Fractionated matrix composition in CV3 Vigarano and alteration processes on the CV parent asteroid

Authors

  • Sean M. HURT,

    1. Department of Earth and Space Sciences, University of California, Los Angeles, California 90095–1567, USA
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  • Alan E. RUBIN,

    1. Institute of Geophysics and Planetary Physics, University of California, Los Angeles, California 90095–1567, USA
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  • John T. WASSON

    Corresponding author
    1. Department of Earth and Space Sciences, University of California, Los Angeles, California 90095–1567, USA
    2. Institute of Geophysics and Planetary Physics, University of California, Los Angeles, California 90095–1567, USA
    3. Department of Chemistry and Biochemistry, University of California, Los Angeles, California 90095–1567, USA
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Corresponding author. E-mail: jtwasson@ucla.edu

Abstract

Abstract— Although CV3 Vigarano is one of the most primitive CV chondrites, it has lost most of the S from the matrix; matrix Na is also depleted relative to the concentration in bulk CV chondrites. We used a matrix-grid technique to study thirteen 50 × 50 μm regions in Vigarano; in each area, we used an electron microprobe to gather data with an electron beam 3 μm in width. We found two end-member types of matrix textures. One is coarse and porous, has lower Fe contents and lower analytical totals; it appears to be contaminated with comminuted chondrule debris. The other is finer grained and appears smooth; its mean composition has higher Fe, but lower S and Al contents, than the coarse matrix areas. Our tentative interpretation is that the larger grain size of the coarse areas resulted from the admixing of comminuted chondrule materials, and thus that the initial fraction of nebular fines was higher in the fine matrix regions. Aside from volatiles, the overall composition of Vigarano matrix is similar to that observed in matrix-grid studies of other carbonaceous chondrites: Al, Si, Fe, and Mn have high whole-chondrite-normalized abundance ratios; Ca concentrations are low and highly variable. Because asteroidal alteration effects are present in our sample, it is difficult to resolve nebular signatures in the compositions of the grid areas.

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