Implications for the origins of pure anorthosites found in the feldspathic lunar meteorites, Dhofar 489 group
© Nagaoka et al.; licensee Springer. 2014
Received: 10 April 2014
Accepted: 2 September 2014
Published: 10 September 2014
Remote observation by the reflectance spectrometers onboard the Japanese lunar explorer Kaguya (SELENE) showed the purest anorthosite (PAN) spots (>98% plagioclase) at some large craters. Mineralogical and petrologic investigations on the feldspathic lunar meteorites, Dhofar 489 and Dhofar 911, revealed the presence of several pure anorthosite clasts. A comparison with Apollo nearside samples of ferroan anorthosite (FAN) indicated that of the FAN samples returned by the Apollo missions, sample 60015 is the largest anorthosite with the highest plagioclase abundance and homogeneous mafic mineral compositions. These pure anorthosites (>98% plagioclase) have large chemical variations in Mg number (Mg# = molar 100 × Mg/(Mg + Fe)) of each coexisting mafic mineral. The variations imply that these pure anorthosites underwent complex formation processes and were not formed by simple flotation of plagioclase. The lunar highland samples with pure anorthosite and the PAN observed by Kaguya suggest that pure anorthosite is widely distributed as lunar crust lithology over the entire Moon.
KeywordsMoon Lunar crust Lunar magma ocean Pure anorthosite Lunar meteorite Lunar returned sample Mineralogy Petrology
On the basis of mineralogical and geochemical investigations of the returned Apollo lunar samples, we determined that ferroan anorthosite (FAN) is the main component of a lunar feldspathic crust (e.g., Taylor et al. 1991). In the global lunar magma ocean (LMO) model, the early lunar feldspathic crust was produced by the crystallization and flotation of plagioclase from the LMO (e.g., Warren 1985). However, the samples returned by Apollo missions were collected from a relatively small and geochemically restricted anomalous region of the central nearside of the Moon (Warren and Kallemeyn 1991). Our more recent knowledge and understanding of the lunar origin and evolution have also been expanded by an analysis of global remote sensing data (e.g., Binder 1998; Kato et al. 2010; Nozette et al. 1994). Compositional dichotomous distributions of Mg numbers (Mg# = molar 100 × Mg/(Mg + Fe)) in highlands determined by the spectral profiler (SP) on Kaguya (Ohtake et al. 2012) and Th abundances revealed by the gamma-ray spectrometer on Kaguya (Kobayashi et al. 2012) indicate that the central farside highland is more primitive because of the lowest Th abundances and highest Mg#. The presence of rocks with high plagioclase abundances at some large craters, according to the Kaguya data, was reported by Ohtake et al. (2009), who proposed the lithology term purest anorthosite (PAN) for rocks with plagioclase content higher than 98%.
A massive PAN layer could be a key for investigating the earliest anorthosite crystallized from the LMO and for providing a constraint on the modeling of the lunar feldspathic crust formation (Ohtake et al. 2009; Yamamoto et al. 2012). However, the presence of pure anorthosite rock samples has not been verified thus far in lunar feldspathic meteorites originating from randomly distributed near-surface materials (Korotev et al. 2010).
Our recent investigations of feldspathic lunar meteorites revealed that such pure anorthosite rock samples occur as common lithic clasts in feldspathic lunar meteorites Dhofar 489 and Dhofar 911 (Nagaoka et al. 2011, 2012; Takeda et al. 2006, 2012). Furthermore, Parmentier and Liang (2010) and Piskorz and Stevenson (2014) discussed the available formation mechanisms of pure anorthosite accumulation from LMO on the basis of each LMO model calculation. These model calculations indicated that pure anorthosite could have been formed from the LMO.
