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Yokoyama T, Wadhwa M, Iizuka T, Rai V, Gautam I, Hibiya Y, Masuda Y, Haba MK, Fukai R, Hines R, Phelan N, Abe Y, Aléon J, Alexander CM, Amari S, Amelin Y, Bajo KI, Bizzarro M, Bouvier A, Carlson RW, Chaussidon M, Choi BG, Dauphas N, Davis AM, Di Rocco T, Fujiya W, Hidaka H, Homma H, Hoppe P, Huss GR, Ichida K, Ireland T, Ishikawa A, Itoh S, Kawasaki N, Kita NT, Kitajima K, Kleine T, Komatani S, Krot AN, Liu MC, McKeegan KD, Morita M, Motomura K, Moynier F, Nakai I, Nagashima K, Nguyen A, Nittler L, Onose M, Pack A, Park C, Piani L, Qin L, Russell S, Sakamoto N, Schönbächler M, Tafla L, Tang H, Terada K, Terada Y, Usui T, Wada S, Walker RJ, Yamashita K, Yin QZ, Yoneda S, Young ED, Yui H, Zhang AC, Nakamura T, Naraoka H, Noguchi T, Okazaki R, Sakamoto K, Yabuta H, Abe M, Miyazaki A, Nakato A, Nishimura M, Okada T, Yada T, Yogata K, Nakazawa S, Saiki T, Tanaka S, Terui F, Tsuda Y, Watanabe SI, Yoshikawa M, Tachibana S, Yurimoto H. Water circulation in Ryugu asteroid affected the distribution of nucleosynthetic isotope anomalies in returned sample. SCIENCE ADVANCES 2023; 9:eadi7048. [PMID: 37939187 PMCID: PMC10631728 DOI: 10.1126/sciadv.adi7048] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/13/2023] [Accepted: 10/05/2023] [Indexed: 11/10/2023]
Abstract
Studies of material returned from Cb asteroid Ryugu have revealed considerable mineralogical and chemical heterogeneity, stemming primarily from brecciation and aqueous alteration. Isotopic anomalies could have also been affected by delivery of exogenous clasts and aqueous mobilization of soluble elements. Here, we show that isotopic anomalies for mildly soluble Cr are highly variable in Ryugu and CI chondrites, whereas those of Ti are relatively uniform. This variation in Cr isotope ratios is most likely due to physicochemical fractionation between 54Cr-rich presolar nanoparticles and Cr-bearing secondary minerals at the millimeter-scale in the bulk samples, likely due to extensive aqueous alteration in their parent bodies that occurred [Formula: see text] after Solar System birth. In contrast, Ti isotopes were marginally affected by this process. Our results show that isotopic heterogeneities in asteroids are not all nebular or accretionary in nature but can also reflect element redistribution by water.
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Affiliation(s)
- Tetsuya Yokoyama
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Tsuyoshi Iizuka
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Vinai Rai
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Ikshu Gautam
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Yuki Hibiya
- Research Center for Advanced Science and Technology, The University of Tokyo, Tokyo 153-0041, Japan
| | - Yuki Masuda
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Makiko K. Haba
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Ryota Fukai
- ISAS/JSEC, JAXA, Sagamihara, 252-5210, Japan
| | - Rebekah Hines
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Nicole Phelan
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Yoshinari Abe
- Graduate School of Engineering, Tokyo Denki University, Tokyo 120-8551, Japan
| | - Jérôme Aléon
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Sorbonne Université, Museum National d'Histoire Naturelle, CNRS UMR 7590, IRD, 75005 Paris, France
| | | | - Sachiko Amari
- McDonnell Center for the Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, USA
- Geochemical Research Center, The University of Tokyo, Tokyo 113-0033, Japan
| | - Yuri Amelin
- Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, GD 510640, China
| | - Ken-ichi Bajo
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Martin Bizzarro
- Centre for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Copenhagen, K 1350, Denmark
| | - Audrey Bouvier
- Bayerisches Geoinstitut, Universität Bayreuth, Bayreuth, 95447, Germany
| | - Richard W. Carlson
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, 20015, USA
| | - Marc Chaussidon
- Université Paris Cité, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Byeon-Gak Choi
- Department of Earth Science Education, Seoul National University, Seoul 08826, Republic of Korea
| | - Nicolas Dauphas
- Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - Andrew M. Davis
- Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - Tommaso Di Rocco
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen, D-37077, Germany
| | - Wataru Fujiya
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Hiroshi Hidaka
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Hisashi Homma
- Osaka Application Laboratory, SBUWDX, Rigaku Corporation, Osaka 569-1146, Japan
| | - Peter Hoppe
- Max Planck Institute for Chemistry, Mainz, 55128, Germany
| | - Gary R. Huss
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Kiyohiro Ichida
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Trevor Ireland
- School of Earth and Environmental Sciences, The University of Queensland, St. Lucia, QLD 4072, Australia
| | - Akira Ishikawa
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Shoichi Itoh
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Noriyuki Kawasaki
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Noriko T. Kita
- Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Koki Kitajima
- Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Thorsten Kleine
- Max Planck Institute for Solar System Research, 37077, Göttingen, Germany
| | - Shintaro Komatani
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Alexander N. Krot
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Ming-Chang Liu
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Kevin D. McKeegan
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Mayu Morita
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | | | - Frédéric Moynier
- Université Paris Cité, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Izumi Nakai
- Department of Applied Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Kazuhide Nagashima
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Ann Nguyen
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
| | - Larry Nittler
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, 20015, USA
| | - Morihiko Onose
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Andreas Pack
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen, D-37077, Germany
| | - Changkun Park
- Earth-System Sciences, Korea Polar Research Institute, Incheon 21990, Korea
| | - Laurette Piani
- Centre de Recherches Pétrographiques et Géochimiques, CNRS - Université de Lorraine, 54500 Nancy, France
| | - Liping Qin
- CAS Key Laboratory of Crust-Mantle Materials and Environments, University of Science and Technology of China, School of Earth and Space Sciences, Anhui 230026, China
| | - Sara Russell
- Department of Earth Sciences, Natural History Museum, London, SW7 5BD, UK
| | - Naoya Sakamoto
- Isotope Imaging Laboratory, Creative Research Institution, Hokkaido University, Sapporo 001-0021, Japan
| | - Maria Schönbächler
- Institute for Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, 8092 Zurich, Switzerland
| | - Lauren Tafla
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Haolan Tang
- CAS Key Laboratory of Crust-Mantle Materials and Environments, University of Science and Technology of China, School of Earth and Space Sciences, Anhui 230026, China
| | - Kentaro Terada
- Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan
| | - Yasuko Terada
- Spectroscopy and Imaging, Japan Synchrotron Radiation Research Institute, Hyogo 679-5198, Japan
| | | | - Sohei Wada
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Richard J. Walker
- Department of Geology, University of Maryland, College Park, MD 20742, USA
| | - Katsuyuki Yamashita
- Graduate School of Natural Science and Technology, Okayama University, Okayama 700-8530, Japan
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California, Davis, CA 95616, USA
| | - Shigekazu Yoneda
- Department of Science and Engineering, National Museum of Nature and Science, Tsukuba 305-0005, Japan
| | - Edward D. Young
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Hiroharu Yui
- Department of Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Ai-Cheng Zhang
- School of Earth Sciences and Engineering, Nanjing University, Nanjing 210023, China
| | - Tomoki Nakamura
- Department of Earth Science, Tohoku University, Sendai 980-8578, Japan
| | - Hiroshi Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Takaaki Noguchi
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Ryuji Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | | | - Hikaru Yabuta
- Earth and Planetary Systems Science Program, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - Masanao Abe
- ISAS/JSEC, JAXA, Sagamihara, 252-5210, Japan
| | | | - Aiko Nakato
- ISAS/JSEC, JAXA, Sagamihara, 252-5210, Japan
| | | | | | - Toru Yada
- ISAS/JSEC, JAXA, Sagamihara, 252-5210, Japan
| | | | | | | | | | - Fuyuto Terui
- Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | | | - Sei-ichiro Watanabe
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | | | - Shogo Tachibana
- UTokyo Organization for Planetary and Space Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Hisayoshi Yurimoto
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
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2
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Deng Z, Schiller M, Jackson MG, Millet MA, Pan L, Nikolajsen K, Saji NS, Huang D, Bizzarro M. Earth's evolving geodynamic regime recorded by titanium isotopes. Nature 2023; 621:100-104. [PMID: 37495699 PMCID: PMC10482698 DOI: 10.1038/s41586-023-06304-0] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/24/2022] [Accepted: 06/09/2023] [Indexed: 07/28/2023]
Abstract
Earth's mantle has a two-layered structure, with the upper and lower mantle domains separated by a seismic discontinuity at about 660 km (refs. 1,2). The extent of mass transfer between these mantle domains throughout Earth's history is, however, poorly understood. Continental crust extraction results in Ti-stable isotopic fractionation, producing isotopically light melting residues3-7. Mantle recycling of these components can impart Ti isotope variability that is trackable in deep time. We report ultrahigh-precision 49Ti/47Ti ratios for chondrites, ancient terrestrial mantle-derived lavas ranging from 3.8 to 2.0 billion years ago (Ga) and modern ocean island basalts (OIBs). Our new Ti bulk silicate Earth (BSE) estimate based on chondrites is 0.052 ± 0.006‰ heavier than the modern upper mantle sampled by normal mid-ocean ridge basalts (N-MORBs). The 49Ti/47Ti ratio of Earth's upper mantle was chondritic before 3.5 Ga and evolved to a N-MORB-like composition between approximately 3.5 and 2.7 Ga, establishing that more continental crust was extracted during this epoch. The +0.052 ± 0.006‰ offset between BSE and N-MORBs requires that <30% of Earth's mantle equilibrated with recycled crustal material, implying limited mass exchange between the upper and lower mantle and, therefore, preservation of a primordial lower-mantle reservoir for most of Earth's geologic history. Modern OIBs record variable 49Ti/47Ti ratios ranging from chondritic to N-MORBs compositions, indicating continuing disruption of Earth's primordial mantle. Thus, modern-style plate tectonics with high mass transfer between the upper and lower mantle only represents a recent feature of Earth's history.
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Affiliation(s)
- Zhengbin Deng
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark.
- Deep Space Exploration Laboratory/CAS Key Laboratory of Crust-Mantle Materials and Environments, School of Earth and Space Sciences, University of Science and Technology of China, Hefei, China.
| | - Martin Schiller
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Matthew G Jackson
- Department of Earth Science, University of California, Santa Barbara, Santa Barbara, CA, USA
| | - Marc-Alban Millet
- School of Earth and Environmental Sciences, Cardiff University, Cardiff, UK
| | - Lu Pan
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
- Deep Space Exploration Laboratory/Laboratory of Seismology and Physics of Earth's Interior, School of Earth and Space Sciences, University of Science and Technology of China, Hefei, China
| | - Katrine Nikolajsen
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Nikitha S Saji
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Dongyang Huang
- Institute of Geochemistry and Petrology, ETH Zürich, Zürich, Switzerland
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
- Institut de Physique du Globe de Paris, Université Paris Cité, Paris, France
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3
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Krestianinov E, Amelin Y, Yin QZ, Cary P, Huyskens MH, Miller A, Dey S, Hibiya Y, Tang H, Young ED, Pack A, Di Rocco T. Igneous meteorites suggest Aluminium-26 heterogeneity in the early Solar Nebula. Nat Commun 2023; 14:4940. [PMID: 37643999 PMCID: PMC10465487 DOI: 10.1038/s41467-023-40026-1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/26/2022] [Accepted: 07/04/2023] [Indexed: 08/31/2023] Open
Abstract
The short-lived radionuclide aluminium-26 (26Al) isotope is a major heat source for early planetary melting. The aluminium-26 - magnesium-26 (26Al-26Mg) decay system also serves as a high-resolution relative chronometer. In both cases, however, it is critical to establish whether 26Al was homogeneously or heterogeneously distributed throughout the solar nebula. Here we report a precise lead-207 - lead-206 (207Pb-206Pb) isotopic age of 4565.56 ± 0.12 million years (Ma) for the andesitic achondrite Erg Chech 002. Our analysis, in conjunction with published 26Al-26Mg data, reveals that the initial 26Al/27Al in the source material of this achondrite was notably higher than in various other well-preserved and precisely dated achondrites. Here we demonstrate that the current data clearly indicate spatial heterogeneity of 26Al by a factor of 3-4 in the precursor molecular cloud or the protoplanetary disk of the Solar System, likely associated with the late infall of stellar materials with freshly synthesized radionuclides.
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Affiliation(s)
- Evgenii Krestianinov
- Research School of Earth Sciences, Australian National University, Canberra, 2601, Australia.
| | - Yuri Amelin
- Research School of Earth Sciences, Australian National University, Canberra, 2601, Australia
- Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, GD, 510640, China
- Korea Basic Science Institute, Ochang, Cheongwon, Cheongju, Chungbuk, 28119, Korea
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California, Davis, Davis, CA, 95616, USA
| | - Paige Cary
- Department of Earth and Planetary Sciences, University of California, Davis, Davis, CA, 95616, USA
| | - Magdalena H Huyskens
- Department of Earth and Planetary Sciences, University of California, Davis, Davis, CA, 95616, USA
| | - Audrey Miller
- Department of Earth and Planetary Sciences, University of California, Davis, Davis, CA, 95616, USA
| | - Supratim Dey
- Department of Earth and Planetary Sciences, University of California, Davis, Davis, CA, 95616, USA
| | - Yuki Hibiya
- Department of General Systems Studies, University of Tokyo, Komaba 3-8-1, Meguro, Tokyo, 153-0041, Japan
- Research Center for Advanced Science and Technology, University of Tokyo, Komaba 4-6-1, Meguro, Tokyo, 153-8904, Japan
| | - Haolan Tang
- Department of Earth, Planetary and Space Sciences, University of California, Los Angeles, Los Angeles, CA, 90095, USA
| | - Edward D Young
- Department of Earth, Planetary and Space Sciences, University of California, Los Angeles, Los Angeles, CA, 90095, USA
| | - Andreas Pack
- Geochemistry and Isotope Geology Department, Georg-August-Universität Göttingen, Goldschmidtstraße 1, 37077, Göttingen, Germany
| | - Tommaso Di Rocco
- Geochemistry and Isotope Geology Department, Georg-August-Universität Göttingen, Goldschmidtstraße 1, 37077, Göttingen, Germany
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4
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Leone G, Tanaka HK. Igneous processes in the small bodies of the Solar System I. Asteroids and comets. iScience 2023; 26:107160. [PMID: 37534155 PMCID: PMC10391981 DOI: 10.1016/j.isci.2023.107160] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 08/04/2023] Open
Abstract
Igneous processes were quite widespread in the small bodies of the Solar System (SBSS) and were initially fueled by short-lived radioisotopes, the proto-Sun, impact heating, and differentiation heating. Once they finished, long-lived radioisotopes continued to warm the active bodies of the Earth, (possibly) Venus, and the cryovolcanism of Enceladus. The widespread presence of olivine and pyroxenes in planets and also in SBSS suggests that they were not necessarily the product of igneous processes and they might have been recycled from previous nebular processes or entrained in comets from interstellar space. The difference in temperature between the inner and the outer Solar System has clearly favored thermal annealing of the olivine close to the proto-Sun. Transport of olivine within the Solar System probably occurred also due to protostellar jets and winds but the entrainment in SBSS from interstellar space would overcome the requirement of initial turbulent regime in the protoplanetary nebula.
