bluuebunny/crossref_metadata_2025_split huggingface dataset:
Brooke‐Spiegler syndrome: report of a case with a novel mutation in the CYLD gene and different types of somatic mutations in benign and malignant tumors
Authors: Kazakov Dmitry V. , Schaller Jörg , Vanecek Tomas , Kacerovska Denisa , Michal Michal 
Published: February 2010

The authors report a case of Brooke‐Spiegler syndrome (BSS) with a novel germline CYLD mutation and various somatic mutations identified in the lesional tissues. The patient was a 46‐year‐old man with multiple lesions on the face. The available histopathological material included 24 trichoepitheliomas, 2 large nodular basal cell carcinomas (BCCs), 2 spiradenomas, 1 spiradenocylindroma and 1 trichoblastoma composed of large and small nodules with prominent clear cell differentiation. Whereas one of the two BCCs manifested a conventional morphology, the second neoplasm additionally showed foci with high grade cytological features characterized by marked pleomorphism and numerous mitotic figures. There were also numerous signet ring cells and cells containing intracytoplasmic eosinophilic inclusions. The germline mutation was a substitution mutation c.1684 + 1G> A. Somatic mutations were investigated in eight tissue blocks from which high quality genomic DNA had been successfully extracted. Somatic mutations included loss of heterozygosity (LOH) in four lesions and a single sequence mutation, namely a single base deletion c. 2322delA causing a frameshift mutation E774DfsX2. LOH occurred in both BCCs, one trichoepithelioma and one spiradenoma. In the remaining three lesions, the somatic event remained undetected.Kazakov DV, Schaller J, Vanecek T, Kacerovska D, Michal M. Brooke‐Spiegler syndrome: report of a case with a novel mutation in the CYLD gene and different types of somatic mutations in benign and malignant tumors.
ORIGINAL ARTICLE: Serum Anti‐endometrial Antibodies in Infertile Women – Potential Risk Factor for Implantation Failure
Authors: Sarapik Aili , Haller‐Kikkatalo Kadri , Utt Meeme , Teesalu Kaupo , Salumets Andres , Uibo Raivo 
Published: February 2010

Citation Sarapik A, Haller‐Kikkatalo K, Utt M, Teesalu K, Salumets A, Uibo R. Serum anti‐endometrial antibodies in infertile women – potential risk factor for implantation failure. Am J Reprod Immunol 2010Problem  Female infertility patients with diverse etiologies show increased production of autoantibodies.Method of study  Immunoblot analysis of sera from patients with endometriosis and tubal factor infertility (TFI) and mass spectrometry identification of candidate antigens.Results  The immunoblot results demonstrated the presence of IgA and IgG anti‐endometrial antibodies (AEA) to various antigens at molecular weights ranging from 10 to 200 kDa. Differences were detected in certain AEA reactions between the patients’ groups and particular AEA were associated with in vitro fertilization (IVF) implantation failure. IgA AEA to a 47‐kDa protein were more prevalent in TFI patients and were associated with unsuccessful IVF treatment. This antigen was subsequently identified as α‐enolase.Conclusion  Determination of the presence and spectra of AEA in patients with endometriosis and TFI undergoing IVF may be a useful marker to predict their pregnancy outcome.
Mobile Cultures: From the Sociology of Transportation to the Study of Mobilities
Authors: Vannini Phillip 
Published: February 2010

AbstractThis article reviews the current state of the research on mobile cultures by situating it within the sociology of mobility, or mobilities. The review focuses in detail on empirical research on the social and cultural aspects of transportation. The study of transport in daily life, or the study of mobile cultures, is reviewed with a particular attention to issues of time and space, as well as the social problems and social inequalities generated by dominant patterns of mobility. It also discusses the mobility turn in sociology and the growth of a new mobility paradigm influencing important shifts in sociological theory and research methodology. It defines the field of mobilities as the study of the social aspects of movement, including the movement of people, material objects, information, and capital – both in the material and the virtual sense. Mobilities for instance may include phenomena as migration, transport, travel and tourism, wireless and portable communication technology use, the social organization of transportation and communication infrastructures, and regional and transnational flows of capital and material things.
A nondestructive analytical method for stone meteorites—and a controversial discrepancy
Authors: FREDRIKSSON K. , BRENNER P. R. , FREDRIKSSON B. J. , OLSEN E. 
Published: February 2010

