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Mineralogical and geochemical study of brachinite clan meteorites : Implications for early differentiation of planetesimals

長谷川, 輝 東京大学 DOI:10.15083/0002002080

2021.10.04

概要

The study of primitive achondrites is expected to lead to an understanding of the variations of planetary differentiation processes and valuable information about the earliest stages of igneous evolution of planetesimals in our solar system. Previously, primitive achondrites are suggested to have come from the asteroids which was partially differentiated (e.g., Prinz et al., 1983; Nehru et al., 1992; Mittlefehldt et al., 1998). Some researchers recently proposed the inner structures of the parent bodies of primitive achondrites (ureilites, acapulcoites/lodranites and winonaites) and their ages have also been determined (e.g., Wilson et al., 2008; Hunt et al., 2018; Li et al., 2018; Toubol et al., 2008, 2009; Theis et al., 2013; Budde et al., 2015; Worsham et al., 2017). Compared to other primitive achondrites, however, brachinites have been poorly understood and their origin and formation processes have been controversial (e.g., Mittlefehldt et al., 2003; Day et al., 2012; Goodrich et al., 2017). This is because the number of brachinites has rapidly increased in the last fifteen years (10 specimens in 2000, but 44 specimens in 2019), but the study on newly found brachinites has been far from sufficient (Meteoritical Bulletin Database, 2019). Another aspect includes that brachinites are mainly composed of olivine and are hard to apply regular mineralogical and isotopic approaches (e.g., geological thermometers, U-Pb absolute age). Furthermore, the rapid increase of the number of brachinites resulted in the complexities of the grouping of brachinites (e.g., the existence of “brachinite-like meteorites”, “ungrouped achondrite related to brachinites” and “brachinite clan”). Therefore, we comprehensively studied twelve olivine-rich achondrites (“brachinite clan meteorites”): Allan Hills (ALH) 84025, Divnoe, Elephant Moraine (EET) 99402, EET 99407, Miller Range (MIL) 090206, MIL 090340, MIL 090405, Northwest Africa (NWA) 4969, NWA 6112, NWA 6308, NWA 10932 and Reid 013, to understand the formation processes and the origin of brachinite clan meteorites. We performed not only conventional petrological and mineralogical study but also chromium isotopic and olivine petrofabric study. Characteristically, we focused on CPO (crystallographic preferred orientation) of olivine. Studying olivine fabrics in rocks is extremely important to obtain the information of the physical environment during and after crystallization. In recent years a lot of observations and experiments of olivine deformation in terrestrial mantle rocks have been performed (e.g., Karato et al., 2008; Ohuchi, 2013). Thus, variation of formation mechanism to produce olivine CPO patterns has been well understood and the olivine CPO patterns observed in natural rocks can be used to estimate the formation condition of the rocks (e.g., Jung et al., 2007; Karato et al., 2008). Brachinite clan meteorites are olivine-rich rocks similar to terrestrial mantle rocks and are expected to exhibit olivine CPO patterns because of the presence of apparent linear structures on the thin sections of some samples. Measuring olivine CPO in brachinite clan meteorites can lead to the better understanding of their formation conditions. However, there are only two olivine fabric studies for four brachinite clan meteorites (Ando et al., 2003; Mittlefehldt et al., 2003), and quantitative evaluation of olivine CPO patterns for brachinite clan meteorites has not been reported. Therefore, a major goal of this study is to obtain the information of formation conditions of brachinite clan meteorites revealed by olivine CPO analysis combining mineralogy and geochemistry for the first time.

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