bluuebunny/crossref_metadata_2025_split huggingface dataset:
Philippine Tektites and the Tektite Problem in General*
Authors: Beyer H. Otley 
Published: June 2012

Great showers of tektites fell upon certain parts of the earth at widely separated geologic periods. The four major geologic groups are:The typical forms—spheroids, disks, or oval, cylindrical, dumb‐bell‐shaped, and pointed, drop‐shaped bodies—suggest natural shapes assumed by molten glass revolving in the atmosphere or a similar gaseous medium. The Australites show a partial re‐fusing of the original glass sphere and backward flow, producing a peculiar button‐like appearance.Group three, which includes the Philippine tektites, may be divided into four major subgroups: (1) Indochinites; (2) Rizalites; (3) Billitonites and Malaysianites; and (4) Java Tektites. The characteristics etc. of these bodies are discussed in some detail.Of the various theories of the origin of tektites, three are still worthy of consideration. These are: (1) the theory of volcanic or other earthly origin; (2) the burning, light‐metal meteorite theory; and (3) the meteorite explosion‐crater theory. An astronomical theory of tektites, proposed by Dr. W. Carl Rufus, is summarized and briefly criticized, pro and con.The Philippines present a unique opportunity for the study of the richest known deposit of tektites in their natural environment. The only local students of the problem are the writer and Dr. Miguel Selga, S.J., joined recently by Mr. J. Van Eck. To stimulate local interest, the present outline was presented to the Philippine National Research Council.
The Ivory‐Coast deposit, believed to be Mesozoic;
The Moldavites, or European, from the Helvetian strata of mid‐Miocene;
The Indo‐malaysianites, undoubtedly mid‐Pleistocene; and
The Australites, believed to be post‐Pleistocene or recent.
A Statistical Study of the Meteoritic Falls of the World as of Date 1941 January 1
Authors: Leonard Frederick C. , Slanin Boris 
Published: June 2012

ABSTRACTThis paper contains 3 tables of statistics, as of date 1941 January 1, for the meteoritic falls of (1) the United States, (2) countries other than the United States, and (3) the continents and the world (1392 falls in all) and a brief discussion of the contents of each table. The data for the tables have been taken from a manuscript catalog of the meteoritic falls of the world now in process of compilation by the writers. The paper ends with a consideration of some 15 factors that favor the recovery of meteorites.
Statistical Studies of the Meteoritic Falls of the World: 3. Their Time Distribution*
Authors: Leonard Frederick C. , Slanin Boris 
Published: June 2012

ABSTRACTThis paper contains a study of all the authentic meteoritic falls of the world, 1314 in number (21 of date earlier than 1790 and 1293 of date 1790 and later), for which reasonably reliable information concerning the time of fall or find is available. By means of a series of tables and graphs, the following subjects are treated: (1) the observed falls by years; (2) the unobserved falls by years; (3) both kinds of falls by years; (4) the observed falls by months; and (5) the observed falls by hours. The average numbers of falls for the decade 1930–39 are compared with the corresponding numbers for the 150‐year interval 1790–1939. The general increase in meteoritical activity, particularly since 1920, is apparent from the material of the paper.
Synthetic Symmetry in Mutual‐Induction Balances: A Practical Problem with Meteorite Detectors*
Authors: Wisman Franklin Otis 
Published: June 2012

ABSTRACTAs has been pointed out in a paper by Dr. Lincoln La Paz recently published in these Contributions (P. A., 50, 157–165, March, 1942), efforts to apply electromagnetic detectors to the problem of locating buried iron meteorites have encountered many difficulties inherent in the instruments employed. In an instrument recently devised by the author, some of these difficulties are eliminated. The new detector has only half the weight and bulk of any comparable instrument, and power‐supply requirements have been materially decreased. The purpose of this paper is to derive the fundamental relations that must be observed in the design of such an instrument.
Nitrogen and its Compounds in Meteorites
Authors: Buddhue John Davis 
Published: June 2012

ABSTRACTMention is made of free nitrogen, titanium nitride (osbornite), cyanogen, and previously reported occurrences of ammonium compounds in meteorites. Ammonia is reported as present in all of the 8 meteoritic stones tested. A new method of analysis is described which was used to determine the amount of ammonia in stones of 5 falls. In Holbrook, Arizona, the ammonia is shown to be present as a compound, at least partly soluble in water. The nitrogen found by Lipman appears to have been largely ammonium nitrogen. Lipman's failure to find water‐soluble nitrates or nitrites is confirmed; in addition, no cyanides were found in Holbrook.
A Preliminary Note on the Exclusively Meteoritic Minerals
Authors: Neuerburg George J. 
Published: June 2012