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Affiliation(s)
- Giovanni Leone
- Instituto de Investigación en Astronomía y Ciencias Planetarias, Universidad de Atacama, Chile
- Virtual Muography Institute, Global, Tokyo, Japan
| | - Hiroyuki K.M. Tanaka
- Virtual Muography Institute, Global, Tokyo, Japan
- International Muography Research Organization (MUOGRAPHIX), The University of Tokyo, Japan
- Earthquake Research Institute, The University of Tokyo, 1-1-1 Yayoi, Bunkyo, Tokyo 113-0032, Japan
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5
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Onyett IJ, Schiller M, Makhatadze GV, Deng Z, Johansen A, Bizzarro M. Silicon isotope constraints on terrestrial planet accretion. Nature 2023; 619:539-544. [PMID: 37316662 PMCID: PMC10356600 DOI: 10.1038/s41586-023-06135-z] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/05/2022] [Accepted: 04/26/2023] [Indexed: 06/16/2023]
Abstract
Understanding the nature and origin of the precursor material to terrestrial planets is key to deciphering the mechanisms and timescales of planet formation1. Nucleosynthetic variability among rocky Solar System bodies can trace the composition of planetary building blocks2-5. Here we report the nucleosynthetic composition of silicon (μ30Si), the most abundant refractory planet-building element, in primitive and differentiated meteorites to identify terrestrial planet precursors. Inner Solar System differentiated bodies, including Mars, record μ30Si deficits of -11.0 ± 3.2 parts per million to -5.8 ± 3.0 parts per million whereas non-carbonaceous and carbonaceous chondrites show μ30Si excesses from 7.4 ± 4.3 parts per million to 32.8 ± 2.0 parts per million relative to Earth. This establishes that chondritic bodies are not planetary building blocks. Rather, material akin to early-formed differentiated asteroids must represent a major planetary constituent. The μ30Si values of asteroidal bodies correlate with their accretion ages, reflecting progressive admixing of a μ30Si-rich outer Solar System material to an initially μ30Si-poor inner disk. Mars' formation before chondrite parent bodies is necessary to avoid incorporation of μ30Si-rich material. In contrast, Earth's μ30Si composition necessitates admixing of 26 ± 9 per cent of μ30Si-rich outer Solar System material to its precursors. The μ30Si compositions of Mars and proto-Earth are consistent with their rapid formation by collisional growth and pebble accretion less than three million years after Solar System formation. Finally, Earth's nucleosynthetic composition for s-process sensitive (molybdenum and zirconium) and siderophile (nickel) tracers are consistent with pebble accretion when volatility-driven processes during accretion and the Moon-forming impact are carefully evaluated.
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Affiliation(s)
- Isaac J Onyett
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark.
| | - Martin Schiller
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Georgy V Makhatadze
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Zhengbin Deng
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - Anders Johansen
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Lund, Sweden
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
- Institut de Physique du Globe de Paris, Université de Paris Cité, Paris, France
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6
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Potiszil C, Ota T, Yamanaka M, Sakaguchi C, Kobayashi K, Tanaka R, Kunihiro T, Kitagawa H, Abe M, Miyazaki A, Nakato A, Nakazawa S, Nishimura M, Okada T, Saiki T, Tanaka S, Terui F, Tsuda Y, Usui T, Watanabe SI, Yada T, Yogata K, Yoshikawa M, Nakamura E. Insights into the formation and evolution of extraterrestrial amino acids from the asteroid Ryugu. Nat Commun 2023; 14:1482. [PMID: 36932072 PMCID: PMC10023693 DOI: 10.1038/s41467-023-37107-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/24/2022] [Accepted: 02/28/2023] [Indexed: 03/19/2023] Open
Abstract
All life on Earth contains amino acids and carbonaceous chondrite meteorites have been suggested as their source at the origin of life on Earth. While many meteoritic amino acids are considered indigenous, deciphering the extent of terrestrial contamination remains an issue. The Ryugu asteroid fragments (JAXA Hayabusa2 mission), represent the most uncontaminated primitive extraterrestrial material available. Here, the concentrations of amino acids from two particles from different touchdown sites (TD1 and TD2) are reported. The concentrations show that N,N-dimethylglycine (DMG) is the most abundant amino acid in the TD1 particle, but below detection limit in the other. The TD1 particle mineral components indicate it experienced more aqueous alteration. Furthermore, the relationships between the amino acids and the geochemistry suggest that DMG formed on the Ryugu progenitor body during aqueous alteration. The findings highlight the importance of aqueous chemistry for defining the ultimate concentrations of amino acids in primitive extraterrestrial samples.
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Affiliation(s)
- Christian Potiszil
- Pheasant Memorial Laboratory, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori, 682-0193, Japan.
| | - Tsutomu Ota
- Pheasant Memorial Laboratory, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori, 682-0193, Japan
| | - Masahiro Yamanaka
- Pheasant Memorial Laboratory, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori, 682-0193, Japan
| | - Chie Sakaguchi
- Pheasant Memorial Laboratory, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori, 682-0193, Japan
| | - Katsura Kobayashi
- Pheasant Memorial Laboratory, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori, 682-0193, Japan
| | - Ryoji Tanaka
- Pheasant Memorial Laboratory, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori, 682-0193, Japan
| | - Tak Kunihiro
- Pheasant Memorial Laboratory, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori, 682-0193, Japan
| | - Hiroshi Kitagawa
- Pheasant Memorial Laboratory, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori, 682-0193, Japan
| | - Masanao Abe
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
- The Graduate University for Advanced Studies (SOKENDAI), Hayama, Japan
| | - Akiko Miyazaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - Aiko Nakato
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - Satoru Nakazawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - Masahiro Nishimura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - Tatsuaki Okada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
- University of Tokyo, Tokyo, Japan
| | - Takanao Saiki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - Satoshi Tanaka
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
- The Graduate University for Advanced Studies (SOKENDAI), Hayama, Japan
- University of Tokyo, Kashiwa, Japan
| | - Fuyuto Terui
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
- Kanagawa Institute of Technology, Atsugi, Japan
| | - Yuichi Tsuda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
- The Graduate University for Advanced Studies (SOKENDAI), Hayama, Japan
| | - Tomohiro Usui
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | | | - Toru Yada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - Kasumi Yogata
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - Makoto Yoshikawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
- The Graduate University for Advanced Studies (SOKENDAI), Hayama, Japan
| | - Eizo Nakamura
- Pheasant Memorial Laboratory, Institute for Planetary Materials, Okayama University, Yamada 827, Misasa, Tottori, 682-0193, Japan
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7
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Yokoyama T, Nagashima K, Nakai I, Young ED, Abe Y, Aléon J, Alexander CMO, Amari S, Amelin Y, Bajo KI, Bizzarro M, Bouvier A, Carlson RW, Chaussidon M, Choi BG, Dauphas N, Davis AM, Di Rocco T, Fujiya W, Fukai R, Gautam I, Haba MK, Hibiya Y, Hidaka H, Homma H, Hoppe P, Huss GR, Ichida K, Iizuka T, Ireland TR, Ishikawa A, Ito M, Itoh S, Kawasaki N, Kita NT, Kitajima K, Kleine T, Komatani S, Krot AN, Liu MC, Masuda Y, McKeegan KD, Morita M, Motomura K, Moynier F, Nguyen A, Nittler L, Onose M, Pack A, Park C, Piani L, Qin L, Russell SS, Sakamoto N, Schönbächler M, Tafla L, Tang H, Terada K, Terada Y, Usui T, Wada S, Wadhwa M, Walker RJ, Yamashita K, Yin QZ, Yoneda S, Yui H, Zhang AC, Connolly HC, Lauretta DS, Nakamura T, Naraoka H, Noguchi T, Okazaki R, Sakamoto K, Yabuta H, Abe M, Arakawa M, Fujii A, Hayakawa M, Hirata N, Hirata N, Honda R, Honda C, Hosoda S, Iijima YI, Ikeda H, Ishiguro M, Ishihara Y, Iwata T, Kawahara K, Kikuchi S, Kitazato K, Matsumoto K, Matsuoka M, Michikami T, Mimasu Y, Miura A, Morota T, Nakazawa S, Namiki N, Noda H, Noguchi R, Ogawa N, Ogawa K, Okada T, Okamoto C, Ono G, Ozaki M, Saiki T, Sakatani N, Sawada H, Senshu H, Shimaki Y, Shirai K, Sugita S, Takei Y, Takeuchi H, Tanaka S, Tatsumi E, Terui F, Tsuda Y, Tsukizaki R, Wada K, Watanabe SI, Yamada M, Yamada T, Yamamoto Y, Yano H, Yokota Y, Yoshihara K, Yoshikawa M, Yoshikawa K, Furuya S, Hatakeda K, Hayashi T, Hitomi Y, Kumagai K, Miyazaki A, Nakato A, Nishimura M, Soejima H, Suzuki A, Yada T, Yamamoto D, Yogata K, Yoshitake M, Tachibana S, Yurimoto H. Samples returned from the asteroid Ryugu are similar to Ivuna-type carbonaceous meteorites. Science 2023; 379:eabn7850. [PMID: 35679354 DOI: 10.1126/science.abn7850] [Citation(s) in RCA: 18] [Impact Index Per Article: 18.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Carbonaceous meteorites are thought to be fragments of C-type (carbonaceous) asteroids. Samples of the C-type asteroid (162173) Ryugu were retrieved by the Hayabusa2 spacecraft. We measured the mineralogy and bulk chemical and isotopic compositions of Ryugu samples. The samples are mainly composed of materials similar to those of carbonaceous chondrite meteorites, particularly the CI (Ivuna-type) group. The samples consist predominantly of minerals formed in aqueous fluid on a parent planetesimal. The primary minerals were altered by fluids at a temperature of 37° ± 10°C, about [Formula: see text] million (statistical) or [Formula: see text] million (systematic) years after the formation of the first solids in the Solar System. After aqueous alteration, the Ryugu samples were likely never heated above ~100°C. The samples have a chemical composition that more closely resembles that of the Sun's photosphere than other natural samples do.
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Affiliation(s)
- Tetsuya Yokoyama
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Kazuhide Nagashima
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - Izumi Nakai
- Department of Applied Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Edward D Young
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Yoshinari Abe
- Graduate School of Engineering Materials Science and Engineering, Tokyo Denki University, Tokyo 120-8551, Japan
| | - Jérôme Aléon
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Sorbonne Université, Museum National d'Histoire Naturelle, Centre National de la Recherche Scientifique Unité Mixte de Recherche 7590, Institut de recherche pour le développement, 75005 Paris, France
| | - Conel M O'D Alexander
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Sachiko Amari
- McDonnell Center for the Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, USA
| | - Yuri Amelin
- Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, GD 510640, China
| | - Ken-Ichi Bajo
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, K 1350 Copenhagen, Denmark
| | - Audrey Bouvier
- Bayerisches Geoinstitut, Universität Bayreuth, 95447 Bayreuth, Germany
| | - Richard W Carlson
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Marc Chaussidon
- Université de Paris, Institut de physique du globe de Paris, Centre National de la Recherche Scientifique, 75005 Paris, France
| | - Byeon-Gak Choi
- Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea
| | - Nicolas Dauphas
- Department of the Geophysical Sciences and Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA
| | - Andrew M Davis
- Department of the Geophysical Sciences and Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA
| | - Tommaso Di Rocco
- Faculty of Geosciences and Geography, University of Göttingen, D-37077 Göttingen, Germany
| | - Wataru Fujiya
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Ryota Fukai
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Ikshu Gautam
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Makiko K Haba
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Yuki Hibiya
- Department of General Systems Studies, University of Tokyo, Tokyo 153-0041, Japan
| | - Hiroshi Hidaka
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Hisashi Homma
- Osaka Application Laboratory, Rigaku Corporation, Osaka 569-1146, Japan
| | - Peter Hoppe
- Max Planck Institute for Chemistry, Mainz 55128, Germany
| | - Gary R Huss
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - Kiyohiro Ichida
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Tsuyoshi Iizuka
- Department of Earth and Planetary Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Trevor R Ireland
- School of Earth and Environmental Sciences, University of Queensland, St Lucia, QLD 4072, Australia
| | - Akira Ishikawa
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Motoo Ito
- Kochi Institute for Core Sample Research, Japan Agency for Marine-Earth Science and Technology, Kochi 783-8502, Japan
| | - Shoichi Itoh
- Department of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Noriyuki Kawasaki
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Noriko T Kita
- Department of Geoscience, University of Wisconsin, Madison, WI 53706, USA
| | - Kouki Kitajima
- Department of Geoscience, University of Wisconsin, Madison, WI 53706, USA
| | - Thorsten Kleine
- Max Planck Institute for Solar System Research, 37077 Göttingen, Germany
| | - Shintaro Komatani
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Alexander N Krot
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - Ming-Chang Liu
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Yuki Masuda
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Kevin D McKeegan
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Mayu Morita
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Kazuko Motomura
- Thermal Analysis Division, Rigaku Corporation, Tokyo 196-8666, Japan
| | - Frédéric Moynier
- Université de Paris, Institut de physique du globe de Paris, Centre National de la Recherche Scientifique, 75005 Paris, France
| | - Ann Nguyen
- Astromaterials Research and Exploration Science Division, National Aeronautics and Space Administration Johnson Space Center, Houston, TX 77058, USA
| | - Larry Nittler
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Morihiko Onose
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Andreas Pack
- Faculty of Geosciences and Geography, University of Göttingen, D-37077 Göttingen, Germany
| | - Changkun Park
- Division of Earth-System Sciences, Korea Polar Research Institute, Incheon 21990, Korea
| | - Laurette Piani
- Centre de Recherches Pétrographiques et Géochimiques, Centre National de la Recherche Scientifique-Université de Lorraine, 54500 Nancy, France
| | - Liping Qin
- School of Earth and Space Sciences, University of Science and Technology of China, Anhui 230026, China
| | - Sara S Russell
- Department of Earth Sciences, Natural History Museum, London SW7 5BD, UK
| | - Naoya Sakamoto
- Isotope Imaging Laboratory, Hokkaido University, Sapporo 001-0021, Japan
| | - Maria Schönbächler
- Institute for Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | - Lauren Tafla
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Haolan Tang
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Kentaro Terada
- Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan
| | - Yasuko Terada
- Spectroscopy and Imaging Division, Japan Synchrotron Radiation Research Institute, Hyogo 679-5198, Japan
| | - Tomohiro Usui
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Sohei Wada
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Richard J Walker
- Department of Geology, University of Maryland, College Park, MD 20742, USA
| | - Katsuyuki Yamashita
- Graduate School of Natural Science and Technology, Okayama University, Okayama 700-8530, Japan
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California, Davis, CA 95616, USA
| | - Shigekazu Yoneda
- Department of Science and Engineering, National Museum of Nature and Science, Tsukuba 305-0005, Japan
| | - Hiroharu Yui
- Department of Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Ai-Cheng Zhang
- School of Earth Sciences and Engineering, Nanjing University, Nanjing 210023, China
| | - Harold C Connolly
- Department of Geology, School of Earth and Environment, Rowan University, Glassboro, NJ 08028, USA
| | - Dante S Lauretta
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85705, USA
| | - Tomoki Nakamura
- Department of Earth Science, Tohoku University, Sendai 980-8578, Japan
| | - Hiroshi Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Takaaki Noguchi
- Department of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Ryuji Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Kanako Sakamoto
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hikaru Yabuta
- Earth and Planetary Systems Science Program, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - Masanao Abe
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masahiko Arakawa
- Graduate School of Science, Kobe University, Kobe 657-8501, Japan
| | - Atsushi Fujii
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masahiko Hayakawa
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Naoyuki Hirata
- Graduate School of Science, Kobe University, Kobe 657-8501, Japan
| | - Naru Hirata
- Department of Computer Science and Engineering, University of Aizu, Aizu-Wakamatsu 965-8580, Japan
| | - Rie Honda
- Faculty of Science and Technology, Kochi University, Kochi 780-8520, Japan
| | - Chikatoshi Honda
- Department of Computer Science and Engineering, University of Aizu, Aizu-Wakamatsu 965-8580, Japan
| | - Satoshi Hosoda
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Yu-Ichi Iijima
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hitoshi Ikeda
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masateru Ishiguro
- Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea
| | - Yoshiaki Ishihara
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Takahiro Iwata
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan.,Graduate University for Advanced Studies, Sokendai, Kanagawa 240-0193, Japan
| | - Kosuke Kawahara
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Shota Kikuchi
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - Kohei Kitazato
- Department of Computer Science and Engineering, University of Aizu, Aizu-Wakamatsu 965-8580, Japan
| | - Koji Matsumoto
- National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - Moe Matsuoka
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | | | - Yuya Mimasu
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Akira Miura
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Tomokatsu Morota
- Department of Earth and Planetary Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Satoru Nakazawa
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Noriyuki Namiki
- National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - Hirotomo Noda
- National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - Rina Noguchi
- Academic Assembly Institute of Science and Technology, Niigata University, Niigata 950-2181, Japan
| | - Naoko Ogawa
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kazunori Ogawa
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Tatsuaki Okada
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan.,Department of Chemistry, University of Tokyo, Tokyo 113-0033, Japan
| | - Chisato Okamoto
- Graduate School of Science, Kobe University, Kobe 657-8501, Japan
| | - Go Ono
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masanobu Ozaki
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan.,Graduate University for Advanced Studies, Sokendai, Kanagawa 240-0193, Japan
| | - Takanao Saiki
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Naoya Sakatani
- College of Science Department of Physics, Rikkyo University, Tokyo 171-8501, Japan
| | - Hirotaka Sawada
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hiroki Senshu
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - Yuri Shimaki
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kei Shirai
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Seiji Sugita
- Department of Earth and Planetary Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Yuto Takei
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hiroshi Takeuchi
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoshi Tanaka
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Eri Tatsumi
- Instituto de Astrofísica de Canarias, University of La Laguna, Tenerife, Spain
| | - Fuyuto Terui
- Graduate School of Engineering, Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | - Yuichi Tsuda
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Ryudo Tsukizaki
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Koji Wada
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - Sei-Ichiro Watanabe
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Manabu Yamada
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - Tetsuya Yamada
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Yukio Yamamoto
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hajime Yano
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Yasuhiro Yokota
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Keisuke Yoshihara
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Makoto Yoshikawa
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kent Yoshikawa
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Shizuho Furuya
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | | | - Tasuku Hayashi
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Yuya Hitomi
- Marine Works Japan Ltd., Yokosuka 237-0063, Japan
| | | | - Akiko Miyazaki
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Aiko Nakato
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masahiro Nishimura
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | | | - Ayako Suzuki
- Marine Works Japan Ltd., Yokosuka 237-0063, Japan
| | - Toru Yada
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Daiki Yamamoto
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kasumi Yogata
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Miwa Yoshitake
- Institute of Space and Astronautical Science/Jaxa Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Shogo Tachibana
- UTokyo Organization for Planetary and Space Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Hisayoshi Yurimoto
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan.,Isotope Imaging Laboratory, Hokkaido University, Sapporo 001-0021, Japan
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8
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Nie NX, Wang D, Torrano ZA, Carlson RW, O'D Alexander CM, Shahar A. Meteorites have inherited nucleosynthetic anomalies of potassium-40 produced in supernovae. Science 2023; 379:372-376. [PMID: 36701465 DOI: 10.1126/science.abn1783] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/27/2023]
Abstract
Meteorites record processes that occurred before and during the formation of the Solar System in the form of nucleosynthetic anomalies: isotopic compositions that differ from the Solar System patterns. Nucleosynthetic anomalies are rarely seen in volatile elements such as potassium at bulk meteorite scale. We measured potassium isotope ratios in 32 meteorites and identified nucleosynthetic anomalies in the isotope potassium-40. The anomalies are larger and more variable in carbonaceous chondrite (CC) meteorites than in noncarbonaceous (NC) meteorites, indicating that CCs inherited more material produced in supernova nucleosynthesis. The potassium-40 anomaly of Earth is close to that of the NCs, implying that Earth's potassium was mostly delivered by NCs.