Abstract— A method is described for whole rock analyses of major elements in stone meteorites using the electron microprobe and requiring only powdering of the sample, most of which can be retrieved after analysis for additional analytical studies, such as instrument neutron activation analysis (INAA), radiochemical neutron activation analysis (RNAA) and O‐isotopic analysis. Whole individual chondrules of > 1 mg can be analyzed. The method is especially attractive for meteorites in short supply or of great rarity. A total of 398 meteorites were analyzed by this method. The results compare favorably with wet chemical analyses.A study was made of seventeen ordinary chondrites to compare their whole rock (metal free) compositions with the averaged compositions of eleven to thirty‐eight of their respective individual chondrules (a total of 374 chondrules). The oxide ratio Al2O3/CaO is generally lower in chondrules than in their respective chondrites, the disparity being larger for petrographic grade 5 than for grade 3. Ordinary chondrites are not simply the sum of their respective chondrules. Furthermore, correlations between CaO, Al2O3 and TiO2 are strong for chondrules in unequilibrated chondrites and nonexistent in equilibrated chondrites. Also H, L and LL chondrite groups have similar bulk compositions within their respective groups, in spite of the different proportions of chondrules, kinds of chondrules, chondrule debris, and matrix. All this brings into question the metamorphic classification in which high petrographic grades are the metamorphosed equivalents of low petrographic grades.
Planetary cratering 2: Studies of saturation equilibrium
Authors: HARTMANN William K. , GASKELL Robert W. 
Published: February 2010

Abstract— A realistic computer model has been developed to display images of imaginary cratered surfaces, taking into account empirically measured input size distributions of primary and secondary craters, ejecta blanket morphology including feathering with distance, obliteration due to ejecta from outside the imaged area, lighting effects, etc. The model allows us to track surface evolution of morphology as new craters are added.Using the model as well as lunar photos, we have studied the approach to saturation equilibrium (defined as a condition when no further proportionate increase in crater density occurs as input cratering increases). We find that an identifiable saturation equilibrium occurs close to a level previously identified for this state (Hartmann, 1984), typically fluctuating around a crater density from ∼0.4 to 2 times that level. This result is fairly robust vis‐à‐vis the range of model parameters we have chosen. Flooding, basin ejecta blankets, and other obliterative effects can introduce structure and oscillations within this range, even after saturation equilibrium is achieved.These findings may constrain or revise certain earlier interpretations of satellite and planet surface evolution and impactor populations, which were predicated on the assumed absence of saturation equilibrium.In our fourth experimental run, we found that suppression of “sandblasting” by subresolution impacts allows the smallest secondaries to rise above the saturation equilibrium line, a result that might be relevant to a similar situation on Gaspra and perhaps some other asteroids.
Mineralogy of meteorite groups
Authors: RUBIN Alan E. 
Published: February 2010

Abstract— Approximately 275 mineral species have been identified in meteorites, reflecting diverse redox environments, and, in some cases, unusual nebular formation conditions. Anhydrous ordinary, carbonaceous and R chondrites contain major olivine, pyroxene and plagioclase; major opaque phases include metallic Fe‐Ni, troilite and chromite. Primitive achondrites are mineralogically similar. The highly reduced enstatite chondrites and achondrites contain major enstatite, plagioclase, free silica and kamacite as well as nitrides, a silicide and Ca‐, Mg‐, Mn‐, Na‐, Cr‐, K‐ and Ti‐rich sulfides. Aqueously altered carbonaceous chondrites contain major amounts of hydrous phyllosilicates, complex organic compounds, magnetite, various sulfates and sulfides, and carbonates.In addition to kamacite and taenite, iron meteorites contain carbides, elemental C, nitrides, phosphates, phosphides, chromite and sulfides. Silicate inclusions in IAB/IIICD and IIE iron meteorites consist of mafic silicates, plagioclase and various sulfides, oxides and phosphates. Eucrites, howardites and diogenites have basaltic to orthopyroxenitic compositions and consist of major pyroxene and calcic plagioclase and several accessory oxides. Ureilites are made up mainly of calcic, chromian olivine and low‐Ca clinopyroxene embedded in a carbonaceous matrix; accessory phases include the C polymorphs graphite, diamond, lonsdaleite and chaoite as well as metallic Fe‐Ni, troilite and halides. Angrites are achondrites rich in fassaitic pyroxene (i.e., Al‐Ti diopside); minor olivine with included magnesian kirschsteinite is also present. Martian meteorites comprise basalts, lherzolites, a dunite and an orthopyroxenite. Major phases include various pyroxenes and olivine; minor to accessory phases include various sulfides, magnetite, chromite and Ca‐phosphates. Lunar meteorites comprise mare basalts with major augite and calcic plagioclase and anorthositic breccias with major calcic plagioclase.Several meteoritic phases were formed by shock metamorphism. Martensite (α2‐Fe,Ni) has a distorted body‐centered‐cubic structure and formed by a shear transformation from taenite during shock reheating and rapid cooling. The C polymorphs diamond, lonsdaleite and chaoite formed by shock from graphite. Suessite formed in the North Haig ureilite by reduction of Fe and Si (possibly from olivine) via reaction with carbonaceous matrix material. Ringwoodite, the spinel form of (Mg,Fe)2SiO4, and majorite, a polymorph of (Mg,Fe)SiO3 with the garnet structure, formed inside shock veins in highly shocked ordinary chondrites.Secondary minerals in meteorite finds that formed during terrestrial weathering include oxides and hydroxides formed directly from metallic Fe‐Ni by oxidation, phosphates formed by the alteration of schreibersite, and sulfates formed by alteration of troilite.
Sodium‐, chlorine‐rich mesostases in Chainpur (LL3) and Parnallee (LL3) chondrules
Authors: BRIDGES J. C. , ALEXANDER C. M. O'D. , HUTCHISON R. , FRANCHI I. A. , PILLINGER C. T. 
Published: February 2010

