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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. SCIENCE ADVANCES 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] [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.
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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
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Potiszil C, Yamanaka M, Sakaguchi C, Ota T, Kitagawa H, Kunihiro T, Tanaka R, Kobayashi K, Nakamura E. Organic Matter in the Asteroid Ryugu: What We Know So Far. Life (Basel) 2023; 13:1448. [PMID: 37511823 PMCID: PMC10381145 DOI: 10.3390/life13071448] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/31/2023] [Revised: 06/20/2023] [Accepted: 06/21/2023] [Indexed: 07/30/2023] Open
Abstract
The Hayabusa2 mission was tasked with returning samples from the C-complex asteroid Ryugu (1999 JU3), in order to shed light on the formation, evolution and composition of such asteroids. One of the main science objectives was to understand whether such bodies could have supplied the organic matter required for the origin of life on Earth. Here, a review of the studies concerning the organic matter within the Ryugu samples is presented. This review will inform the reader about the Hayabusa2 mission, the nature of the organic matter analyzed and the various interpretations concerning the analytical findings including those concerning the origin and evolution of organic matter from Ryugu. Finally, the review puts the findings and individual interpretations in the context of the current theories surrounding the formation and evolution of Ryugu. Overall, the summary provided here will help to inform those operating in a wide range of interdisciplinary fields, including planetary science, astrobiology, the origin of life and astronomy, about the most recent developments concerning the organic matter in the Ryugu return samples and their relevance to understanding our solar system and beyond. The review also outlines the issues that still remain to be solved and highlights potential areas for future work.
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Affiliation(s)
- Christian Potiszil
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori 682-0193, Japan
| | - Masahiro Yamanaka
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori 682-0193, Japan
| | - Chie Sakaguchi
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori 682-0193, Japan
| | - Tsutomu Ota
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori 682-0193, Japan
| | - Hiroshi Kitagawa
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori 682-0193, Japan
| | - Tak Kunihiro
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori 682-0193, Japan
| | - Ryoji Tanaka
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori 682-0193, Japan
| | - Katsura Kobayashi
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori 682-0193, Japan
| | - Eizo Nakamura
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori 682-0193, Japan
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Hoppe P, Rubin M, Altwegg K. A Comparison of Presolar Isotopic Signatures in Laboratory-Studied Primitive Solar System Materials and Comet 67P/Churyumov-Gerasimenko: New Insights from Light Elements, Halogens, and Noble Gases. SPACE SCIENCE REVIEWS 2023; 219:32. [PMID: 37251606 PMCID: PMC10209250 DOI: 10.1007/s11214-023-00977-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 01/30/2023] [Accepted: 05/08/2023] [Indexed: 05/31/2023]
Abstract
Comets are considered the most primitive planetary bodies in our Solar System. ESA's Rosetta mission to Jupiter family comet 67P/Churyumov-Gerasimenko (67P/CG) has provided a wealth of isotope data which expanded the existing data sets on isotopic compositions of comets considerably. In a previous paper (Hoppe et al. in Space Sci. Rev. 214:106, 2018) we reviewed the results for comet 67P/CG from the first four years of data reduction after arrival of Rosetta at the comet in August 2014 and discussed them in the context of respective meteorite data. Since then important new isotope data of several elements, among them the biogenic elements H, C, N, and O, for comet 67P/CG, the Tagish Lake meteorite, and C-type asteroid Ryugu became available which provide new insights into the formation conditions of small planetary bodies in the Solar System's earliest history. To complement the picture on comet 67P/CG and its context to other primitive Solar System materials, especially meteorites, that emerged from our previous paper, we review here the isotopic compositions of H, C, and N in various volatile molecules, of O in water and a suite of other molecules, of the halogens Cl and Br, and of the noble gas Kr in comet 67P/CG. Furthermore, we also review the H isotope data obtained in the refractory organics of the dust grains collected in the coma of 67P/CG. These data are compared with the respective meteoritic and Ryugu data and spectroscopic observations of other comets and extra-solar environments; Cl, Br, and Kr data are also evaluated in the context of a potential late supernova contribution, as suggested by the Si- and S-isotopic data of 67P/CG.
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Affiliation(s)
- Peter Hoppe
- Max Planck Institute for Chemistry, Hahn-Meitner-Weg 1, 55128 Mainz, Germany
| | - Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Kathrin Altwegg
- Center for Space and Habitability, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
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4
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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. SCIENCE ADVANCES 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] [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.
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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
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5
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le Goff S, Godin JP, Albalat E, Nieves JMR, Balter V. Magnesium stable isotope composition, but not concentration, responds to obesity and early insulin-resistant conditions in minipig. Sci Rep 2022; 12:10941. [PMID: 35768618 PMCID: PMC9243132 DOI: 10.1038/s41598-022-14825-3] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/02/2022] [Accepted: 06/13/2022] [Indexed: 11/29/2022] Open
Abstract
Hypomagnesemia is frequently associated with type 2 diabetes and generally correlates with unfavorable disease progression, but the magnesium status in pre-diabetic conditions remains unclear. Here, the magnesium metabolism is scrutinized in a minipig model of obesity and insulin resistance by measuring variations of the metallome—the set of inorganic elements—and the magnesium stable isotope composition in six organs of lean and obese minipigs raised on normal and Western-type diet, respectively. We found that metallomic variations are most generally insensitive to lean or obese phenotypes. The magnesium stable isotope composition of plasma, liver, kidney, and heart in lean minipigs are significantly heavier than in obese minipigs. For both lean and obese minipigs, the magnesium isotope composition of plasma and liver were negatively correlated to clinical phenotypes and plasma lipoproteins concentration as well as positively correlated to hyperinsulinemic-euglycemic clamp output. Because the magnesium isotope composition was not associated to insulin secretion, our results suggest that it is rather sensitive to whole body insulin sensitivity, opening perspectives to better comprehend the onset of insulin-resistant diabetic conditions.
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Affiliation(s)
- Samuel le Goff
- Laboratoire de Géologie de Lyon, ENS de Lyon, Université de Lyon, CNRS, Lyon, France
| | - Jean-Philippe Godin
- Nestlé Research, Institute of Food Safety and Analytical Sciences, Lausanne, Switzerland
| | - Emmanuelle Albalat
- Laboratoire de Géologie de Lyon, ENS de Lyon, Université de Lyon, CNRS, Lyon, France
| | | | - Vincent Balter
- Laboratoire de Géologie de Lyon, ENS de Lyon, Université de Lyon, CNRS, Lyon, France.
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6
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NAKAMURA E, KOBAYASHI K, TANAKA R, KUNIHIRO T, KITAGAWA H, POTISZIL C, OTA T, SAKAGUCHI C, YAMANAKA M, RATNAYAKE DM, TRIPATHI H, KUMAR R, AVRAMESCU ML, TSUCHIDA H, YACHI Y, MIURA H, ABE M, FUKAI R, FURUYA S, HATAKEDA K, HAYASHI T, HITOMI Y, KUMAGAI K, MIYAZAKI A, NAKATO A, NISHIMURA M, OKADA T, SOEJIMA H, SUGITA S, SUZUKI A, USUI T, YADA T, YAMAMOTO D, YOGATA K, YOSHITAKE 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, OKAMOTO C, ONO G, OZAKI M, SAIKI T, SAKATANI N, SAWADA H, SENSHU H, SHIMAKI Y, SHIRAI K, TAKEI Y, TAKEUCHI H, TANAKA S, TATSUMI E, TERUI F, TSUKIZAKI R, WADA K, YAMADA M, YAMADA T, YAMAMOTO Y, YANO H, YOKOTA Y, YOSHIHARA K, YOSHIKAWA M, YOSHIKAWA K, FUJIMOTO M, WATANABE SI, TSUDA Y. On the origin and evolution of the asteroid Ryugu: A comprehensive geochemical perspective. PROCEEDINGS OF THE JAPAN ACADEMY. SERIES B, PHYSICAL AND BIOLOGICAL SCIENCES 2022; 98:227-282. [PMID: 35691845 PMCID: PMC9246647 DOI: 10.2183/pjab.98.015] [Citation(s) in RCA: 25] [Impact Index Per Article: 12.5] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/31/2022] [Accepted: 05/06/2022] [Indexed: 05/28/2023]
Abstract
Presented here are the observations and interpretations from a comprehensive analysis of 16 representative particles returned from the C-type asteroid Ryugu by the Hayabusa2 mission. On average Ryugu particles consist of 50% phyllosilicate matrix, 41% porosity and 9% minor phases, including organic matter. The abundances of 70 elements from the particles are in close agreement with those of CI chondrites. Bulk Ryugu particles show higher δ18O, Δ17O, and ε54Cr values than CI chondrites. As such, Ryugu sampled the most primitive and least-thermally processed protosolar nebula reservoirs. Such a finding is consistent with multi-scale H-C-N isotopic compositions that are compatible with an origin for Ryugu organic matter within both the protosolar nebula and the interstellar medium. The analytical data obtained here, suggests that complex soluble organic matter formed during aqueous alteration on the Ryugu progenitor planetesimal (several 10's of km), <2.6 Myr after CAI formation. Subsequently, the Ryugu progenitor planetesimal was fragmented and evolved into the current asteroid Ryugu through sublimation.
