1
|
Morita M, Yui H, Urashima SH, Onose M, Komatani S, Nakai I, Abe Y, Terada Y, Homma H, Motomura K, Ichida K, Yokoyama T, Nagashima K, Aléon J, O’D. Alexander CM, Amari S, Amelin Y, Bajo KI, Bizzarro M, Bouvier A, Carlson RW, Chaussidon M, Choi BG, Dauphas N, Davis AM, Fujiya W, Fukai R, Gautam I, Haba MK, Hibiya Y, Hidaka H, Hoppe P, Huss GR, Iizuka T, Ireland TR, Ishikawa A, Itoh S, Kawasaki N, Kita NT, Kitajima K, Kleine T, Krot S, Liu MC, Masuda Y, Moynier F, Nguyen A, Nittler L, Pack A, Park C, Piani L, Qin L, Rocco TD, Russell SS, Sakamoto N, Schönbächler M, Tafla L, Tang H, Terada K, Usui T, Wada S, Wadhwa M, Walker RJ, Yamashita K, Yin QZ, Yoneda S, Young ED, Zhang AC, Nakamura T, Naraoka H, Noguchi T, Okazaki R, Sakamoto K, Yabuta H, Abe M, Miyazaki A, Nakato A, Nishimura M, Okada T, Yada T, Yogata K, Nakazawa S, Saiki T, Tanaka S, Terui F, Tsuda Y, Watanabe SI, Yoshikawa M, Tachibana S, Yurimoto H. Analysis of Cation Composition in Dolomites on the Intact Particles Sampled from Asteroid Ryugu. Anal Chem 2024; 96:170-178. [PMID: 38155534 PMCID: PMC10783172 DOI: 10.1021/acs.analchem.3c03463] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/03/2023] [Revised: 11/28/2023] [Accepted: 11/28/2023] [Indexed: 12/30/2023]
Abstract
Characterization of the elemental distribution of samples with rough surfaces has been strongly desired for the analysis of various natural and artificial materials. Particularly for pristine and rare analytes with micrometer sizes embedded on specimen surfaces, non-invasive and matrix effect-free analysis is required without surface polishing treatment. To satisfy these requirements, we proposed a new method employing the sequential combination of two imaging modalities, i.e., microenergy-dispersive X-ray fluorescence (micro-XRF) and Raman micro-spectroscopy. The applicability of the developed method is tested by the quantitative analysis of cation composition in micrometer-sized carbonate grains on the surfaces of intact particles sampled directly from the asteroid Ryugu. The first step of micro-XRF imaging enabled a quick search for the sparsely scattered and micrometer-sized carbonates by the codistributions of Ca2+ and Mn2+ on the Mg2+- and Fe2+-rich phyllosilicate matrix. The following step of Raman micro-spectroscopy probed the carbonate grains and analyzed their cation composition (Ca2+, Mg2+, and Fe2+ + Mn2+) in a matrix effect-free manner via the systematic Raman shifts of the lattice modes. The carbonates were basically assigned to ferroan dolomite bearing a considerable amount of Fe2+ + Mn2+ at around 10 atom %. These results are in good accordance with the assignments reported by scanning electron microscopy-energy-dispersive X-ray spectroscopy, where the thin-sectioned and surface-polished Ryugu particles were applicable. The proposed method requires neither sectioning nor surface polishing; hence, it can be applied to the remote sensing apparatus on spacecrafts and planetary rovers. Furthermore, the non-invasive and matrix effect-free characterization will provide a reliable analytical tool for quantitative analysis of the elemental distribution on the samples with surface roughness and chemical heterogeneity at a micrometer scale, such as art paintings, traditional crafts with decorated shapes, as well as sands and rocks with complex morphologies in nature.
Collapse
Affiliation(s)
- Mayu Morita
- Analytical
Technology Division, Horiba Techno Service
Co., Ltd., Kyoto 601-8125, Japan
| | - Hiroharu Yui
- Department
of Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Shu-hei Urashima
- Department
of Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Morihiko Onose
- Analytical
Technology Division, Horiba Techno Service
Co., Ltd., Kyoto 601-8125, Japan
| | - Shintaro Komatani
- Analytical
Technology Division, Horiba Techno Service
Co., Ltd., Kyoto 601-8125, Japan
| | - Izumi Nakai
- Department
of Applied Chemistry, Tokyo University of
Science, Tokyo 162-8601, Japan
| | - Yoshinari Abe
- Graduate
School of Engineering Materials Science and Engineering, Tokyo Denki University, Tokyo 120-8551, Japan
| | - Yasuko Terada
- Spectroscopy
and Imaging Division, Japan Synchrotron
Radiation Research Institute, Hyogo 679-5198, Japan
| | - Hisashi Homma
- Osaka Application
Laboratory, Rigaku Corporation, Osaka 569-1146, Japan
| | - Kazuko Motomura
- Thermal
Analysis Division, Rigaku Corporation, Tokyo 196-8666, Japan
| | - Kiyohiro Ichida
- Analytical
Technology Division, Horiba Techno Service
Co., Ltd., Kyoto 601-8125, Japan
| | - Tetsuya Yokoyama
- Department
of Earth and Planetary Sciences, Tokyo Institute
of Technology, Tokyo 152-8551, Japan
| | - Kazuhide Nagashima
- Hawai‘i
Institute of Geophysics and Planetology, University of Hawai‘i at Ma̅noa, Honolulu, Hawaii 96822, United States
| | - Jérôme Aléon
- Institut
de Minéralogie, de Physique des Matériaux et de Cosmochimie,
Sorbonne Université, Museum National d’Histoire Naturelle,
Centre National de la Recherche Scientifique Unité Mixte de
Recherche 7590, Institut de recherche pour
le développement, Paris 75005, France
| | - Conel M. O’D. Alexander
- Earth and Planets Laboratory, Carnegie
Institution for Science, Washington, District of Columbia 20015, United States
| | - Sachiko Amari
- McDonnell
Center for the Space Sciences and Physics Department, Washington University, St. Louis, Missouri 63130, United States
- Geochemical
Research Center, The University
of Tokyo, Tokyo 113-0033, Japan
| | - Yuri Amelin
- Guangzhou Institute of Geochemistry, Chinese
Academy of Sciences, Guangzhou, GD 510640, China
| | - Ken-ichi Bajo
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Martin Bizzarro
- Centre
for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen K 1350, Denmark
| | - Audrey Bouvier
- Bayerisches Geoinstitut, Universität
Bayreuth, Bayreuth 95447, Germany
| | - Richard W. Carlson
- Earth and Planets Laboratory, Carnegie
Institution for Science, Washington, District of Columbia 20015, United States
| | - Marc Chaussidon
- Université Paris Cité, Institut de physique
du globe
de Paris, Centre National de la Recherche
Scientifique, Paris 75005, France
| | - Byeon-Gak Choi
- Department of Earth Science Education, Seoul National University, Seoul 08826, Republic of Korea
| | - Nicolas Dauphas
- Department of the
Geophysical Sciences and Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637, United States
| | - Andrew M. Davis
- Department of the
Geophysical Sciences and Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637, United States
| | - Wataru Fujiya
- Faculty of Science, Ibaraki
University, Mito 310-8512, Japan
| | - Ryota Fukai
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Ikshu Gautam
- Department
of Earth and Planetary Sciences, Tokyo Institute
of Technology, Tokyo 152-8551, Japan
| | - Makiko K. Haba
- Department
of Earth and Planetary Sciences, Tokyo Institute
of Technology, Tokyo 152-8551, Japan
| | - Yuki Hibiya
- Department of
General Systems Studies, University of Tokyo, Tokyo 153-0041, Japan
| | - Hiroshi Hidaka
- Department
of Earth and Planetary Sciences, Nagoya
University, Nagoya 464-8601, Japan
| | - Peter Hoppe
- Max Planck Institute for Chemistry, Mainz 55128, Germany
| | - Gary R. Huss
- Hawai‘i
Institute of Geophysics and Planetology, University of Hawai‘i at Ma̅noa, Honolulu, Hawaii 96822, United States
| | - Tsuyoshi Iizuka
- Department
of Earth and Planetary Science, University
of Tokyo, Tokyo 113-0033, Japan
| | - Trevor R. Ireland
- School of Earth and Environmental Sciences, University of Queensland, St Lucia, QLD 4072, Australia
| | - Akira Ishikawa
- Department
of Earth and Planetary Sciences, Tokyo Institute
of Technology, Tokyo 152-8551, Japan
| | - Shoichi Itoh
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Noriyuki Kawasaki
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Noriko T. Kita
- Department of Geoscience, University
of Wisconsin—Madison, Madison, Wisconsin 53706, United States
| | - Kouki Kitajima
- Department of Geoscience, University
of Wisconsin—Madison, Madison, Wisconsin 53706, United States
| | - Thorsten Kleine
- Max Planck Institute for Solar System Research, Göttingen 37077, Germany
| | - Sasha Krot
- Hawai‘i
Institute of Geophysics and Planetology, University of Hawai‘i at Ma̅noa, Honolulu, Hawaii 96822, United States
| | - Ming-Chang Liu
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, California 90095, United States
| | - Yuki Masuda
- Department
of Earth and Planetary Sciences, Tokyo Institute
of Technology, Tokyo 152-8551, Japan
| | - Frédéric Moynier
- Université Paris Cité, Institut de physique
du globe
de Paris, Centre National de la Recherche
Scientifique, Paris 75005, France
| | - Ann Nguyen
- Astromaterials Research and Exploration Science Division, National Aeronautics and Space Administration Johnson
Space Center, Johnson Space Center, Houston, Texas 77058, United States
| | - Larry Nittler
- Earth and Planets Laboratory, Carnegie
Institution for Science, Washington, District of Columbia 20015, United States
| | - Andreas Pack
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Changkun Park
- Division of Earth-System Sciences, Korea
Polar Research Institute, Incheon 21990, Korea
| | - Laurette Piani
- Centre de Recherches Pétrographiques
et Géochimiques, Centre National
de la Recherche Scientifique-Université
de Lorraine, Nancy 54500, France
| | - Liping Qin
- School
of Earth and Space Sciences, University
of Science and Technology of China, Anhui 230026, China
| | - Tommaso Di Rocco
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Sara S. Russell
- Department of Earth Sciences, Natural History Museum, London SW7 5BD, U.K.
| | - Naoya Sakamoto
- Isotope Imaging Laboratory, Hokkaido University, Sapporo 001-0021, Japan
| | - Maria Schönbächler
- Institute for Geochemistry and Petrology,
Department
of Earth Sciences, ETH Zurich, Zurich 8092, Switzerland
| | - Lauren Tafla
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, California 90095, United States
| | - Haolan Tang
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, California 90095, United States
| | - Kentaro Terada
- Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan
| | - Tomohiro Usui
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Sohei Wada
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, Arizona 85281, United States
| | - Richard J. Walker
- Department of Geology, University of Maryland, College
Park, Maryland 20742, United States
| | - Katsuyuki Yamashita
- Graduate School of Natural Science and Technology, Okayama University, Okayama 700-8530, Japan
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California, Davis, California 95616, United States
| | - Shigekazu Yoneda
- Department of Science and Engineering, National Museum of Nature and Science, Tsukuba 305-0005, Japan
| | - Edward D. Young
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, California 90095, United States
| | - Ai-Cheng Zhang
- School
of Earth Sciences and Engineering, Nanjing
University, Nanjing 210023, China
| | - Tomoki Nakamura
- Department of Earth Science, Tohoku University, Sendai 980-8578, Japan
| | - Hiroshi Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Takaaki Noguchi
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Ryuji Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Kanako Sakamoto
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Hikaru Yabuta
- Earth and Planetary Systems Science Program, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - Masanao Abe
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Akiko Miyazaki
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Aiko Nakato
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Masahiro Nishimura
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Tatsuaki Okada
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Toru Yada
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Kasumi Yogata
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Satoru Nakazawa
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Takanao Saiki
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Satoshi Tanaka
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Fuyuto Terui
- Graduate School of Engineering, Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | - Yuichi Tsuda
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Sei-ichiro Watanabe
- Department
of Earth and Planetary Sciences, Nagoya
University, Nagoya 464-8601, Japan
| | - Makoto Yoshikawa
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Shogo Tachibana
- UTokyo Organization for Planetary and Space
Science (UTOPS), University of Tokyo, Tokyo 113-0033, Japan
| | - Hisayoshi Yurimoto
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| |
Collapse
|
2
|
Yokoyama T, Wadhwa M, Iizuka T, Rai V, Gautam I, Hibiya Y, Masuda Y, Haba MK, Fukai R, Hines R, Phelan N, Abe Y, Aléon J, Alexander CM, Amari S, Amelin Y, Bajo KI, Bizzarro M, Bouvier A, Carlson RW, Chaussidon M, Choi BG, Dauphas N, Davis AM, Di Rocco T, Fujiya W, Hidaka H, Homma H, Hoppe P, Huss GR, Ichida K, Ireland T, Ishikawa A, Itoh S, Kawasaki N, Kita NT, Kitajima K, Kleine T, Komatani S, Krot AN, Liu MC, McKeegan KD, Morita M, Motomura K, Moynier F, Nakai I, Nagashima K, Nguyen A, Nittler L, Onose M, Pack A, Park C, Piani L, Qin L, Russell S, Sakamoto N, Schönbächler M, Tafla L, Tang H, Terada K, Terada Y, Usui T, Wada S, Walker RJ, Yamashita K, Yin QZ, Yoneda S, Young ED, Yui H, Zhang AC, Nakamura T, Naraoka H, Noguchi T, Okazaki R, Sakamoto K, Yabuta H, Abe M, Miyazaki A, Nakato A, Nishimura M, Okada T, Yada T, Yogata K, Nakazawa S, Saiki T, Tanaka S, Terui F, Tsuda Y, Watanabe SI, Yoshikawa M, Tachibana S, Yurimoto H. Water circulation in Ryugu asteroid affected the distribution of nucleosynthetic isotope anomalies in returned sample. Sci Adv 2023; 9:eadi7048. [PMID: 37939187 PMCID: PMC10631728 DOI: 10.1126/sciadv.adi7048] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/13/2023] [Accepted: 10/05/2023] [Indexed: 11/10/2023]
Abstract
Studies of material returned from Cb asteroid Ryugu have revealed considerable mineralogical and chemical heterogeneity, stemming primarily from brecciation and aqueous alteration. Isotopic anomalies could have also been affected by delivery of exogenous clasts and aqueous mobilization of soluble elements. Here, we show that isotopic anomalies for mildly soluble Cr are highly variable in Ryugu and CI chondrites, whereas those of Ti are relatively uniform. This variation in Cr isotope ratios is most likely due to physicochemical fractionation between 54Cr-rich presolar nanoparticles and Cr-bearing secondary minerals at the millimeter-scale in the bulk samples, likely due to extensive aqueous alteration in their parent bodies that occurred [Formula: see text] after Solar System birth. In contrast, Ti isotopes were marginally affected by this process. Our results show that isotopic heterogeneities in asteroids are not all nebular or accretionary in nature but can also reflect element redistribution by water.
Collapse
Affiliation(s)
- Tetsuya Yokoyama
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Tsuyoshi Iizuka
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Vinai Rai
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Ikshu Gautam
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Yuki Hibiya
- Research Center for Advanced Science and Technology, The University of Tokyo, Tokyo 153-0041, Japan
| | - Yuki Masuda
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Makiko K. Haba
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Ryota Fukai
- ISAS/JSEC, JAXA, Sagamihara, 252-5210, Japan
| | - Rebekah Hines
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Nicole Phelan
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Yoshinari Abe
- Graduate School of Engineering, Tokyo Denki University, Tokyo 120-8551, Japan
| | - Jérôme Aléon
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Sorbonne Université, Museum National d'Histoire Naturelle, CNRS UMR 7590, IRD, 75005 Paris, France
| | | | - Sachiko Amari
- McDonnell Center for the Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, USA
- Geochemical Research Center, The University of Tokyo, Tokyo 113-0033, Japan
| | - Yuri Amelin
- Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, GD 510640, China
| | - Ken-ichi Bajo
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Martin Bizzarro
- Centre for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Copenhagen, K 1350, Denmark
| | - Audrey Bouvier
- Bayerisches Geoinstitut, Universität Bayreuth, Bayreuth, 95447, Germany
| | - Richard W. Carlson
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, 20015, USA
| | - Marc Chaussidon
- Université Paris Cité, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Byeon-Gak Choi
- Department of Earth Science Education, Seoul National University, Seoul 08826, Republic of Korea
| | - Nicolas Dauphas
- Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - Andrew M. Davis
- Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - Tommaso Di Rocco
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen, D-37077, Germany
| | - Wataru Fujiya
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Hiroshi Hidaka
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Hisashi Homma
- Osaka Application Laboratory, SBUWDX, Rigaku Corporation, Osaka 569-1146, Japan
| | - Peter Hoppe
- Max Planck Institute for Chemistry, Mainz, 55128, Germany
| | - Gary R. Huss
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Kiyohiro Ichida
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Trevor Ireland
- School of Earth and Environmental Sciences, The University of Queensland, St. Lucia, QLD 4072, Australia
| | - Akira Ishikawa
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Shoichi Itoh
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Noriyuki Kawasaki
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Noriko T. Kita
- Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Koki Kitajima
- Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Thorsten Kleine
- Max Planck Institute for Solar System Research, 37077, Göttingen, Germany
| | - Shintaro Komatani
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Alexander N. Krot
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Ming-Chang Liu
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Kevin D. McKeegan
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Mayu Morita
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | | | - Frédéric Moynier
- Université Paris Cité, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Izumi Nakai
- Department of Applied Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Kazuhide Nagashima
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Ann Nguyen
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
| | - Larry Nittler
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, 20015, USA
| | - Morihiko Onose
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Andreas Pack
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen, D-37077, Germany
| | - Changkun Park
- Earth-System Sciences, Korea Polar Research Institute, Incheon 21990, Korea
| | - Laurette Piani
- Centre de Recherches Pétrographiques et Géochimiques, CNRS - Université de Lorraine, 54500 Nancy, France
| | - Liping Qin
- CAS Key Laboratory of Crust-Mantle Materials and Environments, University of Science and Technology of China, School of Earth and Space Sciences, Anhui 230026, China
| | - Sara Russell
- Department of Earth Sciences, Natural History Museum, London, SW7 5BD, UK
| | - Naoya Sakamoto
- Isotope Imaging Laboratory, Creative Research Institution, Hokkaido University, Sapporo 001-0021, Japan
| | - Maria Schönbächler
- Institute for Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, 8092 Zurich, Switzerland
| | - Lauren Tafla
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Haolan Tang
- CAS Key Laboratory of Crust-Mantle Materials and Environments, University of Science and Technology of China, School of Earth and Space Sciences, Anhui 230026, China
| | - Kentaro Terada
- Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan
| | - Yasuko Terada
- Spectroscopy and Imaging, Japan Synchrotron Radiation Research Institute, Hyogo 679-5198, Japan
| | | | - Sohei Wada
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Richard J. Walker
- Department of Geology, University of Maryland, College Park, MD 20742, USA
| | - Katsuyuki Yamashita
- Graduate School of Natural Science and Technology, Okayama University, Okayama 700-8530, Japan
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California, Davis, CA 95616, USA
| | - Shigekazu Yoneda
- Department of Science and Engineering, National Museum of Nature and Science, Tsukuba 305-0005, Japan
| | - Edward D. Young
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Hiroharu Yui
- Department of Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Ai-Cheng Zhang
- School of Earth Sciences and Engineering, Nanjing University, Nanjing 210023, China
| | - Tomoki Nakamura
- Department of Earth Science, Tohoku University, Sendai 980-8578, Japan
| | - Hiroshi Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Takaaki Noguchi
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Ryuji Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | | | - Hikaru Yabuta
- Earth and Planetary Systems Science Program, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - Masanao Abe
- ISAS/JSEC, JAXA, Sagamihara, 252-5210, Japan
| | | | - Aiko Nakato
- ISAS/JSEC, JAXA, Sagamihara, 252-5210, Japan
| | | | | | - Toru Yada
- ISAS/JSEC, JAXA, Sagamihara, 252-5210, Japan
| | | | | | | | | | - Fuyuto Terui
- Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | | | - Sei-ichiro Watanabe
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | | | - Shogo Tachibana
- UTokyo Organization for Planetary and Space Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Hisayoshi Yurimoto
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| |
Collapse
|
3
|
Deng Z, Schiller M, Jackson MG, Millet MA, Pan L, Nikolajsen K, Saji NS, Huang D, Bizzarro M. Earth's evolving geodynamic regime recorded by titanium isotopes. Nature 2023; 621:100-104. [PMID: 37495699 PMCID: PMC10482698 DOI: 10.1038/s41586-023-06304-0] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/24/2022] [Accepted: 06/09/2023] [Indexed: 07/28/2023]
Abstract
Earth's mantle has a two-layered structure, with the upper and lower mantle domains separated by a seismic discontinuity at about 660 km (refs. 1,2). The extent of mass transfer between these mantle domains throughout Earth's history is, however, poorly understood. Continental crust extraction results in Ti-stable isotopic fractionation, producing isotopically light melting residues3-7. Mantle recycling of these components can impart Ti isotope variability that is trackable in deep time. We report ultrahigh-precision 49Ti/47Ti ratios for chondrites, ancient terrestrial mantle-derived lavas ranging from 3.8 to 2.0 billion years ago (Ga) and modern ocean island basalts (OIBs). Our new Ti bulk silicate Earth (BSE) estimate based on chondrites is 0.052 ± 0.006‰ heavier than the modern upper mantle sampled by normal mid-ocean ridge basalts (N-MORBs). The 49Ti/47Ti ratio of Earth's upper mantle was chondritic before 3.5 Ga and evolved to a N-MORB-like composition between approximately 3.5 and 2.7 Ga, establishing that more continental crust was extracted during this epoch. The +0.052 ± 0.006‰ offset between BSE and N-MORBs requires that <30% of Earth's mantle equilibrated with recycled crustal material, implying limited mass exchange between the upper and lower mantle and, therefore, preservation of a primordial lower-mantle reservoir for most of Earth's geologic history. Modern OIBs record variable 49Ti/47Ti ratios ranging from chondritic to N-MORBs compositions, indicating continuing disruption of Earth's primordial mantle. Thus, modern-style plate tectonics with high mass transfer between the upper and lower mantle only represents a recent feature of Earth's history.
