1
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Bose M, Root RA, Guan Y, Eaton J, Wittmann A, Skrmetti T, Desch SJ. Evidence of both molecular cloud and fluid chemistry in Ryugu regolith. SCIENCE ADVANCES 2024; 10:eadp3037. [PMID: 39047107 PMCID: PMC11268420 DOI: 10.1126/sciadv.adp3037] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/18/2024] [Accepted: 06/21/2024] [Indexed: 07/27/2024]
Abstract
The sulfur chemistry of (162173) Ryugu particles can be a powerful tracer of molecular cloud chemistry and small body processes, but it has not been well explored. We report identification of organosulfurs and a sulfate grain in two Ryugu particles, A0070 and A0093. The sulfate grain shows oxygen isotope ratios (δ17O = -11.0 ± 4.3 per mil, δ18O = -7.8 ± 2.3 per mil) that are akin to silicates in Ryugu but exhibit mass-independent sulfur isotopic fractionation (Δ33S = +5 ± 2 per mil). A methionine-like coating on the sulfate grain is isotopically anomalous (δ15N = +62 ± 2 per mil). Both the sulfate and organosulfurs can simultaneously form and survive during aqueous alteration within Ryugu's parent body, under reduced conditions, low temperature, and a pH >7 in the presence of N-rich organic molecules. This work extends the heliocentric zone where anomalous sulfur, formed by selective photodissociation of H2S gas in the molecular cloud, is found.
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Affiliation(s)
- Maitrayee Bose
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
| | - Robert A. Root
- Department of Environmental Science, University of Arizona, Tucson, AZ 85721, USA
| | - Yunbin Guan
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
| | - Jacob Eaton
- Department of Mathematical Sciences, Arizona State University, Tempe, AZ 85287, USA
| | - Axel Wittmann
- Eyring Materials Center, Arizona State University, Tempe, AZ 85287, USA
| | - Thomas Skrmetti
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
| | - Steven J. Desch
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
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2
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Zhang B, Chabot NL, Rubin AE. Compositions of iron-meteorite parent bodies constrain the structure of the protoplanetary disk. Proc Natl Acad Sci U S A 2024; 121:e2306995121. [PMID: 38805273 PMCID: PMC11161762 DOI: 10.1073/pnas.2306995121] [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: 04/28/2023] [Accepted: 04/08/2024] [Indexed: 05/30/2024] Open
Abstract
Magmatic iron-meteorite parent bodies are the earliest planetesimals in the Solar System, and they preserve information about conditions and planet-forming processes in the solar nebula. In this study, we include comprehensive elemental compositions and fractional-crystallization modeling for iron meteorites from the cores of five differentiated asteroids from the inner Solar System. Together with previous results of metallic cores from the outer Solar System, we conclude that asteroidal cores from the outer Solar System have smaller sizes, elevated siderophile-element abundances, and simpler crystallization processes than those from the inner Solar System. These differences are related to the formation locations of the parent asteroids because the solar protoplanetary disk varied in redox conditions, elemental distributions, and dynamics at different heliocentric distances. Using highly siderophile-element data from iron meteorites, we reconstruct the distribution of calcium-aluminum-rich inclusions (CAIs) across the protoplanetary disk within the first million years of Solar-System history. CAIs, the first solids to condense in the Solar System, formed close to the Sun. They were, however, concentrated within the outer disk and depleted within the inner disk. Future models of the structure and evolution of the protoplanetary disk should account for this distribution pattern of CAIs.
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Affiliation(s)
- Bidong Zhang
- Department of Earth, Planetary and Space Sciences, University of California, Los Angeles, CA90095-1567
| | - Nancy L. Chabot
- Space Exploration Sector, Johns Hopkins University Applied Physics Laboratory, Laurel, MD20723
| | - Alan E. Rubin
- Department of Earth, Planetary and Space Sciences, University of California, Los Angeles, CA90095-1567
- Maine Mineral and Gem Museum, Bethel, ME04217
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3
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Maurel C, Gattacceca J. A 4,565-My-old record of the solar nebula field. Proc Natl Acad Sci U S A 2024; 121:e2312802121. [PMID: 38437531 PMCID: PMC10962989 DOI: 10.1073/pnas.2312802121] [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: 07/26/2023] [Accepted: 12/21/2023] [Indexed: 03/06/2024] Open
Abstract
Magnetic fields in protoplanetary disks are thought to play a prominent role in the formation of planetary bodies. Acting upon turbulence and angular momentum transport, they may influence the motion of solids and accretion onto the central star. By searching for the record of the solar nebula field preserved in meteorites, we aim to characterize the strength of a disk field with a spatial and temporal resolution far superior to observations of extrasolar disks. Here, we present a rock magnetic and paleomagnetic study of the andesite meteorite Erg Chech 002 (EC002). This meteorite contains submicron iron grains, expected to be very reliable magnetic recorders, and carries a stable, high-coercivity magnetization. After ruling out potential sources of magnetic contamination, we show that EC002 most likely carries an ancient thermoremanent magnetization acquired upon cooling on its parent body. Using the U-corrected Pb-Pb age of the meteorite's pyroxene as a proxy for the timing of magnetization acquisition, we estimate that EC002 recorded a field of 60 ± 18 µT at a distance of ~2 to 3 astronomical units, 2.0 ± 0.3 My after the formation of calcium-aluminum-rich inclusions. This record can only be explained if EC002 was magnetized by the field prevalent in the solar nebula. This makes EC002's record, particularly well resolved in time and space, one of the two earliest records of the solar nebula field. Such a field intensity is consistent with stellar accretion rates observed in extrasolar protoplanetary disks.
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Affiliation(s)
- Clara Maurel
- CNRS, Aix Marseille Université, IRD, INRAE, Centre de Recherche et d’Enseignement des Géosciences de l’Environnement (CEREGE), Aix-en-Provence13545, France
| | - Jérôme Gattacceca
- CNRS, Aix Marseille Université, IRD, INRAE, Centre de Recherche et d’Enseignement des Géosciences de l’Environnement (CEREGE), Aix-en-Provence13545, France
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4
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Vance SD, Craft KL, Shock E, Schmidt BE, Lunine J, Hand KP, McKinnon WB, Spiers EM, Chivers C, Lawrence JD, Wolfenbarger N, Leonard EJ, Robinson KJ, Styczinski MJ, Persaud DM, Steinbrügge G, Zolotov MY, Quick LC, Scully JEC, Becker TM, Howell SM, Clark RN, Dombard AJ, Glein CR, Mousis O, Sephton MA, Castillo-Rogez J, Nimmo F, McEwen AS, Gudipati MS, Jun I, Jia X, Postberg F, Soderlund KM, Elder CM. Investigating Europa's Habitability with the Europa Clipper. SPACE SCIENCE REVIEWS 2023; 219:81. [PMID: 38046182 PMCID: PMC10687213 DOI: 10.1007/s11214-023-01025-2] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/22/2022] [Accepted: 11/03/2023] [Indexed: 12/05/2023]
Abstract
The habitability of Europa is a property within a system, which is driven by a multitude of physical and chemical processes and is defined by many interdependent parameters, so that its full characterization requires collaborative investigation. To explore Europa as an integrated system to yield a complete picture of its habitability, the Europa Clipper mission has three primary science objectives: (1) characterize the ice shell and ocean including their heterogeneity, properties, and the nature of surface-ice-ocean exchange; (2) characterize Europa's composition including any non-ice materials on the surface and in the atmosphere, and any carbon-containing compounds; and (3) characterize Europa's geology including surface features and localities of high science interest. The mission will also address several cross-cutting science topics including the search for any current or recent activity in the form of thermal anomalies and plumes, performing geodetic and radiation measurements, and assessing high-resolution, co-located observations at select sites to provide reconnaissance for a potential future landed mission. Synthesizing the mission's science measurements, as well as incorporating remote observations by Earth-based observatories, the James Webb Space Telescope, and other space-based resources, to constrain Europa's habitability, is a complex task and is guided by the mission's Habitability Assessment Board (HAB).
