 cubic yards (35,570 cubic meters).
La Malbaie Structure, Quebec—A Palaeozoic Meteorite Impact Site
Authors: ROBERTSON P. B.
Published: June 2012

Abstract Evidence in support of an origin by meteorite impact has been found at La Malbaie structure, 105 km northeast of Quebec City on the north shore of the St. Lawrence River. The structure has a central peak (Mont des Eboulements) 2500 feet (780 meters) above sea level, surrounded by lower hills and a semicircular valley with a diameter of 35 km. The circularity is incomplete as the peripheral valley terminates to the south and east at the St. Lawrence River which obscures an estimated 40 per cent of the crater. Rocks within the crater comprise charnockitic and granitic gneisses, anorthosite and gabbro of Precambrian Grenville age, and Middle Ordovician limestone.
The Oshkosh Meteorite
Authors: READ WILLIAM F.
Published: June 2012

Abstract In the fall of 1961, fragments of an olivine‐bronzite chondrite were found about 2 miles NNW of Oshkosh, Wisconsin, the total weight being 144.8 g. This paper fixes the exact location and describes the circumstances of the find.
THE LADDER CREEK, HORACE, AND TRIBUNE METEORITES (GREELEY COUNTY, KANSAS)
Authors: Mason Brian
Published: June 2012

The Ladder Creek, Horace No. 1, Horace No. 2, and Tribune meteorites were found within a comparatively small area of Greeley County, Kansas, between 1937 and 1958. Microscopic examination and analyses of the principal minerals show that Ladder Creek, Horace No. 2, and Tribune are essentially identical in composition and structure; it seems reasonable to conclude they are fragments of a single meteorite, a hypersthene chondrite. Horace No. 1 is essentially different, being a bronzite chondrite, and is evidently a distinct fall. The name Ladder Creek should be used for specimens previously called Horace No. 2 and Tribune, and the name Horace should be used for specimens previously called Horace No. 1.
THE CURATOR'S DILEMMA
Authors: Hey M. H.
Published: June 2012

The curator of any collection of meteorites has an unenviable task in deciding whether, and on what terms, he should supply material for destructive study. Some relevant considerations and the policy adopted by the British Museum are outlined.
CHEMICAL ANALYSES OF THE MURCHISON AND LOST CITY METEORITES
Authors: Ehmann W. D. , Gillum D. E. , Morgan J. W. , Nadkarni R. A. , Rabagay T. V. , Santoliquido P. M. , Showalter D. L.
Published: June 2012

The abundances of 22 elements have been determined in the recently fallen Murchison and Lost City meteorites. Analyses were performed by 14‐MeV neutron activation, thermal neutron activation, and in a few cases by wet chemical techniques. On the basis of these data the composition of the Murchison chondrite is intermediate between previously reported analyses of Type II and Type III carbonaceous chondrites. The data for the Lost City chondrite in general agree well with mean values reported for H‐group ordinary chondrites. The low oxygen content of the Lost City chondrite suggests that previously reported oxygen abundances in H‐group falls may be too high due to oxidation in storage or weathering prior to collection
THE BORGO SAN DONINO METEORITE: MINERALOGY AND CHEMISTRY
Authors: Baldanza B. , Levi‐Donati G. R. , Lewis C. F.
Published: June 2012

The principal data are collected about the fall, April 19, 1808, and the distribution of the fragments of the Borgo San Donino, Italy, meteorite (long. 44° 52′ N.; lat. 11° 03′ E.). An Almost complete individual, weighing 447 g is described in some detail. Crust morphology, mineralogical composition, chemical composition and petrology were studied. Optical data were established by microscopic analysis of both thin and polished sections. The Borgo San Donino is an ordinary LL‐group chondrite, with a fundamentally hypochondritic texture and evident features of recrystallization and metamorphism. The presence of some anomalous chondrules is discussed
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 + 8.700

where 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 unsatisfactory

With 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.
THE COMPOSITION OF THE JOHNSTOWN METEORITE
Authors: Mason Brian , Jarosewich E.
Published: June 2012

A new analysis of the Johnstown meteorite, a hypersthene achondrite, gives the following results (weight percent): SiO2 53.48, TiO2 0.12, Al2O3 1.43, Cr2O3 0.83, FeO 15.63, MnO 0.54, MgO 25.87, CaO 1.40, Na2O 0.04, K2O 0.00, P2O5 0.00, H2O+ <0.1, H2O‐ 0.05, Ni <0.05, Co <0.01, FeS 1.18, sum 100.57. Published and unpublished data on minor and trace elements in the bulk meteorite and in the pyroxene are presented in tabular form.
MOUNTING PROBLEMS IN THE NAMING OF METEORITE DISCOVERIES
Authors: Huss Glenn I.
Published: June 2012