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Affiliation(s)
- Eizo NAKAMURA
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Katsura KOBAYASHI
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Ryoji TANAKA
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Tak KUNIHIRO
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Hiroshi KITAGAWA
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Christian POTISZIL
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Tsutomu OTA
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Chie SAKAGUCHI
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Masahiro YAMANAKA
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Dilan M. RATNAYAKE
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Havishk TRIPATHI
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Rahul KUMAR
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Maya-Liliana AVRAMESCU
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Hidehisa TSUCHIDA
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Yusuke YACHI
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan
| | - Hitoshi MIURA
- Department of Information and Basic Science, Nagoya City University, Nagoya, Aichi, Japan
| | - Masanao ABE
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- The Graduate University for Advanced Studies (SOKENDAI), Hayama, Kanagawa, Japan
| | - Ryota FUKAI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Shizuho FURUYA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- Graduate School of Science, The University of Tokyo, Tokyo, Japan
| | - Kentaro HATAKEDA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Tasuku HAYASHI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Yuya HITOMI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- Marine Works Japan, Ltd., Yokosuka, Kanagawa, Japan
| | - Kazuya KUMAGAI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- Marine Works Japan, Ltd., Yokosuka, Kanagawa, Japan
| | - Akiko MIYAZAKI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Aiko NAKATO
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Masahiro NISHIMURA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Tatsuaki OKADA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- Graduate School of Science, The University of Tokyo, Tokyo, Japan
| | - Hiromichi SOEJIMA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- Marine Works Japan, Ltd., Yokosuka, Kanagawa, Japan
| | - Seiji SUGITA
- Graduate School of Science, The University of Tokyo, Tokyo, Japan
- Planetary Exploration Research Center (PERC), Chiba Institute of Technology, Narashino, Chiba, Japan
| | - Ayako SUZUKI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- Marine Works Japan, Ltd., Yokosuka, Kanagawa, Japan
| | - Tomohiro USUI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Toru YADA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Daiki YAMAMOTO
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Kasumi YOGATA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Miwa YOSHITAKE
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | | | - Atsushi FUJII
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Masahiko HAYAKAWA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Naoyuki HIRATA
- Graduate School of Science, Kobe University, Kobe, Hyogo, Japan
| | - Naru HIRATA
- Faculty of Computer Science and Engineering, The University of Aizu, Aizu-Wakamatsu, Fukushima, Japan
| | - Rie HONDA
- Faculty of Science and Technology, Kochi University, Kochi, Japan
| | - Chikatoshi HONDA
- Faculty of Computer Science and Engineering, The University of Aizu, Aizu-Wakamatsu, Fukushima, Japan
| | - Satoshi HOSODA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Yu-ichi IIJIMA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Hitoshi IKEDA
- Research and Development Directorate, JAXA, Sagamihara, Kanagawa, Japan
| | - Masateru ISHIGURO
- Department of Physics and Astronomy, Seoul National University, Seoul, Korea
| | - Yoshiaki ISHIHARA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Takahiro IWATA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- The Graduate University for Advanced Studies (SOKENDAI), Hayama, Kanagawa, Japan
| | - Kosuke KAWAHARA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Shota KIKUCHI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- Planetary Exploration Research Center (PERC), Chiba Institute of Technology, Narashino, Chiba, Japan
| | - Kohei KITAZATO
- Faculty of Computer Science and Engineering, The University of Aizu, Aizu-Wakamatsu, Fukushima, Japan
| | - Koji MATSUMOTO
- National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
| | - Moe MATSUOKA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- Observatoire de Paris, Meudon, France
| | - Tatsuhiro MICHIKAMI
- Faculty of Engineering, Kindai University, Higashi-Hiroshima, Hiroshima, Japan
| | - Yuya MIMASU
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Akira MIURA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Tomokatsu MOROTA
- Graduate School of Environmental Studies, Nagoya University, Nagoya, Aichi, Japan
| | - Satoru NAKAZAWA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Noriyuki NAMIKI
- National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
| | - Hirotomo NODA
- National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
| | - Rina NOGUCHI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- Faculty of Science, Niigata University, Niigata, Japan
| | - Naoko OGAWA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Kazunori OGAWA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Chisato OKAMOTO
- Graduate School of Science, Kobe University, Kobe, Hyogo, Japan
| | - Go ONO
- Research and Development Directorate, JAXA, Sagamihara, Kanagawa, Japan
| | - Masanobu OZAKI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Takanao SAIKI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | | | - Hirotaka SAWADA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Hiroki SENSHU
- Planetary Exploration Research Center (PERC), Chiba Institute of Technology, Narashino, Chiba, Japan
| | - Yuri SHIMAKI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Kei SHIRAI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- Graduate School of Science, Kobe University, Kobe, Hyogo, Japan
| | - Yuto TAKEI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Hiroshi TAKEUCHI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Satoshi TANAKA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- The Graduate University for Advanced Studies (SOKENDAI), Hayama, Kanagawa, Japan
- The University of Tokyo, Kashiwa, Chiba, Japan
| | - Eri TATSUMI
- Graduate School of Science, The University of Tokyo, Tokyo, Japan
- Instituto de Astrofisica de Canarias, University of La Laguna, Tenerife, Spain
| | - Fuyuto TERUI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- Faculty of Engineering, Kanagawa Institute of Technology, Atsugi, Kanagawa, Japan
| | - Ryudo TSUKIZAKI
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Koji WADA
- Planetary Exploration Research Center (PERC), Chiba Institute of Technology, Narashino, Chiba, Japan
| | - Manabu YAMADA
- Planetary Exploration Research Center (PERC), Chiba Institute of Technology, Narashino, Chiba, Japan
| | - Tetsuya YAMADA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Yukio YAMAMOTO
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Hajime YANO
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Yasuhiro YOKOTA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Keisuke YOSHIHARA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Makoto YOSHIKAWA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- The Graduate University for Advanced Studies (SOKENDAI), Hayama, Kanagawa, Japan
| | - Kent YOSHIKAWA
- Research and Development Directorate, JAXA, Sagamihara, Kanagawa, Japan
| | - Masaki FUJIMOTO
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
| | - Sei-ichiro WATANABE
- Graduate School of Environmental Studies, Nagoya University, Nagoya, Aichi, Japan
| | - Yuichi TSUDA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan
- Graduate School of Science, The University of Tokyo, Tokyo, Japan
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7
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Fukuda K, Brownlee DE, Joswiak DJ, Tenner TJ, Kimura M, Kita NT. Correlated isotopic and chemical evidence for condensation origins of olivine in comet 81P/Wild 2 and in AOAs from CV and CO chondrites. GEOCHIMICA ET COSMOCHIMICA ACTA 2021; 293:544-574. [PMID: 34866644 PMCID: PMC8637496 DOI: 10.1016/j.gca.2020.09.036] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
Magnesium stable isotope ratios and minor element abundances of five olivine particles from comet 81P/Wild 2 were examined by secondary ion mass spectrometry (SIMS). Wild 2 olivine particles exhibit only small variations in δ25Mg values from -1.0 +0.4/-0.5 ‰ to 0.6 +0.5/- 0.6 ‰ (2σ). This variation can be simply explained by mass-dependent fractionation from Mg isotopic compositions of the Earth and bulk meteorites, suggesting that Wild 2 olivine particles formed in the chondritic reservoir with respect to Mg isotope compositions. We also determined minor element abundances, and O and Mg isotope ratios of olivine grains in amoeboid olivine aggregates (AOAs) from Kaba (CV3.1) and DOM 08006 (CO3.01) carbonaceous chondrites. Our new SIMS minor element data reveal uniform, low FeO contents of ~0.05 wt% among AOA olivines from DOM 08006, suggesting that AOAs formed at more reducing environments in the solar nebula than previously thought. Furthermore, the SIMS-derived FeO contents of the AOA olivines are consistently lower than those obtained by electron microprobe analyses (~1 wt% FeO), indicating possible fluorescence from surrounding matrix materials and/or Fe,Ni-metals in AOAs during electron microprobe analyses. For Mg isotopes, AOA olivines show more negative mass-dependent fractionation (-3.8 ± 0.5‰ ≤ δ25Mg ≤ -0.2 ± 0.3‰; 2σ) relative to Wild 2 olivines. Further, these Mg isotope variations are correlated with their host AOA textures. Large negative Mg isotope fractionations in olivine are often observed in pore-rich AOAs, while those in compact AOAs tend to have near-chondritic Mg isotopic compositions. These observations indicate that pore-rich AOAs preserved their gas-solid condensation histories, while compact AOAs experienced thermal processing in the solar nebula after their condensation and aggregation. Importantly, one 16O-rich Wild 2 LIME olivine particle (T77/F50) shows negative Mg isotope fractionation (δ25Mg = -0.8 ± 0.4‰, δ26Mg = -1.4 ± 0.9‰; 2σ) relative to bulk chondrites. Minor element abundances of T77/F50 are in excellent agreement with those of olivines from pore-rich AOAs in DOM 08006. The observed similarity in O and Mg isotopes, and minor element abundances suggest that T77/F50 formed in an environment similar to AOAs, probably near the proto-Sun, and then was transported to the Kuiper belt, where comet 81P/Wild 2 likely accreted.
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Affiliation(s)
- Kohei Fukuda
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Donald E. Brownlee
- Department of Astronomy, University of Washington, Seattle, WA 98195, USA
| | - David J. Joswiak
- Department of Astronomy, University of Washington, Seattle, WA 98195, USA
| | - Travis J. Tenner
- Chemistry Division, Nuclear and Radiochemistry, Los Alamos National Laboratory, MSJ514, Los Alamos, NM 87545, USA
| | - Makoto Kimura
- National Institute of Polar Research, Tokyo 190-8518, Japan
| | - Noriko T. Kita
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
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8
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Hu JY, Dauphas N, Tissot FLH, Yokochi R, Ireland TJ, Zhang Z, Davis AM, Ciesla FJ, Grossman L, Charlier BLA, Roskosz M, Alp EE, Hu MY, Zhao J. Heating events in the nascent solar system recorded by rare earth element isotopic fractionation in refractory inclusions. SCIENCE ADVANCES 2021; 7:7/2/eabc2962. [PMID: 33523962 PMCID: PMC7787488 DOI: 10.1126/sciadv.abc2962] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/16/2020] [Accepted: 11/16/2020] [Indexed: 05/31/2023]
Abstract
Equilibrium condensation of solar gas is often invoked to explain the abundance of refractory elements in planets and meteorites. This is partly motivated, by the observation that the depletions in both the least and most refractory rare earth elements (REEs) in meteoritic group II calcium-aluminum-rich inclusions (CAIs) can be reproduced by thermodynamic models of solar nebula condensation. We measured the isotopic compositions of Ce, Nd, Sm, Eu, Gd, Dy, Er, and Yb in eight CAIs to test this scenario. Contrary to expectation for equilibrium condensation, we find light isotope enrichment for the most refractory REEs and more subdued isotopic variations for the least refractory REEs. This suggests that group II CAIs formed by a two-stage process involving fast evaporation of preexisting materials, followed by near-equilibrium recondensation. The calculated time scales are consistent with heating in events akin to FU Orionis- or EX Lupi-type outbursts of eruptive pre-main-sequence stars.
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Affiliation(s)
- J Y Hu
- Origins Laboratory, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA.
