Japan Geoscience Union Meeting 2016

Presentation information


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

[P-PS12] Formation and evolution of planetary materials in the solar system

Tue. May 24, 2016 10:45 AM - 12:15 PM 104 (1F)

Convener:*Masaaki Miyahara(Department of Earth and Planetary Systems Science, Graduate School of Science, Hiroshima University), Akira Yamaguchi(National Institute of Polar Research), Tomohiro Usui(Department of Earth and Planetary Sciences,Tokyo Institute of Technology), Yoko Kebukawa(Faculty of Engineering, Yokohama National University), Wataru Fujiya(Ibaraki University, College of Science), Yusuke Seto(Graduate School of Science, Kobe University), Shoichi Itoh(Graduate school of Science, Kyoto University), Chair:Tomohiro Usui(Department of Earth and Planetary Sciences,Tokyo Institute of Technology)

11:45 AM - 12:00 PM

[PPS12-11] Application of scanning-imaging x-ray microscopy to fluid inclusion candidates in carbonates of carbonaceous chondrites.

*Akira Tsuchiyama1, Tsukasa Nakano2, Akira Miyake1, Takeuchi Akihisa3, Kentaro Uesugi1, Yoshio Suzuki, Akira Kitayama1, Junya Matsuno1, Michael E. Zolensky4 (1.Division of Earth and Planetary Sciences, Graduate School of Sciece, Kyoto University, 2.AIST/GSJ, 3.JASRI/SPring-8, 4.NASA/JSC)

Keywords:Tomography, SPring-8, Hayabusa2, hydrous alteration

In order to search for such fluid inclusions in carbonaceous chondrites, a nondestructive technique using x-ray micro-absorption tomography combined with FIB sampling was developped and applied to a carbanaceous chondrite [1,2]. They found fluid inclusion candidates in calcite grains, which were formed by aqueous alteration. However, they could not determine whether they are really aqueous fluids or merely voids.
Phase and absorption contrast images can be simultaneously obtained in 3D by using scanning-imaging x-ray microscopy (SIXM) [3]. In rrefractive index, n=1-δ+iβ, in the real part, 1-δ is the refractive index with decrement, δ, which is nearly proportional to the density, and the imaginary part, β, is the extinction coefficient, which is related to the liner attenuation coefficient, μ. Many phases, including water and organic materials as well as minerals, can be identified by SIXM, and this technique has potential availability for Hayabusa-2 sample analysis too. In this study, we examined quantitative performance of d and m values and the spatial resolution in SIXM by using standard materials, and applied this technique to carbonaceous chondrite samples.
We used POM ([CH2O]n), silicon, quartz, forsterite, corundum, magnetite and nickel as standard materials for examining the δ and μ values. A fluid inclusion in terrestrial quartz and bivalve shell (Atrina vexillum), which are composed of calcite and organic layers with different thickness, were also used for examining the spatial resolution. The Ivuna (CI) and Sutter’s Mill (CM) meteorites were used as carbonaceous chondrite samples. Rod- or cube-shaped samples 20-30 μm in size were extracted by using FIB from cross-sectional surfaces of the standard materials or polished thin sections of the chondrites, which was previously observed with SEM. Then, the sample was attached to a thin W-needle and imaged by SIXM system at beamline BL47XU, SPring-8, Japan. The slice thickness was 109.3 nm and the pixel size was mostly 100 nm.
It was found that μ and d values obtained by SIXM (μSIXM and dSIXM) are proportional to the theoretical values (mcalc and dcalc), respectively, exept for large μ values (>~1000 cm-1), and the following relations were obtained; μSIXM = 0.909(8)×μcalc and δSIXM = 0.908(6)×δcalc. We can quantitatively identify fluid in inclusions of the terrestrial quartz and organic layers in the shell with the spatial resolution of >~1 μm. If they are less than ~1 μm, we cannot quantitatively identify them due to overlapping of the point sprad function.
A hexagonal platy inclusion with facets, or negative crystal (0.7 x 2.3 μm) was found in a calcite grain of the Sutter’s Mill meteorite as a fluid inclusion candidate [4]. The δ value of this inclusion is less than that of water, indicating that any aqueous fluid was not included. As its shape strongly suggests that it was once formed as a fluid inclusion during hydrous alteration in a parent boby, and then the fluid must be escaped. We cannot detect any aqueous fluids in other fluid inclusion candidates, such as a spherical inclusion (~1.8 μm) in a calcite grain of the Sutter’s Mill meteorite, which seems to have a bubble inside [1], and a relatively large inclusion with facets in dolomite in the Ivuna meteorite.
References: [1] Tsuchiyama et al. (2014) MAPS, 49: A404. [2] Zolensky et al. (2014) MAPS, 49: 1997. [3] Takeuchi et al. 2013, J. Synch. Rad., 20: 793. [4] Kitayama et al. (2016) this volume.