bluuebunny/crossref_metadata_2025 huggingface dataset:
Are stumps important for the conservation of saproxylic beetles in managed forests? – Insights from a comparison of assemblages on logs and stumps in oak‐dominated forests and pine plantations
Authors: BRIN ANTOINE , BOUGET CHRISTOPHE , VALLADARES LIONEL , BRUSTEL HERVÉ
Published: June 2012

Abstract.  1. The expanding interest in harvesting stumps for bioenergy may represent a potential threat to forest biodiversity. Whereas stumps are common in managed stands, knowledge of their associated saproxylic assemblages is still incomplete.

2. We used emergence traps to sample saproxylic beetle assemblages in oak and pine large‐diameter (>20 cm) logs and stumps and compared the assemblages from the two sources.

3. With 64–84.5% of the species pool in oak and pine, respectively, stumps definitely constituted a suitable substratum for many saproxylic species in managed forests. Higher species density suggested that stumps are more diverse habitats than logs. Stumps also host rare species and natural enemies of bark beetles. For both tree species, the assemblage composition was significantly different between logs and stumps. The dissimilarity between substratum types was predominantly due to turnover, especially for oak.

4. Our results revealed that not only do stumps constitute a substitute for some log‐dwelling species; they also provide a suitable breeding substratum for many species that may be at risk in case of massive exportation of stumps for bioenergy purposes.
The Determination of the Age of Iron and Stony Meteorites from their Radioactivity*
Authors: Evans Robley D.
Published: June 2012

Abstract

Observed meteor and meteorite velocities (Öpik, Boothroyd) indicate that a small fraction, perhaps in the neighborhood of 15 percent, of all meteorites striking the earth are of extra‐solar origin. Helium‐radium age measurements (Paneth, Urry, & Koeck) on 23 iron meteorites, none of which was of known heliocentric velocity, disclose a uniform distribution of last‐solidification ages with no ages clearly greater than the age of the earth. Thus, either the specimens are all from the solar system, as Paneth proposed, or the galactic system is of the same age as the earth. Two critical experiments are in progress, based on the following evidence. The abundance‐ratio of the C, O, Si, Cl, Fe, Co, and Ni isotopes in meteorites has been studied by various workers, and is found to be the same as in the terrestrial elements. Moreover, the ratio of the two independent isotopes of uranium, 92U235 and 92U238, is the same in all terrestrial specimens, regardless of the geologic age of the mineral in which they are found. It is therefore taken as a reasonable premise, but regarded as a working assumption only, that the original isotopic ratio of any element is a constant of nature and is independent of its place of origin in the galactic system. Measurements of the actinouranium vs. uranium I activity‐ratio, and of the specific activity of potassium, are in progress on stony meteorites selected for their known heliocentric velocities. Some of these are of extra‐solar origin while others are solar‐system meteorites. The final results of the analyses give the difference between the age of the atoms in the meteorites and the same type of atoms in the earth. The method is independent of all influence from varying chemical and physical conditions during the history of the meteorite, as it deals entirely with isotopic ratios. The study of both the AcU, UI ratio and the K40, K41 ratio provides an independent check on the basic assumption of the method. The apparatus, technique, and mathematical background for these experiments are fully described. The announcement of the numerical results of these analyses is deferred until all the observations and control runs have been repeated many times, in order to assure their complete reliability.
On the Meteoritic Origin of the Black Stone of the Ka'bah
Authors: Khan Mohd. A. R.
Published: June 2012

Abstract Various descriptions and a history of the Black Stone of the Ka'bah, and speculations as to its nature and origin, are included in this paper. In the opinion of the writer, many people would prefer to assume that the tradition about the Stone's having been brought by the Angel Gabriel and given to Abraham and Ishmael for setting in a wall of the Ka'bah, arose out of an attempt to explain its witnessed fall as an aërolite, which may have happened not long before the first recorded rebuilding of the Ka'bah.
The Pantar, Lanao, Philippine Islands, Meteorite
Authors: Nininger H. H.
Published: June 2012

Abstract A 2,320‐gram aërolite which was observed to fall on June 16, 1938, at Pantar, Lanao, Philippine Islands, by Mr. R. H. Wygle, is described as being of the ordinary chondritic variety. Mr. Wygle was extremely fortunate also in securing a photograph (herewith reproduced) of the dust cloud which appeared in the wake of the meteorite. There was a press report to the effect that, at the time of the fall of the meteorite, many small particles fell like rain onto the metal roofs of several houses. There is no reason to doubt this report, for a similar occurrence has been recorded in connection with at least four North‐American falls. That this phenomenon is in some way related to meteoritic clouds is reasonable to assume. If the connection is established, then ordinary meteoritic showers will have to be reckoned, probably in tons, instead of grams, of material!
Taenite*
Authors: Buddhue John Davis
Published: June 2012

Abstract

Taenite is really 2 substances. Of these, orthotaenite is a nickel‐rich alloy whose composition is uncertain but seems likely to be Fe2Ni. This formula is based on a statistical study of 26 analyses, and the fact that the iron‐nickel frequency diagram has maxima indicative of this composition. The other constituent, metataenite, is a duplex substance composed probably of an intergrowth of orthotaenite and kamacite. In 9 (1 doubtful) out of 12 octahedrites examined, the taenite lamellae were composed of a dark central band of metataenite, with a band of orthotaenite on either side. The bands are either too thin or too thick to show this arrangement in the other 3 cases. The orthotaenite results from diffusion of nickel from the kamacite, while metataenite is a plessite‐like residue left between the bands, but, because of a higher nickel content, is much finer‐grained than plessite. Metataenite is, nevertheless, more soluble than orthotaenite. The black color is due to the removal of the more soluble constituent (kamacite) by the acid. The resulting surface is optically equivalent to a powder, and hence dark‐colored. The separation of taenite lamellae from Canyon Diablo, Arizona, into 3 layers was accomplished, and the thicknesses of the whole lamella and the 3 constituent layers are given.
An Astronomical Theory of Tektites*
Authors: Rufus W. Carl
Published: June 2012

