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QUE94201 – 12.02 Grams Depleted Basaltic Shergottite

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QUE94201 – 12.02 Grams Depleted Basaltic Shergottite QUE94201 – 12.02 grams Depleted Basaltic Shergottite Figure 1. Photograph illustrating broken interior surface of Martian meteorite QUE94201. Scale is in mm. Cube is 1 cm. (NASA # S96-00376) Introduction QUE94201 was found on a glacial moraine where it zoning in pyroxene in QUE94201 indicates that it cooled “looked different”. A search for other pieces proved quickly from magmatic temperatures. The Fe-Ti oxide unsuccessful (Lofgren, personal communication). compositions indicate that this basalt formed under more reducing conditions than the other shergottites Five sides of QUE94201 are rounded with remnant (McSween et al. 1996; Herd et al. 2001d; Kring et al. fusion crust, while one side appears freshly broken 2003). Karner et al. (2007, 2008) have used Cr and V (figure 1). The interior is coarse-grained, crystalline partitioning between pyroxene and melt, and the valance and glassy (Score and Mason 1995). “Mafic-rich state of V to exactly determine the reducing conditions. areas” (probably shock-melted glass), as large as 5 x 4 mm, were noted during preliminary examination. In Kring et al. (2003) relate QUE94201 to the lherzolitic thin section, the sample is made up of subequal amounts shergottites, because of the LREE depletion, but note of homogeneous maskelynite laths and variable that it was a basaltic liquid before it crystallized. Warren interstitial pyroxene. Maskelynite laths are up to 3.6 et al. (1999) find that QUE94201 analyses are very mm long. low in Ni and Ir content, indicating that it was formed from a magma-source in the interior of Mars, and QUE94201 is a basalt apparently similar to the dark, unrelated to meteorite bombardment. mottled lithology (DML) of Zagami (McSween et al. 1996) as well as “lithology B” of EETA 79001 (Mikouchi The age of QUE94201 is 327 m.y. with an exposure to et al. 1998). However, the phosphorous content of cosmic ray for 2.2 m.y. QUE94201 is high and the REE pattern is strongly depleted in light rare earth elements. The extreme Martian Meteorite Compendium C Meyer 2012 Figure 2. Photomicrograph of thin section of QUE94201,4 illustrating coarse basaltic texture (intergrown plagioclase and pyroxene). Field of view is 2.2 mm. Petrography Harvey et al. (1996) described QUE94201 as a “coarse-grained basalt, consisting of subhedral Fe- The pyroxenes in QUE94201 are complexly zoned rich pigeonite and maskelynite”. Kring et al. (2003) (McKay et al. 1996; Mikouchi et al. 1996; 1998 and not that it was a “bulk melt”, meaning that its composition McSween and Eisenhour 1996). The Mg-rich pigeonite can be used to infer the magmatic source region. Most cores are mantled by Mg-rich augite, which is, in turn, of the pyroxene and maskelynite grains exceed 1 mm rimmed by Fe-rich pigeonite and strongly zoned to in length (up to 3 mm) and are somewhat elongated pyroxferroite (with some hedenbergite at the edge). (figures 2; 7). QUE94201 contains relatively high None of the cores appear