Distributions of the relative isotopic abundances of helium, neon, and argon were measured in situ by laser-probe mass spectrometric analysis of Apollo samples 12070,67 (fines and individual gabbro, basalt, feldspar, and glass fragments); 12018,24 gabbro (interior and exterior surface); and 12010,13 breccia (interior and exterior of matrix and vein of fine-grained material). On a scale of 10−3 to 10−5 gram, the distributions of helium, neon, and argon isotopes in these samples are highly variable. The maximum abundances of these gases are located (1) in rocks within <30 μ of the pitted ‘top’ surface (that surface exposed to solar irradiation), (2) in loose fines from the lunar surface, or (3) in veins of fine-grained material within rock breccias. The relative abundances of the helium, neon, and argon isotopes from the ‘top’ surface (<30 μ) of 12018,24 are similar to the isotopic abundances measured in the lunar fines of 12070,67 and are consistent with an origin by solar-wind implantation, having 3He/4He=5.5 and 4.4±0.3×10−4, 4He/20Ne = 97 ± 14, 4He/36Ar = 1050 ± 150, 20Ne/22Ne = 11.2 ± 0.4, and 21Ne/22Ne = 0.035 ± 0.006. A comparison of the ratios of helium, neon, and argon isotopes from these samples with the ratios determined on the fine-grained vein material of 12010,13 and on the previously analyzed fine-grained vein material of Fayetteville and Kapoeta meteorites shows that the 3He/4He is 30% less in the meteorites than in the lunar samples. Furthermore, although the 4He/20Ne from Kapoeta is consistent with the lunar results, the 4He/36Ar is a factor of 3 higher, whereas the relative abundances of isotopic helium, neon, and argon from Fayetteville are not equivalent to the lunar results. Cosmogenic gases, isotopically similar to the gases produced in achondritic meteorites by galactic cosmic-ray bombardment, as well as 40Ar, which is believed to be radiogenic in origin, are distributed in the interior and occasionally on the exterior of the lunar samples.
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