Thematische Bibliographien / Meteorites Analysis

Auswahl der wissenschaftlichen Literatur zum Thema „Meteorites Analysis“

Autor: Grafiati
Veröffentlicht am 4. Juni 2021
Zuletzt aktualisiert am 28. Januar 2023

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  1. Zeitschriftenartikel
  2. Dissertationen
  3. Bücher
  4. Buchteile
  5. Konferenzberichte

Zeitschriftenartikel zum Thema "Meteorites Analysis":

1

Wampler, James, Mark Thiemens, Shaobo Cheng, Yimei Zhu und Ivan K. Schuller. „Superconductivity found in meteorites“. Proceedings of the National Academy of Sciences 117, Nr. 14 (23.03.2020): 7645–49. http://dx.doi.org/10.1073/pnas.1918056117.

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Meteorites can contain a wide range of material phases due to the extreme environments found in space and are ideal candidates to search for natural superconductivity. However, meteorites are chemically inhomogeneous, and superconducting phases in them could potentially be minute, rendering detection of these phases difficult. To alleviate this difficulty, we have studied meteorite samples with the ultrasensitive magnetic field modulated microwave spectroscopy (MFMMS) technique [J. G. Ramírez, A. C. Basaran, J. de la Venta, J. Pereiro, I. K. Schuller,Rep. Prog. Phys.77, 093902 (2014)]. Here, we report the identification of superconducting phases in two meteorites, Mundrabilla, a group IAB iron meteorite [R. Wilson, A. Cooney,Nature213, 274–275 (1967)] and GRA 95205, a ureilite [J. N. Grossman,Meteorit. Planet. Sci.33, A221–A239 (1998)]. MFMMS measurements detected superconducting transitions in samples from each, above 5 K. By subdividing and remeasuring individual samples, grains containing the largest superconducting fraction were isolated. The superconducting grains were then characterized with a series of complementary techniques, including vibrating-sample magnetometry (VSM), energy-dispersive X-ray spectroscopy (EDX), and numerical methods. These measurements and analysis identified the likely phases as alloys of lead, indium, and tin.
2

Drouard, A., P. Vernazza, S. Loehle, J. Gattacceca, J. Vaubaillon, B. Zanda, M. Birlan et al. „Probing the use of spectroscopy to determine the meteoritic analogues of meteors“. Astronomy & Astrophysics 613 (Mai 2018): A54. http://dx.doi.org/10.1051/0004-6361/201732225.

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Context. Determining the source regions of meteorites is one of the major goals of current research in planetary science. Whereas asteroid observations are currently unable to pinpoint the source regions of most meteorite classes, observations of meteors with camera networks and the subsequent recovery of the meteorite may help make progress on this question. The main caveat of such an approach, however, is that the recovery rate of meteorite falls is low (<20%), implying that the meteoritic analogues of at least 80% of the observed falls remain unknown. Aims. Spectroscopic observations of incoming bolides may have the potential to mitigate this problem by classifying the incoming meteoritic material. Methods. To probe the use of spectroscopy to determine the meteoritic analogues of incoming bolides, we collected emission spectra in the visible range (320–880 nm) of five meteorite types (H, L, LL, CM, and eucrite) acquired in atmospheric entry-like conditions in a plasma wind tunnel at the Institute of Space Systems (IRS) at the University of Stuttgart (Germany). A detailed spectral analysis including a systematic line identification and mass ratio determinations (Mg/Fe, Na/Fe) was subsequently performed on all spectra. Results. It appears that spectroscopy, via a simple line identification, allows us to distinguish the three main meteorite classes (chondrites, achondrites and irons) but it does not have the potential to distinguish for example an H chondrite from a CM chondrite. Conclusions. The source location within the main belt of the different meteorite classes (H, L, LL, CM, CI, etc.) should continue to be investigated via fireball observation networks. Spectroscopy of incoming bolides only marginally helps precisely classify the incoming material (iron meteorites only). To reach a statistically significant sample of recovered meteorites along with accurate orbits (>100) within a reasonable time frame (10–20 years), the optimal solution may be the spatial extension of existing fireball observation networks.
3

Costa, Benilde F. O., Eduardo Ivo Alves, Pedro A. O. C. Silva und António C. Batista. „57Fe Mössbauer Analysis of Meteorites and Tektites“. Minerals 11, Nr. 6 (12.06.2021): 628. http://dx.doi.org/10.3390/min11060628.