The lunar meteorite Dhofar 489, with a weight of 34.4 g, is a feldspathic breccia including feldspathic lithology embedded in a much finer-grained and darker crystalline matrix (Takeda et al. 2006). An additional lunar meteorite Dhofar 911 was paired with Dhofar 489 on the basis of their cosmic-ray exposure (CRE) (Nishiizumi and Caffee 2006) and geochemical data (Korotev 2012). Although brief descriptions of petrography and reflectance spectroscopy of Dhofar 911 have been reported as a conference abstract (Takeda et al. 2012), detailed petrographic descriptions have not been reported thus far. Dhofar 489 exhibits some magnesian anorthosite clasts, including the magnesian anorthosite MA1 clast consisting of 95% plagioclase and 5% olivine (Fo78). Such magnesian anorthosites are plotted on the gap between FAN and the Mg-suite on the An-Mg# diagram (Takeda et al. 2006). Several large anorthosite clasts included in Dhofar 489 and Dhofar 911 are more abundant in plagioclase (>98%) as compared with the previous magnesian anorthosites, which have plagioclase abundances as high as those of PAN (Ohtake et al. 2009). In this work, we confirm that the anorthosite clasts (>1.5 × 1.5 mm) are pure anorthosites (PA), which are characterized on the basis of their mineralogical and petrologic data.
Some portions of Apollo FAN samples have been reported to consist of high abundances of plagioclase (>98%; e.g., Dixon and Papike 1975; James et al. 1989, 1991; McGee 1993; Warren 1990). Moreover, some FAN samples are modally heterogeneous because they contain several lithologies (e.g., 60025 in Floss et al. 1998). The average proportion of plagioclase is approximately 96% for large FAN rocks (mass >1 g), although the mass-weighted average may be biased by Apollo FAN sample 60015 (Wieczorek et al. 2006). The Apollo FAN sample 60015 is the largest anorthosite, with nearly half the mass of the total FAN and the highest abundances of plagioclase (approximately 99%) among FAN. Therefore, excluding 60015, the mass-weighted average proportion of plagioclase in FAN samples drops to 93% (Wieczorek et al. 2006). We reinvestigate the mineralogy and petrology of 60015 and compare the results with those of pure anorthosites available from the Dhofar 489 group.
In this paper, we perform detailed mineralogical and petrologic studies of several pure anorthosite clasts in the Dhofar 489 group and Apollo FAN 60015 to elucidate the formation mechanism of the pure anorthosites. This paper also discusses a model of the origins of pure anorthosite on the basis of both the ground truth data and new remote sensing data.
Lunar meteorites Dhofar 489, Dhofar 911, and Apollo FAN 60015
Because the mineralogy and petrology of d2 have not been investigated thus far, we describe the texture and mineral chemistry of the d2 in Dhofar 489 in more detail in this work. Sample a was further separated into three portions of a1, a2, and a3. Because sample a3 was adjoined to sample d, it contains part of the d2 clast. Three polished thin sections (PTSs), PTS a3-1, PTS a3-2, and PTS a3-3, were created from sample a3 (Figure 1a). A chip of Dhofar 911 provided by the Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), contains a large anorthosite clast (Takeda et al. 2012). In the present study, this chip was divided into two samples (sample x and sample y), the former of which containing the large anorthosite clast was used for PTS x-1 (Figure 1b).
The Apollo 16 returned sample, 60015, is a coarse-grained cataclastic anorthosite weighing 5.57 kg and is rather pure (>98% plagioclase) and pristine in bulk composition (e.g., Dixon and Papike 1975; McGee 1993; Sclar et al. 1973; Warren 1993). We investigated the mineralogy and petrology of 60015 by using a PTS of the sample, 129, provided by the National Aeronautics and Space Administration/Lyndon B. Johnson Space Center (NASA/JSC).
We characterized the petrography of the PTSs by using a combination of petrographic microscopy, electron probe micro-analysis, and reflectance spectroscopy.
Before conducting the scanning electron microscope (SEM) and electron probe micro-analyzer (EPMA) analyses, the PTSs were coated by carbon. The elemental X-ray maps and backscattered electron (BSE) images were collected by using the Hitachi S-3000 N SEM (Hitachi Ltd., Chiyoda-ku, Japan) at Waseda University. Quantitative mineral compositions were analyzed with the JEOL JXA-8900 EPMA (JEOL Ltd., Akishima-shi, Japan) at the Atmosphere and Ocean Research Institute (AORI), University of Tokyo, with a well-characterized oxide and silicate standards at 15 kV, 1.2 × 10-8 A, and an electron beam with a diameter of approximately 5 μm (e.g., Nagaoka et al. 2013; Takeda et al. 2006).
