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Mineralogy of four Itokawa particles collected from the first touchdown site
Earth, Planets and Space volume 66, Article number: 124 (2014)
Four Itokawa particles collected from the first touchdown site were mineralogically investigated by optical microscopy, micro-Raman (μ-Raman) spectrometry, scanning electron microscopy (SEM), electron microprobe analysis (EPMA), X-ray absorption spectroscopy (XAS), and transmission electron microscopy (TEM). Their mineralogy has an affinity to that of LL6 chondrites based on micro-Raman spectroscopy, EPMA, and XAS analyses. However, the space weathering rims on them are less developed than those observed on the Itokawa particles collected from the second touchdown site. Solar flare tracks are rarely observed in the four particles, whose number densities were lower than those observed in the Itokawa particles from the second touchdown site.
In 2005, the Hayabusa spacecraft sampled twice from the Muses-C Regio of the asteroid (25143) Itokawa filled with myriad of pebbles. The distance between two touchdown sites is about 100 m (Nakamura et al.2014). The Itokawa particles investigated during the initial analyses in 2011 were collected from the second touchdown site (sample number: RB-QD04-xxxx), and those from the first touchdown site (sample number: RA-QD02-xxxx) were investigated in the first announcement of opportunity (AO) consortium, which includes this study. The Itokawa particles from the second touchdown site showed mineralogical and isotopic affinities to LL5-6 chondrites (Nakamura et al.2011; Yurimoto et al.2011; Nakamura et al.2012; Tsuchiyama et al.2011,2014; Nakashima et al.2013). Nakamura et al. (2014) reported that olivine, pyroxene, and plagioclase in six particles from the first touchdown site have chemical compositions similar to those from the second touchdown site. As a part of the first AO consortium, four Itokawa particles from the first touchdown site were allocated to us.
Although the sampling sites are located just about 100 m away from each other within the MUSES-C Regio, the reflectance spectra at the MUSES-C Regio show a variation in the relative reflectance associated with wavelength (Ishiguro et al.2007). Because it is thought that the degree of spectral reddening is related to the abundance of nanophase Fe0 on the surface material of Itokawa (e.g., Binzel et al.2001; Hiroi et al.2006), the microstructures of the external surface of the Itokawa particles from the first touchdown site are worth comparing with those from the second touchdown site.
Because the number of Itokawa particles collected from the first touchdown site is limited, six particles allocated to Nakamura et al. (2014), four particles to Tsuchiyama et al. (2014), and another four particles to this study, mineralogical data of the four Itokawa particles would contribute to clarify the mineralogy of the Itokawa particles from the first touchdown site.
The four Itokawa particles collected from the first touchdown site were mineralogically investigated by optical microscopy, micro-Raman (μ-Raman) spectrometry, scanning electron microscopy (SEM), electron microprobe analysis (EPMA), X-ray absorption spectroscopy (XAS), and transmission electron microscopy (TEM). Among these methods, XAS is the newly applied technique for the analysis of the Itokawa samples.
If the affinity of Itokawa particles to LL5-6 chondrites is common, the redox state experienced by the four Itokawa particles in their parent body should be almost identical to that in LL5-6 chondrites. Therefore, the relative abundance of Fe3+ and Fe2+ ions in ferromagnesian silicates, which reflect the redox states, in the particles from Itokawa were measured and compared with those in ferromagnesian silicates in an LL chondrite. We used Tuxtuac LL5 chondrite for comparison. The X-ray absorption near-edge structure (XANES) of Fe K-edge is an X-ray absorption spectroscopy (XAS) technique used to compare Itokawa to chondrite meteorite samples.
Four Itokawa particles collected during the first touchdown were allocated to our group (Table 1). The particles were stored in a sealed box in the clean chamber no. 2, in which the sample curation of the Itokawa particles is going on in an ultrapure N2 atmosphere, and were transferred to and opened in an N2-purged glove box. Both the chamber and the glove box were installed in the Planetary Material Sample Curation Facility of JAXA (PMSCF/JAXA). All the samples were embedded in epoxy resin in the glove box to avoid contact with earth’s atmosphere. Dew-point temperature was around -40°C during embedding and curing. After cure of epoxy, they were stored in an N2-gas-filled aluminum-laminated plastic bag and transferred to Ibaraki University for further processing and analyses.
The cross sections at the external surface of the four particles were observed by using Hitachi HF-3300 cold field-emission (FE) TEM (Hitachi High-Technologies Co., Tokyo, Japan) equipped with EDAX energy dispersive X-ray spectrometer (EDS) (Philips, Amsterdam, Netherlands) at Hitachi High-Technologies Co. An additional TEM observation was performed by using FEI Titan TEM (FEI, Hillsboro, OR, USA) at Lawrence Livermore National Laboratory, USA, and JEOL JEM-2100 TEM (JEOL Ltd., Tokyo, Japan) at Ibaraki University. Solar flare tracks in the Itokawa samples were obtained by a method similar to the weak-beam dark-field method (e.g., Williams and Carter2009).