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This review presents studies on iron meteorites (Campo del Cielo fall and an unregistered iron meteorite), an unregistered stony meteorite from Northwest Africa, and 13 tektites from the American, European, and Australasian strewn fields. The main experimental technique used in the studies was Mössbauer spectroscopy, both in transmission and backscattering geometries. For the latter, a MIMOS II spectrometer was used. Additionally, optical and scanning electron microscopies and X-ray diffraction were used. In the studied iron meteorites, kamacite is found as the main mineral. Campo del Cielo meteorite exhibits Widmanstätten patterns and schreibersite inclusions. The unregistered iron meteorite has Neumann lines and schreibersite inclusions. We have assigned Campo del Cielo as an octahedrite and the unregistered iron meteorite as a hexahedrite. The unregistered stony meteorite is composed mainly of iron-free silicates; at 4.2 K, the spectrum indicates maghemite and 1% troilite. The Cambodian tektite appeared individualized from other australasites, unlike the moldavite, which tends to cluster with them. Our analyses do not allow dismissing doubts on the provenance of tibetanites. The Fe3+/Fe2+ ratio was found to be higher for Muong Nong-type tektites than for splash-form tektites, as expected from their morphology and solidification from melt at lower temperature.
4

Wagle, Bivu, Kaustuv Regmi und Krishna Prasad Adhikari. „Study of Fall Meteorites Over a Century (1922-2021)“. BMC Journal of Scientific Research 5, Nr. 1 (31.12.2022): 97–105. http://dx.doi.org/10.3126/bmcjsr.v5i1.50680.

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Fall meteorites represents to those meteorites whose fall has been witnessed and are later collected from earth surface for further studies. Mass, number of fall events, types, type mass and mass trend of observed fall meteorites are analyzed over a period of recent century (1922-2021) in this paper. The total number of fall meteorites was found to be 706 with total mass of 42800 kg. Decade 2012-2021 and 1932-1941 had the highest number of recorded fall which was 94 times and 89 times respectively. Type L6 meteorite was found to have the greatest number of falls which is 151 times, followed by type H5 and L5 with 109 times and 55 times respectively. The meteorite of type, Iron III AB had the greatest meteorites mass of 23480 kg followed by H5 and L6 with mass 6615 kg and 2347.362 kg respectively. The massive meteorite fall of this century was of Iron III AB type (1947) which weighed 23 tones. The decade 1942-1951 had the highest fall meteorites mass of 24806kg and 1972-1981 had 4858 kg. Various regression model is fitted for the trend analysis of the mass. Over a period of this century, meteorites having mass greater than 100 kg has struck the earth for 32 times while mass greater than 1000 kg has struck for 6 times. The average time between two impacts of meteorite with mass greater than 100kg was calculated to be 3.12 years while mass greater than 1000 kg was found to be 16.6 years.
5

PEREIRA, GONZALO. „¿TIENEN EL MISMO ORIGEN LOS METEORITOS METÁLICOS ENCONTRADOS EN BOLIVIA?“ Revista Boliviana de Física 38, Nr. 38 (30.11.2021): 10–14. http://dx.doi.org/10.53287/eohr3986hv72b.

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While reconstructing the history of meteorites related to Bolivia, we found that the only two metallic meteorites classified as “Found in Bolivia” are the Bolivia and Pooposo meteorites. They are classified within the group of MG IAB iron meteorites and have a similar history. Both were seriously mishandled before reaching the hands of meteorite experts and were commercialized by a priest. In light of these possible matches, some experts have recommended a comparative study of both meteorites to ascertain if they could be part of the same object. In this paper we analyze the data of abundant chemical elements found in both meteorites. The data was obtained from different analyses carried out on all known iron meteorites through methods such as: Radiochemical Neutron Activation Analysis (RNAA) and Instrumental Neutron Activation Analysis (INAA). These data have been published by different researchers: Buchwald (1975a); Scott (1978); Kracher et al. (1980); Wasson & Kallemeyn (2002). Our objective has been to determine if both specimens are part of a larger object that impacted on the surface of the Oruro plateau or if they are simply two independent iron meteorites.
6

Minčeva-Šukarova, Biljana. „Meteorite Struga – overview of previous chemical and recent spectroscopic analyses“. Macedonian Journal of Chemistry and Chemical Engineering 28, Nr. 1 (15.06.2009): 41. http://dx.doi.org/10.20450/mjcce.2009.220.

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Meteorite Struga fell more than 35 years ago near the town of Struga, Republic of Macedonia. Its fall was notified in the Bulletien of the Geological Institute in Skopje in 1973. Since that time, only one chemical analysis has been reported (in 1990) and most recently, preliminary spectrosocpic investigations (in 2006 and in 2008) have been performed. However, this meteorite has not yet been classified in the World’s Database of Meteorites. The aim of this paper is to collect and summarize all available data published until now on this meteorite and open the possibility to clasify it and list it in the World’s Database of Meteorites. In order to make the results more available, the details of the previous chemical and the recent spectrosocpic analyses on this meteorite are presented in this paper. Collected information from both analyses were used for the description of the characteristics of this meteorite. Previous chemical analysis and the recent spectrosocpic investigations are in good agreement and confirm the earlier classification of this meteorite as stony chondrite of H type.
7

Martins, Zita. „Organic molecules in meteorites“. Proceedings of the International Astronomical Union 11, A29B (August 2015): 411–15. http://dx.doi.org/10.1017/s1743921316005676.