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Affiliation(s)
- Nicole X Nie
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Da Wang
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA.,International Center for Planetary Science, College of Earth Sciences, Chengdu University of Technology, 610059 Chengdu, China
| | - Zachary A Torrano
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Richard W Carlson
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Conel M O'D Alexander
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Anat Shahar
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
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9
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Martins R, Kuthning S, Coles BJ, Kreissig K, Rehkämper M. Nucleosynthetic isotope anomalies of zinc in meteorites constrain the origin of Earth's volatiles. Science 2023; 379:369-372. [PMID: 36701454 DOI: 10.1126/science.abn1021] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/27/2023]
Abstract
Material inherited from different nucleosynthesis sources imparts distinct isotopic signatures to meteorites and terrestrial planets. These nucleosynthetic isotope anomalies have been used to constrain the origins of material that formed Earth. However, anomalies have only been identified for elements with high condensation temperatures, leaving the origin of Earth's volatile elements unconstrained. We determined the isotope composition of the moderately volatile element zinc in 18 bulk meteorites and identified nucleosynthetic zinc isotope anomalies. Using a mass-balance model, we find that carbonaceous bodies, which likely formed beyond the orbit of Jupiter, delivered about half of Earth's zinc inventory. Combined with previous constraints obtained from studies of other elements, these results indicate that ~10% of Earth's mass was provided by carbonaceous material.
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Affiliation(s)
- Rayssa Martins
- Department of Earth Science and Engineering, Imperial College London, London SW7 2AZ, UK
| | - Sven Kuthning
- Department of Earth Science and Engineering, Imperial College London, London SW7 2AZ, UK
| | - Barry J Coles
- Department of Earth Science and Engineering, Imperial College London, London SW7 2AZ, UK
| | - Katharina Kreissig
- Department of Earth Science and Engineering, Imperial College London, London SW7 2AZ, UK
| | - Mark Rehkämper
- Department of Earth Science and Engineering, Imperial College London, London SW7 2AZ, UK
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10
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Hopp T, Dauphas N, Abe Y, Aléon J, O'D Alexander CM, Amari S, Amelin Y, Bajo KI, Bizzarro M, Bouvier A, Carlson RW, Chaussidon M, Choi BG, Davis AM, Di Rocco T, Fujiya W, Fukai R, Gautam I, Haba MK, Hibiya Y, Hidaka H, Homma H, Hoppe P, Huss GR, Ichida K, Iizuka T, Ireland TR, Ishikawa A, Ito M, Itoh S, Kawasaki N, Kita NT, Kitajima K, Kleine T, Komatani S, Krot AN, Liu MC, Masuda Y, McKeegan KD, Morita M, Motomura K, Moynier F, Nakai I, Nagashima K, Nesvorný D, Nguyen A, Nittler L, Onose M, Pack A, Park C, Piani L, Qin L, Russell SS, Sakamoto N, Schönbächler M, Tafla L, Tang H, Terada K, Terada Y, Usui T, Wada S, Wadhwa M, Walker RJ, Yamashita K, Yin QZ, Yokoyama T, Yoneda S, Young ED, Yui H, Zhang AC, Nakamura T, Naraoka H, Noguchi T, Okazaki R, Sakamoto K, Yabuta H, Abe M, Miyazaki A, Nakato A, Nishimura M, Okada T, Yada T, Yogata K, Nakazawa S, Saiki T, Tanaka S, Terui F, Tsuda Y, Watanabe SI, Yoshikawa M, Tachibana S, Yurimoto H. Ryugu's nucleosynthetic heritage from the outskirts of the Solar System. SCIENCE ADVANCES 2022; 8:eadd8141. [PMID: 36264823 DOI: 10.1126/sciadv.add8141] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/16/2023]
Abstract
Little is known about the origin of the spectral diversity of asteroids and what it says about conditions in the protoplanetary disk. Here, we show that samples returned from Cb-type asteroid Ryugu have Fe isotopic anomalies indistinguishable from Ivuna-type (CI) chondrites, which are distinct from all other carbonaceous chondrites. Iron isotopes, therefore, demonstrate that Ryugu and CI chondrites formed in a reservoir that was different from the source regions of other carbonaceous asteroids. Growth and migration of the giant planets destabilized nearby planetesimals and ejected some inward to be implanted into the Main Belt. In this framework, most carbonaceous chondrites may have originated from regions around the birthplaces of Jupiter and Saturn, while the distinct isotopic composition of CI chondrites and Ryugu may reflect their formation further away in the disk, owing their presence in the inner Solar System to excitation by Uranus and Neptune.
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Affiliation(s)
- Timo Hopp
- Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Nicolas Dauphas
- Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Yoshinari Abe
- Graduate School of Engineering Materials Science and Engineering, Tokyo Denki University, Tokyo 120-8551, Japan
| | - Jérôme Aléon
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Sorbonne Université, Museum National d'Histoire Naturelle, CNRS UMR 7590, IRD, 75005 Paris, France
| | - Conel M O'D Alexander
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Sachiko Amari
- McDonnell Center for the Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, USA
- Geochemical Research Center, The University of Tokyo, Tokyo 113-0033, Japan
| | - Yuri Amelin
- Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, GD 510640, China
| | - Ken-Ichi Bajo
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Martin Bizzarro
- Centre for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Copenhagen K 1350, Denmark
| | - Audrey Bouvier
- Bayerisches Geoinstitut, Universität Bayreuth, Bayreuth 95447, Germany
| | - Richard W Carlson
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Marc Chaussidon
- Université Paris Cité, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Byeon-Gak Choi
- Department of Earth Science Education, Seoul National University, Seoul 08826, Republic of Korea
| | - Andrew M Davis
- Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Tommaso Di Rocco
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Wataru Fujiya
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Ryota Fukai
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Ikshu Gautam
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Makiko K Haba
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Yuki Hibiya
- Department of General Systems Studies, The University of Tokyo, Tokyo 153-0041, Japan
- Research Center for Advanced Science and Technology, The University of Tokyo, Tokyo 153-8904, Japan
| | - Hiroshi Hidaka
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Hisashi Homma
- Osaka Application Laboratory, SBUWDX, Rigaku Corporation, Osaka 569-1146, Japan
| | - Peter Hoppe
- Max Planck Institute for Chemistry, Mainz 55128, Germany
| | - Gary R Huss
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - Kiyohiro Ichida
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Tsuyoshi Iizuka
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Trevor R Ireland
- School of Earth and Environmental Sciences, The University of Queensland, St. Lucia, QLD 4072, Australia
| | - Akira Ishikawa
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Motoo Ito
- Kochi Institute for Core Sample Research, JAMSTEC, Kochi 783-8502, Japan
| | - Shoichi Itoh
- Department of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Noriyuki Kawasaki
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Noriko T Kita
- Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Kouki Kitajima
- Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Thorsten Kleine
- Max Planck Institute for Solar System Research, 37077 Göttingen, Germany
| | - Shintaro Komatani
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Alexander N Krot
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - Ming-Chang Liu
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
- Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
| | - Yuki Masuda
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Kevin D McKeegan
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Mayu Morita
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | | | - Frédéric Moynier
- Université Paris Cité, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Izumi Nakai
- Thermal Analysis, Rigaku Corporation, Tokyo 196-8666, Japan
| | - Kazuhide Nagashima
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - David Nesvorný
- Department of Space Studies, Southwest Research Institute, Boulder, CO 80302, USA
| | - Ann Nguyen
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
| | - Larry Nittler
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Morihiko Onose
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Andreas Pack
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Changkun Park
- Division of Earth-System Sciences, Korea Polar Research Institute, Incheon 21990, Korea
| | - Laurette Piani
- Centre de Recherches Pétrographiques et Géochimiques, CNRS-Université de Lorraine, 54500 Nancy, France
| | - Liping Qin
- Deep Space Exploration Laboratory/CAS Key Laboratory of Crust-Mantle Materials and Environments, University of Science and Technology of China, Hefei 230026, China
| | - Sara S Russell
- Department of Earth Sciences, Natural History Museum, London SW7 5BD, UK
| | - Naoya Sakamoto
- Isotope Imaging Laboratory, Hokkaido University, Sapporo 001-0021, Japan
| | - Maria Schönbächler
- Institute for Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | - Lauren Tafla
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Haolan Tang
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
- University of Science and Technology of China, Hefei, China
| | - Kentaro Terada
- Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan
| | - Yasuko Terada
- Spectroscopy and Imaging Division, Japan Synchrotron Radiation Research Institute, Hyogo 679-5198, Japan
| | - Tomohiro Usui
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Sohei Wada
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Richard J Walker
- Department of Geology, University of Maryland, College Park, MD 20742, USA
| | - Katsuyuki Yamashita
- Graduate School of Natural Science and Technology, Okayama University, Okayama 700-8530, Japan
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California Davis, Davis, CA 95616, USA
| | - Tetsuya Yokoyama
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Shigekazu Yoneda
- Department Science and Engineering, National Museum of Nature and Science, Tsukuba 305-0005, Japan
| | - Edward D Young
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Hiroharu Yui
- Department of Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Ai-Cheng Zhang
- School of Earth Sciences and Engineering, Nanjing University, Nanjing 210023, China
| | - Tomoki Nakamura
- Department of Earth Science, Tohoku University, Sendai 980-8578, Japan
| | - Hiroshi Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Takaaki Noguchi
- Kochi Institute for Core Sample Research, JAMSTEC, Kochi 783-8502, Japan
| | - Ryuji Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Kanako Sakamoto
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hikaru Yabuta
- Earth and Planetary Systems Science Program, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - Masanao Abe
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Akiko Miyazaki
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Aiko Nakato
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masahiro Nishimura
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Tatsuaki Okada
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Toru Yada
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kasumi Yogata
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoru Nakazawa
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Takanao Saiki
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoshi Tanaka
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Fuyuto Terui
- Graduate School of Engineering, Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | - Yuichi Tsuda
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Sei-Ichiro Watanabe
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Makoto Yoshikawa
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Shogo Tachibana
- UTokyo Organization for Planetary and Space Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Hisayoshi Yurimoto
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
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11
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Broadley MW, Bekaert DV, Piani L, Füri E, Marty B. Origin of life-forming volatile elements in the inner Solar System. Nature 2022; 611:245-255. [DOI: 10.1038/s41586-022-05276-x] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/12/2021] [Accepted: 08/25/2022] [Indexed: 11/11/2022]
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12
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Johnston S, Brandon A, McLeod C, Rankenburg K, Becker H, Copeland P. Nd isotope variation between the Earth-Moon system and enstatite chondrites. Nature 2022; 611:501-506. [PMID: 36203033 DOI: 10.1038/s41586-022-05265-0] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/04/2022] [Accepted: 08/23/2022] [Indexed: 11/09/2022]
Abstract
Reconstructing the building blocks that made Earth and the Moon is critical to constrain their formation and compositional evolution to the present. Neodymium (Nd) isotopes identify these building blocks by fingerprinting nucleosynthetic components. In addition, the 146Sm-142Nd and 147Sm-143Nd decay systems, with half-lives of 103 million years and 108 billion years, respectively, track potential differences in their samarium (Sm)/Nd ratios. The difference in Earth's present-day 142Nd/144Nd ratio compared with chondrites1,2, and in particular enstatite chondrites, is interpreted as nucleosynthetic isotope variation in the protoplanetary disk. This necessitates that chondrite parent bodies have the same Sm/Nd ratio as Earth's precursor materials2. Here we show that Earth and the Moon instead had a Sm/Nd ratio approximately 2.4 ± 0.5 per cent higher than the average for chondrites and that the initial 142Nd/144Nd ratio of Earth's precursor materials is more similar to that of enstatite chondrites than previously proposed1,2. The difference in the Sm/Nd ratio between Earth and chondrites probably reflects the mineralogical distribution owing to mixing processes within the inner protoplanetary disk. This observation simplifies lunar differentiation to a single stage from formation to solidification of a lunar magma ocean3. This also indicates that no Sm/Nd fractionation occurred between the materials that made Earth and the Moon in the Moon-forming giant impact.