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Affiliation(s)
- Steven D. Vance
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - Kathleen L. Craft
- Applied Physics Laboratory, Johns Hopkins University, Laurel, MD USA
| | - Everett Shock
- School of Earth & Space Exploration and School of Molecular Sciences, Arizona State University, Tempe, AZ USA
| | - Britney E. Schmidt
- Department of Astronomy and Department of Earth & Atmospheric Sciences, Cornell University, Ithaca, NY USA
| | - Jonathan Lunine
- Department of Astronomy and Department of Earth & Atmospheric Sciences, Cornell University, Ithaca, NY USA
| | - Kevin P. Hand
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - William B. McKinnon
- Department of Earth and Planetary Sciences and McDonnell Center for the Space Sciences, Washington University in St. Louis, Saint Louis, MO USA
| | - Elizabeth M. Spiers
- School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, GA USA
| | - Chase Chivers
- School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, GA USA
- Applied Ocean Physics and Engineering, Woods Hole Oceanographic Institution, Woods Hole, MA USA
| | - Justin D. Lawrence
- School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, GA USA
- Honeybee Robotics, Altadena, CA USA
| | - Natalie Wolfenbarger
- Institute for Geophysics, John A. and Katherine G. Jackson School of Geosciences, University of Texas at Austin, Austin, TX USA
| | - Erin J. Leonard
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | | | | | - Divya M. Persaud
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - Gregor Steinbrügge
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - Mikhail Y. Zolotov
- School of Earth & Space Exploration and School of Molecular Sciences, Arizona State University, Tempe, AZ USA
| | | | | | | | - Samuel M. Howell
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | | | - Andrew J. Dombard
- Dept. of Earth and Environmental Sciences, University of Illinois Chicago, Chicago, USA
| | | | - Olivier Mousis
- Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), Marseille, France
| | - Mark A. Sephton
- Impacts and Astromaterials Research Centre, Department of Earth Science and Engineering, Imperial College London, London, United Kingdom
| | | | - Francis Nimmo
- Department of Earth and Planetary Sciences, University of California, Santa Cruz, CA USA
| | - Alfred S. McEwen
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ USA
| | - Murthy S. Gudipati
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - Insoo Jun
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
| | - Xianzhe Jia
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI USA
| | - Frank Postberg
- Institut für Geologische Wissenschaften, Freie Universität Berlin, Berlin, Germany
| | - Krista M. Soderlund
- Institute for Geophysics, John A. and Katherine G. Jackson School of Geosciences, University of Texas at Austin, Austin, TX USA
| | - Catherine M. Elder
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
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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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Nakamura T, Matsumoto M, Amano K, Enokido Y, Zolensky ME, Mikouchi T, Genda H, Tanaka S, Zolotov MY, Kurosawa K, Wakita S, Hyodo R, Nagano H, Nakashima D, Takahashi Y, Fujioka Y, Kikuiri M, Kagawa E, Matsuoka M, Brearley AJ, Tsuchiyama A, Uesugi M, Matsuno J, Kimura Y, Sato M, Milliken RE, Tatsumi E, Sugita S, Hiroi T, Kitazato K, Brownlee D, Joswiak DJ, Takahashi M, Ninomiya K, Takahashi T, Osawa T, Terada K, Brenker FE, Tkalcec BJ, Vincze L, Brunetto R, Aléon-Toppani A, Chan QHS, Roskosz M, Viennet JC, Beck P, Alp EE, Michikami T, Nagaashi Y, Tsuji T, Ino Y, Martinez J, Han J, Dolocan A, Bodnar RJ, Tanaka M, Yoshida H, Sugiyama K, King AJ, Fukushi K, Suga H, Yamashita S, Kawai T, Inoue K, Nakato A, Noguchi T, Vilas F, Hendrix AR, Jaramillo-Correa C, Domingue DL, Dominguez G, Gainsforth Z, Engrand C, Duprat J, Russell SS, Bonato E, Ma C, Kawamoto T, Wada T, Watanabe S, Endo R, Enju S, Riu L, Rubino S, Tack P, Takeshita S, Takeichi Y, Takeuchi A, Takigawa A, Takir D, Tanigaki T, Taniguchi A, Tsukamoto K, Yagi T, Yamada S, Yamamoto K, Yamashita Y, Yasutake M, Uesugi K, Umegaki I, Chiu I, Ishizaki T, Okumura S, Palomba E, Pilorget C, Potin SM, Alasli A, Anada S, Araki Y, Sakatani N, Schultz C, Sekizawa O, Sitzman SD, Sugiura K, Sun M, Dartois E, De Pauw E, Dionnet Z, Djouadi Z, Falkenberg G, Fujita R, Fukuma T, Gearba IR, Hagiya K, Hu MY, Kato T, Kawamura T, Kimura M, Kubo MK, Langenhorst F, Lantz C, Lavina B, Lindner M, Zhao J, Vekemans B, Baklouti D, Bazi B, Borondics F, Nagasawa S, Nishiyama G, Nitta K, Mathurin J, Matsumoto T, Mitsukawa I, Miura H, Miyake A, Miyake Y, Yurimoto H, Okazaki R, Yabuta H, Naraoka H, Sakamoto K, Tachibana S, Connolly HC, Lauretta DS, Yoshitake M, Yoshikawa M, Yoshikawa K, Yoshihara K, Yokota Y, Yogata K, Yano H, Yamamoto Y, Yamamoto D, Yamada M, Yamada T, Yada T, Wada K, Usui T, Tsukizaki R, Terui F, Takeuchi H, Takei Y, Iwamae A, Soejima H, Shirai K, Shimaki Y, Senshu H, Sawada H, Saiki T, Ozaki M, Ono G, Okada T, Ogawa N, Ogawa K, Noguchi R, Noda H, Nishimura M, Namiki N, Nakazawa S, Morota T, Miyazaki A, Miura A, Mimasu Y, Matsumoto K, Kumagai K, Kouyama T, Kikuchi S, Kawahara K, Kameda S, Iwata T, Ishihara Y, Ishiguro M, Ikeda H, Hosoda S, Honda R, Honda C, Hitomi Y, Hirata N, Hirata N, Hayashi T, Hayakawa M, Hatakeda K, Furuya S, Fukai R, Fujii A, Cho Y, Arakawa M, Abe M, Watanabe S, Tsuda Y. Formation and evolution of carbonaceous asteroid Ryugu: Direct evidence from returned samples. Science 2023; 379:eabn8671. [PMID: 36137011 DOI: 10.1126/science.abn8671] [Citation(s) in RCA: 20] [Impact Index Per Article: 20.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Samples of the carbonaceous asteroid Ryugu were brought to Earth by the Hayabusa2 spacecraft. We analyzed 17 Ryugu samples measuring 1 to 8 millimeters. Carbon dioxide-bearing water inclusions are present within a pyrrhotite crystal, indicating that Ryugu's parent asteroid formed in the outer Solar System. The samples contain low abundances of materials that formed at high temperatures, such as chondrules and calcium- and aluminum-rich inclusions. The samples are rich in phyllosilicates and carbonates, which formed through aqueous alteration reactions at low temperature, high pH, and water/rock ratios of <1 (by mass). Less altered fragments contain olivine, pyroxene, amorphous silicates, calcite, and phosphide. Numerical simulations, based on the mineralogical and physical properties of the samples, indicate that Ryugu's parent body formed ~2 million years after the beginning of Solar System formation.