One of the most important steps in the recovery and study of meteorites is the concise naming of each fall so that confusion of one fall with another is avoided. The presently‐used system of naming meteorite falls has been arrived at through an evolutionary process spurred on by necessity. The evolutionary history of the naming of meteorite falls is briefly sketched. Current naming practices are defined and the mounting problems of the present system are discussed. Measures for forestalling growing confusion in the naming of contiguous and overlapping falls, based upon a partial survey of curators of meteorite collections, are presented. A suggestion for the elimination of confusion in the dating of meteorite discoveries is included
A NEW CUTTING TECHNIQUE FOR METEORITIC IRONS
Authors: Buchwald V. F.
Published: June 2012

Small iron meteorites may be cut with high‐speed plastic‐bonded carborundum wheels, with hacksaws or automatic modifications of these, and with carbide‐tipped wheels; to date, no simple method has been available for cutting large iron meteorites. The successful sectioning of a 20‐ton meteorite involved the use of a mason's wire‐saw, fed with a slurry of carborundum‐grit. The slab produced measured 1.8 × 1.3 × 0.05 m and could be ground and polished for deep‐etching, with a minimum of weight loss.
THE SEARCH FOR A LARGE METEORITE NEAR PRINCE GEORGE, BRITISH COLUMBIA
Authors: Halliday Ian , Blackwell A. T.
Published: June 2012

A meteoritic event was observed from the vicinity of Prince George, British Columbia, at 5h 58m U.T., August 21, 1969, and an associated ground impact wave was recorded by several seismograph stations. An analysis of the visual and seismic data indicates that a mass of several tons must have reached the ground about 20 km southeast of Prince George. A helicopter search of the area and a study of aerial photographs have failed to locate the impact site
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 content

The 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.
A NEW OLIVINE‐BRONZITE CHONDRITE FROM DE KALB, MISSOURI
Authors: Read William F.
Published: June 2012

In the spring of 1969, an olivine‐bronzite chondrite weighing approximately 575 g was found within the city limits of De Kalb, Missouri. Though the discovery site is only 3 miles west of the known area of Faucett meteorites, “De Kalb” is shown in this paper to represent a distinct fall
A PRELIMINARY SORTING‐OUT OF “NESS COUNTY” METEORITES
Authors: Read William F.
Published: June 2012

With the exception of a distinctive olivine‐bronzite chondrite recognized by H. H. Nininger: “Ness County (1938)”, most of the numerous stony meteorites found in Ness County, Kansas, have been lumped together under the designation “Ness County (1894)”. It is the purpose of this paper to show that at least three separate falls are covered by this name
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 matrix

Major 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 monosulfide

The 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 meteorites

Based 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
THE GOSNELLS IRON — A FRAGMENT OF THE MOUNT DOOLING OCTAHEDRITE
Authors: De Laeter J.R. , McCall G.J.H. , Reed S.J.B.
Published: June 2012

A 1.5 kg iron found in 1960 at Gosnells, near Perth, Western Australia, belongs to Wasson's chemical group I‐An3 and is structurally unusual, being best described as a heat‐altered granular coarse octahedrite. It is chemically and structurally very similar to the Mount Dooling iron, found in 1909 about 400 km away, and has a fracture surface which fits the Mount Dooling mass very closely. The Gosnells fragment was probably transported by human agency, though it is not known when or by whom.
NIOBIAN RUTILE IN AN APOLLO 14 KREEP FRAGMENT
Authors: Hlava P. F. , Prinz Martin , Keil Klaus
Published: June 2012

Niobian rutile was found in a KREEP lithic fragment of basaltic texture. The niobian rutile contains 85.3% TiO2, 7.1% Nb2O5, 2.65% Cr2O3, 0.70% ZrO2, 0.61% SiO2, 0.82% Al2O3 0.61% FeO, 0.52% CaO, 0.22% V2O3 in addition to minor amounts of MnO, MgO, and CeO2. Rare earth elements were not detected, in contrast with lunar niobian rutile of Marvin (1971). Coexisting minerals in the KREEP fragment are major amounts of plagioclase and orthopyroxene, and minor amounts of olivine, ilmenite, augite, barian K‐feldspar, whitlockite, troilite, Ni‐Fe, zirkelite and chromite
THE ORO GRANDE, NEW MEXICO, CHONDRITE AND ITS LITHIC INCLUSION
Authors: Fodor R. V. , Keil Klaus , Jarosewich Eugene
Published: June 2012