The ultraviolet-visible-near infrared (UV-VIS-NIR) bi-directional reflectance spectrum of the d2 clast was measured by a JASCO reflectance spectrometer (JASCO, Hachioji-shi, Japan) at JAXA. A chip sample of the d2 clast used for reflectance measurement was prepared from the cut surface of sample a3 after making PTS a3-1. The spectrometer incidence angle was 30°, and the emission angle was 0°.
Mineral chemistry and petrography of Dhofar 489
Dhofar 489 is a feldspathic breccia consisting of mineral fragments and lithic and glassy clasts embedded in a much finer-grained dark crystalline matrix (Figure 1a). PTS a3-1 (4.3 × 2.5 mm) contains one large anorthosite clast (d2) in the crystalline matrix with fragments of plagioclase and angular olivine up to 0.5 and 0.1 mm across, respectively. The d2 clast is classified as pure anorthosite 1 (PA1). PTS a3-2 (5.3 × 4.9 mm) contains two large anorthosite clasts classified as PA2 and PA3 in the crystalline matrix with fragments of plagioclase and angular olivine up to 0.7 and 0.3 mm across, respectively. PTS a3-3 (5.1 × 4.5 mm) contains one large anorthosite clast classified as PA4 in the crystalline matrix with fragments of plagioclase and angular olivine up to 0.9 and 0.2 mm across, respectively. The descriptions of the Dhofar 489 breccia matrix have been reported in detail by Takeda et al. (2006).
The crystalline matrix in Dhofar 489 shows a magnesian anorthositic composition (31 wt.% average Al2O3, average Mg# 79). The An values of the plagioclase fragments are uniform (An96-97). The Fo contents of the olivine fragments range from Fo73 to Fo88. These analytical data of Dhofar 489 determined by this work are within the range of those reported previously (Fo71-87, An93-99; Takeda et al. 2006).
Average mineral compositions (wt.%) in the PA1 and PA5 clasts
Minerals in the PA1 clast
Minerals in the PA5 clast
No. = 6
No. = 2
No. = 3
No. = 5
No. = 7
Clast PA2: PA2 is a silky white clast (Figure 1a) composed of varying sizes <0.5 mm of angular plagioclase crystals that are apparently finer than those of PA1 (Figure 3a). PA2 (1.9 × 3.4 mm) is composed of nearly 100 area% plagioclase (An94-97) and traces of low-Ca pyroxene (Wo10En66Fs24; Mg# 71 to 72) and troilite (Figure 4b). PA2 may be part of an anorthosite consisting of finer-grained plagioclase than that in PA1. The Mg# of mafic minerals are homogeneous (Mg# 71 to 72).
Clast PA3: PA3 is a silky white clast consisting of fine-grained plagioclase (Figures 1a and 3b). The angular plagioclase crystals are also finer than those in PA1 (Figure 3b), and their grain sizes are mostly <0.3 mm. The PA3 clast (1.7 × 1.7 mm) is a fine-grained anorthosite of >99 area% plagioclase (An95-97) and traces of olivine, low-Ca pyroxene, and augite (Figure 4c). Ferroan olivine (Fo57) and augite (Wo34En20Fs46; Mg# 29) are detected in the upper portion of this clast, and minor magnesian low-Ca pyroxene (Wo12En62Fs26 to Wo12En63Fs25; Mg# 69 to 71) and augite (Wo33En49Fs18; Mg# 72) are present in the center. The Mg# of the mafic minerals are heterogeneous (Mg# 30 to 70).
Clast PA4: PA4 is a silky white clast (Figure 1a) composed of highly shocked anorthosite (Figure 3c). The PA4 clast (1.7 × 3.9 mm) is a fine-grained anorthosite composed of >99 area% plagioclase (An94-96) and traces of olivine (Fo64-68), low-Ca pyroxene (Wo11En63Fs26; Mg# 70), and troilite (Figure 4d). The Mg# of mafic minerals are homogeneous (Mg# 64 to 70).
These four clasts are composed of >98 area% plagioclase and small amounts of mafic minerals (<0.1 mm). Although the texture of PA1 preserves coarse plagioclase (>1 mm), other clasts show finer-grained textures. The anorthosite clast AN1 in Dhofar 489 reported by Takeda et al. (2006) is classified as a pure anorthosite according to our criteria. The Fo content of olivine in AN1 (Fo78) is significantly higher than the ferroan olivines in PA1 (Fo61-63), PA3 (Fo57), and PA4 (Fo64-68).
