Computer Science
Scientific paper
Sep 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988ioch.rept...66b&link_type=abstract
In NASA, Washington, Infrared Observations of Comets Halley and Wilson and Properties of the Grains p 66-67 (SEE N89-13330 04-89
Computer Science
4
Cometary Atmospheres, Halley'S Comet, Interplanetary Dust, Interstellar Matter, Meteorites, Chemical Composition, Grain Size, Isotopes, Mass Spectra
Scientific paper
The variability of the mineral forming elements in the submicron Halley grains provides a powerful basis for comparison of Halley with the different classes of meteoritic materials that have been studied in the lab. The degree of variability in the Halley samples is larger than that seen in chondrites implying that Halley is more heterogeneous at the submicron scale. A critical distinction is that Halley contains abundant pure Mg silicates at the size scale while the carbon rich meteorites do not. The submicron dispersion composition seen in Halley is dramatically different from the narrowly constrained compositions seen in CI and CM (type 1 and 2) carbonaceous chondrites. These meteorites are carbon rich but are dominated by a hydrated silicate with a very narrow range of Mg/Si ratio. The Halley results are also unlike the composition variations seen in most of interplanetary dust types that are dominated by hydrated materials. The only known class of meteoritic material that appear to closely resemble the Halley data is a class of cosmic dust composed entirely of anhydrous minerals. The composition implies that Halley is dominated by olivine, pyroxene, iron sulfide, glass and amorphous carbonaceous matter.
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