Collapse
Affiliation(s)
- Zhengbin Deng
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark.
- Deep Space Exploration Laboratory/CAS Key Laboratory of Crust-Mantle Materials and Environments, School of Earth and Space Sciences, University of Science and Technology of China, Hefei, China.
| | - Martin Schiller
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Matthew G Jackson
- Department of Earth Science, University of California, Santa Barbara, Santa Barbara, CA, USA
| | - Marc-Alban Millet
- School of Earth and Environmental Sciences, Cardiff University, Cardiff, UK
| | - Lu Pan
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
- Deep Space Exploration Laboratory/Laboratory of Seismology and Physics of Earth's Interior, School of Earth and Space Sciences, University of Science and Technology of China, Hefei, China
| | - Katrine Nikolajsen
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Nikitha S Saji
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Dongyang Huang
- Institute of Geochemistry and Petrology, ETH Zürich, Zürich, Switzerland
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
- Institut de Physique du Globe de Paris, Université Paris Cité, Paris, France
| |
Collapse
|
4
|
Nguyen AN, Mane P, Keller LP, Piani L, Abe Y, Aléon J, Alexander CMO, Amari S, Amelin Y, Bajo KI, Bizzarro M, Bouvier A, Carlson RW, Chaussidon M, Choi BG, Dauphas N, Davis AM, Di Rocco T, Fujiya W, Fukai R, Gautam I, Haba MK, Hibiya Y, Hidaka H, Homma H, Hoppe P, Huss GR, Ichida K, Iizuka T, Ireland TR, Ishikawa A, Itoh S, Kawasaki N, Kita NT, Kitajima K, Kleine T, Komatani S, Krot AN, Liu MC, Masuda Y, McKeegan KD, Morita M, Motomura K, Moynier F, Nakai I, Nagashima K, Nesvorný D, Nittler L, Onose M, Pack A, Park C, Qin L, Russell SS, Sakamoto N, Schönbächler M, Tafla L, Tang H, Terada K, Terada Y, Usui T, Wada S, Wadhwa M, Walker RJ, Yamashita K, Yin QZ, Yokoyama T, Yoneda S, Young ED, Yui H, Zhang AC, Nakamura T, Naraoka H, Noguchi T, Okazaki R, Sakamoto K, Yabuta H, Abe M, Miyazaki A, Nakato A, Nishimura M, Okada T, Yada T, Yogata K, Nakazawa S, Saiki T, Tanaka S, Terui F, Tsuda Y, Watanabe SI, Yoshikawa M, Tachibana S, Yurimoto H. Abundant presolar grains and primordial organics preserved in carbon-rich exogenous clasts in asteroid Ryugu. Sci Adv 2023; 9:eadh1003. [PMID: 37450600 PMCID: PMC10348677 DOI: 10.1126/sciadv.adh1003] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 02/09/2023] [Accepted: 06/09/2023] [Indexed: 07/18/2023]
Abstract
Preliminary analyses of asteroid Ryugu samples show kinship to aqueously altered CI (Ivuna-type) chondrites, suggesting similar origins. We report identification of C-rich, particularly primitive clasts in Ryugu samples that contain preserved presolar silicate grains and exceptional abundances of presolar SiC and isotopically anomalous organic matter. The high presolar silicate abundance (104 ppm) indicates that the clast escaped extensive alteration. The 5 to 10 times higher abundances of presolar SiC (~235 ppm), N-rich organic matter, organics with N isotopic anomalies (1.2%), and organics with C isotopic anomalies (0.2%) in the primitive clasts compared to bulk Ryugu suggest that the clasts formed in a unique part of the protoplanetary disk enriched in presolar materials. These clasts likely represent previously unsampled outer solar system material that accreted onto Ryugu after aqueous alteration ceased, consistent with Ryugu's rubble pile origin.
Collapse
Affiliation(s)
- Ann. N. Nguyen
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
| | - Prajkta Mane
- Universities Space Research Association, Lunar and Planetary Institute, Houston, TX 77058, USA
| | - Lindsay P. Keller
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
| | - Laurette Piani
- Centre de Recherches Pétrographiques et Géochimiques, CNRS - Université de Lorraine, Nancy 54500, France
| | - Yoshinari Abe
- Graduate School of Engineering Materials Science and Engineering, Tokyo Denki University, Tokyo 120-8551, Japan
| | - Jérôme Aléon
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Sorbonne Université, Museum National d'Histoire Naturelle, CNRS UMR 7590, IRD, Paris 75005, France
| | | | - Sachiko Amari
- McDonnell Center for the Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, USA
- Geochemical Research Center, The University of Tokyo, Tokyo 113-0033, Japan
| | - Yuri Amelin
- Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, GD 510640, China
| | - Ken-ichi Bajo
- Department of Natural History Sciences, IIL, Hokkaido University, Sapporo 001-0021, Japan
| | - Martin Bizzarro
- Centre for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Copenhagen K 1350, Denmark
| | - Audrey Bouvier
- Bayerisches Geoinstitut, Universität Bayreuth, Bayreuth 95447, Germany
| | - Richard W. Carlson
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Marc Chaussidon
- Université Paris Cités, Institut de physique du globe de Paris, CNRS, Paris 75005, France
| | - Byeon-Gak Choi
- Department of Earth Science Education, Seoul National University, Seoul 08826, Republic of Korea
| | - Nicolas Dauphas
- Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - Andrew M. Davis
- Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - Tommaso Di Rocco
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Wataru Fujiya
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Ryota Fukai
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Ikshu Gautam
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Makiko K. Haba
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Yuki Hibiya
- General Systems Studies, The University of Tokyo, Tokyo 153-0041, Japan
| | - Hiroshi Hidaka
- Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Hisashi Homma
- Osaka Application Laboratory, SBUWDX, Rigaku Corporation, Osaka 569-1146, Japan
| | - Peter Hoppe
- Max Planck Institute for Chemistry, Mainz 55128, Germany
| | - Gary R. Huss
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Kiyohiro Ichida
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Tsuyoshi Iizuka
- Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Trevor R. Ireland
- School of Earth and Environmental Sciences, The University of Queensland, St. Lucia, QLD 4072, Australia
| | - Akira Ishikawa
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Shoichi Itoh
- Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Noriyuki Kawasaki
- Department of Natural History Sciences, IIL, Hokkaido University, Sapporo 001-0021, Japan
| | - Noriko T. Kita
- Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Kouki Kitajima
- Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Thorsten Kleine
- Max Planck Institute for Solar System Research, Göttingen 37077, Germany
| | - Shintaro Komatani
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Alexander N. Krot
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Ming-Chang Liu
- Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Yuki Masuda
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Kevin D. McKeegan
- Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Mayu Morita
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | | | - Frédéric Moynier
- Université Paris Cités, Institut de physique du globe de Paris, CNRS, Paris 75005, France
| | - Izumi Nakai
- Applied Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Kazuhide Nagashima
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - David Nesvorný
- Department of Space Studies, Southwest Research Institute, Boulder, CO 80302, USA
| | - Larry Nittler
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Morihiko Onose
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Andreas Pack
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Changkun Park
- Earth System Sciences, Korea Polar Research Institute, Incheon 21990, Korea
| | - Liping Qin
- CAS Key Laboratory of Crust-Mantle Materials and Environments, University of Science and Technology of China, School of Earth and Space Sciences, Anhui 230026, China
| | - Sara S. Russell
- Department of Earth Sciences, Natural History Museum, London SW7 5BD, UK
| | - Naoya Sakamoto
- Isotope Imaging Laboratory, Creative Research Institution, Hokkaido University, Sapporo 001-0021, Japan
| | - Maria Schönbächler
- Institute for Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | - Lauren Tafla
- Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Haolan Tang
- Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Kentaro Terada
- Earth and Space Science, Osaka University, Osaka 560-0043, Japan
| | - Yasuko Terada
- Spectroscopy and Imaging, Japan Synchrotron Radiation Research Institute, Hyogo 679-5198, Japan
| | - Tomohiro Usui
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Sohei Wada
- Department of Natural History Sciences, IIL, Hokkaido University, Sapporo 001-0021, Japan
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Richard J. Walker
- Department of Geology, University of Maryland, College Park, MD 20742, USA
| | - Katsuyuki Yamashita
- Graduate School of Natural Science and Technology, Okayama University, Okayama 700-8530, Japan
| | - Qing-Zhu Yin
- Earth and Planetary Sciences, University of California, Davis, Davis, CA 95616, USA
| | - Tetsuya Yokoyama
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Shigekazu Yoneda
- Science and Engineering, National Museum of Nature and Science, Tsukuba 305-0005, Japan
| | - Edward D. Young
- Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Hiroharu Yui
- Department of Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Ai-Cheng Zhang
- School of Earth Sciences and Engineering, Nanjing University, Nanjing 210023, China
| | - Tomoki Nakamura
- Department of Earth Science, Tohoku University, Sendai 980-8578, Japan
| | - Hiroshi Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Takaaki Noguchi
- Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Ryuji Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Kanako Sakamoto
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hikaru Yabuta
- Earth and Planetary Systems Science Program, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - Masanao Abe
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Akiko Miyazaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Aiko Nakato
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masahiro Nishimura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Tatsuaki Okada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Toru Yada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kasumi Yogata
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoru Nakazawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Takanao Saiki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoshi Tanaka
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Fuyuto Terui
- Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | - Yuichi Tsuda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | | | - Makoto Yoshikawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Shogo Tachibana
- UTokyo Organization for Planetary and Space Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Hisayoshi Yurimoto
- Department of Natural History Sciences, IIL, Hokkaido University, Sapporo 001-0021, Japan
- Department of Earth Sciences, Natural History Museum, London SW7 5BD, UK
| |
Collapse
|
5
|
Onyett IJ, Schiller M, Makhatadze GV, Deng Z, Johansen A, Bizzarro M. Silicon isotope constraints on terrestrial planet accretion. Nature 2023; 619:539-544. [PMID: 37316662 PMCID: PMC10356600 DOI: 10.1038/s41586-023-06135-z] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/05/2022] [Accepted: 04/26/2023] [Indexed: 06/16/2023]
Abstract
Understanding the nature and origin of the precursor material to terrestrial planets is key to deciphering the mechanisms and timescales of planet formation1. Nucleosynthetic variability among rocky Solar System bodies can trace the composition of planetary building blocks2-5. Here we report the nucleosynthetic composition of silicon (μ30Si), the most abundant refractory planet-building element, in primitive and differentiated meteorites to identify terrestrial planet precursors. Inner Solar System differentiated bodies, including Mars, record μ30Si deficits of -11.0 ± 3.2 parts per million to -5.8 ± 3.0 parts per million whereas non-carbonaceous and carbonaceous chondrites show μ30Si excesses from 7.4 ± 4.3 parts per million to 32.8 ± 2.0 parts per million relative to Earth. This establishes that chondritic bodies are not planetary building blocks. Rather, material akin to early-formed differentiated asteroids must represent a major planetary constituent. The μ30Si values of asteroidal bodies correlate with their accretion ages, reflecting progressive admixing of a μ30Si-rich outer Solar System material to an initially μ30Si-poor inner disk. Mars' formation before chondrite parent bodies is necessary to avoid incorporation of μ30Si-rich material. In contrast, Earth's μ30Si composition necessitates admixing of 26 ± 9 per cent of μ30Si-rich outer Solar System material to its precursors. The μ30Si compositions of Mars and proto-Earth are consistent with their rapid formation by collisional growth and pebble accretion less than three million years after Solar System formation. Finally, Earth's nucleosynthetic composition for s-process sensitive (molybdenum and zirconium) and siderophile (nickel) tracers are consistent with pebble accretion when volatility-driven processes during accretion and the Moon-forming impact are carefully evaluated.
Collapse
Affiliation(s)
- Isaac J Onyett
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark.
| | - Martin Schiller
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Georgy V Makhatadze
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Zhengbin Deng
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Anders Johansen
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Lund, Sweden
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
- Institut de Physique du Globe de Paris, Université de Paris Cité, Paris, France
| |
Collapse
|
6
|
Yokoyama T, Nagashima K, Nakai I, Young ED, Abe Y, Aléon J, Alexander CMO, Amari S, Amelin Y, Bajo KI, Bizzarro M, Bouvier A, Carlson RW, Chaussidon M, Choi BG, Dauphas N, Davis AM, Di Rocco T, Fujiya W, Fukai R, Gautam I, Haba MK, Hibiya Y, Hidaka H, Homma H, Hoppe P, Huss GR, Ichida K, Iizuka T, Ireland TR, Ishikawa A, Ito M, Itoh S, Kawasaki N, Kita NT, Kitajima K, Kleine T, Komatani S, Krot AN, Liu MC, Masuda Y, McKeegan KD, Morita M, Motomura K, Moynier F, Nguyen A, Nittler L, Onose M, Pack A, Park C, Piani L, Qin L, Russell SS, Sakamoto N, Schönbächler M, Tafla L, Tang H, Terada K, Terada Y, Usui T, Wada S, Wadhwa M, Walker RJ, Yamashita K, Yin QZ, Yoneda S, Yui H, Zhang AC, Connolly HC, Lauretta DS, Nakamura T, Naraoka H, Noguchi T, Okazaki R, Sakamoto K, Yabuta H, Abe M, Arakawa M, Fujii A, Hayakawa M, Hirata N, Hirata N, Honda R, Honda C, Hosoda S, Iijima YI, Ikeda H, Ishiguro M, Ishihara Y, Iwata T, Kawahara K, Kikuchi S, Kitazato K, Matsumoto K, Matsuoka M, Michikami T, Mimasu Y, Miura A, Morota T, Nakazawa S, Namiki N, Noda H, Noguchi R, Ogawa N, Ogawa K, Okada T, Okamoto C, Ono G, Ozaki M, Saiki T, Sakatani N, Sawada H, Senshu H, Shimaki Y, Shirai K, Sugita S, Takei Y, Takeuchi H, Tanaka S, Tatsumi E, Terui F, Tsuda Y, Tsukizaki R, Wada K, Watanabe SI, Yamada M, Yamada T, Yamamoto Y, Yano H, Yokota Y, Yoshihara K, Yoshikawa M, Yoshikawa K, Furuya S, Hatakeda K, Hayashi T, Hitomi Y, Kumagai K, Miyazaki A, Nakato A, Nishimura M, Soejima H, Suzuki A, Yada T, Yamamoto D, Yogata K, Yoshitake M, Tachibana S, Yurimoto H. Samples returned from the asteroid Ryugu are similar to Ivuna-type carbonaceous meteorites. Science 2023; 379:eabn7850. [PMID: 35679354 DOI: 10.1126/science.abn7850] [Citation(s) in RCA: 18] [Impact Index Per Article: 18.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Carbonaceous meteorites are thought to be fragments of C-type (carbonaceous) asteroids. Samples of the C-type asteroid (162173) Ryugu were retrieved by the Hayabusa2 spacecraft. We measured the mineralogy and bulk chemical and isotopic compositions of Ryugu samples. The samples are mainly composed of materials similar to those of carbonaceous chondrite meteorites, particularly the CI (Ivuna-type) group. The samples consist predominantly of minerals formed in aqueous fluid on a parent planetesimal. The primary minerals were altered by fluids at a temperature of 37° ± 10°C, about [Formula: see text] million (statistical) or [Formula: see text] million (systematic) years after the formation of the first solids in the Solar System. After aqueous alteration, the Ryugu samples were likely never heated above ~100°C. The samples have a chemical composition that more closely resembles that of the Sun's photosphere than other natural samples do.
