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 5:15 PM - 6:30 PM Poster Hall (International Exhibition Hall HALL6)

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)

5:15 PM - 6:30 PM

[PPS12-P08] The differences among CO3 chondrites from the X-ray diffraction

*Naoya Imae1,2, Yoshihiro Nakamuta3 (1.Antarctic Meteorite Research Center, National Institute of Polar Research, 2.SOKENDAI, 3.Kyushu University)

Keywords:X-ray diffraction, CO3 chondrite, olivine, pyroxene

1. Introduction
The X-ray diffraction method is one of a powerful tool for studying the subtle differences of thermal metamorphism and initial condition of unequalibrated chondrites. The X-ray gives the global feature of constituent mineral phases including submicron-sized matrices. The petrologic type of the CO chemical group, constituting a group of carbonaceous chondrites, is three, which is subdivided into 3.0-3.9. In the present study, the X-ray powder diffraction patterns were obtained from the polished thin sections of the CO3 chondrites, and new insights were obtained on the differences among the subtypes.
2. Experiments
The X-ray diffractometer, SmarLab (RIGAKU), at National Institute of Polar Research installed in 1994 was used for the present study. The sample stage of the automatically sample change (ASC10) was used for the sample holder of the polished thins sections (PTSs), Y-81020 CO3.0, Colony CO3.0, Y-791717 CO3.3, Lance CO3.5, ALH-77003 CO3.6, Isna CO3.8, A-882094, and Y983589. The X-ray was generated from the Cu target and K beta was removed using the Ni filter. Tube voltage and tube current were 40 kV and 30 mA, respectively. The scan speed of the solid-state detector (D/tex Ultra 250) was 0.4degree/min. The width of the incident X-ray was 10 mm. The PTS was rotated within the plane during the measurements at 100 rpm. It was confirmed that the method gives the consistent diffraction pattern with the powder X-ray diffraction method (Imae, 2015). The half width and intensity of the diffraction was analyzed using the program by the software Visual Basic 6.0 runtime.
3. Results and discussion
The diffraction of olivine (130) is doublet when the subtype is less than 3.5, corresponding to ferroan olivines in matrices (Fa~35-45) at lower diffraction angle and magnesian olivines in the type I chondrules at higher diffraction angle. It is single when the subtype is more than 3.6. In more detail (Fig. 1), the half width increases and the peak position shifts lower (to ferroan) at higher diffraction angle when the subtype changes from 3.0 to 3.5, but the peak vanishes more than the subtype of 3.6. On the other hand, the half width decreases and the peak intensity increases at lower diffraction angle when the subtype changes from 3.0 to 3.8. The series of sensitive change occurs during the weak thermal metamorphism accompanying the Mg-Fe diffusion in olivines and bulk sample.
The (22-1) of clinoenstatite was detected irrespective of the subtype, and the (321) of orthoenstatite was also identified irrespective of the subtype (Fig. 2). It is considered that the orthoenstatite in lower petrologic subtype is high temperature type formed during the chondrule formation although that in higher subtype may be low temperature type formed during the thermal metamorphism on the CO parent body. The unique occurrence of the orthoenstatite phases would suggest that the thermal history during the chondrule formation is different from that for the ordinary chondrites. The result is consistent with that by Imae et al. (2013) based on the EPMA.
4. Acknowledgment
NI is grateful to Dr. Shugo Ohi in Shiga Univ., who indicated the diffractions of clinoenstatite.
5. References
Imae N. et al. (2013) Geochim. et Cosmochim. Acta 100, 116-157.
Imae N. (2015) NIPR Symposium on Antarctic Meteorites.