Denton S. EBEL^1,2,3, Marina E. GEMMA^1,4, Samuel P. ALPERT^1,3, Jasmine BAYRON⁵, Ana H. LOBO⁶, and Michael K. WEISBERG^1,3,7
Meteoritics & Planetary Science (in Press)
Link to Article [https://doi.org/10.1111/maps.14191]
¹Department of Earth and Planetary Sciences, American Museum of Natural History, New York, New York, USA
²Lamont-Doherty Earth Observatory, Columbia University, Palisades, New York, USA
³Department of Earth and Environmental Sciences, Graduate Center of the City University of New York, New York,
New York, USA
⁴Department of Geosciences, Stony Brook University, Stony Brook, New York, USA
⁵Department of Geography, Hunter College, City University of New York, New York, New York, USA
⁶Department Physics & Astronomy, University of California Irvine, Irvine, California, USA
⁷Department of Physical Sciences, Kingsborough College, City University of New York, Brooklyn, New York, USA
Published by arrangement with John Wiley & Sons

Abundances, apparent sizes, and individual chemical compositions of chondrules, refractory inclusions, other objects, and surrounding matrix have been determined for Semarkona (LL3.00) and Renazzo (CR2) using consistent methods and criteria on X-ray element intensity maps. These represent the non-carbonaceous (NC, Semarkona) and carbonaceous chondrite (CC, Renazzo) superclans of chondrite types. We compare object and matrix abundances with similar data for CM, CO, K, and CV chondrites. We assess, pixel-by-pixel, the major element abundance in each object and in the entire matrix. We determine the abundance of “metallic chondrules” in LL chondrites. Chondrules with high Mg/Si and low Fe/Si and matrix carrying opposing ratios complement each other to make whole rocks with near-solar major element ratios in Renazzo. Similar Mg/Si and Fe/Si chondrule–matrix relationships are seen in Semarkona, which is within 11% of solar Mg/Si but significantly Fe-depleted. These results provide a robust constraint in support of single-reservoir models for chondrule formation and accretion, ruling out whole classes of astrophysical models and constraining processes of chondrite component formation and accretion into chondrite parent bodies.