Raman spectra of potted butts of the four samples (the epoxy-embedded sample remained after ultramicrotomy) were measured with a μ-Raman spectrometer (JASCO Inc., NRS-3100, Tokyo, Japan) at Ibaraki University to identify minerals. The wavelength of excitation laser is 532 nm. The beam diameter of the laser is 2 μm. The peak position of the strongest Raman shift peak of metallic Si was calibrated to 520 cm-1. Measuring time was 40 s × 2, and the laser power was from 1 to 10 mW. After micro-Raman measurements, the potted butts were coated by carbon, and their textures were studied with a focused ion beam combined with scanning electron microscope (FIB-SEM) JEOL JIB-4501 equipped with JED-2100 EDS (JEOL Ltd., Tokyo, Japan) at Ibaraki University. Mineral chemistry was measured with a JEOL JXA-8530F FE-EPMA (JEOL Ltd., Tokyo, Japan) at JEOL Co. Acceleration voltage and probe current were 15 kV and 9 nA, respectively. ZAF-oxide correction was applied to calculate chemical compositions of minerals.
The potted butts of the four Itokawa particles and a polished thin section of the Tuxtuac LL5 chondrite were analyzed using the Beamline I18 X-ray micro-focus spectroscopy beamline (Diamond Light Source Ltd, Oxfordshire, UK) at the Diamond Light Source, Oxfordshire, UK. Diamond is a 3-GeV synchrotron with ring currents of approximately 250 mA. Energy selection with fractional energy resolutions of 10-4 to 10-5 are achieved with an Si (111) and (311) double crystal monochromator, respectively. An Si drift vortex detector was used to measure the X-ray fluorescence and absorbance of elements with Z >40. Fe K-edge X-ray absorption spectroscopy (XAS) was performed on approximately 2.5-μm spots and also with a mapping routine over approximately 5 × 40 μm areas. Typical experimental conditions used for XAS were 1-s integration at each 5.0 eV energy step up to approximately 7,100 eV, followed by a higher resolution of 0.1 eV energy steps over the XANES features up to 7,150 eV, and continuing over the EXAFS region with steps of 2 to 4 eV up to 7,660 eV. The errors of the Fe K-edge positions were ±0.05 eV.
After the XAS, FIB sections of RB-QD04-0008 and RB-QD04-0024 were prepared from their potted butts by JEOL JIB-4501 FIB-SEM (JEOL Ltd., Tokyo, Japan) and an ultra-low energy Ar ion milling machine Fischione NanoMill (E.A. Fischione Instruments, Inc., Corporate Circle Export, PA, USA) at Ibaraki University. Because the external surfaces of the Itokawa particles existed at the bottom of these potted butt samples, the ultrathin sections and the FIB sections were prepared from the opposite sides of these particles although the thickness of these particles were unknown. The FIB sections were observed by FE-TEM JEOL JEM-2800 at JEOL Co. and JEOL JEM-2100 TEM (JEOL Ltd., Tokyo, Japan) at Ibaraki University.
Description of the four Itokawa particles
The optical photomicrographs of the four allocated particles before ultramicrotomy and backscattered electron (BSE) images of their potted butts after ultramicrotomy are presented in Figures 1 and2, respectively. RB-QD04-0008 is an approximately 40-μm-wide composite grain. An approximately 20-μm equigranular olivine attaches a high-Ca pyroxene similar in form and size (Figure 1a). Both of the olivine and high-Ca pyroxene in this sample contain small opaque grains (<2 μm in diameter: black dots in Figure 1a). Three of them were cropped out to the surface of the potted butt and are enriched in Fe and S. Therefore, the opaque minerals include troilite (Figure 2a). Both RB-QD04-0011 and RB-QD04-0015 are 35 and 46 μm wide, respectively, and composed only of anhedral olivine including small amounts of opaque minerals (<2 μm in diameter) (Figure 1b,c). No opaque mineral was exposed to the surfaces of their potted butts (Figure 2b,c). RB-QD04-0024 is a flat and thin (<10 μm) approximately 50-μm-long grain composed of low-Ca pyroxene and plagioclase containing with abundant small (<2 μm in diameter) opaque minerals. The opaque minerals appeared on the potted butts are troilite (Figure 2d). Olivine, low-Ca pyroxene, and high-Ca pyroxene in these Itokawa particles do not show clear undulatory extinction. Because low-Ca pyroxene in RB-QD04-0024 does not display polysynthetic twinning, it is expected to be orthopyroxene, which is supported by μ-Raman spectrometry, which will be described in the next section. The optical features of plagioclase in RB-QD04-0024 were not able to be determined due to the small grain size.