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - N Dauphas
- Origins Laboratory, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - F L H Tissot
- Origins Laboratory, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
- The Isotoparium, Division of Geological and Planetary Sciences, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USA
| | - R Yokochi
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - T J Ireland
- Origins Laboratory, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
- Department of Earth and Environment, Boston University, 685 Commonwealth Avenue, Boston, MA 02215, USA
| | - Z Zhang
- Origins Laboratory, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - A M Davis
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - F J Ciesla
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - L Grossman
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - B L A Charlier
- School of Geography, Earth and Environmental Sciences, Victoria University of Wellington, Wellington 6140, New Zealand
| | - M Roskosz
- IMPMC, CNRS, UMR 7590, Sorbonne Universités, Université Pierre et Marie Curie, Muséum National d'Histoire Naturelle, CP 52, 57 rue Cuvier, Paris F-75231, France
| | - E E Alp
- Advanced Photon Source, Argonne National Laboratory, 9700 South Cass Avenue, Argonne, IL 60439, USA
| | - M Y Hu
- Advanced Photon Source, Argonne National Laboratory, 9700 South Cass Avenue, Argonne, IL 60439, USA
| | - J Zhao
- Advanced Photon Source, Argonne National Laboratory, 9700 South Cass Avenue, Argonne, IL 60439, USA
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9
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Rubin M, Engrand C, Snodgrass C, Weissman P, Altwegg K, Busemann H, Morbidelli A, Mumma M. On the Origin and Evolution of the Material in 67P/Churyumov-Gerasimenko. SPACE SCIENCE REVIEWS 2020; 216:102. [PMID: 32801398 PMCID: PMC7392949 DOI: 10.1007/s11214-020-00718-2] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/09/2019] [Accepted: 07/03/2020] [Indexed: 06/02/2023]
Abstract
Primitive objects like comets hold important information on the material that formed our solar system. Several comets have been visited by spacecraft and many more have been observed through Earth- and space-based telescopes. Still our understanding remains limited. Molecular abundances in comets have been shown to be similar to interstellar ices and thus indicate that common processes and conditions were involved in their formation. The samples returned by the Stardust mission to comet Wild 2 showed that the bulk refractory material was processed by high temperatures in the vicinity of the early sun. The recent Rosetta mission acquired a wealth of new data on the composition of comet 67P/Churyumov-Gerasimenko (hereafter 67P/C-G) and complemented earlier observations of other comets. The isotopic, elemental, and molecular abundances of the volatile, semi-volatile, and refractory phases brought many new insights into the origin and processing of the incorporated material. The emerging picture after Rosetta is that at least part of the volatile material was formed before the solar system and that cometary nuclei agglomerated over a wide range of heliocentric distances, different from where they are found today. Deviations from bulk solar system abundances indicate that the material was not fully homogenized at the location of comet formation, despite the radial mixing implied by the Stardust results. Post-formation evolution of the material might play an important role, which further complicates the picture. This paper discusses these major findings of the Rosetta mission with respect to the origin of the material and puts them in the context of what we know from other comets and solar system objects.
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Affiliation(s)
- Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Cécile Engrand
- CNRS/IN2P3, IJCLab, Université Paris-Saclay, 91405 Orsay Cedex, France
| | - Colin Snodgrass
- Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9 3HJ UK
| | | | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Henner Busemann
- Institute of Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | | | - Michael Mumma
- NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, 20771 MD USA
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Hazen RM, Morrison SM. An evolutionary system of mineralogy. Part I: Stellar mineralogy (>13 to 4.6 Ga). THE AMERICAN MINERALOGIST 2020; 105:627-651. [PMID: 33867541 PMCID: PMC8051151 DOI: 10.2138/am-2020-7173] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Minerals preserve records of the physical, chemical, and biological histories of their origins and subsequent alteration, and thus provide a vivid narrative of the evolution of Earth and other worlds through billions of years of cosmic history. Mineral properties, including trace and minor elements, ratios of isotopes, solid and fluid inclusions, external morphologies, and other idiosyncratic attributes, represent information that points to specific modes of formation and subsequent environmental histories-information essential to understanding the co-evolving geosphere and biosphere. This perspective suggests an opportunity to amplify the existing system of mineral classification, by which minerals are defined solely on idealized end-member chemical compositions and crystal structures. Here we present the first in a series of contributions to explore a complementary evolutionary system of mineralogy-a classification scheme that links mineral species to their paragenetic modes. The earliest stage of mineral evolution commenced with the appearance of the first crystals in the universe at >13 Ga and continues today in the expanding, cooling atmospheres of countless evolved stars, which host the high-temperature (T > 1000 K), low-pressure (P < 10-2 atm) condensation of refractory minerals and amorphous phases. Most stardust is thought to originate in three distinct processes in carbon- and/or oxygen-rich mineral-forming stars: (1) condensation in the cooling, expanding atmospheres of asymptotic giant branch stars; (2) during the catastrophic explosions of supernovae, most commonly core collapse (Type II) supernovae; and (3) classical novae explosions, the consequence of runaway fusion reactions at the surface of a binary white dwarf star. Each stellar environment imparts distinctive isotopic and trace element signatures to the micro- and nanoscale stardust grains that are recovered from meteorites and micrometeorites collected on Earth's surface, by atmospheric sampling, and from asteroids and comets. Although our understanding of the diverse mineral-forming environments of stars is as yet incomplete, we present a preliminary catalog of 41 distinct natural kinds of stellar minerals, representing 22 official International Mineralogical Association (IMA) mineral species, as well as 2 as yet unapproved crystalline phases and 3 kinds of non-crystalline condensed phases not codified by the IMA.
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Affiliation(s)
- Robert M. Hazen
- Earth and Planets Laboratory, Carnegie Institution for Science, 5251 Broad Branch Road NW, Washington, DC 20015, U.S.A
| | - Shaunna M. Morrison
- Earth and Planets Laboratory, Carnegie Institution for Science, 5251 Broad Branch Road NW, Washington, DC 20015, U.S.A
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11
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Sandford SA, Nuevo M, Bera PP, Lee TJ. Prebiotic Astrochemistry and the Formation of Molecules of Astrobiological Interest in Interstellar Clouds and Protostellar Disks. Chem Rev 2020; 120:4616-4659. [DOI: 10.1021/acs.chemrev.9b00560] [Citation(s) in RCA: 71] [Impact Index Per Article: 17.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 12/31/2022]
Affiliation(s)
- Scott A. Sandford
- NASA Ames Research Center, MS 245-6, Moffett Field, California 94035, United States
| | - Michel Nuevo
- NASA Ames Research Center, MS 245-6, Moffett Field, California 94035, United States
- BAER Institute, NASA Research Park, MS 18-4, Moffett Field, California 94035, United States
| | - Partha P. Bera
- NASA Ames Research Center, MS 245-6, Moffett Field, California 94035, United States
- BAER Institute, NASA Research Park, MS 18-4, Moffett Field, California 94035, United States
| | - Timothy J. Lee
- NASA Ames Research Center, MS 245-3, Moffett Field, California 94035, United States
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12
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Kebukawa Y, Ito M, Zolensky ME, Greenwood RC, Rahman Z, Suga H, Nakato A, Chan QHS, Fries M, Takeichi Y, Takahashi Y, Mase K, Kobayashi K. A novel organic-rich meteoritic clast from the outer solar system. Sci Rep 2019; 9:3169. [PMID: 30816187 PMCID: PMC6395772 DOI: 10.1038/s41598-019-39357-1] [Citation(s) in RCA: 18] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/08/2018] [Accepted: 01/22/2019] [Indexed: 11/09/2022] Open
Abstract
The Zag meteorite which is a thermally-metamorphosed H ordinary chondrite contains a primitive xenolithic clast that was accreted to the parent asteroid after metamorphism. The cm-sized clast contains abundant large organic grains or aggregates up to 20 μm in phyllosilicate-rich matrix. Here we report organic and isotope analyses of a large (~10 μm) OM aggregate in the Zag clast. The X-ray micro-spectroscopic technique revealed that the OM aggregate has sp2 dominated hydrocarbon networks with a lower abundance of heteroatoms than in IOM from primitive (CI,CM,CR) carbonaceous chondrites, and thus it is distinguished from most of the OM in carbonaceous meteorites. The OM aggregate has high D/H and 15N/14N ratios (δD = 2,370 ± 74‰ and δ15N = 696 ± 100‰), suggesting that it originated in a very cold environment such as the interstellar medium or outer region of the solar nebula, while the OM is embedded in carbonate-bearing matrix resulting from aqueous activities. Thus, the high D/H ratio must have been preserved during the extensive late-stage aqueous processing. It indicates that both the OM precursors and the water had high D/H ratios. Combined with 16O-poor nature of the clast, the OM aggregate and the clast are unique among known chondrite groups. We further propose that the clast possibly originated from D/P type asteroids or trans-Neptunian Objects.
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Affiliation(s)
- Yoko Kebukawa
- Faculty of Engineering, Yokohama National University, 79-5 Tokiwadai, Hodogaya-ku, Yokohama, 240-8501, Japan.
| | - Motoo Ito
- Kochi Institute for Core Sample Research, JAMSTEC, B200 Monobe, Nankoku, Kochi, 783-8502, Japan
| | - Michael E Zolensky
- ARES, NASA Johnson Space Center, 2101 NASA Parkway, Houston, TX, 77058, USA
| | - Richard C Greenwood
- Planetary and Space Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA, United Kingdom
| | - Zia Rahman
- Jacobs, NASA Johnson Space Center, Houston, TX, 77058, USA
| | - Hiroki Suga
- Department of Earth and Planetary Systems Science, Hiroshima University, Kagamiyama, Higashi-Hiroshima, Hiroshima, 739-8526, Japan.,Department of Earth and Planetary Science, The University of Tokyo, Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan
| | - Aiko Nakato
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Sagamihara, 252-5210, Japan
| | - Queenie H S Chan
- ARES, NASA Johnson Space Center, 2101 NASA Parkway, Houston, TX, 77058, USA.,Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK
| | - Marc Fries
- ARES, NASA Johnson Space Center, 2101 NASA Parkway, Houston, TX, 77058, USA
| | - Yasuo Takeichi
- Institute of Materials Structure Science, High-Energy Accelerator Research Organization (KEK), 1-1 Oho, Tsukuba, Ibaraki, 305-0801, Japan
| | - Yoshio Takahashi
- Department of Earth and Planetary Science, The University of Tokyo, Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan
| | - Kazuhiko Mase
- Institute of Materials Structure Science, High-Energy Accelerator Research Organization (KEK), 1-1 Oho, Tsukuba, Ibaraki, 305-0801, Japan
| | - Kensei Kobayashi
- Faculty of Engineering, Yokohama National University, 79-5 Tokiwadai, Hodogaya-ku, Yokohama, 240-8501, Japan
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13
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Contributions from Accreted Organics to Titan’s Atmosphere: New Insights from Cometary and Chondritic Data. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/aaf561] [Citation(s) in RCA: 26] [Impact Index Per Article: 5.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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14
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NAKAMURA E, KUNIHIRO T, OTA T, SAKAGUCHI C, TANAKA R, KITAGAWA H, KOBAYASHI K, YAMANAKA M, SHIMAKI Y, BEBOUT GE, MIURA H, YAMAMOTO T, MALKOVETS V, GROKHOVSKY V, KOROLEVA O, LITASOV K. Hypervelocity collision and water-rock interaction in space preserved in the Chelyabinsk ordinary chondrite. PROCEEDINGS OF THE JAPAN ACADEMY. SERIES B, PHYSICAL AND BIOLOGICAL SCIENCES 2019; 95:165-177. [PMID: 30971619 PMCID: PMC6541723 DOI: 10.2183/pjab.95.013] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/25/2019] [Accepted: 03/04/2019] [Indexed: 06/01/2023]
Abstract
A comprehensive geochemical study of the Chelyabinsk meteorite reveals further details regarding its history of impact-related fragmentation and melting, and later aqueous alteration, during its transit toward Earth. We support an ∼30 Ma age obtained by Ar-Ar method (Beard et al., 2014) for the impact-related melting, based on Rb-Sr isotope analyses of a melt domain. An irregularly shaped olivine with a distinct O isotope composition in a melt domain appears to be a fragment of a silicate-rich impactor. Hydrogen and Li concentrations and isotopic compositions, textures of Fe oxyhydroxides, and the presence of organic materials located in fractures, are together consistent with aqueous alteration, and this alteration could have pre-dated interaction with the Earth's atmosphere. As one model, we suggest that hypervelocity capture of the impact-related debris by a comet nucleus could have led to shock-wave-induced supercritical aqueous fluids dissolving the silicate, metallic, and organic matter, with later ice sublimation yielding a rocky rubble pile sampled by the meteorite.
