JpGU-AGU Joint Meeting 2017

Presentation information

[JJ] Oral

P (Space and Planetary Sciences) » P-PS Planetary Sciences

[P-PS10] [JJ] Formation and evolution of planetary materials in the solar system

Tue. May 23, 2017 3:30 PM - 5:00 PM 105 (International Conference Hall 1F)

convener:Tomohiro Usui(Earth-Life Science Institute, Tokyo Institute of Technology ), Masaaki Miyahara(Department of Earth and Planetary Systems Science, Graduate School of Science, Hiroshima University), Akira Yamaguchi(National Institute of Polar Research), Yoko Kebukawa(Faculty of Engineering, Yokohama National University), Chairperson:Yoko Kebukawa(Faculty of Engineering, Yokohama National University)

4:00 PM - 4:15 PM

[PPS10-27] Zn stable isotope contribution to constraint ureilite formation process

*Genevieve Claire Hublet1, Vinciane Debaille2, Luc S Doucet2, Richard C Greenwood3, Akira Yamaguchi1, Nadine Mattielli2 (1.National Institute of Polar Research, 2.Université Libre de Bruxelles, 3.The Open University)

Ureilites are ultramafic achondrites. They are usually considered to be derived from a single parent body (UPB) now-disrupted. There are mainly composed of olivine and pigeonite. This is already demonstrated that ureilites are mantle restites. But, this hypothesis is not consistent to explained preservation of the primitive characteristics such as the O heterogeneity in ureilites [1] and confirmed by the new Δ17O data in our samples. In this study, we report new Zn stable isotopic composition and also 26Al-26Mg systematic for seven monomict ureilites Yamato (Y) 790981, Y 791538, Y 981750, Y 981810, Asuka (A) 881931, Allan Hills (ALH) 81101 and ALH 84136 to constraint the ureilite formation by smelting process.
Zn isotope analysis of our seven samples yielded non-chondritic and heterogeneous composition in δ66Zn signatures ranging +0.61 ± 0.01‰ to +2.68 ± 0.11‰. This heterogeneity in Zn can reflected the isotopic signature of the precursor(s). In opposition, Zn is a moderately volatile element, and alternative explanation already mentioned by previous studies suggested this heavy isotope enrichment may reflect volatilization process following major impact [2]. This explanation is generally supported by the correlation between the δ66Zn and the Zn abundance in ureilites. However, this hypothesis is not well supported by the shock degrees. In our study, we evaluated the possibility that δ66Zn signature could be produced by smelting process during ureilites genesis like already suggested by [3-4]. To evaluate the effects of such a volatilization process during smelting, we modeled the Zn isotope fractionation in ureilites on the basis of the Rayleigh distillation equation, according to [5] when Zn isotope fractionation was explored during the smelting process in the metallurgic industry. In this model, we made the assumption that UPB precursor had an initial composition in Zn content and δ66Zn signature similar to a CI type chondrite. The smelting degrees of our samples were evaluated based on their Zn content. Based on this assumption, we show that the observed δ66Zn variability in our ureilites match the data obtained using the smelting process model.
On the other hand, smelting process can occur only if the UPB precursor starts to melt. During this step, the ureilite witch is the residues should be depleted in incompatible elements like suggested by the REE pattern in ureilites [6]. Based on the new REE data [6] and our data, we evidenced correlation between (Dy/Lu)n ratios and the degrees of smelting modeled. This observation suggests that smelting degrees increased with the degrees of melting (F).
Finally, based on 26Al-26Mg isotopic system, no isochron has been obtained with the δ26Mg* and 27Al/24Mg data analyzed in our samples. If all these samples crystallized at the same time, the δ26Mg* data suggest our samples could come from different parent bodies. However, our data set could also reflect different crystallization ages from a single parent body. Considering the smelting process for ureilites formation, this hypothesis could be considered since smelting was a local process. Assuming all the ureilites originated from a single parent body with a chondritic composition, a model age can be determined. This model age reflects the time when the ureilite common source differentiated from a chondritic reservoir. This differentiation can be modeled at 1.09 ± 0.75 Ma after the CAI formation. [1] Clayton R. & Mayeda T. (1988) GCA, 52, 1313-1318. [2] Moynier F. et al. (2010) Chem. Geol., 276, 374–379. [3] Singletary S. & Grove T. (2003) Meteorit. Planet. Sci., 38, 95-108. [4] Goodrich C.A. et al. (2007) GCA, 71, 2876-2895. [5] Mattielli N. et al. (2009) Atmos. Environ., 43, 1265-1272. [6] Barrat J.-A. et al. (2016), GCA, 194, 163-178