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Physical and Mineralogical Properties of Anhydrous Interplanetary Dust Particles in the Analytical Electron Microscope

Published online by Cambridge University Press:  12 April 2016

J. P. Bradley
J. P. Bradley*
Affiliation:
McCrone Associates, Westmont, Illinois 60559, USA

Abstract

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The fine grained mineralogy and petrography of anhydrous “pyroxene” and “olivine” classes of chondritic interplanetary dust have been investigated by numerous electron microscopic studies. The “pyroxene” interplanetary dust particles (IDPs) are porous, unequilibrated assemblages of mineral grains, metal, glass, and carbonaceous material. They contain enstatite whiskers, FeNi carbides, and high-Mn olivines and pyroxenes, all of which are likely to be well preserved products of nebular gas reactions. Solar flare tracks are prominent in most “pyroxene” IDPs, indicating that they were not strongly heated during atmospheric entry. The “olivine” IDPs are coarse grained, equilibrated mineral assemblages that have probably experienced strong heating. Since most “olivine” IDPs do not contain tracks, it is possible that this heating occurred during atmospheric entry.

Type
Interplanetary Dust: Physical and Chemical Analysis
Information
International Astronomical Union Colloquium , Volume 126: Origin and Evolution of Interplanetary Dust , 1991 , pp. 63 - 70
Copyright
Copyright © Kluwer 1991

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