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Affiliation(s)
- Eizo NAKAMURA
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Tottori, Japan
| | - Tak KUNIHIRO
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Tottori, Japan
| | - Tsutomu OTA
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Tottori, Japan
| | - Chie SAKAGUCHI
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Tottori, Japan
| | - Ryoji TANAKA
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Tottori, Japan
| | - Hiroshi KITAGAWA
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Tottori, Japan
| | - Katsura KOBAYASHI
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Tottori, Japan
| | - Masahiro YAMANAKA
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Tottori, Japan
| | - Yuri SHIMAKI
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Tottori, Japan
| | - Gray E. BEBOUT
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Tottori, Japan
- Department of Earth and Environmental Sciences, Lehigh University, Bethlehem, PA, U.S.A.
| | - Hitoshi MIURA
- Graduate School of Natural Sciences, Nagoya City University, Nagoya, Japan
| | - Tetsuo YAMAMOTO
- Institute of Low Temperature Science, Hokkaido University, Sapporo, Japan
| | - Vladimir MALKOVETS
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Tottori, Japan
| | - Victor GROKHOVSKY
- Institute of Physics and Technology, Ural Federal University, Yekaterinburg, Russia
| | - Olga KOROLEVA
- Institute of Mineralogy, Ural Branch of the Russian Academy of Sciences, Miass, Russia
- South-Ural State University, Chelyabinsk, Russia
| | - Konstantin LITASOV
- V.S. Sobolev Institute of Geology and Mineralogy, Siberian Branch of the Russian Academy of Sciences, Novosibirsk, Russia
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15
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Ishii HA. Comparison of GEMS in Interplanetary Dust Particles and GEMS-like Objects in a Stardust Impact Track in Aerogel. METEORITICS & PLANETARY SCIENCE 2019; 54:202-219. [PMID: 30713419 PMCID: PMC6350812 DOI: 10.1111/maps.13182] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/25/2018] [Accepted: 07/06/2018] [Indexed: 06/09/2023]
Abstract
Comet 81P/Wild 2 dust, the first comet sample of known provenance, was widely expected to resemble anhydrous chondritic porous (CP) interplanetary dust particles (IDPs). GEMS, distinctly characteristic of CP IDPs, have yet to be unambiguously identified in the Stardust mission samples despite claims of likely candidates. One such candidate is Stardust impact track 57 "Febo" in aerogel, which contains fine-grained objects texturally and compositionally similar to GEMS. Their position adjacent the terminal particle suggests that they may be indigenous, fine-grained, cometary material, like that in CP IDPs, shielded by the terminal particle from damage during deceleration from hypervelocity. Darkfield imaging and multi-detector energy-dispersive x-ray mapping were used to compare GEMS-like-objects in the Febo terminal particle with GEMS in an anhydrous, chondritic IDP. GEMS in the IDP are within 3× CI (solar) abundances for major and minor elements. In the Febo GEMS-like objects, Mg and Ca are systematically and strongly depleted relative to CI; S and Fe are somewhat enriched; and Au, a known aerogel contaminant is present, consistent with ablation, melting, abrasion and mixing of the SiOx aerogel with crystalline Fe-sulfide and minor enstatite, high-Ni sulfide and augite identified by elemental mapping in the terminal particle. Thus, GEMS-like objects in "caches" of fine-grained debris abutting terminal particles are most likely deceleration debris packed in place during particle transit through the aerogel.
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Affiliation(s)
- Hope A Ishii
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
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16
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Carbon and oxygen isotopic fractionation in the products of low-temperature VUV photodissociation of carbon monoxide. Chem Phys 2018. [DOI: 10.1016/j.chemphys.2018.05.022] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/22/2022]
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17
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Hoppe P, Rubin M, Altwegg K. Presolar Isotopic Signatures in Meteorites and Comets: New Insights from the Rosetta Mission to Comet 67P/Churyumov-Gerasimenko. SPACE SCIENCE REVIEWS 2018; 214:106. [PMID: 37265997 PMCID: PMC10229468 DOI: 10.1007/s11214-018-0540-3] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/28/2017] [Accepted: 08/20/2018] [Indexed: 06/01/2023]
Abstract
Comets are considered the most primitive planetary bodies in our Solar System, i.e., they should have best preserved the solid components of the matter from which our Solar System formed. ESA's recent Rosetta mission to Jupiter family comet 67P/Churyumov-Gerasimenko (67P/CG) has provided a wealth of isotope data which expanded the existing data sets on isotopic compositions of comets considerably. In this paper we review our current knowledge on the isotopic compositions of H, C, N, O, Si, S, Ar, and Xe in primitive Solar System materials studied in terrestrial laboratories and how the Rosetta data acquired with the ROSINA (Rosetta Orbiter Sensor for Ion and Neutral Analysis) and COSIMA (COmetary Secondary Ion Mass Analyzer) mass spectrometer fit into this picture. The H, Si, S, and Xe isotope data of comet 67P/CG suggest that this comet might be particularly primitive and might have preserved large amounts of unprocessed presolar matter. We address the question whether the refractory Si component of 67P/CG contains a presolar isotopic fingerprint from a nearby Type II supernova (SN) and discuss to which extent C and O isotope anomalies originating from presolar grains should be observable in dust from 67P/CG. Finally, we explore whether the isotopic fingerprint of a potential late SN contribution to the formation site of 67P/CG in the solar nebula can be seen in the volatile component of 67P/CG.
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Affiliation(s)
- Peter Hoppe
- Max Planck Institute for Chemistry, Hahn-Meitner-Weg 1, 55128 Mainz, Germany
| | - Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
- Center for Space and Habitability, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
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18
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Nittler LR, Alexander CMO, Davidson J, Riebe MEI, Stroud RM, Wang J. High Abundances of Presolar Grains and 15N-rich Organic Matter in CO3.0 Chondrite Dominion Range 08006. GEOCHIMICA ET COSMOCHIMICA ACTA 2018; 226:107-131. [PMID: 29628527 PMCID: PMC5881170 DOI: 10.1016/j.gca.2018.01.038] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
NanoSIMS C-, N-, and O-isotopic mapping of matrix in CO3.0 chondrite Dominion Range (DOM) 08006 revealed it to have in its matrix the highest abundance of presolar O-rich grains (257 +76/-96 ppm, 2σ) of any meteorite. It also has a matrix abundance of presolar SiC of 35 (+25/-17, 2σ) ppm, similar to that seen across primitive chondrite classes. This provides additional support to bulk isotopic and petrologic evidence that DOM 08006 is the most primitive known CO meteorite. Transmission electron microscopy of five presolar silicate grains revealed one to have a composite mineralogy similar to larger amoeboid olivine aggregates and consistent with equilibrium condensation, two non-stoichiometric amorphous grains and two olivine grains, though one is identified as such solely based on its composition. We also found insoluble organic matter (IOM) to be present primarily as sub-micron inclusions with ranges of C- and N-isotopic anomalies similar to those seen in primitive CR chondrites and interplanetary dust particles. In contrast to other primitive extraterrestrial materials, H isotopic imaging showed normal and homogeneous D/H. Most likely, DOM 08006 and other CO chondrites accreted a similar complement of primitive and isotopically anomalous organic matter to that found in other chondrite classes and IDPs, but the very limited amount of thermal metamorphism experienced by DOM 08006 has caused loss of D-rich organic moieties, while not substantially affecting either the molecular carriers of C and N anomalies or most inorganic phases in the meteorite. One C-rich grain that was highly depleted in 13C and 15N was identified; we propose it originated in the Sun's parental molecular cloud.
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Affiliation(s)
- Larry R Nittler
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA
| | - Conel M O'D Alexander
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA
| | - Jemma Davidson
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA
| | - My E I Riebe
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA
| | - Rhonda M Stroud
- Materials Science and Technology Division, Code 6366, US Naval Research Laboratory, Washington, DC 20375-5320, USA
| | - Jianhua Wang
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA
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Levasseur-Regourd AC, Agarwal J, Cottin H, Engrand C, Flynn G, Fulle M, Gombosi T, Langevin Y, Lasue J, Mannel T, Merouane S, Poch O, Thomas N, Westphal A. Cometary Dust. SPACE SCIENCE REVIEWS 2018; 214:64. [PMID: 35095119 PMCID: PMC8793767 DOI: 10.1007/s11214-018-0496-3] [Citation(s) in RCA: 12] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/13/2017] [Accepted: 03/16/2018] [Indexed: 05/15/2023]
Abstract
This review presents our understanding of cometary dust at the end of 2017. For decades, insight about the dust ejected by nuclei of comets had stemmed from remote observations from Earth or Earth's orbit, and from flybys, including the samples of dust returned to Earth for laboratory studies by the Stardust return capsule. The long-duration Rosetta mission has recently provided a huge and unique amount of data, obtained using numerous instruments, including innovative dust instruments, over a wide range of distances from the Sun and from the nucleus. The diverse approaches available to study dust in comets, together with the related theoretical and experimental studies, provide evidence of the composition and physical properties of dust particles, e.g., the presence of a large fraction of carbon in macromolecules, and of aggregates on a wide range of scales. The results have opened vivid discussions on the variety of dust-release processes and on the diversity of dust properties in comets, as well as on the formation of cometary dust, and on its presence in the near-Earth interplanetary medium. These discussions stress the significance of future explorations as a way to decipher the formation and evolution of our Solar System.
