Japan Geoscience Union Meeting 2015

Presentation information


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

[P-PS22] Formation and evolution of planetary materials in the solar system

Thu. May 28, 2015 4:15 PM - 6:00 PM A02 (APA HOTEL&RESORT TOKYO BAY MAKUHARI)

Convener:*Shoichi Itoh(Graduate school of Science, Kyoto University), Tomohiro Usui(Department of Earth and Planetary Sciences,Tokyo Institute of Technology), Yusuke Seto(Graduate School of Science, Kobe University), Masaaki Miyahara(Department of Earth and Planetary Systems Science, Graduate School of Science, Hiroshima University), Makoto Kimura(Faculty of Science, Ibaraki University), Eiji Ohtani(Department of Earth and Planetary Materials Science, Graduate School of Science, Tohoku University), Hitoshi Miura(Graduate School of Natural Sciences, Department of Information and Biological Sciences, Nagoya City University), Hikaru Yabuta(Osaka University, Department of Earth and Space Science), Chair:Tomohiro Usui(Department of Earth and Planetary Sciences,Tokyo Institute of Technology)

5:00 PM - 5:15 PM

[PPS22-23] 147Sm-143Nd and 146Sm-142Nd chronology of a basaltic eucrite, NWA 7188

*Saya KAGAMI1, Tetsuya YOKOYAMA1, Tomohiro USUI1, Ryota FUKAI1 (1.Department of Earth and Planetary Sciences, Tokyo Institute of Technology)

Keywords:basaltic eucrite, Sm-Nd chronology, NWA 7188

Eucrites are achondritic meteorites originating from the Vesta’s crust. They can be petrographically classified into basaltic and cumulate eucrites. Determination of precise ages for eucrites will constrain the period of igneous activity and the following thermal metamorphism of Vesta and may further provide insights into its differentiation and thermal history. We investigate the long-lived 147Sm-143Nd (T1/2 = 1.06×1011 yr) and the short-lived 146Sm-142Nd (T1/2 = 6.8×107 yr [1]) systematics of a basaltic eucrite, NWA 7188 and compare the results with the ages obtained in previous chorological studies on cumulate and basaltic eucrites. To obtain highly precise age data, we developed the techniques for determining Nd and Sm concentrations and Nd isotope compositions in meteorite samples.
NWA 7188 was crushed and sieved into four sizes; G1) 500—1700 μm, G2) 250—500 μm, G3) 106—250 μm, and G4) ≤106 μm. G3 and G4 were separated into pyroxene and plagioclase grains by handpicking. We determined the 147Sm-143Nd and 146Sm-142Nd ages of NWA 7188 using G1, G3-px, G4-px, G3-pl, and G4-pl. These were dissolved using a mixture of concentrated pure acids (HClO4, HF, and HNO3). After the sample digestion, ∼10% of the solution was removed and mixed with 149Sm- and 145Nd-enriched spikes to determine the Sm and Nd concentrations by ID-ICP-MS (X-series Ⅱ, Thermo). The remainder of the sample solution was used for highly precise Nd isotope analysis by TIMS (TRITON plus) with the dynamic multicollection mode. Nd was separated by a three-step column chemistry procedure; 1) major elements were removed by passing through a cation exchange resin, 2) Ce was removed using the LN resin (Eichrom) by oxidizing Ce3+ into Ce4+ using KBrO3 [2] and 3) Nd was separated from Sm using the LN resin. We achieved Ce/Nd = ∼3×10-5 and Sm/Nd = ∼4×10-5 with ≥91% Nd recovery.
The 147Sm-143Nd mineral isochron of NWA 7188 yields an age of 4203±970 Ma. In contrast, we obtained a much older 146Sm-142Nd mineral isochron age of 4549±2840 Ma when an initial solar system ratio of 146Sm/144Sm = 0.0094 at 4568 Ma was applied [1]. It is presumed that thermal metamorphism on the Vesta has some effects on the 147Sm-143Nd age while the 146Sm-142Nd age represents the timing of the last Sm-Nd isotopic closure. Therefore, we use the 146Sm-142Nd age of NWA 7188 in the following discussion.
The 146Sm-142Nd age (4549±2840 Ma) for NWA 7188 is consistent with the 147Sm-143Nd age for cumulate eucrites (4546±8 Ma [3]) within analytical uncertainties. This suggests that the parent body processes associated with the last Sm-Nd isotopic closure were contemporaneous for basaltic and cumulate eucrites. Likewise, the 146Sm-142Nd age of NWA 7188 is not resolvable from the metamorphic age of Agoult [4]. According to the 53Mn-53Cr systematics [5], the last global Mn/Cr fractionation in the mantle of the Vesta occurred at 4564.8±0.9 Ma, the timing when basaltic magmas have formed in the mantle. This implies that basaltic eucrites quenched rapidly on the surface of eucrite parent body, but thermal metamorphism may have affected both Sm-Nd and U-Pb systematics. No apparent age difference between basaltic and cumulate eucrites implies that both types of eucrites might have experienced similar cooling history as opposed to their petrographic distinction, or more likely that the time difference is too subtle to be resolved by the 146Sm-142Nd system.
References: [1] Kinoshita, N. et al. (2012) Science, 335, 1614-1617. [2] Tazoe, H. et al. (2007) JAAS, 22, 616-622. [3] Boyet, M. et al. (2010) EPSL, 291, 172-181. [4] Iizuka, T. et al. (2014) EPSL, 409, 182-192. [5] Lugmair, G.W. and Shukolyulov, A. (1998) GCA, 62, 16, 2863-2886.