Collapse
Affiliation(s)
- Tetsuya Yokoyama
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Kazuhide Nagashima
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - Izumi Nakai
- Department of Applied Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Edward D Young
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Yoshinari Abe
- Graduate School of Engineering Materials Science and Engineering, Tokyo Denki University, Tokyo 120-8551, Japan
| | - Jérôme Aléon
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Sorbonne Université, Museum National d'Histoire Naturelle, Centre National de la Recherche Scientifique Unité Mixte de Recherche 7590, Institut de recherche pour le développement, 75005 Paris, France
| | - Conel M O'D Alexander
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Sachiko Amari
- McDonnell Center for the Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, USA
| | - Yuri Amelin
- Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, GD 510640, China
| | - Ken-Ichi Bajo
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, K 1350 Copenhagen, Denmark
| | - Audrey Bouvier
- Bayerisches Geoinstitut, Universität Bayreuth, 95447 Bayreuth, Germany
| | - Richard W Carlson
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Marc Chaussidon
- Université de Paris, Institut de physique du globe de Paris, Centre National de la Recherche Scientifique, 75005 Paris, France
| | - Byeon-Gak Choi
- Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea
| | - Nicolas Dauphas
- Department of the Geophysical Sciences and Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA
| | - Andrew M Davis
- Department of the Geophysical Sciences and Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA
| | - Tommaso Di Rocco
- Faculty of Geosciences and Geography, University of Göttingen, D-37077 Göttingen, Germany
| | - Wataru Fujiya
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Ryota Fukai
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Ikshu Gautam
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Makiko K Haba
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Yuki Hibiya
- Department of General Systems Studies, University of Tokyo, Tokyo 153-0041, Japan
| | - Hiroshi Hidaka
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Hisashi Homma
- Osaka Application Laboratory, Rigaku Corporation, Osaka 569-1146, Japan
| | - Peter Hoppe
- Max Planck Institute for Chemistry, Mainz 55128, Germany
| | - Gary R Huss
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - Kiyohiro Ichida
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Tsuyoshi Iizuka
- Department of Earth and Planetary Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Trevor R Ireland
- School of Earth and Environmental Sciences, University of Queensland, St Lucia, QLD 4072, Australia
| | - Akira Ishikawa
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Motoo Ito
- Kochi Institute for Core Sample Research, Japan Agency for Marine-Earth Science and Technology, Kochi 783-8502, Japan
| | - Shoichi Itoh
- Department of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Noriyuki Kawasaki
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Noriko T Kita
- Department of Geoscience, University of Wisconsin, Madison, WI 53706, USA
| | - Kouki Kitajima
- Department of Geoscience, University of Wisconsin, Madison, WI 53706, USA
| | - Thorsten Kleine
- Max Planck Institute for Solar System Research, 37077 Göttingen, Germany
| | - Shintaro Komatani
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Alexander N Krot
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - Ming-Chang Liu
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Yuki Masuda
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Kevin D McKeegan
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Mayu Morita
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Kazuko Motomura
- Thermal Analysis Division, Rigaku Corporation, Tokyo 196-8666, Japan
| | - Frédéric Moynier
- Université de Paris, Institut de physique du globe de Paris, Centre National de la Recherche Scientifique, 75005 Paris, France
| | - Ann Nguyen
- Astromaterials Research and Exploration Science Division, National Aeronautics and Space Administration Johnson Space Center, Houston, TX 77058, USA
| | - Larry Nittler
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Morihiko Onose
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Andreas Pack
- Faculty of Geosciences and Geography, University of Göttingen, D-37077 Göttingen, Germany
| | - Changkun Park
- Division of Earth-System Sciences, Korea Polar Research Institute, Incheon 21990, Korea
| | - Laurette Piani
- Centre de Recherches Pétrographiques et Géochimiques, Centre National de la Recherche Scientifique-Université de Lorraine, 54500 Nancy, France
| | - Liping Qin
- School of Earth and Space Sciences, University of Science and Technology of China, Anhui 230026, China
| | - Sara S Russell
- Department of Earth Sciences, Natural History Museum, London SW7 5BD, UK
| | - Naoya Sakamoto
- Isotope Imaging Laboratory, Hokkaido University, Sapporo 001-0021, Japan
| | - Maria Schönbächler
- Institute for Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | - Lauren Tafla
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Haolan Tang
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Kentaro Terada
- Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan
| | - Yasuko Terada
- Spectroscopy and Imaging Division, Japan Synchrotron Radiation Research Institute, Hyogo 679-5198, Japan
| | - Tomohiro Usui
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Sohei Wada
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Richard J Walker
- Department of Geology, University of Maryland, College Park, MD 20742, USA
| | - Katsuyuki Yamashita
- Graduate School of Natural Science and Technology, Okayama University, Okayama 700-8530, Japan
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California, Davis, CA 95616, USA
| | - Shigekazu Yoneda
- Department of Science and Engineering, National Museum of Nature and Science, Tsukuba 305-0005, Japan
| | - Hiroharu Yui
- Department of Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Ai-Cheng Zhang
- School of Earth Sciences and Engineering, Nanjing University, Nanjing 210023, China
| | - Harold C Connolly
- Department of Geology, School of Earth and Environment, Rowan University, Glassboro, NJ 08028, USA
| | - Dante S Lauretta
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85705, USA
| | - Tomoki Nakamura
- Department of Earth Science, Tohoku University, Sendai 980-8578, Japan
| | - Hiroshi Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Takaaki Noguchi
- Department of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Ryuji Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Kanako Sakamoto
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hikaru Yabuta
- Earth and Planetary Systems Science Program, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - Masanao Abe
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masahiko Arakawa
- Graduate School of Science, Kobe University, Kobe 657-8501, Japan
| | - Atsushi Fujii
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masahiko Hayakawa
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Naoyuki Hirata
- Graduate School of Science, Kobe University, Kobe 657-8501, Japan
| | - Naru Hirata
- Department of Computer Science and Engineering, University of Aizu, Aizu-Wakamatsu 965-8580, Japan
| | - Rie Honda
- Faculty of Science and Technology, Kochi University, Kochi 780-8520, Japan
| | - Chikatoshi Honda
- Department of Computer Science and Engineering, University of Aizu, Aizu-Wakamatsu 965-8580, Japan
| | - Satoshi Hosoda
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Yu-Ichi Iijima
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hitoshi Ikeda
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masateru Ishiguro
- Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea
| | - Yoshiaki Ishihara
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Takahiro Iwata
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan.,Graduate University for Advanced Studies, Sokendai, Kanagawa 240-0193, Japan
| | - Kosuke Kawahara
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Shota Kikuchi
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - Kohei Kitazato
- Department of Computer Science and Engineering, University of Aizu, Aizu-Wakamatsu 965-8580, Japan
| | - Koji Matsumoto
- National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - Moe Matsuoka
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | | | - Yuya Mimasu
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Akira Miura
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Tomokatsu Morota
- Department of Earth and Planetary Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Satoru Nakazawa
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Noriyuki Namiki
- National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - Hirotomo Noda
- National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - Rina Noguchi
- Academic Assembly Institute of Science and Technology, Niigata University, Niigata 950-2181, Japan
| | - Naoko Ogawa
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kazunori Ogawa
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Tatsuaki Okada
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan.,Department of Chemistry, University of Tokyo, Tokyo 113-0033, Japan
| | - Chisato Okamoto
- Graduate School of Science, Kobe University, Kobe 657-8501, Japan
| | - Go Ono
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masanobu Ozaki
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan.,Graduate University for Advanced Studies, Sokendai, Kanagawa 240-0193, Japan
| | - Takanao Saiki
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Naoya Sakatani
- College of Science Department of Physics, Rikkyo University, Tokyo 171-8501, Japan
| | - Hirotaka Sawada
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hiroki Senshu
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - Yuri Shimaki
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kei Shirai
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Seiji Sugita
- Department of Earth and Planetary Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Yuto Takei
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hiroshi Takeuchi
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoshi Tanaka
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Eri Tatsumi
- Instituto de Astrofísica de Canarias, University of La Laguna, Tenerife, Spain
| | - Fuyuto Terui
- Graduate School of Engineering, Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | - Yuichi Tsuda
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Ryudo Tsukizaki
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Koji Wada
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - Sei-Ichiro Watanabe
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Manabu Yamada
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - Tetsuya Yamada
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Yukio Yamamoto
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hajime Yano
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Yasuhiro Yokota
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Keisuke Yoshihara
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Makoto Yoshikawa
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kent Yoshikawa
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Shizuho Furuya
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | | | - Tasuku Hayashi
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Yuya Hitomi
- Marine Works Japan Ltd., Yokosuka 237-0063, Japan
| | | | - Akiko Miyazaki
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Aiko Nakato
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masahiro Nishimura
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | | | - Ayako Suzuki
- Marine Works Japan Ltd., Yokosuka 237-0063, Japan
| | - Toru Yada
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Daiki Yamamoto
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kasumi Yogata
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Miwa Yoshitake
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Shogo Tachibana
- UTokyo Organization for Planetary and Space Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Hisayoshi Yurimoto
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan.,Isotope Imaging Laboratory, Hokkaido University, Sapporo 001-0021, Japan
| |
Collapse
|
7
|
Kawasaki N, Nagashima K, Sakamoto N, Matsumoto T, Bajo KI, Wada S, Igami Y, Miyake A, Noguchi T, Yamamoto D, Russell SS, Abe Y, Aléon J, Alexander CM, Amari S, Amelin Y, Bizzarro M, Bouvier A, Carlson RW, Chaussidon M, Choi BG, Dauphas N, Davis AM, Di Rocco T, Fujiya W, Fukai R, Gautam I, Haba MK, Hibiya Y, Hidaka H, Homma H, Hoppe P, Huss GR, Ichida K, Iizuka T, Ireland TR, Ishikawa A, Ito M, Itoh S, Kita NT, Kitajima K, Kleine T, Komatani S, Krot AN, Liu MC, Masuda Y, McKeegan KD, Morita M, Motomura K, Moynier F, Nakai I, Nguyen A, Nittler L, Onose M, Pack A, Park C, Piani L, Qin L, Schönbächler M, Tafla L, Tang H, Terada K, Terada Y, Usui T, Wadhwa M, Walker RJ, Yamashita K, Yin QZ, Yokoyama T, Yoneda S, Young ED, Yui H, Zhang AC, Nakamura T, Naraoka H, Okazaki R, Sakamoto K, Yabuta H, Abe M, Miyazaki A, Nakato A, Nishimura M, Okada T, Yada T, Yogata K, Nakazawa S, Saiki T, Tanaka S, Terui F, Tsuda Y, Watanabe SI, Yoshikawa M, Tachibana S, Yurimoto H. Oxygen isotopes of anhydrous primary minerals show kinship between asteroid Ryugu and comet 81P/Wild2. Sci Adv 2022; 8:eade2067. [PMID: 36525483 PMCID: PMC9757743 DOI: 10.1126/sciadv.ade2067] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 08/01/2022] [Accepted: 11/17/2022] [Indexed: 06/17/2023]
Abstract
The extraterrestrial materials returned from asteroid (162173) Ryugu consist predominantly of low-temperature aqueously formed secondary minerals and are chemically and mineralogically similar to CI (Ivuna-type) carbonaceous chondrites. Here, we show that high-temperature anhydrous primary minerals in Ryugu and CI chondrites exhibit a bimodal distribution of oxygen isotopic compositions: 16O-rich (associated with refractory inclusions) and 16O-poor (associated with chondrules). Both the 16O-rich and 16O-poor minerals probably formed in the inner solar protoplanetary disk and were subsequently transported outward. The abundance ratios of the 16O-rich to 16O-poor minerals in Ryugu and CI chondrites are higher than in other carbonaceous chondrite groups but are similar to that of comet 81P/Wild2, suggesting that Ryugu and CI chondrites accreted in the outer Solar System closer to the accretion region of comets.
Collapse
Affiliation(s)
- Noriyuki Kawasaki
- Department of Natural History Sciences, Hokkaido University Sapporo 060-0810, Japan
| | - Kazuhide Nagashima
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Naoya Sakamoto
- Isotope Imaging Laboratory, Creative Research Institution, Hokkaido University, Sapporo 001-0021, Japan
| | - Toru Matsumoto
- The Hakubi Center for Advanced Research, Kyoto University, Kitashirakawaoiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
- Division of Earth and Planetary Sciences, Kyoto University, Kitashirakawaoiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Ken-ichi Bajo
- Department of Natural History Sciences, Hokkaido University Sapporo 060-0810, Japan
| | - Sohei Wada
- Department of Natural History Sciences, Hokkaido University Sapporo 060-0810, Japan
| | - Yohei Igami
- Division of Earth and Planetary Sciences, Kyoto University, Kitashirakawaoiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Akira Miyake
- Division of Earth and Planetary Sciences, Kyoto University, Kitashirakawaoiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Takaaki Noguchi
- Division of Earth and Planetary Sciences, Kyoto University, Kitashirakawaoiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Daiki Yamamoto
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Sara S. Russell
- Department of Earth Sciences, Natural History Museum, London, SW7 5BD, UK
| | - Yoshinari Abe
- Graduate School of Engineering Materials Science and Engineering, Tokyo Denki University, Tokyo 120-8551, Japan
| | - Jérôme Aléon
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Sorbonne Université, Museum National d’Histoire Naturelle, Centre National de la Recherche Scientifique Unité Mixte de Recherche 7590, IRD, Paris 75005, France
| | | | - Sachiko Amari
- McDonnell Center for the Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, USA
- Geochemical Research Center, The University of Tokyo, Tokyo 113-0033, Japan
| | - Yuri Amelin
- Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, GD 510640, China
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen K 1350, Denmark
| | - Audrey Bouvier
- Bayerisches Geoinstitut, Universität Bayreuth, Bayreuth 95447, Germany
| | - Richard W. Carlson
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Marc Chaussidon
- Université de Paris, Institut de physique du globe de Paris, Centre National de la Recherche Scientifique, Paris 75005, France
| | - Byeon-Gak Choi
- Department of Earth Science Education, Seoul National University, Seoul 08826, Republic of Korea
| | - Nicolas Dauphas
- Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Andrew M. Davis
- Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Tommaso Di Rocco
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Wataru Fujiya
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Ryota Fukai
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Ikshu Gautam
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Makiko K. Haba
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Yuki Hibiya
- Department of General Systems Studies, The University of Tokyo, Tokyo 153-0041, Japan
| | - Hiroshi Hidaka
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Hisashi Homma
- Osaka Application Laboratory, Rigaku Corporation, Osaka 569-1146, Japan
| | - Peter Hoppe
- Max Planck Institute for Chemistry, Mainz 55128, Germany
| | - Gary R. Huss
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Kiyohiro Ichida
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Tsuyoshi Iizuka
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Trevor R. Ireland
- School of Earth and Environmental Sciences, The University of Queensland, St. Lucia QLD 4072, Australia
| | - Akira Ishikawa
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Motoo Ito
- Kochi Institute for Core Sample Research, Japan Agency for Marine-Earth Science and Technology, Kochi 783-8502, Japan
| | - Shoichi Itoh
- Division of Earth and Planetary Sciences, Kyoto University, Kitashirakawaoiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Noriko T. Kita
- Department of Geoscience, University of Wisconsin- Madison, Madison, WI 53706, USA
| | - Kouki Kitajima
- Department of Geoscience, University of Wisconsin- Madison, Madison, WI 53706, USA
| | - Thorsten Kleine
- Max Planck Institute for Solar System Research, Göttingen 37077, Germany
| | - Shintaro Komatani
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Alexander N. Krot
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Ming-Chang Liu
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, USA
- Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
| | - Yuki Masuda
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Kevin D. McKeegan
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, USA
| | - Mayu Morita
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | | | - Frédéric Moynier
- Université de Paris, Institut de physique du globe de Paris, Centre National de la Recherche Scientifique, Paris 75005, France
| | - Izumi Nakai
- Department of Applied Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Ann Nguyen
- Astromaterials Research and Exploration Science Division, National Aeronautics and Space Administration Johnson Space Center, Houston, TX 77058, USA
| | - Larry Nittler
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Morihiko Onose
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Andreas Pack
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Changkun Park
- Division of Earth-System Sciences, Korea Polar Research Institute, Incheon 21990, Republic of Korea
| | - Laurette Piani
- Centre de Recherches Pétrographiques et Géochimiques, Centre National de la Recherche Scientifique–Université de Lorraine, Nancy 54500, France
| | - Liping Qin
- School of Earth and Space Sciences, University of Science and Technology of China,, Anhui 230026, China
| | - Maria Schönbächler
- Institute for Geochemistry and Petrology, Department of Earth Sciences, Eidgenössische Technische Hochschule Zürich, Zürich, Switzerland
| | - Lauren Tafla
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, USA
| | - Haolan Tang
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, USA
| | - Kentaro Terada
- Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan
| | - Yasuko Terada
- Spectroscopy and Imaging, Japan Synchrotron Radiation Research Institute, Hyogo 679-5198, Japan
| | - Tomohiro Usui
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Richard J. Walker
- Department of Geology, University of Maryland, College Park, MD 20742, USA
| | - Katsuyuki Yamashita
- Graduate School of Natural Science and Technology, Okayama University, Okayama 700-8530, Japan
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California, Davis CA 95616, USA
| | - Tetsuya Yokoyama
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Shigekazu Yoneda
- Department of Science and Engineering, National Museum of Nature and Science, Tsukuba 305-0005, Japan
| | - Edward D. Young
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, USA
| | - Hiroharu Yui
- Department of Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Ai-Cheng Zhang
- School of Earth Sciences and Engineering, Nanjing University, Nanjing 210023, China
| | - Tomoki Nakamura
- Department of Earth Science, Tohoku University, Sendai 980-8578, Japan
| | - Hiroshi Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Ryuji Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Kanako Sakamoto
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hikaru Yabuta
- Earth and Planetary Systems Science Program, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - Masanao Abe
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Akiko Miyazaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Aiko Nakato
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masahiro Nishimura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Tatsuaki Okada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Toru Yada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kasumi Yogata
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoru Nakazawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Takanao Saiki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoshi Tanaka
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Fuyuto Terui
- Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | - Yuichi Tsuda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Sei-ichiro Watanabe
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Makoto Yoshikawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Shogo Tachibana
- Tokyo Organization for Planetary and Space Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Hisayoshi Yurimoto
- Department of Natural History Sciences, Hokkaido University Sapporo 060-0810, Japan
- Isotope Imaging Laboratory, Creative Research Institution, Hokkaido University, Sapporo 001-0021, Japan
| |
Collapse
|
8
|
Hu Y, Moynier F, Bizzarro M. Potassium isotope heterogeneity in the early Solar System controlled by extensive evaporation and partial recondensation. Nat Commun 2022; 13:7669. [PMID: 36509778 PMCID: PMC9744853 DOI: 10.1038/s41467-022-35362-7] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/07/2022] [Accepted: 11/28/2022] [Indexed: 12/14/2022] Open
Abstract
Volatiles are vital ingredients for a habitable planet. Angrite meteorites sample the most volatile-depleted planetesimal in the Solar System, particularly for the alkali elements. They are prime targets for investigating the formation of volatile-poor rocky planets, yet their exceptionally low volatile content presents a major analytical challenge. Here, we leverage improved sensitivity and precision of K isotopic analysis to constrain the mechanism of extreme K depletion (>99.8%) in angrites. In contrast with the isotopically heavy Moon and Vesta, we find that angrites are strikingly depleted in the heavier K isotopes, which is best explained by partial recondensation of vaporized K following extensive evaporation on the angrite parent body (APB) during magma-ocean stage. Therefore, the APB may provide a rare example of isotope fractionation controlled by condensation, rather than evaporation, at a planetary scale. Furthermore, nebula-wide K isotopic variations primarily reflect volatility-driven fractionations instead of presolar nucleosynthetic heterogeneity proposed previously.