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AbstractThe analysis of the organic content of meteorites provides a window into the conditions of the early solar system, such as the extension of aqueous alteration or thermal metamorphism on the meteorite parent bodies. The analysis of the soluble organic content of CM chondrites indicates that extensive aqueous alteration on their meteorite parent body may result on 1) the decomposition of α-amino acids; 2) synthesis of β- and γ-amino acids; 3) higher relative abundances of alkylated polycyclic aromatic hydrocarbons (PAHs); and 4) higher L-enantiomer excess (Lee) value of isovaline. Exogenous delivery of organic matter by meteorites may have contributed to the organic inventory of the early Earth, providing a diversity of resources to the first living organisms on Earth and on other places of our solar system where life could have potentially originated.
8

Rai, Abhishek K., Jayanta K. Pati, Christian G. Parigger, Sonali Dubey, Awadhesh K. Rai, Balen Bhagabaty, Amulya C. Mazumdar und Kalpana Duorah. „The Plasma Spectroscopic Study of Dergaon Meteorite, India“. Molecules 25, Nr. 4 (22.02.2020): 984. http://dx.doi.org/10.3390/molecules25040984.

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Meteorites are the recoverable portions of asteroids that reach the surface of the Earth. Meteorites are rare extraterrestrial objects studied extensively to improve our understanding of planetary evolution. In this work, we used calibration-free laser-induced breakdown spectroscopy (CF-LIBS) to evaluate the quantitative elemental and molecular analyses of the Dergaon meteorite, a H 4-5 chondrite fall sample from Assam, India. Spectral signatures of H, N, O, Na, Mg, Al, Si, P, K, Ca, Ti, Cr, Mn, Fe, Co, Ni, andIrweredetected. Along with the atomic emission, this work reports the molecular emission from FeO molecules. The concentration of the measured elements obtained using CF-LIBS is in close agreement with earlier reports. The elements H, N, and O and their concentrations are estimated by using CF-LIBS for the first time. This study applies laser spectroscopy to establish the presence of Ni, Cr, Co, and Ir in meteorites. The elemental analysis forms the basis for the establishment of the potential molecular composition of the Dergaon meteorite. Moreover, the elemental analysis approach bodes well for in-situ analyses of extraterrestrial objects including applications in planetary rover missions.
9

Cooper, George, Andro Rios und Michel Nuevo. „Monosaccharides and Their Derivatives in Carbonaceous Meteorites: A Scenario for Their Synthesis and Onset of Enantiomeric Excesses“. Life 8, Nr. 3 (27.08.2018): 36. http://dx.doi.org/10.3390/life8030036.

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Carbonaceous meteorites provide the best glimpse into the solar system’s earliest physical and chemical processes. These ancient objects, ~4.56 billion years old, contain evidence of phenomena ranging from solar system formation to the synthesis of organic compounds by aqueous and (likely) low-temperature photolytic reactions. Collectively, chemical reactions resulted in an insoluble kerogen-like carbon phase and a complex mixture of discrete soluble compounds including amino acids, nucleobases, and monosaccharide (or “sugar”) derivatives. This review presents the documented search for sugars and their derivatives in carbonaceous meteorites. We examine early papers, published in the early 1960s, and note the analytical methods used for meteorite analysis as well as conclusions on the results. We then present the recent finding of sugar derivatives including sugar alcohols and several sugar acids: The latter compounds were found to possess unusual “d” enantiomeric (mirror-image) excesses. After discussions on the possible roles of interstellar grain chemistry and meteorite parent body aqueous activity in the synthesis of sugar derivatives, we present a scenario that suggests that most of Earth’s extraterrestrial sugar alcohols (e.g., glycerol) were synthesized by interstellar irradiation and/or cold grain chemistry and that the early solar disk was the location of the initial enantiomeric excesses in meteoritic sugar derivatives.
10

Boaca, Ioana, Maria Gritsevich, Mirel Birlan, Alin Nedelcu, Tudor Boaca, François Colas, Adrien Malgoyre, Brigitte Zanda und Pierre Vernazza. „Characterization of the Fireballs Detected by All-sky Cameras in Romania“. Astrophysical Journal 936, Nr. 2 (01.09.2022): 150. http://dx.doi.org/10.3847/1538-4357/ac8542.