ABSTRACTIt is shown in this preliminary note that the earlier lists of the exclusively meteoritic minerals are in error. On the basis of a review and an analysis of the available literature, it is proposed that a tentative, revised list of these minerals should include the following: daubréelite, kosmochlor, merrillite, oldhamite, osbornite, phosphorus, schreibersite, taenite, and weinbergerite.
Desiderata for a General or Comprehensive Catalog of the Meteoritic Falls of the World*
Authors: Leonard Frederick C. 
Published: June 2012

ABSTRACTThe following 10 “desiderata” for a general or comprehensive catalog of the meteoritic falls of the world are discussed in order: (1) coördinate number; (2) name; (3) class; (4) time of fall or find; (5) total weight; (6) number etc. of individual masses; (7) additional data for a multiple fall or a shower; (8) physical and chemical characters; (9) depositories; and (10) bibliography. A set of abbreviations, for words most often used in the description of meteorites, meteoritic falls, etc., is recommended.
Meteoritical Pictographs
Authors: La Paz Lincoln 
Published: June 2012

ABSTRACTThis paper calls attention to certain undoubtedly genuine meteoritical pictographs and to other examples of picture‐writing that probably have meteoritical significance. It is urged that anthropologists, archeologists, and ethnologists coöperate with meteoriticists in the collection, collation, and dating of pictographs portraying meteoritical phenomena.
The Cavour, South Dakota, Aerolites (980,442)
Authors: Buddhue John Davis 
Published: June 2012

ABSTRACTThe Cavour, Beadle County, South Dakota, aerolites (C.N. = 980,442) belong to a shower of at least 7 stones. The description based on one of them shows that the fall is an old one, because the specimen is badly oxidized. Analyses are given (in Table 1) of the soluble silicate, insoluble silicate, and metal. The last‐named component is present partly in the form of small plates, in addition to the more common irregular grains. The stone is probably a brecciated crystalline chondrite (symbol = C, kb).
A Reply to an Article by Mr. Brandon Barringer on the Origin of the “Carolina Bays”*
Authors: Prouty William F. 
Published: June 2012

ABSTRACTThe 5 points of criticism raised by Mr. Brandon Barringer against the probable meteoritic origin of the “Carolina Bays” are each briefly discussed, and the conclusion is reached that these objections are not valid under the existing conditions and under the modified meteoritic theory of bay origin.
A Composite Spectrum of a Perseid Meteor of 1948*
Authors: Russell John A. 
Published: June 2012

ABSTRACTA spectrum of a Perseid meteor, observed on 1948 August 11, from a place near Blairsden, Plumas County, California, is discussed. This spectrum exhibits, along successive segments of the visible path of the meteor, the characteristics of all 3 spectral types, Z, X, Y, in that order. These variations in the spectrum of a single meteor substantiate the hypothesis that differences in meteor spectra result from changes in the excitation of the meteoritic vapor, rather than from differences in the composition of the meteorites themselves.
Reduced Meteoritic Iron Oxide
Authors: Buddhue John Davis 
Published: June 2012

ABSTRACTWeighed pieces of Canyon Diablo, Arizona, oxide were reduced to metal by heating in hydrogen. In two cases, the oxide was analyzed before reduction, and the resulting metal was analyzed after reduction. From the data obtained, it is possible to calculate the oxygen content of the original oxide by three different methods. The results are in fair agreement, and indicate an oxygen content of about 29%.
Miscellaneous Notes on Meteorites from Holbrook, Richardton, Xiquipilco, and Mount Elden*
Authors: Buddhue John Davis 
Published: June 2012

ABSTRACTFrom time to time, minor observations have been made on meteorites. These included the following: A Holbrook, Arizona, aerolite contained 0.23% of water‐soluble salt, which included 0.02% of sulfate and a trace of calcium. The same stone had a variable moisture content, which depended upon the relative humidity of its surroundings. A Richardton, North Dakota, aerolite contained only 0.033% of moisture. A Xiquipilco, Mexico, siderite probably contained a trace of nitride. An analysis is given of the taenite in a Mount Elden, Arizona, siderite. Much of the graphite in this mass appeared to be cliftonite or otherwise crystalline.
Some Remarks on the Origin of Earthly Meteorites*
Authors: Leonard Frederick C. 
Published: June 2012