Collapse
Affiliation(s)
- Yan Hu
- grid.9489.c0000 0001 0675 8101Université Paris Cité, Institut de Physique du Globe de Paris, CNRS, UMR 7154, Paris, 75005 France
| | - Frédéric Moynier
- grid.9489.c0000 0001 0675 8101Université Paris Cité, Institut de Physique du Globe de Paris, CNRS, UMR 7154, Paris, 75005 France
| | - Martin Bizzarro
- grid.9489.c0000 0001 0675 8101Université Paris Cité, Institut de Physique du Globe de Paris, CNRS, UMR 7154, Paris, 75005 France ,grid.5254.60000 0001 0674 042XStarPlan - Centre for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, Copenhagen, DK-1350 Denmark
| |
Collapse
|
9
|
Hopp T, Dauphas N, Abe Y, Aléon J, O'D Alexander CM, Amari S, Amelin Y, Bajo KI, Bizzarro M, Bouvier A, Carlson RW, Chaussidon M, Choi BG, Davis AM, Di Rocco T, Fujiya W, Fukai R, Gautam I, Haba MK, Hibiya Y, Hidaka H, Homma H, Hoppe P, Huss GR, Ichida K, Iizuka T, Ireland TR, Ishikawa A, Ito M, Itoh S, Kawasaki N, Kita NT, Kitajima K, Kleine T, Komatani S, Krot AN, Liu MC, Masuda Y, McKeegan KD, Morita M, Motomura K, Moynier F, Nakai I, Nagashima K, Nesvorný D, Nguyen A, Nittler L, Onose M, Pack A, Park C, Piani L, Qin L, Russell SS, Sakamoto N, Schönbächler M, Tafla L, Tang H, Terada K, Terada Y, Usui T, Wada S, Wadhwa M, Walker RJ, Yamashita K, Yin QZ, Yokoyama T, Yoneda S, Young ED, Yui H, Zhang AC, Nakamura T, Naraoka H, Noguchi T, Okazaki R, Sakamoto K, Yabuta H, Abe M, Miyazaki A, Nakato A, Nishimura M, Okada T, Yada T, Yogata K, Nakazawa S, Saiki T, Tanaka S, Terui F, Tsuda Y, Watanabe SI, Yoshikawa M, Tachibana S, Yurimoto H. Ryugu's nucleosynthetic heritage from the outskirts of the Solar System. Sci Adv 2022; 8:eadd8141. [PMID: 36264823 DOI: 10.1126/sciadv.add8141] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/16/2023]
Abstract
Little is known about the origin of the spectral diversity of asteroids and what it says about conditions in the protoplanetary disk. Here, we show that samples returned from Cb-type asteroid Ryugu have Fe isotopic anomalies indistinguishable from Ivuna-type (CI) chondrites, which are distinct from all other carbonaceous chondrites. Iron isotopes, therefore, demonstrate that Ryugu and CI chondrites formed in a reservoir that was different from the source regions of other carbonaceous asteroids. Growth and migration of the giant planets destabilized nearby planetesimals and ejected some inward to be implanted into the Main Belt. In this framework, most carbonaceous chondrites may have originated from regions around the birthplaces of Jupiter and Saturn, while the distinct isotopic composition of CI chondrites and Ryugu may reflect their formation further away in the disk, owing their presence in the inner Solar System to excitation by Uranus and Neptune.
Collapse
Affiliation(s)
- Timo Hopp
- Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Nicolas Dauphas
- Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Yoshinari Abe
- Graduate School of Engineering Materials Science and Engineering, Tokyo Denki University, Tokyo 120-8551, Japan
| | - Jérôme Aléon
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Sorbonne Université, Museum National d'Histoire Naturelle, CNRS UMR 7590, IRD, 75005 Paris, France
| | - Conel M O'D Alexander
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Sachiko Amari
- McDonnell Center for the Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, USA
- Geochemical Research Center, The University of Tokyo, Tokyo 113-0033, Japan
| | - Yuri Amelin
- Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, GD 510640, China
| | - Ken-Ichi Bajo
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Martin Bizzarro
- Centre for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Copenhagen K 1350, Denmark
| | - Audrey Bouvier
- Bayerisches Geoinstitut, Universität Bayreuth, Bayreuth 95447, Germany
| | - Richard W Carlson
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Marc Chaussidon
- Université Paris Cité, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Byeon-Gak Choi
- Department of Earth Science Education, Seoul National University, Seoul 08826, Republic of Korea
| | - Andrew M Davis
- Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Tommaso Di Rocco
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Wataru Fujiya
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Ryota Fukai
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Ikshu Gautam
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Makiko K Haba
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Yuki Hibiya
- Department of General Systems Studies, The University of Tokyo, Tokyo 153-0041, Japan
- Research Center for Advanced Science and Technology, The University of Tokyo, Tokyo 153-8904, Japan
| | - Hiroshi Hidaka
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Hisashi Homma
- Osaka Application Laboratory, SBUWDX, Rigaku Corporation, Osaka 569-1146, Japan
| | - Peter Hoppe
- Max Planck Institute for Chemistry, Mainz 55128, Germany
| | - Gary R Huss
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - Kiyohiro Ichida
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Tsuyoshi Iizuka
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Trevor R Ireland
- School of Earth and Environmental Sciences, The University of Queensland, St. Lucia, QLD 4072, Australia
| | - Akira Ishikawa
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Motoo Ito
- Kochi Institute for Core Sample Research, JAMSTEC, Kochi 783-8502, Japan
| | - Shoichi Itoh
- Department of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Noriyuki Kawasaki
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Noriko T Kita
- Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Kouki Kitajima
- Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Thorsten Kleine
- Max Planck Institute for Solar System Research, 37077 Göttingen, Germany
| | - Shintaro Komatani
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Alexander N Krot
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - Ming-Chang Liu
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
- Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
| | - Yuki Masuda
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Kevin D McKeegan
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Mayu Morita
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | | | - Frédéric Moynier
- Université Paris Cité, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Izumi Nakai
- Thermal Analysis, Rigaku Corporation, Tokyo 196-8666, Japan
| | - Kazuhide Nagashima
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - David Nesvorný
- Department of Space Studies, Southwest Research Institute, Boulder, CO 80302, USA
| | - Ann Nguyen
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
| | - Larry Nittler
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Morihiko Onose
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Andreas Pack
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Changkun Park
- Division of Earth-System Sciences, Korea Polar Research Institute, Incheon 21990, Korea
| | - Laurette Piani
- Centre de Recherches Pétrographiques et Géochimiques, CNRS-Université de Lorraine, 54500 Nancy, France
| | - Liping Qin
- Deep Space Exploration Laboratory/CAS Key Laboratory of Crust-Mantle Materials and Environments, University of Science and Technology of China, Hefei 230026, China
| | - Sara S Russell
- Department of Earth Sciences, Natural History Museum, London SW7 5BD, UK
| | - Naoya Sakamoto
- Isotope Imaging Laboratory, Hokkaido University, Sapporo 001-0021, Japan
| | - Maria Schönbächler
- Institute for Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | - Lauren Tafla
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Haolan Tang
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
- University of Science and Technology of China, Hefei, China
| | - Kentaro Terada
- Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan
| | - Yasuko Terada
- Spectroscopy and Imaging Division, Japan Synchrotron Radiation Research Institute, Hyogo 679-5198, Japan
| | - Tomohiro Usui
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Sohei Wada
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Richard J Walker
- Department of Geology, University of Maryland, College Park, MD 20742, USA
| | - Katsuyuki Yamashita
- Graduate School of Natural Science and Technology, Okayama University, Okayama 700-8530, Japan
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California Davis, Davis, CA 95616, USA
| | - Tetsuya Yokoyama
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Shigekazu Yoneda
- Department Science and Engineering, National Museum of Nature and Science, Tsukuba 305-0005, Japan
| | - Edward D Young
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Hiroharu Yui
- Department of Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Ai-Cheng Zhang
- School of Earth Sciences and Engineering, Nanjing University, Nanjing 210023, China
| | - Tomoki Nakamura
- Department of Earth Science, Tohoku University, Sendai 980-8578, Japan
| | - Hiroshi Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Takaaki Noguchi
- Kochi Institute for Core Sample Research, JAMSTEC, Kochi 783-8502, Japan
| | - Ryuji Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Kanako Sakamoto
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hikaru Yabuta
- Earth and Planetary Systems Science Program, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - Masanao Abe
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Akiko Miyazaki
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Aiko Nakato
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masahiro Nishimura
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Tatsuaki Okada
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Toru Yada
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kasumi Yogata
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoru Nakazawa
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Takanao Saiki
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoshi Tanaka
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Fuyuto Terui
- Graduate School of Engineering, Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | - Yuichi Tsuda
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Sei-Ichiro Watanabe
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Makoto Yoshikawa
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Shogo Tachibana
- UTokyo Organization for Planetary and Space Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Hisayoshi Yurimoto
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| |
Collapse
|
10
|
Zhu K, Schiller M, Pan L, Saji NS, Larsen KK, Amsellem E, Rundhaug C, Sossi P, Leya I, Moynier F, Bizzarro M. Late delivery of exotic chromium to the crust of Mars by water-rich carbonaceous asteroids. Sci Adv 2022; 8:eabp8415. [PMID: 36383650 PMCID: PMC9668285 DOI: 10.1126/sciadv.abp8415] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 03/06/2022] [Accepted: 09/27/2022] [Indexed: 06/16/2023]
Abstract
The terrestrial planets endured a phase of bombardment following their accretion, but the nature of this late accreted material is debated, preventing a full understanding of the origin of inner solar system volatiles. We report the discovery of nucleosynthetic chromium isotope variability (μ54Cr) in Martian meteorites that represent mantle-derived magmas intruded in the Martian crust. The μ54Cr variability, ranging from -33.1 ± 5.4 to +6.8 ± 1.5 parts per million, correlates with magma chemistry such that samples having assimilated crustal material define a positive μ54Cr endmember. This compositional endmember represents the primordial crust modified by impacting outer solar system bodies of carbonaceous composition. Late delivery of this volatile-rich material to Mars provided an exotic water inventory corresponding to a global water layer >300 meters deep, in addition to the primordial water reservoir from mantle outgassing. This carbonaceous material may also have delivered a source of biologically relevant molecules to early Mars.
Collapse
Affiliation(s)
- Ke Zhu
- Université de Paris, Institut de Physique du Globe de Paris, Paris, France
| | - Martin Schiller
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Lu Pan
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Nikitha Susan Saji
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Kirsten K. Larsen
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Elsa Amsellem
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Courtney Rundhaug
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Paolo Sossi
- Institute of Geochemistry and Petrology, ETH Zürich, Zürich, Switzerland
| | - Ingo Leya
- Physics Institute, University of Bern, Bern, Switzerland
| | - Frederic Moynier
- Université de Paris, Institut de Physique du Globe de Paris, Paris, France
| | - Martin Bizzarro
- Université de Paris, Institut de Physique du Globe de Paris, Paris, France
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| |
Collapse
|
11
|
Liu B, Johansen A, Lambrechts M, Bizzarro M, Haugbølle T. Natural separation of two primordial planetary reservoirs in an expanding solar protoplanetary disk. Sci Adv 2022; 8:eabm3045. [PMID: 35452282 PMCID: PMC9032962 DOI: 10.1126/sciadv.abm3045] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 09/08/2021] [Accepted: 03/08/2022] [Indexed: 06/14/2023]
Abstract
Meteorites display an isotopic composition dichotomy between noncarbonaceous (NC) and carbonaceous (CC) groups, indicating that planetesimal formation in the solar protoplanetary disk occurred in two distinct reservoirs. The prevailing view is that a rapidly formed Jupiter acted as a barrier between these reservoirs. We show a fundamental inconsistency in this model: If Jupiter is an efficient blocker of drifting pebbles, then the interior NC reservoir is depleted by radial drift within a few hundred thousand years. If Jupiter lets material pass it, then the two reservoirs will be mixed. Instead, we demonstrate that the arrival of the CC pebbles in the inner disk is delayed for several million years by the viscous expansion of the protoplanetary disk. Our results support the hypothesis that Jupiter formed in the outer disk (>10 astronomical units) and allowed a considerable amount of CC material to pass it and become accreted by the terrestrial planets.
Collapse
Affiliation(s)
- Beibei Liu
- Zhejiang Institute of Modern Physics, Department of Physics and Zhejiang University–Purple Mountain Observatory Joint Research Center for Astronomy, Zhejiang University, 38 Zheda Road, Hangzhou 310027, China
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 22100 Lund, Sweden
| | - Anders Johansen
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 22100 Lund, Sweden
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
| | - Michiel Lambrechts
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 22100 Lund, Sweden
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
| | - Martin Bizzarro
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
| | - Troels Haugbølle
- Niels Bohr Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
| |
Collapse
|
12
|
Köksal ES, Põldsalu I, Friis H, Mojzsis SJ, Bizzarro M, Gözen I. Spontaneous Formation of Prebiotic Compartment Colonies on Hadean Earth and Pre‐Noachian Mars. ChemSystemsChem 2022. [DOI: 10.1002/syst.202200013] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
Affiliation(s)
- Elif S. Köksal
- Centre for Molecular Medicine Norway Faculty of Medicine University of Oslo 0318 Oslo Norway
| | - Inga Põldsalu
- Centre for Molecular Medicine Norway Faculty of Medicine University of Oslo 0318 Oslo Norway
| | - Henrik Friis
- Natural History Museum University of Oslo Postboks 1172 Blindern 0318 Oslo Norway
| | - Stephen J. Mojzsis
- Research Centre for Astronomy and Earth Sciences 15–17 Konkoly Thege Miklós Road Budapest 1121 Hungary
- Department of Lithospheric Research University of Vienna UZA 2, Althanstraße 14 1090 Vienna Austria
- Department of Geological Sciences University of Colorado UCB 399, 2200 Colorado Avenue Boulder CO 80309-0399 USA
| | - Martin Bizzarro
- Centre for Star and Planet Formation GLOBE Institute University of Copenhagen 1350 Copenhagen K Denmark
| | - Irep Gözen
- Centre for Molecular Medicine Norway Faculty of Medicine University of Oslo 0318 Oslo Norway
- Department of Chemistry, Faculty of Mathematics and Natural Sciences University of Oslo 0315 Oslo Norway
| |
Collapse
|
13
|
Köksal ES, Põldsalu I, Friis H, Mojzsis SJ, Bizzarro M, Gözen I. Spontaneous Formation of Prebiotic Compartment Colonies on Hadean Earth and Pre‐Noachian Mars. ChemSystemsChem 2022. [DOI: 10.1002/syst.202200012] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Elif S. Köksal
- Centre for Molecular Medicine Norway Faculty of Medicine University of Oslo 0318 Oslo Norway
| | - Inga Põldsalu
- Centre for Molecular Medicine Norway Faculty of Medicine University of Oslo 0318 Oslo Norway
| | - Henrik Friis
- Natural History Museum University of Oslo Postboks 1172 Blindern 0318 Oslo Norway
| | - Stephen J. Mojzsis
- Research Centre for Astronomy and Earth Sciences 15–17 Konkoly Thege Miklós Road Budapest 1121 Hungary
- Department of Lithospheric Research University of Vienna UZA 2, Althanstraße 14 1090 Vienna Austria
- Department of Geological Sciences University of Colorado UCB 399, 2200 Colorado Avenue Boulder CO 80309-0399 USA
| | - Martin Bizzarro
- Centre for Star and Planet Formation GLOBE Institute University of Copenhagen 1350 Copenhagen K Denmark
| | - Irep Gözen
- Centre for Molecular Medicine Norway Faculty of Medicine University of Oslo 0318 Oslo Norway
- Department of Chemistry, Faculty of Mathematics and Natural Sciences University of Oslo 0315 Oslo Norway
| |
Collapse
|
14
|
Köksal ES, Põldsalu I, Friis H, Mojzsis SJ, Bizzarro M, Gözen I. Spontaneous Formation of Prebiotic Compartment Colonies on Hadean Earth and Pre‐Noachian Mars**. ChemSystemsChem 2022. [DOI: 10.1002/syst.202100040] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Elif S. Köksal
- Centre for Molecular Medicine Norway Faculty of Medicine University of Oslo 0318 Oslo Norway
| | - Inga Põldsalu
- Centre for Molecular Medicine Norway Faculty of Medicine University of Oslo 0318 Oslo Norway
| | - Henrik Friis
- Natural History Museum University of Oslo Postboks 1172 Blindern 0318 Oslo Norway
| | - Stephen J. Mojzsis
- Research Centre for Astronomy and Earth Sciences 15–17 Konkoly Thege Miklós Road Budapest 1121 Hungary
- Department of Lithospheric Research University of Vienna UZA 2, Althanstraße 14 1090 Vienna Austria
- Department of Geological Sciences University of Colorado UCB 399, 2200 Colorado Avenue Boulder CO 80309-0399 USA
| | - Martin Bizzarro
- Centre for Star and Planet Formation GLOBE Institute University of Copenhagen 1350 Copenhagen K Denmark
| | - Irep Gözen
- Centre for Molecular Medicine Norway Faculty of Medicine University of Oslo 0318 Oslo Norway
- Department of Chemistry, Faculty of Mathematics and Natural Sciences University of Oslo 0315 Oslo Norway
| |
Collapse
|
15
|
Põldsalu I, Koksal ES, Friis H, Mojzsis S, Bizzarro M, Gozen I. Spontaneous formation of prebiotic compartment colonies on Hadean Earth and Pre-Noachian Mars. Biophys J 2022. [DOI: 10.1016/j.bpj.2021.11.2351] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022] Open
|
16
|
Rochette P, Beck P, Bizzarro M, Braucher R, Cornec J, Debaille V, Devouard B, Gattacceca J, Jourdan F, Moustard F, Moynier F, Nomade S, Reynard B. Impact glasses from Belize represent tektites from the Pleistocene Pantasma impact crater in Nicaragua. Commun Earth Environ 2021; 2:94. [PMID: 34409303 PMCID: PMC7611520 DOI: 10.1038/s43247-021-00155-1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/05/2020] [Accepted: 03/26/2021] [Indexed: 06/13/2023]
Abstract
Tektites are terrestrial impact-generated glasses that are ejected long distance (up to 11,000 km), share unique characteristics and have a poorly understood formation process. Only four tektite strewn-fields are known, and three of them are sourced from known impact craters. Here we show that the recently discovered Pantasma impact crater (14 km diameter) in Nicaragua is the source of an impact glass strewn-field documented in Belize 530 km away. Their cogenesis is documented by coincidental ages, at 804 ± 9 ka, as well as consistent elemental compositions and isotopic ratios. The Belize impact glass share many characteristics with known tektites but also present several peculiar features. We propose that these glasses represent a previously unrecognized tektite strewn-field. These discoveries shed new light on the tektite formation process, which may be more common than previously claimed, as most known Pleistocene >10 km diameter cratering events have generated tektites.