It is supposed that the small, natural‐glass bodies known as tektites were originally derived in major part from the glassy basalt, or tachylyte, which forms the deeper crustal layer of the earth, exposed chiefly on the floor of the Pacific basin, at the time of the fissional separation of the moon; furthermore, that the earthly tektites represent only a small section of the vast swarms of tiny satellites which remained revolving about the earth within the Roche limit, and particularly that section of the satellites having a revolutional period closely coinciding with the period of the earth's rotation. Such swarms would have remained approximately above the Pacific basin, but would have gradually fallen behind and tended to be drawn to the earth, on account of perturbations resulting from the gradual retardation of the moon. Cumulative perturbations and other related factors have caused swarms of these bodies to come down to the earth at widely separated geologic periods in the earth's history, such falls having been particularly extensive along a great‐circle route crossing the western edge of the Pacific basin. This circumstance would account for the great quantity and wide distribution of the Indo‐malaysian tektites ***espeoially, which are of almost identical chemical composition, while other showers of tektites came at different geologic periods and varied somewhat in composition and physical appearance.
A New Type of Nickel‐Iron Meteorite from the Vicinity of the Arizona Meteorite Crater*
Authors: Nininger H. H. , Webb Robert W.
Published: June 2012

Among the meteorites gathered in the vicinity of the Arizona Meteorite Crater, a few individuals have been found whose etching pattern differs markedly from that of the typical Canyon Diablo irons; and chemical analysis reveals a considerably higher content of nickel: about 8.4%. According to accepted methods of identification, these distinctive individuals are regarded as belonging to a different type of meteorite. The majority of the irons of this new type show striking deformation of the kamacite plates, a feature almost unknown in the usual Canyon Diablo irons. An explanation for this is offered. It is suggested that the new type of nickel‐iron meteorite from the region of Meteorite Crater be called Canyon Diablo, Arizona, No. 2.
Collecting Small Meteoritic Particles
Authors: Nininger H. H.
Published: June 2012

The importance of the showering of small particles associated with meteoritic falls is emphasized and some of the difficulties encountered by those who attempt to investigate the phenomenon are pointed out. A trial search for specimens at the site of the Holbrook, Arizona, fall of 1912 July 19, made in April, 1940, is described. 3 small aërolites with a combined weight of 0.0948 g., which were recovered in the course of the search, are recorded. The method of collecting specimens is described and a plan for obtaining a quantitative estimate of the total amount of material that fell in this shower is outlined.
Small Aërolites Recovered from the Site of the Holbrook, Arizona, Fall of 1912*
Authors: Leonard Frederick C.
Published: June 2012

This paper includes an account of the recovery and a description of 8 more aërolitic particles, ranging in weight from 0.0628 to 0.0074 g., that were recently collected from ant hills at the site of the Holbrook, Arizona, fall of 1912. (The total number of such specimens now known is 11.) All 8 of these particles were discovered by means of “alnico” magnets—4 of the little stones in the field and 4 of them in the laboratory. The latter were detected in a quantity of 5515 g. of the ant‐mound gravel that was brought home for examination, and all 4 of these were found in the material of the same jar, which contained 771 g. of this gravel. From the data available, the ratios of both the numbers and the weights of the terrestrial and the meteoritic stones are calculated and various other comparisons between the 2 kinds of particles are made. Probably the most significant conclusion is that completely incrusted aërolites, weighing down to 0.0074 g., not only have been demonstrated to exist but have actually been reclaimed at the place of the Holbrook shower.
The Schertz, Guadalupe County, Texas, Meteorite Proved Identical with Canyon Diablo, Arizona*
Authors: Monnig Oscar E.
Published: June 2012

The Schertz, Guadalupe County, Texas, iron meteorite of 308 g., which has been listed in two catalogs of Texas meteorites, resembles a typical Canyon Diablo, Arizona, iron. An investigation at Schertz and at other points in south Texas revealed that a large shipment of iron meteorites from Canyon Diablo was sent there about 1893, and that subsequently all of these irons were abandoned or lost except one piece of some 175 lbs., now at Yorktown, Texas. The so‐called Schertz iron is in all probability one of the samples of this shipment.
Concerning the Meteor Observed on January 30, 1868, which Fell through the Atmosphere as a Shower of Stones at Pultusk in the Kingdom of Poland*
Authors: Galle J. G.
Published: June 2012

This paper presents eyewitness accounts of the phenomena attending the fall of the Pultusk, Poland, meteorites. On the basis of the observational data thus provided, the real path and the heliocentric orbit pursued by the meteorites are determined.]
Some Symbols Recommended for Use in the Classification of Meteorites etc.
Authors: Leonard Frederick C.
Published: June 2012