Raman shift peaks assignable to olivine, low-Ca pyroxene, and high-Ca pyroxene were obtained (Table 2). However, no peaks of plagioclase in RB-QD04-0024 were detected, and we did not identify whether it is maskelynite or not. Olivine grains in RB-QD04-0008, RB-QD04-0011, and RB-QD04-0015 show a doublet peak. According to Kuebler et al. (2006), the shorter and the longer wavenumber peaks of the olivine doublet are called DB1 (doublet peak #1) and DB2 (doublet peak #2), respectively. The peak positions of DB1 and DB2 are displayed in Table 2 and plotted in a DB2 position vs DB1 position diagram (Figure 3). A hatched area in Figure 3, which appears as a narrow curved band along the Fo70 curve, shows the range of forsterite (Fo) mol% obtained by EPMA for these olivine grains. Forsterite mol% estimated by the DB1 and DB2 positions is approximately 10 percentage points higher than the actual Fo mol%. Low-Ca pyroxene in RB-QD04-0024 shows a doublet near approximately 670 cm-1 (677.6 and 656.1 cm-1), which is indicative of orthopyroxene (Wang et al.2001).
Chemical compositions of olivine and pyroxenes
Chemical compositions of olivine, low-Ca pyroxene, and high-Ca pyroxene were obtained by EPMA. Representative data are shown in Table 3. A histogram of Fa mol% (100-Fo mol%) is shown in Figure 4. Olivine in the four Itokawa grains are homogeneous, and their Fa mol% are within the range of those in the equilibrated grains investigated during the initial analysis (Fa27.1-30.7: Nakamura et al.2011). Average and standard deviation of Fa mol% of olivine in RB-QD04-0008, RB-QD04-0011, and RB-QD04-0015 are 30.5 ± 0.6 (n = 3), 29.7 ± 0.3 (n = 3), and 31.0 ± 0.7 (n = 2), respectively.
Chemical compositions of low-Ca and high-Ca pyroxenes are plotted on a pyroxene quadrilateral diagram (Figure 5). Average and standard deviation of En and Wo mol% of low-Ca pyroxene in RB-QD04-0024 are 74.3 ± 0.3 and 2.2 ± 0.02 (n = 3), respectively. En and Wo mol% of high-Ca pyroxene in RB-QD04-0008 are 46.1 and 41.9, respectively. Chemical composition of plagioclase was not obtained due to its small size.
Fe K-edge XANES of olivine
The Fe K-edge XANES plots of olivine in three Itokawa particles show a clear absorption pre-edge feature, which is common to olivine in the Tuxtuac LL5 (Fo71.0 ± 0.3, n = 25) and terrestrial San Carlos olivine (approximately Fo90) (Figure 6a). The edge positions and the pre-edge centroid positions of olivine in the three Itokawa particles are 7,119.5 to 7,119.8 eV and 7,112.5 to 7,112.6 eV, respectively. These values are indistinguishable from those in terrestrial olivine and olivine in Tuxtuac (Table 4).
Fe K-edge XANES of pyroxene
The edge position and the pre-edge centroid position of low-Ca pyroxene in the Itokawa grain 0024 are 7,119.7 to 7,119.8 and 7,112.6 eV, respectively (Figure 6b). These values are indistinguishable from those measured in low-Ca pyroxene in the Tuxtuac LL5 chondrite (Wo1.5 ± 0.3En75.1 ± 0.5, n = 15): 7,119.8 and 7,112.6 eV, respectively (Table 4).
Surface modification at the external surfaces of the four Itokawa particles was investigated using FE-TEM. High-resolution bright-field TEM images show that two Itokawa particles RB-QD04-0015 and RB-QD04-0024 have an amorphous zone (labeled ‘I’ in Figure 7c,d) and a partially amorphized zone (labeled ‘II’ in Figure 7c,d), while those of the other two particles (RB-QD04-0008 and RB-QD04-0011) display sharp lattice fringes to the surface (Figure 7a,b). The thickness of the amorphous layer is 5 to 8 nm (indicated by double-headed arrows marked ‘I’ in Figure 7c,d). In both cases, approximately 2-nm-size poorly crystalline nanophase inclusions (indicated by arrows) exist on the external surface. By comparing Figure 7, high-angle annular dark field-scanning transmission electron microscope (HAADF-STEM) images and elemental distribution maps (Figure 8), the nanophases form a densely arranged array at the external surface, which is indicated by arrows in HAADF-STEM images of Figure 8. Mg and Fe elemental maps indicate that the inclusions are enriched in these elements (Figure 8). Figure 8 shows that the nanophase inclusions in RB-QD04-015 are enriched in S as well as Mg and Fe.
