Spitzer Fridolin, Kleine Thorsten, Burkhardt Christoph, Hopp Timo, Yokoyama Tetsuya, Abe Yoshinari, Aléon Jérôme, O'D Alexander Conel M, Amari Sachiko, Amelin Yuri, Bajo Ken-Ichi, Bizzarro Martin, Bouvier Audrey, Carlson Richard W, Chaussidon Marc, Choi Byeon-Gak, Dauphas Nicolas, Davis Andrew M, Di Rocco Tommaso, Fujiya Wataru, Fukai Ryota, Gautam Ikshu, Haba Makiko K, Hibiya Yuki, Hidaka Hiroshi, Homma Hisashi, Hoppe Peter, Huss Gary R, Ichida Kiyohiro, Iizuka Tsuyoshi, Ireland Trevor R, Ishikawa Akira, Itoh Shoichi, Kawasaki Noriyuki, Kita Noriko T, Kitajima Kouki, Komatani Shintaro, Krot Alexander N, Liu Ming-Chang, Masuda Yuki, Morita Mayu, Moynier Fréderic, Motomura Kazuko, Nakai Izumi, Nagashima Kazuhide, Nguyen Ann, Nittler Larry, Onose Morihiko, Pack Andreas, Park Changkun, Piani Laurette, Qin Liping, Russell Sara S, Sakamoto Naoya, Schönbächler Maria, Tafla Lauren, Tang Haolan, Terada Kentaro, Terada Yasuko, Usui Tomohiro, Wada Sohei, Wadhwa Meenakshi, Walker Richard J, Yamashita Katsuyuki, Yin Qing-Zhu, Yoneda Shigekazu, Young Edward D, Yui Hiroharu, Zhang Ai-Cheng, Nakamura Tomoki, Naraoka Hiroshi, Noguchi Takaaki, Okazaki Ryuji, Sakamoto Kanako, Yabuta Hikaru, Abe Masanao, Miyazaki Akiko, Nakato Aiko, Nishimura Masahiro, Okada Tatsuaki, Yada Toru, Yogata Kasumi, Nakazawa Satoru, Saiki Takanao, Tanaka Satoshi, Terui Fuyuto, Tsuda Yuichi, Watanabe Sei-Ichiro, Yoshikawa Makoto, Tachibana Shogo, Yurimoto Hisayoshi
Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany.
Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan.
Sci Adv. 2024 Sep 27;10(39):eadp2426. doi: 10.1126/sciadv.adp2426.
The isotopic compositions of samples returned from Cb-type asteroid Ryugu and Ivuna-type (CI) chondrites are distinct from other carbonaceous chondrites, which has led to the suggestion that Ryugu/CI chondrites formed in a different region of the accretion disk, possibly around the orbits of Uranus and Neptune. We show that, like for Fe, Ryugu and CI chondrites also have indistinguishable Ni isotope anomalies, which differ from those of other carbonaceous chondrites. We propose that this unique Fe and Ni isotopic composition reflects different accretion efficiencies of small FeNi metal grains among the carbonaceous chondrite parent bodies. The CI chondrites incorporated these grains more efficiently, possibly because they formed at the end of the disk's lifetime, when planetesimal formation was also triggered by photoevaporation of the disk. Isotopic variations among carbonaceous chondrites may thus reflect fractionation of distinct dust components from a common reservoir, implying CI chondrites/Ryugu may have formed in the same region of the accretion disk as other carbonaceous chondrites.
从C型小行星龙宫返回的样本以及伊武纳型（CI）球粒陨石的同位素组成与其他碳质球粒陨石不同，这使人认为龙宫/CI球粒陨石是在吸积盘的不同区域形成的，可能是在天王星和海王星的轨道附近。我们发现，与铁一样，龙宫和CI球粒陨石也有难以区分的镍同位素异常，这与其他碳质球粒陨石不同。我们提出，这种独特的铁和镍同位素组成反映了碳质球粒陨石母体中小的铁镍金属颗粒的不同吸积效率。CI球粒陨石更有效地吸收了这些颗粒，可能是因为它们形成于吸积盘寿命的末期，当时行星形成也由吸积盘的光致蒸发引发。因此，碳质球粒陨石之间的同位素变化可能反映了来自共同储库的不同尘埃成分的分馏，这意味着CI球粒陨石/龙宫可能与其他碳质球粒陨石在吸积盘的同一区域形成。
Zotero 插件
