Open Access

Mineralogy of some evolved LL chondrites with reference to asteroid materials and solar system evolution

  • Hiroshi Takeda1, 2Email author,
  • Hiroshi Nagaoka3,
  • Akira Yamaguchi4, 5,
  • Yuzuru Karouji6 and
  • Yuuki Yazawa7
Earth, Planets and Space201567:5

https://doi.org/10.1186/s40623-014-0167-x

Received: 13 February 2014

Accepted: 4 December 2014

Published: 13 January 2015

Abstract

Mineralogy of three LL chondrites including Y-981971, Y-793214, and Y-790782 indicates that granulitic materials may have been formed in some depth of their parent body by an impact event. This process of high-temperature episodes is different from the records in the differentiated achondrites (howardite-eucrite-diogenite (HED)) possibly from the Vesta-like asteroid.

Keywords

LL chondrite Partial melting Metamorphism Differentiation Pyroxene Olivine

Findings

Introduction

Because of the recent investigations on the returned dusts from the Itokawa by the Hayabusa Mission (e.g., Nakamura et al. 2011), we have a renewed interest in the LL chondrites in order to better understand the evolutional processes on an asteroidal body. Nakamura et al. (2011) reported that Itokawa dusts have LL composition. It is generally believed that the chondritic materials preserve the chemical records of the primitive solar system materials (Fujiwara et al. 2006). Shock partial melting and recrystallization during breccia formation were extensive on the LL chondrite parent body (Takeda et al. 1984), but no fractional crystallization took place from the melt.

Among Yamato (Y-) LL chondrites, we found the first evidence of a product of partial melting with albite and diopside assemblage in Y-74160 (Takeda et al. 1984). This assemblage is the first andesitic material in the solar system other than the Earth. The andesite was produced by a shock partial melting, but we also found such material in the silicate inclusions in the iron meteorites (Takeda et al. 2000; Takeda et al. 2003). Y-790964 and Y-790143 (Miyamoto et al. 1984; Yamaguchi et al. 1998) are unusual impact-melted LL chondrites and experienced nearly total melting, yet partly preserve chondritic textures.

We performed mineralogical studies of the Y-981971, Y-793214, and Y-790782 LL chondrites to better understand surface materials of the Itokawa asteroid. We looked for the diopside-albite assemblage (andesitic material) together with olivine and orthopyroxene (Opx). Although these LL chondrites have brecciated and metamorphosed textures, remnants of chondrule are present. Total melting in much larger scale is recorded in a group of meteorite including howardite-eucrite-diogenite (HED) achondrites (e.g., Takeda 1997).

Samples and methods

Three polished thin sections (PTSs) of LL chondrites Y-981971,51-1 (Figure 1a), Y-793214,92-1 (Figure 1b), Y-790782,91-2 (Figure 1c), prepared at the National Institute of Polar Research (NIPR), were observed by a petrographic microscope. Y-981971 (Figure 1d), Y-793214 (Figure 1e), and Y-790782 (Figure 1f), were analyzed with a JEOL 8900 Electron Probe Microanalyzer (EPMA) (JEOL Ltd., Tokyo, Japan) at Atmosphere and Ocean Research Institute (AORI). Areal analyses of a region 30 × 40 μm of a granulitic clast were also obtained at AORI. Seven points were analyzed along the X and Y directions.
Figure 1

Photomicrograms of polished thin sections (PTS) of three LL chondrites from Antarctica. Left column; entire PTSs: open light; width is 1.2 cm. (a) Breccia textures with many crystalline clasts in Y-981971,51-1. (b) The entire view of Y-793214,92-1 PTS. (c) An entire PTS of Y-790782,91-2 LL. Right column: enlarged views of those on the left side, width 1.3 mm. Open polarized light: (d) an unbrecciated granulitic clast in Y-981971,51-1 LL. (e) An unbrecciated granulitic mass with an opaque vein in Y-793214 LL. (f) Opaque spherules in Y-790782 LL PTS.

Results

PTS Y-981971

Y-981971 shows breccia textures with many crystalline clasts (Figure 1a), which contain silicates with sub-rounded boundaries and a few opaque minerals filling interstices of silicate crystals. It is difficult to find remnants of chondrules, except for one part with metamorphosed barred olivine crystals. Former matrices between the bars now show crystalline textures. Chemical compositions of pyroxenes in Y-981971 are mostly uniform and are within the range of the LL chondrite.

In order to find the diopside-albite assemblage, modal abundances of minerals were obtained by the aerial analyses of JEOL 8900 EPMA for a selected area 30 × 40 μm above the irregular opaque grain in Figure 1d: olivine 53%, augite 39, Opx 5, and albite 3 excluding a few low-sum analyses of grain boundaries, etc. The presence of augite and albite suggests presence of the andesitic material. Chemical compositions of olivines in Mg number (= molar Mg/(Mg + Fe) × 100) is 68 mol%. In a part of granulitic clasts, we found a sizable grain of albite in mafic silicates. The plagioclase in the clast has alkali-rich composition Ab87.3An10.7Or1.9.

