¹M. Mijjum,²B. J. Andrews,²T. J. McCoy,²C. M. Corrigan,^1,3M. W. Caffee,¹M. M. Tremblay
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.14309]
¹Department of Earth, Atmospheric and Planetary Sciences, Purdue University, West Lafayette, Indiana, USA
²Department of Mineral Sciences, Smithsonian National Museum of Natural History, Washington, DC, USA
³Department of Physics and Astronomy, Purdue University, West Lafayette, Indiana, USA
Published by arrangement with John Wiley & Sons

Cosmic ray exposure (CRE) ages provide information about the parent bodies and source regions of meteorite classes. Cosmogenic noble gases are often used to quantify exposure time scales ranging from tens of ka to hundreds of Ma. The production rate of cosmogenic noble gases is primarily controlled by a meteorite’s chemical composition. Historically, an average chemical composition for an entire meteorite class or subgroup was used to calculate production rates. At the scale needed for noble gas measurements, however, some meteorites exhibit mineral abundance variabilities that translate into chemical heterogeneities, necessitating subsample-specific production rates. We find that the metal and sulfide content can vary significantly between ~100 and 300 mg subsamples of the same enstatite (E) chondrite, leading to >10% differences in cosmogenic 21Ne production rates between subsamples. We demonstrate an approach to determining subsample-specific production rates using E chondrites. We use electron microprobe analysis and X-ray computed microtomography to quantify the chemical composition and abundances, respectively, of metal, sulfide, and silicate minerals in six E chondrites and calculate subsample-specific production rates of 3He and 21Ne. By applying this method to more E chondrite subsamples alongside noble gas measurements, we may begin to address broader questions, such as whether peaks in the E chondrite CRE age distribution can be attributed to distinct impact events.