Just below the nanophase-rich layer, there are Si enrichment and depletion in Mg and Fe in both of RB-QD04-0015 and RB-QD04-0024. In the case of RB-QD04-0024, the lower part of the amorphous layer (labeled as B) is more electron transparent than the upper part (labeled as A), suggestive of lower density. In addition, a slight enrichment of Al is detected in RB-QD04-0015.
Below the amorphous layer, underlying olivine and low-Ca pyroxene show partial amorphization indicated by arrows marked ‘II’ in Figure 7c,d. The partially amorphized olivine and low-Ca pyroxene contains 2-to-4-nm-size nanophases (Figure 7e,f). Their lattice fringes range from 0.19 to 0.20 nm, suggestive of (110) of α-iron metal (Noguchi et al.2014). The amorphous layer containing nanophase (Fe,Mg)S and the underlying partially amorphized minerals containing nanophase Fe are similar to the composite rims observed on the Itokawa particles investigated in the initial analysis (Noguchi et al.2014). The composite rim is composed of a redeposition zone and a partially amorphized zone, called zones I and II, respectively (Noguchi et al.2014).
Surface modification of two different areas within a single particle
To assess whether surface modification was heterogeneously distributed on a single Itokawa particle, two FIB sections were prepared from two Itokawa particles. By using both ultrathin sections and FIB sections, surface modification on the opposite sides of these particles was able to be examined. In both cases, the same mineral existed on the opposite sides. One is RB-QD04-0008, which has almost no surface modification, and the other is RB-QD04-0024 having a composite rim. Figure 9 shows dark-field images of the FIB sections of these particles. The FIB section of the former does not show any surface modification, and the latter has surface modification of approximately 50 nm thick (indicated by an arrow), which corresponds to the total thickness of the composite rim.
Solar flare tracks
The solar flare tracks in the four Itokawa particles were searched based on the dark-field TEM observation. The tracks are rare in the Itokawa particles investigated in this study. Figure 10a shows a possible solar flare track in olivine in an ultrathin section of RB-QD04-0015. The number density of the solar flare tracks was estimated to be <1 × 109 tracks/cm2. A composite rim of <50 nm thick is seen on the external surface. On the other hand, the number density of the solar flare tracks is obviously higher in some Itokawa particles collected at the first touchdown site that were investigated in the initial analysis. For example, Figure 10b shows a dark-field image of low-Ca pyroxene in a FIB section of RA-QD02-0009, in which solar flare tracks are indicated by arrows. The track number density was estimated to be 2 × 109 cm-2. This particle has a vesicular composite rim of approximately 80 nm (Noguchi et al.2014).
Morphology and mineralogy of RB-QD4-0008
Because their sizes (approximately 35 to approximately 50 μm) are comparable to the smallest grains investigated during the initial analysis (whole size range: approximately 30 to approximately 180 μm) (Nakamura et al.2011,2014), the petrography of the Itokawa grains investigated in this study is simpler than that of those investigated in the initial analysis. Among them, RB-QD04-0008 has a unique morphology although the other Itokawa particles are fragments composed of an olivine grain (RB-QD04-0011 and RB-QD04-0015) or low-Ca pyroxene and plagioclase (RB-QD04-0024). The particle is composed of partially-connected equigranular olivine and high-Ca pyroxene. Itokawa particles having a morphology similar to these particles have been reported previously (Nakamura et al.2011; Matsumoto et al.2012; Noguchi et al.2014). For example, RA-QD02-0060 is composed of a large twinned low-Ca clinopyroxene and small olivine and vesiculated plagioclase. In this particle, the dislocation density of olivine grains is variable. This fact suggests that such porous aggregate particles were formed by the recrystallization of mineral particles, each of which has a different history.
The Enstatite (En) and Wo contents (mol%) in the high-Ca pyroxene in RB-QD04-0008 are 46.1 and 41.9, respectively, which are outside the range of the En and Wo contents in high-Ca pyroxene in the highly equilibrated grains investigated in the initial analysis (Nakamura et al.2011) (Figure 5). The mol% of Wo is similar to those of high-Ca pyroxene in LL6 chondrites (McSween and Patchen1989). By considering the above discussion, RB-QD04-0008 may have been formed by recrystallization and it contains mineral fragments that experienced thermal metamorphism as high as most LL6 chondrites experienced.