ABSTRACT AND INTRODUCTION

In the first column of the following table are presented some symbols that the writer has found convenient in classifying meteorites etc. and that he would recommend to other workers. The majority of these symbols stand for various classes in the Rose‐Tschermak‐Brezina system of meteoritic classification1 and are accordingly but revisions of the rather unsatisfactory symbols already in use, while a few are innovations. In the second column of the table is given in each case the corresponding old symbol2 (if such exists) and in the third and last, the term that the preceding symbol or symbols characterize. It is recommended furthermore that all of the symbols in the forenamed system, other than those enumerated in the second column of the accompanying table, be left unchanged until such time as the whole system of classification may be revised.
The Eaton, Colorado, Meteorite: Introducing a New Type
Authors: Nininger H. H.
Published: June 2012

This paper contains an account of a 29.547‐g. coppery nugget reported to have been observed to fall in May, 1931, at Eaton, Weld Co., Colorado (coördinate number = 1047,405), that the writer is able to explain only on the hypothesis that the specimen is a meteorite of an entirely new type (copper‐zinc‐lead), coördinate with the sideritic variety (or nickel‐irons).
Remarks on Four Notes Recently Published by C. C. Wylie
Authors: La Paz Lincoln
Published: June 2012

ABSTRACT AND INTRODUCTION

The present communication, in so far as it relates to a note on contraterrene meteorites,1 is simply an elaboration of certain remarks which I made extemporaneously at the time the then Secretary, Dr. Robert W. Webb, read Dr. C. C. Wylie's paper at the Eighth Meeting of the Society for Research on Meteorites held in Flagstaff, Arizona, in June, 1941. In so far as this communication relates to three more recent notes on the mass of the meteorite responsible for the Canyon Diablo, Arizona, Meteorite Crater,2 it is intended to justify objections to Wylie's results already expressed in private letters to him.
A Study of the Multiple Meteoritic Falls of the World
Authors: Herrig George H.
Published: June 2012

The meteoritic falls of the world have been studied in an attempt to learn whether they support the hypothesis that a governing cause of multiple falls is the fact that stones are more friable than irons and are thus more likely to disintegrate under the effects of external forces. A statistical test has been applied to the data and has been found strongly to support this hypothesis.
The Formation of Meteoritic Iron Oxide
Authors: Buddhue John Davis
Published: June 2012

Meteoritic iron oxide occurs in three forms: coarsely lamellar, finely lamellar, and massive. The lamellar forms result from oxidation proceeding parallel to the surface of the metal. The thickness of the lamellae may be proportional to the rate of oxidation. Massive oxide results when electrolysis causes the oxide to invade the metal or when redeposition of dissolved oxide obliterates the original lamellar structure. The action of lawrencite produces a friable, porous type of oxide which is confined largely to specimens in collections. The effect of electrolysis on the differential oxidation of meteoritic minerals is briefly discussed. Three new analyses of meteoritic oxides (by F. G. Hawley) are given (Table 1).
Some Observations on the Soil near the Canyon Diablo, Arizona, Meteorite Crater
Authors: Buddhue John Davis
Published: June 2012

Four samples of soil from 2 places approximately 2 miles from the Canyon Diablo, Arizona, Meteorite Crater contain no nickel or fragments of oxide, but material resembling volcanic ash is fairly abundant. The pH of the soils is near 8.5. This mild alkalinity would tend to help the irons resist corrosion. One partial analysis is given.
An Announcement to Collectors of Meteorites concerning the Pantar, Lanao, Philippine Islands, Fall
Authors: Nininger H. H.
Published: June 2012

Herein is related how the aerolites from the Pantar, Lanao, Philippine Islands, fall of 1938 June 16 escaped the Japanese invasion of the Philippines. On behalf of Mr. H. J. Detrick, thru whose painstaking efforts the collection of these aerolites was made possible and the specimens themselves were preserved, an appeal is made to collectors of meteorites.
Comments on the Preceding Paper by Professor M. A. R. Khan
Authors: Kaplan Joseph
Published: June 2012

This communication presents comments on Professor M. A. R. Khan's paper concerning the possibility of detecting the strongest radiations of terrestrial polar auroras in the spectrum of the earthshine. It also suggests the desirability of photographing the Moon in infra‐red radiation corresponding to the O‐O band of the first positive system of N2. The possibility of extending Professor Khan's proposal by studying the lunar ionosphere and by studying other phenomena suggested by known solar‐terrestrial relationships is briefly discussed.
An Investigation of the Time Distribution of Meteoritic Falls by Years†
Authors: Russell John A.
Published: June 2012

An attempt is made in this paper quantitatively to remove the systematic human factors from the annual counts of observed meteoritic falls from 1790 to 1939, inclusive. The probability that the fluctuations remaining in the counts are due solely to errors of sampling is then determined. These remaining fluctuations are shown to be normally distributed, to a close approximation, except for the years 1868 and 1933.
A Possible Meteorite Crater in the Aleutians*
Authors: La Paz Lincoln
Published: June 2012

Neither theory nor the results of numerous observations made from military and commercial aircraft support the generally accepted belief that meteorite craters will prove to be quite easily discoverable by search from the air. As an indirect result of a campaign to discover new meteorite craters by air search, a possible meteorite crater on Amak Island in the Aleutians was reported by Charles Keenan, Second Batallion, 53rd Infantry, a member of the United States Ground Forces. All details concerning the location and nature of this Aleutian crater so far made available to me are presented in this paper.
The Rockwell Hardness of Siderites*
Authors: Bddhue John Davis
Published: June 2012