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Affiliation(s)
- Shelby Johnston
- Department of Earth and Atmospheric Sciences, University of Houston, Houston, TX, USA
| | - Alan Brandon
- Department of Earth and Atmospheric Sciences, University of Houston, Houston, TX, USA.
| | - Claire McLeod
- Department of Geology and Environmental Earth Science, Miami University, Oxford, OH, USA
| | - Kai Rankenburg
- John De Laeter Centre, Curtin University, Bentley, Western Australia, Australia
| | | | - Peter Copeland
- Department of Earth and Atmospheric Sciences, University of Houston, Houston, TX, USA
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13
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Zhang B, Chabot NL, Rubin AE. Compositions of carbonaceous-type asteroidal cores in the early solar system. SCIENCE ADVANCES 2022; 8:eabo5781. [PMID: 36112692 PMCID: PMC9481128 DOI: 10.1126/sciadv.abo5781] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 02/12/2022] [Accepted: 08/01/2022] [Indexed: 06/15/2023]
Abstract
The parent cores of iron meteorites belong to the earliest accreted bodies in the solar system. These cores formed in two isotopically distinct reservoirs: noncarbonaceous (NC) type and carbonaceous (CC) type in the inner and outer solar system, respectively. We measured elemental compositions of CC-iron groups and used fractional crystallization modeling to reconstruct the bulk compositions and crystallization processes of their parent asteroidal cores. We found generally lower S and higher P in CC-iron cores than in NC-iron cores and higher HSE (highly siderophile element) abundances in some CC-iron cores than in NC-iron cores. We suggest that the different HSE abundances among the CC-iron cores are related to the spatial distribution of refractory metal nugget-bearing calcium aluminum-rich inclusions (CAIs) in the protoplanetary disk. CAIs may have been transported to the outer solar system and distributed heterogeneously within the first million years of solar system history.
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Affiliation(s)
- Bidong Zhang
- Department of Earth, Planetary and Space Sciences, University California, Los Angeles, CA 90095-1567, USA
| | - Nancy L. Chabot
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - Alan E. Rubin
- Department of Earth, Planetary and Space Sciences, University California, Los Angeles, CA 90095-1567, USA
- Maine Mineral and Gem Museum, 99 Main Street, P.O. Box 500, Bethel, ME 04217, USA
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14
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Liu B, Johansen A, Lambrechts M, Bizzarro M, Haugbølle T. Natural separation of two primordial planetary reservoirs in an expanding solar protoplanetary disk. SCIENCE ADVANCES 2022; 8:eabm3045. [PMID: 35452282 PMCID: PMC9032962 DOI: 10.1126/sciadv.abm3045] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 09/08/2021] [Accepted: 03/08/2022] [Indexed: 06/14/2023]
Abstract
Meteorites display an isotopic composition dichotomy between noncarbonaceous (NC) and carbonaceous (CC) groups, indicating that planetesimal formation in the solar protoplanetary disk occurred in two distinct reservoirs. The prevailing view is that a rapidly formed Jupiter acted as a barrier between these reservoirs. We show a fundamental inconsistency in this model: If Jupiter is an efficient blocker of drifting pebbles, then the interior NC reservoir is depleted by radial drift within a few hundred thousand years. If Jupiter lets material pass it, then the two reservoirs will be mixed. Instead, we demonstrate that the arrival of the CC pebbles in the inner disk is delayed for several million years by the viscous expansion of the protoplanetary disk. Our results support the hypothesis that Jupiter formed in the outer disk (>10 astronomical units) and allowed a considerable amount of CC material to pass it and become accreted by the terrestrial planets.
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Affiliation(s)
- Beibei Liu
- Zhejiang Institute of Modern Physics, Department of Physics and Zhejiang University–Purple Mountain Observatory Joint Research Center for Astronomy, Zhejiang University, 38 Zheda Road, Hangzhou 310027, China
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 22100 Lund, Sweden
| | - Anders Johansen
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 22100 Lund, Sweden
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
| | - Michiel Lambrechts
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 22100 Lund, Sweden
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
| | - Martin Bizzarro
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
| | - Troels Haugbølle
- Niels Bohr Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
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15
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The origin of volatile elements in the Earth-Moon system. Proc Natl Acad Sci U S A 2022; 119:2115726119. [PMID: 35165180 PMCID: PMC8872726 DOI: 10.1073/pnas.2115726119] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Accepted: 12/23/2021] [Indexed: 11/18/2022] Open
Abstract
The origin of volatile species such as water in the Earth-Moon system is a subject of intense debate but is obfuscated by the potential for volatile loss during the Giant Impact that resulted in the formation of these bodies. One way to address these topics and place constraints on the temporal evolution of volatile components in planetary bodies is by using the observed decay of 87Rb to 87Sr because Rb is a moderately volatile element, whereas Sr is much more refractory. Here, we show that lunar highland rocks that crystallized ∼4.35 billion years ago exhibit very limited ingrowth of 87Sr, indicating that prior to the Moon-forming impact, the impactor commonly referred to as "Theia" and the proto-Earth both must have already been strongly depleted in volatile elements relative to primitive meteorites. These results imply that 1) the volatile element depletion of the Moon did not arise from the Giant Impact, 2) volatile element distributions on the Moon and Earth were principally inherited from their precursors, 3) both Theia and the proto-Earth probably formed in the inner solar system, and 4) the Giant Impact occurred relatively late in solar system history.
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16
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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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17
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Burkhardt C, Spitzer F, Morbidelli A, Budde G, Render JH, Kruijer TS, Kleine T. Terrestrial planet formation from lost inner solar system material. SCIENCE ADVANCES 2021; 7:eabj7601. [PMID: 34936445 PMCID: PMC8694615 DOI: 10.1126/sciadv.abj7601] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 05/31/2021] [Accepted: 11/03/2021] [Indexed: 06/14/2023]
Abstract
Two fundamentally different processes of rocky planet formation exist, but it is unclear which one built the terrestrial planets of the solar system. They formed either by collisions among planetary embryos from the inner solar system or by accreting sunward-drifting millimeter-sized “pebbles” from the outer solar system. We show that the isotopic compositions of Earth and Mars are governed by two-component mixing among inner solar system materials, including material from the innermost disk unsampled by meteorites, whereas the contribution of outer solar system material is limited to a few percent by mass. This refutes a pebble accretion origin of the terrestrial planets but is consistent with collisional growth from inner solar system embryos. The low fraction of outer solar system material in Earth and Mars indicates the presence of a persistent dust-drift barrier in the disk, highlighting the specific pathway of rocky planet formation in the solar system.
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Affiliation(s)
- Christoph Burkhardt
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany
| | - Fridolin Spitzer
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany
| | - Alessandro Morbidelli
- Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Boulevard de l’Observatoire, 06304 Nice, Cedex 4, France
| | - Gerrit Budde
- Division of Geological and Planetary Sciences, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125, USA
| | - Jan H. Render
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany
| | - Thomas S. Kruijer
- Museum für Naturkunde, Leibniz Institute for Evolution and Biodiversity Science, Invalidenstraße 43, 10115 Berlin, Germany
- Institut für Geologische Wissenschaften, Freie Universität Berlin, Malteserstraße 74-100, 12249 Berlin, Germany
| | - Thorsten Kleine
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany
- Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
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18
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Torrano ZA, Schrader DL, Davidson J, Greenwood RC, Dunlap DR, Wadhwa M. The relationship between CM and CO chondrites: Insights from combined analyses of titanium, chromium, and oxygen isotopes in CM, CO, and ungrouped chondrites. GEOCHIMICA ET COSMOCHIMICA ACTA 2021; 301:70-90. [PMID: 34316079 PMCID: PMC8312627 DOI: 10.1016/j.gca.2021.03.004] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
A close relationship between CM and CO chondrites has been suggested by previous petrologic and isotopic studies, leading to the suggestion that they may originate from similar precursor materials or even a common parent body. In this study, we evaluate the genetic relationship between CM and CO chondrites using Ti, Cr, and O isotopes. We first provide additional constraints on the ranges of ε50Ti and ε54Cr values of bulk CM and CO chondrites by reporting the isotopic compositions of CM2 chondrites Murchison, Murray, and Aguas Zarcas and the CO3.8 chondrite Isna. We then report the ε50Ti and ε54Cr values for several ungrouped and anomalous carbonaceous chondrites that have been previously reported to exhibit similarities to the CM and/or CO chondrite groups, including Elephant Moraine (EET) 83226, EET 83355, Grosvenor Mountains (GRO) 95566, MacAlpine Hills (MAC) 87300, MAC 87301, MAC 88107, and Northwest Africa (NWA) 5958, and the O-isotope compositions of a subset of these samples. We additionally report the Ti, Cr, and O isotopic compositions of additional ungrouped chondrites LaPaz Ice Field (LAP) 04757, LAP 04773, Lewis Cliff (LEW) 85332, and Coolidge to assess their potential relationships with known carbonaceous and ordinary chondrite groups. LAP 04757 and LAP 04773 exhibit isotopic compositions indicating they are low-FeO ordinary chondrites. The isotopic compositions of Murchison, Murray, Aguas Zarcas, and Isna extend the compositional ranges defined by the CM and CO chondrites in ε50Ti versus ε54Cr space. The majority of the ungrouped carbonaceous chondrites with documented similarities to the CM and/or CO chondrites plot outside the CM and CO group fields in plots of ε50Ti versus ε54Cr, Δ17O versus ε50Ti, and Δ17O versus ε54Cr. Therefore, based on differences in their Ti, Cr, and O isotopic compositions, we conclude that the CM, CO, and ungrouped carbonaceous chondrites likely represent samples of multiple distinct parent bodies. We also infer that these parent bodies formed from precursor materials that shared similar isotopic compositions, which may indicate formation in regions of the protoplanetary disk that were in close proximity to each other.
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Affiliation(s)
- Zachary A. Torrano
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
| | - Devin L. Schrader
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
- Center for Meteorite Studies, Arizona State University, Tempe, AZ 85287, USA
| | - Jemma Davidson
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
- Center for Meteorite Studies, Arizona State University, Tempe, AZ 85287, USA
| | - Richard C. Greenwood
- Planetary and Space Sciences, School of Physical Sciences, The Open University, Milton Keynes MK7 6AA, United Kingdom
| | - Daniel R. Dunlap
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
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19
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Zhu K, Moynier F, Schiller M, Alexander CMO, Davidson J, Schrader DL, van Kooten E, Bizzarro M. Chromium isotopic insights into the origin of chondrite parent bodies and the early terrestrial volatile depletion. GEOCHIMICA ET COSMOCHIMICA ACTA 2021; 301:158-186. [PMID: 34393262 PMCID: PMC7611480 DOI: 10.1016/j.gca.2021.02.031] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
Chondrites are meteorites from undifferentiated parent bodies that provide fundamental information about early Solar System evolution and planet formation. The element Cr is highly suitable for deciphering both the timing of formation and the origin of planetary building blocks because it records both radiogenic contributions from 53Mn-53Cr decay and variable nucleosynthetic contributions from the stable 54Cr nuclide. Here, we report high-precision measurements of the massindependent Cr isotope compositions (ε53Cr and ε54Cr) of chondrites (including all carbonaceous chondrites groups) and terrestrial samples using for the first time a multi-collection inductively-coupled-plasma mass-spectrometer to better understand the formation histories and genetic relationships between chondrite parent bodies. With our comprehensive dataset, the order of decreasing ε54Cr (per ten thousand deviation of the 54Cr/52Cr ratio relative to a terrestrial standard) values amongst the carbonaceous chondrites is updated to CI = CH ≥ CB ≥ CR ≥ CM ≈ CV ≈ CO ≥ CK > EC > OC. Chondrites from CO, CV, CR, CM and CB groups show intra-group ε54Cr heterogeneities that may result from sample heterogeneity and/or heterogeneous accretion of their parent bodies. Resolvable ε54Cr (with 2SE uncertainty) differences between CV and CK chondrites rule out an origin from a common parent body or reservoir as has previously been suggested. The CM and CO chondrites share common ε54Cr characteristics, which suggests their parent bodies may have accreted their components in similar proportions. The CB and CH chondrites have low-Mn/Cr ratios and similar ε53Cr values to the CI chondrites, invalidating them as anchors for a bulk 53Mn-53Cr isochron for carbonaceous chondrites. Bulk Earth has a ε53Cr value that is lower than the average of chondrites, including enstatite chondrites. This depletion may constrain the timing of volatile loss from the Earth or its precursors to be within the first million years of Solar System formation and is incompatible with Earth's accretion via any of the known chondrite groups as main contributors, including enstatite chondrites.
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Affiliation(s)
- Ke Zhu
- Universite' de Paris, Institut de Physique du Globe de Paris, CNRS UMR 7154, 1 rue Jussieu, Paris 75005, France
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5-7, Copenhagen DK-1350, Denmark
- Earth and Planetary Laboratory, Carnegie Institution for Science, 5241 Broad Branch Road, Washington, DC 20015, USA
- Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, 781 East Terrace Road, Tempe, AZ 85287-6004, USA
| | - Frédéric Moynier
- Universite' de Paris, Institut de Physique du Globe de Paris, CNRS UMR 7154, 1 rue Jussieu, Paris 75005, France
| | - Martin Schiller
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5-7, Copenhagen DK-1350, Denmark
| | - Conel M O'D Alexander
- Earth and Planetary Laboratory, Carnegie Institution for Science, 5241 Broad Branch Road, Washington, DC 20015, USA
| | - Jemma Davidson
- Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, 781 East Terrace Road, Tempe, AZ 85287-6004, USA
| | - Devin L Schrader
- Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, 781 East Terrace Road, Tempe, AZ 85287-6004, USA
| | - Elishevah van Kooten
- Universite' de Paris, Institut de Physique du Globe de Paris, CNRS UMR 7154, 1 rue Jussieu, Paris 75005, France
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5-7, Copenhagen DK-1350, Denmark
| | - Martin Bizzarro
- Universite' de Paris, Institut de Physique du Globe de Paris, CNRS UMR 7154, 1 rue Jussieu, Paris 75005, France
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5-7, Copenhagen DK-1350, Denmark
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20
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Hazen RM, Morrison SM, Prabhu A. An evolutionary system of mineralogy. Part III: Primary chondrule mineralogy (4566 to 4561 Ma). THE AMERICAN MINERALOGIST 2021; 106:325-350. [PMID: 33867542 PMCID: PMC8051150 DOI: 10.2138/am-2020-7564] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Information-rich attributes of minerals reveal their physical, chemical, and biological modes of origin in the context of planetary evolution, and thus they provide the basis for an evolutionary system of mineralogy. Part III of this system considers the formation of 43 different primary crystalline and amorphous phases in chondrules, which are diverse igneous droplets that formed in environments with high dust/gas ratios during an interval of planetesimal accretion and differentiation between 4566 and 4561 Ma. Chondrule mineralogy is complex, with several generations of initial droplet formation via various proposed heating mechanisms, followed in many instances by multiple episodes of reheating and partial melting. Primary chondrule mineralogy thus reflects a dynamic stage of mineral evolution, when the diversity and distribution of natural condensed solids expanded significantly.
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Affiliation(s)
- Robert M. Hazen
- Earth and Planets Laboratory, Carnegie Institution for Science, 5251 Broad Branch Road NW, Washington, D.C. 20015, U.S.A
| | - Shaunna M. Morrison
- Earth and Planets Laboratory, Carnegie Institution for Science, 5251 Broad Branch Road NW, Washington, D.C. 20015, U.S.A
| | - Anirudh Prabhu
- Tetherless World Constellation, Department of Earth and Environmental Sciences, Rensselaer Polytechnic Institute, Troy, New York 12180, U.S.A
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21
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Goodrich CA, Sanborn ME, Yin QZ, Kohl I, Frank D, Daly RT, Walsh KJ, Zolensky ME, Young ERD, Jenniskens P, Shaddad MH. Chromium Isotopic Evidence for Mixing of NC and CC Reservoirs in Polymict Ureilites: Implications for Dynamical Models of the Early Solar System. THE PLANETARY SCIENCE JOURNAL 2021; 2:13. [PMID: 33681766 PMCID: PMC7931809 DOI: 10.3847/psj/abd258] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Nucleosynthetic isotope anomalies show that the first few million years of solar system history were characterized by two distinct cosmochemical reservoirs, CC (carbonaceous chondrites and related differentiated meteorites) and NC (the terrestrial planets and all other groups of chondrites and differentiated meteorites), widely interpreted to correspond to the outer and inner solar system, respectively. At some point, however, bulk CC and NC materials became mixed, and several dynamical models offer explanations for how and when this occurred. We use xenoliths of CC materials in polymict ureilite (NC) breccias to test the applicability of such models. Polymict ureilites represent regolith on ureilitic asteroids but contain carbonaceous chondrite-like xenoliths. We present the first 54Cr isotope data for such clasts, which, combined with oxygen and hydrogen isotopes, show that they are unique CC materials that became mixed with NC materials in these breccias. It has been suggested that such xenoliths were implanted into ureilites by outer solar system bodies migrating into the inner solar system during the gaseous disk phase ~3-5 Myr after CAI, as in the "Grand Tack" model. However, combined textural, petrologic, and spectroscopic observations suggest that they were added to ureilitic regolith at ~50-60 Myr after CAI, along with ordinary, enstatite, and Rumuruti-type chondrites, as a result of breakup of multiple parent bodies in the asteroid belt at this time. This is consistent with models for an early instability of the giant planets. The C-type asteroids from which the xenoliths were derived were already present in inner solar system orbits.
