Chondrites: Their metallic minerals, thermal histories, and parent planets

Wood, John A.

doi:10.1016/0019-1035(67)90002-4

Cited by 410 publications

(243 citation statements)

References 60 publications

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“…This suggests a thermal remanent magnetization (TRM), thermo-chemical remanent magnetization (TCRM), or chemical remanent magnetization (CRM), acquired prior to falling to earth. Previous studies on meteorites (summarized by ANDERS, 1971) have presented several strong lines of evidence supporting the contention that some carbonaceous chondrites, including at least some of the C2 chondrites shown in Further evidence suggests that the mineralogical components of carbonaceous chondrites represent relatively unaltered "planetary material" remaining from the early solar system formation (see e. g., WooD, 1967;ANDER5, 1971). It is possible that the magnetization of carbonaceous meteorites may be a depositional remanent magnetization (DRM) Of materials with a previously acquired TRM (BANERJEE and HARGRAVES, 1972;BRECHER, 1972;HERNDON, 1972;WEAVING, 1962b).…”

Section: Carbonaceous Meteoritesmentioning

confidence: 78%

Partial A. F. Demagnetization Studies of 40 Meteorites

Larson

Watson

Herndon

et al. 1973

J. geomagn. geoelec

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Section: Carbonaceous Meteoritesmentioning

confidence: 78%

Partial A. F. Demagnetization Studies of 40 Meteorites

Larson

Watson

Herndon

et al. 1973

J. geomagn. geoelec

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“…An attempt to deduce the cooling rate of minerals in extra-terrestrial materials and their parent body, has been made by WOOD (1964WOOD ( , 1967, GOLDSTEIN and SHORT (1967 a, b) who applied the growth of taenite in iron-nickel alloy to iron and stony-iron meteorites and iron-rich chondrites.…”

Section: Discussionmentioning

confidence: 99%

Evaluation of a crust model of eucrites from the width of exsolved pyroxene.

Miyamoto

Takeda

1977

Geochem. J.

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An attempt has been made to locate known eucrites within a proposed crust model by estimating the absolute cooling rates from the width of exsolution lamellae of augite in pigeonite. We simplified the model of exsolution phenomena such that the growth of the exsolution lamella will be controlled by the diffusion of Ca atom perpendicular to the lamella. By taking into account temperature dependency of Ca atomic diffusion coefficient in pigeonite and the temperature-time variations at a given depth of the crust, we integrated the equation derived from diffusion equation, with respect to temperature (1,200 850°C) by the numerical method to match the observed width of lamellae for the bulk Ca content of pigeonite. For a proposed achondrite parent body of 1,000km in diameter, the depth estimated for Moama is 12km below the surface, Moore County 9km, Juvinas 1.7km and Mt. Padbury 0.5km. The absolute cooling rate for the first two meteorites is about 1°C/104years. The eucritic crust of the parent body may be thinner than about 15 km. INTRODUCTIONBased on geochemical evidences of eucrites, diogenites, howardites and silicate inclusions ,in mesosiderites, and on crystallographic data of their pyroxenes, we have deduced the pyroxene crystallization trends and have proposed a layered crust model for a parent body of these genetically related achondrites (TAKEDA et al., 1976). However, known meteorites have not been located within the proposed crust, partly because of the lack of information on pyroxene exsolution.

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“…Under these conditions, zoned taenite and kamacite phases formed by diffusion controlled transformations are expected (Massalski et al, 1966;Reisener and Goldstein, 2003b). Wood (1967) showed the Ni diffusion differences between kamacite and taenite lead to an M shape when plotting Ni concentration across a taenite grain as the grain boundaries are enriched with Ni, and the center is left with lower Ni concentrations. Wood (1967) concluded the zoned "M"-shaped profile is the result of incomplete diffusion during cooling.…”

Section: Shock Processing Of Chondrites and The Potential Utility Of mentioning

confidence: 95%

“…Wood (1967) showed the Ni diffusion differences between kamacite and taenite lead to an M shape when plotting Ni concentration across a taenite grain as the grain boundaries are enriched with Ni, and the center is left with lower Ni concentrations. Wood (1967) concluded the zoned "M"-shaped profile is the result of incomplete diffusion during cooling. The central composition reflects the temperature at which diffusion began to cease in the grain (Ts), while the rim composition is indicative of the final temperature at which diffusion ceased (Tf).…”

Section: Shock Processing Of Chondrites and The Potential Utility Of mentioning

confidence: 99%

“…If the grains had been significantly reheated, it is likely this structure would be destroyed (Bennett and McSween, 1996). The size of this zoning has been shown to be a function of the cooling rate, meaning the central Ni content and the diameter of the taenite grain can be used together to determine a cooling rate (Wood, 1967;Willis and Goldstein, 1981;Taylor et al, 1987).…”

Section: Shock Processing Of Chondrites and The Potential Utility Of mentioning

confidence: 99%

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