The Rockwell hardness of 22 siderites (nickel‐iron meteorites) was determined and found to range from 45T‐42 to 45T‐69 and from B‐60 to B‐92. Differences were found between the unaltered and the granulated parts of siderites with an alteration zone. Metal near nodules may differ from that farther away. Some experiments were made to determine the effect of heat on the hardness of siderites.
A Sieve Analysis of Crushed Sandstone from the Canyon Diablo, Arizona, Meteorite Crater
Authors: Buddhue John Davis
Published: June 2012

The impact of the Canyon Diablo, Arizona, meteorite crushed, but did not disperse, some of the white sandstone bedrock. An analysis of the particle‐size of this material is given. The finest particles are indistinguishable in size from particles of “rock‐flour.” The results of a “Photelometric” determination of the particle‐sizes in “rock‐flour” also are given.
The Furnas County Stone of the Norton County, Kansas‐Furnas County, Nebraska, Achondritic Fall (1000,400)*
Authors: Leonard Frederick C.
Published: June 2012

A preliminary account is given in this paper of a record‐breaking meteorite—the Furnas County member of the extraordinary Norton County, Kansas‐Furnas County, Nebraska, achondritic fall of 1948 February 18 (coördinate number = 1000,400). This specimen, discovered on 1948 August 16, is conservatively estimated to weigh 1 metric ton (2200 lbs.). If that estimate is correct, or nearly correct, then the Furnas County stone is by far the largest known aerolite in the world and the largest meteorite of any type ever observed to fall. Several other significant facts concerning this remarkable meteorite are noted and briefly discussed. The giant aerolite was recovered thru the combined efforts of the Institute of Meteoritics of the University of New Mexico and the University of Nebraska State Museum, which have acquired joint ownership of it.
A Simplified Classification of Meteorites and its Symbolism*
Authors: Leonard Frederick C.
Published: June 2012

An attempt is made in this paper to effect a simplification of the classification of meteorites and a revision of the symbols that pertain to it. Meteorites (symbol = Mi) are classified, first, into 3 divisions: aerolites (Ae), siderolites (So), and siderites (Si); second, into 7 classes: achondrites (A), chondrites (C), sideraerolites (S), lithosiderites (L), hexahedrites (H), octahedrites (O), and ataxites (D); and third, into 29 separately distinguishable subclasses, of which the symbol, in each case, indicates primarily the class to which the meteorite belongs. Table 1 is a list of 16 “Qualifying Symbols or Qualifiers”—single, lower‐case letters—used in connection with the symbols of the divisions, the classes, and the subclasses—in the last‐named case, to form the symbols of variants or secondary subclasses. Table 2, entitled “Subclasses of Meteorites and their Symbols,” gives the names of the subclasses and both their new and their old symbols. Several matters relating to this system of classification are discussed; the classificational sequence of meteorites, in terms of the 7 classes of meteorites, is reviewed in the light of it; and, finally, 3 recommendations are made concerning the system and its application to future studies of meteorites and meteoritic falls—in particular, statistical studies of the latter.
A Request for Information concerning Newly Reported Meteoritic Falls*
Authors: Leonard Frederick C.
Published: June 2012

The coöperation of all persons concerned, in supplying 7 essential items of information regarding newly reported meteoritic falls, is solicited, for the reasons stated.
Streak Meteors without Perceptible Nuclei*
Authors: Khan A. R.
Published: June 2012

The phenomena of streak meteors without perceptible nuclei are described, and a possible explanation of the phenomena is given.
The Meteorites of Santa Rosa de Viterbo, Boyacá, Colombia (730,059)*
Authors: Ramírez J. Emilio
Published: June 2012

In April, 1810, a large mass of nickel and iron was found by Cecilia Corredor, on Tocavita Hill, not quite a mile from the main square of the town of Santa Rosa de Viterbo, Department of Boyacá, Republic of Colombia. It was recognized as a meteorite by two fellow travelers, Mariano de Rivero and Jean Baptiste Boussingault, in 1823, who found it in the local smithy, where it was doing duty as an anvil. The history of this and another inseparable meteorite, known as Rasgatá, is outlined from that time up to the present, and some suggestions are made to eliminate the confusion that has prevailed regarding these two meteorites. Finally, two large specimens of meteorites found recently near Santa Rosa de Viterbo are described.
A Possible Meteorite Crater in Northeastern New Mexico
Authors: Lapaz Lincoln
Published: June 2012

This note presents a brief description of a possible meteorite crater found in northeastern New Mexico, in December, 1948, during an air search for another meteoritic fall.
On Naming New Subclasses of Meteorites
Authors: Leonard Frederick C.
Published: June 2012

It is proposed that any subclass of meteorite that may in future be required be named for the fall that proves to be the archetype of the subclass; e.g., if the Norton County, Kansas‐Furnas County, Nebraska (1000,400), fall of 1948 February 18 be found to represent a new subclass, this would well be termed nortonite, with the symbol A2no.
A Quantity for Evaluating the Effectiveness of Field Search in Meteoritics
Authors: Finnegan Bernard J.
Published: June 2012

The recovery index of a meteoritic shower is defined and its application is discussed.
The Mechanism of the Sounds from Meteors*
Authors: Barringer Brandon , Hart Harry C.
Published: June 2012

This paper reviews records of sounds from meteors that were heard simultaneously with the appearance of the meteors. Such sounds are carried presumably by electromagnetic waves. A number of different conceivable mechanisms for the generation of the radiation, which have the necessary characteristics, are considered. It is concluded that the most likely mechanism involves the radiation that originates in large numbers of air molecules that are ionized by the impacts of the invading meteorites.
Intensity Variations in the Spectrum of a Perseid Meteor*
Authors: Russell John A.
Published: June 2012