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Affiliation(s)
- Cyrena A Goodrich
- Lunar and Planetary Institute, Universities Space Research Association, 3600 Bay Area Blvd, Houston, TX 77058 USA
| | - Matthew E Sanborn
- Department of Earth and Planetary Sciences, University of California at Davis, Davis, CA 95616 USA
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California at Davis, Davis, CA 95616 USA
| | - Issaku Kohl
- Department of Earth and Planetary Sciences, University of California at Los Angeles, 595 Charles Young Drive East, Los Angeles, CA 90095 USA
| | - David Frank
- Hawai'i Institute of Geophysics and Planetology, Department of Earth Sciences, University of Hawai'i at Mānoa, Honolulu HI 96822 USA
| | - R Terik Daly
- The Johns Hopkins University Applied Physics Laboratory 11100 Johns Hopkins Road
| | - Kevin J Walsh
- Southwest Research Institute, 1050 Walnut St. Suite 300, Boulder, CO 80302 USA
| | - Michael E Zolensky
- Astromaterials Research and Exploration Science, NASA-Johnson Space Center Houston, TX 77058 USA
| | - Edward R D Young
- Department of Earth and Planetary Sciences, University of California at Los Angeles, 595 Charles Young Drive East, Los Angeles, CA 90095 USA
| | | | - Muawia H Shaddad
- Physics Department, University of Khartoum, Khartoum 11115 Sudan
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22
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Johansen A, Ronnet T, Bizzarro M, Schiller M, Lambrechts M, Nordlund Å, Lammer H. A pebble accretion model for the formation of the terrestrial planets in the Solar System. SCIENCE ADVANCES 2021; 7:7/8/eabc0444. [PMID: 33597233 PMCID: PMC7888959 DOI: 10.1126/sciadv.abc0444] [Citation(s) in RCA: 16] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/10/2020] [Accepted: 12/30/2020] [Indexed: 06/02/2023]
Abstract
Pebbles of millimeter sizes are abundant in protoplanetary discs around young stars. Chondrules inside primitive meteorites-formed by melting of dust aggregate pebbles or in impacts between planetesimals-have similar sizes. The role of pebble accretion for terrestrial planet formation is nevertheless unclear. Here, we present a model where inward-drifting pebbles feed the growth of terrestrial planets. The masses and orbits of Venus, Earth, Theia (which later collided with Earth to form the Moon), and Mars are all consistent with pebble accretion onto protoplanets that formed around Mars' orbit and migrated to their final positions while growing. The isotopic compositions of Earth and Mars are matched qualitatively by accretion of two generations of pebbles, carrying distinct isotopic signatures. Last, we show that the water and carbon budget of Earth can be delivered by pebbles from the early generation before the gas envelope became hot enough to vaporize volatiles.
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Affiliation(s)
- Anders Johansen
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark.
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 221 00 Lund, Sweden
| | - Thomas Ronnet
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 221 00 Lund, Sweden
| | - Martin Bizzarro
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
| | - Martin Schiller
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen, Denmark
| | - Michiel Lambrechts
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 221 00 Lund, Sweden
| | - Åke Nordlund
- Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark
| | - Helmut Lammer
- Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, 8042 Graz, Austria
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23
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Lichtenberg T, Dra Żkowska J, Schönbächler M, Golabek GJ, Hands TO. Bifurcation of planetary building blocks during Solar System formation. Science 2021; 371:365-370. [PMID: 33479146 DOI: 10.1126/science.abb3091] [Citation(s) in RCA: 49] [Impact Index Per Article: 16.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/02/2020] [Accepted: 12/10/2020] [Indexed: 11/02/2022]
Abstract
Geochemical and astronomical evidence demonstrates that planet formation occurred in two spatially and temporally separated reservoirs. The origin of this dichotomy is unknown. We use numerical models to investigate how the evolution of the solar protoplanetary disk influenced the timing of protoplanet formation and their internal evolution. Migration of the water snow line can generate two distinct bursts of planetesimal formation that sample different source regions. These reservoirs evolve in divergent geophysical modes and develop distinct volatile contents, consistent with constraints from accretion chronology, thermochemistry, and the mass divergence of inner and outer Solar System. Our simulations suggest that the compositional fractionation and isotopic dichotomy of the Solar System was initiated by the interplay between disk dynamics, heterogeneous accretion, and internal evolution of forming protoplanets.
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Affiliation(s)
- Tim Lichtenberg
- Atmospheric, Oceanic and Planetary Physics, Department of Physics, University of Oxford, Oxford, UK.
| | - Joanna Dra Żkowska
- University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität München, Munich, Germany
| | - Maria Schönbächler
- Institute for Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | - Gregor J Golabek
- Bayerisches Geoinstitut, University of Bayreuth, Bayreuth, Germany
| | - Thomas O Hands
- Institute for Computational Science, University of Zurich, Zurich, Switzerland
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24
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25
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Fujiya W, Furukawa Y, Sugahara H, Koike M, Bajo KI, Chabot NL, Miura YN, Moynier F, Russell SS, Tachibana S, Takano Y, Usui T, Zolensky ME. Analytical protocols for Phobos regolith samples returned by the Martian Moons eXploration (MMX) mission. EARTH, PLANETS, AND SPACE : EPS 2021; 73:120. [PMID: 34776735 PMCID: PMC8550573 DOI: 10.1186/s40623-021-01438-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/03/2020] [Accepted: 05/10/2021] [Indexed: 05/12/2023]
Abstract
Japan Aerospace Exploration Agency (JAXA) will launch a spacecraft in 2024 for a sample return mission from Phobos (Martian Moons eXploration: MMX). Touchdown operations are planned to be performed twice at different landing sites on the Phobos surface to collect > 10 g of the Phobos surface materials with coring and pneumatic sampling systems on board. The Sample Analysis Working Team (SAWT) of MMX is now designing analytical protocols of the returned Phobos samples to shed light on the origin of the Martian moons as well as the evolution of the Mars-moon system. Observations of petrology and mineralogy, and measurements of bulk chemical compositions and stable isotopic ratios of, e.g., O, Cr, Ti, and Zn can provide crucial information about the origin of Phobos. If Phobos is a captured asteroid composed of primitive chondritic materials, as inferred from its reflectance spectra, geochemical data including the nature of organic matter as well as bulk H and N isotopic compositions characterize the volatile materials in the samples and constrain the type of the captured asteroid. Cosmogenic and solar wind components, most pronounced in noble gas isotopic compositions, can reveal surface processes on Phobos. Long- and short-lived radionuclide chronometry such as 53Mn-53Cr and 87Rb-87Sr systematics can date pivotal events like impacts, thermal metamorphism, and aqueous alteration on Phobos. It should be noted that the Phobos regolith is expected to contain a small amount of materials delivered from Mars, which may be physically and chemically different from any Martian meteorites in our collection and thus are particularly precious. The analysis plan will be designed to detect such Martian materials, if any, from the returned samples dominated by the endogenous Phobos materials in curation procedures at JAXA before they are processed for further analyses.
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Affiliation(s)
- Wataru Fujiya
- Ibaraki University, 2-1-1 Bunkyo, Mito, Ibaraki 310-8512 Japan
| | - Yoshihiro Furukawa
- Tohoku University, 6-3 Aza-aoba, Aramaki, Aoba-ku, Sendai, 980-8578 Japan
| | - Haruna Sugahara
- Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 252-5210 Japan
| | - Mizuho Koike
- Hiroshima University, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 739-8526 Japan
| | - Ken-ichi Bajo
- Department of Earth and Planetary Sciences, Hokkaido University, N10W8 Kita-ku, Sapporo, 060-0810 Japan
| | - Nancy L. Chabot
- Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA
| | - Yayoi N. Miura
- Earthquake Research Institute, University of Tokyo, 1-1-1 Yayoi, Bunkyo-ku, Tokyo, 113-0032 Japan
| | - Frederic Moynier
- Institut de Physique du Globe de Paris, CNRS, University of Paris, Paris, France
| | - Sara S. Russell
- Department of Earth Sciences, Natural History Museum, Cromwell Road, London, SW7 5BD UK
| | - Shogo Tachibana
- Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 252-5210 Japan
- UTOPS, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, 113-0033 Japan
| | - Yoshinori Takano
- Biogeochemistry Research Center, Japan Agency for Marine-Earth Science and Technology, 2-15 Natsushima, Yokosuka, 237-0061 Japan
| | - Tomohiro Usui
- Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 252-5210 Japan
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26
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Brennecka GA, Burkhardt C, Budde G, Kruijer TS, Nimmo F, Kleine T. Astronomical context of Solar System formation from molybdenum isotopes in meteorite inclusions. Science 2020; 370:837-840. [PMID: 33184211 DOI: 10.1126/science.aaz8482] [Citation(s) in RCA: 14] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/14/2019] [Accepted: 09/16/2020] [Indexed: 11/02/2022]
Abstract
Calcium-aluminum-rich inclusions (CAIs) in meteorites are the first solids to have formed in the Solar System, defining the epoch of its birth on an absolute time scale. This provides a link between astronomical observations of star formation and cosmochemical studies of Solar System formation. We show that the distinct molybdenum isotopic compositions of CAIs cover almost the entire compositional range of material that formed in the protoplanetary disk. We propose that CAIs formed while the Sun was in transition from the protostellar to pre-main sequence (T Tauri) phase of star formation, placing Solar System formation within an astronomical context. Our results imply that the bulk of the material that formed the Sun and Solar System accreted within the CAI-forming epoch, which lasted less than 200,000 years.
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Affiliation(s)
- Gregory A Brennecka
- Lawrence Livermore National Laboratory, Livermore, CA, USA. .,Institut für Planetologie, University of Münster, Münster, Germany
| | | | - Gerrit Budde
- Institut für Planetologie, University of Münster, Münster, Germany.,Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Thomas S Kruijer
- Lawrence Livermore National Laboratory, Livermore, CA, USA.,Museum für Naturkunde, Leibniz Institute for Evolution and Biodiversity Science, Berlin, Germany
| | - Francis Nimmo
- Department of Earth & Planetary Sciences, University of California Santa Cruz, Santa Cruz, CA, USA
| | - Thorsten Kleine
- Institut für Planetologie, University of Münster, Münster, Germany
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27
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Tornabene HA, Hilton CD, Bermingham KR, Ash RD, Walker RJ. Genetics, Age and Crystallization History of Group IIC Iron Meteorites. GEOCHIMICA ET COSMOCHIMICA ACTA 2020; 288:36-50. [PMID: 33273746 PMCID: PMC7709713 DOI: 10.1016/j.gca.2020.07.036] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
The eight iron meteorites currently classified as belonging to the IIC group were characterized with respect to the compositions of 21 siderophile elements. Several of these meteorites were also characterized for mass independent isotopic compositions of Mo, Ru and W. Chemical and isotopic data for one, Wiley, indicate that it is not a IIC iron meteorite and should be reclassified as ungrouped. The remaining seven IIC iron meteorites exhibit broadly similar bulk chemical and isotopic characteristics, consistent with an origin from a common parent body. Variations in highly siderophile element (HSE) abundances among the members of the group can be well accounted for by a fractional crystallization model with all the meteorites crystallizing between ~10 and ~26% of the original melt, assuming initial S and P concentrations of 8 wt.% and 2 wt.%, respectively. Abundances of HSE estimated for the parental melt suggest a composition with chondritic relative abundances of HSE ~6 times higher than in bulk carbonaceous chondrites, consistent with the IIC irons sampling a parent body core comprising ~17% of the mass of the body. Radiogenic 182W abundances of two group IIC irons, corrected for a nucleosynthetic component, indicate a metal-silicate segregation age of 3.2 ± 0.5 Myr subsequent to the formation of Calcium-Aluminum-rich Inclusions (CAI). When this age is coupled with thermal modeling, and assumptions about the Hf/W of precursor materials, a parent body accretion age of 1.4 ± 0.5 Myr (post-CAI) is obtained. The IIC irons and Wiley have 100Ru mass independent "genetic" isotopic compositions that are identical to other irons with so-called carbonaceous chondrite (CC) type genetic affinities, but enrichments in 94,95,97Mo and 183W that indicate greater s-process deficits relative to most known CC iron meteorites. If the IIC irons and Wiley are of the CC type, this indicates variable s-process deficits within the CC reservoir, similar to the s-process variability within the NC reservoir observed for iron meteorites. Nucleosynthetic models indicate that Mo and 183W s-process variability should correlate with Ru isotopic variability, which is not observed. This may indicate the IIC irons and Wiley experienced selective thermal processing of nucleosynthetic carriers, or are genetically distinct from the CC and NC precursor materials.
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Affiliation(s)
- Hope A Tornabene
- Department of Geology, University of Maryland, College Park, Maryland, 20742, USA
| | - Connor D Hilton
- Department of Geology, University of Maryland, College Park, Maryland, 20742, USA
| | | | - Richard D Ash
- Department of Geology, University of Maryland, College Park, Maryland, 20742, USA
| | - Richard J Walker
- Department of Geology, University of Maryland, College Park, Maryland, 20742, USA
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28
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Ku Y, Jacobsen SB. Potassium isotope anomalies in meteorites inherited from the protosolar molecular cloud. SCIENCE ADVANCES 2020; 6:6/41/eabd0511. [PMID: 33036981 PMCID: PMC7546711 DOI: 10.1126/sciadv.abd0511] [Citation(s) in RCA: 10] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/28/2020] [Accepted: 08/19/2020] [Indexed: 05/31/2023]
Abstract
Potassium (K) and other moderately volatile elements are depleted in many solar system bodies relative to CI chondrites, which closely match the composition of the Sun. These depletions and associated isotopic fractionations were initially believed to result from thermal processing in the protoplanetary disk, but so far, no correlation between the K depletion and its isotopic composition has been found. Our new high-precision K isotope data correlate with other neutron-rich nuclides (e.g., 64Ni and 54Cr) and suggest that the observed 41K variations have a nucleosynthetic origin. We propose that K isotope anomalies are inherited from an isotopically heterogeneous protosolar molecular cloud, and were preserved in bulk primitive meteorites. Thus, the heterogeneous distribution of both refractory and moderately volatile elements in chondritic meteorites points to a limited radial mixing in the protoplanetary disk.