Mineral chemistry and petrography of Dhofar 911
Dhofar 911 is a feldspathic breccia consisting of mineral fragments and lithic clasts in a dark fine-grained crystalline matrix, similar to that of Dhofar 489 (Takeda et al. 2006). PTS x-1 (7.6 × 5.4 mm) contains two large clasts in the crystalline matrix (Figure 1b). The first is classified as pure anorthosite 5 (PA5), and the second is a magnesian anorthosite with a granulitic breccia texture. Such clasts as spinel troctolite with the Mg-Al spinel in Dhofar 489 and magnesian troctolitic granulite in the Dhofar 489 group (Takeda et al. 2006, 2007, 2008; Treiman et al. 2010) are not detected in PTS x-1. Plagioclase fragments up to 0.9 mm across and large angular fragments of orange-yellow olivine crystals with a maximum size of 0.4 × 0.2 mm are present in the crystalline matrix. The large orange-yellow olivines are common in the matrix of other rocks of the Dhofar 489 group (Takeda et al. 2006, 2007, 2008).
The crystalline matrix in Dhofar 911 has a magnesian anorthositic composition (30 wt.% average Al2O3, average Mg# 78) similar to that in Dhofar 489. The An values of plagioclase fragments in Dhofar 911 PTS x-1 range from An96 to An97, and the Fo contents of olivine fragments range from Fo73 to Fo86. The largest angular olivine fragment composition is Fo76. Both compositional ranges of An96-97 in plagioclase fragments and Fo73-86 in olivine fragments in Dhofar 911 PTS x-1 are in the range of those in Dhofar 489 (An96-97; Fo73-88). Similar compositions of the crystalline matrix and mineral fragments could support the pairing of Dhofar 489 and Dhofar 911 (Nishiizumi and Caffee 2006).
Clast PA5: PA5 (1.9 × 1.9 mm) is a silky white clast (Figure 1b) composed of 98.6 area% plagioclase (An95-96), 1.0 area% olivine (Fo75-85), and traces of troilite (Figures 3d and 4e). The largest plagioclase crystal is coarse up to 1.8 mm. The shock textures by meteor impact are disturbed by networks of weathering products (Figure 3d). Some small olivine crystals (<0.1 mm) are located at the marginal part of the largest crystalline plagioclase grains, which partly retain albite twinning. The coarse twinned plagioclase grains indicate an igneous origin, similar to that of PA1. The average mineral compositions are presented in Table 1.
Magnesian anorthosite with granulitic breccia texture
The sizes of olivines at the left edge of this clast are larger than those in the pure anorthosites (<0.1 mm across; PA1 to PA5). The amoeboid aggregate of olivines with rounded shapes suggests that this clast may be a coarse-grained granulitic breccia. The textures of granulitic olivines and the mineral mode in this clast are very close to the description of the magnesian anorthosite (MA1) in Dhofar 489 (Takeda et al. 2006). The mineral compositions of granulitic olivines (Fo85) are slightly more magnesian than those in MA1 (Fo79) are.
Reflectance-spectroscopic results of pure anorthosite
Mineral chemistry and petrography of Apollo FAN, 60015
Plagioclase is the most dominant mineral (>98 area%) in 60015, 129. The An values of euhedral to subhedral plagioclase are uniform (An96-97) and are consistent with reported values of An95-98 (Sclar and Bauer 1974) and An96.4-97.1 (Dixon and Papike 1975).
Eighteen grains of orthopyroxene and three grains of augite are recognized in this section (60015, 129). The average composition of the orthopyroxenes is Wo2En64Fs34, and that of the augites is Wo45En41Fs14. The orthopyroxene compositions are within very limited ranges. The Mg# 62 to 68 are consistent with that of orthopyroxene reported by Dixon and Papike (63; 1975) and McGee (63 to 64; 1993). The augite compositions are also within very limited ranges. The Mg# 73 to 77 are consistent with that of augite reported by Dixon and Papike (74 to 75; 1975) and McGee (76; 1993).