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Affiliation(s)
- Anny-Chantal Levasseur-Regourd
- Sorbonne Université; UVSQ; CNRS/INSU; Campus Pierre et Marie Curie, BC 102, 4 place Jussieu, F-75005 Paris, France, Tel.: + 33 144274875,
| | - Jessica Agarwal
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg, 3, D-37077, Göttingen, Germany
| | - Hervé Cottin
- Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA), UMR CNRS 7583, Université Paris-Est Créteil et Université Paris Diderot, Institut Pierre Simon Laplace, 94000 Créteil, France
| | - Cécile Engrand
- Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), CNRS/IN2P3 Université Paris Sud - UMR 8609, Université Paris-Saclay, Bâtiment 104, 91405 Orsay Campus, France
| | - George Flynn
- SUNY-Plattsburgh, 101 Broad St, Plattsburgh, NY 12901, United States
| | - Marco Fulle
- INAF - Osservatorio Astronomico, Via Tiepolo 11, 34143 Trieste Italy
| | - Tamas Gombosi
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI 48109, USA
| | - Yves Langevin
- Institut dAstrophysique Spatiale (IAS), CNRS/Université Paris Sud, Bâtiment 121, 91405 Orsay France
| | - Jérémie Lasue
- IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
| | - Thurid Mannel
- Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria; Physics Institute, University of Graz, Universitätsplatz 5, 8010 Graz, Austria
| | - Sihane Merouane
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg, 3, D-37077, Göttingen, Germany
| | - Olivier Poch
- Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
| | - Nicolas Thomas
- Physikalisches Institut, Universität Bern, Sidlerstrasse 5, 3012, Bern, Switzerland
| | - Andrew Westphal
- Space Sciences Laboratory, U.C. Berkeley, Berkeley, California 94720-7450 USA
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Abstract
Measurements by the Genesis mission have shown that solar wind oxygen is depleted in the rare isotopes, 17O and 18O, by approximately 80 and 100‰, respectively, relative to Earth's oceans, with inferred photospheric values of about -60‰ for both isotopes. Direct astronomical measurements of CO absorption lines in the solar photosphere have previously yielded a wide range of O isotope ratios. Here, we reanalyze the line strengths for high-temperature rovibrational transitions in photospheric CO from ATMOS FTS data, and obtain an 18O depletion of δ18O = -50 ± 11‰ (1σ). From the same analysis we find a carbon isotope ratio of δ13C = -48 ± 7‰ (1σ) for the photosphere. This implies that the primary reservoirs of carbon on the terrestrial planets are enriched in 13C relative to the bulk material from which the solar system formed, possibly as a result of CO self-shielding or inheritance from the parent cloud.
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Wooden DH, Ishii HA, Zolensky ME. Cometary dust: the diversity of primitive refractory grains. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2017; 375:20160260. [PMID: 28554979 PMCID: PMC5454228 DOI: 10.1098/rsta.2016.0260] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 04/13/2017] [Indexed: 05/07/2023]
Abstract
Comet dust is primitive and shows significant diversity. Our knowledge of the properties of primitive cometary particles has expanded significantly through microscale investigations of cosmic dust samples (anhydrous interplanetary dust particles (IDPs), chondritic porous (CP) IDPs and UltraCarbonaceous Antarctic micrometeorites, Stardust and Rosetta), as well as through remote sensing (Spitzer IR spectroscopy). Comet dust are aggregate particles of materials unequilibrated at submicrometre scales. We discuss the properties and processes experienced by primitive matter in comets. Primitive particles exhibit a diverse range of: structure and typology; distribution of constituents; concentration and form of carbonaceous and refractory organic matter; Mg- and Fe-contents of the silicate minerals; sulfides; existence/abundance of type II chondrule fragments; high-temperature calcium-aluminium inclusions and ameboid-olivine aggregates; and rarely occurring Mg-carbonates and magnetite, whose explanation requires aqueous alteration on parent bodies. The properties of refractory materials imply there were disc processes that resulted in different comets having particular selections of primitive materials. The diversity of primitive particles has implications for the diversity of materials in the protoplanetary disc present at the time and in the region where the comets formed.This article is part of the themed issue 'Cometary science after Rosetta'.
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Affiliation(s)
- D H Wooden
- NASA Ames Research Center, Moffett Field, CA 94035-0001, USA
| | - H A Ishii
- University of Hawaii, Hawai'i Institute of Geophysics and Planetology, Honolulu, HI 96822, USA
| | - M E Zolensky
- NASA Johnson Space Center, ARES, X12 2010 NASA Parkway, Houston, TX 77058-3607, USA
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Defouilloy C, Nakashima D, Joswiak DJ, Brownlee DE, Tenner TJ, Kita NT. Origin of crystalline silicates from Comet 81P/Wild 2: Combined study on their oxygen isotopes and mineral chemistry. EARTH AND PLANETARY SCIENCE LETTERS 2017; 465:145-154. [PMID: 30705461 PMCID: PMC6350803 DOI: 10.1016/j.epsl.2017.02.045] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
In order to explore the link between comet 81P/Wild 2 and materials in primitive meteorites, seven particles 5 to 15 μm in diameter from comet 81P/Wild 2 have been analyzed for their oxygen isotope ratios using a secondary ion mass spectrometer. Most particles are single minerals consisting of olivine or pyroxene with Mg# higher than 85, which are relatively minor in 81P/Wild 2 particles (~1/3 of the 16O-poor cluster). Four particles extracted from Track 149 are 16O-poor and show Δ17O (= δ17O - 0.52 × δ18O) values from -2%0 to +1%0, similar to previous studies, while one enstatite (En99) particle shows lower Δ17O value of -7±4%o (2σ). This compositional range has not been reported among 16O-poor particles in 81P/Wild 2, but is commonly observed among chondrules in carbonaceous chondrites and in particular in CR chondrites. The distribution in Δ17O indicates that 16O-poor 81P/Wild 2 particles are most similar to chondrules (and their fragments) in the CR chondrites and Tagish Lake-like WIS91600 chondrite chondrule silicate grains, which indicates that they likely come from a reservoir with similar dust/ice ratios as CR chondrites and WIS91600. However, differences in the Mg# distribution imply that the 81P/Wild 2 reservoir was comparatively more oxidized, with a higher dust enrichment. Two nearly pure enstatite grains from track 172 are significantly enriched in 16O, with δ18O values of -51.2 ± 1.5%0 (2σ) and -43.0 ± 1.3% (2σ), respectively, and Δ17O values of -22.3 ± 1.9% (2σ) and -21.3 ± 2.3%0 (2σ), respectively. They are the first 16O-rich pyroxenes found among 81P/Wild 2 particles, with similar Δ17O values to those of 16O-rich low-iron, manganese-enriched (LIME) olivine and CAI (calcium and aluminum-rich inclusions) -like particles from 81P/Wild 2. The major element and oxygen isotopic compositions of the pyroxenes are similar to those of enstatite in amoeboid olivine aggregates (AOAs) in primitive chondrites, in which 16O-rich pyroxenes have previously been found, and thus suggest a condensation origin.
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Affiliation(s)
- Céline Defouilloy
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Daisuke Nakashima
- Division of Earth and Planetary Materials Science, Tohoku University, Miyagi 980-8578, Japan
| | - David J. Joswiak
- Department of Astronomy, University of Washington, Seattle, WA 98195, USA
| | - Donald E. Brownlee
- Department of Astronomy, University of Washington, Seattle, WA 98195, USA
| | - Travis J. Tenner
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Noriko T. Kita
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
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Chakraborty S, Jackson TL, Rude B, Ahmed M, Thiemens MH. Nitrogen isotopic fractionations in the low temperature (80 K) vacuum ultraviolet photodissociation of N2. J Chem Phys 2016. [DOI: 10.1063/1.4962447] [Citation(s) in RCA: 10] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/11/2023] Open
Affiliation(s)
- Subrata Chakraborty
- Department of Chemistry and Biochemistry, University of California, San Diego, 9500 Gilman Drive, La Jolla, California 92093-0356, USA
| | - Teresa L. Jackson
- Department of Chemistry and Biochemistry, University of California, San Diego, 9500 Gilman Drive, La Jolla, California 92093-0356, USA
| | - Bruce Rude
- Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA
| | - Musahid Ahmed
- Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA
| | - M. H. Thiemens
- Department of Chemistry and Biochemistry, University of California, San Diego, 9500 Gilman Drive, La Jolla, California 92093-0356, USA
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Mandt K, Mousis O, Marty B, Cavalié T, Harris W, Hartogh P, Willacy K. Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites. SPACE SCIENCE REVIEWS 2015; 197:297-342. [PMID: 31105346 PMCID: PMC6525011 DOI: 10.1007/s11214-015-0161-z] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
Comets play a dual role in understanding the formation and evolution of the solar system. First, the composition of comets provides information about the origin of the giant planets and their moons because comets formed early and their composition is not expected to have evolved significantly since formation. They, therefore serve as a record of conditions during the early stages of solar system formation. Once comets had formed, their orbits were perturbed allowing them to travel into the inner solar system and impact the planets. In this way they contributed to the volatile inventory of planetary atmospheres. We review here how knowledge of comet composition up to the time of the Rosetta mission has contributed to understanding the formation processes of the giant planets, their moons and small icy bodies in the solar system. We also discuss how comets contributed to the volatile inventories of the giant and terrestrial planets.