Mineralogy of low-Ca pyroxene in RB-QD4-0024
As described in the ‘Raman spectroscopy’ section, the low-Ca pyroxene in RB-QD04-0024 is orthopyroxene. The average Wo mol% of the low-Ca pyroxene is 2.2, which is higher than that of the equilibrated Itokawa particles (Wo1.4: Nakamura et al.2011,2014) and within the range of LL6 chondrites (Wo1.7-2.6: McSween and Patchen1989). The highly equilibrated particles (HEP) from the second touchdown site were regarded as being comparable with LL5-6 chondrites based on the Wo mol% of both low- and high-Ca pyroxene (Nakamura et al.2011,2014), and the low-Ca pyroxene in RB-QD04-0024 is plotted at the highest Wo mol% of low-Ca pyroxene in the HEP (Figure 5). These data suggest that RB-QD04-0024 is a mineral fragment that experienced thermal metamorphism comparable with the typical LL6 chondrites. Although we investigated only four Itokawa particles in this study, each particle experienced a different metamorphic history, which is consistent with the previous studies of Itokawa particles (Nakamura et al.2011,2014).
Space weathering and solar flare track density
Two of the four Itokawa particles investigated in this study show textural modification at the external surfaces based on TEM observation. They have amorphous surface layers and underlying partially amorphized olivine or low-Ca pyroxene (Figures 7 and8). In RB-QD04-0015, the amorphous surface layer contains Al, which is not contained in olivine. These features correspond to those of the composite rims, which have probably been formed by space weathering (Noguchi et al.2011,2014).
The rims of RB-QD04-0015 and RB-QD04-0024 do not have blisters that are lenticular bubbles formed by ion implantation (e.g., Igarashi et al.2002). On the other hand, blisters were observed in 3 among 12 Itokawa particles in the initial analysis (Noguchi et al.2014). Although the number of particles investigated in this study is limited, the degrees of space weathering may have been more modest than those experienced by the Itokawa particles collected at the first touchdown site that were investigated in the initial analysis.
This interpretation is consistent with the difference in the number density of solar flare tracks between the Itokawa particles investigated in this study and those in the initial analysis. Solar flare tracks were observed in RB-QD04-115, and its number density was estimated to be <1 × 109 cm-2 (Figure 10a). On the other hand, some Itokawa particles investigated in the initial analysis show much higher track density: 1 × 1010 cm-2 in RA-QD02-0033 and 2 × 109 cm-2 in RA-QD02-0009 (Figure 10b). By considering these results, the degrees of space weathering may be different between the two touchdown sites.
Nagao et al. (2011) also predicted the duration for solar wind to be shorter than 103 years based on solar 20Ne concentrations. Considering the solar flare track densities observed in RA-QD02-0033 corresponding to approximately 104 years (Bradley et al.1984), the duration for surface modification should be between 103 and 104 years. For the particles collected at the second touchdown site, the duration could be shorter and <103 years. During such a short duration, the difference in the degrees of space weathering between the two touchdown sites could have resulted.
Surface modification within a single Itokawa particle
Two TEM samples that were prepared from the opposite sides of RB-QD04-0008 do not show any detectable surface modification. On the other hand, two TEM samples that were also prepared from the opposite sides of RB-QD04-0024 have rims similar to the composite rims described in Noguchi et al. (2014), who have also reported that two TEM samples prepared from RA-QD02-0032 had a composite rim. These data suggest that the Hayabusa spacecraft was able to recover Itokawa particles without significant modification and that fine-grained particles on the surface of Itokawa were homogeneously irradiated by solar wind, which may be a result of the low surface gravity on Itokawa (approximately 10-4 ms-2; Hirata et al.2009) and levitation of fine-grained particles by electrostatic repulsion caused by a photoelectron effect (Lee1996; Hartzell and Scheeres2013).
In the initial analysis, Nagao et al. (2011) analyzed noble gas isotopes in the Itokawa particles collected at the first touchdown. They revealed that the noble gas compositions and the release profiles vary even among the particles collected at the same touchdown site. The variety was thought to reflect different trapping sites of solar wind noble gases: Noble gases released at lower temperatures could be solar winds with lower kinetic energy and hence be trapped in the outermost layer of the grains, whereas gases released at higher temperatures could reside in deeper layers due to their higher kinetic energy. In the shallower surface layer of each grain, helium could be more enriched compared to that in the deeper surface layer, as observed in the bulk metallic glass of the Genesis (Grimberg et al.2008). These noble gas signatures are consistent with the interpretation of our TEM results; the Itokawa particles could have been collected by the Hayabusa spacecraft as is on the Itokawa surface.
