Superior analyses of iron meteorites.
Iron meteorites analysis for Ni, Co, P, C, S and Cu elements by milling technique, noting superiority degree based on Co-Ni correlation
Lewis, C. F.↗
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Work strengthening by a deformation-induced phase transformation in 'MP Alloys'
Work strengthening and microstructure of Co-Ni base alloys containing Cr and Mo, discussing deformation induced martensitic transformation
Graham, A. H.↗
Chemistry and thermal history of metal particles in Luna 20 soils.
Individual metal particles from Luna 20 thin sections 521, 513 and 514 as well as several small metallic inclusions in silicate particles from Luna 20 thin sections 501 and 502 were examined using optical microscopy and the electron microprobe. All the metallic particles and inclusions analyzed are of meteoritic Co-Ni content as are most of the metallic particles from the Fra Mauro and the Apollo 16 highlands sites. It is proposed that most of the metal at these 3 sites had its origin in the meteoritic projectiles that bombarded and accumulated in the early lunar crust. It is apparent that the metallic particles and some of the metallic inclusions in the Luna 20 soil have been subjected to reheating on the moon and this process has removed any evidence of the original meteoritic microstructure of the metal.
Goldstein, J. I.↗
Metallic particles in the glassy constituents of three lunar highland samples 65315, 67435 and 78235
Electron probe microanalysis and analytical electron microscopy techniques were employed to obtain structural and chemical analyses of metal particles in the size range of less than 1000 A and greater than 5 microns from the glassy constituents of 3 lunar highland samples 65315, 67435 and 78235. Most of the micron size metal particles in the glass coatings of the three samples are of meteoritic Co-Ni content. The Ni content of submicron metal often differs significantly from the micron size metal in the same glass. This difference can be explained by one of 3 reasons: (a) the presence of metal of different sizes and Ni contents in the rock prior to the shock event, (b) the presence of metal particles in the lunar soil of meteoritic or variable Ni content which were incorporated when the glass formed and (c) the production of submicroscopic Fe metal from the reduction of Fe(+2) in the shock produced melt.
Mehta, S.↗