JpGU-AGU Joint Meeting 2020

Presentation information

[J] Poster

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

[P-PS10] Formation and evolution of planetary materials in the Solar System

convener:Wataru Fujiya(Ibaraki University, College of Science), Megumi Matsumoto(Graduate School of Science, Tohoku University), Shin Ozawa(Department of Earth Science, Graduate School of Science, Tohoku University), Yuki Hibiya(Submarine Resources Research Center, Japan Agency for Marine-Earth Science and Technology)

[PPS10-P06] Microtexutural observations of TCIs in five CM carbonaceous chondrites and implications to aqueous environments on CM parent bodies.

Akane Iemoto1, *Yusuke Seto1, Akira Miyake2 (1.Graduate School of Science, Kobe University, 2.Graduate School of Science, Kyoto University)

Keywords:Carbonaceous chondrite, Aqueous alteration, Tochilinite

Introduction: CM chondrites are aqueously altered meteorites which contain around 10 wt% H2O in hydrous minerals. TCIs, fine intergrowths of tochilinite (6(Fe0.9S)・5[(Mg,Fe)(OH)2]) and cronstedtite (Fe-bearing serpentine), are one of the characteristic products of CM parent body aqueous alteration. TCIs are considered to be divided into two types based on the textural feature. Type I TCIs are generally found in the chondrules and believed to be altered from iron metal because they often contain kamacite inside [e.g., 1]. Type-II TCIs are found within the matrices. Although several formation processes of type-II have been proposed [e.g., 2,3], the argument has not yet been settled. TCIs potentially provide important information regarding aqueous environments on chondrite parent bodies. Here, we report microtextures of type-II TCIs in five CM chondrites and discuss the formation processes.

Materials and methods: We observed the following five CM chondrites; Cold Bokkeveld (2.2), Nogoya (2.2) , Murray (2.4-2.5), Murchison (2.5) , QUE 97990 (2.6). The numbers in parenthesis are the alteration index for CM chondrites proposed by Rubin et al. (2007) [4], in which the index is defined ranging from 2.6 (less altered) to 2.0 (highly altered). Textural observation and chemical analyses were performed using an SEM-EDS (JEOL, JSM-6480LAII), and nanometer-scale observations using an STEM-EDS (JEOL, JEM-2100F) after processing into thin films using an FIB (FEI, Quanta 3DS).

Results and discussion: In the less altered CM chondrites (QUE 97990 and Murchison), their type-II TCIs showed a similar texture. They are widely distributed in the matrices as compact aggregates of a few hundred nm-sized tochilinite and cronstedtite. From the TEM observations, thin veins of tochilinite were developed inside cracks or cleavages of cronstedtite, suggesting that tochilinite had been crystallized after the formation of cronstedtite. In contrast, the TCIs in Cold Bokkeveld (highly altered) showed core-rim structure. The core region is often rich in mixed layer phase (MLP; alternately stacked phase of tochilinite/cronstedtite layer in nanometer scale), and the rim mainly consists of coarse-grained tochilinite and cronstedtite, which resembles those of the less altered meteorites. Another highly altered meteorite Nogoya (2.2) also has TCIs with zonal texture, where very fine (several tens of nm) and fluffy serpentine rich material is located around core, and toward rim, gradually changed to fibrous cronstedtite and MLP. Murray, intermediately altered CM, has both type of TCIs seen in less and highly altered ones as noted above, indicating Murray was at an intermediate stage during the course of TCIs formation. All observed type-II TCIs in the present study do not include any precursor minerals such as anhydrous silicates or iron metal. TCIs of the two highly altered CM chondrites (Cold Bokkeveld and Nogoya) showed fluffy texture at their core region. These results probably suggest that fluffy type-II TCIs were not formed directly from solid material (like type-I), but crystallized under mobile environments such as water solution. In the case, changes of the fluid condition during the TCI formation resulted in the zonal texture as seen in the highly altered meteorites. The fact that the TCIs in QUE 97990 and Murchison resembles the coarse-grained rim of those in Cold Bokkeveld indicates the two less altered meteorites had experienced aqueous alteration similar to the last stage of aqueous alteration that Cold Bokkeveld had experienced.

References: [1] Tomeoka and Buseck. (1985) Geochimica et Cosmochimica Acta 49:2149–2163. [2] Pignatelli. et al. (2016) Meteoritics & Planetary Science 51:785-805. [3] Lee et al. (2013) Geochimica et Cosmochimica Acta 121:452-466. [4] Rubin et al. (2007) Geochimica et Cosmochimica Acta 71:2361-2382.