Collapse
Affiliation(s)
- Pierre Rochette
- Aix-Marseille Université, CNRS, IRD, INRAE, UM 34 CEREGE,
Aix-en-Provence, France
| | - Pierre Beck
- IPAG Université Grenoble Alpes, CNRS, Institut de
Planétologie et d’Astrophysique de Grenoble, Grenoble, France
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Globe Institute, University of
Copenhagen, Copenhagen, Denmark
| | - Régis Braucher
- Aix-Marseille Université, CNRS, IRD, INRAE, UM 34 CEREGE,
Aix-en-Provence, France
| | | | - Vinciane Debaille
- Laboratoire G-Time, Université Libre de Bruxelles, Brussels,
Belgium
| | - Bertrand Devouard
- Aix-Marseille Université, CNRS, IRD, INRAE, UM 34 CEREGE,
Aix-en-Provence, France
| | - Jérôme Gattacceca
- Aix-Marseille Université, CNRS, IRD, INRAE, UM 34 CEREGE,
Aix-en-Provence, France
| | - Fred Jourdan
- School of Earth and Planetary Sciences, Curtin University, Perth,
Australia
| | - Fabien Moustard
- Aix-Marseille Université, CNRS, IRD, INRAE, UM 34 CEREGE,
Aix-en-Provence, France
| | - Frédéric Moynier
- Institut de Physique du Globe de Paris, Université Sorbonne
Paris Cité, CNRS UMR 7154, Paris, France
| | - Sébastien Nomade
- LSCE, CEA, UVSQ et Université Paris-Saclay UMR 8212,
Gif–sur-Yvette, France
| | - Bruno Reynard
- Université de Lyon, ENSL, UCBL, CNRS, LGL-TPE, Lyon,
France
| |
Collapse
|
17
|
Zhu K, Moynier F, Schiller M, Alexander CMO, Davidson J, Schrader DL, van Kooten E, Bizzarro M. Chromium isotopic insights into the origin of chondrite parent bodies and the early terrestrial volatile depletion. Geochim Cosmochim Acta 2021; 301:158-186. [PMID: 34393262 PMCID: PMC7611480 DOI: 10.1016/j.gca.2021.02.031] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
Chondrites are meteorites from undifferentiated parent bodies that provide fundamental information about early Solar System evolution and planet formation. The element Cr is highly suitable for deciphering both the timing of formation and the origin of planetary building blocks because it records both radiogenic contributions from 53Mn-53Cr decay and variable nucleosynthetic contributions from the stable 54Cr nuclide. Here, we report high-precision measurements of the massindependent Cr isotope compositions (ε53Cr and ε54Cr) of chondrites (including all carbonaceous chondrites groups) and terrestrial samples using for the first time a multi-collection inductively-coupled-plasma mass-spectrometer to better understand the formation histories and genetic relationships between chondrite parent bodies. With our comprehensive dataset, the order of decreasing ε54Cr (per ten thousand deviation of the 54Cr/52Cr ratio relative to a terrestrial standard) values amongst the carbonaceous chondrites is updated to CI = CH ≥ CB ≥ CR ≥ CM ≈ CV ≈ CO ≥ CK > EC > OC. Chondrites from CO, CV, CR, CM and CB groups show intra-group ε54Cr heterogeneities that may result from sample heterogeneity and/or heterogeneous accretion of their parent bodies. Resolvable ε54Cr (with 2SE uncertainty) differences between CV and CK chondrites rule out an origin from a common parent body or reservoir as has previously been suggested. The CM and CO chondrites share common ε54Cr characteristics, which suggests their parent bodies may have accreted their components in similar proportions. The CB and CH chondrites have low-Mn/Cr ratios and similar ε53Cr values to the CI chondrites, invalidating them as anchors for a bulk 53Mn-53Cr isochron for carbonaceous chondrites. Bulk Earth has a ε53Cr value that is lower than the average of chondrites, including enstatite chondrites. This depletion may constrain the timing of volatile loss from the Earth or its precursors to be within the first million years of Solar System formation and is incompatible with Earth's accretion via any of the known chondrite groups as main contributors, including enstatite chondrites.
Collapse
Affiliation(s)
- Ke Zhu
- Universite' de Paris, Institut de Physique du Globe de Paris, CNRS UMR 7154, 1 rue Jussieu, Paris 75005, France
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5-7, Copenhagen DK-1350, Denmark
- Earth and Planetary Laboratory, Carnegie Institution for Science, 5241 Broad Branch Road, Washington, DC 20015, USA
- Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, 781 East Terrace Road, Tempe, AZ 85287-6004, USA
| | - Frédéric Moynier
- Universite' de Paris, Institut de Physique du Globe de Paris, CNRS UMR 7154, 1 rue Jussieu, Paris 75005, France
| | - Martin Schiller
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5-7, Copenhagen DK-1350, Denmark
| | - Conel M O'D Alexander
- Earth and Planetary Laboratory, Carnegie Institution for Science, 5241 Broad Branch Road, Washington, DC 20015, USA
| | - Jemma Davidson
- Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, 781 East Terrace Road, Tempe, AZ 85287-6004, USA
| | - Devin L Schrader
- Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, 781 East Terrace Road, Tempe, AZ 85287-6004, USA
| | - Elishevah van Kooten
- Universite' de Paris, Institut de Physique du Globe de Paris, CNRS UMR 7154, 1 rue Jussieu, Paris 75005, France
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5-7, Copenhagen DK-1350, Denmark
| | - Martin Bizzarro
- Universite' de Paris, Institut de Physique du Globe de Paris, CNRS UMR 7154, 1 rue Jussieu, Paris 75005, France
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5-7, Copenhagen DK-1350, Denmark
| |
Collapse
|
18
|
Johansen A, Ronnet T, Bizzarro M, Schiller M, Lambrechts M, Nordlund Å, Lammer H. A pebble accretion model for the formation of the terrestrial planets in the Solar System. Sci Adv 2021; 7:7/8/eabc0444. [PMID: 33597233 PMCID: PMC7888959 DOI: 10.1126/sciadv.abc0444] [Citation(s) in RCA: 16] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/10/2020] [Accepted: 12/30/2020] [Indexed: 06/02/2023]
Abstract
Pebbles of millimeter sizes are abundant in protoplanetary discs around young stars. Chondrules inside primitive meteorites-formed by melting of dust aggregate pebbles or in impacts between planetesimals-have similar sizes. The role of pebble accretion for terrestrial planet formation is nevertheless unclear. Here, we present a model where inward-drifting pebbles feed the growth of terrestrial planets. The masses and orbits of Venus, Earth, Theia (which later collided with Earth to form the Moon), and Mars are all consistent with pebble accretion onto protoplanets that formed around Mars' orbit and migrated to their final positions while growing. The isotopic compositions of Earth and Mars are matched qualitatively by accretion of two generations of pebbles, carrying distinct isotopic signatures. Last, we show that the water and carbon budget of Earth can be delivered by pebbles from the early generation before the gas envelope became hot enough to vaporize volatiles.
Collapse
Affiliation(s)
- Anders Johansen
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark.
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 221 00 Lund, Sweden
| | - Thomas Ronnet
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 221 00 Lund, Sweden
| | - Martin Bizzarro
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
| | - Martin Schiller
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
| | - Michiel Lambrechts
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 221 00 Lund, Sweden
| | - Åke Nordlund
- Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark
| | - Helmut Lammer
- Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, 8042 Graz, Austria
| |
Collapse
|
19
|
Livermore B, Dahl T, Bizzarro M, Connelly J. Uranium isotope compositions of biogenic carbonates - Implications for U uptake in shells and the application of the paleo-ocean oxygenation proxy. Geochim Cosmochim Acta 2020; 287:50-64. [PMID: 34354297 PMCID: PMC7611457 DOI: 10.1016/j.gca.2020.07.005] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
The application of U isotopes in carbonates as a paleo-ocean oxygenation proxy is based on the critical assumption that the calcareous shell-building organisms incorporate U into their shells without fractionation relative to the U isotopic composition of ambient seawater. Recent studies claim a small, but resolvable, isotopic offset during abiotic and biogenic aragonite precipitation, whereas no isotope fractionation has been recorded during calcite precipitation. Although aragonite is meta-stable and not preserved over geological timescales (>1 Myr) and U precipitates during diagenesis, the U isotope composition of biogenic aragonite is important because aragonite precipitation is an important U sink to carbonate sediments. In contrast, low-magnesium calcite (LMC) is preserved over geological timescales and may provide a reliable fingerprint of ancient ocean chemistry. Therefore, a more general study is needed that compares U isotope compositions of primary marine biogenic carbonate precipitates. We report the U isotope compositions of 32 modern samples from geographically distinct localities in the Atlantic Ocean including corals (Scleractinia, Octocorallia), brachiopods (Articulata), molluscs (Tellina Listeri, Codahia Obicularis) and barnacles as well as one fossil mollusc. These samples reflect variable primary minerals, water temperatures, water depths, pH-values of ambient water, and U concentrations. Several seawater samples have also been measured to compare our methods with those of previously published studies. The analyzed modern corals and brachiopods display U isotopic compositions that are indistinguishable from modern seawater. This suggests that these carbonates have the potential to faithfully record the U isotopic composition of the surrounding seawater in which they form. The analyzed brachiopods are of particular interest as they are composed of the calcium carbonate polymorph LMC that is stable over geological timescales. While this study shows for the first time that LMC phases are robust targets in ancient samples, their low U abundance presents analytical challenges for precise U isotope analyses. We also show that two barnacle shells collected with ambient seawater have U isotopic compositions that are both lighter and heavier than the ambient seawater. The mechanism to explain this offset is not determined, but it demonstrates that at least barnacle shells are not representative of the seawater in which they last lived. Two of three partially fossilized mollusc shells also show resolvable offsets from seawater, likely indicating secondary processes that are known to shift or fractionate U isotopes. Collectively, our new data indicate that: 1) aragonite delivers U with a seawater composition to carbonate sediments, and 2) LMC shells of brachiopods that are stable over geological timescales may be more suitable for reconstructing the U isotope composition of ancient oceans.
Collapse
Affiliation(s)
- B.D. Livermore
- Centre for Star and Planet Formation, University of Copenhagen, DK-1350 Copenhagen K, Denmark
| | - T.W. Dahl
- GLOBE Institute, University of Copenhagen, DK-1350 Copenhagen K, Denmark
| | - M. Bizzarro
- Centre for Star and Planet Formation, University of Copenhagen, DK-1350 Copenhagen K, Denmark
- GLOBE Institute, University of Copenhagen, DK-1350 Copenhagen K, Denmark
| | - J.N. Connelly
- Centre for Star and Planet Formation, University of Copenhagen, DK-1350 Copenhagen K, Denmark
- GLOBE Institute, University of Copenhagen, DK-1350 Copenhagen K, Denmark
| |
Collapse
|
20
|
Krot AN, Nagashima K, Lyons JR, Lee JE, Bizzarro M. Oxygen isotopic heterogeneity in the early Solar System inherited from the protosolar molecular cloud. Sci Adv 2020; 6:eaay2724. [PMID: 33067241 PMCID: PMC7567603 DOI: 10.1126/sciadv.aay2724] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 06/04/2019] [Accepted: 09/02/2020] [Indexed: 06/11/2023]
Abstract
The Sun is 16O-enriched (Δ17O = -28.4 ± 3.6‰) relative to the terrestrial planets, asteroids, and chondrules (-7‰ < Δ17O < 3‰). Ca,Al-rich inclusions (CAIs), the oldest Solar System solids, approach the Sun's Δ17O. Ultraviolet CO self-shielding resulting in formation of 16O-rich CO and 17,18O-enriched water is the currently favored mechanism invoked to explain the observed range of Δ17O. However, the location of CO self-shielding (molecular cloud or protoplanetary disk) remains unknown. Here we show that CAIs with predominantly low (26Al/27Al)0, <5 × 10-6, exhibit a large inter-CAI range of Δ17O, from -40‰ to -5‰. In contrast, CAIs with the canonical (26Al/27Al)0 of ~5 × 10-5 from unmetamorphosed carbonaceous chondrites have a limited range of Δ17O, -24 ± 2‰. Because CAIs with low (26Al/27Al)0 are thought to have predated the canonical CAIs and formed within first 10,000-20,000 years of the Solar System evolution, these observations suggest oxygen isotopic heterogeneity in the early solar system was inherited from the protosolar molecular cloud.
Collapse
Affiliation(s)
- Alexander N Krot
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI, USA.
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Denmark
| | - Kazuhide Nagashima
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI, USA
| | - James R Lyons
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | - Jeong-Eun Lee
- Department of Astronomy and Space Science, School of Space Research, Kyung Hee University, Korea
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Denmark
| |
Collapse
|
21
|
Deng Z, Moynier F, Villeneuve J, Jensen NK, Liu D, Cartigny P, Mikouchi T, Siebert J, Agranier A, Chaussidon M, Bizzarro M. Early oxidation of the martian crust triggered by impacts. Sci Adv 2020; 6:6/44/eabc4941. [PMID: 33127679 PMCID: PMC7608801 DOI: 10.1126/sciadv.abc4941] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/27/2020] [Accepted: 09/10/2020] [Indexed: 05/26/2023]
Abstract
Despite the abundant geomorphological evidence for surface liquid water on Mars during the Noachian epoch (>3.7 billion years ago), attaining a warm climate to sustain liquid water on Mars at the period of the faint young Sun is a long-standing question. Here, we show that melts of ancient mafic clasts from a martian regolith meteorite, NWA 7533, experienced substantial Fe-Ti oxide fractionation. This implies early, impact-induced, oxidation events that increased by five to six orders of magnitude the oxygen fugacity of impact melts from remelting of the crust. Oxygen isotopic compositions of sequentially crystallized phases from the clasts show that progressive oxidation was due to interaction with an 17O-rich water reservoir. Such an early oxidation of the crust by impacts in the presence of water may have supplied greenhouse gas H2 that caused an increase in surface temperature in a CO2-thick atmosphere.
Collapse
Affiliation(s)
- Zhengbin Deng
- Université de Paris, Institut de physique du globe de Paris, CNRS, 75005 Paris, France.
| | - Frédéric Moynier
- Université de Paris, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Johan Villeneuve
- CRPG (UMR 7350) Université de Lorraine, CNRS, 7358 Vandoeuvre-lès-Nancy, France
| | - Ninna K Jensen
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Deze Liu
- Université de Paris, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Pierre Cartigny
- Université de Paris, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | | | - Julien Siebert
- Université de Paris, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Arnaud Agranier
- Laboratoire Géosciences Océan (UMR CNRS 6538), Université de Bretagne Occidentale et Institut Universitaire Européen de la Mer, Plouzané, France
| | - Marc Chaussidon
- Université de Paris, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Martin Bizzarro
- Université de Paris, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| |
Collapse
|
22
|
Merle RE, Nemchin AA, Whitehouse MJ, Snape JF, Kenny GG, Bellucci JJ, Connelly JN, Bizzarro M. Pb-Pb ages and initial Pb isotopic composition of lunar meteorites: NWA 773 clan, NWA 4734, and Dhofar 287. Meteorit Planet Sci 2020; 55:1808-1832. [PMID: 34376965 PMCID: PMC7611475 DOI: 10.1111/maps.13547] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/21/2019] [Accepted: 06/16/2020] [Indexed: 06/13/2023]
Abstract
Constraining the duration of magmatic activity on the Moon is essential to understand how the lunar mantle evolved chemically through time. Determining age and initial isotopic compositions of mafic lunar meteorites is a critical step in defining the periods of magmatic activity that occurred during the history of the Moon and to constrain the chemical characteristics of mantle components involved in the sources of the magmas. We have used the in situ Pb-Pb SIMS technique to investigate eight lunar gabbros and basalts, including six meteorites from the Northwest Africa (NWA) 773 clan (NWA 2727, NWA 2700, NWA 3333, NWA 2977, NWA 773, and NWA 3170), NWA 4734, and Dhofar 287A. These samples have been selected as there is no clear agreement on their age and they are all from the dominant low titanium chemical group. We have obtained ages of 2981 ± 12 Ma for NWA 4734 and 3208 ± 22 Ma for Dhofar 287. For the NWA 773 clan, four samples (the fine-grained basalt NWA 2727 and the three gabbros NWA 773, NWA 2977, NWA 3170) out of six yielded isochron-calculated ages that are identical within uncertainties and yielding an average age of 3086 ± 5 Ma. The age obtained for the fine-grained basalt NWA 2700 is not precise enough for comparison with the other samples. The gabbroic sample NWA 3333 yielded an age of 3038 ± 20 Ma suggesting that two distinct magmatic events may be recorded in the meteorites of the NWA 773 clan. The present study aims to identify and assess all potential issues that are associated with different ways to date lunar rocks using U-Pb-based methods. To achieve this, we have compared the new ages with the previously published data set. The entire age data set from lunar mafic meteorites was also screened to identify data showing analytical issues and evidence of resetting and terrestrial contamination. The data set combining the ages of mafic lunar meteorites and Apollo rocks suggests pulses of magmatic activity with two distinct phases between 3950 and 3575 Ma and between 3375 and 3075 Ma with the two phases separated by a gap of approximately 200 Ma. The evolution of the Pb initial ratios of the low-Ti mare basalts between approximately 3400 and 3100 Ma suggests that these rocks were progressively contaminated by a KREEP-like component.
