Differentiated meteorites

Wasson, J. T.

doi:10.1029/eo052i007piu441

Cited by 4 publications

(1 citation statement)

References 219 publications

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“…Meteorites have generally been regarded as either "primitive" (or "chondritic") or "differentiated" [e.g., Wasson, 1971]. These terms actually reflect properties of their parent bodies: Chondrite bodies were never molten, except for occasional minor shock melting, whereas the parent bodies of achondrites, stony-irons, and most iron meteorites were probably fully differentiated into core (metallic), mantle (cumulates and unmelted residua, if any), and crust (basaltic), although brecciation may have obscured these relationships in any given meteorite sample.…”

Section: Introductionmentioning

confidence: 99%

The evolution of partially differentiated planetesimals: Evidence from iron meteorite groups IAB and IIICD

Kracher¹

1985

J. Geophys. Res.

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Group IAB irons probably come from a parent body that partially differentiated into a sulfur‐rich molten core and a primitive silicate outer layer in which only minor or localized melting occurred. Although the complexity of meteorites from this parent body or bodies (irons with and without massive silicate inclusions, stony meteorites like Winona, sulfide‐rich meteorites like Mundrabilla, etc.) implies a complicated history, the partial differentiation model is consistent with most properties of these meteorites. The behavior of five model parent bodies of different composition during heating to 1400 K (the temperature recorded in many I AB silicates) shows that meteorites like IAB irons can form by this process. Sulfide‐rich parent bodies differentiate into a liquid, S‐rich core and a primitive, metal‐bearing mantle around 1230 K, but in parent bodies lower in sulfide abundance this process may be delayed until minor melting of silicates occurs (1370 ± 30 K). In most cases any silicate melt that may have formed resolidified in situ. The sulfide melt fractionally crystallized along the (Fe,Ni)‐FeS cotectic. Some melt was injected into silicates to form Copiapo‐type breccias. Considerations of graphite‐metal‐silicate equilibrium, and the retention of noble gases suggest that brecciated IABs formed at depth inside a moderately large (a few tens to a hundred kilometers) parent body. The correlation of I‐Xe ages with Ni content is interpreted as the result of an excess 129Xe component associated with the S‐rich melt, which increases with melt evolution.

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Section: Introductionmentioning

confidence: 99%

The evolution of partially differentiated planetesimals: Evidence from iron meteorite groups IAB and IIICD

Kracher¹

1985

J. Geophys. Res.

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Meteors and Meteorites

Jager¹

1973

Transactions of the International Astronomical Union Volume XVA

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Report of the Meteorite Committee

Anders¹,

Yavnel²

1973

Trans. Int. Astron. Union

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Work on meteorites has slowed perceptibly since 1969, because many meteoriticists are now working on lunar samples. Nonetheless, progress has been made. Meteorites are providing new clues to traditionally astronomical questions, such as early stellar evolution, interstellar molecules, and composition of comets and asteroids. Numerous reviews have appeared in 1971-72, and the present report will therefore be brief. The 1967-71 U.S. report to the IUGG is a well-referenced, comprehensive source of information (though restricted mainly to U.S. work), with excellent reviews on noble gases (Bogard, 1971), ages (Burnett, 1971), chondrites (Dodd, 1971), and other meteorite classes (Wasson, 1971a). Reviews concerned mainly with meteorites and the early solar system were written by Pellas (1972), Wasson (1972), and Anders (06.107.002; 1972a, b). Interrelations with asteroids and comets as well as with orbital data were discussed by Wetherill and Anders {Coll. 12). A variety of cosmochemical topics are covered in a book by Sobotovich (1971). Data on the chemical composition of meteorites are compiled in a handbook edited by Mason (06.003.027). More specialized reviews or monographs have been published on the following topics: Canyon Diablo meteorite (Vdovykin, 1971), diamonds in meteorites (03.003.133), composition of basaltic achondrites (06.003.031), ureilites (03.105.075), carbonaceous chondrites (05.105.062; Van Schmus and Hayes, 1973), meteorites and interstellar molecules (Anders, 1972c), trace elements in meteoritic minerals (Mason and Graham, 1970), and meteorite craters (05.105.088; Horz and Ronca, 1971). To conserve space, the reference list comprises only reviews and books. Papers are cited in the text by year only, but the reader can trace them through the sources given or through Astronomy and Astrophysics Abstracts.

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Differentiated meteorites

Cited by 4 publications

References 219 publications

The evolution of partially differentiated planetesimals: Evidence from iron meteorite groups IAB and IIICD

The evolution of partially differentiated planetesimals: Evidence from iron meteorite groups IAB and IIICD

Meteors and Meteorites

Report of the Meteorite Committee

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