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Affiliation(s)
- Y Ku
- Department of Earth and Planetary Sciences, Harvard University, 20 Oxford Street, Cambridge, MA 02138, USA.
| | - S B Jacobsen
- Department of Earth and Planetary Sciences, Harvard University, 20 Oxford Street, Cambridge, MA 02138, USA
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29
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Williams CD, Sanborn ME, Defouilloy C, Yin QZ, Kita NT, Ebel DS, Yamakawa A, Yamashita K. Chondrules reveal large-scale outward transport of inner Solar System materials in the protoplanetary disk. Proc Natl Acad Sci U S A 2020; 117:23426-23435. [PMID: 32900966 PMCID: PMC7519341 DOI: 10.1073/pnas.2005235117] [Citation(s) in RCA: 31] [Impact Index Per Article: 7.8] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Dynamic models of the protoplanetary disk indicate there should be large-scale material transport in and out of the inner Solar System, but direct evidence for such transport is scarce. Here we show that the ε50Ti-ε54Cr-Δ17O systematics of large individual chondrules, which typically formed 2 to 3 My after the formation of the first solids in the Solar System, indicate certain meteorites (CV and CK chondrites) that formed in the outer Solar System accreted an assortment of both inner and outer Solar System materials, as well as material previously unidentified through the analysis of bulk meteorites. Mixing with primordial refractory components reveals a "missing reservoir" that bridges the gap between inner and outer Solar System materials. We also observe chondrules with positive ε50Ti and ε54Cr plot with a constant offset below the primitive chondrule mineral line (PCM), indicating that they are on the slope ∼1.0 in the oxygen three-isotope diagram. In contrast, chondrules with negative ε50Ti and ε54Cr increasingly deviate above from PCM line with increasing δ18O, suggesting that they are on a mixing trend with an ordinary chondrite-like isotope reservoir. Furthermore, the Δ17O-Mg# systematics of these chondrules indicate they formed in environments characterized by distinct abundances of dust and H2O ice. We posit that large-scale outward transport of nominally inner Solar System materials most likely occurred along the midplane associated with a viscously evolving disk and that CV and CK chondrules formed in local regions of enhanced gas pressure and dust density created by the formation of Jupiter.
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Affiliation(s)
- Curtis D Williams
- Department of Earth and Planetary Sciences, University of California, Davis, CA 95616;
| | - Matthew E Sanborn
- Department of Earth and Planetary Sciences, University of California, Davis, CA 95616
| | - Céline Defouilloy
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California, Davis, CA 95616;
| | - Noriko T Kita
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706
| | - Denton S Ebel
- Department of Earth and Planetary Sciences, American Museum of Natural History, New York, NY 10024
| | - Akane Yamakawa
- Department of Earth and Planetary Sciences, University of California, Davis, CA 95616
| | - Katsuyuki Yamashita
- Graduate School of Natural Science and Technology, Okayama University, Kita-ku, 700-8530 Okayama, Japan
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30
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Hilton CD, Walker RJ. New implications for the origin of the IAB main group iron meteorites and the isotopic evolution of the noncarbonaceous (NC) reservoir. EARTH AND PLANETARY SCIENCE LETTERS 2020; 540:116248. [PMID: 33273744 PMCID: PMC7709715 DOI: 10.1016/j.epsl.2020.116248] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
The origin of the IAB main group (MG) iron meteorites is explored through consideration of 182W isotopic compositions, thermal modeling of 26Al decay, and mass independent (nucleosynthetic) Mo isotopic compositions of planetesimals formed in the noncarbonaceous (NC) protosolar isotopic reservoir. A refined 182W model age for the meteorites Campo del Cielo, Canyon Diablo, and Nantan suggests that the IAB-MG parent body underwent some form of metal-silicate segregation as early as 5.3 ± 0.4 Myr after calcium-aluminum rich inclusion (CAI) formation or as late as 13.8 ± 1.4 Myr after CAI formation. If melting of the IAB-MG occurred prior to 7 Myr after CAI formation, it was likely driven by 26Al decay for a parent body radius >40 km. Otherwise, additional heat from impact is required for melting metal this late in Solar System history. If melting was partially or wholly the result of internal heating, a thermal model of 26Al decay heat production constrains the accretion age of the IAB-MG parent body to ~1.7 ± 0.4 Myr after CAI formation. If melting was, instead, dominantly caused by impact heating, thermal modeling suggests the parent body accreted more than 2 Myr after CAI formation. Comparison of Mo mass independent isotopic compositions of the IAB-MG to other NC bodies with constrained accretion ages suggests that the Mo isotopic composition of the NC reservoir changed with time, and that the IAB-MG parent body accreted between 2 to 3 Myr after CAI formation, thus requiring an origin by impact. The relationship between nucleosynthetic Mo isotopic compositions and accretion ages of planetesimals from the NC reservoir suggests that isotopic heterogeneity developed from either addition of s-process material to, or removal of coupled r-/p-process material from the NC reservoir.
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Affiliation(s)
- Connor D Hilton
- Department of Geology, University of Maryland, College Park, Maryland, 20742, USA
| | - Richard J Walker
- Department of Geology, University of Maryland, College Park, Maryland, 20742, USA
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31
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Larsen K, Wielandta D, Schillera M, Krot A, Bizzarro M. Episodic formation of refractory inclusions in the Solar System and their presolar heritage. EARTH AND PLANETARY SCIENCE LETTERS 2020; 535:116088. [PMID: 34334802 PMCID: PMC7611424 DOI: 10.1016/j.epsl.2020.116088] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
Refractory inclusions [Ca-Al-rich Inclusions (CAIs) and Amoeboid Olivine Aggregates (AOAs)] in primitive meteorites are the oldest Solar System solids. They formed in the hot inner protoplanetary disk and, as such, provide insights into the earliest disk dynamics and physicochemical processing of the dust and gas that accreted to form the Sun and its planetary system. Using the short-lived 26Al to 26Mg decay system, we show that bulk refractory inclusions in CV (Vigarano-type) and CR (Renazzo-type) carbonaceous chondrites captured at least two distinct 26Al-rich (26Al/27Al ratios of ~5 × 10-5) populations of refractory inclusions characterized by different initial 26Mg/24Mg isotope compositions (μ26Mg*0). Another 26Al-poor CAI records an even larger μ26Mg*0 deficit. This suggests that formation of refractory inclusions was punctuated and recurrent, possibly associated with episodic outbursts from the accreting proto-Sun lasting as short as <8000 yr. Our results support a model in which refractory inclusions formed close to the hot proto-Sun and were subsequently redistributed to the outer disk, beyond the orbit of Jupiter, plausibly via stellar outflows with progressively decreasing transport efficiency. We show that the magnesium isotope signatures in refractory inclusions mirrors the presolar grain record, demonstrating a mutual exclusivity between 26Al enrichments and large nucleosynthetic Mg isotope effects. This suggests that refractory inclusions formed by incomplete thermal processing of presolar dust, thereby inheriting a diluted signature of their isotope systematics. As such, they record snapshots in the progressive sublimation of isotopically anomalous presolar carriers through selective thermal processing of young dust components from the proto-Solar molecular cloud. We infer that 26Al-rich refractory inclusions incorporated 26Al-rich dust which formed <5 Myr prior to our Sun, whereas 26Al-poor inclusions (such as FUN- and PLAC-type CAIs) incorporated >10 Myr old dust.
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Affiliation(s)
- K.K. Larsen
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
| | - D. Wielandta
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
| | - M. Schillera
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
| | - A.N. Krot
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
- Hawai’i Institute of Geophysics and Planetology, University of Hawai’i at Manoa, HI 96822, USA
| | - M. Bizzarro
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
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32
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Gregory T, Luu TH, Coath CD, Russell SS, Elliott T. Primordial formation of major silicates in a protoplanetary disc with homogeneous 26Al/ 27Al. SCIENCE ADVANCES 2020; 6:eaay9626. [PMID: 32195348 PMCID: PMC7065882 DOI: 10.1126/sciadv.aay9626] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 08/01/2019] [Accepted: 12/11/2019] [Indexed: 06/10/2023]
Abstract
Understanding the spatial variability of initial 26Al/27Al in the solar system, i.e., (26Al/27Al)0, is of prime importance to meteorite chronology, planetary heat production, and protoplanetary disc mixing dynamics. The (26Al/27Al)0 of calcium-aluminum-rich inclusions (CAIs) in primitive meteorites (~5 × 10-5) is frequently assumed to reflect the (26Al/27Al)0 of the entire protoplanetary disc, and predicts its initial 26Mg/24Mg to be ~35 parts per million (ppm) less radiogenic than modern Earth (i.e., Δ'26Mg0 = -35 ppm). Others argue for spatially heterogeneous (26Al/27Al)0, where the source reservoirs of most primitive meteorite components have lower (26Al/27Al)0 at ~2.7 × 10-5 and Δ'26Mg0 of -16 ppm. We measured the magnesium isotope compositions of primitive meteoritic olivine, which originated outside of the CAI-forming reservoir(s), and report five grains whose Δ'26Mg0 are within uncertainty of -35 ppm. Our data thus affirm a model of a largely homogeneous protoplanetary disc with (26Al/27Al)0 of ~5 × 10-5, supporting the accuracy of the 26Al→26Mg chronometer.
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Affiliation(s)
- Timothy Gregory
- School of Earth Sciences, University of Bristol, Wills Memorial Building, Bristol BS8 1RJ, UK
- Department of Earth Sciences, The Natural History Museum, Cromwell Road, London SW7 5BD, UK
- National Environmental Isotope Facility, British Geological Survey, Nottingham NG12 5GG, UK
| | - Tu-Han Luu
- School of Earth Sciences, University of Bristol, Wills Memorial Building, Bristol BS8 1RJ, UK
| | - Christopher D. Coath
- School of Earth Sciences, University of Bristol, Wills Memorial Building, Bristol BS8 1RJ, UK
| | - Sara S. Russell
- Department of Earth Sciences, The Natural History Museum, Cromwell Road, London SW7 5BD, UK
| | - Tim Elliott
- School of Earth Sciences, University of Bristol, Wills Memorial Building, Bristol BS8 1RJ, UK
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33
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van Kooten E, Cavalcante L, Wielandt D, Bizzarro M. The role of Bells in the continuous accretion between the CM and CR chondrite reservoirs. METEORITICS & PLANETARY SCIENCE 2020; 55:575-590. [PMID: 32362738 PMCID: PMC7188250 DOI: 10.1111/maps.13459] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 12/10/2018] [Accepted: 01/28/2020] [Indexed: 06/11/2023]
Abstract
CM meteorites are dominant members of carbonaceous chondrites (CCs), which evidently accreted in a region separated from the terrestrial planets. These chondrites are key in determining the accretion regions of solar system materials, since in Mg and Cr isotope space, they intersect between what are identified as inner and outer solar system reservoirs. In this model, the outer reservoir is represented by metal-rich carbonaceous chondrites (MRCCs), including CR chondrites. An important question remains whether the barrier between MRCCs and CCs was a temporal or spatial one. CM chondrites and chondrules are used here to identify the nature of the barrier as well as the timescale of chondrite parent body accretion. We find based on high precision Mg and Cr isotope data of seven CM chondrites and 12 chondrules, that accretion in the CM chondrite reservoir was continuous lasting <3 Myr and showing late accretion of MRCC-like material reflected by the anomalous CM chondrite Bells. We further argue that although MRCCs likely accreted later than CM chondrites, CR chondrules must have initially formed from a reservoir spatially separated from CM chondrules. Finally, we hypothesize on the nature of the spatial barrier separating these reservoirs.
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Affiliation(s)
- Elishevah van Kooten
- Institut de Physique du Globe de ParisUniversité de ParisCNRSUMR 71541 rue Jussieu75238ParisFrance
| | | | - Daniel Wielandt
- Centre for Star and Planet Formation and Natural History Museum of DenmarkUniversity of CopenhagenDK‐1350CopenhagenDenmark
| | - Martin Bizzarro
- Centre for Star and Planet Formation and Natural History Museum of DenmarkUniversity of CopenhagenDK‐1350CopenhagenDenmark
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34
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Schiller M, Bizzarro M, Siebert J. Iron isotope evidence for very rapid accretion and differentiation of the proto-Earth. SCIENCE ADVANCES 2020; 6:eaay7604. [PMID: 32095530 PMCID: PMC7015677 DOI: 10.1126/sciadv.aay7604] [Citation(s) in RCA: 11] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/16/2019] [Accepted: 11/26/2019] [Indexed: 06/02/2023]
Abstract
Nucleosynthetic isotope variability among solar system objects provides insights into the accretion history of terrestrial planets. We report on the nucleosynthetic Fe isotope composition (μ54Fe) of various meteorites and show that the only material matching the terrestrial composition is CI (Ivuna-type) carbonaceous chondrites, which represent the bulk solar system composition. All other meteorites, including carbonaceous, ordinary, and enstatite chondrites, record excesses in μ54Fe. This observation is inconsistent with protracted growth of Earth by stochastic collisional accretion, which predicts a μ54Fe value reflecting a mixture of the various meteorite parent bodies. Instead, our results suggest a rapid accretion and differentiation of Earth during the ~5-million year disk lifetime, when the volatile-rich CI-like material is accreted to the proto-Sun via the inner disk.
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Affiliation(s)
- Martin Schiller
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5–7, DK-1350 Copenhagen, Denmark
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5–7, DK-1350 Copenhagen, Denmark
- Institut de Physique du Globe de Paris, Université Sorbonne Paris Cité, 75005 Paris, France
| | - Julien Siebert
- Institut de Physique du Globe de Paris, Université Sorbonne Paris Cité, 75005 Paris, France
- Institut Universitaire de France, Paris, France
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35
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Si-Mg isotopes in enstatite chondrites and accretion of reduced planetary bodies. Sci Rep 2020; 10:1273. [PMID: 31988372 PMCID: PMC6985146 DOI: 10.1038/s41598-020-57635-1] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/03/2019] [Accepted: 12/03/2019] [Indexed: 11/23/2022] Open
Abstract
Among the primitive meteorite classes, Enstatite Chondrites (EC) are believed to share a common origin with the Earth due to its close similarity with terrestrial mantle (Bulk Silicate Earth, BSE) for numerous isotope systematics. Si isotopes are an exception to this trend and the large δ30Si difference of ~0.3‰ between bulk EC and BSE has been used to argue against any major contribution of EC like planetary materials in Earth’s accretion. However, Si possess a bimodal distribution among silicate and metallic fractions of EC because of its formation under highly reducing conditions. Based on high precision Si isotope analyses in micro-milled phase separates of EH3 chondrites, here we report the presence of significantly light Si isotopes in EC-metals (δ30Si ≥ −6.94 ± 0.09‰, Mg/Si = ~0.001) whereas its silicate phases are isotopically heavier (Av. δ30SiEC-silicates = −0.33 ± 0.11‰, Mg/Si = ~1.01) and closer to BSE (δ30SiBSE = −0.29 ± 0.08‰). We discuss the origin of the observed Si isotope heterogeneity in terms of gas-solid interaction processes associated with metal-silicate condensation at high C/O environment (~0.83). Although the elevated δ30Si of BSE compared to chondrites is consistent with earlier conclusions that lighter Si has partitioned into Earth’s metallic core, our results indicate that the super-chondritic Si isotope composition of BSE does not reflect the sole consequence of high temperature-pressure core and mantle equilibration in a deep magma-ocean. Instead, Si along with Mg isotope analyses carried out in the same aliquot of EC micro-phase separates suggest that processes such as metal-silicate Si isotope fractionation at reduced nebular environment and vapor loss of lighter Si isotopes during planetary volatilization were also influential in establishing the Si isotope composition of terrestrial mantle.
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Ceballos E, Margalef-Martí R, Carrey R, Frei R, Otero N, Soler A, Ayora C. Characterisation of the natural attenuation of chromium contamination in the presence of nitrate using isotopic methods. A case study from the Matanza-Riachuelo River basin, Argentina. THE SCIENCE OF THE TOTAL ENVIRONMENT 2020; 699:134331. [PMID: 31670212 DOI: 10.1016/j.scitotenv.2019.134331] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/27/2019] [Revised: 08/10/2019] [Accepted: 09/05/2019] [Indexed: 06/10/2023]
Abstract
The groundwater contamination by hexavalent chromium (Cr(VI)) in a site of the Matanza-Riachuelo River basin (MRB), Argentina, has been evaluated by determining the processes that control the natural mobility and attenuation of Cr(VI) in the presence of high nitrate (NO3-) contents. The groundwater Cr(VI) concentrations ranged between 1.9E-5 mM and 0.04 mM, while the NO3- concentrations ranged between 0.5 mM and 3.9 mM. In order to evaluate the natural attenuation of Cr(VI) and NO3- in the MRB groundwater, Cr and N isotopes were measured in these contaminants. In addition, laboratory batch experiments were performed to determine the isotope fractionation (ε) during the reduction of Cr(VI) under denitrifying conditions. While the Cr(VI) reduction rate is not affected by the presence of NO3-, the NO3- attenuation is slower in the presence of Cr(VI). Nevertheless, no significant differences on ε values were observed when testing the absence or presence of each contaminant. The ε53Cr determined in the batch experiments describe a two- stage trend, in which Stage I is characterized by ε53Cr ~-1.8‰ and Stage II by ε53Cr ~-0.9‰. The respective ε15NNO3 obtained is -23.9‰ whereas ε18ONO3 amount to -25.7‰. Using these ε values and a Rayleigh fractionation model we estimate that an average of 60% of the original Cr(VI) is removed from the groundwater of the contaminated site. Moreover, the average degree of NO3- attenuation by denitrification is found to be about 20%. This study provides valuable information about the dynamics of a complex system that can serve as a basis for efficient management of contaminated groundwater in the most populated and industrialized basin of Argentina.
