Feldspathic clasts in Yamato-86032: Remnants of the lunar crust with implications for its formation and impact history

Low concentrations of Th and Fe in the Yamato (Y)-86032 bulk meteorite support earlier suggestions that Y-86032 comes from a region of the moon far distant from the Procellarum KREEP Terrain (PKT), probably from the lunar farside. Ar-39-Ar-40, Rb-Sr, Sm-Nd, and Sm-isotopic studies characterize the chronology of Y-86032 and its precursors in the mega regolith. One of the rock types present in a light gray breccia lithology is an anorthosite characterized by plagioclase with An similar to 93, i.e., more sodic than lunar FANs, but with very low Rb-87/Sr-86 and Sr-87/Sr-86 similar to those of FANs. (FAN stands for Ferroan Anorthosite). This An93 anorthosite has Nd-isotopic systematics similar to those of nearside norites. A FAN-like An97 anorthosite is present in a second light-colored feldspathic breccia clast and has a more negative epsilon(Nd) value consistent with residence in a LREE-enriched environment as would be provided by an early plagioclase flotation crust on the Lunar Magma Ocean (LMO). This result contrasts with generally positive values of epsilon(Nd) for Apollo 16 FANs suggesting the possibility of assymetric development of the LMO. Other possible explanations for the dichotomy in epsilon(Nd) values are advanced in the text. The Y-86032 protolith formed at least 4.43 +/- 0.03 Ga ago as determined from a Sm-Nd isochron for mineral fragments from the breccia, clast composed predominantly of An93 anorthosite and a second clast of more varied composition. We interpret the mineral fragments as being predominatly from a cogenetic rock suite. An Ar-39-Ar-40 age of 4.36-4.41 +/- 0.035 Ga for a third clast composed predominantly of An97 anorthosite supports an old age for the protolith. Initial Nd-143/Nd-144 in that clast was -0.64 +/- +/- 0.13 epsilon-units below Nd-143/Nd-144 in reservoirs having chondritic Sm/Nd ratios, consistent with prior fractionation of mafic cumulates from the LMO. A maximum in the Ar-39-Ar-40 age spectrum of 4.23 +/- 0.03 Ga for a second sample of the same feldspathic breccia clast probably reflects some diffusive Ar-40 loss. Lack of solar wind and lunar atmosphere implanted Ar in the light gray breccia clast allows determination of an Ar-39/Ar-40 age of 4.10 +/- 0.02 Ga, which is interpreted as the time of initial brecciation of this litholgy. After correction for implanted lunar atmosphere 40Ar, impact melt and dark regolith clasts give Ar ages of 3.8 +/- 0.1 Ga implying melt formation and final breccia assembly similar to 3.8 Ga ago. Some breccia lithologies were exposed to thermal neutron fluences of similar to 2 x 10(15) n/cm(2), only about 1% of the fluence experienced by some other lunar highlands meteorites. Other lithologies experienced neutron fluences of similar to 1 X 10(15) n/cm(2). Thus, Y-86032 spent most of the time following final brecciation deeply buried in the megaregolith. The neutron fluence data are consistent with cosmogenic Ar-38(cos) cosmic ray exposure ages of similar to 10 Ma. Variations among differing lithologies in the amount of several regolith exposure indicators, including cosmogenic noble gas abundances, neutron capture induced variations in Sm isotopic abundances, and Ir contents, are consistent with a period of early (greater than or similar to 3. 8 Ga ago) lunar regolith exposure, subsequent deep burial at greater than or similar to 5 m depth, an ejection from the moon similar to 7-10 Ma ago. (c) 2006 Elsevier Inc. All rights reserved.