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Abstract Some of the fields of research that have captured the persistent interest of both scientists and the general public are meteor phenomena. The main goal in the study of meteoroid impacts into Earth’s atmosphere is the recovery of the remnant matter after the ablation in the form of meteorites. This is a complementary approach, yet cheap alternative, to a sample return mission. Meteoroids are messengers since the time of the formation of the solar system due to the fact that they have preserved the same composition. The study of meteorites provides information regarding the chemical composition from which the planets formed. The increasing number of all-sky camera networks in recent years has resulted in a large set of events available for study. Thus, it is very important to use a method that determines whether the meteoroid could produce a meteorite or not. In this paper we study the meteors detected by the FRIPON network in Romania with the use of all-sky cameras. We focus on the events with noticeable deceleration (V f /V 0 < 0.8). We determine the ballistic coefficient α and the mass-loss parameter β for the selected sample. Based on this analysis the events are classified in three categories: (1) meteoroids that are likely to produce meteorites; (2) meteoroids that can possibly produce meteorites; (3) meteoroids that are unlikely to produce meteorites. The entry and final mass are determined for each event. From the recorded fireballs, we identified one possible meteorite dropper, and we analyzed its dynamical evolution.
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Zeitschriftenartikel Dissertationen Bücher

Dissertationen zum Thema "Meteorites Analysis":

1

Malvin, Daniel Joshua 1959. „EXPERIMENTAL PARTITIONING OF SIDEROPHILE ELEMENTS IN THE SYSTEMS IRON - NICKEL - SULFUR - PHOSPHORUS AND FORSTERITE - ANORTHITE - DIOPSIDE“. Thesis, The University of Arizona, 1987. http://hdl.handle.net/10150/276501.

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Partition coefficients in the Fe-Ni-S-P system measured utilizing "static" equilibration experiments cannot be reconciled with the results of "dynamic" experiments which mimic fractional crystallization. New tests of the "static" experiments demonstrate that they yield reliable equilibrium Ni, P and Ge partition coefficients. Partition coefficients in the Fe-Ni-S-P system are well matched by interpolation between the Fe-Ni-S and Fe-Ni-P subsystems. The crystal/liquid partitioning of Ga and Ge has been measured experimentally between forsterite, diopside, anorthite and spinel and melts in the forsterite-diopside-anorthite system. The coefficients for the exchange of Ga and Al and the exchange of Ge and Si between minerals and melts are within a factor of two of unity. Application of these results to the interpretation of natural basaltic samples demonstrates that Ga/Al and Ge/Si ratios can be used to discriminate between different mantle source regions.
2

Shober, Patrick M. „Meteoroid Orbital Analysis: Connecting Meteorites and Asteroids“. Thesis, Curtin University, 2021. http://hdl.handle.net/20.500.11937/86776.

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Since people started studying meteorites, scientists have attempted to better understand the parent bodies they originated from. Although, this is difficult because, unlike a terrestrial rock, you do not have access to the outcrop. The Near-Earth Object (NEO) population is the source of all meteorites found on Earth. Using the orbital data collected from the Desert Fireball Network, my work clarified the connections between meteorites and their source NEOs. I primarily did this analysis by employing rigorous numerical modeling techniques to constrain the dynamical and physical properties of asteroidal debris.
3

Hontsova, S. S., und E. M. Maksimova. „X-Ray analysis of meteorite“. Thesis, Sumy State University, 2014. http://essuir.sumdu.edu.ua/handle/123456789/39427.

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Meteorites are one of the most accessible objects of extraterrestrial matter. Therefore the study of the structural features and physical properties of crystals of meteorites can provide information about the formation of the crystal structure of matter in extraterrestrial conditions.
4

Spitz, Anna Hargrave, und Anna Hargrave Spitz. „Trace element analysis of ureilite meteorites and implications for their petrogenesis“. Diss., The University of Arizona, 1991. http://hdl.handle.net/10150/185743.

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Ureilite meteorites are the second largest class of achondrite meteorites. They are perhaps the most enigmatic of all classes of meteorites and the dilemma over how they were formed has perplexed the meteoritic community for over a decade. This research was undertaken to illuminate the details of the petrogenesis of ureilites through the collection of trace element data. The results presented here indicate that many of the petrogenesis hypotheses promoted are no longer tenable and that the available data on ureilites are not sufficient to unravel the mystery of their origin. This dissertation discusses the data collected using two techniques: neutron activation analysis and inductively coupled plasma-mass spectrometry. Specific procedures required to study the ureilites (due to low concentrations of some trace elements) are delineated. Results are presented for the following elements: Ca, Co, Zn, Ga, Cu, Cs, Rb, Sr, Mo, Y, Ba, REE, Hf, W, Re and Ir. The results lead to the conclusion that the ureilites must be considered a mixture of materials--an original ultramafic rock formed by melting of processed source material combined with carbonaceous material added after the ultramafic formation. This conclusion explains the trace element chemical signatures and is supported by the age information obtained from Sm-Nd and Rb-Sr isotopic systems.
5

Daly, Luke. „Understanding Our Protoplanetary Disk by Chemical Analysis of Components in Meteorites“. Thesis, Curtin University, 2017. http://hdl.handle.net/20.500.11937/59045.