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Affiliation(s)
- Elina Ceballos
- Instituto de Hidrología de Llanuras "Dr. Eduardo J. Usunoff", CONICET-UNCPBA-CIC, República de Italia 780, 47 (B7300), Azul, Buenos Aires, Argentina.
| | - Rosanna Margalef-Martí
- Grup MAiMA, SGR Mineralogia Aplicada, Geoquímica i Geomicrobiologia, Departament de Mineralogia, Petrologia i Geologia Aplicada, Facultat de Ciències de la Terra, Universitat de Barcelona, UB, C/Martí i Franquès, s/n, 08028 Barcelona, Spain
| | - Raul Carrey
- Grup MAiMA, SGR Mineralogia Aplicada, Geoquímica i Geomicrobiologia, Departament de Mineralogia, Petrologia i Geologia Aplicada, Facultat de Ciències de la Terra, Universitat de Barcelona, UB, C/Martí i Franquès, s/n, 08028 Barcelona, Spain
| | - Robert Frei
- Department of Geosciences and Natural Resource Management, University of Copenhagen, Copenhagen, Denmark
| | - Neus Otero
- Grup MAiMA, SGR Mineralogia Aplicada, Geoquímica i Geomicrobiologia, Departament de Mineralogia, Petrologia i Geologia Aplicada, Facultat de Ciències de la Terra, Universitat de Barcelona, UB, C/Martí i Franquès, s/n, 08028 Barcelona, Spain; Serra Húnter Fellow, Generalitat de Catalunya, Spain
| | - Albert Soler
- Grup MAiMA, SGR Mineralogia Aplicada, Geoquímica i Geomicrobiologia, Departament de Mineralogia, Petrologia i Geologia Aplicada, Facultat de Ciències de la Terra, Universitat de Barcelona, UB, C/Martí i Franquès, s/n, 08028 Barcelona, Spain
| | - Carlos Ayora
- Department of Geoscience, Institute of Environmental Assessment and Water Research, IDAEA-CSIC, C/Jordi Girona, 18, 08028 Barcelona, Spain
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Factors Controlling the Chromium Isotope Compositions in Podiform Chromitites. MINERALS 2019. [DOI: 10.3390/min10010010] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
The application of Cr isotope compositions to the investigation of magmatic and post-magmatic effects on chromitites is unexplored. This study presents and compiles the first Cr stable isotope data (δ53Cr values) with major and trace element, contents from the Balkan Peninsula, aiming to provide an overview of the compositional variations of δ53Cr values in ophiolite-hosted chromitites and to delineate geochemical constraints controlling the composition of chromitites. The studied chromitites exhibit δ53Cr values ranging from −0.184‰ to +0.159‰, falling in the range of so-called “igneous Earth” or “Earth’s mantle inventory” with values −0.12 ± 0.11‰ to 0.079 ± 0.129‰ (2sd). A characteristic feature is the slightly positively fractionated δ53Cr values of all chromitite samples from Othrys (+0.043 ± 0.03‰), and the occurrence of a wide range of δ53Cr values spanning from positively, slightly negatively to the most negatively fractionated signatures (Pindos, δ53Cr = −0.147 to +0.009‰; Skyros, δ53Cr = −0.078 to +0.159‰). The observed negative trend between δ53Cr values and Cr/(Cr + Al) ratios may reflect a decrease in the δ53Cr values of chromitites with increasing partial melting degree. Alternatively, it may point to processes related to magmatic differentiation, as can be seen in our data from Mikrokleisoura (Vourinos).
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Torrano ZA, Brennecka GA, Williams CD, Romaniello SJ, Rai VK, Wadhwa M. Titanium isotope signatures of calcium-aluminum-rich inclusions from CV and CK chondrites: Implications for early Solar System reservoirs and mixing. GEOCHIMICA ET COSMOCHIMICA ACTA 2019; 263:13-30. [PMID: 33414563 PMCID: PMC7786560 DOI: 10.1016/j.gca.2019.07.051] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Calcium-aluminum-rich inclusions (CAIs) are the first solids to form in the early Solar System, and they exhibit nucleosynthetic anomalies in many isotope systems. The overwhelming majority of isotopic data for CAIs has been limited to inclusions from the CV chondrite Allende and a select few other CV, CO, CM, and ordinary chondrites. It is therefore important to ascertain whether previously reported values for CAIs are representative of the broader CAI-forming region and to make a more rigorous assessment of the extent and implications of isotopic heterogeneity in the early Solar System. Here, we report the mass-independent Ti isotopic compositions of a suite of 23 CAIs of diverse petrologic and geochemical types, including 11 from Allende and 12 from seven other CV3 and CK3 chondrites; the data for CAIs from CK chondrites represent the first reported measurements of Ti isotope compositions of refractory inclusions from this meteorite class. The resolved variation in the mass-independent Ti isotopic compositions of these CAIs indicates that the CAI-forming region of the early Solar System preserved isotopic variability at their time of formation. Nevertheless, the range of Ti isotope compositions reported here for CAIs from CV and CK chondrites falls within the range observed in previously analyzed CAIs from CV, CO, CM, and ordinary chondrites. This implies that CAIs from CV, CK, CO, CM, and ordinary chondrites originated from a common nebular source reservoir characterized by mass-independent isotopic variability in Ti (and other select elements). We further interpret these data to indicate that the Ti isotope anomalies in CAIs represent the isotopic signatures of supernova components in presolar grains that were incorporated into the Solar System in an initially poorly mixed reservoir that was progressively homogenized over time. We conclude that the differing degrees of isotopic variability observed for different elements in normal CAIs are the result of distinct carrier phases and that these CAIs were likely formed towards the final stages of homogenization of the large-scale isotopic heterogeneity that initially existed in the solar nebula.
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Affiliation(s)
- Zachary A. Torrano
- Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, Tempe, AZ, 85287, USA
| | | | - Curtis D. Williams
- Department of Earth and Planetary Sciences, University of California at Davis, Davis, CA 95616, USA
| | - Stephen J. Romaniello
- Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, Tempe, AZ, 85287, USA
| | - Vinai K. Rai
- Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, Tempe, AZ, 85287, USA
| | - Meenakshi Wadhwa
- Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, Tempe, AZ, 85287, USA
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Shollenberger QR, Wittke A, Render J, Mane P, Schuth S, Weyer S, Gussone N, Wadhwa M, Brennecka GA. Combined mass-dependent and nucleosynthetic isotope variations in refractory inclusions and their mineral separates to determine their original Fe isotope compositions. GEOCHIMICA ET COSMOCHIMICA ACTA 2019; 263:215-234. [PMID: 33353988 PMCID: PMC7751496 DOI: 10.1016/j.gca.2019.07.021] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Calcium-aluminum-rich inclusions (CAIs) are the oldest dated materials that provide crucial information about the isotopic reservoirs present in the early Solar System. For a variety of elements, CAIs have isotope compositions that are uniform yet distinct from later formed solid material. However, despite being the most abundant metal in the Solar System, the isotopic composition of Fe in CAIs is not well constrained. In an attempt to determine the Fe isotopic compositions of CAIs, we combine extensive work from a previously studied CAI sample set with new isotopic work characterizing mass-dependent and mass-independent (nucleosynthetic) signatures in Mg, Ca, and Fe. This investigation includes work on three mineral separates of the Allende CAI Egg 2. For all isotope systems investigated, we find that in general, fine-grained CAIs exhibit light mass-dependent isotopic signatures relative to terrestrial standards, whereas igneous CAIs have heavier isotopic compositions relative to the fine-grained CAIs. Importantly, the mass-dependent Fe isotope signatures of bulk CAIs show a range of both light (fine-grained CAIs) and heavy (igneous CAIs) isotopic signatures relative to bulk chondrites, suggesting that Fe isotope signatures in CAIs largely derive from mass fractionation events such as condensation and evaporation occurring in the nebula. Such signatures show that a significant portion of the secondary alteration experienced by CAIs, particularly prevalent in fine-grained inclusions, occurred in the nebula prior to accretion into their respective parent bodies. Regarding nucleosynthetic Fe isotope signatures, we do not observe any variation outside of analytical uncertainty in bulk CAIs compared to terrestrial standards. In contrast, all three Egg 2 mineral separates display resolved mass-independent excesses in 56Fe compared to terrestrial standards. Furthermore, we find that the combined mass-dependent and nucleosynthetic Fe isotopic compositions of the Egg 2 mineral separates are well correlated, likely indicating that Fe indigenous to the CAI is mixed with less anomalous Fe, presumably from the solar nebula. Thus, these reported nucleosynthetic anomalies may point in the direction of the original Fe isotope composition of the CAI-forming region, but they likely only provide a minimum isotopic difference between the original mass-independent Fe isotopic composition of CAIs and that of later formed solids.
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Affiliation(s)
- Quinn R. Shollenberger
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Straße 10, 48149 Münster, Germany
| | - Andreas Wittke
- Institut für Mineralogie, University of Münster, Corrensstraße 24, 48149 Münster, Germany
| | - Jan Render
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Straße 10, 48149 Münster, Germany
| | - Prajkta Mane
- School of Earth and Space Exploration, Arizona State University, PO Box 871404, Tempe, AZ 85287-1404 USA
| | - Stephan Schuth
- Institut für Mineralogie, Leibniz University Hannover, Callinstraße 3, 30167 Hannover, Germany
| | - Stefan Weyer
- Institut für Mineralogie, Leibniz University Hannover, Callinstraße 3, 30167 Hannover, Germany
| | - Nikolaus Gussone
- Institut für Mineralogie, University of Münster, Corrensstraße 24, 48149 Münster, Germany
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, PO Box 871404, Tempe, AZ 85287-1404 USA
| | - Gregory A. Brennecka
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Straße 10, 48149 Münster, Germany
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Jansen C, Brenker F, Krot A, Zipfel J, Pack A, Labenne L, Bizzarro M, Schiller M. MINERALOGY, PETROLOGY AND OXYGEN ISOTOPIC COMPOSITION OF NORTHWEST AFRICA (NWA) 12379, A NEW METAL-RICH CHONDRITE WITH AFFINITY TO ORDINARY CHONDRITES. PROCEEDINGS OF LUNAR AND PLANETARY SCIENCE 2019; 50:2741. [PMID: 31631921 PMCID: PMC6800724 DOI: 10.1016/j.chemer.2019.125537] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Affiliation(s)
- C.A. Jansen
- Institute for Geosciences, Goethe University, Germany
| | - F.E. Brenker
- Institute for Geosciences, Goethe University, Germany
| | - A.N. Krot
- Institute for Geosciences, Goethe University, Germany
- Hawai’i Institute of Geophysics & Planetology, University of Hawai’i, Honolulu, USA
| | - J. Zipfel
- Senckenberg Forschungsinstitut & Naturmuseum, Germany
| | - A. Pack
- Georg-August-Universität, Göttingen, Germany
| | | | - M. Bizzarro
- Centre for Star & Planet Formation, Copen-hagen, Denmark
| | - M. Schiller
- Centre for Star & Planet Formation, Copen-hagen, Denmark
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Krot AN. CHONDRITES AND THEIR COMPONENTS: RECORDS OF EARLY SOLAR SYSTEM PROCESSES. METEORITICS & PLANETARY SCIENCE 2019; 54:1647-1691. [PMID: 31379423 PMCID: PMC6677159 DOI: 10.1111/maps.13350] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/04/2019] [Accepted: 06/06/2019] [Indexed: 06/10/2023]
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Hibiya Y, Archer GJ, Tanaka R, Sanborn ME, Sato Y, Iizuka T, Ozawa K, Walker RJ, Yamaguchi A, Yin QZ, Nakamura T, Irving AJ. The origin of the unique achondrite Northwest Africa 6704: Constraints from petrology, chemistry and Re-Os, O and Ti isotope systematics. GEOCHIMICA ET COSMOCHIMICA ACTA 2019; 245:597-627. [PMID: 30983599 PMCID: PMC6457475 DOI: 10.1016/j.gca.2018.04.031] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
Northwest Africa (NWA) 6704 is a unique achondrite characterized by a near-chondritic major element composition with a remarkably intact igneous texture. To investigate the origin of this unique achondrite, we have conducted a combined petrologic, chemical, and 187Re-187Os, O, and Ti isotopic study. The meteorite consists of orthopyroxene megacrysts (En55-57Wo3-4Fs40-42; Fe/Mn = 1.4) up to 1.7 cm in length with finer interstices of olivine (Fa50-53; Fe/Mn = 1.1-2.1), chromite (Cr# ~ 0.94), awaruite, sulfides, plagioclase (Ab92An5Or3) and merrillite. The results of morphology, lattice orientation analysis, and mineral chemistry indicate that orthopyroxene megacrysts were originally hollow dendrites that most likely crystallized under high super-saturation and super-cooling conditions (1-102 °C/h), whereas the other phases crystallized between branches of the dendrites in the order of awaruite, chromite → olivine → merrillite → plagioclase. In spite of the inferred high supersaturation, the remarkably large size of orthopyroxene can be explained as a result of crystallization from a melt containing a limited number of nuclei that are preserved as orthopyroxene megacryst cores having high Mg# or including vermicular olivine. The Re-Os isotope data for bulk and metal fractions yield an isochron age of 4576 ± 250 Ma, consistent with only limited open system behavior of highly siderophile elements (HSE) since formation. The bulk chemical composition is characterized by broadly chondritic absolute abundances and only weakly fractionated chondrite-normalized patterns for HSE and rare earth elements (REE), together with substantial depletion of highly volatile elements relative to chondrites. The HSE and REE characteristics indicate that the parental melt and its protolith had not undergone significant segregation of metals, sulfides, or silicate minerals. These combined results suggest that a chondritic precursor to NWA 6704 was heated well above its liquidus temperature so that highly volatile elements were lost and the generated melt initially contained few nuclei of relict orthopyroxene, but the melting and subsequent crystallization took place on a timescale too short to allow magmatic differentiation. Such rapid melting and crystallization might occur as a result of impact on an undifferentiated asteroid. The O-Ti isotope systematics (Δ17O = -1.052 ± 0.004, 2 SD; ε50Ti = 2.28 ± 0.23, 2 SD) indicate that the NWA 6704 parent body sampled the same isotopic reservoirs in the solar nebula as the carbonaceous chondrite parent bodies. This is consistent with carbonaceous chondrite-like refractory element abundances and oxygen fugacity (FMQ = -2.6) in NWA 6704. Yet, the Si/Mg ratio of NWA 6704 is remarkably higher than those of carbonaceous chondrites, suggesting significant nebular fractionation of forsterite in its provenance.