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Affiliation(s)
- T Nakamura
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - M Matsumoto
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - K Amano
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - Y Enokido
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - M E Zolensky
- NASA Johnson Space Center; Houston, TX 77058, USA
| | - T Mikouchi
- The University Museum, The University of Tokyo, Tokyo 113-0033, Japan
| | - H Genda
- Earth-Life Science Institute, Tokyo Institute of Technology, Tokyo 152-8550, Japan
| | - S Tanaka
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - M Y Zolotov
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
| | - K Kurosawa
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - S Wakita
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - R Hyodo
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - H Nagano
- Department of Mechanical Systems Engineering, Nagoya University, Nagoya 464-8603, Japan
| | - D Nakashima
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - Y Takahashi
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan.,Isotope Science Center, The University of Tokyo, Tokyo 113-0032, Japan
| | - Y Fujioka
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - M Kikuiri
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - E Kagawa
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - M Matsuoka
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris, Meudon 92195 France.,Geological Survey of Japan, National Institute of Advanced Industrial Science and Technology (AIST), Tsukuba, 305-8567, Japan
| | - A J Brearley
- Department of Earth and Planetary Sciences, University of New Mexico, Albuquerque, NM 87131, USA
| | - A Tsuchiyama
- Research Organization of Science and Technology, Ritsumeikan University, Kusatsu 525-8577, Japan.,Key Laboratory of Mineralogy and Metallogeny, Guangdong Provincial Key Laboratory of Mineral Physics and Materials, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences (CAS), Guangzhou 510640, China.,Center for Excellence in Deep Earth Science, CAS, Guangzhou 510640, China
| | - M Uesugi
- Scattering and Imaging Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - J Matsuno
- Research Organization of Science and Technology, Ritsumeikan University, Kusatsu 525-8577, Japan
| | - Y Kimura
- Institute of Low Temperature Science, Hokkaido University, Sapporo 060-0819, Japan
| | - M Sato
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - R E Milliken
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - E Tatsumi
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan.,Instituto de Astrofísica de Canarias, University of La Laguna, Tenerife 38205, Spain
| | - S Sugita
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan.,Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - T Hiroi
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - K Kitazato
- Aizu Research Center for Space Informatics, The University of Aizu, Aizu-Wakamatsu 965-8580, Japan
| | - D Brownlee
- Department of Astronomy, University of Washington, Seattle, WA 98195 USA
| | - D J Joswiak
- Department of Astronomy, University of Washington, Seattle, WA 98195 USA
| | - M Takahashi
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - K Ninomiya
- Institute for Radiation Sciences, Osaka University, Toyonaka 560-0043, Japan
| | - T Takahashi
- Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Kashiwa 277-8583, Japan.,Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan
| | - T Osawa
- Materials Sciences Research Center, Japan Atomic Energy Agency, Tokai 319-1195, Japan
| | - K Terada
- Department of Earth and Space Science, Osaka University, Toyonaka 560-0043, Japan
| | - F E Brenker
- Institute of Geoscience, Goethe University, Frankfurt, 60438 Frankfurt am Main, Germany
| | - B J Tkalcec
- Institute of Geoscience, Goethe University, Frankfurt, 60438 Frankfurt am Main, Germany
| | - L Vincze
- Department of Chemistry, Ghent University, Krijgslaan 281 S12, Ghent, Belgium
| | - R Brunetto
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - A Aléon-Toppani
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - Q H S Chan
- Department of Earth Sciences, Royal Holloway, University of London, Egham TW20 0EX, UK
| | - M Roskosz
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, Muséum National d'Histoire Naturelle, Centre national de la recherche scientifique (CNRS), Sorbonne Université, Paris, France
| | - J-C Viennet
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, Muséum National d'Histoire Naturelle, Centre national de la recherche scientifique (CNRS), Sorbonne Université, Paris, France
| | - P Beck
- Institut de Planétologie et d'Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, 38000 Grenoble, France
| | - E E Alp
- Advanced Photon Source, Argonne National Laboratory, Argonne, IL 60439, USA
| | - T Michikami
- Faculty of Engineering, Kindai University, Higashi-Hiroshima 739-2116, Japan
| | - Y Nagaashi
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan.,Department of Planetology, Kobe University, Kobe 657-8501, Japan
| | - T Tsuji
- Department of Earth Resources Engineering, Kyushu University, Fukuoka 819-0395, Japan.,School of Engineering, The University of Tokyo, Tokyo 113-0033, Japan
| | - Y Ino
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Physics, Kwansei Gakuin University, Sanda 669-1330, Japan
| | - J Martinez
- NASA Johnson Space Center; Houston, TX 77058, USA
| | - J Han
- Department of Earth and Atmospheric Sciences, University of Houston, Houston, TX 77204, USA
| | - A Dolocan
- Texas Materials Institute, The University of Texas at Austin, Austin, TX 78712, USA
| | - R J Bodnar
- Department of Geoscience, Virginia Tech, Blacksburg, VA 24061, USA
| | - M Tanaka
- Materials Analysis Station, National Institute for Materials Science, Tsukuba 305-0047, Japan
| | - H Yoshida
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - K Sugiyama
- Institute for Materials Research, Tohoku University, Sendai 980-8577, Japan
| | - A J King
- Department of Earth Science, Natural History Museum, London SW7 5BD, UK
| | - K Fukushi
- Institute of Nature and Environmental Technology, Kanazawa University, Kanazawa 920-1192, Japan
| | - H Suga
- Spectroscopy Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - S Yamashita
- Department of Materials Structure Science, The Graduate University for Advanced Studies (SOKENDAI), Tsukuba, Ibaraki 305-0801, Japan.,Institute of Materials Structure Science, High-Energy Accelerator Research Organization, Tsukuba 305-0801, Japan
| | - T Kawai
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - K Inoue
- Institute of Nature and Environmental Technology, Kanazawa University, Kanazawa 920-1192, Japan
| | - A Nakato
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - T Noguchi
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan.,Faculty of Arts and Science, Kyushu University, Fukuoka 819-0395, Japan
| | - F Vilas
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - A R Hendrix
- Planetary Science Institute, Tucson, AZ 85719, USA
| | | | - D L Domingue
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - G Dominguez
- Department of Physics, California State University, San Marcos, CA 92096, USA
| | - Z Gainsforth
- Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
| | - C Engrand
- Laboratoire de Physique des 2 Infinis Irène Joliot-Curie, Université Paris-Saclay, CNRS, 91405 Orsay, France
| | - J Duprat
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, Muséum National d'Histoire Naturelle, Centre national de la recherche scientifique (CNRS), Sorbonne Université, Paris, France
| | - S S Russell
- Department of Earth Science, Natural History Museum, London SW7 5BD, UK
| | - E Bonato
- Institute for Planetary Research, Deutsches Zentrum für Luftund Raumfahrt, Rutherfordstraße 2 12489 Berlin, Germany
| | - C Ma
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena CA 91125, USA
| | - T Kawamoto
- Department of Geosciences, Shizuoka University, Shizuoka 422-8529, Japan
| | - T Wada
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - S Watanabe
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Kashiwa 277-8583, Japan
| | - R Endo
- Department of Materials Science and Engineering, Tokyo Institute of Technology, Tokyo 152-8550, Japan
| | - S Enju
- Graduate School of Science and Engineering, Ehime University, Matsuyama 790-8577, Japan
| | - L Riu
- European Space Astronomy Centre, 28692 Villanueva de la Cañada, Spain
| | - S Rubino
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - P Tack
- Department of Chemistry, Ghent University, Krijgslaan 281 S12, Ghent, Belgium