Abstract— Forty‐six chondrules from Chainpur (LL3.4) and 39 chondrules and clasts from Parnallee (LL3.6) have been sectioned and searched for Na‐, Cl‐rich phases by electron probe microanalysis (EPMA). Oxygen isotopic compositions, I‐Xe ages and ion probe data were also obtained on some of these chondrules. Sodium‐, Cl‐rich glass and microcrystalline sodalite (Na4Al3Si3O12Cl), nepheline (NaAlSiO4), scapolite (Na4Al3Si9O24Cl) have been identified in 7% of the Chainpur and 8% of the Parnallee samples. These phases are present in chondrule mesostases or, in one case, the plagioclase of a barred‐olivine chondrule. None of the chondrules contain >5 vol% Na‐, Cl‐rich phases. In the Chainpur chondrules, they originated through partial devitrification of silica‐undersaturated, rare‐earth‐element‐(REE), Na‐ and Cl‐rich mesostases. Two processes have been identified that led to the formation of these mesostases. In two of the chondrules, which consist mainly of low‐Ca pyroxene, the extended, metastable crystallization of low‐Ca pyroxene created silica‐undersaturated, REE‐rich residua. Barium‐ and Cl‐enrichments in nepheline and scapolite of one chondrule suggest that there was also an influx of alkalis and Cl during crystallization of the low‐Ca pyroxene. Similarly, another one of the Chainpur chondrules, mainly composed of olivine phenocrysts, is markedly enriched in Cl (10 × OC). As there is no evidence of corrosive metasomatism in any of the chondrules, Cl‐ (and alkali) enrichment is believed to have occurred when they were still partially molten. The chondrules were derived from normal O‐isotopic reservoirs, so the postulated influx of Ba, Na and Cl did not occur on an exotic parent body.Trace amounts of nepheline and sodalite, present in two Parnallee chondrules, crystallized from small Na‐, Cl‐, REE‐rich residua following extended crystallization of anorthite. An I‐Xe age of 5.0 Ma post‐Bjurböle obtained on one of these Parnallee chondrules dates the crystallization of feldspathoid and, thus, formation of the chondrule.
Clues to the nature of the impacting bodies from platinum‐group elements (rhenium and gold) in borehole samples from the Clearwater East crater (Canada) and the Boltysh impact crater (Ukraine)
Authors: SCHMIDT GERHARD 
Published: February 2010