Olivine is not observed in this section, nor is it found in other sections (e.g., Dixon and Papike 1975).
Dhofar 489 has the lowest Th content and the highest Mg# among the feldspathic lunar meteorites (Korotev et al. 2006; Takeda et al. 2006). Takeda et al. (2006) reported that the global map of Th and Fe distributions (e.g., Jolliff et al. 2000) suggests that Dhofar 489 may be derived from the farside of the Moon, owing to its very low Th and Fe contents. On the contrary, Korotev et al. (2006) suggested that its low concentrations of incompatible elements reflect depth and not necessarily distance from the Procellarum KREEP Terrane (PKT) (Jolliff et al. 2000) on the nearside. ‘KREEP’ materials are enriched in such elements as potassium (K), rare earth elements (REE), and phosphorus (P) (e.g., Taylor et al. 1991). The recent Kaguya data (Kobayashi et al. 2012; Ohtake et al. 2012) revealed that the central farside highland has a more primitive aspect owing to the lower Th content and higher Mg#. Ohtake et al. (2009) reported the presence of pure anorthosite from observations by the multi-band imager (MI) data onboard Kaguya, in which the spatial resolution is 20-m VIS and 62-m NIR per pixel at a nominal altitude of 100 km. As shown by Kobayashi et al. (2012), the spatial resolution of the Th map is 450 km, which was degraded in order to improve the precision of the Th abundance, and the relative error is within several percentage points. The spatial resolution of the Mg# map was 1° × 1° (=30 × 30 km in the equatorial area), and the relative error is within several percentage points (Ohtake et al. 2012). The spatial resolution of the remote sensing data could be originally larger than the representative scales of the chemical compositions of the lunar rock samples. In this case, the remote sensing data could provide the average composition of each footprint. Although the precision of remote sensing data is not quite as high as that of the sample data, the global trend of Th content and Mg# over the Moon can be confirmed by the positional information because the variations of Th and Mg# are significantly larger than their errors. With reference to their observation by the remote sensing data, we discuss the global anorthositic crust lithology by comparing the lunar highland samples.
Mineralogy and petrology of the pure anorthosite clasts in feldspathic lunar meteorites, Dhofar 489 group
In this section, the mineralogy and petrology of the five large pure anorthosite clasts embedded in Dhofar 489 and Dhofar 911 will be considered. Their textures are classified into three groups; most of the differences among textures may be associated with shock effects. Their shock textures by meteoritic impacts are commonly disturbed by networks of weathered products such as calcite produced at the hot desert in Oman (Korotev 2012).
Group II includes PA2 and PA4, which are composed of plagioclase crystals of varying sizes (Figure 3) that are apparently finer than those of PA1. These brecciated anorthosites may have experienced shock events and were then metamorphosed from coarse-grained igneous anorthosite such as PA1 or larger single crystals of plagioclase. The compositions of minerals in each clast are homogeneous and include plagioclase (An94-97) and traces of low-Ca pyroxene (Mg# 71 to 72) in PA2 and plagioclase (An94-96), olivine (Fo64-68), and low-Ca pyroxene (Mg# 70) in PA4.
Group III includes PA3, which is a highly shocked brecciated anorthosite consisting of fine-grained plagioclase (An95-97) similar to those in group II. The chemical compositions of the mafic minerals in the d4 clast are heterogeneous (Mg# 30 to 70) and include olivine (Fo57), low-Ca pyroxene (Mg# 69 to 71), and augite (Mg# 29, 72). Although the texture is similar to that of group II, this clast could be a mechanically mixed breccia of differentiated pure anorthosite lithologies, as indicated by the large compositional variation in the mafic minerals.
Plagioclase compositions in the four pure anorthosite clasts in Dhofar 489 are within a very narrow compositional range (An94-97). The mafic mineral compositions in PA1 (Fo61-63 of olivine; Mg# 60 to 66 of Opx), PA2 (Mg# 71 to 72 of low-Ca pyroxene), and PA4 (Fo64-68 of olivine; Mg# 70 of low-Ca pyroxene) are uniform in each clast. Previous research of Dhofar 489 (Takeda et al. 2006) indicated that the olivine (Fo78) in AN1 is more magnesian than the mafic minerals in other pure anorthosites in Dhofar 489 (PA1 to PA4). The plagioclase compositions in PA5 in Dhofar 911 are within a very narrow range (An95-96) similar to the pure anorthosites in Dhofar 489 (PA1 to PA4). Olivine compositions in PA5 (Fo75-85) are more magnesian than the mafic minerals in the Dhofar 489 pure anorthosites. These pure anorthosite clasts in the Dhofar 489 group show chemical variations in the Mg# of mafic minerals.