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Affiliation(s)
- K.E. Mandt
- Southwest Research Institute, San Antonio, TX, USA
| | - O. Mousis
- Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388, Marseille, France
| | - B. Marty
- CRPG-CNRS, Nancy-Université, Vandoeuvre-lès-Nancy, France
| | - T. Cavalié
- Max Planck Institute for Solar System Research, Göttingen, Germany
| | - W. Harris
- University of Arizona, Tucson, AZ, USA
| | - P. Hartogh
- Max Planck Institute for Solar System Research, Göttingen, Germany
| | - K. Willacy
- Jet Propulsion Laboratory, Pasadena, CA, USA
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25
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Wirtz T, Philipp P, Audinot JN, Dowsett D, Eswara S. High-resolution high-sensitivity elemental imaging by secondary ion mass spectrometry: from traditional 2D and 3D imaging to correlative microscopy. NANOTECHNOLOGY 2015; 26:434001. [PMID: 26436905 DOI: 10.1088/0957-4484/26/43/434001] [Citation(s) in RCA: 48] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/26/2023]
Abstract
Secondary ion mass spectrometry (SIMS) constitutes an extremely sensitive technique for imaging surfaces in 2D and 3D. Apart from its excellent sensitivity and high lateral resolution (50 nm on state-of-the-art SIMS instruments), advantages of SIMS include high dynamic range and the ability to differentiate between isotopes. This paper first reviews the underlying principles of SIMS as well as the performance and applications of 2D and 3D SIMS elemental imaging. The prospects for further improving the capabilities of SIMS imaging are discussed. The lateral resolution in SIMS imaging when using the microprobe mode is limited by (i) the ion probe size, which is dependent on the brightness of the primary ion source, the quality of the optics of the primary ion column and the electric fields in the near sample region used to extract secondary ions; (ii) the sensitivity of the analysis as a reasonable secondary ion signal, which must be detected from very tiny voxel sizes and thus from a very limited number of sputtered atoms; and (iii) the physical dimensions of the collision cascade determining the origin of the sputtered ions with respect to the impact site of the incident primary ion probe. One interesting prospect is the use of SIMS-based correlative microscopy. In this approach SIMS is combined with various high-resolution microscopy techniques, so that elemental/chemical information at the highest sensitivity can be obtained with SIMS, while excellent spatial resolution is provided by overlaying the SIMS images with high-resolution images obtained by these microscopy techniques. Examples of this approach are given by presenting in situ combinations of SIMS with transmission electron microscopy (TEM), helium ion microscopy (HIM) and scanning probe microscopy (SPM).
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Affiliation(s)
- T Wirtz
- Advanced Instrumentation for Ion Nano-Analytics (AINA), MRT Department, Luxembourg Institute of Science and Technology (LIST), 41 rue du Brill, L-4422 Belvaux, Luxembourg
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Gainsforth Z, Butterworth AL, Stodolna J, Westphal AJ, Huss GR, Nagashima K, Ogliore R, Brownlee DE, Joswiak D, Tyliszczak T, Simionovici AS. Constraints on the formation environment of two chondrule-like igneous particles from Comet 81P/Wild 2. METEORITICS & PLANETARY SCIENCE 2015; 50:976-1004. [PMID: 31031558 PMCID: PMC6480418 DOI: 10.1111/maps.12445] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
Using chemical and petrologic evidence and modeling, we deduce that two chondrule-like particles named Iris and Callie, from Stardust cometary track C2052,12,74, formed in an environment very similar to that seen for type II chondrules in meteorites. Iris was heated near liquidus, equilibrated, and cooled at ≤ 100 °C/hr and within ≈ 2 log units of the IW buffer with a high partial pressure of Na such as would be present with dust enrichments of ≈ 103. There was no detectable metamorphic, nebular or aqueous alteration. In previous work Ogliore et al. (2012) reported that Iris formed late, > 3 Myr after CAIs, assuming 26Al was homogenously distributed, and was rich in heavy oxygen. Iris may be similar to assemblages found only in interplanetary dust particles and Stardust cometary samples called Kool particles. Callie is chemically and isotopically very similar but not identical to Iris.
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Affiliation(s)
- Zack Gainsforth
- Space Sciences Laboratory, University of California at Berkeley, Berkeley, CA 94720 USA
| | - Anna L. Butterworth
- Space Sciences Laboratory, University of California at Berkeley, Berkeley, CA 94720 USA
| | - Julien Stodolna
- Space Sciences Laboratory, University of California at Berkeley, Berkeley, CA 94720 USA
| | - Andrew J. Westphal
- Space Sciences Laboratory, University of California at Berkeley, Berkeley, CA 94720 USA
| | - Gary R. Huss
- Hawai’i Institute of Geophysics and Planetology, University of Hawai’i at Mānoa, Honolulu, HI 96822 USA
| | - Kazu Nagashima
- Hawai’i Institute of Geophysics and Planetology, University of Hawai’i at Mānoa, Honolulu, HI 96822 USA
| | - Ryan Ogliore
- Hawai’i Institute of Geophysics and Planetology, University of Hawai’i at Mānoa, Honolulu, HI 96822 USA
| | - Donald E. Brownlee
- Department of Astronomy, University of Washington, Seattle, WA 98195 USA
| | - David Joswiak
- Department of Astronomy, University of Washington, Seattle, WA 98195 USA
| | - Tolek Tyliszczak
- Advanced Light Source, Lawrence Berkeley National Laboratory, Berkeley, CA 94720 USA
| | - Alexandre S. Simionovici
- Institut des Sciences de la Terre, Observatoire des Sciences de l’Univers de Grenoble, Grenoble, France
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Nanoscale infrared spectroscopy as a non-destructive probe of extraterrestrial samples. Nat Commun 2014; 5:5445. [PMID: 25487365 DOI: 10.1038/ncomms6445] [Citation(s) in RCA: 45] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/03/2014] [Accepted: 10/02/2014] [Indexed: 11/08/2022] Open
Abstract
Advances in the spatial resolution of modern analytical techniques have tremendously augmented the scientific insight gained from the analysis of natural samples. Yet, while techniques for the elemental and structural characterization of samples have achieved sub-nanometre spatial resolution, infrared spectral mapping of geochemical samples at vibrational 'fingerprint' wavelengths has remained restricted to spatial scales >10 μm. Nevertheless, infrared spectroscopy remains an invaluable contactless probe of chemical structure, details of which offer clues to the formation history of minerals. Here we report on the successful implementation of infrared near-field imaging, spectroscopy and analysis techniques capable of sub-micron scale mineral identification within natural samples, including a chondrule from the Murchison meteorite and a cometary dust grain (Iris) from NASA's Stardust mission. Complementary to scanning electron microscopy, energy-dispersive X-ray spectroscopy and transmission electron microscopy probes, this work evidences a similarity between chondritic and cometary materials, and inaugurates a new era of infrared nano-spectroscopy applied to small and invaluable extraterrestrial samples.
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Wampfler SF, Jørgensen JK, Bizzarro M, Bisschop SE. Observations of nitrogen isotope fractionation in deeply embedded protostars. ASTRONOMY AND ASTROPHYSICS 2014; 572:A24. [PMID: 25684776 PMCID: PMC4326685 DOI: 10.1051/0004-6361/201423773] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/06/2023]
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.
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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
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Massive isotopic effect in vacuum UV photodissociation of N2 and implications for meteorite data. Proc Natl Acad Sci U S A 2014; 111:14704-9. [PMID: 25267643 DOI: 10.1073/pnas.1410440111] [Citation(s) in RCA: 20] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Nitrogen isotopic distributions in the solar system extend across an enormous range, from -400‰, in the solar wind and Jovian atmosphere, to about 5,000‰ in organic matter in carbonaceous chondrites. Distributions such as these require complex processing of nitrogen reservoirs and extraordinary isotope effects. While theoretical models invoke ion-neutral exchange reactions outside the protoplanetary disk and photochemical self-shielding on the disk surface to explain the variations, there are no experiments to substantiate these models. Experimental results of N2 photolysis at vacuum UV wavelengths in the presence of hydrogen are presented here, which show a wide range of enriched δ(15)N values from 648‰ to 13,412‰ in product NH3, depending upon photodissociation wavelength. The measured enrichment range in photodissociation of N2, plausibly explains the range of δ(15)N in extraterrestrial materials. This study suggests the importance of photochemical processing of the nitrogen reservoirs within the solar nebula.
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Mandt KE, Mousis O, Lunine J, Gautier D. PROTOSOLAR AMMONIA AS THE UNIQUE SOURCE OF TITAN's NITROGEN. THE ASTROPHYSICAL JOURNAL. LETTERS 2014; 788:L24. [PMID: 31069045 PMCID: PMC6501209 DOI: 10.1088/2041-8205/788/2/l24] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/06/2023]
Abstract
The origin of Titan's nitrogen-rich atmosphere is thought to be ammonia ice, but this has not yet been confirmed. Furthermore, it is uncertain whether the building blocks of Titan formed within the Saturnian subnebula or in the colder protosolar nebula (PSN). Recent measurements of the nitrogen isotope ratio in cometary ammonia, combined with evolutionary constraints on the nitrogen isotopes in Titan's atmosphere provide firm evidence that the nitrogen in Titan's atmosphere must have originated as ammonia ice formed in the PSN under conditions similar to that of cometary formation. This result has important implications for the projected D/H ratio in cometary methane, nitrogen isotopic fractionation in the PSN and the source of nitrogen for Earth's atmosphere.
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Affiliation(s)
- Kathleen E Mandt
- Space Science and Engineering Division, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA
| | - Olivier Mousis
- Université de Franche-Comté, Institut UTINAM, CNRS/INSU, UMR 6213, Observatoire des Sciences de l'Univers de Besancon, France
| | - Jonathan Lunine
- Cornell University, Center for Radiophysics and Space Research, Ithaca, NY, USA
| | - Daniel Gautier
- Observatoire de Paris, 61 Avenue de l'Observatoire, F-75014 Paris, France
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31
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Sandford SA, Bernstein MP, Materese CK. The Infrared Spectra of Polycyclic Aromatic Hydrocarbons with Excess Peripheral H Atoms (H n-PAHs) and their Relation to the 3.4 and 6.9 µm PAH Emission Features. THE ASTROPHYSICAL JOURNAL. SUPPLEMENT SERIES 2013; 205:8. [PMID: 26435553 PMCID: PMC4589261 DOI: 10.1088/0067-0049/205/1/8] [Citation(s) in RCA: 17] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/30/2023]
Abstract
Polycyclic aromatic hydrocarbons (PAHs) are likely responsible for the family of infrared emission features seen in a wide variety of astrophysical environments. A potentially important subclass of these materials are PAHs whose edges contain excess H atoms (Hn-PAHs). This type of compound may be present in space, but it has been difficult to assess this possibility because of a lack of suitable laboratory spectra to assist with analysis of astronomical data. We present 4000-500 cm-1 (2.5-20 µm) infrared spectra of 23 Hn-PAHs and related molecules isolated in argon matrices under conditions suitable for interpretation of astronomical data. Spectra of molecules with mixed aromatic and aliphatic domains show characteristics that distinguish them from fully aromatic PAH equivalents. Two major changes occur as PAHs become more hydrogenated: (1) aromatic C-H stretching bands near 3.3 µm weaken and are replaced with stronger aliphatic bands near 3.4 µm, and (2) aromatic C-H out-of-plane bending mode bands in the 11-15 µm region shift and weaken concurrent with growth of a strong aliphatic -CH2-deformation mode near 6.9 µm. Implications for interpreting astronomical spectra are discussed with emphasis on the 3.4 and 6.9 µm features. Laboratory data is compared with emission spectra from IRAS 21282+5050, an object with normal PAH emission features, and IRAS 22272+5435 and IRAS 0496+3429, two protoplanetary nebulae with abnormally large 3.4 µm features. We show that 'normal' PAH emission objects contain relatively few Hn-PAHs in their emitter populations, but less evolved protoplanetary nebulae may contain significant abundances of these molecules.