Abstract

Density measurements of the spectrum of a Perseid meteor reveal an increase in the strength of the K line of ionized calcium with respect to the neutral iron‐magnesium blend at 3830 A., particularly during bursts. The greater strengthening of high‐excitation lines relative to low‐excitation lines during bursts appears to be fairly general thruout the spectrum. Effective‐temperature determinations, based upon the relative intensities of certain iron multiplets, however, indicate lower excitation of iron vapor during bursts than between them. The effective‐temperature difference is of the order of 20° to 30° C.
The Chemical Composition and Some Physical Characteristics of Tektites
Authors: Hammond Charles R.
Published: June 2012

Abstract

Accurate density‐measurements are given for 2 australites and for 3 moldavites, and a chemical analysis, made of a moldavite, is compared with that of other tektites and with those of ancient and modern glasses. The chemical analysis is then used to approximate the coefficient of thermal expansion and other physical characteristics of tektitic material.
Trigonometric Criteria for Determining Whether Meteoritic Falls Lie on the Same Great Circle*
Authors: Leonard Frederick C.
Published: June 2012

Abstract

This paper is divided into 6 sections, of which an enumeration will constitute its abstract: (1) introduction; (2) trigonometric criteria for determining whether a given point Q lies on the great circle passing thru 2 other given points, A and B, of north pole P; (3) and (4) methods of determining the geographic coördinates of pole P; (5) determination of the distance of a given point R from the great circle; and (6) determination of the coördinates of point S, the point on the great circle closest to the given point R. Several subtopics are discussed in the notes to the paper.
The Lost Port Orford, Oregon, Meteorite (ECN =+ 1245,428:)*
Authors: Pruett J. Hugh
Published: June 2012

Abstract

In 1859, when Dr. John Evans, government geologist, was working in southwestern Oregon, he came upon an unusual rocky formation protruding from the ground. He reported the locality as “about 40 miles from Port Orford.” Specimens analyzed in New York and Vienna were found to be pallasite. Plans were made to move the mass, estimated to weigh 10,000 kg., to the Smithsonian Institution, but, before the expedition could be organized, Dr. Evans died. No one else could be found who knew the location of the find. The Smithsonian Institution has a small specimen of the original find weighing 28 gm. The large mass has not since been located, altho search parties are frequently in the field.
Meteor or Meteoric Cloud?*
Authors: Wylie C. C.
Published: June 2012

Abstract

A picture purporting to be a photograph of the great meteor of 1933 March 24 in flight was a photograph, not of the meteor itself, but of the meteoric cloud left in the wake of the meteor.
Observations on the Toluca, Mexico, Meteoritic Iron (ECN =+997,194)*
Authors: Beck Carl W.
Published: June 2012

Abstract

An interesting fragment of the Toluca, Mexico, sideritic shower (ECN = +997,194) is described. It is interesting from the viewpoint of the concentration of minor meteoritic constituents in abundance and from the viewpoint of structure. The principal constituent is kamacite, but the fragment contains macroscopically visible schreibersite, graphite, troilite, daubréelite, and lawrencite. One (1) figure and 4 tables are given.
The Spectrum of a Perseid Meteor of 1949*
Authors: Russell John A.
Published: June 2012

Abstract

A Perseid spectrum, obtained in 1949, is compared with 5 other Perseid spectra. Density measures for this spectrum indicate a marked increase in strength, during bursts, of the H and K lines of CaII relative to the strong neutral Fe and Mg line at 3830 A. The available data indicate tentatively that: (1) Perseid spectra resemble one another more than do type‐Y spectra as a whole; (2) the meteorites producing Perseid meteors are less diverse in composition than are aerolites in general.
A Method for Permanently Marking the Exact Locations of Meteorite Discoveries
Authors: Morley Russell A.
Published: June 2012

Abstract

A method for permanently marking the exact location of each meteorite discovered, and a plan for the construction and erection of a convenient type of permanent marker, similar to those in use by the United States Coast and Geodetic Survey, are described.
A Restudy of the Coolac, New South Wales, Australia, Meteorite (ECN =—1481,350)*
Authors: Henderson Edward P.
Published: June 2012

Abstract

A new analysis and a redetermination of the density of the Coolac, New South Wales, Australia, meteorite, which bring this iron into agreement with other meteorites of the same general type, are given. The Coolac meteorite resembles the Canyon Diablo, Arizona, irons. The presence of cohenite was confirmed, and the variation in the internal structure is well shown by the 4 accompanying illustrations (Figs. 1 and 2).
Oxidite or “Meteoritic Shale,” Terrestrialization, and Terrestrialite
Authors: Leonard Frederick C.
Published: June 2012

Abstract

The term oxidite is proposed to replace the synonyms meteoritic shale and iron‐shale. Terrestrialization means the terrestrial transformation of a meteorite into something that can no longer be properly regarded as being a meteorite, and terrestrialite signifies the product of that transformation. Both oxidite and meteorodes (defined in n. (3) to the paper) are varieties of terrestrialite.
Striated Surfaces on Meteorites: Shock Fractures, Not Slickensides
Authors: DIETZ ROBERT S.
Published: June 2012

Abstract Veined and brecciated chondrites commonly display striated fractures which have been interpreted as slickensides (fault dislocations). Observations on several such fractures in various collections suggest they are not true slickensides but, instead, are probably shock features related to shatter coning.
Temperatures of Meteoroids in Space
Authors: BUTLER CLAY P.
Published: June 2012

