Elemental Abundances in the Haverö Meteorite

Gillum, D. E.; Janghorbani, Morteza; Miller, M. D.; Chyi, L. L.; Ehmann, W. D.

doi:10.1111/j.1945-5100.1972.tb00139.x

Cited by 8 publications

(2 citation statements)

References 8 publications

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“…Except for isolation of siderophile elements at right, elements are sequenced according to solar nebula condensation temperature (Wasson, 1985), decreasing toward the right. Shown for comparison are averages for Nilpena and North Haig (McCall and Cleverly, 1968;Bogard et al, 1973;Binz et al, 1975;Jaques and Fitzgerald, 1982;Grady et al, 1985) and an average for ordinary ureilites (many sources, but most notably, for seldom-determined elements: Gillum et al, 1972;Wanke et al, 1972;Binz et al, 1975;Boynton et al, 1976;Higuchi et al. 1976;Wasson et al, 1976;Kolesov, 1976;Jarosewich, 1980;Goodrich et al, 1987b;and Janssens et al, 1987).…”

Section: Resultsmentioning

confidence: 99%

Geochemistry of polymict ureilite EET83309, and a partially‐disruptive impact model for ureilite origin

Warren

Kallemeyn

1989

Meteoritics

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For most elements, polymict ureilite EET83309 shows no significant compositional difference from other ureilites, including ordinary ("monomict") ureilites. Polymict ureilites appear to be mixtures of a wide variety of ordinary ureilites, with little dilution by "foreign" extra-ureilitic materials. Thus, they apparently were mixed (i.e.• the ureilites in general formed) on a very small number of parent bodies. In one respect, polymict ureilites do stand out. Along with the only other polymict ureilite that has been analyzed for REE (Nilpena), EET83309 has much higher concentrations of light-middle REE than most ordinary ureilites. Despite these relative enrichments in LREE, polymict ureilites are nearly devoid ofbasaltic (Al-rich) material. A basaltic component should have formed along with (and presumably above) the ultramafic ureilites, in any closed-system differentiation ofan originally chondritic asteroid. This scarcity ofcomplementary basaltic materials may be an important clue to ureilite origins. We suggest that ureilites originated as paracumulates (mushy, cumulate-like, partial melt residues) deep within a primordiallyheated asteroid or asteroids. While still largely molten, the asteroid was severely disrupted, and most of its external basaltic portion was permanently blown away, by impact ofa large, C-rich projectile. This partially-disruptive impact tended to permeate the paracumulates with C-rich, noble-gas-rich, and IOO-rich magma derived mainly from shock-melting of the projectile. After reaccumulation and cooling, the resultant mixtures of cumulus mafic silicates with essentially "foreign" C-matrix became "monomict" ureilites. Further small impacts produced polymict ureilites as components of a newly-developed, basalt-poor megaregolith. The consistently moderate pyroxene/olivine ratios of the ureilites are as expected for partial melt residues, but not for cumulate (sensu stricto) rocks. The final projectile/target mixing ratio tended to be greatest among the more magnesian and pyroxene-rich portions of the paracumulate, because these portions were lowest in density, and thus concentrated toward the upper surface of the paracumulate layer. As a result, ureilites show correlations among C,~J70, and silicate-core mg. This model appears to reconcile many paradoxical aspects of ureilite composition (primitive, near-chondritic, except depleted in basalt, diverse~170) and petrography (igneous, cumulate-like).

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Section: Resultsmentioning

confidence: 99%

Geochemistry of polymict ureilite EET83309, and a partially‐disruptive impact model for ureilite origin

Warren

Kallemeyn

1989

Meteoritics

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“…TiO 2 is very Uncertainties are shown where they are larger than normal 70% confidence levels (i.e., ''normal'' for moderate-high concentrations). Abbreviations: B75, Binz et al (1975); B76, Boynton et al (1976); BH93, Boynton and Hill (1993); G72, Gillum et al (1972); G87, Goodrich et al (1987); H76, Higuchi et al (1976); H78, Hintenberger et al (1978); J70, Jerome (1970); J87, Janssens et al (1987); J90, Jarosewich (1990); JF82, Jaques and Fitzgerald (1982); K.U. Krahenbuhl (unpublished); MC68, McCall and Cleverly (1968); S72, Schmitt et al (1972); S92, Spitz (1992); SB91, Spitz and Boynton (1991); W72, Wiik (1972); W76, Wasson et al (1976); WK92, Warren and Kallemeyn (1992); and WL95, Wang and Lipschutz (1995 marginally higher than in any of the comparison pyroxenes, but among Wo $ 5 ureilitic pyroxenes, that of Y-74130 (which, however, is distinctly ferroan, mg = 79: Tak eda, 1987) shows a precise match (0.13 wt% TiO 2 ).…”

Section: Samplesmentioning

confidence: 99%

Siderophile geochemistry of ureilites: A record of early stages of planetesimal core formation

Warren¹,

Ulff-Møller²,

Huber³

et al. 2006

Geochimica et Cosmochimica Acta

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The Haver� meteorite

Vdovykin

1975

Space Sci Rev

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The meteorite Haver6, which fell on 2 August 1971 in Finland is a representative of a rare, but highly interesting group of stony meteorites -ureihtes. Like other ureilites it is enriched in carbon (up to 2 ~) chiefly represented by diamond and graphite. The meteorite is strongly recrystallized; as a result its chief mineral component -olivine -has been transformed into a mosaic of small grains among which kamacite with an extremely low Ni content (N 1.7 ~) is distributed. Polysynthetic twinning is characteristic of pyroxene grains. The meteorite is penetrated by a system of cavities being stretched approximately in one direction. The cavities are sometimes occupied by kamacite plates containing N 4 % Ni. The peculiarities of the mineral and chemical composition of the meteorite indicate that its material had formed during a disequilibrium process. The content of cosmogenic isotopes witnesses to an unusual orbit of the meteorite.

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Elemental Abundances in the Haverö Meteorite

Cited by 8 publications

References 8 publications

Geochemistry of polymict ureilite EET83309, and a partially‐disruptive impact model for ureilite origin

Geochemistry of polymict ureilite EET83309, and a partially‐disruptive impact model for ureilite origin

Siderophile geochemistry of ureilites: A record of early stages of planetesimal core formation

The Haver� meteorite

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