The bulk chemical composition of PA1 (d2) was reported in previous works (Karouji et al. 2004; Takeda et al. 2006). The texture of the PA1 is partly disturbed by networks of weathered products (e.g., calcite) at the hot desert in Oman (Figure 2c). Therefore, the bulk composition of PA1 (Takeda et al. 2006) may involve terrestrial weathered products (Korotev 2012). Siderophile element abundances in PA1 are Co at 1.6 ppm, Ni at <18 ppm, and Ir at <3 ppb. The bulk Ni content in the PA1 clast is below the detection limit and thus gives a low bulk Ni/Co ratio of <11 (Karouji et al. 2004; Takeda et al. 2006). These data support the theory that this clast is a pristine rock fragment scarcely affected by meteoritic contamination.
Mineralogy and petrology of Apollo FAN 60015 as compared with other Apollo FAN samples
Anorthosites of the Apollo samples, referred to as FAN owing to their ferroan compositions, were produced in the more evolved magma ocean (e.g., Warren 1985, 1990). According to the modal and mineralogical data of FAN, this suite could be divided into several subgroups including anorthositic ferroan (AF), mafic magnesian (MM), anorthositic sodic (AS), and mafic ferroan (MF), as explained by James et al. (1989, 2002) and Floss et al. (1998).
Implication for lunar anorthositic crust model on the study of lunar anorthosite samples
The original LMO model on the basis of the Apollo samples assumed that flotation of plagioclase was produced by one-dimensional convection on the magma surface. However, the gamma-ray spectrometer and spectral profiler on Kaguya revealed compositional dichotomous distributions in the highlands of Th abundances (Kobayashi et al. 2012) and Mg# (Ohtake et al. 2012) in which indicated the central farside highland showed the lowest Th abundance and highest Mg# among feldspathic highland regions.
Studies of Apollo/Luna samples and lunar meteorites have revealed that nearly all feldspathic highland samples are polymict rocks heavily brecciated by numerous impacts and metamorphosed by shock heating (e.g., Cahill et al. 2004; Cohen et al. 2005; Joy et al. 2010; Korotev 2005; Lindstrom and Lindstrom 1986; Nagaoka et al. 2013; Warren et al. 2005; Yamaguchi et al. 2010).
The samples of the Dhofar 489 group are crystalline matrix anorthositic breccias composed of diverse mixtures of lithic or glassy clasts including impact-melt breccias and granulitic breccias (Takeda et al. 2006, 2007, 2008; Treiman et al. 2010). Although magnesian anorthosites (MA1, MA2; Takeda et al. 2006) and the magnesian anorthosite with the granulitic breccia texture (Figure 5) are less metamorphosed than the lunar magnesian granulitic breccias in the Dhofar 489 group (e.g., Takeda et al. 2006, 2007, 2008; Treiman et al. 2010), their textures including aggregates of olivines with rounded shapes suggest that they may have been thermally metamorphosed. Such magnesian clasts found in feldspathic lunar meteorites are implied to be different from Mg-suite rocks returned from the central nearside by Apollo missions due to a lack of incompatible elements such as REEs (e.g., Takeda et al. 2006; Treiman et al. 2010). The origin of these magnesian rocks without KREEP signatures is assumed to be not a direct formation from a magma ocean; rather, they could be products of more complex crustal formation processes (Gross et al. 2014). Furthermore, these magnesian clasts are commonly brecciated by numerous impacts and were thermally metamorphosed by shock heating; thus, they could have experienced complex metamorphic processes (Takeda et al. 2012).
