Meteorites in history: an overview from the Renaissance to the 20th century

Marvin, Ursula B.

doi:10.1144/gsl.sp.2006.256.01.02

Cited by 15 publications

(22 citation statements)

References 58 publications

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“…Here we adopt a broad definition of "eucrite" that does not require the source body to be identified, and return to this question in the final section. Note that the original eucrites were meteorites named by Rose in 1863 (e.g., Greshake, 2006), not terrestrial rocks as commonly believed (e.g., Marvin, 2006).…”

Section: Samples Analyzed and Terminolgymentioning

confidence: 99%

Oxygen isotopic constraints on the origin and parent bodies of eucrites, diogenites, and howardites

Scott

Greenwood

Franchi

et al. 2009

Geochimica et Cosmochimica Acta

148

177

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A few eucrites have anomalous oxygen isotopic compositions. To help understand their origin and identify additional samples, we have analyzed the oxygen isotopic compositions of 18 eucrites and four diogenites. Except for five eucrites, these meteorites have ∆ 17 O values that lie within 2σ of their mean value viz., -0.242±0.016‰, consistent with igneous isotopic homogenization of Vesta. The five exceptional eucrites-NWA 1240, Pasamonte (both clast and matrix samples), PCA 91007, A-881394, and Ibitira-have ∆ 17 O values that lie respectively 4σ, 5σ, 5σ, 15σ, and 21σ away from this mean value. NWA 1240 has a δ 18 O value that is 5σ below the mean eucrite value. Four of the five outliers are unbrecciated and unshocked basaltic eucrites, like NWA 011, the first eucrite found to have an anomalous oxygen isotopic composition. The fifth outlier, Pasamonte, is composed almost entirely of unequilibrated basaltic clasts. Published chemical data for the six eucrites with anomalous oxygen isotopic compositions (including NWA 011) exclude contamination by chondritic projectiles as a source of the oxygen anomalies. Only NWA 011 has an anomalous Fe/Mn ratio, but several anomalous eucrites have exceptional Na, Ti, or Cr concentrations. We infer that the six anomalous eucrites are probably derived from five distinct Vesta-like parent bodies (Pasamonte and PCA 91007 could come from one body). These anomalous eucrites, like many unbrecciated eucrites from Vesta, are probably deficient in brecciation and shock effects because they were sequestered in small asteroids (~10 km diameter) during the Late Heavy Bombardment following ejection from Vesta-like bodies. The preservation of Vesta's crust and the lack of deeply buried samples from the hypothesized Vestalike bodies are consistent with the removal of these bodies from the asteroid belt by gravitational perturbations from planets and protoplanets, rather than by collisonal grinding.

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Section: Samples Analyzed and Terminolgymentioning

confidence: 99%

Oxygen isotopic constraints on the origin and parent bodies of eucrites, diogenites, and howardites

Scott

Greenwood

Franchi

et al. 2009

Geochimica et Cosmochimica Acta

148

177

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“…In contrast, achondrites, representing 8% of meteorites overall [67], are known to pass both stages of melting and differentiation [68]. Their chemical composition and principal minerals (e.g., [69] [70]) are similar to those of magmatic rocks of Earth's crust and upper mantle, and contain PGE amounts (see Table 2 and Table 3) about two orders of magnitude lower than CI carbonaceous chondrites (e.g., [71]) which have about the same level of the PGE content that the Earth's upper mantle rocks. Interestingly, that achondrites do not have chondrules, which most likely were re-worked during melting, differentiation and alteration processes passed by achondrites.…”

Section: On the Formation Of Pges And Pgms And Their Content In Rocksmentioning

confidence: 99%

Concentration of Platinum Group Elements during the Early Earth Evolution: A Review*

Pilchin¹,

Eppelbaum²

2017

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Numerous unique geological processes [1] took place during the early Earth evolution; several of them, especially those occurring in the Hadean-Early Archean and later, are reflected in the modern geological (geophysical, geochemical, etc.) pattern. One such significant enigmatic feature is the preservation of extremely dense and heavy platinum group elements (PGEs): Pt, Pd, Rh, Ru, Ir, Os. Concentration of PGEs during this period could have taken place in two ways: 1) presence of particular matter capable of preserving PGEs near the earth's surface, 2) transportation of PGEs by magma flows from deep lithospheric (asthenospheric) layers (slabs) to the subsurface. Clearly, much of the dense and heavy PGEs did not sink through to the Earth's mantle (core) at the time of the magma-ocean, and occur near Earth's surface in abundances for formation of ore deposits with PGE concentrations found to be 2 -3 orders of magnitude greater than those in their host media. Their enrichments are associated in numerous cases with such enigmatic phenomena as formation of anorthosites and anorthosite-bearing layered magmatic intrusions. PGE deposits and mineralization zones are also found in associations with chromitites, dunites and serpentinites. In this review, problems related to the initial concentration and preservation of PGEs, their association with anorthosites, and formation of layered intrusions are discussed in detail. The main aim of this article is analysis of the requirements-initial concentration and preservation of PGE and PGM (Platinum Group Minerals) during the early Earth evolution, as well as examination of the distribution behavior of some PGEs in different ore deposits and meteorites. It is supposed that meteoritic bombardment of Earth has played a significant role in formation of PGEs deposits. Some conclusions made in this article may be useful for developing and enhancing strategies of prospecting for PGEs deposits.

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“…That meteorites might have their origin in the depths of space was first postulated by the German physicist Ernst Florenz Friedrich Chladni (1756Chladni ( -1827 in 1794 when, following a study of numerous eyewitness accounts, including that of the 1751 I-Iraschina meteorite (that fell in Croatia in 1751), he postulated (see Marvin 1996Marvin , 2006 that there existed small 104 R.J. HOWARTH celestial bodies with compositions similar to planets, which were attracted by the Earth's gravitational field and, falling at great speed, the atmospheric friction heated them and made them luminous. Although it is uncertain whether he ever actually saw a fragment of the Pallas iron, 2 composed of olivine and nickeliferous iron metal and reported to have fallen to Earth from a fireball in Siberia in 1749 (Ivanova & Nazarov 2006), he realized from accounts that its mineralogical composition was quite different to that of known terrestrial rocks.…”

Section: Meteorite Classificationmentioning

confidence: 99%

“…Although systematic collections of meteorites began to be built up at the Natural History Museum of Vienna (under Carl Franz Anton, Ritter von Schreibers (1775-1852, who published a book on the subject in 1820), at the University of Berlin (Chladni 1825) and elsewhere much of the early investigative work on meteorites was conducted by mineralogists and chemists who were largely content to establish the individual compositions of these objects, rather than obtaining an overall view (Marvin 2006).…”

Section: Meteorite Classificationmentioning

confidence: 99%

Understanding the nature of meteorites: the experimental work of Gabriel-Auguste Daubrée

Howarth

2006

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Meteorites in history: an overview from the Renaissance to the 20th century

Cited by 15 publications

References 58 publications

Oxygen isotopic constraints on the origin and parent bodies of eucrites, diogenites, and howardites

Oxygen isotopic constraints on the origin and parent bodies of eucrites, diogenites, and howardites

Concentration of Platinum Group Elements during the Early Earth Evolution: A Review*

Understanding the nature of meteorites: the experimental work of Gabriel-Auguste Daubrée

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