| | - S Takeshita
- High Energy Accelerator Research Organization, Tokai 319-1106, Japan
| | - Y Takeichi
- Department of Materials Structure Science, The Graduate University for Advanced Studies (SOKENDAI), Tsukuba, Ibaraki 305-0801, Japan.,Institute of Materials Structure Science, High-Energy Accelerator Research Organization, Tsukuba 305-0801, Japan.,Department of Applied Physics, Osaka University, Suita 565-0871, Japan
| | - A Takeuchi
- Scattering and Imaging Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - A Takigawa
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - D Takir
- NASA Johnson Space Center; Houston, TX 77058, USA
| | | | - A Taniguchi
- Institute for Integrated Radiation and Nuclear Science, Kyoto University, Kumatori 590-0494, Japan
| | - K Tsukamoto
- Department of Earth Sciences, Tohoku University, Sendai 980-8578, Japan
| | - T Yagi
- National Metrology Institute of Japan, AIST, Tsukuba 305-8565, Japan
| | - S Yamada
- Department of Physics, Rikkyo University, Tokyo 171-8501, Japan
| | - K Yamamoto
- Japan Fine Ceramics Center, Nagoya 456-8587, Japan
| | - Y Yamashita
- National Metrology Institute of Japan, AIST, Tsukuba 305-8565, Japan
| | - M Yasutake
- Scattering and Imaging Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - K Uesugi
- Scattering and Imaging Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - I Umegaki
- High Energy Accelerator Research Organization, Tokai 319-1106, Japan.,Toyota Central Research and Development Laboratories, Nagakute 480-1192, Japan
| | - I Chiu
- Institute for Radiation Sciences, Osaka University, Toyonaka 560-0043, Japan
| | - T Ishizaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - S Okumura
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - E Palomba
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome 00133, Italy
| | - C Pilorget
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France.,Institut Universitaire de France, Paris, France
| | - S M Potin
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris, Meudon 92195 France.,Faculty of Aerospace Engineering, Delft University of Technology, Delft, Netherlands
| | - A Alasli
- Department of Mechanical Systems Engineering, Nagoya University, Nagoya 464-8603, Japan
| | - S Anada
- Japan Fine Ceramics Center, Nagoya 456-8587, Japan
| | - Y Araki
- Department of Physical Sciences, Ritsumeikan University, Shiga 525-0058, Japan
| | - N Sakatani
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Physics, Rikkyo University, Tokyo 171-8501, Japan
| | - C Schultz
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - O Sekizawa
- Spectroscopy Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - S D Sitzman
- Physical Sciences Laboratory, The Aerospace Corporation, CA 90245, USA
| | - K Sugiura
- Earth-Life Science Institute, Tokyo Institute of Technology, Tokyo 152-8550, Japan
| | - M Sun
- Key Laboratory of Mineralogy and Metallogeny, Guangdong Provincial Key Laboratory of Mineral Physics and Materials, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences (CAS), Guangzhou 510640, China.,Center for Excellence in Deep Earth Science, CAS, Guangzhou 510640, China.,University of Chinese Academy of Sciences, Beijing 100049, China
| | - E Dartois
- Institut des Sciences Moléculaires d'Orsay, Université Paris-Saclay, CNRS, 91405 Orsay, France
| | - E De Pauw
- Department of Chemistry, Ghent University, Krijgslaan 281 S12, Ghent, Belgium
| | - Z Dionnet
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - Z Djouadi
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - G Falkenberg
- Deutsches Elektronen-Synchrotron Photon Science, 22603 Hamburg, Germany
| | - R Fujita
- Department of Mechanical Systems Engineering, Nagoya University, Nagoya 464-8603, Japan
| | - T Fukuma
- Nano Life Science Institute, Kanazawa University, Kanazawa 920-1192, Japan
| | - I R Gearba
- Texas Materials Institute, The University of Texas at Austin, Austin, TX 78712, USA
| | - K Hagiya
- Graduate School of Life Science, University of Hyogo, Hyogo 678-1297, Japan
| | - M Y Hu
- Advanced Photon Source, Argonne National Laboratory, Argonne, IL 60439, USA
| | - T Kato
- Japan Fine Ceramics Center, Nagoya 456-8587, Japan
| | - T Kawamura
- Institut de Physique du Globe de Paris, Université de Paris, Paris 75205, France
| | - M Kimura
- Department of Materials Structure Science, The Graduate University for Advanced Studies (SOKENDAI), Tsukuba, Ibaraki 305-0801, Japan.,Institute of Materials Structure Science, High-Energy Accelerator Research Organization, Tsukuba 305-0801, Japan
| | - M K Kubo
- Division of Natural Sciences, International Christian University, Mitaka 181-8585, Japan
| | - F Langenhorst
- Institute of Geosciences, Friedrich-Schiller-Universität Jena, 07745 Jena, Germany
| | - C Lantz
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - B Lavina
- Center for Advanced Radiation Sources, University of Chicago, Chicago, IL 60637, USA
| | - M Lindner
- Institute of Geoscience, Goethe University, Frankfurt, 60438 Frankfurt am Main, Germany
| | - J Zhao
- Advanced Photon Source, Argonne National Laboratory, Argonne, IL 60439, USA
| | - B Vekemans
- Department of Chemistry, Ghent University, Krijgslaan 281 S12, Ghent, Belgium
| | - D Baklouti
- Institut d'Astrophysique Spatiale, Université Paris-Saclay, Orsay 91405, France
| | - B Bazi
- Department of Chemistry, Ghent University, Krijgslaan 281 S12, Ghent, Belgium
| | - F Borondics
- Optimized Light Source of Intermediate Energy to LURE (SOLEIL) L'Orme des Merisiers, Gif sur Yvette F-91192, France
| | - S Nagasawa
- Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Kashiwa 277-8583, Japan.,Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan
| | - G Nishiyama
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - K Nitta
- Spectroscopy Division, Japan Synchrotron Radiation Research Institute, Sayo 679-5198, Japan
| | - J Mathurin
- Institut Chimie Physique, Université Paris-Saclay, CNRS, 91405 Orsay, France
| | - T Matsumoto
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - I Mitsukawa
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - H Miura
- Graduate School of Science, Nagoya City University, Nagoya 467-8501, Japan
| | - A Miyake
- Division of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Y Miyake
- High Energy Accelerator Research Organization, Tokai 319-1106, Japan
| | - H Yurimoto
- Department of Natural History Sciences, Hokkaido University, Sapporo 060-0810, Japan
| | - R Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - H Yabuta
- Graduate School of Advanced Science and Engineering, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - H Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - K Sakamoto
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - S Tachibana
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - H C Connolly
- Department of Geology, Rowan University, Glassboro, NJ 08028, USA
| | - D S Lauretta
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - M Yoshitake
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - M Yoshikawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - K Yoshikawa
- Research and Development Directorate, JAXA, Sagamihara 252-5210, Japan
| | - K Yoshihara
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Y Yokota
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - K Yogata
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - H Yano
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - Y Yamamoto
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - D Yamamoto
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - M Yamada
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - T Yamada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - T Yada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - K Wada
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - T Usui
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - R Tsukizaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - F Terui
- Department of Mechanical Engineering, Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | - H Takeuchi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - Y Takei
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - A Iwamae
- Marine Works Japan, Yokosuka 237-0063, Japan
| | - H Soejima
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Marine Works Japan, Yokosuka 237-0063, Japan
| | - K Shirai
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Y Shimaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - H Senshu
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan
| | - H Sawada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - T Saiki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - M Ozaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - G Ono