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This thesis has explored the capability of novel high resolution in situ analyses such as Synchrotron radiation, atom probe microscopy and transmission kikuchi diffraction in the analyses of primitive meteorites. Crystallographic, geochemical and isotopic data extracted using these techniques from refractory metal nuggets in primitive meteorites has implications for our understanding of how these grains formed, particle migration in the protoplanetary disk, and a suggestion that refractory metal nuggets may have a pre-solar origin.
6

Armstrong, Katherine. „Chemical and Petrographic Survey of Large, Igneous-Textured Inclusions in Ordinary Chondrites“. PDXScholar, 2014. https://pdxscholar.library.pdx.edu/open_access_etds/2070.

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Our inventory of material from the early solar system includes large, igneous-textured inclusions in O chondrites, whose origin and relationship to their host meteorite is unclear. These inclusions occur in approximately 4% of O chondrites, and are mineralogically, petrographically, and chemically diverse. Petrographic and chemical data from 29 inclusions from 23 host meteorites were collected with optical light and scanning electron microscopy, allowing for the determination of major phase modal abundance and major element bulk chemistry. No correlation between any inclusion property and host meteorite type were found, but some trends were observed. Nine of the inclusions show strong evidence, such as radial variations in texture and chemistry, for having crystallized as a free-floating droplet in a space environment, and may share the same formation process as chondrules. One inclusion is almost certainly shock-melted material that intruded into the host material. Thirteen inclusions have bulk chemistry patterns that suggest the material was vapor fractionated; the remaining sixteen are essentially chondritic, i.e., unfractionated. Broadly, the data support the conclusions of Ruzicka et al. (1998, 2000), which divided large inclusions into Na-poor (vapor fractionated) and Na-rich (unfractionated) groups, suggesting at least two different origins. There is no evidence that any of the inclusions studied formed by igneous differentiation.
7

Schepker, Kristy Lee. „Complex Thermal Histories of L Melt Breccias NWA 5964 and NWA 6580“. PDXScholar, 2014. https://pdxscholar.library.pdx.edu/open_access_etds/1835.

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To constrain the thermal histories of two complex L chondrite melt breccia samples (NWA 5964 and NWA 6580) we compare textures and chemical compositions of metal and sulfide to L melt rock (NWA 6454 and NWA 6579) and strongly shocked (shock stage S6) (NWA 4860) samples. The inferred thermal histories can be used to evaluate formation settings on the L chondrite parent body. The L melt samples probably formed as different melt units within warm but largely unmelted material relatively close to the surface of the parent body, and the same is true for the S6 sample, except it experienced less melting. The breccia samples likely formed deeper, below different impact craters, by the injection of shock melt into a cooler chondritic basement. Carbide grains in the melt breccias could have formed by a contact metamorphic process caused by heating of the chondritic basement in proximity to the melt. Within the melt regions of the various samples, inferred cooling rates are on the order of 1-10 °C/sec, whereas in the chondritic portions of the melt breccias, the inferred cooling rates are many orders of magnitude slower, ~1-100 °C/My. The complex intergrowths of metal and FeS (hereafter referred to as dendritic grains) within the melt are recording cooling rates above the metal-sulfide eutectic, while the metal grains outside of the melt regions are recording cooling rates at much lower temperatures. It is likely the melt regions in the breccias cooled substantially prior to coming to rest against the chondritic basement, and thereafter the melt-chondrite rocks cooled more slowly.
8

Maksimova, E. M., S. S. Hontsova und I. A. Nauhatsky. „XRD Analysis of Crystal Structure of the Fragment of the Campo Del Cielo Meteorite“. Thesis, Sumy State University, 2015. http://essuir.sumdu.edu.ua/handle/123456789/40668.

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Meteorites are the key, and often the only source of information about the pre-planetary and planetary early history of our solar system. Currently, the following classification of meteorites: stone (aerolites) stoney-iron (siderolites) and iron (siderites), depending on the ratio of silicate minerals in them, and nickel-iron.
9

Hays, Naydene Richelle. „Geochronology of Shergottite Meteorites: Using LA-MC-ICP-MS Analysis to Examine U-Th-Pb Systematics of Baddeleyites and Phosphates“. Thesis, The University of Arizona, 2011. http://hdl.handle.net/10150/202753.

