He/Ar and Ne/Ar solar wind ratios in metal separates from ACFER 111, Fayetteville, and Noblesville

Details He/Ar and Ne/Ar solar wind ratios in metal separates from ACFER 111, Fayetteville, and Noblesville He/Ar and Ne/Ar solar wind ratios in metal separates from ACFER 111, Fayetteville, and Noblesville

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994metic..29r.506m&link_type=abstract

Meteoritics (ISSN 0026-1114), vol. 29, no. 4, p. 506-507

Computer Science

3

Chondrites, Lunar Soil, Radioactive Isotopes, Shock Heating, Solar Wind, Energetic Particles, Isotopic Enrichment, Metals, Rare Gases

Scientific paper

All major minerals in lunar soils lost part of their light solar noble gases, shown by the low He-4/Ar-36 and Ne-20/Ar-36 ratios in the first steps of closed-system stepped etching (CSSE) runs. We therefore looked for elementally unfractionated solar noble gases in Fe-Ni separates of chondrites. Fayetteville, Acfer 111, and Noblesville were analyzed by CSSE using copper chloride. Helium, Ne, and Ar isotope ratios display the familiar Solar Wind-Solar Energetic Particle (SW-SEP) two-component structure. Neon-20/neon-22 ratios close to the SW value of 13.8 +/- 0.1 determined from lunar ilmenites are observed in the first steps of Fayetteville and Acfer 111, whereas in Noblesville the highest Ne-20/Ne-22 is 13.4. In all meteorites isotopically heavy SEP Ne is released in later steps. The smoothed Ne-20/Ar-36 ratios for Fayetteville and in the first half of the Acfer 111 run are rather constant and close to present-day solar wind. For Noblesville even the individual steps show a nearly flat Ne-20/Ar-36 pattern with a mean value of 45 +/- 5, identical to present-day solar wind. This shows that the metal retains unfractionated SW-Ne and -Ar and that SW and SEP have nearly identical Ne-20/Ar-36 ratios. The nominal SEP contribution of 30-40% in Noblesville metal is similar to those deduced for Acfer 111, Fayetteville, and ilmenite. These SEP fractions are much higher than the expected ratio of the flux of SW ions to that of higher-energy solar particles.

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