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Affiliation(s)
- Scott A Sandford
- NASA-Ames Research Center, Mail Stop 245-6, Moffett Field, CA 94035-1000
| | - Max P Bernstein
- NASA-Ames Research Center, Mail Stop 245-6, Moffett Field, CA 94035-1000 ; NASA Headquarters, Mail Code 3K39, 300 E Street SW, Washington, DC 20546
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Bheekhun N, Abu Talib AR, Hassan MR. Aerogels in Aerospace: An Overview. ADVANCES IN MATERIALS SCIENCE AND ENGINEERING 2013; 2013:1-18. [DOI: 10.1155/2013/406065] [Citation(s) in RCA: 49] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 09/02/2023]
Abstract
Aerogels are highly porous structures prepared via a sol-gel process and supercritical drying technology. Among the classes of aerogels, silica aerogel exhibits the most remarkable physical properties, possessing lower density, thermal conductivity, refractive index, and dielectric constant than any solids. Its acoustical property is such that it can absorb the sound waves reducing speed to 100 m/s compared to 332 m/s for air. However, when it comes to commercialization, the result is not as expected. It seems that mass production, particularly in the aerospace industry, has dawdled behind. This paper highlights the evolution of aerogels in general and discusses the functions and significances of silica aerogel in previous astronautical applications. Future outer-space applications have been proposed as per the current research trend. Finally, the implementation of conventional silica aerogel in aeronautics is argued with an alternative known as Maerogel.
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Affiliation(s)
- Nadiir Bheekhun
- Department of Aerospace Engineering, Propulsion and Thermofluids Group, Universiti Putra Malaysia, 43400 Serdang, Selangor Darul Ehsan, Malaysia
| | - Abd. Rahim Abu Talib
- Department of Aerospace Engineering, Propulsion and Thermofluids Group, Universiti Putra Malaysia, 43400 Serdang, Selangor Darul Ehsan, Malaysia
| | - Mohd Roshdi Hassan
- Department of Mechanical and Manufacturing Engineering, Universiti Putra Malaysia, 43400 Serdang, Selangor Darul Ehsan, Malaysia
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Tsou P, Brownlee DE, McKay CP, Anbar AD, Yano H, Altwegg K, Beegle LW, Dissly R, Strange NJ, Kanik I. LIFE: Life Investigation For Enceladus A Sample Return Mission Concept in Search for Evidence of Life. ASTROBIOLOGY 2012; 12:730-742. [PMID: 22970863 DOI: 10.1089/ast.2011.0813] [Citation(s) in RCA: 10] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
Life Investigation For Enceladus (LIFE) presents a low-cost sample return mission to Enceladus, a body with high astrobiological potential. There is ample evidence that liquid water exists under ice coverage in the form of active geysers in the "tiger stripes" area of the southern Enceladus hemisphere. This active plume consists of gas and ice particles and enables the sampling of fresh materials from the interior that may originate from a liquid water source. The particles consist mostly of water ice and are 1-10 μ in diameter. The plume composition shows H(2)O, CO(2), CH(4), NH(3), Ar, and evidence that more complex organic species might be present. Since life on Earth exists whenever liquid water, organics, and energy coexist, understanding the chemical components of the emanating ice particles could indicate whether life is potentially present on Enceladus. The icy worlds of the outer planets are testing grounds for some of the theories for the origin of life on Earth. The LIFE mission concept is envisioned in two parts: first, to orbit Saturn (in order to achieve lower sampling speeds, approaching 2 km/s, and thus enable a softer sample collection impact than Stardust, and to make possible multiple flybys of Enceladus); second, to sample Enceladus' plume, the E ring of Saturn, and the Titan upper atmosphere. With new findings from these samples, NASA could provide detailed chemical and isotopic and, potentially, biological compositional context of the plume. Since the duration of the Enceladus plume is unpredictable, it is imperative that these samples are captured at the earliest flight opportunity. If LIFE is launched before 2019, it could take advantage of a Jupiter gravity assist, which would thus reduce mission lifetimes and launch vehicle costs. The LIFE concept offers science returns comparable to those of a Flagship mission but at the measurably lower sample return costs of a Discovery-class mission.
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Affiliation(s)
- Peter Tsou
- Sample Exploration Systems La Cañada, California, USA
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Thiemens MH, Chakraborty S, Dominguez G. The Physical Chemistry of Mass-Independent Isotope Effects and Their Observation in Nature. Annu Rev Phys Chem 2012; 63:155-77. [DOI: 10.1146/annurev-physchem-032511-143657] [Citation(s) in RCA: 56] [Impact Index Per Article: 4.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Abstract
Historically, the physical chemistry of isotope effects and precise measurements in samples from nature have provided information on processes that could not have been obtained otherwise. With the discovery of a mass-independent isotopic fractionation during the formation of ozone, a new physical chemical basis for isotope effects required development. Combined theoretical and experimental developments have broadened this understanding and extended the range of chemical systems where these unique effects occur. Simultaneously, the application of mass-independent isotopic measurements to an extensive range of both terrestrial and extraterrestrial systems has furthered the understanding of events such as solar system origin and evolution and planetary atmospheric chemistry, present and past.
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Affiliation(s)
- Mark H. Thiemens
- Department of Chemistry and Biochemistry, University of California San Diego, La Jolla, California 92093;,
| | - Subrata Chakraborty
- Department of Chemistry and Biochemistry, University of California San Diego, La Jolla, California 92093;,
| | - Gerardo Dominguez
- Department of Physics, California State University, San Marcos, San Marcos, California 92096
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Savin DW, Brickhouse NS, Cowan JJ, Drake RP, Federman SR, Ferland GJ, Frank A, Gudipati MS, Haxton WC, Herbst E, Profumo S, Salama F, Ziurys LM, Zweibel EG. The impact of recent advances in laboratory astrophysics on our understanding of the cosmos. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2012; 75:036901. [PMID: 22790424 DOI: 10.1088/0034-4885/75/3/036901] [Citation(s) in RCA: 10] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
An emerging theme in modern astrophysics is the connection between astronomical observations and the underlying physical phenomena that drive our cosmos. Both the mechanisms responsible for the observed astrophysical phenomena and the tools used to probe such phenomena-the radiation and particle spectra we observe-have their roots in atomic, molecular, condensed matter, plasma, nuclear and particle physics. Chemistry is implicitly included in both molecular and condensed matter physics. This connection is the theme of the present report, which provides a broad, though non-exhaustive, overview of progress in our understanding of the cosmos resulting from recent theoretical and experimental advances in what is commonly called laboratory astrophysics. This work, carried out by a diverse community of laboratory astrophysicists, is increasingly important as astrophysics transitions into an era of precise measurement and high fidelity modeling.
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Affiliation(s)
- D W Savin
- Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA
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Polerecky L, Adam B, Milucka J, Musat N, Vagner T, Kuypers MMM. Look@NanoSIMS--a tool for the analysis of nanoSIMS data in environmental microbiology. Environ Microbiol 2012; 14:1009-23. [PMID: 22221878 DOI: 10.1111/j.1462-2920.2011.02681.x] [Citation(s) in RCA: 132] [Impact Index Per Article: 11.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/27/2022]
Abstract
We describe an open-source freeware programme for high throughput analysis of nanoSIMS (nanometre-scale secondary ion mass spectrometry) data. The programme implements basic data processing and analytical functions, including display and drift-corrected accumulation of scanned planes, interactive and semi-automated definition of regions of interest (ROIs), and export of the ROIs' elemental and isotopic composition in graphical and text-based formats. Additionally, the programme offers new functions that were custom-designed to address the needs of environmental microbiologists. Specifically, it allows manual and automated classification of ROIs based on the information that is derived either from the nanoSIMS dataset itself (e.g. from labelling achieved by halogen in situ hybridization) or is provided externally (e.g. as a fluorescence in situ hybridization image). Moreover, by implementing post-processing routines coupled to built-in statistical tools, the programme allows rapid synthesis and comparative analysis of results from many different datasets. After validation of the programme, we illustrate how these new processing and analytical functions increase flexibility, efficiency and depth of the nanoSIMS data analysis. Through its custom-made and open-source design, the programme provides an efficient, reliable and easily expandable tool that can help a growing community of environmental microbiologists and researchers from other disciplines process and analyse their nanoSIMS data.
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Affiliation(s)
- Lubos Polerecky
- Max-Planck Institute for Marine Microbiology, Bremen, Germany.
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Abstract
The biological record suggests that life on Earth arose as soon as conditions were favorable, which indicates that life either originated quickly, or arrived from elsewhere to seed Earth. Experimental research under the theme of “astrobiology” has produced data that some view as strong evidence for the second possibility, known as the panspermia hypothesis. While it is not unreasonable to consider the possibility that Earth’s life originated elsewhere and potentially much earlier, we conclude that the current literature offers no definitive evidence to support this hypothesis.
Chladni’s view, that they fall from the skies, pronounced in 1795, was ridiculed by the learned men of the times. (Rachel, 1881) Evidence of life on Mars, even if only in the distant past, would finally answer the age-old question of whether living beings on Earth are alone in the universe. The magnitude of such a discovery is illustrated by President Bill Clinton’s appearance at a 1996 press conference to announce that proof had been found at last. A meteorite chipped from the surface of the Red Planet some 15 million years ago appeared to contain the fossil remains of tiny life-forms that indicated life had once existed on Mars. (Young and Martel, 2010)
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Abstract
AbstractThe insoluble organic material preserved in primitive chondritic meteorites shares many similarities with the refractory organic material in interplanetary dust particles and comets, suggesting that there is a genetic link between the organic matter in objects that formed between ~3 AU and ~30 AU from the Sun. These similarities include large D and 15N enrichments in bulk and even more extreme enrichments in isotopic hotspots. The enrichments attest to formation in very cold environments, either in the outer Solar System or the protosolar molecular cloud. There are many properties of this organic material that are consistent with an interstellar origin, but a Solar System origin cannot be ruled out. Similar organic material is presumably an important component of most protoplanetary disks, and heating or sputtering of this material would be a source of PAHs in disks. The soluble organic matter was more heavily effected by processes on the chondritic parent bodies than the insoluble material. Amino acids, for instance, probably formed by reaction of ketones and aldehydes with NH3 and HCN. The accretion of the relatively volatile NH3 and HCN, presumably in ices, strengthens the chondrite-comet connection. However, unlike most comets the water in chondrites, when it was accreted, had D/H ratios that were similar to or depleted relative to Earth.