Abstract— Seven large (10 g) impact melt rock samples from boreholes from the Boltysh impact crater (Ukraine) and six samples from the East Clearwater crater (Canada) were analyzed for Os, Ir, Ru, Rh, Pd, Re and Au by the nickel sulfide technique in combination with neutron activation. Earlier analyses of Clearwater East impact melt rocks have shown that they are strongly enriched in Ir, Os, Pd and Re. In this work, I confirm earlier findings and demonstrate similarly high enrichments of Rh and Ru. The average Os/Ir, Ru/Ir, Pd/Ir, Rh/Ir and Ru/Rh ratios of the melt rock samples from Clearwater East are CI‐chondritic and yield an average Ir content of 25.2 ± 6.5 ng/g relative to an average upper crust concentration of 0.03 ± 0.02 ng/g Ir. The amount of meteoritic component corresponds to 4 to 7% of a nominal CI component for Clearwater East.The impact melt rock samples from a bore hole from Boltysh are low in Ir with an average of 0.2 ± 0.1 ng/g. The CI‐normalized abundances increase from the refractory to the more volatile siderophile elements (Os < Ir < Ru < Rh ∼ Pd ∼ Au ∼ Ni ∼ Co). Because of the low Ir anomaly and uncertainties in making corrections (correlations are weak) for indigenous siderophile elements, no clear projectile assignment can be made.
Vesta as the howardite, eucrite and diogenite parent body: Implications for the size of a core and for large‐scale differentiation
Authors: RUZICKA ALEX , SNYDER GREGORY A. , TAYLOR LAWRENCE A. 
Published: February 2010

Abstract—If Vesta is the parent body of the howardite, eucrite, and diogenite (HED) meteorites, then geo‐chemical and petrologic constraints for the meteorites may be used in conjunction with astronomical constraints for the size and mass of Vesta to (1) determine the size of a possible metal core in Vesta and (2) model the igneous differentiation and internal structure of Vesta.The density of Vesta and petrologic models for HED meteorites together suggest that the amount of metal in the parent body is <25 mass%, with a best estimate of ∼5%, assuming no porosity. For a porosity of up to 5% in the silicate fraction of the asteroid, the permissible metal content is <30%. These results suggest that any metal core in the HED parent body and Vesta is not unusually large.A variety of geochemical and other data for HED meteorites are consistent with the idea that they originated in a magma ocean. It appears that diogenites formed by crystal accumulation in a magma ocean cumulate pile and that most noncumulate eucrites (excepting such eucrites as Bouvante and Statinem) formed by subsequent crystallization of the residual melts. Modelling results suggest that the HED parent body is enriched in rare earth elements by a factor of ∼2.5–3.5 relative to CI‐chondrites and that it has approximately chondritic Mg/Si and Al/Sc ratios. Stokes settling calculations for a Vesta‐wide, nonturbulent magma ocean suggest that early‐crystallizing magnesian olivine, orthopyroxene, and pigeonite would have settled relatively quickly, permitting fractional crystallization to occur, but that later‐crystallizing phases would have settled (or floated) an order of magnitude more slowly, allowing, instead, a closer approach to equilibrium crystallization for the more evolved (eucritic) melts. This would have inhibited the formation of a plagioclase‐flotation crust on Vesta.Plausible models for the interior of Vesta, which are consistent with the data for HED meteorites and Vesta, include a metal core (<130 km radius), an olivine‐rich mantle (∼65–220 km thick), a lower crustal unit (∼12–43 km thick) composed of pyroxenite, from which diogenites were derived, and an upper crustal unit (∼23–42 km thick), from which eucrites originated. The present shape of Vesta (with ∼60 km difference in the maximum and minimum radius) suggests that all of the crustal materials, and possibly some of the underlying olivine from the mantle, could have been locally excavated or exposed by impact cratering.
Petrology, chemistry, and isotopic compositions of the lunar highland regolith breccia Dar al Gani 262
Authors: BISCHOFF A. , WEBER D. , CLAYTON R. N. , FAESTERMANN T. , FRANCHI I. A. , HERPERS U. , KNIE K. , KORSCHINEK G. , KUBIK P. W. , MAYEDA T. K. , MERCHEL S. , MICHEL R. , NEUMANN S. , PALME H. , PILLINGER C. T. , SCHULTZ L. , SEXTON A. S. , SPETTEL B. , VERCHOVSKY A. B. , WEBER H. W. , WECKWERTH G. , WOLF D. 
Published: February 2010

