¹J. L. MacArthur,¹K. H. Joy,¹R. H. Jones,²T. A. Harvey,³N. V. Almeida
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.14273]
¹Department of Earth and Environmental Sciences, University of Manchester, Manchester, UK
²The Geological Society of London, Burlington House, London, UK
³Planetary Materials Group, Natural History Museum, London, UK
Published by arrangement with John Wiley & Sons

The field of advanced curation is important for existing astromaterials collections, which includes samples returned by space missions, and meteorites and cosmic dust samples that have been recovered from here on Earth. In order to maximize the scientific return of the samples, contamination needs to be minimized at all stages of sample collection, preliminary examination, classification, and curation. Utilizing best practice methods, a detailed acquisition and curation plan was implemented during the UK’s first two expeditions to collect Antarctic meteorites from two new blue icefields, Hutchison Icefields and Outer Recovery Icefields. This article documents the design and execution of the procedures used during the project’s curation and classification processes. It describes two case studies showing the processes applied to the recovered meteorites, and reviews our experiences and lessons learned for the future.

^1,2Kohei Fukuda,^3,4Yuki Hibiya,⁵Craig R. Kastelle,⁴Katsuhiko Suzuki,⁶Tsuyoshi Iizuka,⁷Katsuyuki Yamashita,⁵Thomas E. Helser,¹Noriko T. Kita
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.14276]
¹WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, Wisconsin, USA
²Forefront Research Center, Graduate School of Science, Osaka University, Toyonaka, Osaka, Japan
³Research Center for Advanced Science and Technology, Graduate School of Science, The University of Tokyo, Meguro, Tokyo, Japan
⁴Submarine Resources Research Center, Japan Agency for Marine-Earth Science Technology, Yokosuka, Kanagawa, Japan
⁵National Oceanic and Atmospheric Administration, Seattle, Washington, USA
⁶Department of Earth and Planetary Science, Graduate School of Science, The University of Tokyo, Bunkyo, Tokyo, Japan
⁷Graduate School of Environmental, Life, Natural Science and Technology, Okayama University, Okayama, Okayama, Japan
Published by arrangement with John Wiley & Sons

Understanding the material transport and mixing processes in the Solar protoplanetary disk provides important constraints on the origin of chemical and isotopic diversities of our planets. The limited extent of radial transport and mixing between the inner and outer Solar System has been suggested based on a fundamental isotopic dichotomy between non-carbonaceous (NC) and carbonaceous (CC) meteorite groups. The limited transport and mixing could be further tested by tracing the formation regions of individual meteoritic components, such as Ca-Al-rich inclusions (CAIs) and chondrules. Here, we show further evidence for the outward transport of CAIs and chondrules from the inner and subsequent thermal processing in the outer region of the protoplanetary disk based on the petrography and combined Cr-Ti-O isotope systematics of chondrules from the Vigarano-like (CV) carbonaceous chondrite Allende. One chondrule studied consists of an olivine core that exhibits NC-like Ti and O, but CC-like Cr isotopic signatures, which is enclosed by a pyroxene igneous rim with CC-like O isotope ratios. These observations indicate that the olivine core formed in the inner Solar System. The olivine core then migrated into the outer Solar System and experienced nebular thermal processing that generated the pyroxene igneous rim. The nebular thermal processing would result in Cr isotope exchange between the olivine core and CC-like materials, but secondary alteration effects on the parent body are also responsible for the CC-like Cr isotope signature. By combining previously reported Cr-Ti-O isotope systematics of CV chondrules, we show that some CV chondrules larger than ~1 mm would have formed in the inner Solar System. The accretion of the millimeter-sized, inner Solar System solids onto the CV carbonaceous chondrite parent body would require their very early migration into the outer Solar System within the first 1 million years after the Solar System formation.