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Abstract
AbstractComets are made of ices, organics and minerals that record the chemistry of the outer regions of the primitive solar nebula where they agglomerated 4.6 Gyr ago. Compositional analyses of comets can provide important clues on the chemical and physical processes that occurred in the early phases of Solar System formation, and possibly in the natal molecular cloud that predated the formation of the solar nebula. This paper presents a short review of our present knowledge of the composition of comets. Implications for the origin of cometary materials are discussed.
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McKeegan KD, Kallio APA, Heber VS, Jarzebinski G, Mao PH, Coath CD, Kunihiro T, Wiens RC, Nordholt JE, Moses RW, Reisenfeld DB, Jurewicz AJG, Burnett DS. The oxygen isotopic composition of the Sun inferred from captured solar wind. Science 2011; 332:1528-32. [PMID: 21700868 DOI: 10.1126/science.1204636] [Citation(s) in RCA: 271] [Impact Index Per Article: 20.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
All planetary materials sampled thus far vary in their relative abundance of the major isotope of oxygen, (16)O, such that it has not been possible to define a primordial solar system composition. We measured the oxygen isotopic composition of solar wind captured and returned to Earth by NASA's Genesis mission. Our results demonstrate that the Sun is highly enriched in (16)O relative to the Earth, Moon, Mars, and bulk meteorites. Because the solar photosphere preserves the average isotopic composition of the solar system for elements heavier than lithium, we conclude that essentially all rocky materials in the inner solar system were enriched in (17)O and (18)O, relative to (16)O, by ~7%, probably via non-mass-dependent chemistry before accretion of the first planetesimals.
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Affiliation(s)
- K D McKeegan
- Department of Earth and Space Sciences, University of California-Los Angeles (UCLA), Los Angeles, CA 90095-1567, USA.
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Synthesis and characterization of a nanocrystalline diamond aerogel. Proc Natl Acad Sci U S A 2011; 108:8550-3. [PMID: 21555550 DOI: 10.1073/pnas.1010600108] [Citation(s) in RCA: 42] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Aerogel materials have myriad scientific and technological applications due to their large intrinsic surface areas and ultralow densities. However, creating a nanodiamond aerogel matrix has remained an outstanding and intriguing challenge. Here we report the high-pressure, high-temperature synthesis of a diamond aerogel from an amorphous carbon aerogel precursor using a laser-heated diamond anvil cell. Neon is used as a chemically inert, near-hydrostatic pressure medium that prevents collapse of the aerogel under pressure by conformally filling the aerogel's void volume. Electron and X-ray spectromicroscopy confirm the aerogel morphology and composition of the nanodiamond matrix. Time-resolved photoluminescence measurements of recovered material reveal the formation of both nitrogen- and silicon- vacancy point-defects, suggesting a broad range of applications for this nanocrystalline diamond aerogel.
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42
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Establishing a molecular relationship between chondritic and cometary organic solids. Proc Natl Acad Sci U S A 2011; 108:19171-6. [PMID: 21464292 DOI: 10.1073/pnas.1015913108] [Citation(s) in RCA: 65] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Multidimensional solid-state NMR spectroscopy is used to refine the identification and abundance determination of functional groups in insoluble organic matter (IOM) isolated from a carbonaceous chondrite (Murchison, CM2). It is shown that IOM is composed primarily of highly substituted single ring aromatics, substituted furan/pyran moieties, highly branched oxygenated aliphatics, and carbonyl groups. A pathway for producing an IOM-like molecular structure through formaldehyde polymerization is proposed and tested experimentally. Solid-state (13)C NMR analysis of aqueously altered formaldehyde polymer reveals considerable similarity with chondritic IOM. Carbon X-ray absorption near edge structure spectroscopy of formaldehyde polymer reveals the presence of similar functional groups across certain Comet 81P/Wild 2 organic solids, interplanetary dust particles, and primitive IOM. Variation in functional group concentration amongst these extraterrestrial materials is understood to be a result of various degrees of processing in the parent bodies, in space, during atmospheric entry, etc. These results support the hypothesis that chondritic IOM and cometary refractory organic solids are related chemically and likely were derived from formaldehyde polymer. The fine-scale morphology of formaldehyde polymer produced in the experiment reveals abundant nanospherules that are similar in size and shape to organic nanoglobules that are ubiquitous in primitive chondrites.
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Nanodiamonds do not provide unique evidence for a Younger Dryas impact. Proc Natl Acad Sci U S A 2011; 108:40-4. [PMID: 21173270 DOI: 10.1073/pnas.1007695108] [Citation(s) in RCA: 32] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Microstructural, δ(13)C isotope and C/N ratio investigations were conducted on excavated material from the black Younger Dryas boundary in Lommel, Belgium, aiming for a characterisation of the carbon content and structures. Cubic diamond nanoparticles are found in large numbers. The larger ones with diameters around or above 10 nm often exhibit single or multiple twins. The smaller ones around 5 nm in diameter are mostly defect-free. Also larger flake-like particles, around 100 nm in lateral dimension, with a cubic diamond structure are observed as well as large carbon onion structures. The combination of these characteristics does not yield unique evidence for an exogenic impact related to the investigated layer.
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Sivaraman B, Mebel AM, Mason NJ, Babikov D, Kaiser RI. On the electron-induced isotope fractionation in low temperature32O2/36O2ices—ozone as a case study. Phys Chem Chem Phys 2011; 13:421-7. [DOI: 10.1039/c0cp00448k] [Citation(s) in RCA: 12] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/22/2023]
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Affiliation(s)
- Larry R Nittler
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, NW, Washington, DC 20015, USA.
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46
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Duprat J, Dobrica E, Engrand C, Aleon J, Marrocchi Y, Mostefaoui S, Meibom A, Leroux H, Rouzaud JN, Gounelle M, Robert F. Extreme Deuterium Excesses in Ultracarbonaceous Micrometeorites from Central Antarctic Snow. Science 2010; 328:742-5. [DOI: 10.1126/science.1184832] [Citation(s) in RCA: 137] [Impact Index Per Article: 9.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
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Matzel JEP, Ishii HA, Joswiak D, Hutcheon ID, Bradley JP, Brownlee D, Weber PK, Teslich N, Matrajt G, McKeegan KD, MacPherson GJ. Constraints on the formation age of cometary material from the NASA Stardust mission. Science 2010; 328:483-6. [PMID: 20185683 DOI: 10.1126/science.1184741] [Citation(s) in RCA: 64] [Impact Index Per Article: 4.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
We measured the 26Al-26Mg isotope systematics of a approximately 5-micrometer refractory particle, Coki, returned from comet 81P/Wild 2 in order to relate the time scales of formation of cometary inclusions to their meteoritic counterparts. The data show no evidence of radiogenic 26Mg and define an upper limit to the abundance of 26Al at the time of particle formation: 26Al/27Al < 1 x 10(-5). The absence of 26Al indicates that Coki formed >1.7 million years after the oldest solids in the solar system, calcium- and aluminum-rich inclusions (CAIs). The data suggest that high-temperature inner solar system material formed, was subsequently transferred to the Kuiper Belt, and was incorporated into comets several million years after CAI formation.
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Affiliation(s)
- J E P Matzel
- Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, Livermore, CA 94550, USA.
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Holzapfel C, Soldera F, Vollmer C, Hoppe P, Mücklich F. TEM foil preparation of sub-micrometre sized individual grains by focused ion beam technique. J Microsc 2009; 235:59-66. [PMID: 19566627 DOI: 10.1111/j.1365-2818.2009.03181.x] [Citation(s) in RCA: 14] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
Abstract
Analysis of presolar silicate grains provides new knowledge on interstellar and circumstellar environments and can be used to test models of the Galactic chemical evolution. However, structural information of these grains is rare because sample preparation for transmission electron microscopy is very difficult due to the small dimensions of these grains (<0.5 mum). With the use of the focused ion beam technique thin foils from these grains for transmission electron microscopy analysis can be prepared. Nevertheless, reaching the required precision of some tens of nanometres for the preparation of the transmission electron microscopy foil in the place of interest is not trivial. Furthermore, in the current samples, the grain of interest can only be identified by its different isotopic composition; i.e. there is no contrast difference in scanning electron microscopy or transmission electron microscopy images which allow the identification of the grain. Therefore, the grain has to be marked in some way before preparing the transmission electron microscopy foil. In the present paper, a method for transmission electron microscopy foil preparation of grains about 200 to 400 nm in diameter is presented. The method utilizes marking of the grain by Pt deposition and milling of holes to aid in the exact orientation of the transmission electron microscopy foil with respect to the grain. The proposed method will be explained in detail by using an example grain.
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Affiliation(s)
- C Holzapfel
- Department Materials Science, Saarland University, Saarbrücken, Germany
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50
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Pristine extraterrestrial material with unprecedented nitrogen isotopic variation. Proc Natl Acad Sci U S A 2009; 106:10522-7. [PMID: 19528640 DOI: 10.1073/pnas.0901546106] [Citation(s) in RCA: 22] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Pristine meteoritic materials carry light element isotopic fractionations that constrain physiochemical conditions during solar system formation. Here we report the discovery of a unique xenolith in the metal-rich chondrite Isheyevo. Its fine-grained, highly pristine mineralogy has similarity with interplanetary dust particles (IDPs), but the volume of the xenolith is more than 30,000 times that of a typical IDP. Furthermore, an extreme continuum of N isotopic variation is present in this xenolith: from very light N isotopic composition (delta(15)N(AIR) = -310 +/- 20 per thousand), similar to that inferred for the solar nebula, to the heaviest ratios measured in any solar system material (delta(15)N(AIR) = 4,900 +/- 300 per thousand). At the same time, its hydrogen and carbon isotopic compositions exhibit very little variation. This object poses serious challenges for existing models for the origin of light element isotopic anomalies.
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