The Oro Grande, New Mexico, U.S.A., chondrite was found in 1971. Electron microprobe analyses and microscopic examination show the following mineralogy: olivine (Fa 19.3 mole percent), orthopyroxene (Fs 16.2 mole percent), diopside, feldspar (An 13.6 mole percent), chlorapatite, whitlockite, kamacite, taenite, troilite, chromite, and an iron‐bearing terrestrial weathering product. A bulk chemical analysis of the meteorite shows the following results (weight percent): Fe 0.84, Ni 1.46, Co 0.07, FeS 3.62, SiO2 34.18, TiO2 0.14, Al2O3 1.83, Cr2O3 0.55, Fe2O3 21.25, FeO 9.13, MnO 0.31, MgO 21.52, CaO 1.72, Na2O 0.70, K2O 0.08, P2O5 0.25, H2O+ 2.14, H2O‐ 0.40, C 0.22, Sum 100.41. On the basis of composition and texture, the Oro Grande meteorite is classified as an H5 chondrite. A large lithic fragment (∼5 mm long) with a very fine‐grained texture different from that of the host meteorite was analyzed for bulk composition using the broad beam of an electron microprobe, and was found to be enriched in Ca, Al, Na, and K, and depleted in Mg and Fe relative to the bulk composition of the host meteorite. Its mineral compositions, however, are very similar to those of the host. It is suggested that the fragment is not a xenolith of a previously undescribed type of achondrite, but is probably an impact‐produced partial melt of the host chondrite or a fragment of an unusually large chondrule.
THE HAVERÖ UREILITE*
Authors: Neuvonen K.J. , Ohlson B. , Papunen Heikki , Häkli T.A. , Ramdohr Paul
Published: June 2012

The Haverö ureilite fell on August 2, 1971 on the Island of Haverö, Finland, lat 22° 03‘ 43“ E., long 60° 14’ 44” N. The meteorite contains curved open fractures partly filled with kamacite foils or drops, clusters of olivine mosaic with preferred orientation, very fine‐lamellar polysynthetic twinned clino‐***bronzite and carbonaceous matter as laths up to 4 mm in length. The carbon laths are in preferred orientation and contain in addition to graphite, kamacite, chromite and diamonds. The petrology, textural features and origin are discussed.
COSMOGENEIC RADIONUCLIDES IN THE HAVERÖ METEORITE
Authors: Cressy P. J.
Published: June 2012

An 87‐gram sample of the Haverö ureilite has been analyzed by non‐destructive gamma‐ray spectrometry. The results of the measurements, in dpm/kg at time of fall, are: 22Na, 71 ± 3; 26Al, 43 ± 3; 46Sc, 3.4 ± 2.1; 54Mn, 35 ± 6; 60Co, 0.7, 2*** limit. Haverö has 77 ± 14% of the 26Al activity calculated for its chemical composition. When averaged with previously‐reported analyses of Goalpara and Novo Urei, ureilites as a class have 74 ± 7% of their expected 26Al activity. The depletion in 26Al could be the coincidental result of identical “shielding” effects in three meteorites of apparently very different preatmospheric sizes. Alternatively, ureilites may have been exposed to a lower cosmic‐ray flux than that experienced by most chondrites, probably the result of characteristically different orbits
MORPHOLOGIES OF IRON CRYSTALS FROM THE HAVERÖ METEORITE
Authors: Jedwab Jacques
Published: June 2012

Studies of unpolished chips of the Haverö meteorite using the scanning electron microscope (SEM) and the electron microprobe (EMP), show two types of metallic iron particles: A, discrete convex globules of 5 to 50 microns made up of lamellae and interlocked grains, evenly interspersed among the matrix; B, flattened contorted crystals, less than one micron, lining the iron globules and cavities in the silicates or forming rounded spiny bodies. This second type of iron is interpreted, according to the current theory, as resulting from the in situ reduction of iron‐magnesium silicates
FORMS OF CARBON IN THE NEW HAVERÖ UREILITE OF FINLAND
Authors: Vdovykin Gennady P.
Published: June 2012

Based on its mineral composition and structure the Haverö meteorite, which fell on August 2, 1971, in Finland, is a ureilite, the sixth meteorite in this rare group. Elementary carbon in this meteorite is represented by diamond, lonsdaleite, graphite and chaoite microcrystals in the intergrowths. The presence of lonsdaleite and chaoite indicates that diamonds were formed in the Haverö meteorite due to the action of strong shock waves
ARGON‐37, ARGON‐39, AND TRITIUM RADIOACTIVITIES IN THE HAVERÖ METEORITE
Authors: Fireman E. L. , Spannagel G.
Published: June 2012

