Titanium Stable Isotopic Variations in Chondrites, Achondrites and Lunar Rocks

1Nicolas D. Greber, 1Nicolas Dauphas, 2Igor S. Puchtel, 3Beda A. Hofmann, 4Nicholas T. Arndt
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2017.06.033]
1Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60615, USA
2Department of Geology, University of Maryland, College Park, MD 20742, USA
3Naturhistorisches Museum der Burgergemeinde Bern, Bernastrasse 15, Bern, Switzerland
4Université Grenoble Alpes, Institute Science de la Terre (ISTerre), CNRS, F-38041 Grenoble, France
Copyright Elsevier

Titanium isotopes are potential tracers of processes of evaporation/condensation in the solar nebula and magmatic differentiation in planetary bodies. To gain new insights into the processes that control Ti isotopic variations in planetary materials, 25 komatiites, 15 chondrites, 11 HED-clan meteorites, 5 angrites, 6 aubrites, a martian shergottite, and a KREEP-rich impact melt breccia have been analyzed for their mass-dependent Ti isotopic compositions, presented using the δ49Ti notation (deviation in permil of the 49Ti/47Ti ratio relative to the OL-Ti standard). No significant variation in δ 49Ti is found among ordinary, enstatite, and carbonaceous chondrites, and the average chondritic δ49Ti value of +0.004 ± 0.010 ‰ is in excellent agreement with the published estimate for the bulk silicate Earth, the Moon, Mars, and the HED and angrite parent-bodies. The average δ49Ti value of komatiites of -0.001 ± 0.019 ‰ is also identical to that of the bulk silicate Earth and chondrites. OL-Ti has a Ti isotopic composition that is indistinguishable from chondrites and is therefore a suitable material for reporting δ49Ti values. Previously published isotope data on another highly refractory element, Ca, show measurable variations among chondrites. The decoupling between Ca and Ti isotope systematics most likely occurred during condensation in the solar nebula.

Aubrites exhibit significant variations in δ49Ti, from -0.07 to +0.24 ‰. This is likely due to the uniquely reducing conditions under which the aubrite parent-body differentiated, allowing chalcophile Ti3+ and lithophile Ti4+ to co-exist. Consequently, the observed negative correlation between δ49Ti values and MgO concentrations among aubrites is interpreted to be the result of isotope fractionation driven by the different oxidation states of Ti in this environment, such that isotopically heavy Ti4+ was concentrated in the residual liquid during magmatic differentiation.

Finally, KREEPy impact melt breccia Sau 169 exhibits a heavy δ49Ti of +0.330 ± 0.034 ‰ which is interpreted to result from Ti isotopic fractionation during ilmenite precipitation in the late stages of lunar magma ocean crystallization. A Rayleigh distillation calculation assuming a crystallization temperature of 1175°C predicts that a δ49Ti value of +0.330 ‰ is achieved after removal of 94% of the Ti in ilmenite with an ilmenite-melt Ti isotopic fractionation of –0.12‰.


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