ABSTRACTIn general, fallen meteorites are probably of planetary origin, whereas consumed meteorites, perhaps in most cases, if not in all, are of cometary origin. The latter variety of bodies are evidently of insufficient mass to escape total vaporization within the Earth's atmosphere. Since no comet—and probably no meteorite, either—has ever been showed to have been traveling on an unmistakably hyperbolic heliocentric orbit, if Earthly meteorites are of planetary and cometary origin, their elliptic heliocentric orbits and their origin within the Solar System are readily explained.
The Albuquerque, Bernalillo County, New Mexico, Siderite (ECN =+ 1068,350)
Authors: Beck Carl W. , La Paz Lincoln 
Published: June 2012

AbstractIn this paper are given details concerning the acquisition of an iron meteorite (siderite) found approximately 13 miles west‐southwest of Albuquerque, in Bernalillo County, New Mexico (equatorial coördinate number (ECN) = + 1068,350). The total mass recovered to date is a single specimen weighing 157.3 gm. Mineralogical, chemical, and radiochemical studies have been made, and, on the basis of these investigations, the meteorite is classified as a medium octahedrite (Om). The original belief that this meteorite might be a stray specimen of the Canyon Diablo, Arizona, fall is refuted by the mineralogical, chemical, and radiochemical findings, especially the last two.
The Discovery of an Additional Sams Valley, Oregon, Meteorite (ECN =+ 1229,425)
Authors: Morley Russell A. 
Published: June 2012

AbstractThe discovery, in the summer of 1949, of an additional Sams Valley, Oregon, meteorite (ECN = + 1229,425; cl. = Om) on the Frank B. Payne property, near Beagle, Jackson County, Oregon, in the Trail Quadrangle, is announced. This meteorite was found by Mr. Payne's father in the late 1800′s, but has never before been reported. It is now on display in the Jacksonville Museum. The specimen measures 12.5 × 4.5 × 4 cm. (overall dimensions), and has a specific gravity (sp. gr.) of 6.82 and a hardness of 5.5–6.0, and weighs about 1028 gm.
THE LEONIDS BY RADAR—1957 TO 19681
Authors: McIntosh Bruce A. , Millman Peter M. 
Published: June 2012

Radar observations of the Leonid meteor shower, made near Ottawa during the years from 1957 to 1968 inclusive, are analyzed and reduced to give comparative flux rates. A strength classification has been made in terms of the ratio of shower rates to background rates. The relative strengths found by radar, showing marked variability from year to year, are confirmed by analysis of available visual observations.There is also great variation in the distribution of particle sizes. The high rates of the 1966 return were accompanied by a relatively high percentage of small particles. In 1965 there was a much higher proportion of large particles, and the high rates of 1961 showed a mass or size distribution intermediate between that of 1966 and of 1965.
METASTABLE GROWTH PATTERNS IN SOME TERRESTRIAL AND LUNAR ROCKS
Authors: Drever Harald I. , Johnston Robert 
Published: June 2012

With reference to new information on the textures in some terrestrial mafic and ultramafic igneous rocks of Tertiary age, textural patterns attributable to metastable crystallization are described, illustrated and reviewed. The igneous textural terminology, employed in the descriptive text, is reviewed and the use of certain new terms is advocated. Compared with these textural patterns are the skeletal crystal growth and intergrowth in igneous rock samples obtained, mainly by the Apollo 12 Mission, from the moon. Both orientated and unorientated metastable growth yield characteristic dendritic or skeletal olivine crystals, and a texture which has been termed “intrafasciculate” is also attributed to metastable crystallization of plagioclase and pyroxene. The three principal terrestrial textures defined and described are ‘Willow Lake’ texture, intrafasciculate texture and harrisitic texture. The term “thermotactic” is preferred to ‘Willow Lake’ or ‘crescumulate’ to define a texture with orientation of crystal growth in the direction of the thermal gradientAttention is drawn to the importance in petrogenesis of such metastable crystallization, as inferred from crystal growth and textural observations. It is apparent that analogous ‘metastable’ textures occur through a remarkable range in geological contextMore detailed work is advocated on the pegmatitic eucrites and peridotites of Rhum. Since the evidence suggests that these rocks represent hydrous ultrabasic liquids, not cumulates, the conditions governing the growth of olivine in them must differ from those of any lunar analog
MAJOR ELEMENT COMPOSITION OF GLASSES IN THREE APOLLO 15 SOILS
Authors: Reid Arch M. , Warner Jeff , Ridley W. I. , Brown R. W. 
Published: June 2012