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I present in-situ analysis of U-Pb systematics in baddeleyite and whitlockite grains from a suite of Martian shergottites. 9 baddeleyite grains (5 from basaltic shergottite NWA 2986 and 4 from olivine-phyric shergottite RBT 04262) were analyzed by LA-MC-ICP-MS. Despite low uranium and radiogenic lead concentrations , maximum ages could be determined for both samples: 187 ± 50 to 1236 ± 430 for NWA 2986 and 100 ± 9 to 526 ± 48 for RBT 04262. The same analytical procedures were used for whitlockites in NWA 2986, ALHA 77005, EETA 79001, NWA 2646 and LAR 06319. As with the baddeleyite analyses, maximum ages were calculated. These ages ranged from 110 ± 1 for LAR 06319 to 561 ± 185 for NWA 2646. These results, which are consistent with previous analyses, mean that the ~ 4 Ga age determined from Pb-Pb analyses cannot time the igneous crystallization of these meteorites.
10

Joy, Katherine H. „Topics in lunar evolution using sample analysis and remotely sensed information“. Thesis, University College London (University of London), 2007. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.606784.

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Bücher zum Thema "Meteorites Analysis":

1

I͡Udin, I. A. Mineralogii͡a meteoritov. Sverdlovsk: Akademii͡a nauk SSSR, Uralʹskiĭ nauch. t͡sentr, 1987.

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2

Wilson, Graham C. Petrographic notes on miscellaneous samples: Ten slags and glassy materials, seven alkaline rocks and five mafic-ultramafic rocks : miscellaneous observations on behalf of slag, meteorite and ore deposits research. Toronto: Turnstone Geological Services, 2000.

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3

Mog, R. A. Global nonlinear optimization of spacecraft protective structures design. [Marshall Space Flight Center, Ala.]: National Aeronautics and Space Administration, George C. Marshall Space Flight Center, 1990.

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4

United States. National Aeronautics and Space Administration, Hrsg. Lunar sample analysis: Final report for the period February 3, 1971 through October l, 1986. [Thousand Oaks, CA]: Rockwell International Science Center, 1986.

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5

Eugene, Jarosewich, Clarke Roy S und Barrows Julie N, Hrsg. The Allende meteorite reference sample. Washington, D.C: Smithsonian Institution Press, 1986.

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6

United States. National Aeronautics and Space Administration., Hrsg. Lunar sample analysis: Annual report 13 for the period January 1, 1984 through December 3l, 1984. [Thousand Oaks, CA]: Rockwell International Science Center, 1985.

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7

Farrington, Oliver C. Analysis Of Iron And Stone Meteorites - Field Columbian Museum. Merchant Books, 2006.

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8

K, Nishiizumi, und United States. National Aeronautics and Space Administration., Hrsg. Exposure history of lunar meteorites Queen Alexandra Range 93069 and 94269. [Washington, DC: National Aeronautics and Space Administration, 1996.

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9

G, Sears D. W., und United States. National Aeronautics and Space Administration., Hrsg. Meteorite infall and transport in Antarctica: An analysis of icefields as accumulation surfaces. [Washington, DC: National Aeronautics and Space Administration, 1997.

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10

G, Sears D. W., und United States. National Aeronautics and Space Administration., Hrsg. Meteorite infall and transport in Antarctica: An analysis of icefields as accumulation surfaces. [Washington, DC: National Aeronautics and Space Administration, 1997.

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Buchteile zum Thema "Meteorites Analysis":

1

Nakai, Izumi, und Atsuo Iida. „Application of SR-XRF Imaging and Micro-XANES to Meteorites, Archaeological Objects and Animal Tissues“. In Advances in X-Ray Analysis, 1307–15. Boston, MA: Springer US, 1992. http://dx.doi.org/10.1007/978-1-4615-3460-0_79.

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Becker, Luann. „Application of Laser Desorption Mass Spectrometry (LDMS) to Cosmogeochemistry: Direct Analysis of Organic Compounds in Meteorites“. In Laboratory Astrophysics and Space Research, 377–98. Dordrecht: Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-011-4728-6_14.

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Cronin, John R., und Sherwood Chang. „Organic Matter in Meteorites: Molecular and Isotopic Analyses of the Murchison Meteorite“. In The Chemistry of Life’s Origins, 209–58. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-1936-8_9.

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Xie, Xiande, und Ming Chen. „Neutron Activation Analysis of Trace Elements in Yanzhuang“. In Yanzhuang Meteorite: Mineralogy and Shock Metamorphism, 205–22. Singapore: Springer Singapore, 2020. http://dx.doi.org/10.1007/978-981-15-0735-9_11.