to be cumulate phases, as proportions of maskelynite and phosphate when was the case for Shergotty, Zagami and EETA79001B. compared with the other shergottites. The texture is Some of the pyroxenes in QUE94201 are also found to nicely illustrated in figure 7. Melt inclusions are found be sector zoned. in the relict plagioclase (Kring et al. 2003), but no melt inclusions were found in the pyroxene. Interstitial to the pyroxene and shocked plagioclase, are a number of late-stage phases including large Fe-Ti oxides (ulvöspinel, rutile, ilmenite), whitlockite and large Mineralogical Mode for QUE94201 “pockets” of mesostasis similar to the “DN pockets” Harvey Mikouchi of Zagami (McCoy et al. 1995). These “pockets” et al. (1998) et al. (1996) contain an intergrowth of silica and fayalite, as well as, Pyroxene 44 vol. % 43 maskelynite, whitlockite, Fe-Ti oxides, sufides, minor Maskelynite 46 42 augite, chlorapatite and a Zr-rich phase, probably Opaque 2 4 baddelyite (McSween et al. 1996). Fayalite-silica Phosphate 4 6 intergrowths are also found in the cores of large skeletal Mesostasis 4 5 Martian Meteorite Compendium C Meyer 2012 100 REE/CC1 for QUE 94201 10 1 Shergotty (Lodders) QUE 94201 (Lodders) Figure 3. Composition diagram for pyroxene and 0.1 olivine in QUE94201. Data are from Kring et al. La Ce Pr Nd Sm Eu Gd Tb Dy Ho Er Yb Lu (1996), McKay et al. (1996), McSween and Eisenhower Figure 4. Normalized rare earth element (1996) and Mikouchi et al. (1996). Olivine is pure diagram for QUE94201 compared with that of fayalite. Shergotty. phosphate grains adjacent to these pockets (Harvey et Maskelynite: Plagioclase (An66-52) crystallized al. 1996). Aramovich et al. (2002) have carefully throughout the crystallization sequence (McSween and studied the symplectite intergrowths associated with Eisenhour 1996; Mikouchi et al. 1999). The cores are merrillite grains in QUE94201 and conclude that the the most An-rich among the basaltic Martian meteorites. early formation of Ca and Mg-rich merrillite lead to the It has been shocked to maskelynite. Plagioclase is formation of metastable pyroxferroite and ferrosilite, found to include melt inclusions (Kring et al. 2003). which then broke down to become the fine-grained intergrowths. Phosphates: QUE94201 contains more phosphates than other SNC meteorites. Whitlockite (merrillite) has Shock features include maskelynite, mosaicism in been studied by Wadhwa and Crozaz (1996) and found pyroxene and large pockets of glass formed in-situ. to have a more extreme depletion of LREE than for The shock-melted glass is rich in phosphorous (Mikouchi any other shergottite. Mikouchi et al. (1998) analyzed et al. 1998). Papike et al. (2009) compare QUE94201 merrillite up to 3 mm long. Mikouchi et al. (1996, 1998), with the other shergottites. McSween et al. (1996) and Leshin et al. (1996) also report minor chlorapatite in the mesostasis. Aramovich Mineral Chemistry et al. (2002) show that the formation of merrillite is Pyroxene: Pyroxene zoning is extreme (figures 3, 8), often surrounded by symplectite intergrowths. including sector zoning in the cores (Kring et al. 1996; Mikouchi et al. 1996, 1998; McKay