Tungsten and hafnium distribution in calcium-aluminum inclusions (CAIs) from Allende and Efremovka

Recent Hf-182-W-182 age determinations on Allende Ca-, Al-rich refractory inclusions (CAIs) and on iron meteorites indicate that CAIs have initial e W-182 (-3.47 +/- 0.20, 2 sigma) identical to that of magmatic iron meteorites after correction of cosmogenic W-182 burn-out (-3.47 +/- 0.35, 2 sigma). Either the Allende CAIs were isotopically disturbed or the differentiation of magmatic irons (groups IIAB, IID, IIIAB, and IVB) all occurred <1 m.y. after CAI formation. To assess the extent of isotopic disturbance, we have analyzed the elemental distribution of Hf and W in two CAIs, Ef2 from Efremovka (CV3 reduced), and Golfball from Allende (CV3 oxidized). Fassaite is the sole host of Hf (10-25 ppm) and, therefore, of radiogenic W in CAIs, with Hf-180/W-184 > 10(3), which is lowered by the ubiquitous presence of metal inclusions to Hf-180/W-184 > 10 in bulk fassaite. Metal alloy (Ni similar to 50%) is the sole host of W (similar to 500 ppm) in Ef2, while opaque assemblages (OAs) and secondary veins are the hosts of W in Golfball. A large metal alloy grain from Ef2, EM2, has Hf-180/W-184 < 0.006. Melilite has both Hf and W below detection limits (<0.01 ppm), but the presence of numerous metallic inclusions or OAs makes melilite a carrier for W, with Hf-110/W-114 < I in bulk melilite. Secondary processes had little impact on the Hf-182-W-182 systematics of Ef2, but a vein cross-cutting fassaite in Golfball has >100 ppm W with no detectable Pt or S. This vein provides evidence for transport of oxidized W in the CAI. Because of the ubiquitous distribution of OAs, interpretations of the Hf-182-W-184 isochron reported for Allende CAIs include: (i) all W in the OAs was derived by alteration of CAI metal, or (ii) at least some of the W in OAs may have been equilibrated with radiogenic W during metamorphism of Allende. Since (ii) cannot be ruled out, new Hf-182-W-182 determinations on CAIs from reduced CV3 chondrites are needed to firmly establish the initial W isotopic composition of the solar system. (C) 2007 Elsevier Ltd. All rights reserved.