Collapse
Affiliation(s)
- R. E. Merle
- Swedish Museum of Natural History, SE-104 05 Stockholm, Sweden
| | - A. A. Nemchin
- Swedish Museum of Natural History, SE-104 05 Stockholm, Sweden
- School of Earth and Planetary Sciences (EPS), Curtin University, GPO Box U1987, Perth, WA 6845, Australia
| | | | - J. F. Snape
- Faculty of Earth and Life Sciences, VU Amsterdam, De Boelelaan 1085,1081 HVAmsterdam, the Netherlands
| | - G. G. Kenny
- Swedish Museum of Natural History, SE-104 05 Stockholm, Sweden
| | - J. J. Bellucci
- Swedish Museum of Natural History, SE-104 05 Stockholm, Sweden
| | - J. N. Connelly
- Centre for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, DK-1350 Copenhagen, Denmark
| | - M. Bizzarro
- Centre for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, DK-1350 Copenhagen, Denmark
| |
Collapse
|
23
|
Larsen K, Wielandta D, Schillera M, Krot A, Bizzarro M. Episodic formation of refractory inclusions in the Solar System and their presolar heritage. Earth Planet Sci Lett 2020; 535:116088. [PMID: 34334802 PMCID: PMC7611424 DOI: 10.1016/j.epsl.2020.116088] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
Refractory inclusions [Ca-Al-rich Inclusions (CAIs) and Amoeboid Olivine Aggregates (AOAs)] in primitive meteorites are the oldest Solar System solids. They formed in the hot inner protoplanetary disk and, as such, provide insights into the earliest disk dynamics and physicochemical processing of the dust and gas that accreted to form the Sun and its planetary system. Using the short-lived 26Al to 26Mg decay system, we show that bulk refractory inclusions in CV (Vigarano-type) and CR (Renazzo-type) carbonaceous chondrites captured at least two distinct 26Al-rich (26Al/27Al ratios of ~5 × 10-5) populations of refractory inclusions characterized by different initial 26Mg/24Mg isotope compositions (μ26Mg*0). Another 26Al-poor CAI records an even larger μ26Mg*0 deficit. This suggests that formation of refractory inclusions was punctuated and recurrent, possibly associated with episodic outbursts from the accreting proto-Sun lasting as short as <8000 yr. Our results support a model in which refractory inclusions formed close to the hot proto-Sun and were subsequently redistributed to the outer disk, beyond the orbit of Jupiter, plausibly via stellar outflows with progressively decreasing transport efficiency. We show that the magnesium isotope signatures in refractory inclusions mirrors the presolar grain record, demonstrating a mutual exclusivity between 26Al enrichments and large nucleosynthetic Mg isotope effects. This suggests that refractory inclusions formed by incomplete thermal processing of presolar dust, thereby inheriting a diluted signature of their isotope systematics. As such, they record snapshots in the progressive sublimation of isotopically anomalous presolar carriers through selective thermal processing of young dust components from the proto-Solar molecular cloud. We infer that 26Al-rich refractory inclusions incorporated 26Al-rich dust which formed <5 Myr prior to our Sun, whereas 26Al-poor inclusions (such as FUN- and PLAC-type CAIs) incorporated >10 Myr old dust.
Collapse
Affiliation(s)
- K.K. Larsen
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
| | - D. Wielandta
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
| | - M. Schillera
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
| | - A.N. Krot
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
- Hawai’i Institute of Geophysics and Planetology, University of Hawai’i at Manoa, HI 96822, USA
| | - M. Bizzarro
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
| |
Collapse
|
24
|
van Kooten E, Cavalcante L, Wielandt D, Bizzarro M. The role of Bells in the continuous accretion between the CM and CR chondrite reservoirs. Meteorit Planet Sci 2020; 55:575-590. [PMID: 32362738 PMCID: PMC7188250 DOI: 10.1111/maps.13459] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 12/10/2018] [Accepted: 01/28/2020] [Indexed: 06/11/2023]
Abstract
CM meteorites are dominant members of carbonaceous chondrites (CCs), which evidently accreted in a region separated from the terrestrial planets. These chondrites are key in determining the accretion regions of solar system materials, since in Mg and Cr isotope space, they intersect between what are identified as inner and outer solar system reservoirs. In this model, the outer reservoir is represented by metal-rich carbonaceous chondrites (MRCCs), including CR chondrites. An important question remains whether the barrier between MRCCs and CCs was a temporal or spatial one. CM chondrites and chondrules are used here to identify the nature of the barrier as well as the timescale of chondrite parent body accretion. We find based on high precision Mg and Cr isotope data of seven CM chondrites and 12 chondrules, that accretion in the CM chondrite reservoir was continuous lasting <3 Myr and showing late accretion of MRCC-like material reflected by the anomalous CM chondrite Bells. We further argue that although MRCCs likely accreted later than CM chondrites, CR chondrules must have initially formed from a reservoir spatially separated from CM chondrules. Finally, we hypothesize on the nature of the spatial barrier separating these reservoirs.
Collapse
Affiliation(s)
- Elishevah van Kooten
- Institut de Physique du Globe de ParisUniversité de ParisCNRSUMR 71541 rue Jussieu75238ParisFrance
| | | | - Daniel Wielandt
- Centre for Star and Planet Formation and Natural History Museum of DenmarkUniversity of CopenhagenDK‐1350CopenhagenDenmark
| | - Martin Bizzarro
- Centre for Star and Planet Formation and Natural History Museum of DenmarkUniversity of CopenhagenDK‐1350CopenhagenDenmark
| |
Collapse
|
25
|
Schiller M, Bizzarro M, Siebert J. Iron isotope evidence for very rapid accretion and differentiation of the proto-Earth. Sci Adv 2020; 6:eaay7604. [PMID: 32095530 PMCID: PMC7015677 DOI: 10.1126/sciadv.aay7604] [Citation(s) in RCA: 11] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/16/2019] [Accepted: 11/26/2019] [Indexed: 06/02/2023]
Abstract
Nucleosynthetic isotope variability among solar system objects provides insights into the accretion history of terrestrial planets. We report on the nucleosynthetic Fe isotope composition (μ54Fe) of various meteorites and show that the only material matching the terrestrial composition is CI (Ivuna-type) carbonaceous chondrites, which represent the bulk solar system composition. All other meteorites, including carbonaceous, ordinary, and enstatite chondrites, record excesses in μ54Fe. This observation is inconsistent with protracted growth of Earth by stochastic collisional accretion, which predicts a μ54Fe value reflecting a mixture of the various meteorite parent bodies. Instead, our results suggest a rapid accretion and differentiation of Earth during the ~5-million year disk lifetime, when the volatile-rich CI-like material is accreted to the proto-Sun via the inner disk.
Collapse
Affiliation(s)
- Martin Schiller
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5–7, DK-1350 Copenhagen, Denmark
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5–7, DK-1350 Copenhagen, Denmark
- Institut de Physique du Globe de Paris, Université Sorbonne Paris Cité, 75005 Paris, France
| | - Julien Siebert
- Institut de Physique du Globe de Paris, Université Sorbonne Paris Cité, 75005 Paris, France
- Institut Universitaire de France, Paris, France
| |
Collapse
|
26
|
Jansen C, Brenker F, Krot A, Zipfel J, Pack A, Labenne L, Bizzarro M, Schiller M. MINERALOGY, PETROLOGY AND OXYGEN ISOTOPIC COMPOSITION OF NORTHWEST AFRICA (NWA) 12379, A NEW METAL-RICH CHONDRITE WITH AFFINITY TO ORDINARY CHONDRITES. Proc Lunar Planet Sci 2019; 50:2741. [PMID: 31631921 PMCID: PMC6800724 DOI: 10.1016/j.chemer.2019.125537] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Affiliation(s)
- C.A. Jansen
- Institute for Geosciences, Goethe University, Germany
| | - F.E. Brenker
- Institute for Geosciences, Goethe University, Germany
| | - A.N. Krot
- Institute for Geosciences, Goethe University, Germany
- Hawai’i Institute of Geophysics & Planetology, University of Hawai’i, Honolulu, USA
| | - J. Zipfel
- Senckenberg Forschungsinstitut & Naturmuseum, Germany
| | - A. Pack
- Georg-August-Universität, Göttingen, Germany
| | | | - M. Bizzarro
- Centre for Star & Planet Formation, Copen-hagen, Denmark
| | - M. Schiller
- Centre for Star & Planet Formation, Copen-hagen, Denmark
| |
Collapse
|
27
|
Saji N, Larsen K, Wielandt D, Schiller M, Costa M, Whitehouse M, Rosing M, Bizzarro M. Hadean geodynamics inferred from time-varying 142Nd/ 144Nd in the early Earth rock record. Geochem Perspect Lett 2018; 7:43-48. [PMID: 33073040 PMCID: PMC7116189 DOI: 10.7185/geochemlet.1818] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Indexed: 06/11/2023]
Abstract
Tracking the secular evolution of 142Nd/144Nd anomalies is important towards understanding the crust-mantle dynamics in the early Earth. Excessive scatter in the published data, however, precludes identifying the fine structure of 142Nd/144Nd evolution as the expected variability is on the order of few parts per million. We report ultra-high precision 142Nd/144Nd data for Eoarchean and Palaeoarchean rocks from the Isua Supracrustal Belt (SW Greenland) that show a well-resolved 142Nd/144Nd temporal variability suggesting progressive convective homogenisation of the Hadean Isua depleted mantle. This temporally decreasing 142Nd/144Nd signal provides a direct measure of early mantle dynamics, defining a stirring timescale of <250 Myr consistent with vigorous convective stirring in the early mantle. The 142Nd/144Nd evolution suggests protracted crustal residence times of ~1000-2000 Myr, inconsistent with modern-style plate tectonics in the Archean. In contrast, a stagnant-lid regime punctuated by episodes of mantle overturns accounts for the long life-time estimated here for the Hadean proto-crust.
Collapse
Affiliation(s)
- N.S. Saji
- Centre for Star and Planet Formation, University of Copenhagen,
Copenhagen, Denmark
| | - K. Larsen
- Centre for Star and Planet Formation, University of Copenhagen,
Copenhagen, Denmark
| | - D. Wielandt
- Centre for Star and Planet Formation, University of Copenhagen,
Copenhagen, Denmark
| | - M. Schiller
- Centre for Star and Planet Formation, University of Copenhagen,
Copenhagen, Denmark
| | - M.M. Costa
- Centre for Star and Planet Formation, University of Copenhagen,
Copenhagen, Denmark
| | | | - M.T. Rosing
- Natural History Museum of Denmark, University of Copenhagen,
Copenhagen, Denmark
| | - M. Bizzarro
- Centre for Star and Planet Formation, University of Copenhagen,
Copenhagen, Denmark
| |
Collapse
|
28
|
Bollard J, Connelly JN, Whitehouse MJ, Pringle EA, Bonal L, Jørgensen JK, Nordlund Å, Moynier F, Bizzarro M. Early formation of planetary building blocks inferred from Pb isotopic ages of chondrules. Sci Adv 2017; 3:e1700407. [PMID: 28808680 PMCID: PMC5550225 DOI: 10.1126/sciadv.1700407] [Citation(s) in RCA: 28] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/07/2017] [Accepted: 07/11/2017] [Indexed: 06/01/2023]
Abstract
The most abundant components of primitive meteorites (chondrites) are millimeter-sized glassy spherical chondrules formed by transient melting events in the solar protoplanetary disk. Using Pb-Pb dates of 22 individual chondrules, we show that primary production of chondrules in the early solar system was restricted to the first million years after the formation of the Sun and that these existing chondrules were recycled for the remaining lifetime of the protoplanetary disk. This finding is consistent with a primary chondrule formation episode during the early high-mass accretion phase of the protoplanetary disk that transitions into a longer period of chondrule reworking. An abundance of chondrules at early times provides the precursor material required to drive the efficient and rapid formation of planetary objects via chondrule accretion.
Collapse
Affiliation(s)
- Jean Bollard
- Centre for Star and Planet Formation, University of Copenhagen, Copenhagen, Denmark
| | - James N. Connelly
- Centre for Star and Planet Formation, University of Copenhagen, Copenhagen, Denmark
| | | | - Emily A. Pringle
- Institut de Physique du Globe de Paris, Université Paris Diderot, Sorbonne Paris Cité, Paris, France
| | - Lydie Bonal
- Institut de Planétologie et d’Astrophysique de Grenoble, Grenoble, France
| | - Jes K. Jørgensen
- Centre for Star and Planet Formation, University of Copenhagen, Copenhagen, Denmark
| | - Åke Nordlund
- Centre for Star and Planet Formation, University of Copenhagen, Copenhagen, Denmark
| | - Frédéric Moynier
- Institut de Physique du Globe de Paris, Université Paris Diderot, Sorbonne Paris Cité, Paris, France
| | - Martin Bizzarro
- Centre for Star and Planet Formation, University of Copenhagen, Copenhagen, Denmark
- Institut de Physique du Globe de Paris, Université Paris Diderot, Sorbonne Paris Cité, Paris, France
| |
Collapse
|
29
|
Olsen MB, Wielandt D, Schiller M, Van Kooten EM, Bizzarro M. Magnesium and 54Cr isotope compositions of carbonaceous chondrite chondrules - Insights into early disk processes. Geochim Cosmochim Acta 2016; 191:118-138. [PMID: 27563152 PMCID: PMC4993235 DOI: 10.1016/j.gca.2016.07.011] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/08/2023]
Abstract
We report on the petrology, magnesium isotopes and mass-independent 54Cr/52Cr compositions (μ54Cr) of 42 chondrules from CV (Vigarano and NWA 3118) and CR (NWA 6043, NWA 801 and LAP 02342) chondrites. All sampled chondrules are classified as type IA or type IAB, have low 27Al/24Mg ratios (0.04-0.27) and display little or no evidence for secondary alteration processes. The CV and CR chondrules show variable 25Mg/24Mg and 26Mg/24Mg values corresponding to a range of mass-dependent fractionation of ~500 ppm (parts per million) per atomic mass unit. This mass-dependent Mg isotope fractionation is interpreted as reflecting Mg isotope heterogeneity of the chondrule precursors and not the result of secondary alteration or volatility-controlled processes during chondrule formation. The CV and CR chondrule populations studied here are characterized by systematic deficits in the mass-independent component of 26Mg (μ26Mg*) relative to the solar value defined by CI chondrites, which we interpret as reflecting formation from precursor material with a reduced initial abundance of 26Al compared to the canonical 26Al/27Al of ~5 × 10-5. Model initial 26Al/27Al values of CV and CR chondrules vary from (1.5 ± 4.0) × 10-6 to (2.2 ± 0.4) × 10-5. The CV chondrules display significant μ54Cr variability, defining a range of compositions that is comparable to that observed for inner Solar System primitive and differentiated meteorites. In contrast, CR chondrites are characterized by a narrower range of μ54Cr values restricted to compositions typically observed for bulk carbonaceous chondrites. Collectively, these observations suggest that the CV chondrules formed from precursors that originated in various regions of the protoplanetary disk and were then transported to the accretion region of the CV parent asteroid whereas CR chondrule predominantly formed from precursor with carbonaceous chondrite-like μ54Cr signatures. The observed μ54Cr variability in chondrules from CV and CR chondrites suggest that the matrix and chondrules did not necessarily formed from the same reservoir. The coupled μ26Mg* and μ54Cr systematics of CR chondrules establishes that these objects formed from a thermally unprocessed and 26Al-poor source reservoir distinct from most inner Solar System asteroids and planetary bodies, possibly located beyond the orbits of the gas giants. In contrast, a large fraction of the CV chondrules plot on the inner Solar System correlation line, indicating that these objects predominantly formed from thermally-processed, 26Al-bearing precursor material akin to that of inner Solar System solids, asteroids and planets.
Collapse
Affiliation(s)
- Mia B. Olsen
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, DK-1350, Denmark
| | - Daniel Wielandt
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, DK-1350, Denmark
| | - Martin Schiller
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, DK-1350, Denmark
| | - Elishevah M.M.E. Van Kooten
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, DK-1350, Denmark
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, DK-1350, Denmark
| |
Collapse
|
30
|
Saji NS, Wielandt D, Paton C, Bizzarro M. Ultra-high-precision Nd-isotope measurements of geological materials by MC-ICPMS. J Anal At Spectrom 2016; 31:1490-1504. [PMID: 27429505 PMCID: PMC4946631 DOI: 10.1039/c6ja00064a] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/06/2023]
Abstract
We report novel techniques allowing the measurement of Nd-isotope ratios with unprecedented accuracy and precision by multi-collector inductively coupled plasma mass spectrometry. Using the new protocol, we have measured the Nd-isotopic composition of rock and synthetic Nd standards as well as that of the Allende carbonaceous chondrite. Analyses of BCR-2, BHVO-2 and GSP-2 rock standards yield mass-independent compositions identical to the JNdi-1 Nd-reference standard, with an external reproducibility of 2.4, 1.6, 1.6 and 3.5 ppm respectively, on μ142Nd, μ145Nd, μ146Nd and μ150Nd (μ representing the ppm-deviation of the ratios from JNdi-1) using 148Nd/144Nd for internal normalization. This represents an improvement in precision by a factor of 2, 7 and 9 respectively for μ142Nd, μ145Nd and μ150Nd. Near-quantitative recovery from purification chemistry and sample-standard bracketing allow for the determination of mass-dependent Nd-isotopic composition of samples. Synthetic standards, namely La Jolla and AMES, record mass-dependent variability of up to 1.2 ε per atomic mass unit and mass-independent compositions resolvable by up to 3 ppm for μ142Nd and 8 ppm for μ150Nd, relative to JNdi-1. The mass-independent compositions are consistent with equilibrium mass fractionation during purification. The terrestrial rock standards define a uniform stable ε145Nd of -0.24 ± 0.19 (2SD) relative to JNdi-1, indistinguishable from the mean Allende ε145Nd of -0.19 ± 0.09. We consider this value to represent the mass-dependent Nd-isotope composition of Bulk Silicate Earth (BSE). The modest mass-dependent fractionation of JNdi-1 relative to BSE results in potential effects on mass-independent composition that cannot be resolved within the reproducibility of our analyses when correcting for natural and instrumental mass fractionation by kinetic law, making it a suitable reference standard for analysis of unknowns. Analysis of Allende (CV3) carbonaceous chondrite returns an average μ142Nd deficit of -30.1 ± 3.7 ppm in agreement with previous studies. The apparent deficit is, however, lowered to -23.8 ± 4.0 ppm while normalizing to 148Nd/144Nd instead of 146Nd/144Nd. We interpret this as the effect of a possible nucleosynthetic anomaly of -6.3 ± 0.5 ppm in μ146Nd. As 142Nd and 146Nd are both s-process-dominated nuclides, this hints at the possibility that terrestrial μ142Nd excess may not reflect 146Sm decay as widely accepted.