Approximately 180 glasses in each of three Apollo 15 soils have been analyzed for nine elements. Cluster analysis techniques allow the recognition of preferred glass compositions that are equated with parent rock compositionsGreen glass rich in Fe and Mg, poor in Al and Ti may be derived from deep seated pyroxenitic material now present at the Apennine Front. Fra Mauro basalt (KREEP) is most abundant in the LM soil and is tentatively identified as ray material from the Aristillus‐Autolycus area. Highland basalt (anorthositic gabbro), believed to be derived from the lunar highlands, has the same composition as at other landing sites, but is less abundant. The Apennine Front is probably not true highland material but may contain a substantial amount of material with the composition of Fra Mauro basalt, but lacking the high‐K content. Glasses with mare basalt compositions are present in the soils and four subgroups are recognized, one of which is compositionally equivalent to the large Apollo 15 basalt samples
THE CHEMICAL COMPOSITION OF MAJOR ELEMENTS AND HEAVY TRACE METALS IN CHONDRITES PARAMBÙ AND MARILIA
Authors: Shima M. , Jochum K.P. , Sighinolfi G.P. , Hintenberger H. 
Published: June 2012

The chemical composition of the newly observed fallen chondrites Parambù, 1967, and Marilia, 1971, was determined. Wet chemical methods were used for major elements analyses and the abundances of heavy trace elements from tungsten to uranium were determined by spark source mass spectrometry.The chemical composition confirmed the classification of Marilia as an H‐group chondrite by Avanzo et al. (1973): Parambù was classified as an LL‐group chondrite.
YAMATO METEORITES COLLECTED IN ANTARCTICA IN 1969
Authors: Nagata Takesi 
Published: June 2012

The meteoritic community has been tantalized by reports of extensive meteorite finds in Antarctica by members of the Japanese Antarctic Research Expedition. The National Institute of Polar Research has published this introduction and review of the Yamato meteorites collected in Antarctica in 1969.This welcome review reveals that nine meteorite fragments of meteoritic material were found in the region of the Yamato Mountains. Four pieces greater than 60 g in weight have been identified as an enstatite chondrite, a hypersthene achondrite, a type III carbonaceous chondrite and a bronzite chondrite. In 1973 eleven additional suspected meteorites were recovered. Preliminary results show that three bronzite chondrites and one achondrite are among the new finds. In 1974 over 600 pieces of meteorite‐like rock have been collected.The volume contains five articles on the original 1969 material. These include a general discussion on their discovery including photographs of the individuals, and notes on the chemical, mineralogical and petrological characteristics of the four large samples. Two articles deal with detailed mineralogic and magnetic properties of these specimens.Information on these interesting finds is welcome. Information on the 1969 and 1974 material is anxiously awaited.
OLIVINE MICROPORPHYRY IN THE ST. MESMIN CHONDRITE
Authors: Dodd Robert T. , Jarosewich Eugene 
Published: June 2012

Olivine microporphyry, of metal‐ and troilite‐poor LL‐group composition and composed chiefly of olivine (58 vol. %), pyroxenes (18%, including orthopyroxene, pigeonite, and subcalcic augite), and quartz‐oligoclase glass (22%), occurs in and locally intrudes clasts in the St. Mesmin chondrite (LL‐group breccia). Its crystallization history resembles that of many Apollo 12 lunar basalts, modified somewhat by a lower bulk Fe/Mg ratio and a higher (Fe+Mg)/Ca ratio.The microporphyry crystallized from a melt which was emplaced during a period of brecciation or between two episodes of brecciation, but after the thermal metamorphism recorded in other components of the breccia. This melt originated by complete melting of normal LL‐group material with loss of Fe, Ni, and S, or, less likely, by fusion of such material (LL‐7?) which had lost these elements during prior anatexis. Comparison of the St. Mesmin microporphyry with similar material in the Parnallee chondrite (Binns, 1968) suggests that the latter was derived from a different parent, perhaps of C‐1 chondritic composition.
PIANCALDOLI METEORITE: CHEMISTRY, MINERALOGY AND PETROLOGY
Authors: Carapezza Marcello , Nuccio P. Mario , Valenza Mariano 
Published: June 2012