Ohtake et al. (2012) presented an asymmetric crustal growth model for interpreting the dichotomy of Mg# distribution with a higher Mg# in the farside than that in the nearside. The model (Ohtake et al. 2012) uses a surface convectional force from the nearside to the farside generated by a higher temperature on the nearside caused by thermal shielding of the Earth on a tilted convection model (Loper and Werner 2002). This force-transported plagioclase crystallized at the first stage of crustal formation in the farside. Moreover, a high Mg# anorthosite ‘rockburg’ developed in the farside, and the ferroan crust crystallized from the more evolved magma formed in the nearside (Ohtake et al. 2012). If large Mg# variations of mafic minerals among the pure anorthosites could reflect the global trend of the anorthositic crust as observed by the remote sensing data, the Mg# variations of mafic minerals among the pure anorthosites could be explained by the different timing of crystallization sequence during the asymmetric crustal growth crystallization (Ohtake et al. 2012), which resulted in either lateral (regional) or vertical (depth) heterogeneity of the putative massive layer of pure anorthosite (Ohtake et al. 2009; Yamamoto et al. 2012).
If the variations in Mg# could be derived from relatively local variations over small distances inside the same cumulate rock, merely a sequence of compositional changes by crystallization of a huge magma system could not explain such local variations. If so, pure anorthosite may have undergone fractional crystallization in the cumulate pile, which resulted in large variations of Mg# (from approximately 80 to approximately 60) over small distances. A special mechanism to explain such large variations within local regions is required, although a specific process explaining the variations on the Moon has not been determined thus far. Anorthosites with high abundances of plagioclase (>95%) on the Earth are produced by deformation (Lafrance et al. 1996). If the lunar pure anorthosite could be produced by deformation or recrystallization, such Mg# variation could occur locally by such processes. Relatively mafic-rich anorthosite could be derived from the remaining liquid, as discussed by Ohtake et al. (2009). However, although we could confirm a global trend of Mg# in the lunar anorthositic crust (Ohtake et al. 2012), it would be difficult to explain such a global trend merely by local variations of Mg# caused by recrystallization and deformation processes.
In this paper, we performed mineralogical and petrologic investigations on lunar meteorites Dhofar 489 and Dhofar 911 and the Apollo returned FAN sample 60015. Several pure anorthosite clasts have been found in the Dhofar samples, and 60015 is an anorthosite with high abundance of plagioclase and uniform composition in comparison with other FAN samples. These anorthosite samples are thought to be identified as pure anorthosite rocks composed of high abundances of igneous plagioclase (>98% plagioclase) or metamorphosed anorthosite from such pure anorthosites. The recent remote observation by the Kaguya (Ohtake et al. 2009; Yamamoto et al. 2012) showed that PAN (>98% plagioclase) spots are widely distributed over the Moon. These samples may be able to indicate the ground truth of PAN.
The combination of our petrologic and mineralogical studies for the pure anorthosite samples and Kaguya remote sensing results of PAN could have a profound implication for the global existence of PAN in feldspathic rocks. Furthermore, these pure anorthosites of the Dhofar 489 group show large chemical variations in Mg# from nearly 60 to more than 80 of each coexisting mafic mineral. The variations of Mg# observed among the pure anorthosite samples imply that those pure anorthosites were not formed from simple flotation of plagioclase but instead underwent a more complex formation process. The presence of pure anorthosite samples necessitates reconsideration of the origin and processes of crustal formation.
electron probe micro-analyzer
inductively coupled plasma mass spectrometry
lunar magma ocean
- MA clast:
magnesian anorthosite clast
- PA clast:
pure anorthosite clast
neutron-induced prompt gamma-ray analysis
polished thin section
scanning electron microscope
We appreciate professor emeritus Manabu Kato of JAXA/ISAS for providing us with the meteorite sample Dhofar 911. The study of the PTS of 60015 (60015, 129) was enabled by NASA/JSC (PI: Makiko Ohtake). Mineralogical analyses were supported by the National Institute of Polar Research, Tokyo, and the cooperative program (2012, No. 108; 2013, No. 111; H. Takeda) of the Atmosphere and Ocean Research Institute at the University of Tokyo. This work was in part supported by Research Fellowships of the Japan Society for the Promotion of Science for Young Scientists, and a Waseda University Grant for Special Research Projects (Project No. 2013A-900). We greatly appreciate Yasuo Ogawa, Hauke Hussmann, and two anonymous reviewers for their helpful comments and suggestions for improving this manuscript.
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