- Research and Development Directorate, JAXA, Sagamihara 252-5210, Japan
| | - T Okada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Chemistry, The University of Tokyo, Tokyo 113-0033, Japan
| | - N Ogawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - K Ogawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - R Noguchi
- Faculty of Science, Niigata University, Niigata 950-2181, Japan
| | - H Noda
- National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - M Nishimura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - N Namiki
- Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan.,National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - S Nakazawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - T Morota
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - A Miyazaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - A Miura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Y Mimasu
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - K Matsumoto
- Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan.,National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - K Kumagai
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Marine Works Japan, Yokosuka 237-0063, Japan
| | - T Kouyama
- Digital Architecture Research Center, National Institute of Advanced Industrial Science and Technology, Tokyo 135-0064, Japan
| | - S Kikuchi
- Planetary Exploration Research Center, Chiba Institute of Technology, Narashino 275-0016, Japan.,National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
| | - K Kawahara
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - S Kameda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Physics, Rikkyo University, Tokyo 171-8501, Japan
| | - T Iwata
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - Y Ishihara
- JAXA Space Exploration Center, JAXA, Sagamihara 252-5210, Japan
| | - M Ishiguro
- Department of Physics and Astronomy, Seoul National University, Seoul 08826, Korea
| | - H Ikeda
- Research and Development Directorate, JAXA, Sagamihara 252-5210, Japan
| | - S Hosoda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - R Honda
- Department of Information Science, Kochi University, Kochi 780-8520, Japan.,Center for Data Science, Ehime University, Matsuyama 790-8577, Japan
| | - C Honda
- Aizu Research Center for Space Informatics, The University of Aizu, Aizu-Wakamatsu 965-8580, Japan
| | - Y Hitomi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Marine Works Japan, Yokosuka 237-0063, Japan
| | - N Hirata
- Department of Planetology, Kobe University, Kobe 657-8501, Japan
| | - N Hirata
- Aizu Research Center for Space Informatics, The University of Aizu, Aizu-Wakamatsu 965-8580, Japan
| | - T Hayashi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - M Hayakawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - K Hatakeda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Marine Works Japan, Yokosuka 237-0063, Japan
| | - S Furuya
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - R Fukai
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - A Fujii
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
| | - Y Cho
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - M Arakawa
- Department of Planetology, Kobe University, Kobe 657-8501, Japan
| | - M Abe
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, The Graduate University for Advanced Studies (SOKENDAI), Hayama 240-0193, Japan
| | - S Watanabe
- Department of Earth and Environmental Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Y Tsuda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara 252-5210, Japan
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7
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Castillo‐Rogez J, Weiss B, Beddingfield C, Biersteker J, Cartwright R, Goode A, Melwani Daswani M, Neveu M. Compositions and Interior Structures of the Large Moons of Uranus and Implications for Future Spacecraft Observations. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2023; 128:e2022JE007432. [PMID: 37034459 PMCID: PMC10078161 DOI: 10.1029/2022je007432] [Citation(s) in RCA: 4] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 06/14/2022] [Revised: 11/29/2022] [Accepted: 12/02/2022] [Indexed: 06/19/2023]
Abstract
The five large moons of Uranus are important targets for future spacecraft missions. To motivate and inform the exploration of these moons, we model their internal evolution, present-day physical structures, and geochemical and geophysical signatures that may be measured by spacecraft. We predict that if the moons preserved liquid until present, it is likely in the form of residual oceans less than 30 km thick in Ariel, Umbriel, and less than 50 km in Titania, and Oberon. The preservation of liquid strongly depends on material properties and, potentially, on dynamical circumstances that are presently unknown. Miranda is unlikely to host liquid at present unless it experienced tidal heating a few tens of million years ago. We find that since the thin residual layers may be hypersaline, their induced magnetic fields could be detectable by future spacecraft-based magnetometers. However, if the ocean is maintained primarily by ammonia, and thus well below the water freezing point, then its electrical conductivity may be too small to be detectable by spacecraft. Lastly, our calculated tidal Love number (k 2) and dissipation factor (Q) are consistent with the Q/k 2 values previously inferred from dynamical evolution models. In particular, we find that the low Q/k 2 estimated for Titania supports the hypothesis that Titania currently holds an ocean.
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Affiliation(s)
| | - Benjamin Weiss
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
- Department of Earth, Atmospheric and Planetary SciencesMassachusetts Institute of Technology (MIT)CambridgeMAUSA
| | - Chloe Beddingfield
- SETI InstituteMountain ViewCAUSA
- NASA Ames Research CenterMountain ViewCAUSA
| | - John Biersteker
- Department of Earth, Atmospheric and Planetary SciencesMassachusetts Institute of Technology (MIT)CambridgeMAUSA
| | | | - Allison Goode
- Department of Earth, Atmospheric and Planetary SciencesMassachusetts Institute of Technology (MIT)CambridgeMAUSA
| | | | - Marc Neveu
- University of MarylandCollege ParkMDUSA
- NASA Goddard Space Flight CenterGreenbeltMDUSA
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8
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Kawasaki N, Nagashima K, Sakamoto N, Matsumoto T, Bajo KI, Wada S, Igami Y, Miyake A, Noguchi T, Yamamoto D, Russell SS, Abe Y, Aléon J, Alexander CM, Amari S, Amelin Y, Bizzarro M, Bouvier A, Carlson RW, Chaussidon M, Choi BG, Dauphas N, Davis AM, Di Rocco T, Fujiya W, Fukai R, Gautam I, Haba MK, Hibiya Y, Hidaka H, Homma H, Hoppe P, Huss GR, Ichida K, Iizuka T, Ireland TR, Ishikawa A, Ito M, Itoh S, Kita NT, Kitajima K, Kleine T, Komatani S, Krot AN, Liu MC, Masuda Y, McKeegan KD, Morita M, Motomura K, Moynier F, Nakai I, Nguyen A, Nittler L, Onose M, Pack A, Park C, Piani L, Qin L, Schönbächler M, Tafla L, Tang H, Terada K, Terada Y, Usui T, Wadhwa M, Walker RJ, Yamashita K, Yin QZ, Yokoyama T, Yoneda S, Young ED, Yui H, Zhang AC, Nakamura T, Naraoka H, Okazaki R, Sakamoto K, Yabuta H, Abe M, Miyazaki A, Nakato A, Nishimura M, Okada T, Yada T, Yogata K, Nakazawa S, Saiki T, Tanaka S, Terui F, Tsuda Y, Watanabe SI, Yoshikawa M, Tachibana S, Yurimoto H. Oxygen isotopes of anhydrous primary minerals show kinship between asteroid Ryugu and comet 81P/Wild2. SCIENCE ADVANCES 2022; 8:eade2067. [PMID: 36525483 PMCID: PMC9757743 DOI: 10.1126/sciadv.ade2067] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 08/01/2022] [Accepted: 11/17/2022] [Indexed: 06/17/2023]
Abstract
The extraterrestrial materials returned from asteroid (162173) Ryugu consist predominantly of low-temperature aqueously formed secondary minerals and are chemically and mineralogically similar to CI (Ivuna-type) carbonaceous chondrites. Here, we show that high-temperature anhydrous primary minerals in Ryugu and CI chondrites exhibit a bimodal distribution of oxygen isotopic compositions: 16O-rich (associated with refractory inclusions) and 16O-poor (associated with chondrules). Both the 16O-rich and 16O-poor minerals probably formed in the inner solar protoplanetary disk and were subsequently transported outward. The abundance ratios of the 16O-rich to 16O-poor minerals in Ryugu and CI chondrites are higher than in other carbonaceous chondrite groups but are similar to that of comet 81P/Wild2, suggesting that Ryugu and CI chondrites accreted in the outer Solar System closer to the accretion region of comets.
