¹Juan A. Sanchez,²Vishnu Reddy,³Audrey Thirouin,⁴Edward L. Wright,^5,6Tyler R. Linder,²Theodore Kareta,²Benjamin Sharkey
The Astrophysical Journal Letters 881, L6 Link to Article [DOI
https://doi.org/10.3847/2041-8213/ab31ac]
¹Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA
²Lunar and Planetary Laboratory, University of Arizona, 1629 East University Blvd, Tucson, AZ 85721-0092, USA
³Lowell Observatory, 1400 West Mars Hill Road, Flagstaff, AZ 86001, USA
⁴Division of Astronomy and Astrophysics, University of California Los Angeles, 430 Portola Plaza, Box 951547, Los Angeles, CA 90095-1547, USA
⁵Astronomical Research Institute, 1015 Cr 1300N, Sullivan, IL 61951, USA
⁶University of North Dakota, Clifford Hall Room 512, 4149 University Avenue Stop 9008, Grand Forks, ND 58202, USA

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^1,2Aki Takigawa,³Tae-Hee Kim,⁴Yohei Igami,²Tatsuki Umemoto,^2,7Akira Tsuchiyama,⁵Chiyoe Koike,²Junya Matsuno,⁶Takayuki Watanabe
The Astrophysical Journal Letters, 878, L7 Link to Article [DOI
https://doi.org/10.3847/2041-8213/ab1f80]
¹The Hakubi Center for Advanced Research, Kyoto University, Kitashirakawa-Oiwakecho, Sakyo, Kyoto 606-8502, Japan
²Division of Earth and Planetary Sciences, Kyoto University, Kitashirakawa-Oiwakecho, Sakyo, Kyoto 606-8502, Japan
³Institute for Nuclear Science and Technology, Department of Nuclear and Energy Engineering, Jeju National University, 102 Jejudaehak-ro, Jeju-si, Jeju, 63243, Republic of Korea
⁴Institute of Materials and Systems for Sustainability, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8603, Japan
⁵Department of Physics, Ritsumeikan University, 1-1-1 Nojihigashi, Kusatsu-shi, Shiga 525-8577, Japan
⁶Department of Chemical Engineering, Kyushu University, Fukuoka 819-0395, Japan
⁷Present addresses: Research Organization of Science and Technology, Ritsumeikan University, 1-1-1 Nojihigashi, Kusatsu, Shiga 525-8577, Japan, and Guangzhou Institute of Geochemistry, Chinese Academy of Sciences 511 Kehua Street, Wushan, Tianhe District, Guangzhou, 510640, China.

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

¹Ioannis Kouvatsis,²Beda A. Hofmann
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13410]
¹Institute of Geological Sciences, University of Bern, Baltzerstrasse 1 + 3, 3012 Bern, Switzerland
²Natural History Museum Bern, Bernastrasse 15, 3005 Bern, Switzerland
Published by arrangement with John Wiley & Sons

¹Jeremy B. Tatum
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13403]
¹Department of Physics and Astronomy, University of Victoria, PO Box 1700, STN CSC, Victoria, British Columbia, Canada, V8P 2Y2
Published by arrangement with John Wiley & Sons

A table is provided to determine the angles within the Widmanstätten pattern as a function of orientation of the slice, and methods are provided to solve the inverse problem, namely to determine the orientation of the slice from measurements of the Widmanstätten pattern.

¹M. R. Lee,¹B. E. Cohen,²A. J. King
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13405]
¹School of Geographical and Earth Sciences, University of Glasgow, Gregory Building, Lilybank Gardens, Glasgow, G12 8QQ UK
²Department of Earth Science, Natural History Museum (London), Cromwell Rd, London, SW7 5BD UK
Published by arrangement with John Wiley & Sons

Meteorite Hills (MET) 01075 is unique among the CM carbonaceous chondrites in containing the feldspathoid mineral sodalite, and hence it may provide valuable evidence for a nebular or parent body process that has not been previously recorded by this meteorite group. MET 01075 is composed of aqueously altered chondrules and calcium‐ and aluminum‐rich inclusions (CAIs) in a matrix that is predominantly made of serpentine‐ and tochilinite‐rich particles. The chondrules have been impact flattened and define a foliation petrofabric. Sodalite occurs in a 0.6 mm size CAI that also contains spinel, perovskite, and diopside together with Fe‐rich phyllosilicate and calcite. By analogy with feldspathoid‐bearing CAIs in the CV and CO carbonaceous chondrites, the sodalite is interpreted to have formed by replacement of melilite or anorthite during alkali‐halogen metasomatism in a parent body environment. While it is possible that the CAI was metasomatized in a precursor parent body, then excavated and incorporated into the MET 01075 parent body, in situ metasomatism is the favored model. The brief episode of relatively high temperature water–rock interaction was driven by radiogenic or impact heating, and most of the evidence for metasomatism was erased by subsequent lower temperature aqueous alteration. MET 01075 is very unusual in sampling a CM parent body region that underwent early alkali‐halogen metasomatism and has retained one of its products.