PTS Y-793214

PTS Y-793214 (Figure 1b) is listed as LL5 in the catalogue of NIPR, but we cannot detect any chondrule. It is different from a fragmental breccia as in Y-981971 PTS (Figure 1a). The overall texture is nearly crystalline granulitic feature with a few opaque veins. Along such veins, clear mafic silicate crystals are abundant with rounded gain boundaries (Figure 1e). The chemical composition of the mafic silicates is within the range of the LL chondrites.

PTS Y-790782

This PTS (0.9 × 0.8 cm in size) consists of dark fine-grained mafic silicates (Figure 1c). The PTS is characterized by many opaque spherules (Figure 1f). The presence of Fe, Ni, and S suggests that these spherules are products of partial melting of chondritic metals and sulfides. The opaque spherules distribute throughout the PTS (Figure 1c), indicating total melting. The texture is different from that of Y-790964 (Yamaguchi et al. 1998). A few clasts of crystalline materials are present in the matrices (Figure 1c). These clasts show a granulitic texture with an opaque vein. The matrix resembles devitrified glass, but an enlarged photograph (Figure 1f) shows that they are aggregates of fine fragments of low-Ca pyroxene and olivine. Some fragments are large enough to give single-mineral compositions, but fine materials between the fine fragments give compositions intermediate between low-Ca pyroxene and olivine. The pyroxene compositions are nearly uniform (average Ca5Mg73Fe22).

Discussion

Geothermometry based on the compositions of pyroxenes of the LL-group chondrites has been discussed by McSween and Patchen (1989). The sampled materials of Itokawa were thermally metamorphosed, as is the case for most ordinary chondrites. Nakamura et al. (2011) show that almost all of the olivine and pyroxene grains in the Itokawa dusts are quite uniform in composition, and the entire collection falls almost entirely within the LL field. To be heated sufficiently, the samples must have originated inside a much larger asteroid. The trend of a zoned grain in the Hayabusa dusts is different from that of the LL3 pyroxene and is similar to the pyroxene crystals in Y-790964 (Miyamoto et al. 1984). The zoning trends of the Itokawa dusts indicate that at least a part of the Itokawa asteroid body is melted by an impact event at high temperature. Our discovery of granulitic clasts with the diopside-albite assemblage indicates that there is an andesitic material (partial melt) in some parts of the LL parent body. The presence of the product of a partial melt in a chondrite parent body suggests that even the primitive solar system material, such as LL chondrites experienced strong thermal events. The granulitic textures in some lunar samples are widely believed to have formed deep in the lunar crust. The granulitic materials in the LL parent body may also have been formed at some depth of their parent body by an impact event. Granulitic breccias and granulites in lunar crust have been discussed by many lunar investigators (e.g., Lindstrom and Lindstrom 1986).

Products of high-temperature episodes in the solar system materials other than the terrestrial planets are represented by the differentiated achondrites. The mineralogy of Vesta, based on data obtained by the Dawn Mission (De Sanctis et al. 2012), is consistent with HED achondrites and confirmed the presence of the proposed layered crust model (Takeda 1979). It is important to recognize that high-temperature events took place in a region of the LL chondrite parent body, from where Itokawa and parent asteroids of the Antarctic meteorites were ejected. It is to be remembered that chondritic materials keep records of primitive solar system (McSween and Patchen 1989), but some parts are partly melted and heavily metamorphosed.

Abbreviations

HED: 

Howardite-eucrite-diogenite

Opx: 

Orthopyroxene

Declarations

Acknowledgements

We thank the NIPR for the samples and PTS preparation. We thank Prof. M Miyamoto and Dr. T Mikouchi of the Graduate School of Sciences, University of Tokyo, Prof. N Hasebe of Research Institute for Science and Engineering, Waseda University, Prof. T Nakamura of Tohoku University, and Dr. T Noguchi of Kyushu University for their discussion and support of our researches. This research was supported in part for NIPR, the Cooperative Program (No. 108, 2012) of AORI, the University of Tokyo, and for a program of Research Forum of Chiba Institute of Technology.

Authors’ Affiliations

(1)
Department of Earth and Planetary Science, Graduate School of Sciences, University of Tokyo
(2)
Forum Research, Chiba Institute of Technology
(3)
Research Institute for Science and Engineering, Waseda University
(4)
National Institute of Polar Research
(5)
Department of Polar Science, School of Multidisciplinary Sciences, Graduate University for Advanced Studies
(6)
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency
(7)
Department of Life and Environmental Sciences, Chiba Institute of Technology

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Copyright

© Takeda et al.; licensee Springer. 2015

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