Collapse
Affiliation(s)
- Nikitha Susan Saji
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350, Copenhagen, Denmark
| | - Daniel Wielandt
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350, Copenhagen, Denmark
| | - Chad Paton
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350, Copenhagen, Denmark
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350, Copenhagen, Denmark
| |
Collapse
|
31
|
Larsen K, Schiller M, Bizzarro M. Accretion timescales and style of asteroidal differentiation in an 26Al-poor protoplanetary disk. Geochim Cosmochim Acta 2016; 176:295-315. [PMID: 27445415 PMCID: PMC4950964 DOI: 10.1016/j.gca.2015.10.036] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/24/2023]
Abstract
The decay of radioactive 26Al to 26Mg (half-life of 730,000 years) is postulated to have been the main energy source promoting asteroidal melting and differentiation in the nascent solar system. High-resolution chronological information provided by the 26Al-26Mg decay system is, therefore, intrinsically linked to the thermal evolution of early-formed planetesimals. In this paper, we explore the timing and style of asteroidal differentiation by combining high-precision Mg isotope measurements of meteorites with thermal evolution models for planetesimals. In detail, we report Mg isotope data for a suite of olivine-rich [Al/Mg ~ 0] achondritic meteorites, as well as a few chondrites. Main Group, pyroxene and the Zinder pallasites as well as the lodranite all record deficits in the mass-independent component of μ26Mg (μ26Mg*) relative to chondrites and Earth. This isotope signal is expected for the retarded ingrowth of radiogenic 26Mg* in olivine-rich residues produced through partial silicate melting during 26Al decay and consistent with their marginally heavy Mg isotope composition relative to ordinary chondrites, which may reflect the early extraction of isotopically light partial melts from the source rock. We propose that their parent planetesimals started forming within ~250,000 years of solar system formation from a hot (>~500 K) inner protoplanetary disk region characterized by a reduced initial (26Al/27Al)0 abundance (~1-2 × 10-5) relative to the (26Al/27Al)0 value in CAIs of 5.25 × 10-5. This effectively reduced the total heat production and allowed for the preservation of solid residues produced through progressive silicate melting with depth within the planetesimals. These 'non-carbonaceous' planetesimals acquired their mass throughout an extended period (>3 Myr) of continuous accretion, thereby generating onion-shell structures of incompletely differentiated zones, consisting of olivine-rich residues, overlaid by metachondrites and undifferentiated chondritic crusts. In contrast, individual olivine crystals from Eagle Station pallasites record variable μ26Mg* excesses, suggesting that these crystals captured the 26Mg* evolution of a magmatic reservoir controlled by fractional crystallization processes during the lifespan of 26Al. Similar to previous suggestions based on isotopic evidence, we suggest that Eagle Station pallasites formed from precursor material similar in composition to carbonaceous chondrites from a cool outer protoplanetary disk region characterized by (26Al/27Al)0 ≥ 2.7 × 10-5. Protracted planetesimal accretion timescales at large orbital distances, with onset of accretion 0.3-1 Myr post-CAIs, may have resulted in significant radiative heat loss and thus efficient early interior cooling of slowly accreting 'carbonaceous' planetesimals.
Collapse
|
32
|
Holst JC, Paton C, Wielandt D, Bizzarro M. Tungsten isotopes in bulk meteorites and their inclusions-Implications for processing of presolar components in the solar protoplanetary disk. Meteorit Planet Sci 2015; 50:1643-1660. [PMID: 27445452 PMCID: PMC4950963 DOI: 10.1111/maps.12488] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/06/2023]
Abstract
We present high precision, low- and high-resolution tungsten isotope measurements of iron meteorites Cape York (IIIAB), Rhine Villa (IIIE), Bendego (IC), and the IVB iron meteorites Tlacotepec, Skookum, and Weaver Mountains, as well as CI chondrite Ivuna, a CV3 chondrite refractory inclusion (CAI BE), and terrestrial standards. Our high precision tungsten isotope data show that the distribution of the rare p-process nuclide 180W is homogeneous among chondrites, iron meteorites, and the refractory inclusion. One exception to this pattern is the IVB iron meteorite group, which displays variable excesses relative to the terrestrial standard, possibly related to decay of rare 184Os. Such anomalies are not the result of analytical artifacts and cannot be caused by sampling of a protoplanetary disk characterized by p-process isotope heterogeneity. In contrast, we find that 183W is variable due to a nucleosynthetic s-process deficit/r-process excess among chondrites and iron meteorites. This variability supports the widespread nucleosynthetic s/r-process heterogeneity in the protoplanetary disk inferred from other isotope systems and we show that W and Ni isotope variability is correlated. Correlated isotope heterogeneity for elements of distinct nucleosynthetic origin (183W and 58Ni) is best explained by thermal processing in the protoplanetary disk during which thermally labile carrier phases are unmixed by vaporization thereby imparting isotope anomalies on the residual processed reservoir.
Collapse
|
33
|
Bollard J, Connelly JN, Bizzarro M. Pb-Pb dating of individual chondrules from the CB a chondrite Gujba: Assessment of the impact plume formation model. Meteorit Planet Sci 2015; 50:1197-1216. [PMID: 27429545 PMCID: PMC4946626 DOI: 10.1111/maps.12461] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/08/2023]
Abstract
The CB chondrites are metal-rich meteorites with characteristics that sharply distinguish them from other chondrite groups. Their unusual chemical and petrologic features and a young formation age of bulk chondrules dated from the CBa chondrite Gujba are interpreted to reflect a single-stage impact origin. Here, we report high-precision internal isochrons for four individual chondrules of the Gujba chondrite to probe the formation history of CB chondrites and evaluate the concordancy of relevant short-lived radionuclide chronometers. All four chondrules define a brief formation interval with a weighted mean age of 4562.49 ± 0.21 Myr, consistent with its origin from the vapor-melt impact plume generated by colliding planetesimals. Formation in a debris disk mostly devoid of nebular gas and dust sets an upper limit for the solar protoplanetary disk lifetime at 4.8 ± 0.3 Myr. Finally, given the well-behaved Pb-Pb systematics of all four chondrules, a precise formation age and the concordancy of the Mn-Cr, Hf-W, and I-Xe short-lived radionuclide relative chronometers, we propose that Gujba may serve as a suitable time anchor for these systems.
Collapse
Affiliation(s)
- Jean Bollard
- Centre for Star and Planet Formation, Natural History Museum of Denmark, DK-1350 Copenhagen, Denmark
| | - James N. Connelly
- Centre for Star and Planet Formation, Natural History Museum of Denmark, DK-1350 Copenhagen, Denmark
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Natural History Museum of Denmark, DK-1350 Copenhagen, Denmark
| |
Collapse
|
34
|
Schiller M, Connelly JN, Glad AC, Mikouchi T, Bizzarro M. Early accretion of protoplanets inferred from a reduced inner solar system 26Al inventory. Earth Planet Sci Lett 2015; 420:45-54. [PMID: 27429474 PMCID: PMC4946628 DOI: 10.1016/j.epsl.2015.03.028] [Citation(s) in RCA: 25] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/08/2023]
Abstract
The mechanisms and timescales of accretion of 10-1000 km sized planetesimals, the building blocks of planets, are not yet well understood. With planetesimal melting predominantly driven by the decay of the short-lived radionuclide 26Al (26Al→26Mg; t1/2 = 0.73 Ma), its initial abundance determines the permissible timeframe of planetesimal-scale melting and its subsequent cooling history. Currently, precise knowledge about the initial 26Al abundance [(26Al/27Al)0] exists only for the oldest known solids, calcium aluminum-rich inclusions (CAIs) - the so-called canonical value. We have determined the 26Al/27Al of three angrite meteorites, D'Orbigny, Sahara 99555 and NWA 1670, at their time of crystallization, which corresponds to (3.98 ± 0.15)×10-7, (3.64 ± 0.18)×10-7, and (5.92 ± 0.59)×10-7, respectively. Combined with a newly determined absolute U-corrected Pb-Pb age for NWA 1670 of 4564.39 ± 0.24 Ma and published U-corrected Pb-Pb ages for the other two angrites, this allows us to calculate an initial (26Al/27Al)0 of [Formula: see text] for the angrite parent body (APB) precursor material at the time of CAI formation, a value four times lower than the accepted canonical value of 5.25 × 10-5. Based on their similar 54Cr/52Cr ratios, most inner solar system materials likely accreted from material containing a similar 26Al/27Al ratio as the APB precursor at the time of CAI formation. To satisfy the abundant evidence for widespread planetesimal differentiation, the subcanonical 26Al budget requires that differentiated planetesimals, and hence protoplanets, accreted rapidly within 0.25 ± 0.15 Ma of the formation of canonical CAIs.
Collapse
Affiliation(s)
- Martin Schiller
- Centre for Star and Planet Formation, University of Copenhagen, Øster Voldgade 5-7, DK-1350, Denmark
- Corresponding author. (M. Schiller)
| | - James N. Connelly
- Centre for Star and Planet Formation, University of Copenhagen, Øster Voldgade 5-7, DK-1350, Denmark
| | - Aslaug C. Glad
- Centre for Star and Planet Formation, University of Copenhagen, Øster Voldgade 5-7, DK-1350, Denmark
| | - Takashi Mikouchi
- Department of Earth & Planetary Science, University of Tokyo, Tokyo, Japan
| | - Martin Bizzarro
- Centre for Star and Planet Formation, University of Copenhagen, Øster Voldgade 5-7, DK-1350, Denmark
| |
Collapse
|
35
|
Johansen A, Low MMM, Lacerda P, Bizzarro M. Growth of asteroids, planetary embryos, and Kuiper belt objects by chondrule accretion. Sci Adv 2015; 1:e1500109. [PMID: 26601169 PMCID: PMC4640629 DOI: 10.1126/sciadv.1500109] [Citation(s) in RCA: 39] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/27/2015] [Accepted: 03/15/2015] [Indexed: 05/06/2023]
Abstract
Chondrules are millimeter-sized spherules that dominate primitive meteorites (chondrites) originating from the asteroid belt. The incorporation of chondrules into asteroidal bodies must be an important step in planet formation, but the mechanism is not understood. We show that the main growth of asteroids can result from gas drag-assisted accretion of chondrules. The largest planetesimals of a population with a characteristic radius of 100 km undergo runaway accretion of chondrules within ~3 My, forming planetary embryos up to Mars's size along with smaller asteroids whose size distribution matches that of main belt asteroids. The aerodynamical accretion leads to size sorting of chondrules consistent with chondrites. Accretion of millimeter-sized chondrules and ice particles drives the growth of planetesimals beyond the ice line as well, but the growth time increases above the disc lifetime outside of 25 AU. The contribution of direct planetesimal accretion to the growth of both asteroids and Kuiper belt objects is minor. In contrast, planetesimal accretion and chondrule accretion play more equal roles in the formation of Moon-sized embryos in the terrestrial planet formation region. These embryos are isolated from each other and accrete planetesimals only at a low rate. However, the continued accretion of chondrules destabilizes the oligarchic configuration and leads to the formation of Mars-sized embryos and terrestrial planets by a combination of direct chondrule accretion and giant impacts.
Collapse
Affiliation(s)
- Anders Johansen
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 22100 Lund, Sweden
- Corresponding author. E-mail:
| | - Mordecai-Mark Mac Low
- Department of Astrophysics, American Museum of Natural History, 79th Street at Central Park West, New York, NY 10024–5192, USA
| | - Pedro Lacerda
- Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Martin Bizzarro
- Centre for Star and Planet Formation and Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
| |
Collapse
|
36
|
Schiller M, Paton C, Bizzarro M. Evidence for nucleosynthetic enrichment of the protosolar molecular cloud core by multiple supernova events. Geochim Cosmochim Acta 2015; 149:88-102. [PMID: 25684790 PMCID: PMC4326683 DOI: 10.1016/j.gca.2014.11.005] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/13/2023]
Abstract
The presence of isotope heterogeneity of nucleosynthetic origin amongst meteorites and their components provides a record of the diverse stars that contributed matter to the protosolar molecular cloud core. Understanding how and when the solar system's nucleosynthetic heterogeneity was established and preserved within the solar protoplanetary disk is critical for unraveling the earliest formative stages of the solar system. Here, we report calcium and magnesium isotope measurements of primitive and differentiated meteorites as well as various types of refractory inclusions, including refractory inclusions (CAIs) formed with the canonical 26Al/27Al of ~5 × 10-5 (26Al decays to 26Mg with a half-life of ~0.73 Ma) and CAIs that show fractionated and unidentified nuclear effects (FUN-CAIs) to understand the origin of the solar system's nucleosynthetic heterogeneity. Bulk analyses of primitive and differentiated meteorites along with canonical and FUN-CAIs define correlated, mass-independent variations in 43Ca, 46Ca and 48Ca. Moreover, sequential dissolution experiments of the Ivuna carbonaceous chondrite aimed at identifying the nature and number of presolar carriers of isotope anomalies within primitive meteorites have detected the presence of multiple carriers of the short-lived 26Al nuclide as well as carriers of anomalous and uncorrelated 43Ca, 46Ca and 48Ca compositions, which requires input from multiple and recent supernovae sources. We infer that the solar system's correlated nucleosynthetic variability reflects unmixing of old, galactically-inherited homogeneous dust from a new, supernovae-derived dust component formed shortly prior to or during the evolution of the giant molecular cloud parental to the protosolar molecular cloud core. This implies that similarly to 43Ca, 46Ca and 48Ca, the short-lived 26Al nuclide was heterogeneously distributed in the inner solar system at the time of CAI formation.
Collapse
|
37
|
Abstract
CONTEXT The terrestrial planets, comets, and meteorites are significantly enriched in 15N compared to the Sun and Jupiter. While the solar and jovian nitrogen isotope ratio is believed to represent the composition of the protosolar nebula, a still unidentified process has caused 15N-enrichment in the solids. Several mechanisms have been proposed to explain the variations, including chemical fractionation. However, observational results that constrain the fractionation models are scarce. While there is evidence of 15N-enrichment in prestellar cores, it is unclear how the signature evolves into the protostellar phases. AIMS The aim of this study is to measure the 14N/15N ratio around three nearby, embedded low- to intermediate-mass protostars. METHODS Isotopologues of HCN and HNC were used to probe the 14N/15N ratio. A selection of J = 3-2 and 4-3 transitions of H13CN, HC15N, HN13C, and H15NC was observed with the Atacama Pathfinder EXperiment telescope (APEX). The 14N/15N ratios were derived from the integrated intensities assuming a standard 12C/13C ratio. The assumption of optically thin emission was verified using radiative transfer modeling and hyperfine structure fitting. RESULTS Two sources, IRAS 16293A and R CrA IRS7B, show 15N-enrichment by a factor of ~1.5-2.5 in both HCN and HNC with respect to the solar composition. IRAS 16293A falls in the range of typical prestellar core values. Solar composition cannot be excluded for the third source, OMC-3 MMS6. Furthermore, there are indications of a trend toward increasing 14N/15N ratios with increasing outer envelope temperature. CONCLUSIONS The enhanced 15N abundances in HCN and HNC found in two Class 0 sources (14N/15N ~ 160-290) and the tentative trend toward a temperature-dependent 14N/15N ratio are consistent with the chemical fractionation scenario, but 14N/15N ratios from additional tracers are indispensable for testing the models. Spatially resolved observations are needed to distinguish between chemical fractionation and isotope-selective photochemistry.
Collapse
Affiliation(s)
- S F Wampfler
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, 1350 København K, Denmark ; Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 København Ø, Denmark
| | - J K Jørgensen
- Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 København Ø, Denmark ; Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, 1350 København K, Denmark
| | - M Bizzarro
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, 1350 København K, Denmark
| | - S E Bisschop
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, 1350 København K, Denmark ; Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 København Ø, Denmark
| |
Collapse
|
38
|
Dahl TW, Boyle RA, Canfield DE, Connelly JN, Gill BC, Lenton TM, Bizzarro M. Uranium isotopes distinguish two geochemically distinct stages during the later Cambrian SPICE event. Earth Planet Sci Lett 2014; 401:313-326. [PMID: 25684783 PMCID: PMC4326682 DOI: 10.1016/j.epsl.2014.05.043] [Citation(s) in RCA: 11] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
Anoxic marine zones were common in early Paleozoic oceans (542-400 Ma), and present a potential link to atmospheric pO2 via feedbacks linking global marine phosphorous recycling, primary production and organic carbon burial. Uranium (U) isotopes in carbonate rocks track the extent of ocean anoxia, whereas carbon (C) and sulfur (S) isotopes track the burial of organic carbon and pyrite sulfur (primary long-term sources of atmospheric oxygen). In combination, these proxies therefore reveal the comparative dynamics of ocean anoxia and oxygen liberation to the atmosphere over million-year time scales. Here we report high-precision uranium isotopic data in marine carbonates deposited during the Late Cambrian 'SPICE' event, at ca. 499 Ma, documenting a well-defined -0.18‰ negative δ238U excursion that occurs at the onset of the SPICE event's positive δ13C and δ34S excursions, but peaks (and tails off) before them. Dynamic modelling shows that the different response of the U reservoir cannot be attributed solely to differences in residence times or reservoir sizes - suggesting that two chemically distinct ocean states occurred within the SPICE event. The first ocean stage involved a global expansion of euxinic waters, triggering the spike in U burial, and peaking in conjunction with a well-known trilobite extinction event. During the second stage widespread euxinia waned, causing U removal to tail off, but enhanced organic carbon and pyrite burial continued, coinciding with evidence for severe sulfate depletion in the oceans (Gill et al., 2011). We discuss scenarios for how an interval of elevated pyrite and organic carbon burial could have been sustained without widespread euxinia in the water column (both non-sulfidic anoxia and/or a more oxygenated ocean state are possibilities). Either way, the SPICE event encompasses two different stages of elevated organic carbon and pyrite burial maintained by high nutrient fluxes to the ocean, and potentially sustained by internal marine geochemical feedbacks.