The fall occurred near Piancaldoli, Florence, Italy, at 19.14 U.T. on the 10th August 1968. The fireball broke up in the atmosphere producing a cloud like a balloon.The trajectory and the terminal point were calculated, leading to the recovery of three small meteoritic fragments, found on the roof of a house. Chemical analysis gave the following results: SiO2 40.80; TiO2 0.15; Al2O3 2. 70; Cr2O3 0.47; FeO 17.20; MnO 0.07; MgO 25.18; CaO 1.95; Na2O 0.64; K2O 0.07; P2O5 0.20; NiS 0.93; FeS 6.24; Fe° 2.40; Ni° 0.40; Co 0.05; sum 99.45.In the lithic portion of the meteorite the following minerals were found: both clino and orthopyroxenes (En = 76 to 98%), olivines (Fo = 66 to 98%), troilite, pyrrhotite, pentlandite, kamacite, ilmenite, apatite, merillite, schreibersite, chromite and Henderson phase.From all the mineralogical and petrological data, we conclude that the Piancaldoli meteorite is an “unequilibrated ordinary chondrite,” LL3. The microbrecciated structure of the rock and some shock features were observed, while the rock as a whole is unshocked, suggesting that these features were caused by impact events which took place during the accretion of the parent body.
NOBLE GAS ANOMALIES AND SYNTHESIS OF THE CHEMICAL ELEMENTS
Authors: Sabu D.D. , Manuel O.K. 
Published: June 2012

There are two types of planetary noble gases: One, containing isotopically “anomalous” argon, krypton and xenon but isotopically “normal” helium and neon, was derived from outer stellar regions. The other, consisting almost entirely of isotopically “normal” argon, krypton and xenon, with little or no helium or neon, was derived from inner stellar regions.Mixing of nucleosynthesis products from different regions of a supernova is responsible for the observed correlations between elemental and isotopic ratios of planetary noble gases in different classes of meteorites. The solar system condensed directly from the chemically and isotopically heterogeneous debris of a single supernova.There is no convincing evidence, however, of separate nucleogenetic components in neon. Fractionation and spallation can account for all previously identified components of trapped meteoritic neon, Ne‐A, Ne‐B, Ne‐C, Ne‐D, Ne‐E, Ne‐Al, Ne‐A2, Ne‐E(L), Ne‐E(H) and Ne‐O, and this same mechanism also explains differences between the isotopic compositions of meteoritic, atmospheric, and solar wind neon.Variations in the abundance pattern of planetary noble gases are primarily the result of stellar fusion reactions and physical adsorption, rather than gas solubility.
THE LOOP CHONDRITE: PETROLOGY, MINERAL CHEMISTRY, AND OPAQUE MINERALOGY
Authors: Boctor Nabil Z. , Kullerud Gunnar 
Published: June 2012

The Loop meteorite was found in 1962 in Gaines County, Texas, at a location very close to that where the Ashmore chondrite was found in 1969. The two specimens were assumed to be fragments of the same meteorite.The Loop meteorite is a type L6 chondrite composed of olivine (Fo75.4Fa24.6), orthopyroxene (En77.6Wo1.5Fs20.9), clinopyroxene (En47.5Wo45.1Fs7.4), plagioclase (Ab84.3Or5.5An10.2), Fe‐Ni metal, troilite, and chromite. Fe‐Ni metal is represented by kamacite (5.8‐6.4 wt % Ni, 0.88‐1.00 wt % Co), taenite (30.0–52.9 wt % Ni, 0.16‐0.34 wt % Co), and plessite (16.8–28.5 wt % Ni, 0.38‐0.54 wt % Co). Native copper occurs as rare inclusions in Fe‐Ni metal. Both chondrules and matrix have similar mineral compositions.The mineral chemistry of the Loop meteorite is quite different from that of the Ashmore, which was classified as an H5 chondrite by Bryan and Kullerud (1975). Therefore, the Ashmore and Loop meteorites are two different chondrites, even though they were recovered from the same geographic location.
INTEROBJECT STRUCTURE OF UNGROUPED IRON METEORITES AS REVEALED BY ADVANCED CLUSTERING: METHODS AND CHEMICAL FEATURES
Authors: Esbensen Kim H. , Kaufman L. , Massart D.L. 
Published: June 2012

Using the MASLOC clustering strategy, 61 ungrouped iron meteorites are probed for physico‐chemical clusters. The existing classification of 13 resolved chemical groups is used as an internal coherence reference.Results include tentative establishment of a new group: ID (7 members), with chemical features similar to those of the non‐magnetic groups IAB and IIICD. Six additional pairings, all with magmatic chemical signatures, are also recognized.