Mineralogy of interplanetary dust particles from the 'olivine' infrared class

Details Mineralogy of interplanetary dust particles from the 'olivine' infrared class Mineralogy of interplanetary dust particles from the 'olivine' infrared class

May 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986e%26psl..78...53c&link_type=abstract

Earth and Planetary Science Letters (ISSN 0012-821X), vol. 78, no. 1, May 1986, p. 53-66.

Other

23

Grain Size, Infrared Spectra, Interplanetary Dust, Mineralogy, Olivine, Electron Microscopy, Microstructure, Solar Flares, Interplanetary Dust, Particles, Mineralogy, Electron Microscopy, Origin, Tem, Olivine, Samples, Extraterrestrial, Infrared, Wavelengths, Spectra, Composition, Mineralogy, Matrix, Structure, Exposure Age, Formation

Scientific paper

Analytical electron microscopy observations establish that olivine is abundant and the predominant silicate phase in three interplanetary dust particles (IDPs) from the 'olivine' infrared spectra category. Two of the particles have microstructures resembling those of most nonhydrous chondritic IDPs, consisting of micron to submicron grains together with a matrix composed of amorphous carbonaceous material and sub-500 A grains. In addition to olivine these particles respectively contain enstatite and magnetite, and pentlandite plus Ca-rich clinopyroxene. The third IDP consists mostly of olivine and pyrrhotite with little or no matrix material. Olivine grains in this particle contain prominent solar-flare ion tracks with densities corresponding to a space-exposure age between 1000 to 100,000 years. Although the three particles have olivine-rich mineralogies in common, other aspects of their mineralogies and microstructures suggest that they experienced different formation histories. The differences between the particles indicate that the olivine infrared spectral category is a diverse collection of IDPs that probably incorporates several genetic groups.

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