Redox state of the four Itokawa particles and comparison with that of the Tuxtuac LL5 chondrite
By measuring the Fe K-edge XANES of olivine and low-Ca pyroxene in the four Itokawa samples, we checked whether they were as reduced as ordinary chondrites. We found this to be the case, and this is one more piece of evidence about the similarity to LL chondrites. The Fe K-edge positions and the Fe K pre-edge centroid positions of olivine, low-Ca pyroxene, and high-Ca pyroxene in the four Itokawa grains overlap with those in the Tuxtuac LL5 chondrite (Table 4). These data indicate a negligible abundance of Fe3+ ions in ferromagnesian silicates in both the Itokawa grains and equivalent Tuxtuac minerals, which is consistent with the mineralogical, petrological, and oxygen isotopic data of the Itokawa grains investigated in the initial analyses (Nakamura et al.2011,2014; Tsuchiyama et al.2011,2014; Nakamura et al.2012; Yurimoto et al.2011; Nakashima et al.2013).
None of the Itokawa particles investigated in this study contain pentlandite inclusions, which is consistent with the low abundance of pentlandite in LL chondrites (<<1%) (Graham et al.1988; Jamsja and Ruzicka2010).
Relationships between Fo mol% estimated by Raman spectroscopy and Fo mol% obtained by EPMA
Forsterite mol% estimated by Raman spectroscopy in this study is Fo80, which is 10 percentage points higher than the Fo mol% obtained by EPMA (Figures 3 and4). On the other hand, Fo mol% estimated by Raman spectroscopy in Noguchi et al. (2012) was consistent with that obtained by EPMA in Noguchi et al. (2012). The wavelength of the excitation laser is different between these studies. A green laser (λ = 532 nm) was applied in this study, while a near infrared laser (λ = 785 nm) was used in Noguchi et al. (2012). Some Raman shift peaks are excited from epoxy by a green laser. On the other hand, no significant peaks are excited from epoxy by a near infrared laser. Because a broad peak from epoxy (approximately 830 cm-1) overlaps with the olivine doublet centered at approximately 830 cm-1, it is likely that the overlap reflects the deconvolution of the doublet.
We investigated four Itokawa particles collected from the first touchdown site. They are indistinguishable from LL6 chondrites based on Raman spectroscopy, EPMA, and XANES analyses. The space weathered rims on them are observed but less developed on the Itokawa particles collected from the second touchdown site. This result may be consistent with the difference of the solar flare track density between the particles collected during the first touchdown and those collected during the second touchdown. However, a further study is needed to confirm this estimation because of the limited numbers of the particles investigated in this study.
Binzel RP, Rivkin AS, Bus SJ, Sunshine JM, Burbine TH: MUSES-C target asteroid (25143) 1998 SF36: a reddened ordinary chondrite. Meteorit Planet Sci 2001, 36: 1167–1172. 10.1111/j.1945-5100.2001.tb01950.x
Bradley JP, Brownlee DE, Fraundorf P: Discovery of nuclear tracks in interplanetary dust. Science 1984, 226: 1432–1434. 10.1126/science.226.4681.1432
Graham AM, Christophe Michel-Levy M, Danon J, Easton AJ: The Tuxtuac, Mexico, meteorite, an LL5 Chondrite fall. Meteoritics 1988, 23: 321–323. 10.1111/j.1945-5100.1988.tb00916.x
Grimberg A, Baur H, Bühler F, Bochsler P, Wieler R: Solar wind helium, neon, and argon isotopic and elemental composition: data from the metallic glass flown on NASA’s Genesis mission. Geochim Cosmochim Acta 2008, 72: 626–645. 10.1016/j.gca.2007.10.017
Hartzell CM, Scheeres DJ: Dust levitation on asteroids and the Moon. J Geophy Res Planet 2013, 118: 116–125. 10.1029/2012JE004162
Hirata N, Barnouin-Jha OS, Honda C, Nakamura R, Miyamoto H, Sasaki S, Demura H, Nakamura AM, Michikami T, Gaskell RW, Saito J: A survey of possible impact structures on 25143 Itokawa. Icarus 2009, 200: 486–502. 10.1016/j.icarus.2008.10.027
Hiroi T, Abe M, Kitazato K, Abe S, Clark BE, Sasaki S, Ishiguro M, Barnouin-Jhaet OS: Developing space weathering on the asteroid 25143 Itokawa. Nature 2006, 443: 56–58. 10.1038/nature05073
Igarashi S, Muto S, Tanabe T: Surface blistering of ion irradiated SiC studied by grazing incidence electron microscopy. J Nucl Mater 2002, 307–311: 1126–1129.