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Xie, Xiande, und Ming Chen. „LA-ICP-MS Analysis of Trace Elements in Yanzhuang“. In Yanzhuang Meteorite: Mineralogy and Shock Metamorphism, 223–37. Singapore: Springer Singapore, 2020. http://dx.doi.org/10.1007/978-981-15-0735-9_12.

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Xie, Xiande, und Ming Chen. „PIXE Analysis of Trace Elements in Eutectic FeNi-FeS Blobs“. In Yanzhuang Meteorite: Mineralogy and Shock Metamorphism, 239–46. Singapore: Springer Singapore, 2020. http://dx.doi.org/10.1007/978-981-15-0735-9_13.

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Wallenwein, R., H. Blank, E. K. Jessberger und K. Traxel. „Proton Induced X-Ray Emission (PIXE) Analysis of Meteoritic Microsamples“. In Properties and Interactions of Interplanetary Dust, 157–58. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5464-9_33.

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Martin, Ellinor, Birger Schmitz, Fredrik Terfelt, Luis Erick Aguirre-Palafox und Walter Alvarez. „The micrometeorite flux in the Albian–Aptian age (ca. 103–117 Ma): A search for Tycho ejecta in pelagic sediments using chrome spinels“. In From the Guajira Desert to the Apennines, and from Mediterranean Microplates to the Mexican Killer Asteroid: Honoring the Career of Walter Alvarez. Geological Society of America, 2022. http://dx.doi.org/10.1130/2022.2557(23).

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ABSTRACT Numerical models of meteorite delivery from impacts on the Moon have demonstrated that the impact event forming the lunar crater Tycho (~85 km diameter; ca. 109 Ma age) would have delivered considerable amounts of ejected material to Earth. The ejecta, containing lunar Ti- and V-rich chrome spinels, would have been distributed globally and admixed with seafloor sediments over a few meters of a typical marine stratigraphic interval. In order to locate such ejecta, samples weighing ~12–25 kg each, with one-meter spacing were extracted over an ~30 m interval of the deep-sea formed Calera Limestone, Albian and Aptian age (ca. 103–117 Ma), from the Pacifica Quarry, south of San Francisco. The limestone samples were leached in acids and residues searched for possible lunar Ti-rich chrome-spinel grains. In a total of 689 kg of limestone, 1154 chrome-spinel grains were found. Of these, 319 contain &gt;0.45 wt% V2O3, of which 227 originate from equilibrated ordinary chondrites. The majority of the other 92 grains with &gt;0.45 wt% V2O3 are most likely from different types of achondritic meteorites. Among these, we found eleven particularly Ti-rich chrome-spinel grains. The elemental abundances of these grains were compared with chrome spinel from lunar, howardite-eucrite-diogenite (HED) and R-chondritic meteorites. This showed that only one of these grains could potentially be of lunar origin. The bulk of the other grains likely originate from HED meteorites based on oxygen isotopic analysis of similar grains in previous studies. Grains with TiO2 &gt;10 wt%, common among lunar spinels are not found, further supporting an HED source for the Ti-rich grains. In summary, Albian and Aptian strata in the Pacifica quarry do not likely record any major lunar impact event. Either the timing of the impact is located within a ca. 110–114 Ma unconformity in the middle part of the section or the impact is likely older than the interval searched.
9

Adam, John A. „Tsunamis“. In Rays, Waves, and Scattering. Princeton University Press, 2017. http://dx.doi.org/10.23943/princeton/9780691148373.003.0013.

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This chapter describes a mathematical model of tsunami propagation (transient waves). A tsunami is a series of ocean waves triggered by large-scale disturbances of the ocean, including earthquakes, as well as landslides, volcanic eruptions, and meteorites. Tsunamis have very long wavelengths (typically hundreds of kilometers). They have also been called “tidal waves” or “seismic sea waves,” but both terms are misleading. The chapter first considers the boundary-value problem before modeling two special cases of tsunami generation, one due to an initial displacement on the free surface and the other due to tilting of the seafloor. It also discusses surface waves on deep water and how fast the wave energy propagates and concludes with an analysis of leading waves due to a transient disturbance.
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Zipfel, Jutta. „Isotopic analyses of primitive meteorites“. In Planetary Mineralogy. Mineralogical Society of Great Britain and Ireland, 2015. http://dx.doi.org/10.1180/emu-notes.15.7.

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Konferenzberichte zum Thema "Meteorites Analysis":

1

Klöck, W., und F. J. Stadermann. „Mineralogical and chemical relationships of interplanetary dust particles, micrometeorites, and meteorites“. In Analysis of interplanetary dust: NASA/LPI workshop. AIP, 1994. http://dx.doi.org/10.1063/1.46523.