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Affiliation(s)
- Noriyuki Kawasaki
- Department of Natural History Sciences, Hokkaido University Sapporo 060-0810, Japan
| | - Kazuhide Nagashima
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Naoya Sakamoto
- Isotope Imaging Laboratory, Creative Research Institution, Hokkaido University, Sapporo 001-0021, Japan
| | - Toru Matsumoto
- The Hakubi Center for Advanced Research, Kyoto University, Kitashirakawaoiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
- Division of Earth and Planetary Sciences, Kyoto University, Kitashirakawaoiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Ken-ichi Bajo
- Department of Natural History Sciences, Hokkaido University Sapporo 060-0810, Japan
| | - Sohei Wada
- Department of Natural History Sciences, Hokkaido University Sapporo 060-0810, Japan
| | - Yohei Igami
- Division of Earth and Planetary Sciences, Kyoto University, Kitashirakawaoiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Akira Miyake
- Division of Earth and Planetary Sciences, Kyoto University, Kitashirakawaoiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Takaaki Noguchi
- Division of Earth and Planetary Sciences, Kyoto University, Kitashirakawaoiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Daiki Yamamoto
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Sara S. Russell
- Department of Earth Sciences, Natural History Museum, London, SW7 5BD, UK
| | - Yoshinari Abe
- Graduate School of Engineering Materials Science and Engineering, Tokyo Denki University, Tokyo 120-8551, Japan
| | - Jérôme Aléon
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Sorbonne Université, Museum National d’Histoire Naturelle, Centre National de la Recherche Scientifique Unité Mixte de Recherche 7590, IRD, Paris 75005, France
| | | | - Sachiko Amari
- McDonnell Center for the Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, USA
- Geochemical Research Center, The University of Tokyo, Tokyo 113-0033, Japan
| | - Yuri Amelin
- Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, GD 510640, China
| | - Martin Bizzarro
- Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen K 1350, Denmark
| | - Audrey Bouvier
- Bayerisches Geoinstitut, Universität Bayreuth, Bayreuth 95447, Germany
| | - Richard W. Carlson
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Marc Chaussidon
- Université de Paris, Institut de physique du globe de Paris, Centre National de la Recherche Scientifique, Paris 75005, France
| | - Byeon-Gak Choi
- Department of Earth Science Education, Seoul National University, Seoul 08826, Republic of Korea
| | - Nicolas Dauphas
- Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Andrew M. Davis
- Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Tommaso Di Rocco
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Wataru Fujiya
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Ryota Fukai
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Ikshu Gautam
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Makiko K. Haba
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Yuki Hibiya
- Department of General Systems Studies, The University of Tokyo, Tokyo 153-0041, Japan
| | - Hiroshi Hidaka
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Hisashi Homma
- Osaka Application Laboratory, Rigaku Corporation, Osaka 569-1146, Japan
| | - Peter Hoppe
- Max Planck Institute for Chemistry, Mainz 55128, Germany
| | - Gary R. Huss
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Kiyohiro Ichida
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Tsuyoshi Iizuka
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Trevor R. Ireland
- School of Earth and Environmental Sciences, The University of Queensland, St. Lucia QLD 4072, Australia
| | - Akira Ishikawa
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Motoo Ito
- Kochi Institute for Core Sample Research, Japan Agency for Marine-Earth Science and Technology, Kochi 783-8502, Japan
| | - Shoichi Itoh
- Division of Earth and Planetary Sciences, Kyoto University, Kitashirakawaoiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Noriko T. Kita
- Department of Geoscience, University of Wisconsin- Madison, Madison, WI 53706, USA
| | - Kouki Kitajima
- Department of Geoscience, University of Wisconsin- Madison, Madison, WI 53706, USA
| | - Thorsten Kleine
- Max Planck Institute for Solar System Research, Göttingen 37077, Germany
| | - Shintaro Komatani
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Alexander N. Krot
- Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, HI 96822, USA
| | - Ming-Chang Liu
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, USA
- Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
| | - Yuki Masuda
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Kevin D. McKeegan
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, USA
| | - Mayu Morita
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | | | - Frédéric Moynier
- Université de Paris, Institut de physique du globe de Paris, Centre National de la Recherche Scientifique, Paris 75005, France
| | - Izumi Nakai
- Department of Applied Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Ann Nguyen
- Astromaterials Research and Exploration Science Division, National Aeronautics and Space Administration Johnson Space Center, Houston, TX 77058, USA
| | - Larry Nittler
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Morihiko Onose
- Analytical Technology, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Andreas Pack
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Changkun Park
- Division of Earth-System Sciences, Korea Polar Research Institute, Incheon 21990, Republic of Korea
| | - Laurette Piani
- Centre de Recherches Pétrographiques et Géochimiques, Centre National de la Recherche Scientifique–Université de Lorraine, Nancy 54500, France
| | - Liping Qin
- School of Earth and Space Sciences, University of Science and Technology of China,, Anhui 230026, China
| | - Maria Schönbächler
- Institute for Geochemistry and Petrology, Department of Earth Sciences, Eidgenössische Technische Hochschule Zürich, Zürich, Switzerland
| | - Lauren Tafla
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, USA
| | - Haolan Tang
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, USA
| | - Kentaro Terada
- Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan
| | - Yasuko Terada
- Spectroscopy and Imaging, Japan Synchrotron Radiation Research Institute, Hyogo 679-5198, Japan
| | - Tomohiro Usui
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Richard J. Walker
- Department of Geology, University of Maryland, College Park, MD 20742, USA
| | - Katsuyuki Yamashita
- Graduate School of Natural Science and Technology, Okayama University, Okayama 700-8530, Japan
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California, Davis CA 95616, USA
| | - Tetsuya Yokoyama
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Shigekazu Yoneda
- Department of Science and Engineering, National Museum of Nature and Science, Tsukuba 305-0005, Japan
| | - Edward D. Young
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, USA
| | - Hiroharu Yui
- Department of Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Ai-Cheng Zhang
- School of Earth Sciences and Engineering, Nanjing University, Nanjing 210023, China
| | - Tomoki Nakamura
- Department of Earth Science, Tohoku University, Sendai 980-8578, Japan
| | - Hiroshi Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Ryuji Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Kanako Sakamoto
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hikaru Yabuta
- Earth and Planetary Systems Science Program, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - Masanao Abe
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Akiko Miyazaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Aiko Nakato
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masahiro Nishimura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Tatsuaki Okada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Toru Yada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kasumi Yogata
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoru Nakazawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Takanao Saiki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoshi Tanaka
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Fuyuto Terui
- Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | - Yuichi Tsuda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Sei-ichiro Watanabe
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Makoto Yoshikawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Shogo Tachibana
- Tokyo Organization for Planetary and Space Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Hisayoshi Yurimoto
- Department of Natural History Sciences, Hokkaido University Sapporo 060-0810, Japan
- Isotope Imaging Laboratory, Creative Research Institution, Hokkaido University, Sapporo 001-0021, Japan
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9
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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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10
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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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11
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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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12
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Elkins-Tanton LT, Asphaug E, Bell JF, Bierson CJ, Bills BG, Bottke WF, Courville SW, Dibb SD, Jun I, Lawrence DJ, Marchi S, McCoy TJ, Merayo JMG, Oran R, O’Rourke JG, Park RS, Peplowski PN, Prettyman TH, Raymond CA, Weiss BP, Wieczorek MA, Zuber MT. Distinguishing the Origin of Asteroid (16) Psyche. SPACE SCIENCE REVIEWS 2022; 218:17. [PMID: 35431348 PMCID: PMC9005435 DOI: 10.1007/s11214-022-00880-9] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/06/2021] [Accepted: 03/16/2022] [Indexed: 06/02/2023]
Abstract
The asteroid (16) Psyche may be the metal-rich remnant of a differentiated planetesimal, or it may be a highly reduced, metal-rich asteroidal material that never differentiated. The NASA Psyche mission aims to determine Psyche's provenance. Here we describe the possible solar system regions of origin for Psyche, prior to its likely implantation into the asteroid belt, the physical and chemical processes that can enrich metal in an asteroid, and possible meteoritic analogs. The spacecraft payload is designed to be able to discriminate among possible formation theories. The project will determine Psyche's origin and formation by measuring any strong remanent magnetic fields, which would imply it was the core of a differentiated body; the scale of metal to silicate mixing will be determined by both the neutron spectrometers and the filtered images; the degree of disruption between metal and rock may be determined by the correlation of gravity with composition; some mineralogy (e.g., modeled silicate/metal ratio, and inferred existence of low-calcium pyroxene or olivine, for example) will be detected using filtered images; and the nickel content of Psyche's metal phase will be measured using the GRNS.