et al. 1996; Silica: Silica occurs as distinctive intergrowth with McSween and Eisenhour 1996). Papike (2005 fayalite in “patches” up to 1 mm in-between pyroxene onward) has been obsessed with these pyroxenes. and plagioclase grains (Harvey et al. 1996). Silica was Harvey et al. (1996) report pigeonite zoning to Fs85. also reported as an alteration product by Wentworth Wadhwa and Crozaz (1996), McSween et al. (1996) and Gooding (1991). and Wadhwa et al. (1998) have determined the REE patterns of the pyroxenes and suggested that merrillites Olivine: Fayalite (Fa96-99) occurs as a fine dendritic began crystallizing relatively early. The Eu anomaly intergrowth with silica (Harvey et al. 1996). indicates reducing conditions. Opaques: Large grains of ilmenite are the major “Pyroxferroite”: An analysis of “pyroxferroite” is opaque phase. Analyses for ilmenite and ulvöspinel given in Mikouchi et al. (1998), however, Aramovich are reported in Kring et al. (1996), McSween et al. et al. (2002) point out that the reported composition (1996), Mikouchi et al. (1998) and Herd et al. (2001). (Wo37En3Fs60) is too Ca-rich for it to be termed Chromite has been found in Mg-rich pigeonite core “pyroxferroite”. (Mikouchi et al.). Ulvöspinel exhibits subsolidus Martian Meteorite Compendium C Meyer 2012 Table 1a. Chemical composition of QUE94201. Warren96 Dreibus96 Kring 96 Kring 96 Mikouchi96 Mittlefehldt 96 Warren 97 weight 305 mg 179.8 mg 250mg fusion crust fusion crust 52.74 mg 305 mg SiO2 % 47.06 (a) 43.5 (d) 44.3 (d) 48.00 (d) TiO2 1.95 (a) 1.8 (b) 1.7 (b) 1.81 (d) 2 (d) 1.98 (b) Al2O3 9.64 (a) 12 (b) 11.1 (b) 7.46 (d) 7 (d) 9.82 (b) FeO 18.65 (a) 18.3 (b) 18.3 (b) 24.2 (d) 21 (d) 20.0 (b) 19.16 MnO 0.48 (a) 0.436 (b) 0.44 (b) 0.63 (d) 0.6 (d) 0.47 (b) CaO 11.3 (a) 11.3 (b) 10.9 (d) 11.2 (d) 10.7 (b) 11.48 MgO 6.3 (a) 6.2 (b) 6.04 (d) 6.4 (d) 6.3 (d) Na2O 1.39 (a) 1.75 (b) 1.16 (d) 1.1 (d) 1.53 (b) 1.39 K2O 0.038 (a) 0.052 (b) 0.04 (d) 0.04 P2O3 2.77 (d) 3.4 (d) sum 96.81 98.51 97 98.64 Li ppm C F 40 (b) S Cl 91 (b) Sc 49 (b) 46.6 (b) 51.5 (b) 49.0 (b) V 124 (b) 103 (b) 124 Cr 1030 (b) 890 (b) 1010 Co 24.4 (b) 22.8 (b) 25.9 (b) 24.4 Ni <40 (c) <20 (b) <40 Cu Zn 108 (c) 130 108 Ga 26 (b) 27.1 (b) 25.9 Ge As 0.77 (b) Se Br 0.35 (b) Borg 97 Borg 97 0.38 Rb (b) 0.518 (f) 0.691 (f) <6 Sr 59 (b) 80 (b) 41.3 (f) 49.8 (f) 70 59 Y 31.2 (e) Zr 94 (b) 97.1 (e) 80 94 Nb 0.68 (e) Mo Pd ppb Ag ppb Cd ppb In ppb Sb ppb Te ppb I ppm 4.6 (b) Cs ppm <0.12 Ba <41 (b) <15 (b) <41 La 0.44 (b) 0.35 (b) 0.31 0.44 Ce 1.63 (b) 1.3 (b) 1.0 1.63 Pr Borg 97 Nd 2.4 (b) 1.9 (b) 1.482 (f) 2.36 Sm 2.55 (b) 2.02 (b) 1.233 (f) 1.92 2.55 Eu 1.09 (b) 0.99 (b) 0.9 1.09 Gd 4.3 (b) Tb 0.93 (b) 0.802 (b) 0.78 0.93 Dy 6.1 (b) 5.53 (b) Ho 1.19 (b) Er Tm Yb 3.5 (b) 3.09 (b) 3.02 Lu 0.54 (b) 0.455 (b) 0.42 0.54 Hf 3.4 (b) 3.42 (b) 4.2 3.4 Ta <0.08 (b) 0.023 (b) 0.03 <0.08 W ppb Re ppb Os ppb Ir ppb <2.4 (b) <3 (b) <2.4 Au ppb <1.5 (b) <0.5 Tl ppb Bi ppb Th ppm <0.09 (b) 0.05 (e) <0.09 U ppm 0.0125 (e) <0.2 technique: (a) emp fused bead, (b) INAA, (c ) RNAA, (d) emp, (e) spark sourrce mass spec., (f) isotope dilution mass spec.
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