The 37Ar and 39Ar radioactivities were measured in a dissolved and in a melted sample of Haverö. The 37Ar in the metal was 12.4 ± 2.6 dpm/kg (Fe + Ni). The 39Ar in the metal was 49.3 ± 5.5 dpm/kg (Fe + Ni). The 37Ar activity is within 30 percent of that in the Lost City meteorite, while the 39Ar activity is a factor of two higher than in Lost City. The similarity in the 37Ar activities of the metal of the two meteorites indicates that these two bodies had similar preatmospheric sizes. The higher 39Ar activity in the metal of Haverö indicates that the aphelion of Haverö's orbit was at least 4.3 A.U. The 3H radioactivity in Haverö was measured to be 415 ± 30 dpm/kg. The 3H activity combined with the 3He content gives a 3He/23H exposure age for Haverö of (29.5 ± 2.5) X 610 years.
ELEMENTAL ABUNDANCES IN THE HAVERÖ METEORITE
Authors: Gillum D. E. , Janghorbani M. , Miller M. D. , Chyi L. L. , Ehmann W. D.
Published: June 2012

Abundances of 15 major, minor and trace elements have been determined in powders and interior chips derived from the Haverö ureilite. The values are in close agreement with mean values for other ureilites, as reported in the literature. The powdered samples exhibited slightly higher abundances of O and Si, than the interior chips. It is suggested that this may be due to alteration of the samples during the powdering process
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.
GRAVITY RECONNAISSANCE AT THREE MAURITANIAN CRATERS OF EXPLOSIVE ORIGIN
Authors: FUDALI R. F. , CASSIDY W. A.
Published: June 2012

We have carried out reconnaissance gravity surveys across three Mauritanian craters: Aouelloul, an undoubted meteorite crater; Tenoumer, a probable meteorite crater with a unique array of concentric dikes on its outer rim flanks containing xenoliths of country rock showing abundant shock artifacts; and Temimichat Ghallaman, a crater of possible meteorite impact origin. All three have residual negative gravity anomalies associated with their interiors. In all cases the gravity values return to “normal” immediately outside their rims. At Tenoumer the anomaly has the form and magnitude expected for a meteorite crater which has been subsequently in‐filled with unconsolidated sediments to the level of the surrounding country. Maximum depth from the present crater floor to the bottom of the sedimentary fill (top of the original crater floor) is at least 750 feet. With a rim‐rim diameter of 6,300 feet, the origin depth/diameter ratio of about 1:8 is virtually identical with that of Meteor Crater, Arizona. Temimichat, with a rim‐rim diameter of 2,100 to 2,400 feet, is somewhat larger than has been previously reported. If it is meteoritic in origin the gravity data dictate a surprisingly shallow structure, with a depth from the present floor to the original crater floor of 150 feet maximum and an original depth/diameter ratio of 1:15. No positive evidence for an impact origin has yet been found for Temimichat. Aouelloul is also larger than generally reported, with a rim‐rim diameter averaging 1,275 feet. As for Temimichat the gravity data dictate a remarkably shallow structure having a depth/diameter ratio of about 1:13. The combination of a shallow depth and a reasonably high rim apparently requires a scaled depth of burst for the impact event substantially in excess of 0.50, a value previously considered a maximum for explosive impacts. The morphological resemblance between Temimichat and Aouelloul is striking but, without additional evidence, this fact alone cannot be used to infer a similar origin.
A POSSIBLE RECENT METEORITE IMPACT SITE NEAR THE BORDER BETWEEN ZAMBIA AND MALAWI
Authors: MOSSMAN DAVID J.
Published: June 2012

A crater, 80 m diameter by 6 m deep, was created in 1959 on the Nyika Plateau between Zambia and Malawi. It may have been the result of a meteorite.
MAGNETISM OF METEORITES: A REVIEW OF RUSSIAN STUDIES
Authors: Herndon J. M. , Rowe M. W. , Larson E. E. , Watson D. E.
Published: June 2012

We present here a summary review of the work of Russian scientists, primarily Gus'kova and Pochtarev, on the magnetism of meteorites. They have measured the initial natural remanent magnetization and the magnetic susceptibility in more than 900 meteorite samples from collections throughout the Soviet Union. More sophisticated studies, involving both thermal and alternating field demagnetization experiments, were also conducted on a few samples. Meteorites almost invariably retain evidence of ancient magnetic fields in their pre‐terrestrial history
THE MUNDRABILLA METEORITE SHOWER
Authors: DeLaeter J. R.
Published: June 2012

