The mid-infrared transmission spectra of Antarctic ureilites.
The mid-infrared (4000-450 cm-1; 2.5-22.2 micrometers) transmission spectra of seven Antarctic ureilites and 10 Antarctic H-5 ordinary chondrites are presented.  The ureilite spectra show a number of absorption bands, the strongest of which is a wide, complex feature centered near 1000 cm-1 (10 micrometers) due to Si-O stretching vibrations in silicates.  The profiles and positions of the substructure in this feature indicate that Mg-rich olivines and pyroxenes are the main silicates responsible.  The relative abundances of these two minerals, as inferred from the spectra, show substantial variation from meteorite to meteorite, but generally indicate olivine is the most abundant (olivine:pyroxene = 60:40 to 95:5).  Both the predominance of olivine and the variable olivine-to-pyroxene ratio are consistent with the known composition and heterogeneity of ureilites.  The H-5 ordinary chondrites spanned a range of weathering classes and were used to provide a means of addressing the extent to which the ureilite spectra may have been altered by weathering processes.  It was found that, while weathering of these meteorites produces some weak bands due to the formation of small amounts of carbonates and hydrates, the profile of the main silicate feature has been little affected by Antarctic exposure in the meteorites studied here.  The mid-infrared ureilite spectra provide an additional means of testing potential asteroidal parent bodies for the ureilites.  At present, the best candidates include the subset of S-type asteroids having low albedos and weak absorption features in the near infrared.
Sandford
S A
SA
NASA Ames Research Center, Mountain View, CA 94035, USA.
D000864:Antarctic Regions; D019443:Cosmic Dust; D005118:Extraterrestrial Environment; D006838:Hydrocarbons; D058085:Iron Compounds / Q000032:analysis*; D017616:Magnesium Compounds / Q000032:analysis*; D019110:Meteoroids; D008903:Minerals / Q000032:analysis*; D018543:Minor Planets; D017640:Silicates / Q000032:analysis*; D013055:Spectrophotometry, Infrared
D019443:Cosmic Dust; D006838:Hydrocarbons; D058085:Iron Compounds; D017616:Magnesium Compounds; D008903:Minerals; D017640:Silicates; C092478:pyroxene; C034475:olivine