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Affiliation(s)
- Linda T. Elkins-Tanton
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 86387-2001 USA
| | - Erik Asphaug
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0092 USA
| | - James F. Bell
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 86387-2001 USA
| | - Carver J. Bierson
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 86387-2001 USA
| | | | | | - Samuel W. Courville
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 86387-2001 USA
| | - Steven D. Dibb
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 86387-2001 USA
| | - Insoo Jun
- Jet Propulsion Laboratory, Pasadena, CA 91109 USA
| | - David J. Lawrence
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723 USA
| | | | - Timothy J. McCoy
- Smithsonian National Museum of Natural History, Washington, DC 20013 USA
| | - Jose M. G. Merayo
- National Space Institute, Danish Technical University, Lyngby, Denmark
| | - Rona Oran
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307 USA
| | - Joseph G. O’Rourke
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 86387-2001 USA
| | - Ryan S. Park
- Jet Propulsion Laboratory, Pasadena, CA 91109 USA
| | | | | | | | - Benjamin P. Weiss
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307 USA
| | - Mark A. Wieczorek
- Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Université Côte d’Azur, Nice, France
| | - Maria T. Zuber
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307 USA
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13
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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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14
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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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15
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Ray S, Garvie LAJ, Rai VK, Wadhwa M. Correlated iron isotopes and silicon contents in aubrite metals reveal structure of their asteroidal parent body. Sci Rep 2021; 11:22552. [PMID: 34799673 PMCID: PMC8605012 DOI: 10.1038/s41598-021-99160-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/05/2021] [Accepted: 09/17/2021] [Indexed: 11/13/2022] Open
Abstract
Iron isotopes record the physical parameters, such as temperature and redox conditions, during differentiation processes on rocky bodies. Here we report the results of a correlated investigation of iron isotope compositions and silicon contents of silicon-bearing metal grains from several aubritic meteorites. Based on their Fe isotopic and elemental Si compositions and thermal modelling, we show that these aubrite metals equilibrated with silicates at temperatures ranging from ~ 1430 to ~ 1640 K and likely sampled different depths within their asteroidal parent body. The highest temperature in this range corresponds to their equilibration at a minimum depth of up to ~ 35 km from the surface of the aubrite parent body, followed by brecciation and excavation by impacts within the first ~ 4 Myr of Solar System history.
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Affiliation(s)
- Soumya Ray
- School of Earth and Space Exploration, Arizona State University, Tempe, 85287, USA.
| | - Laurence A J Garvie
- School of Earth and Space Exploration, Arizona State University, Tempe, 85287, USA.,Center for Meteorite Studies, Arizona State University, Tempe, 85287, USA
| | - Vinai K Rai
- School of Earth and Space Exploration, Arizona State University, Tempe, 85287, USA
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, 85287, USA
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16
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Borlina CS, Weiss BP, Bryson JFJ, Bai XN, Lima EA, Chatterjee N, Mansbach EN. Paleomagnetic evidence for a disk substructure in the early solar system. SCIENCE ADVANCES 2021; 7:eabj6928. [PMID: 34652938 PMCID: PMC8519560 DOI: 10.1126/sciadv.abj6928] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/26/2021] [Accepted: 08/25/2021] [Indexed: 06/02/2023]
Abstract
Astronomical observations and isotopic measurements of meteorites suggest that substructures are common in protoplanetary disks and may even have existed in the solar nebula. Here, we conduct paleomagnetic measurements of chondrules in CO carbonaceous chondrites to investigate the existence and nature of these disk substructures. We show that the paleomagnetism of chondrules in CO carbonaceous chondrites indicates the presence of a 101 ± 48 μT field in the solar nebula in the outer solar system (~3 to 7 AU from the Sun). The high intensity of this field relative to that inferred from inner solar system (~<3 AU) meteorites indicates a factor of ~5 to 150 mismatch in nebular accretion between the two reservoirs. This suggests substantial mass loss from the disk associated with a major disk substructure, possibly due to a magnetized disk wind.
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Affiliation(s)
- Cauê S. Borlina
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Benjamin P. Weiss
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | | | - Xue-Ning Bai
- Institute for Advanced Study and Department of Astronomy, Tsinghua University, Beijing, China
| | - Eduardo A. Lima
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Nilanjan Chatterjee
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Elias N. Mansbach
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
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17
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Bekaert DV, Auro M, Shollenberger QR, Liu MC, Marschall H, Burton KW, Jacobsen B, Brennecka GA, McPherson GJ, von Mutius R, Sarafian A, Nielsen SG. Fossil records of early solar irradiation and cosmolocation of the CAI factory: A reappraisal. SCIENCE ADVANCES 2021; 7:eabg8329. [PMID: 34586847 PMCID: PMC8480928 DOI: 10.1126/sciadv.abg8329] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 02/01/2021] [Accepted: 08/05/2021] [Indexed: 06/13/2023]
Abstract
Calcium-aluminum–rich inclusions (CAIs) in meteorites carry crucial information about the environmental conditions of the nascent Solar System prior to planet formation. Based on models of 50V–10Be co-production by in-situ irradiation, CAIs are considered to have formed within ~0.1 AU from the proto-Sun. Here, we present vanadium (V) and strontium (Sr) isotopic co-variations in fine- and coarse-grained CAIs and demonstrate that kinetic isotope effects during partial condensation and evaporation best explain V isotope anomalies previously attributed to solar particle irradiation. We also report initial excesses of 10Be and argue that CV CAIs possess essentially a homogeneous level of 10Be, inherited during their formation. Based on numerical modeling of 50V–10Be co-production by irradiation, we show that CAI formation during protoplanetary disk build-up likely occurred at greater heliocentric distances than previously considered, up to planet-forming regions (~1AU), where solar particle fluxes were sufficiently low to avoid substantial in-situ irradiation of CAIs.
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Affiliation(s)
- David V. Bekaert
- NIRVANA Laboratories, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
| | - Maureen Auro
- NIRVANA Laboratories, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
| | - Quinn R. Shollenberger
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Straße 10, Münster 48149, Germany
- Department of Earth, Planetary and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Ming-Chang Liu
- Department of Earth, Planetary and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Horst Marschall
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
- Institut für Geowissenschaften, Goethe Universität, Altenhöferallee 1, 60438 Frankfurt am Main, Germany
- Frankfurt Isotope and Element Research Center, Goethe Universität, 60438 Frankfurt am Main, Germany
| | - Kevin W. Burton
- Department of Earth Sciences, Durham University, Elvet Hill, Durham DH1 3LE, UK
| | - Benjamin Jacobsen
- Nuclear and Chemical Sciences Division, Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
| | - Gregory A. Brennecka
- Nuclear and Chemical Sciences Division, Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
| | - Glenn J. McPherson
- U.S. National Museum of Natural History, Smithsonian Institution, Washington, DC 20560, USA
| | - Richard von Mutius
- Institut für Geowissenschaften, Goethe Universität, Altenhöferallee 1, 60438 Frankfurt am Main, Germany
| | - Adam Sarafian
- NIRVANA Laboratories, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
| | - Sune G. Nielsen
- NIRVANA Laboratories, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
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18
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Melwani Daswani M, Vance SD, Mayne MJ, Glein CR. A Metamorphic Origin for Europa's Ocean. GEOPHYSICAL RESEARCH LETTERS 2021; 48:e2021GL094143. [PMID: 35865189 PMCID: PMC9286408 DOI: 10.1029/2021gl094143] [Citation(s) in RCA: 11] [Impact Index Per Article: 3.7] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/07/2021] [Revised: 07/26/2021] [Accepted: 08/04/2021] [Indexed: 05/28/2023]
Abstract
Europa likely contains an iron-rich metal core. For it to have formed, temperatures within Europa reached ≳ 1250 K. Going up to that temperature, accreted chondritic minerals - for example, carbonates and phyllosilicates - would partially devolatilize. Here, we compute the amounts and compositions of exsolved volatiles. We find that volatiles released from the interior would have carried solutes, redox-sensitive species, and could have generated a carbonic ocean in excess of Europa's present-day hydrosphere, and potentially an early CO 2 atmosphere. No late delivery of cometary water was necessary. Contrasting with prior work, CO 2 could be the most abundant solute in the ocean, followed by Ca 2 + , SO 4 2 - , and HCO 3 - . However, gypsum precipitation going from the seafloor to the ice shell decreases the dissolved S/Cl ratio, such that Cl > S at the shallowest depths, consistent with recently inferred endogenous chlorides at Europa's surface. Gypsum would form a 3-10 km thick sedimentary layer at the seafloor.