A detailed examination of the geographical location, external appearance, microstructure and chemical composition of the Loongana Station, Mundrabilla and Premier Downs siderites has led to the conclusion that they are all members of the one meteorite shower. The cobalt, nickel, gallium and germanium contents of four of these meteorites have been measured by X‐ray fluorescence spectrometry and this data enables them to be classified as anomalous, but probably related to Chemical Group I
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.
QUARTZ AND FELDSPAR GLASSES PRODUCED BY NATURAL AND EXPERIMENTAL SHOCK
Authors: Stöffler Dieter , Hornemann U.
Published: June 2012

Refractive index, density and infrared absorption studies of naturally and experimentally shocked‐produced glasses formed from quartz, plagioclase, and alkali‐feldspar confirm the existence of two main groups of amorphous forms of the framework silicates: solid‐state and liquid‐state glasses. These were apparently formed as metastable release products of high‐pressure‐phases above and below the glass transition temperatures. Solid‐state glasses exhibit a series of structural states with increasing disorder caused by increasing shock pressures and temperatures. They gradually merge into the structural state of fused minerals similar to that of synthetic glasses quenched from a melt. Shock‐fused alkali feldspars can, however, be distinguished from their laboratory‐fused counterparts by infrared absorption and by higher density. It is concluded from recovery shock experiments on single crystals that solid‐state glasses are formed by shock pressures between about 300 and 450 kb (feldspars) and 350 and 500 kb (quartz), whereas pressures exceeding some 430 kb (feldspars) and 500 kb (quartz) are necessary to produce liquid‐state glasses
ON THE BRITTLENESS OF GIBEON METEORITIC IRON
Authors: Auten Thomas A.
Published: June 2012

The iron‐nickel alloy of the Gibeon octahedrite exhibited a transition from the normal ductile behavior to brittle behavior in tensile tests conducted below 103 °K. This result contradicts data published previously and implies that a temperature‐induced transition could explain the fragmentation of a large parent metallic mass into meteorite‐sized objects, since the micro‐structures of existing octahedrites are consistent with brittle rather than ductile fracture events. Examination of the fractures and microstructures of the tensile specimens affirmed that the observed transition is consistent with meteoritic structures. It is concluded that the mechanical properties of Gibeon meteoritic iron are compatible with both the solid iron core and the metallic “raisin” models for the structure of the parent planet with respect to fragmentation mechanisms.
PREPARATION OF ULTRA SMALL SAMPLES FOR OPTICAL AND MICROPROBE ANALYSIS
Authors: Inman Clarissa S.
Published: June 2012

This paper describes a simple but satisfactory new method for the preparation of tiny, varied and specialized specimens for electron or ion‐microprobe analysis developed over the past five years. Microtektites, individual chondrules, single grains, blebs from lunar samples and meteoritic minerals have been prepared by this technique. A description of the preparation of these usually difficult samples from the initial mounting through the various polishing steps to their final polish is presented in detail. The procedures used to prevent any contamination of these specimens by the polishing agents and to prevent cross contamination to the other samples used for geochronology studies are presented.
THE WILLOWBAR METEORITE*
Authors: Lange David E. , Moore Carleton B. , Rhoton Kendall
Published: June 2012

The Willowbar, Oklahoma meteorite was found by Kendall Rhoton in December, 1971, lat 36° 44′ N.; long 102° 12′ W. It is a shocked brecciated L6 chondrite (Fa‐24.3) with large black veins cutting areas of normal chondritic texture. It weighed 2.07 kg.
METEORITIC METAL IN APOLLO 16 SAMPLES
Authors: Reed S. J. B. , Taylor S. R.
Published: June 2012

One hundred metallic particles from Apollo 16 soils (61181, 65701) and rocks (60018, 60315, 66055) have been investigated microscopically and by electron microprobe analysis. Their cobalt content indicates a meteoritic origin for all but one particle. However, most contain more phosphorus than typical meteoritic metal, possibly due to the reduction of phosphates in the lunar rocks. Compositions of coexisting kamacite and schreibersite indicate temperatures of about 550–650°C which are thought to have occurred during metamorphism. The bulk nickel content of the lunar metal is somewhat low by comparison with most iron meteorites or the metallic component of common stony meteorites. However, this may be due to compositional changes that occurred after emplacement in the lunar surface layer.