Mathematics – Logic
Scientific paper
Jul 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992metic..27r.258m&link_type=abstract
Meteoritics, vol. 27, no. 3, volume 27, page 258
Mathematics
Logic
9
Scientific paper
The IAB and IIICD iron meteorite groups exhibit much larger ranges in siderophile concentrations than other groups and commonly contain silicate inclusions. Extensive studies of metal in both groups and silicates in IAB irons have led to a variety of ideas to explain the genesis of these groups. Wasson et al. (1980) envision each meteorite forming in a separate impact melt pool. Kracher (1982, 1985) suggested that the siderophile trends might result from fractional crystallization of both metal and troilite in a S-saturated magma. A role for oxidation-reduction in these groups has been proposed by Scott and Bild (1974). Similarities in siderophile elemental trends indicate that IIICD metal has a similar origin, although data on silicate inclusions in IIICD irons are scarce (Ramdohr, 1973; Scott and Bild, 1974; Kracher and Kurat, 1977; Prinz et al., 1982; Clayton et al., 1983). We report the first detailed study of silicate inclusions in IIICD iron meteorites in an attempt to elucidate their history. We have studied the only silicate-bearing IIICD irons - Carlton, Dayton, and the recently reported Maltahohe. Silicate-graphite-phosphate inclusions comprise at most a few percent of the bulk meteorite, and silicates comprise <25 vol% of the inclusion. Silicate mineralogy and chemistry vary systematically with increasing M content of the metal. Maltahohe (10.7 wt% Ni) and Carlton (13.0%) contain olivine, pyroxene, and plagioclase, whereas Dayton (17.0%) contains pyroxene, plagioclase, and SiO2. Pyroxene becomes more FeO-rich from Maltahohe (FS(sub)7.8) to Carlton (Fs(sub)9.7) to Dayton (Fs(sub)11.6). Inverse FeO zoning in silicates and lower Fa than Fs indicate reduction in all three meteorites. Plagioclase compositions in IIICD (An(sub)1.1-4.9) are lower than IAB (An(sub)9.2-2l.5) and uncorrelated with Ni content. The abundances of associated phases also vary. Graphite comprises ~25 vol% of Maltahohe silicate inclusions, but only a few percent in Carlton, and is absent in Dayton silicate inclusions. Phosphate mineralogy and modal abundance also vary, with phosphates absent in Maltahohe, chlorapatite comprising 0-70 vol% of inclusions in Carlton, and the unusual phosphates brianite and panethite, along with whitlockite, comprising up to 55 vol% of Dayton's inclusions. The small number of silicate-bearing IIICD irons require that any conclusions must be considered tentative. The precursor silicate assemblage was similar for IAB and IIICD, as suggested by the general similarity between Maltahohe and IAB silicate inclusions. With increasing Ni contents, however, IIICD and IAB silicate inclusions become dramatically different, as indicated by the mineralogical and chemical trends present in IIICD and absent in IAB silicate inclusions. Silicate inclusions in the Ni-rich IAB irons (e.g., San Cristobal, 25 wt% Ni) do not resemble the phosphate-rich, evolved-silicate assemblages observed in Dayton. It is clear that one or more processes were capable of producing changes in metal compositions and silicate inclusion mineralogy, which correlated with one another. None of the observed trends in silicate mineralogy are predicted by the impact-melt model, although impact might have played a role in mixing silicates into the metallic magma. Some trends are consistent with oxidation-reduction, but variations in some siderophiles (e.g., Ir, Cu) cannot be explained easily by this mechanism. We believe that solid silicates must have been mixed with an evolving metallic melt, with the metallic magma dramatically influencing the mineralogy and chemistry of the inclusion, similar to the fractional crystallization model of Kracher (1982,1985). However, many details of this process remain obscure, including the mechanism that concentrated a S-rich melt, the mixing of metal and silicates, and the fractionation of S. References: Clayton et al. (1983) EPSL 65, 229-232. Kracher (1982) GRL 9, 412-415. Kracher (1985) PLPSC 15, C689-C698. Kracher and Kurat (1977) Meteoritics 12, 282-283. Scott and Bild (1974) GCA 38, 1379-1391. Prinz et al. (1982) LPSC XIlI, 632-633. Ramdohr (1973) Elsevier Pub. Co. Wasson et al. (1980) Z. Naturforsch. 35a, 781-795.
Haack Henning
Keil Klaus
McCoy Timothy James
Scott Edward R. D.
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