Collapse
Affiliation(s)
- Tais W. Dahl
- Nordic Center for Earth Evolution (NordCEE) and Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen K, Denmark
| | - Richard A. Boyle
- College of Life and Environmental Sciences, University of Exeter, Exeter, UK
- Nordic Center for Earth Evolution (NordCEE) and University of Southern Denmark, Odense, Denmark
| | - Donald E. Canfield
- Nordic Center for Earth Evolution (NordCEE) and University of Southern Denmark, Odense, Denmark
| | - James N. Connelly
- Centre for Star and Planet Formation (StarPlan) and Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen K, Denmark
| | - Benjamin C. Gill
- Department of Geosciences, Virginia Polytechnic Institute and State University, Blacksburg, VA 24061, USA
| | - Timothy M. Lenton
- College of Life and Environmental Sciences, University of Exeter, Exeter, UK
| | - Martin Bizzarro
- Centre for Star and Planet Formation (StarPlan) and Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen K, Denmark
| |
Collapse
|
39
|
Affiliation(s)
- Martin Bizzarro
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark.
| |
Collapse
|
40
|
Schiller M, Van Kooten E, Holst JC, Olsen MB, Bizzarro M. Precise measurement of chromium isotopes by MC-ICPMS. J Anal At Spectrom 2014; 29:1406-1416. [PMID: 25071300 PMCID: PMC4110669 DOI: 10.1039/c4ja00018h] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/13/2023]
Abstract
We report novel analytical procedures allowing for the concurrent determination of the stable and mass-independent Cr isotopic composition of silicate materials by multiple collector inductively coupled mass spectrometry (MC-ICPMS). In particular, we focus on improved precision of the measurement of the neutron-rich isotope 54Cr. Because nitride and oxide interferences are a major obstacle to precise and accurate 54Cr measurements by MC-ICPMS, our approach is designed to minimize these interferences. Based on repeat measurements of standards, we show that the mass-independent 53Cr and 54Cr compositions can be routinely determined with an external reproducibility better than 2.5 and 5.8 ppm (2 sd), respectively. This represents at least a two-fold improvement compared to previous studies. Although this approach uses significantly more Cr (30-60 μg) than analysis by thermal ionization mass spectrometry (TIMS), our result indicate that it is possible to obtain an external reproducibility of 19 ppm for the μ54Cr when consuming amounts similar to that typically analyzed by TIMS (1 μg). In addition, the amount of time required for analysis by MC-ICPMS is much shorter thereby enabling a higher sample throughput. As a result of the improved analytical precision, we identified small apparent mass-independent differences between different synthetic Cr standards and bulk silicate Earth (BSE) when using the kinetic law for the mass bias correction. These differences are attributed to the Cr loss by equilibrium processes during production of the synthetic standards. The stable isotope data concurrently obtained have a precision of 0.05‰ Da -1, which is comparable to earlier studies. Comparison of the measured isotopic composition of four meteorites with published data indicates that Cr isotope data measured by the technique described here are accurate to stated uncertainties. The stable Cr composition of the Bilanga and NWA 2999 achondrites suggests that the differences in the stable Cr isotope composition of Earth and chondrites may reflect heterogeneity of their precursor material rather than Cr isotope fractionation during metal-silicate segregation of Earth. Lastly, a step wise dissolution experiment of the CI chondrite Ivuna reveals previously unknown carriers of large mass-dependent Cr stable isotope variations that co-vary with the known presence of carriers of large nucleosynthetic anomalies, demonstrating one advantage of this technique.
Collapse
Affiliation(s)
- Martin Schiller
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350, Copenhagen, Denmark
| | - Elishevah Van Kooten
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350, Copenhagen, Denmark
| | - Jesper C. Holst
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350, Copenhagen, Denmark
| | - Mia B. Olsen
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350, Copenhagen, Denmark
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350, Copenhagen, Denmark
| |
Collapse
|
41
|
Buchhave LA, Bizzarro M, Latham DW, Sasselov D, Cochran WD, Endl M, Isaacson H, Juncher D, Marcy GW. Three regimes of extrasolar planet radius inferred from host star metallicities. Nature 2014; 509:593-5. [PMID: 24870544 PMCID: PMC4048851 DOI: 10.1038/nature13254] [Citation(s) in RCA: 210] [Impact Index Per Article: 21.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/21/2013] [Accepted: 03/12/2014] [Indexed: 11/08/2022]
Abstract
Approximately half of the extrasolar planets (exoplanets) with radii less than four Earth radii are in orbits with short periods. Despite their sheer abundance, the compositions of such planets are largely unknown. The available evidence suggests that they range in composition from small, high-density rocky planets to low-density planets consisting of rocky cores surrounded by thick hydrogen and helium gas envelopes. Here we report the metallicities (that is, the abundances of elements heavier than hydrogen and helium) of more than 400 stars hosting 600 exoplanet candidates, and find that the exoplanets can be categorized into three populations defined by statistically distinct (∼4.5σ) metallicity regions. We interpret these regions as reflecting the formation regimes of terrestrial-like planets (radii less than 1.7 Earth radii), gas dwarf planets with rocky cores and hydrogen-helium envelopes (radii between 1.7 and 3.9 Earth radii) and ice or gas giant planets (radii greater than 3.9 Earth radii). These transitions correspond well with those inferred from dynamical mass estimates, implying that host star metallicity, which is a proxy for the initial solids inventory of the protoplanetary disk, is a key ingredient regulating the structure of planetary systems.
Collapse
Affiliation(s)
- Lars A Buchhave
- 1] Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA [2] Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark
| | - David W Latham
- Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA
| | - Dimitar Sasselov
- Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA
| | - William D Cochran
- McDonald Observatory, The University of Texas, Austin, Texas 78712, USA
| | - Michael Endl
- McDonald Observatory, The University of Texas, Austin, Texas 78712, USA
| | | | - Diana Juncher
- 1] Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark [2] Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark
| | | |
Collapse
|
42
|
Creech J, Baker J, Handler M, Bizzarro M. Platinum stable isotope analysis of geological standard reference materials by double-spike MC-ICPMS. Chem Geol 2014; 363:293-300. [PMID: 25684781 PMCID: PMC4326679 DOI: 10.1016/j.chemgeo.2013.11.009] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/21/2023]
Abstract
We report a method for the chemical purification of Pt from geological materials by ion-exchange chromatography for subsequent Pt stable isotope analysis by multiple-collector inductively coupled plasma mass spectrometry (MC-ICPMS) using a 196Pt-198Pt double-spike to correct for instrumental mass bias. Double-spiking of samples was carried out prior to digestion and chemical separation to correct for any mass-dependent fractionation that may occur due to incomplete recovery of Pt. Samples were digested using a NiS fire assay method, which pre-concentrates Pt into a metallic bead that is readily dissolved in acid in preparation for anion-exchange chemistry. Pt was recovered from anion-exchange resin in concentrated HNO3 acid after elution of matrix elements, including the other platinum group elements (PGE), in dilute HCl and HNO3 acids. The separation method has been calibrated using a precious metal standard solution doped with a range of synthetic matrices and results in Pt yields of ≥90% with purity of ≥95%. Using this chemical separation technique, we have separated Pt from 11 international geological standard reference materials comprising of PGE ores, mantle rocks, igneous rocks and one sample from the Cretaceous-Paleogene boundary layer. Pt concentrations in these samples range from ca. 5 ng g-1 to 4 μg g-1. This analytical method has been shown to have an external reproducibility on δ198Pt (permil difference in the 198Pt/194Pt ratio from the IRMM-010 standard) of ±0.040 (2 sd) on Pt solution standards (Creech et al., 2013, J. Anal. At. Spectrom. 28, 853-865). The reproducibility in natural samples is evaluated by processing multiple replicates of four standard reference materials, and is conservatively taken to be ca. ±0.088 (2 sd). Pt stable isotope data for the full set of reference materials have a range of δ198Pt values with offsets of up to 0.4‰ from the IRMM-010 standard, which are readily resolved with this technique. These results demonstrate the potential of the Pt isotope system as a tracer in geochemical systems.
Collapse
Affiliation(s)
- J.B. Creech
- School of Geography, Environment and Earth Sciences, Victoria University of Wellington, P.O. Box 600, Wellington, New Zealand
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark
- Corresponding author. Fax: +64 4 463 5186. (J.B. Creech)
| | - J.A. Baker
- School of Environment, The University of Auckland, Private Bag 92019, Auckland, New Zealand
| | - M.R. Handler
- School of Geography, Environment and Earth Sciences, Victoria University of Wellington, P.O. Box 600, Wellington, New Zealand
| | - M. Bizzarro
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark
| |
Collapse
|
43
|
Connelly JN, Bizzarro M, Krot AN, Nordlund Å, Wielandt D, Ivanova MA. The absolute chronology and thermal processing of solids in the solar protoplanetary disk. Science 2012; 338:651-5. [PMID: 23118187 DOI: 10.1126/science.1226919] [Citation(s) in RCA: 105] [Impact Index Per Article: 8.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
Abstract
Transient heating events that formed calcium-aluminum-rich inclusions (CAIs) and chondrules are fundamental processes in the evolution of the solar protoplanetary disk, but their chronology is not understood. Using U-corrected Pb-Pb dating, we determined absolute ages of individual CAIs and chondrules from primitive meteorites. CAIs define a brief formation interval corresponding to an age of 4567.30 ± 0.16 million years (My), whereas chondrule ages range from 4567.32 ± 0.42 to 4564.71 ± 0.30 My. These data refute the long-held view of an age gap between CAIs and chondrules and, instead, indicate that chondrule formation started contemporaneously with CAIs and lasted ~3 My. This time scale is similar to disk lifetimes inferred from astronomical observations, suggesting that the formation of CAIs and chondrules reflects a process intrinsically linked to the secular evolution of accretionary disks.
Collapse
Affiliation(s)
- James N Connelly
- Centre for Star and Planet Formation and Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark.
| | | | | | | | | | | |
Collapse
|
44
|
Fejerskov O, Guldager Bilde P, Bizzarro M, Connelly JN, Skovhus Thomsen J, Nyvad B. Dental caries in Rome, 50-100 AD. Caries Res 2012; 46:467-73. [PMID: 22796661 DOI: 10.1159/000339664] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/09/2012] [Accepted: 05/21/2012] [Indexed: 11/19/2022] Open
Abstract
Scarce information exists on the clinical features of dental caries in the Imperial Roman population and no structural data on caries lesions from this period have so far been published. We report on the findings of 86 teeth (50-100 AD) found during archaeological excavations of the temple of Castor and Pollux in the Forum Romanum. We found that nearly all teeth had large carious cavities extending into the pulp. The distribution and size of the caries lesions were similar to those found in contemporary adult populations in Africa and China living without access to dental care. Most lesions had a hypermineralized zone in the dentin at the advancing front of the carious cavities as revealed by micro-computed tomography. This biological dentin reaction combined with the morphology of the cavities might indicate that some temporary topical pain relief and intervention treatment slowed down the rate of lesion progression. This is indirectly supported by examination of cavities of similar size and depth from a contemporary population without access to dental health care. In contrast to the lesions in the Roman teeth, these lesions did not exhibit a hypermineralized dentin reaction. We investigated whether the Pb isotopic composition of enamel and/or dentin of a single tooth matched that of a sample of an ancient Forum water lead pipe. The Pb isotopic composition of the tooth did not match that of the tube, suggesting that the subjects were exposed to different Pb sources during their lifetime other than the lead tubes.
Collapse
Affiliation(s)
- O Fejerskov
- Department of Biomedicine-Anatomy, Aarhus University, Aarhus, Denmark.
| | | | | | | | | | | |
Collapse
|
45
|
Buchhave LA, Latham DW, Johansen A, Bizzarro M, Torres G, Rowe JF, Batalha NM, Borucki WJ, Brugamyer E, Caldwell C, Bryson ST, Ciardi DR, Cochran WD, Endl M, Esquerdo GA, Ford EB, Geary JC, Gilliland RL, Hansen T, Isaacson H, Laird JB, Lucas PW, Marcy GW, Morse JA, Robertson P, Shporer A, Stefanik RP, Still M, Quinn SN. An abundance of small exoplanets around stars with a wide range of metallicities. Nature 2012; 486:375-7. [DOI: 10.1038/nature11121] [Citation(s) in RCA: 472] [Impact Index Per Article: 39.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/23/2011] [Accepted: 04/05/2012] [Indexed: 11/09/2022]
|
46
|
Trinquier A, Elliott T, Ulfbeck D, Coath C, Krot AN, Bizzarro M. Origin of nucleosynthetic isotope heterogeneity in the solar protoplanetary disk. Science 2009; 324:374-6. [PMID: 19372428 DOI: 10.1126/science.1168221] [Citation(s) in RCA: 369] [Impact Index Per Article: 24.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Stable-isotope variations exist among inner solar system solids, planets, and asteroids, but their importance is not understood. We report correlated, mass-independent variations of titanium-46 and titanium-50 in bulk analyses of these materials. Because titanium-46 and titanium-50 have different nucleosynthetic origins, this correlation suggests that the presolar dust inherited from the protosolar molecular cloud was well mixed when the oldest solar system solids formed, but requires a subsequent process imparting isotopic variability at the planetary scale. We infer that thermal processing of molecular cloud material, probably associated with volatile-element depletions in the inner solar system, resulted in selective destruction of thermally unstable, isotopically anomalous presolar components, producing residual isotopic heterogeneity. This implies that terrestrial planets accreted from thermally processed solids with nonsolar isotopic compositions.
Collapse
Affiliation(s)
- Anne Trinquier
- Center for Stars and Planets, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
| | | | | | | | | | | |
Collapse
|
47
|
Bizzarro M, Ulfbeck D, Trinquier A, Thrane K, Connelly JN, Meyer BS. Evidence for a late supernova injection of 60Fe into the protoplanetary disk. Science 2007; 316:1178-81. [PMID: 17525336 DOI: 10.1126/science.1141040] [Citation(s) in RCA: 99] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
High-precision 60Fe-60Ni isotope data show that most meteorites originating from differentiated planetesimals that accreted within 1 million years of the solar system's formation have 60Ni/58Ni ratios that are approximately 25 parts per million lower than samples from Earth, Mars, and chondrite parent bodies. This difference indicates that the oldest solar system planetesimals formed in the absence of 60Fe. Evidence for live 60Fe in younger objects suggests that 60Fe was injected into the protoplanetary disk approximately 1 million years after solar system formation, when 26Al was already homogeneously distributed. Decoupling the first appearance of 26Al and 60Fe constrains the environment where the Sun's formation could have taken place, indicating that it occurred in a dense stellar cluster in association with numerous massive stars.
Collapse
Affiliation(s)
- Martin Bizzarro
- Geological Institute, University of Copenhagen, Øster Voldgade 10, DK-1350, Denmark.
| | | | | | | | | | | |
Collapse
|
48
|
Abstract
BACKGROUND Nitric oxide (NO) is a prevalent molecule in the human body responsible for many physiologic activities including pulmonary vasodilation. An exogenous, inhaled form (iNO) exists that mimics this action without directly affecting systemic blood pressure. This therapy has been implemented in the treatment of pulmonary hypertension. This review examines the efficacy of iNO in the postoperative management of infants and children with congenital heart disease. OBJECTIVES To compare the effects of postoperative iNO versus placebo and/or conventional management on infants and children with congenital heart disease. The primary outcome was mortality, while secondary outcomes included length of hospital stay, assessment of neurodevelopmental disability, number of pulmonary hypertensive crises (PHTC), changes in haemodynamics including mean pulmonary arterial pressure (MPAP), mean arterial pressure (MAP), and heart rate (HR), changes in oxygenation measured as the ratio PaO2:FiO2, and measurement of maximum methaemoglobin level as a marker of toxicity. SEARCH STRATEGY We searched the Cochrane Central Register of Controlled Trials (CENTRAL) (The Cochrane Library, Issue 3, 2004), MEDLINE (1966 to 2004), and EMBASE (1980 to 2004). We included abstracts and all languages. SELECTION CRITERIA We included randomized and quasi-randomized controlled trials comparing iNO with placebo and conventional management, or both. Trials included only children with congenital heart disease requiring surgery and complicated by pulmonary hypertension. DATA COLLECTION AND ANALYSIS Data were collected on mortality, number of PHTC, changes in MPAP, MAP, HR, and PaO2:FiO2, and maximum methaemoglobin level, while data on long-term mortality, neurodevelopmental disability, and length of hospital stay were unavailable. We performed subgroup analysis by age and method of control. We performed sensitivity analysis using studies of highest methodologic quality. MAIN RESULTS We included four randomized trials. We observed no differences between groups with respect to mortality (P = 0.50), PHTC (P = 0.79), change in MPAP (P = 0.16), MAP (P = 0.40), HR (P = 1.00), or PaO2:FiO2 (P = 0.46). There was a significant reduction in MPAP in the subgroup of patients from birth to three months (P = 0.005), although this finding was based on a small number of patients (N = 23). AUTHORS' CONCLUSIONS We observed no differences with the use of iNO as compared with control in the majority of outcomes reviewed. No data were available for analysis with respect to several clinical outcomes including long-term mortality and neurodevelopmental outcome. We found it difficult to draw valid conclusions because of concerns regarding methodologic quality, bias, sample size, and heterogeneity.
Collapse
Affiliation(s)
- M Bizzarro
- Yale-New Haven Hospital, Pediatrics, 333 Cedar Street WP493, P.O. Box 208064, New Haven, CT 06520-8064, USA.
| | | |
Collapse
|
49
|
Baker J, Bizzarro M, Wittig N, Connelly J, Haack H. Early planetesimal melting from an age of 4.5662 Gyr for differentiated meteorites. Nature 2005; 436:1127-31. [PMID: 16121173 DOI: 10.1038/nature03882] [Citation(s) in RCA: 209] [Impact Index Per Article: 11.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/21/2004] [Accepted: 06/01/2005] [Indexed: 11/08/2022]
Abstract
Long- and short-lived radioactive isotopes and their daughter products in meteorites are chronometers that can test models for Solar System formation. Differentiated meteorites come from parent bodies that were once molten and separated into metal cores and silicate mantles. Mineral ages for these meteorites, however, are typically younger than age constraints for planetesimal differentiation. Such young ages indicate that the energy required to melt their parent bodies could not have come from the most likely heat source-radioactive decay of short-lived nuclides ((26)Al and (60)Fe) injected from a nearby supernova-because these would have largely decayed by the time of melting. Here we report an age of 4.5662 +/- 0.0001 billion years (based on Pb-Pb dating) for basaltic angrites, which is only 1 Myr younger than the currently accepted minimum age of the Solar System and corresponds to a time when (26)Al and (60)Fe decay could have triggered planetesimal melting. Small (26)Mg excesses in bulk angrite samples confirm that (26)Al decay contributed to the melting of their parent body. These results indicate that the accretion of differentiated planetesimals pre-dated that of undifferentiated planetesimals, and reveals the minimum Solar System age to be 4.5695 +/- 0.0002 billion years.
Collapse
Affiliation(s)
- Joel Baker
- School of Earth Sciences, Victoria University of Wellington, PO Box 600, Wellington, New Zealand.
| | | | | | | | | |
Collapse
|
50
|
|