Chemical variation of the large Apollo 15 olivine‐normative mare basalt rock samples

Ryder, G.; Schuraytz, B. C.

doi:10.1029/2000je001368

Cited by 53 publications

(40 citation statements)

References 23 publications

(23 reference statements)

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“…The coarse-grained nature of MIL 05035 requires a large amount of sample for a representative bulk rock analysis, as suggested previously for other coarsely crystalline mare basalts (e.g., Ryder and Schuraytz 2001). Previous studies on MIL 05035 have already demonstrated compositional variation in bulk rock compositions, due to the coarse-grain size (Arai et al 2007;Joy et al 2007Joy et al , 2008Korotev and Zeigler 2007).…”

Section: Bulk Rock Compositionsmentioning

confidence: 81%

Petrogenesis of lunar mare basalt meteorite Miller Range 05035

Liu

Floss

Day

et al. 2009

Meteorit & Planetary Scien

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. Symplectites (intergrowth of Fe-augite, fayalite, and silica) of different textures and bulk compositions in MIL 05035 suggest formation by decomposition of ferro-pyroxene during shock-induced heating, which is supported by the total maskelynitization of plagioclase, melt pockets, and the presence of a relict pyroxferroite grain. Petrography and mineral chemistry imply that crystallization of MIL 05035 occurred in the sequence of Fe-poor pyroxenes (Mg# = 50-54), followed by plagioclase and Fe-rich pyroxenes (Mg# = 20-50), and finally hedenbergite, Fe-Ti oxides, and minor late-stage phases. Petrography, bulk chemistry, mineral compositions, and the age of MIL 05035 suggest it is possibly source crater-paired with Asuka (A-) 881757 and Yamato (Y-) 793169, and may also be launch-paired with Meteorite Hills (MET) 01210. MIL 05035 represents an old (~3.8-3.9 Ga), incompatible element-depleted low-Ti basalt that was not sampled during the Apollo or Luna missions. The light-REE depleted nature and lack of Eu anomalies for this meteorite are consistent with an origin distant from the Procellarum KREEP Terrane, and genesis from an early cumulate mantle-source region generated by extensive differentiation of the Moon.

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Section: Bulk Rock Compositionsmentioning

confidence: 81%

Petrogenesis of lunar mare basalt meteorite Miller Range 05035

Liu

Floss

Day

et al. 2009

Meteorit & Planetary Scien

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“…Sample masses for chemical analyses of martian meteorites (when given) are typically 100-500 mg, and this is generally too small to yield representative analyses of crystalline basalt rocks (Ryder and Schuraytz 2001). This problem is exacerbated for the most incompatible trace elements, which are concentrated in small, dispersed mineral grains or melt pockets.…”

Section: Data Sourcesmentioning

confidence: 99%

Chemical compositions of martian basalts (shergottites): Some inferences on b; formation, mantle metasomatism, and differentiation in Mars

Treiman

2003

Meteorit & Planetary Scien

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Abstract-Bulk chemical compositions of the shergottite basalts provide important constraints on magma genesis and mantle processes in Mars. Abundances of many major and trace elements in the shergottites covary in 2 distinct groups: Group 1 (G1) includes mostly highly incompatible elements (e.g., La, Th), and Group 2 (G2) includes mostly moderately incompatible elements (e.g., Ti, Lu, Al, Hf). Covariations of G2 elements (not necessarily linear) are consistent with partitioning between basalt magma and orthopyroxene + olivine. This fractionation represents partial melting to form the shergottites and their crystallization; the restite minerals cannot include aluminous phase(s), phosphate, ilmenite, zircon, or sulfides. Overall, abundances of G1 elements are decoupled from those of G2. In graphing abundances of a G1 element against those of a G2 element, G1/G2 abundance ratios do not appear to be random but are restricted to 4 values. Shergottites with a given G1/G2 value need not have the same crystallization age and need not fall on a single fractionation trajectory involving compatible elements (e.g., Ti versus Fe*). These observations imply that the G1/G2 families were established before basalt formation and suggest metasomatic enrichment of their source region (major carrier of G2 elements) by a component rich in G1 elements.Group 1 elements were efficiently separated from G2 elements very early in Mars' history. Such efficient fractionation is not consistent with simple petrogenesis; it requires multiple fractionations, "complex" petrogenetic processes, or minerals with unusual geochemistry. The behavior of phosphorus in this early fractionation event is inexplicable by normal petrogenetic processes and minerals. Several explanations are possible, including significant compatibility of P in majoritic garnet and the presence of P-bearing iron metal (or a phosphide phase) in the residual solid assemblage (carrier of G2 elements). If the latter, Mars' mantle is more oxidized now than during the ancient fractionation event.

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“…Primitive Apollo 12 and 15 basalts that have been suggested to represent parental compositions for their particular petrographic suites (olivine, pigeonite and ilmenite basalts), have MgO ranging from 8 to 13 wt% (Neal et al, 1994;Ryder and Schuraytz, 2001;Snyder et al, 1997). Thermodynamic modeling of the crystallization sequence of primitive low-Ti Apollo 12 and 15 olivine basalts such as 12009, 12072 and 15555, using the MELTS and MAGFOX codes yield major element compositions that match the LAP basalts (Righter et al, 2005).…”

Section: Constraints On the Lap Source Regionmentioning

confidence: 99%