Listed in The Meteoritical Bulletin, No. 76
Elephant Moraine 87521 (EET 87521)
Dimensions (cm): 3.7 x 2.5 x 2
Physical Description: Carol Schwarz. About 30% of this smooth rounded specimen is covered with black to brown shiny fusion crust. The interior of this breccia is dark and fine-grained with white and yellowish inclusions. It is coherent and has several large 2-3 mm white inclusions located near the exterior of the specimen.
Petrographic Description: Brian Mason. The section shows a microbreccia of pale brown pyroxene and colorless plagioclase clasts, up to 1.2 mm across, in a comminuted groundmass of these minerals. Pyroxene compositions show a wide range: Wo15-39, Fs41-61, En12-41, but cluster around Wo20Fs45 and Wo37Fs48 (one grain is Wo22Fs61). One grain of Fe-rich olivine, Fa91, was analyzed. Plagioclase composition is An68-89. An SiO2 polymorph, probably tridymite, is present in accessory amounts. The meteorite is a brecciated eucrite, but the iron-rich nature of the pyroxenes and the presence of fayalitic olivine distinguishes it from most eucrites.
Lunar Basaltic Breccia
Macroscopic Description: Carol Schwarz and Marilyn Lindstrom. About 30% of this smooth rounded specimen is covered with black to brown shiny fusion crust. The interior of this coherent breccia is dark and fine-grained and contains numerous small white and yellow inclusions. Two 2-3 mm clasts are visible on the surface: One is a white clast consisting of plagioclase with 10-15% yellow and black mafic minerals; the other is a buff-colored clast made up of plagioclase and 35-50% yellow and black mafic minerals.
Thin Section (EET87521,8 & ,9) and Bulk Composition (EET87521,6) Description: Jeremy Delaney and Paul Warren. EET87521 was originally classified as a eucrite. However, more detailed investigations indicate that it is a very-low-titanium (VLT) basaltic breccia of lunar derivation. The modal mineralogy is 5-10% olivine, 45-50% pyroxene, 35-40% plagioclase and 1-2% ilmenite, chromite, ulvospinel/magnetite, sulfide, silica minerals, and FeNi-metal. The matrix of the meteorite also contains several percent of glass similar in composition to the bulk meteorite. The olivine ranges in composition from Fo65 to Fo5, a range typical of VLT mare basalts, and shows a strong bimodality with clusters centered at Fo57-65 and Fo5-15. Intermediate olivine compositions are uncommon. Molar Fe/Mn ratios of the olivine are 90-100. The pyroxene is pigeonite/subcalcic augite/augite with a composition range of En65Wo5-10 to En20Wo15-40. Most pyroxene is iron-rich and comparable to eucritic pyroxene, but is generally more calcic than eucritic pyroxene. The pyroxene does not show the bimodal distribution of the olivine. Pyroxene Fe/Mn ratios are 50-75. These ratios are typical of mare basalts, and much higher than those of basaltic achondrites (30-40). The feldspar is mostly An93-97 with a few more sodic grains present. Several clasts within the thin sections have survived with textures little altered by brecciation. These clasts tend to be relatively coarse-grained, by mare basalt standards. Thin section [,9] contains a small (1 mm) clast of what is probably a highlands impact melt breccia. This extremely fine-grained clast contains at least 70% plagioclase. It also contains the only observed grains of FeNi-metal, with compositions (average 94.1% Fe, 4.53% Ni, 0.37% Co) typical of metals derived as “contamination” from metal-rich meteorites. The bulk composition of EET87521 has been studied by INAA, using two adjacent chips, 278-290 mg in mass. The TiO2 concentration is 0.8-1.1%, and results for ratios such as Fe/Mn, Ga/Al, Na/Ca, and Co/Cr indicate that this sample is lunar, and certainly not a eucrite. In general, the bulk composition shows a striking resemblance to VLT mare basalts from Luna 24. Perhaps the most significant difference is that EET87521 has higher concentrations of incompatible elements, especially light REE. This difference might be caused by the highlands component associated with the FeNi-bearing clast. However, the bulk-rock Ni content (29-43 µg/g) indicates that the total proportion of non-VLT “contaminant” is probably small.
References: J. Delaney (1989) Nature 342, 889-890. P. Warren and G. Kallemeyn (1989) Geochim. Cosmochim. Acta 53, 3323-3330.
Oxygen Isotopic Composition: Robert Clayton. The oxygen isotopic composition is δ18O = +5.39, δ17O = +2.79. These analyses are comparable to those of previously analyzed lunar meteorites and Apollo lunar samples and distinct from those of eucrites.
Listed in The Meteoritical Bulletin, No. 82
Elephant Moraine 96008
Dimensions (cm): 4.5×3.5×1.5
Lunar Basaltic Breccia
Macroscopic Description: Kathleen McBride. 50% of this meteorite is covered by a black glassy fusion crust. Areas that lack fusion crust appear virtually unweathered. The fusion crust is very thinly distributed over the surface of the rock. The matrix is fine grained, medium gray with numerous inclusions. These inclusions are white, light gray and tan and are angular and subangular in shape. Metal and rust are not visible. This is a brecciated basalt, possibly lunar in origin.
Thin Section (,4) Description: Brian Mason. The section shows a microbreccia of pyroxene and plagioclase clasts, up to 1.2 mm across; traces of nickel-iron and sulfide are present, as small scattered grains. Microprobe analyses show that most of the pyroxene ranges from Wo11Fs31 to Wo40 Fs18, with a few more iron-rich grains; plagioclase composition is An93-96. A few olivine grains of variable composition, Fa41-64, were analyzed. Fe/Mn in pyroxene is about 70. The meteorite is a lunar basaltic breccia.
The paired stones we found 9 years apart.
There are some compositional reasons to suspect that EET 87/96 is launch-paired with DEW 12007, QUE 94281, Yamato 793274/981031, NWA 4884, the NWA 7611 clan. See discussion at the NWA 7611 clan.
Meteoritical Bulletin Database
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