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Affiliation(s)
- Yuki Hibiya
- Department of Earth and Planetary Science, University of Tokyo, Hongo 7-3-1, Bunkyo, Tokyo 113-0033, Japan
| | - Gregory J. Archer
- Department of Geology, University of Maryland, College Park, MD 20742, USA
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Straße 10, 48149 Münster, Germany
| | - Ryoji Tanaka
- The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials (IPM), Okayama University, Misasa, Tottori 682-0193, Japan
| | - Matthew E. Sanborn
- Department of Earth and Planetary Sciences, University of California-Davis, One Shields Avenue, Davis, CA 95616, USA
| | - Yuya Sato
- Laboratory for Early Solar System Evolution, Division of Earth and Planetary Materials Science, Graduate School of Science, Tohoku University, Aoba, Sendai, Miyagi 980-8578, Japan
| | - Tsuyoshi Iizuka
- Department of Earth and Planetary Science, University of Tokyo, Hongo 7-3-1, Bunkyo, Tokyo 113-0033, Japan
| | - Kazuhito Ozawa
- Department of Earth and Planetary Science, University of Tokyo, Hongo 7-3-1, Bunkyo, Tokyo 113-0033, Japan
| | - Richard J. Walker
- Department of Geology, University of Maryland, College Park, MD 20742, USA
| | - Akira Yamaguchi
- National Institute of Polar Research, 10-3, Midori-cho, Tachikawa-shi, Tokyo 190-8518, Japan
- Department of Polar Science, School of Multidisciplinary Science, SOKENDAI (The Graduate University for Advanced Studies), Tokyo 190-8518, Japan
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California-Davis, One Shields Avenue, Davis, CA 95616, USA
| | - Tomoki Nakamura
- Laboratory for Early Solar System Evolution, Division of Earth and Planetary Materials Science, Graduate School of Science, Tohoku University, Aoba, Sendai, Miyagi 980-8578, Japan
| | - Anthony J. Irving
- Department of Earth and Space Sciences, University of Washington, Seattle, WA, USA
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Holden NE, Coplen TB, Böhlke JK, Tarbox LV, Benefield J, de Laeter JR, Mahaffy PG, O’Connor G, Roth E, Tepper DH, Walczyk T, Wieser ME, Yoneda S. IUPAC Periodic Table of the Elements and Isotopes (IPTEI) for the Education Community (IUPAC Technical Report). PURE APPL CHEM 2018. [DOI: 10.1515/pac-2015-0703] [Citation(s) in RCA: 52] [Impact Index Per Article: 8.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 12/19/2022]
Abstract
Abstract
The IUPAC (International Union of Pure and Applied Chemistry) Periodic Table of the Elements and Isotopes (IPTEI) was created to familiarize students, teachers, and non-professionals with the existence and importance of isotopes of the chemical elements. The IPTEI is modeled on the familiar Periodic Table of the Chemical Elements. The IPTEI is intended to hang on the walls of chemistry laboratories and classrooms. Each cell of the IPTEI provides the chemical name, symbol, atomic number, and standard atomic weight of an element. Color-coded pie charts in each element cell display the stable isotopes and the relatively long-lived radioactive isotopes having characteristic terrestrial isotopic compositions that determine the standard atomic weight of each element. The background color scheme of cells categorizes the 118 elements into four groups: (1) white indicates the element has no standard atomic weight, (2) blue indicates the element has only one isotope that is used to determine its standard atomic weight, which is given as a single value with an uncertainty, (3) yellow indicates the element has two or more isotopes that are used to determine its standard atomic weight, which is given as a single value with an uncertainty, and (4) pink indicates the element has a well-documented variation in its atomic weight, and the standard atomic weight is expressed as an interval. An element-by-element review accompanies the IPTEI and includes a chart of all known stable and radioactive isotopes for each element. Practical applications of isotopic measurements and technologies are included for the following fields: forensic science, geochronology, Earth-system sciences, environmental science, and human health sciences, including medical diagnosis and treatment.
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Affiliation(s)
- Norman E. Holden
- National Nuclear Data Center, Brookhaven National Laboratory , Upton, NY , USA
| | | | | | | | | | | | | | | | - Etienne Roth
- Commissariat à l’énergie atomique (CEA) , Gif-sur-Yvette, France
| | | | - Thomas Walczyk
- Department of Chemistry , National University of Singapore , Singapore , Singapore
| | - Michael E. Wieser
- Department of Physics and Astronomy , University of Calgary , Calgary , Canada
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The Effect of Jupiter's Formation on the Distribution of Refractory Elements and Inclusions in Meteorites. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4365/aad95f] [Citation(s) in RCA: 115] [Impact Index Per Article: 19.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Isotopic evolution of the protoplanetary disk and the building blocks of Earth and the Moon. Nature 2018; 555:507-510. [PMID: 29565359 PMCID: PMC5884421 DOI: 10.1038/nature25990] [Citation(s) in RCA: 100] [Impact Index Per Article: 16.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/28/2017] [Accepted: 01/22/2018] [Indexed: 11/10/2022]
Abstract
Nucleosynthetic isotope variability amongst Solar System objects is commonly used to probe the genetic relationship between meteorite groups and rocky planets, which, in turn, may provide insights into the building blocks of the Earth-Moon system1–5. Using this approach, it is inferred that no primitive meteorite matches the terrestrial composition such that the nature of the disk material that accreted to form the Earth and Moon is unconstrained6. This conclusion, however, is based on the assumption that the observed nucleosynthetic variability amongst inner Solar System objects predominantly reflects spatial heterogeneity. Here, we use the isotopic composition of the refractory element calcium to show that the inner Solar System’s nucleosynthetic variability in the mass-independent 48Ca/44Ca ratio (μ48Ca) primarily represents a rapid change in the μ48Ca composition of disk solids associated with early mass accretion to the proto-Sun. In detail, the μ48Ca values of samples originating from the ureilite and angrite parent bodies as well as Vesta, Mars and Earth are positively correlated to the masses of the inferred parent asteroids and planets – a proxy of their accretion timescales – implying a secular evolution of the bulk μ48Ca disk composition in the terrestrial planet-forming region. Individual chondrules from ordinary chondrites formed within 1 Myr of proto-Sun collapse7 record the full range of inner Solar System μ48Ca compositions, indicating a rapid change in the composition of the disk material. We infer that this secular evolution reflects admixing of pristine outer Solar System material to the thermally-processed inner protoplanetary disk associated with the accretion of mass to the proto-Sun. The indistinguishable μ48Ca composition of the Earth (0.2±3.9 ppm) and Moon (3.7±1.9 ppm) reported here is a prediction of our model if the Moon-forming impact involved protoplanets or precursors that completed their accretion near the end of the disk lifetime.
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Bermingham K, Worsham E, Walker R. New insights into Mo and Ru isotope variation in the nebula and terrestrial planet accretionary genetics. EARTH AND PLANETARY SCIENCE LETTERS 2018; 487:221-229. [PMID: 30880823 PMCID: PMC6417891 DOI: 10.1016/j.epsl.2018.01.017] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/13/2023]
Abstract
When corrected for the effects of cosmic ray exposure, Mo and Ru nucleosynthetic isotope anomalies in iron meteorites from at least nine different parent bodies are strongly correlated in a manner consistent with variable depletion in s-process nucleosynthetic components. In contrast to prior studies, the new results show no significant deviations from a single correlation trend. In the refined Mo-Ru cosmic correlation, a distinction between the non-carbonaceous (NC) group and carbonaceous chondrite (CC) group is evident. Members of the NC group are characterized by isotope compositions reflective of variable s-process depletion. Members of the CC group analyzed here plot in a tight cluster and have the most s-process depleted Mo and Ru isotopic compositions, with Mo isotopes also slightly enriched in r- and possibly p-process contributions. This indicates that the nebular feeding zone of the NC group parent bodies was characterized by Mo and Ru with variable s-process contributions, but with the two elements always mixed in the same proportions. The CC parent bodies sampled here, by contrast, were derived from a nebular feeding zone that had been mixed to a uniform s-process depleted Mo-Ru isotopic composition. Six molybdenite samples, four glacial diamictites, and two ocean island basalts were analyzed to provide a preliminary constraint on the average Mo isotope composition of the bulk silicate Earth (BSE). Combined results yield an average μ 97Mo value of +3 ± 6. This value, coupled with a previously reported μ 100Ru value of +1 ± 7 for the BSE, indicates that the isotopic composition of the BSE falls precisely on the refined Mo-Ru cosmic correlation. The overlap of the BSE with the correlation implies that there was homogeneous accretion of siderophile elements for the final accretion of 10 to 20 wt% of Earth's mass. The only known cosmochemical materials with an isotopic match to the BSE, with regard to Mo and Ru, are some members of the IAB iron meteorite complex and enstatite chondrites.
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Affiliation(s)
- K.R. Bermingham
- Department of Geology, University of Maryland, College Park, MD 20742, USA
| | | | - R.J. Walker
- Department of Geology, University of Maryland, College Park, MD 20742, USA
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Extremely 54Cr- and 50Ti-rich presolar oxide grains in a primitive meteorite: Formation in rare types of supernovae and implications for the astrophysical context of solar system birth. ACTA ACUST UNITED AC 2018; 856. [PMID: 31049193 DOI: 10.3847/2041-8213/aab61f] [Citation(s) in RCA: 37] [Impact Index Per Article: 6.2] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
Abstract
We report the identification of 19 presolar oxide grains from the Orgueil CI meteorite with substantial enrichments in 54Cr, with 54Cr/52Cr ratios ranging from 1.2 to 56 times the solar value. The most enriched grains also exhibit enrichments at mass 50, most likely due in part to 50Ti, but close-to-normal or depleted 53Cr/52Cr ratios. There is a strong inverse relationship between 54Cr enrichment and grain size; the most extreme grains are all <80 nm in diameter. Comparison of the isotopic data with predictions of nucleosynthesis calculations indicate that these grains most likely originated in either rare, high-density Type Ia supernovae (SNIa), or in electron-capture supernovae (ECSN) which may occur as the end stage of evolution for stars of mass 8-10 M ⊙. This is the first evidence for preserved presolar grains from either type of supernova. An ECSN origin is attractive since these likely occur much more frequently than high-density SNIa, and their evolutionary timescales (~20 Myr) are comparable to those of molecular clouds. Self-pollution of the Sun's parent cloud from an ECSN may explain the heterogeneous distribution of n-rich isotopic anomalies in planetary materials, including a recently reported dichotomy in Mo isotopes in the solar system. The stellar origins of three grains with solar 54Cr/52Cr, but anomalies in 50Cr or 53Cr, as well as of a grain enriched in 57Fe, are unclear.
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Scott ERD, Krot AN, Sanders IS. Isotopic Dichotomy among Meteorites and Its Bearing on the Protoplanetary Disk. THE ASTROPHYSICAL JOURNAL 2018; 854:164. [PMID: 30842684 PMCID: PMC6398615 DOI: 10.3847/1538-4357/aaa5a5] [Citation(s) in RCA: 11] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
Abstract
Whole rock Δ17O and nucleosynthetic isotopic variations for chromium, titanium, nickel, and molybdenum in meteorites define two isotopically distinct populations: carbonaceous chondrites (CCs) and some achondrites, pallasites, and irons in one and all other chondrites and differentiated meteorites in the other. Since differentiated bodies accreted 1-3 Myr before the chondrites, the isotopic dichotomy cannot be attributed to temporal variations in the disk. Instead, the two populations were most likely separated in space, plausibly by proto-Jupiter. Formation of CCs outside Jupiter could account for their characteristic chemical and isotopic composition. The abundance of refractory inclusions in CCs can be explained if they were ejected by disk winds from near the Sun to the disk periphery where they spiraled inward due to gas drag. Once proto-Jupiter reached 10-20 M ⊕, its external pressure bump could have prevented millimeter- and centimeter-sized particles from reaching the inner disk. This scenario would account for the enrichment in CCs of refractory inclusions, refractory elements, and water. Chondrules in CCs show wide ranges in Δ17O as they formed in the presence of abundant 16O-rich refractory grains and 16O-poor ice particles. Chondrules in other chondrites (ordinary, E, R, and K groups) show relatively uniform, near-zero Δ17O values as refractory inclusions and ice were much less abundant in the inner solar system. The two populations were plausibly mixed together by the Grand Tack when Jupiter and Saturn migrated inward emptying and then repopulating the asteroid belt with roughly equal masses of planetesimals from inside and outside Jupiter's orbit (S- and C-type asteroids).
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Affiliation(s)
- Edward R D Scott
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i, Honolulu, HI 96822, USA
| | - Alexander N Krot
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i, Honolulu, HI 96822, USA
| | - Ian S Sanders
- Department of Geology, Trinity College, Dublin 2, Ireland
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O'D Alexander CM, McKeegan KD, Altwegg K. Water Reservoirs in Small Planetary Bodies: Meteorites, Asteroids, and Comets. SPACE SCIENCE REVIEWS 2018; 214:36. [PMID: 30842688 PMCID: PMC6398961 DOI: 10.1007/s11214-018-0474-9] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/10/2018] [Accepted: 01/11/2018] [Indexed: 06/09/2023]
Abstract
Asteroids and comets are the remnants of the swarm of planetesimals from which the planets ultimately formed, and they retain records of processes that operated prior to and during planet formation. They are also likely the sources of most of the water and other volatiles accreted by Earth. In this review, we discuss the nature and probable origins of asteroids and comets based on data from remote observations, in situ measurements by spacecraft, and laboratory analyses of meteorites derived from asteroids. The asteroidal parent bodies of meteorites formed ≤4 Ma after Solar System formation while there was still a gas disk present. It seems increasingly likely that the parent bodies of meteorites spectroscopically linked with the E-, S-, M- and V-type asteroids formed sunward of Jupiter's orbit, while those associated with C- and, possibly, D-type asteroids formed further out, beyond Jupiter but probably not beyond Saturn's orbit. Comets formed further from the Sun than any of the meteorite parent bodies, and retain much higher abundances of interstellar material. CI and CM group meteorites are probably related to the most common C-type asteroids, and based on isotopic evidence they, rather than comets, are the most likely sources of the H and N accreted by the terrestrial planets. However, comets may have been major sources of the noble gases accreted by Earth and Venus. Possible constraints that these observations can place on models of giant planet formation and migration are explored.
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Affiliation(s)
- Conel M O'D Alexander
- Dept. Terrestrial Magnetism, Carnegie Institution for Science, 5241 Broad Branch Road NW, Washington, DC 20015, USA. . Tel. (202) 478 8478
| | - Kevin D McKeegan
- Department of Earth, Planetary, and Space Sciences, University of California-Los Angeles, Los Angeles, CA 90095-1567, USA.
| | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland.
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Hunt AC, Ek M, Schönbächler M. Separation of Platinum from Palladium and Iridium in Iron Meteorites and Accurate High-Precision Determination of Platinum Isotopes by Multi-Collector ICP-MS. GEOSTANDARDS AND GEOANALYTICAL RESEARCH 2017; 41:633-647. [PMID: 29399018 PMCID: PMC5784402 DOI: 10.1111/ggr.12176] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 01/13/2017] [Accepted: 05/09/2017] [Indexed: 06/07/2023]
Abstract
This study presents a new measurement procedure for the isolation of Pt from iron meteorite samples. The method also allows for the separation of Pd from the same sample aliquot. The separation entails a two-stage anion-exchange procedure. In the first stage, Pt and Pd are separated from each other and from major matrix constituents including Fe and Ni. In the second stage, Ir is reduced with ascorbic acid and eluted from the column before Pt collection. Platinum yields for the total procedure were typically 50-70%. After purification, high-precision Pt isotope determinations were performed by multi-collector ICP-MS. The precision of the new method was assessed using the IIAB iron meteorite North Chile. Replicate analyses of multiple digestions of this material yielded an intermediate precision for the measurement results of 0.73 for ε192Pt, 0.15 for ε194Pt and 0.09 for ε196Pt (2 standard deviations). The NIST SRM 3140 Pt solution reference material was passed through the measurement procedure and yielded an isotopic composition that is identical to the unprocessed Pt reference material. This indicates that the new technique is unbiased within the limit of the estimated uncertainties. Data for three iron meteorites support that Pt isotope variations in these samples are due to exposure to galactic cosmic rays in space.
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Affiliation(s)
- Alison C. Hunt
- Institute of Geochemistry and PetrologyETH ZürichClausiusstrasse 25Zürich8092Switzerland
| | - Mattias Ek
- Institute of Geochemistry and PetrologyETH ZürichClausiusstrasse 25Zürich8092Switzerland
| | - Maria Schönbächler
- Institute of Geochemistry and PetrologyETH ZürichClausiusstrasse 25Zürich8092Switzerland
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