Ishiguro M, Hiroi T, Tholen DJT, Sasaki S, Ueda Y, Nimura T, Abe M, Clark BE, Yamamoto A, Yoshida F, Nakamura R, Hirata N, Miyamoto H, Yokota Y, Hashimoto T, Kubota T, Nakamura AM, Gaskell RW, Saito J: Global mapping of the degree of space weathering on asteroid 25143 Itokawa by Hayabusa/AMICA observations. Meteorit Planet Sci 2007, 42: 1791–1800. 10.1111/j.1945-5100.2007.tb00538.x
Jamsja N, Ruzicka A: Shock and thermal history of Northwest Africa 4859, an annealed impact-melt breccia of LL chondrite parentage containing unusual igneous features and pentlandite. Meteorit Planet Sci 2010, 45: 828–849. 10.1111/j.1945-5100.2010.01056.x
Kuebler KE, Jolliff BL, Wang A, Haskin LA: Extracting olivine (Fo-Fa) compositions from Raman spectral peak positions. Geochim Cosmochim Acta 2006, 70: 6201–6222. 10.1016/j.gca.2006.07.035
Lee P: Dust levitation on asteroids. Icarus 1996, 124: 181–194. 10.1006/icar.1996.0197
Matsumoto T, Tsuchiyama A, Gucsik A, Noguchi R, Matsuno J, Nagano T, Imai Y, Shimada A, Uesugi M, Uesugi K, Nakano T, Takeuchi A, Suzuki Y, Nakamura T, Noguchi T, Mukai T, Abe M, Yada T, Fujimura A: Micro-structure of particle surfaces of Itokawa regolith and LL chondrite fragments. 43rd Lunar Planet Sci Conf; 2012. Abstract #1969 CD-ROM Abstract #1969 CD-ROM
McSween HY Jr, Patchen AD: Pyroxene thermobarometry in LL-group chondrites and implications for parent body metamorphism. Meteoritics 1989, 24: 219–226. 10.1111/j.1945-5100.1989.tb00696.x
Nagao K, Okazaki R, Nakamura T, Miura YN, Osawa T, Bajo K, Matsuda S, Ebihara M, Ireland TR, Kitajima F, Naraoka H, Noguchi T, Tsuchiyama A, Yurimoto H, Zolensky ME, Uesugi M, Shirai K, Abe M, Yada T, Ishibashi Y, Fujimura A, Mukai T, Ueno M, Okada T, Yoshikawa M, Kawaguchi J: Irradiation history of Itokawa regolith material deduced from noble gases in the Hayabusa samples. Science 2011, 333: 1128–1131. 10.1126/science.1207785
Nakamura T, Noguchi T, Tanaka M, Zolensky ME, Kimura M, Tsuchiyama A, Nakato A, Ogami T, Ishida H, Uesugi M, Yada T, Shirai K, Fujimura A, Okazaki R, Sandford SA, Ishibashi Y, Abe M, Okada T, Ueno M, Mukai T, Yoshikawa M, Kawaguchi J: Itokawa dust particles: a direct link between S-type asteroids and ordinary chondrites. Science 2011, 333: 1113–1116. 10.1126/science.1207758
Nakamura E, Makishima A, Moriguti T, Kobayashi K, Tanaka R, Kunihiro T, Tsujimori T, Sakaguchi C, Kitagawa H, Ota T, Yachi Y, Yada T, Abe M, Fujimura A, Ueno M, Mukai T, Yoshikawa M, Kawaguchi J: Space environment of an asteroid preserved on micrograins returned by the Hayabusa spacecraft. Proc Natl Acad Sci U S A 2012, 109: 4031–4032.
Nakamura T, Nakato A, Ishida H, Wakita S, Noguchi T, Zolensky ME, Tanaka M, Kimura M, Tsuchiyama A, Ogami T, Hashimoto T, Konno M, Uesugi M, Yada T, Shirai K, Fujimura A, Okazaki R, Sandford SA, Ishibashi Y, Abe M, Okada T, Ueno M, Kawaguchi J: Mineral chemistry of MUSES-C Regio inferred from analysis of dust particles collected from the first- and second-touchdown sites on asteroid Itokawa. Meteorit Planet Sci 2014, 49: 215–227. 10.1111/maps.12247
Nakashima D, Kita NT, Ushikubo T, Noguchi T, Nakamura T, Valley JW: Oxygen three-isotope ratios of silicate particles returned from asteroid Itokawa by the Hayabusa spacecraft: a strong link with equilibrated LL chondrites. Earth Planet Sci Lett 2013, 379: 127–136.