Abstract On the basis of reported optical measurements of iron and stony meteorites, upper and lower limits for solar absorptance and hemispherical emittance of the surfaces of meteoroids have been established. Temperatures of three classes of meteoroids, none larger than approximately 10 meters in radius, have been calculated for various orbits and a/e ratios. These classes are light chondrites, dark chondrites and the irons. Temperatures for a meteoroid in a Mercury orbit range from 100° C for a light chondrite to 400° C for an iron.
The Fremont Butte, Washington Co., Colorado, Meteorite
Authors: HUSS GLENN I. , MOORE CARLETON B. , BUSEK PETER R.
Published: June 2012

Abstract The Fremont Butte meteorite was found near Fremont Butte, Colorado, in 1963. A single individual was found weighing 6.6 kg. It is an olivine‐hypersthene or L group chondrite showing brecciation and a small number of well formed chondrules and olivine phenocrysts.
Jenkins: A New Iron Meterorite from Missouri
Authors: READ WILLIAM F.
Published: June 2012

Abstract Jenkins was found about 1946 and identified as a meteorite in 1965. The weight before sectioning was 122 lbs. It is a coarse octahedrite with irregular nodules of troilite and sizeable patches of graphite, schreibersite, and lawrencite.
A New Octahedrite from South Africa
Authors: COMERFORD MATTHIAS F. , CORKELL ROBERT H. MC , TISHLER SAMUEL W.
Published: June 2012

Abstract Examination of an iron meteorite found in South Africa discloses it to be a coarse octahedrite containing 6.90 weight‐percent nickel. The meteorite body contains several inclusions of troilite, or troilite plus graphite, and at least one of pure graphite veined with kamacite. Kamacite, cohenite, and phosphides are the other major constituents of the structure.
THE NEEDLES (CALIFORNIA) IRON METEORITE
Authors: Wasson John T. , Kimberlin Jerome
Published: June 2012

The Needles fine octahedrite, which weighs 45.3 kg, was found in 1962 in the Turtle Mountains, about 50 km SSW of Needles, California. It contains 10.3% Ni, 77 ppm Ga, 93 ppm Ge and 4.8 ppm Ir, and is a member of chemical group II D. It is rather similar to the Wallapai, Arizona, meteorite, and may possibly be a transported mass from this multiple fall. The compositional evidence slightly favors the interpretation that Needles is a distinct fall.
MICRO‐CHONDRULES
Authors: Levi‐Donati G. R.
Published: June 2012

Very small chondrules, which are less than 250μ in size and are referred to as microchondrules, were discovered in twelve chondritic meteorites. The morphology, composition, and structure of these microchondritic bodies are investigated. In particular, the description of the principal, minor, and accessory minerals is given in some detail. Microphotographs are presented which show the internal texture of the bodies and the integration between matrix and microchondrules. Several porphyritic microchondrules are completely surrounded by opaque minerals, and here the matrix‐chondrule integration is practically absent. A possible evolutionary sequence for microchondrules is discussed.
ELECTROLYTIC CORROSION OF IRON METEORITES
Authors: Tackett Stanford L. , Tucker Ray A. , Duncan Floyd R.
Published: June 2012

Six iron meteorites were electrolyzed and the resulting corrosion was studied by a potentiostatic technique. It was found that both iron and nickel in the kamacite phase dissolve, and that neither iron nor nickel dissolve from taenite. The rate of corrosion was shown to be inversely proportional to the nickel content. However, structure, as well as nickel content, plays an important part in the electrolytic process. The Coya Norte, Chile meteorite dissolved more rapidly and more easily (at a lower potential) than did pure iron even though the Coya Norte meteorite contains 5.5% nickel.
PETROLOGICAL CHARACTER OF THE LUNA 16 SAMPLE FROM MARE FECUNDITATIS
Authors: Wood John A. , Reid John B. , Taylor G. Jeffrey , Marvin Ursula B.
Published: June 2012

We have classified 1858 lithic and vitreous fragments from the Luna 16 core‐tube sample. They were taken from the soil fractions ranging in size from 150 to 425 μ, at levels A and G (γ). No important differences are observed between the proportions of particle types in levels A and G, nor between the soils of Luna 16 and those from the Apollo 11 landing site in the nearby Mare Tranquillitatis. Luna 16 basalts are texturally and mineralogically similar to Apollo 11 basalts, though the former are characterized by more Fe‐rich olivines and pyroxenes and by lower ilmenite contents than are Apollo 11 basalts. The atomic ratio Al/Ti in Luna 16 basalt pyroxenes in about 1.5; Apollo 11 basalt pyroxenes have Al/Ti = 2.0, indicating the possibility of a lower mean valence for Ti in the Luna 16 material than in the Apollo 11 material. Most light‐colored lithic fragments are anorthositic rather than noritic in character and are comparable to Apollo 11 anorthosites in mineral chemistry. We believe they are samples of terra regions to the north of the Luna 16 landing site. Triangular diagrams plotting normative plagioclase, normative mafics plus oxides, and normative orthoclase plus apatite neatly separate the three major types of lunar materials — mare basalts, anorthosites, and noritic rocks — and reveal that the Luna 16 regolith is composed of mare basalt and anorthosite, with very little norite component. Colorless‐to‐greenish glass occurs in the Luna 16 sample, which has high Fe and low Ti; it may represent gabbroic rock related to the anorthosites
PETROLOGICAL FEATURES OF SHOCK METAMORPHISM IN CHONDRITES: ALFIANELLO
Authors: Levi‐Donati G. R.
Published: June 2012