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Gibson, Everett K., und Roberta Bustin. „Volatiles in interplanetary dust particles: A comparison with volatile-rich meteorites“. In Analysis of interplanetary dust: NASA/LPI workshop. AIP, 1994. http://dx.doi.org/10.1063/1.46533.

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Ananthachar, Adarsh, Unnikrishnan V.K., Santhosh C und Surya Harikrishnan. „Elemental analysis of meteorites using laser-induced breakdown spectroscopy (LIBS)“. In Astronomical Optics: Design, Manufacture, and Test of Space and Ground Systems, herausgegeben von Pascal Hallibert, Tony B. Hull und Dae Wook Kim. SPIE, 2018. http://dx.doi.org/10.1117/12.2285922.

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Nakazato, Masaki, Shuji Yamashita und Takafumi Hirata. „Elemental Analysis of Individual Nanograins in Meteorites by ICP-TOF-MS“. In Goldschmidt2020. Geochemical Society, 2020. http://dx.doi.org/10.46427/gold2020.1886.

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Joy, Katherine, Jane MacArthur, Thomas Harvey und Rhian Jones. „The Lost Meteorites of Antarctica: Field campaigns and coordinated sample analysis approach to preliminary scientific study“. In Goldschmidt2021. France: European Association of Geochemistry, 2021. http://dx.doi.org/10.7185/gold2021.4762.

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Cavell, Ronald G. „Hard X-Ray Spectro Microprobe Analysis of Inhomogeneous Solids: A Case Study. Element Distribution and Speciation in Selected Iron Meteorites“. In PORTABLE SYNCHROTRON LIGHT SOURCES AND ADVANCED APPLICATIONS: International Symposium on Portable Synchrotron Light Sources and Advanced Applications. AIP, 2004. http://dx.doi.org/10.1063/1.1796579.

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Vaci, Zoltan. „ELECTRON PROBE MICROANALYSIS, MICRO X-RAY DIFFRACTION, AND DEUTERIUM-HYDROGEN ANALYSIS OF HYDROUS ALTERATION IN MARTIAN METEORITES NORTHWEST AFRICA 10416 AND 8159“. In 68th Annual Rocky Mountain GSA Section Meeting. Geological Society of America, 2016. http://dx.doi.org/10.1130/abs/2016rm-276180.

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Potapov, Sergey Sergeevich, Natalya Vladimirovna Parshina, Vladimir Pavlovich Lyutoev und Roman Andreevich Filenko. „Results of studying the mineral composition of the supposed Yablonovy meteorite“. In Проблемы минералогии, петрографии и металлогении. Научные чтения памяти П. Н. Чирвинского. ПЕРМСКИЙ ГОСУДАРСТВЕННЫЙ НАЦИОНАЛЬНЫЙ ИССЛЕДОВАТЕЛЬСКИЙ УНИВЕРСИТЕТ, 2022. http://dx.doi.org/10.17072/chirvinsky.2022.209.

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Using a complex of methods (X-ray phase analysis, X-ray fluorescence semi-quantitative chemical analysis, Infrared Fourier spectroscopy, synchronous thermal analysis), the mineral composition of the supposed Yablonovy meteorite from Transbaikalia was studied. It was found that the sample consists of native iron (practically free of nickel impuritie; Ni - 0.18 %), okermanite, melilite (gelenite), magnetite, goethite, calcite, siderite, which does not correspond to the composition of meteorite matter. The found sample is nothing more than a slag with a large amount of a metallic iron alloy of some, not yet established, historical metallurgical production on the territory of Transbaikalia.
9

Kruglikov, N. A., A. Yu Pastuhovich, G. A. Yakovlev, V. I. Grokhovsky und O. Unsalan. „Analysis of the bright fireball over Turkey on may 27, 2020 followed by meteorite recovery campaign“. In Всероссийская с международным участием научная конференция студентов и молодых ученых, посвященная памяти Полины Евгеньевны Захаровой «Астрономия и исследование космического пространства». Ural University Press, 2021. http://dx.doi.org/10.15826/b978-5-7996-3229-8.30.

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Bright fireball on May 27, 2020 was imaged in a lot of points in Turkey, Georgia and Armenia, as well as from Stavropol Region (Russia). Based on these observations we present results on luminous trajectory reconstruction which led to several meteorite expeditions in next few months.
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Sitek, J., J. Dekan, J. Degmová und K. Sedlačková. „Phase analysis of Košice meteorite: Preliminary results“. In MOSSBAUER SPECTROSCOPY IN MATERIALS SCIENCE - 2012: Proceedings of the International Conference MSMS-12. AIP, 2012. http://dx.doi.org/10.1063/1.4759485.

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