Analytical results for the material of the Chelyabinsk meteorite

Geochemistry International (Impact Factor: 0.58). 07/2013; 51(7). DOI: 10.1134/S0016702913070100


This paper presents the results of the mineralogical, petrographic, elemental, and isotopic analysis of the Chelyabinsk meteorite and their geochemical interpretation. It was shown that the meteorite can be assigned to LL5-group ordinary chondrites and underwent moderate shock metamorphism (stage S4). The Chelyabinsk meteorite contains a significant fraction (approximately one-third by volume) of shock-melted material similar in composition to the main volume of the meteorite. The results of isotopic analysis suggest that the history of meteorite formation included an impact event approximately 290 Ma ago.

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Available from: M. A. Nazarov,
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    • "It is natural to assume that a larger parent body could have been disrupted at Sun-grazing conditions. The recovered fragments of the Chelyabinsk meteorite contain significant portions of shock blackened material and melt veins (Galimov et al., 2013; Kohout et al., 2014; Ozawa et al., 2014) that could be produced in the Sun atmosphere (a temperature of the shock-melt vein matrix formation is estimated over 1700-2000º C in (Ozawa et al., 2014)). "
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    ABSTRACT: The orbit of the Chelyabinsk object is calculated, applying the least-squares method directly to astrometric positions. The dynamical evolution of this object in the past is studied by integrating equations of motion for particles with orbits from the confidence region. It is found that the majority of the Chelyabinsk clones reach the near-Sun state. Sixty-seven percent of these objects have collisions with the Sun for 15 Myr in our numerical simulations. The distribution of minimum solar distances shows that the most probable time for the encounters of the Chelyabinsk object with the Sun lies in the interval from −0.8 Myr to −2 Myr. This is consistent with the estimate of a cosmic ray exposure age of 1.2 Myr (Popova et al. 2013). A parent body of the Chelyabinsk object should experience strong tidal and thermal effects at this time. The possible association of the Chelyabinsk object with 86039 (1999 NC43) and 2008 DJ is discussed.
    11/2014; 49(12). DOI:10.1111/maps.12382
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    • "Compositions of olivine and pyroxene from sample 10–90 (Table 4) are very similar to those of LL chondrites and are located in low-Fe region of the Fs-Fa diagram occupied by LL chondrites (Brearly and Jones 1998). These data agree well with previously published data on the olivine and pyroxene compositions of the Chelyabinsk LL5 chondrite (Galimov et al. 2013). Chromite compositions (Table 4) also agree well with expected compositions for LL chromites (Brearly and Jones 1998; Wlotzka 2005). "
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    ABSTRACT: Here we characterize the magnetic properties of the Chelyabinsk chondrite (LL5, S4, W0) and constrain the composition, concentration, grain size distribution, and mineral fabric of the meteorite's magnetic mineral assemblage. Data were collected from 10 to 1073 K and include measurements of low‐field magnetic susceptibility (χ0), the anisotropy of χ0, hysteresis loops, first‐order reversal curves, Mössbauer spectroscopy, and X‐ray microtomography. The REM and REM′ paleointensity protocols suggest that the only magnetizations recorded by the chondrite are components of the Earth's magnetic field acquired during entry into our planet's atmosphere. The Chelyabinsk chondrite consists of light and dark lithologies. Fragments of the light lithology show logχ0 = 4.57 ± 0.09 (s.d.) (n = 135), while the dark lithology shows 4.65 ± 0.09 (n = 39) (where χ0 is in 10−9 m3 kg−1). Thus, Chelyabinsk is three times more magnetic than the average LL5 fall, but is similar to a subgroup of metal‐rich LL5 chondrites (Paragould, Aldsworth, Bawku, Richmond) and L/LL5 chondrites (Glanerbrug, Knyahinya). The meteorite's room‐temperature magnetization is dominated by multidomain FeNi alloys taenite and kamacite (no tetrataenite is present). However, below approximately 75 K remanence is dominated by chromite. The metal contents of the light and dark lithologies are 3.7 and 4.1 wt%, respectively, and are based on values of saturation magnetization.
    Meteoritics & planetary science 06/2014; 49(6). DOI:10.1111/maps.12307 · 3.10 Impact Factor

  • Meteoritics & planetary science 48. · 3.10 Impact Factor
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