Abstract— Lunar meteorite Dar al Gani 262 (DG 262)—found in the Libyan part of the Sahara—is a mature, anorthositic regolith breccia with highland affinities. The origin from the Moon is undoubtedly indicated by its bulk chemical composition; radionuclide concentrations; noble gas, N, and O isotopic compositions; and petrographic features. Dar al Gani 262 is a typical anorthositic highland breccia similar in mineralogy and chemical composition to Queen Alexandra Range (QUE) 93069.About 52 vol% of the studied thin sections of Dar al Gani 262 consist of fine‐grained(100 μm) constituents, and 48 vol% is mineral and lithic clasts and impact‐melt veins. The most abundant clast types are feldspathic fine‐grained to microporphyritic crystalline melt breccias (50.2 vol%; includes recrystallized melt breccias), whereas mafic crystalline melt breccias are extremely rare (1.4 vol%). Granulitic lithologies are 12.8 vol%, intragranularly recrystallized anorthosites and cataclastic anorthosites are 8.8 and 8.2 vol%, respectively, and (devitrified) glasses are 2.7 vol%. Impact‐melt veins (5.5 vol% of the whole thin sections) cutting across the entire thin section were probably formed subsequent to the lithification process of the bulk rock at pressures below 20 GPa, because the bulk rock never experienced a higher peak shock pressure.Mafic crystalline melt breccias are very rare in Dar al Gani 262 and are similar in abundance to those in QUE 93069. The extremely low abundance of mafic components and the bulk composition may constrain possible areas of the Moon from which the breccia was derived. The source area of Dar al Gani 262 must be a highland terrain lacking significant mafic impact melts or mare components.On the basis of radionuclide activities, an irradiation position of DG 262 on the Moon at a depth of 55–85 g/cm3and a maximum transit time to Earth <0.15 Ma is suggested. Dar al Gani 262 contains high concentrations of solar‐wind‐implanted noble gases. The isotopic abundance ratio 40Ar/36Ar < 3 is characteristic of lunar soils.The terrestrial weathering of DG 262 is reflected by the occurrence of fractures filled with calcite and by high concentrations of Ca, Ba, Cs, Br, and As. There is also a large amount of terrestrial C and some N in the sample, which was released at low temperatures during stepped heating. High concentrations of Ni, Co, and Ir indicate a significant meteoritic component in the lunar surface regolith from which DG 262 was derived.
Investigation of a bright flying object over northwest Spain, 1994 January 18
Authors: DOCOBO J. A. , SPALDING R. E. , CEPLECHA Z. , DIAZ‐FIERROS F. , TAMAZIAN V. , ONDA Y. 
Published: February 2010

Abstract— On the early morning of 1994 January 18, a very bright luminous object crossed the sky of Santiago de Compostela, Spain. From visual sightings, it is concluded that the object wasn't a meteoric fireball (bolide). A surface “crater” in Cando (close to Santiago) with dimensions 29 × 13 m and 1.5 m deep was later discovered within 1 km of the projected “impact” point of the luminous object. At this site, in addition to the topsoil, full‐grown pine trees >20 m high were thrown downhill over a nearby road, leaving the down‐slope edge of the “crater” untouched and with a steep interior wall (this would not be the case if a regular landslide were responsible for the transport). Standing trees below the “crater” showed embedded soil and plant residues up to heights >3 m. No strange materials (meteorites or artifacts) were recovered in or close to the “crater”; all materials belonged to the site and were not shocked; thus, an impact is very improbable.A possible explanation capable of reconciling all of the observations is presented. It hypothesizes an eruption of earth gases to create the crater, with the rising gas plume then interacting with atmospheric electricity to produce the propagating fireball that was observed.
Geochemical and petrographic studies of oldhamite, diopside, and roedderite in enstatite meteorites
Authors: HSU WEIBIAO 
Published: February 2010

Abstract— In Qingzhen (EH3), oldhamite contains numerous types of inclusions and intergrows with other phases; but in equilibrated enstatite chondrites and aubrites, it usually occurs as individual grains. I suggest that oldhamite in unequilibrated enstatite chondrites (UECs) crystallized from a melt, probably during chondrule formation. Subsequent thermal metamorphism on the parent bodies further modified the oldhamite occurrences in enstatite chondrites. This suggestion is consistent with the results of melting experiments on UECs and aubrites and with the volatile element enrichments in this mineral.I analyzed minor and trace element abundances in diopside from two aubrites. These data and petrographic observations suggest that diopside formed by igneous crystallization.I report the first known occurrence of roedderite in an aubrite and its major, minor, and trace element concentrations. This mineral is rich in alkalis but is depleted in siderophile and refractory lithophile elements.A negative Sm anomaly was noted in albite from equilibrated enstatite chondrites and aubrites.