The Alfianello meteorite was inspected by optical microscopy, both by transmitted and reflected light, in order to look for evidence of shock metamorphism. The stone is a well‐recrystallized olivine‐hypersthene chondrite that shows unambiguous features of dynamic deformation. Some examples of planar deformation structures, which are notable in olivine and plagioclase feldspar crystals, are reported. The presence of several shock‐transformed components is described in some detail. Alfianello appears to belong to a class of chondrites lightly‐to‐moderately shocked.
THE CARBONACEOUS CHONDRITES—A SELECTIVE REVIEW
Authors: Mason Brian
Published: June 2012

The presently known carbonaceous chondrites are listed, and their densities and contents of Fe, Si, and Mg recorded. A review of classification schemes indicate that Wiik's (1956) division into Types I, II, and III reflects basic differences in chemical and mineralogical composition and structure, and is preferable to the Van Schmus‐Wood (1967) classification into C1, C2, C3, and C4 types. Renazzo is a Type II meteorite. The Van Schmus division of Type III meteorites into two subtypes is sustained, and is shown to involve not only textural differences but also differences in total iron content. The genesis of the different types of carbonaceous chondrites is ascribed to condensation in different temperature regions within the early solar nebula.
THE NAZARETH(b) METEORITE
Authors: Gooley R. , Lewis C. F. , Moore C. B. , Huss Glenn I.
Published: June 2012

The Nazareth(b) meteorite is a medium octahedrite found in 1968 near Nazareth, Texas. It contains 8.75% nickel and large schreibersite inclusions
THE CHEMICAL COMPOSITION OF THE HAVERÖ METEORITE AND THE GENESIS OF THE UREILITES
Authors: Wiik H. B.
Published: June 2012

The chemical composition of Haverö is presented and compared with the composition of the other five ureilites
ON NAMING METEORITES
Authors: Buchwald V. F. , Wasson John T.
Published: June 2012

To improve the labelling value of meteoritic names, new meteorites should be assigned geographical names which are not used for other meteorites, which are simple, and, if possible, of mnemonic value. A Committee on Meteoritic Nomenclature should be established to supervise the assignment of new meteorite names, and to assist in the work necessary to confirm that new meteorite finds are not paired with meteorites which were previously cataloged.
HAMMOND DOWNS, A NEW CHONDRITE FROM THE TENHAM AREA, QUEENSLAND, AUSTRALIA
Authors: Mason Brian
Published: June 2012

Among a collection of meteorites from the area of the Tenham shower (Queensland, Australia) was a 27 kg stone which proved to be different from the other Tenham stones. It is a bronzite, H4, chondrite, the principal minerals being olivine (average composition Fa 18.8), clinobronzite and bronzite (average composition Fs16.4), nickel‐iron, and troilite; it is considerably weathered, much of the nickel‐iron being converted to limonite. It has a highly chondritic structure, with devitrified glass within the chondrules, and without visible plagioclase. This meteorite was found about 1950 near the Hammond Downs station, hence the name; its coordinates are lat 25° 28′ S., long 142° 48′ E.
A NOTE ON THE MINERALOGY AND CLASSIFICATION OF THE VILNA METEORITE
Authors: Smith D. G. W. , Folinsbee R. E. , Hall‐Beyer M.
Published: June 2012

Electron microprobe analyses of olivine, orthopyroxene, clinopyroxene, plagioclase feldspar, chromite, whitlockite, apatite, troilite and metals indicate that the Vilna meteorite is a hypersthene chondrite belonging to the L5 or L6 subgroups.
THE NORTON COUNTY METEOROID: A CASE FOR STATISTICAL STUDY OF METEORITE FRAGMENTS
Authors: Lang Bruno , Liszewska Krystyna
Published: June 2012

The size distribution of 15,000 fragments from the Norton County meteorite was examined with size‐frequency histogram. The size is measured in phi units. The estimates of the moments β1 and β2 of the empirical distribution were used for approximating the latter with a theoretical frequency curve in terms of the Pearson system It was suggested that the beta distribution obtained from the Pearson system can be regarded as a superposition of two simpler distributions: a near to normal one, corresponding to a slower process of fragmentation, and a power‐law one, assumed to result from fast fragmentation process.

… All meteorite falls are important but some are more important than others …

… This fall was of outstanding importance because with its arrival the entire picture of the word meteorite as portrayed in the total of collections throughout the world was notably altered …

H. H. Nininger, 1949. Significance of the Norton, Kansas, meteorite in Transactions of the Kansas Academy of Sciences 52, 113.
FRACTIONATION OF MODERATELY VOLATILE ELEMENTS IN ORDINARY CHONDRITES
Authors: Wasson John T. , Chou Chen‐Lin
Published: June 2012

Observed differences in the abundance ratios of moderately volatile elements found in ordinary chondrites relative to CI chondrites may have resulted from a continuous loss of nebular gas from the ordinary‐chondrite formation region during condensation. If this occurred, the nebular volatility of these elements should be inversely correlated with their abundance ratios. Such a nebular gas loss can occur as a result of momentum exchange between solids and gases, as a result of interactions between the nebular gas and solar photons or particles at the surface of the nebula, or as a result of the settling of previously condensed solids to the median plane of the nebula.
NEW CHEMICAL ANALYSES OF SIX ACHONDRITES AND ONE CHONDRITE
Authors: McCarthy T.S. , Erlank A J. , Willis J.P. , Ahrens L.H.
Published: June 2012

