Abundance, Major Element Composition and Size of Components and Matrix in CV, CO and Acfer 094 Chondrites
| Autor: | Chelsea Brunner, Hugo Rodriguez, Jon M. Friedrich, K. Konrad, Michael K. Weisberg, Kristin Leftwich, Muzhou Lu, Denton S. Ebel, E. J. Crapster-Pregont, Isabelle Erb |
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| Rok vydání: | 2023 |
| Předmět: |
Earth and Planetary Astrophysics (astro-ph.EP)
Refractory metals Mineralogy Chondrule FOS: Physical sciences Element composition 010502 geochemistry & geophysics 01 natural sciences Geophysics (physics.geo-ph) Physics - Geophysics Geochemistry and Petrology Chondrite 0103 physical sciences Porosity Astrophysics - Instrumentation and Methods for Astrophysics 010303 astronomy & astrophysics Instrumentation and Methods for Astrophysics (astro-ph.IM) Mineral matrix Geology 0105 earth and related environmental sciences Astrophysics - Earth and Planetary Astrophysics |
| DOI: | 10.48550/arxiv.2306.12650 |
| Popis: | The relative abundances and chemical compositions of the macroscopic components or "inclusions" (chondrules and refractory inclusions) and fine-grained mineral matrix in chondritic meteorites provide constraints on astrophysical theories of inclusion formation and chondrite accretion. We present new techniques for analysis of low count per pixel Si, Mg, Ca, Al, Ti and Fe x-ray intensity maps of rock sections, and apply them to large areas of CO and CV chondrites, and the ungrouped Acfer 094 chondrite. For many thousands of manually segmented and type-identified inclusions, we are able to assess, pixel-by-pixel, the major element content of each inclusion. We quantify the total fraction of those elements accounted for by various types of inclusion and matrix. Among CO chondrites, both matrix and inclusion Mg to Si ratios approach the solar (and bulk CO) ratio with increasing petrologic grade, but Si remains enriched in inclusions relative to matrix. The oxidized CV chondrites with higher matrix-inclusion ratios exhibit more severe aqueous alteration (oxidation), and their excess matrix accounts for their higher porosity relative to reduced CV chondrites. Porosity could accommodate an original ice component of matrix as the direct cause of local alteration of oxidized CV chondrites. We confirm that major element abundances among inclusions differ greatly, across a wide range of CO and CV chondrites. These abundances in all cases add up to near-chondritic (solar) bulk abundance ratios in these chondrites, despite wide variations in matrix-inclusion ratios and inclusion sizes: chondrite components are complementary. This "complementarity" provides a robust meteoritic constraint for astrophysical disk models. Comment: 72 pages, 18 figures, 8 tables, with supplementary tables (2) and figues (12). Extended digital supplement available |
| Databáze: | OpenAIRE |
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