Noguchi T, Nakamura T, Kimura M, Zolensky ME, Tanaka M, Hashimoto T, Konno M, Nakato A, Ogami T, Fujimura A, Abe M, Yada T, Mukai T, Ueno M, Okada T, Shirai K, Ishibashi Y, Okazaki R: Incipient space weathering observed on the surface of Itokawa dust particles. Science 2011, 333: 1121–1125. 10.1126/science.1207794
Noguchi T, Kimura M, Nakamura T, Kitajima T, Tsuchiyama A, Abe M, Fujimura A, Mukai T, Okada T, Ueno M, Yada T, Ishibashi Y, Shirai K, Okazaki R: An attempt to identify minerals in the Itokawa dust particles by micro-Raman spectroscopy. Bunseki Kagaku 2012, 61: 299–310. 10.2116/bunsekikagaku.61.299
Noguchi T, Kimura M, Hashimoto T, Konno M, Nakamura T, Zolensky ME, Okazaki R, Tanaka M, Tsuchiyama A, Nakato A, Ogami T, Ishida H, Sagae R, Tsujimoto S, Matsumoto T, Matsuno J, Fujimura A, Abe M, Yada T, Mukai T, Ueno M, Okada T, Shirai K, Ishibashi Y: Space weathered rims found on the surfaces of the Itokawa dust particles. Meteorit Planet Sci 2014, 49: 188–214. 10.1111/maps.12111
Tsuchiyama A, Uesugi M, Matsushima T, Michikami T, Kadono T, Nakamura T, Uesugi K, Nakano T, Sandford SA, Noguchi R, Matsumoto T, Matsuno J, Nagano T, Imai Y, Takeuchi A, Suzuki Y, Ogami T, Katagiri J, Ebihara M, Ireland TR, Kitajima F, Nagao K, Naraoka H, Noguchi T, Okazaki R, Yurimoto H, Zolensky ME, Mukai T, Abe M, Yada T, et al.: Three-dimensional structure of Hayabusa samples: origin and evolution of Itokawa regolith. Science 2011, 333: 1121–1125. 10.1126/science.1207794
Tsuchiyama A, Uesugi M, Uesugi K, Nakano T, Noguchi R, Matsumoto T, Matsuno NT, Imai Y, Shimada A, Takeuchi A, Suzuki Y, Nakamura T, Noguchi T, Abe M, Yada T, Fujimura A: Three-dimensional microstructure of samples recovered from asteroid 25143 Itokawa: comparison with LL5 and LL6 chondrite particles Meteorit. Planet Sci 2014, 42: 172–187.
Wang A, Jolliff BL, Haskin LA, Kuebler KE, Viskupic KM: Characterization and comparison of structural and compositional features of planetary quadrilateral pyroxenes by Raman spectroscopy. Am Mineral 2001, 86: 790–806.
Williams DB, Carter CB: Transmission electron microscopy: a textbook for materials science. 2nd edition. Springer, New York, NY, USA; 2009:760.
Yurimoto H, Abe K, Abe M, Ebihara M, Fujimura A, Hashiguchi M, Hashizume K, Ireland TR, Itoh S, Katayama J, Kato C, Kawaguchi J, Kawasaki N, Kitajima F, Kobayashi S, Meike T, Mukai T, Nagao K, Nakamura T, Naraoka H, Noguchi T, Okazaki R, Park C, Sakamoto N, Seto Y, Takei M, Tsuchiyama A, Uesugi M, Wakaki S, Yada T, et al.: Oxygen isotopic compositions of asteroidal materials returned from Itokawa by the Hayabusa mission. Science 2011, 333: 1116–1119. 10.1126/science.1207776
We thank the Hayabusa project team for the return sample. We express our thanks to N. Mori, I. Ohnishi, and K. Shimada for supporting to use FE-EPMA and FE-TEM at JEOL Corporation and Kyushu University. L. P. Keller was appreciated for the discussion on the track density at the Hayabusa symposium. We are grateful for T. Mikouchi’s and A. Tsuchiyama’s valuable referee comments. T. Noguchi was supported by JSPS KAKENHI grant number 2424408. J Bridges and L. Hicks were supported by STFC, UK.
The authors declare that they have no competing interests.
The manuscript was written by TN and verified for accuracy by all authors. TN performed ultramicrotomy and TEM observation. JCB, LJH, and SG obtained Fe XANES data. TN, MK, TH, MK, and JPB performed STEM observation. TN, TN, RO, MU, TY, YK, MA, and TO prepared Itokawa samples. RO supported FE-EPMA analysis. MT performed FIB sample preparation. HK provided information of XANES of ferromagnesian silicates. All authors read and approved the final manuscript.
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Noguchi, T., Bridges, J.C., Hicks, L.J. et al. Mineralogy of four Itokawa particles collected from the first touchdown site. Earth Planet Sp 66, 124 (2014). https://doi.org/10.1186/1880-5981-66-124
- Space weathering
- Solar flare tracks