Quantitative analytical data on 11 elements in chondrite Pampa del Infierno and achondrites Manegaon, Chassigny, Goalpara, Nakhla, Lakangaon and Shergotty are given. To our knowledge, Manegaon and Lakangaon have not been analysed before. Composition, assignment and origin of each meteorite are briefly discussed.
GLASS PARTICLES AND SHOCK FEATURES IN THE BUNUNU HOWARDITE
Authors: Noonan Albert F.
Published: June 2012

Glass particles have been separated from the Bununu howardite microbreccia and analyzed with the electron microprobe. Preliminary SEM studies of the glass reveal fragments, spherules, teardrops, and rods: particles reminiscent of glasses recovered from the lunar surface. When plotted, individual glass analyses from both the Bununu and Malvern howardites range through the howardite group and extend into the eucrite group with the average glass compositions slightly enriched in CaO and depleted in MgO when compared with the bulk chemical analyses. These glasses presumably represent quenched, impact‐melted rocks, or partial melts of the major rock types and/or matrix in Bununu and Malvern.

Shock‐produced features which have been observed in known terrestrial and lunar impact breccias are also present in Bununu. Crystal deformation, maskeylenite and glass veining in clasts and glass spherules and shards in the matrix point to impact brecciation as the likely mechanism to form the features observed in Bununu and other howardites.
THE ELLICOTT METEORITE
Authors: Olsen Edward J. , Huss Glenn I. , Pearl Richard M.
Published: June 2012

Two individual specimens (total weight 15.7 kg) of a new medium octahedrite were found near Ellicott, El Paso County, Colorado. The find is only 1.2 km from the find (in 1890) of the Franceville medium octahedrite. Ellicott and Franceville are distinct meteorites, the latter exhibiting pronounced differences in shock features, kamacite band width, and Ni, Ga, Ge, and Ir contents. Ellicott is a group IA iron while Franceville is in group IIIA.
THE MAGNETIC INVESTIGATION OF THE SIKHOTE‐ALIN IRON METEORITE SHOWER AT THE SITE OF FALL
Authors: Gorshkov E. S. , Gus'kova E. G. , Pochtare V. I.
Published: June 2012

Individual and splinter specimens of the iron meteorite shower of Sikhote‐Alin and rock samples from impact craters have been studied magnetically. The results indicate that: 1) Histograms for the distribution of natural remanent magnetization Jn of individual and splinter specimens are characterized by a high correlation coefficient (0.82 ± 0.06). For the splinter specimens, a trend to an increase in number of specimens with anomalously high Jn values is observed; 2) the Earth's magnetic field did not greatly affect the magnetic properties of this iron meteorite; and 3) for rock samples taken from different craters, there was found to be a relation between the natural remanent magnetization and the energy conditions of the crater formation.
MINERALOGY AND CHEMISTRY OF THE ASHMORE CHONDRITE
Authors: Bryan W. B. , Kullerud G.
Published: June 2012

The Ashmore olivine‐bronzite chondrite is a group H, type 5 stone which differs from other H5 chondrites mainly in its higher proportion of chromite (0.9 wt %) and in the relatively lower iron and higher magnesium content of the chromite. The modal proportions of opaque phases were obtained by point‐counting in reflected light, and the modal proportions of nonopaque silicate phases in the matrix were estimated from traverses of a selected small area by electron microprobe. The consistency between the bulk chemical analysis and the chemical composition calculated from the modal mineral proportions implies that the bulk silicate composition of the chondrules is very similar to that of the silicate matrix and suggests a common source for both chondrules and matrix.
THE SAN JUAN CAPISTRANO METEORITE
Authors: Finkel R. C. , Marti K. , Jones R. E.
Published: June 2012

The San Juan Capistrano chondrite fell on 15 March 1973; the total recovered mass was 56 g. Electron microprobe, chemical and petrographic studies show it to be a member of the H group and of petrologic type 6. Rare gas studies show that only minor radiogenic gas loss has occurred and yield a K‐Ar age of 4.6 × 109 years and a Kr‐Kr exposure age of 29 × 106 years.
MINERALOGY, PETROLOGY AND CHEMISTRY OF THE ISNA (C3) METEORITE
Authors: Methot Robert L. , Noonan Albert F. , Jarosewich Eugene , deGasparis Aurelio A. , Al‐Far D.M.
Published: June 2012

A total chemical analysis of the Isna, Egypt, meteorite is similar to analyses for chondrites of type C3, Ornans sub‐type; however, comparison with one group of chemical data indicates that Isna is intermediate between the C3(O)'s and C3(V)'s in terms of total Fe. On the basis of atom ratios of Fe, Ca, Al, and Ti to Si, Isna can also be placed into a chemical group which includes types C1 and C2, as well as C3(O). Thin sections show a variety of small, closely‐packed chondrules, fragments, and aggregate‐like masses in a poorly translucent matrix. Olivine + clinoenstatite inclusions rich in metal and troilite, and olivine‐rich inclusions are abundant and show evidence of shock. Ca‐Al‐Ti‐rich inclusions, of probable high‐temperature origin, contain olivine, spinel, Ca‐rich nepheline, gehlenite, diopside, augite, enstatite, and anorthite. Kamacite and taenite from various occurrences in the meteorite have rather uniform Ni and Co contents, and Ni/Co for kamacite is close to that for several C3(O)'s.