Other
Scientific paper
Jul 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994metic..29r.446b&link_type=abstract
Meteoritics (ISSN 0026-1114), vol. 29, no. 4, p. 446-447
Other
Achondrites, Chemical Composition, Chondrites, Line Spectra, Meteoritic Composition, Spectral Reflectance, Abundance, Emission Spectra, Iron Oxides, Mineralogy, Solar System Evolution
Scientific paper
The link between individual classes of meteorites and their parent bodies is an important question for solar system history. Besides the reflectance spectroscopy of asteroids, the study of pre-counter orbits of meteorites could reveal the direct relation between different types of asteroids and meteorite classes. The spectral observation of meteors can be used to derive the bulk chemical components of meteoroids. The accuracy is much lower than in laboratory studies of meteorites. The radiation of meteors, consisting of emission spectral lines, is produced by the hot gaseous envelope around the meteor body. The gas is formed by the vapors of the ablated material and the atmosphere. To derive the chemical composition of the meteoroid from meteor spectra, we have to eliminate all other factors. This can be done by physical modeling or by comparing meteors of similar parameters (velocity, brightness, height). A search was performed in part of the Ondrejov meteor spectra archives. Most meteors were found to have 'normal' spectra, which are consistent with normal solar system abundances of the observed elements. Most meteoroids are therefore either chondrites or of cometary origin. Among 53 meteors, only one Fe meteoroid and one probable diogenite was found. The abundances computed from meteor spectra are usually given relative to Fe. This is because Fe lines are by far the most numerous in meteor spectra. The temperature and other parameters are based mostly on the appearance of the Fe spectrum and the abundances of other elements result naturally as ratios to Fe. The meteoroid of original mass of about 0.7 kg was completely destroyed in the atmosphere. The spectrum of this meteor is unique in our sample by the low intensity of the Na line and high intensity of the Mg line. It was found that the Na/Fe ratio was at least seven times lower than in other meteors and the ratios of Mg, Si, and Cr to Fe at least twice as high.
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