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Origin of lunar ultramafic green glasses: constraints from phase equilibrium studies

Origin of lunar ultramafic green glasses: constraints from phase equilibrium studies,10.1016/S0016-7037(00)00365-3,Geochimica Et Cosmochimica Acta,L.

Origin of lunar ultramafic green glasses: constraints from phase equilibrium studies   (Citations: 22)
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Phase equilibria experiments on an Apollo 14B green glass composition are used to develop a petrogenetic model for the Apollo 14B green glasses. New compositional data for the Apollo 14B green glasses are presented, which replace the original data set of Delano (1986). Near-liquidus phase relations of the 14B green glass are determined from 1.3 to 2.7 GPa and 1380 to 1570°C. The liquidus is saturated with olivine to 2.4 GPa and orthopyroxene above 2.4 GPa. A multiple saturation point with olivine and orthopyroxene occurs at 1560°C and 2.4 GPa. Crystallization of the ol + opx saturation boundary involves 40 wt% ol and 60 wt% opx, and occurs over a 140°C interval before cpx appears at a reaction boundary. Crystallization/melting models are developed to reproduce the compositional variations displayed by the Apollo 14B glasses using these phase equilibrium constraints. Fractional crystallization alone cannot account for the observed variation in the major element abundance of the Apollo 14B green glasses. Assimilation is also necessary, in particular, to fit variations in TiO2, FeO, Na2O and Al2O3. The 14B glasses show evidence of simultaneous high-Ti assimilation and fractional crystallization of olivine, followed by simultaneous KREEP assimilation and olivine fractionation. The data requires the high-Ti assimilant to be at a greater depth than the KREEP assimilant, but only constrains the total assimilation/fractional crystallization process to occur between approximately 2.3 and 0.5 GPa. Assimilation of a high-Ti cumulate within this depth range is consistent with an overturn/hybrid mantle remelting model. Highlands crust assimilation is precluded for the Apollo 14B green glasses.
Journal: Geochimica Et Cosmochimica Acta - GEOCHIM COSMOCHIM ACTA , vol. 64, no. 13, pp. 2339-2350, 2000
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    • ...Beginning with small planetary bodies, such as the Earth's Moon, we calculated the P-Ts of Lunar basalts from Apollo 17 (Warner et al., 1975) and high Mg Lunar glasses (green picritic glasses) from Apollo 14B (Elkins et al., 2000 )( Fig. 5A)...
    • ...Apollo 14 glasses yield much higher temperatures of 1550–1600 °C and pressures of 1.6–3.0 GPa (300–600 km), within error of multiple saturation experiments, which yield 1560 °C and 2.4 GPa (Elkins et al., 2000; Shearer et al., 2006)...

    Cin-Ty A. Leeet al. Constraints on the depths and temperatures of basaltic magma generatio...

    • ...High-Ca pyroxene, plagioclase and ilmenite are not stable on the liquidus at high P even in the most Ti-rich glasses (Delano, 1986; Wagner and Grove, 1997; Elkins et al., 2000)...
    • ...Results are from studies by Elkins et al. (2000) and Draper et al. (2006)...
    • ...This process was further modeled by Spera (1992), Hess and Parmentier (1995), and Elkins et al. (2000) with varying degrees of success...

    C. K. Sheareret al. Big returns on small samples: Lessons learned from the analysis of sma...

    • ...However, Delano [52] has pointed out that if lunar picritic glasses originated from source regions at pressures of 2 GPa in the Moon [53], the pressure dependence of the C–CO–CO2 buffer would cause the redox state at those pressures in the Moon to be ∼1.5 log units fO2, above the IW buffer...

    A. Khanet al. Constraining the composition and thermal state of the moon from an inv...

    • ...This residual mantle is very deep, on the order of 500 km for the Apollo 14 picritic green glasses [Elkins et al., 2000] and the Apollo 15 picritic red glasses [Delano, 1980]...

    Alyssa R. Becket al. Dunite channels as viable pathways for mare basalt transport in the de...

    • ...Multiple saturation points references are as follows: Luna 24, 17 VLT [31]; 70215, 70017 [32]; 15065, 15555 [33]; 12009 [34]; 14072 [35]; 15016 [36,37]; 74275 [38]; 12002 [39]; 12022 [40]; 14 black [41]; 15C, 15A [28] ;1 4 VLT[42]; 74220 [43]; 14B [44]; 15 red [45]...

    Linda T. Elkins-Tantonet al. Magmatic effects of the lunar late heavy bombardment

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