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Affiliation(s)
| | - Steven D. Vance
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Matthew J. Mayne
- Department of Earth SciencesStellenbosch UniversityStellenboschSouth Africa
| | - Christopher R. Glein
- Space Science and Engineering DivisionSouthwest Research InstituteSan AntonioTXUSA
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19
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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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20
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Chaumard N, Defouilloy C, Hertwig AT, Kita NT. Oxygen isotope systematics of chondrules in the Paris CM2 chondrite: indication for a single large formation region across snow line. GEOCHIMICA ET COSMOCHIMICA ACTA 2021; 299:199-218. [PMID: 34776527 PMCID: PMC8588000 DOI: 10.1016/j.gca.2021.02.012] [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
In-situ oxygen three-isotope analyses of chondrules and isolated olivine grains in the Paris (CM) chondrite were conducted by secondary ion mass spectrometry (SIMS). Multiple analyses of olivine and/or pyroxene in each chondrule show indistinguishable Δ17O values, except for minor occurrences of relict olivine grains (and one low-Ca pyroxene). A mean Δ17O value of these homogeneous multiple analyses was obtained for each chondrule, which represent oxygen isotope ratios of the chondrule melt. The Δ17O values of individual chondrules range from -7‰ to -2‰ and generally increase with decreasing Mg# of olivine and pyroxene in individual chondrules. Most type I (FeO-poor) chondrules have high Mg# (~99) and variable Δ17O values from -7.0‰ to -3.3‰. Other type I chondrules (Mg# ≤97), type II (FeO-rich) chondrules, and two isolated FeO-rich olivine grains have host Δ17O values from -3‰ to -2‰. Eight chondrules contain relict grains that are either 16O-rich or 16O-poor relative to their host chondrule and show a wide range of Δ17O values from -13‰ to 0‰. The results from chondrules in the Paris meteorite are similar to those in Murchison (CM). Collectively, the Δ17O values of chondrules in CM chondrites continuously increase from -7‰ to -2‰ with decreasing Mg# from 99 to 37. The majority of type I chondrules (Mg# >98) show Δ17O values from -6‰ to -4‰, while the majority of and type II chondrules (Mg# 60-70) show Δ17O values of -2.5‰. The covariation of Δ17O versus Mg# observed among chondrules in CM chondrites may suggest that most chondrules in carbonaceous chondrites formed in a single large region across the snow line where the contribution of 16O-poor ice to chondrule precursors and dust enrichment factors varied significantly.
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Affiliation(s)
- Noël Chaumard
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, 1215 W. Dayton Street, Madison, WI 53706-1692, USA
- Fi Group, Direction scientifique, 14 terrasse Bellini, 92800 Puteaux, France
| | - Céline Defouilloy
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, 1215 W. Dayton Street, Madison, WI 53706-1692, USA
- CAMECA, 29 quai des Grésillons, 92622 Gennevilliers Cedex, France
| | - Andreas T. Hertwig
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, 1215 W. Dayton Street, Madison, WI 53706-1692, USA
- Institut für Geowissenschaften, Universitat Heidelberg, Im Neuenheimer Feld 234-236, 69120 Heidelberg, Germany
| | - Noriko T. Kita
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, 1215 W. Dayton Street, Madison, WI 53706-1692, USA
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21
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Tsuchiyama A, Miyake A, Okuzumi S, Kitayama A, Kawano J, Uesugi K, Takeuchi A, Nakano T, Zolensky M. Discovery of primitive CO 2-bearing fluid in an aqueously altered carbonaceous chondrite. SCIENCE ADVANCES 2021; 7:7/17/eabg9707. [PMID: 33883146 PMCID: PMC8059924 DOI: 10.1126/sciadv.abg9707] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/07/2021] [Accepted: 03/05/2021] [Indexed: 06/01/2023]
Abstract
Water is abundant as solid ice in the solar system and plays important roles in its evolution. Water is preserved in carbonaceous chondrites as hydroxyl and/or H2O molecules in hydrous minerals, but has not been found as liquid. To uncover such liquid, we performed synchrotron-based x-ray computed nanotomography and transmission electron microscopy with a cryo-stage of the aqueously altered carbonaceous chondrite Sutter's Mill. We discovered CO2-bearing fluid (CO2/H2O > ~0.15) in a nanosized inclusion incorporated into a calcite crystal, appearing as CO2 ice and/or CO2 hydrate at 173 K. This is direct evidence of dynamic evolution of the solar system, requiring the Sutter's Mill's parent body to have formed outside the CO2 snow line and later transportation to the inner solar system because of Jupiter's orbital instability.
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Affiliation(s)
- Akira Tsuchiyama
- Research Organization of Science and Technology, Ritsumeikan University, 1-1-1 Nojihigashi, Kusatsu, Shiga 525-8577, Japan.
- CAS Key Laboratory of Mineralogy and Metallogeny/Guangdong Provincial Key Laboratory of Mineral Physics and Materials, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, 511 Kehua Street, Wushan, Tianhe District, Guangzhou 510640, China
- CAS Center for Excellence in Deep Earth Science, 511 Kehua Street, Wushan, Tianhe District, Guangzhou, 510640, China
| | - Akira Miyake
- Department of Earth and Planetary Sciences, Graduate School of Science, Kyoto University, Kitashirakawa-Oiwakecho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Satoshi Okuzumi
- Department of Earth and Planetary Sciences, School of Science, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan
| | - Akira Kitayama
- Department of Earth and Planetary Sciences, Graduate School of Science, Kyoto University, Kitashirakawa-Oiwakecho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Jun Kawano
- Department of Earth and Planetary Sciences, Faculty of Science, Hokkaido University, Kita-10 Nishi-8, Kita-ku, Sapporo 060-0810, Japan
| | - Kentaro Uesugi
- Japan Synchrotron Radiation Research Institute, Hyogo 679-5198, Japan
| | - Akihisa Takeuchi
- Japan Synchrotron Radiation Research Institute, Hyogo 679-5198, Japan
| | - Tsukasa Nakano
- Geological Survey of Japan, National Institute of Advanced Industrial Science and Technology, Ibaraki 305-8567, Japan
| | - Michael Zolensky
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
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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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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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Fukuda K, Brownlee DE, Joswiak DJ, Tenner TJ, Kimura M, Kita NT. Correlated isotopic and chemical evidence for condensation origins of olivine in comet 81P/Wild 2 and in AOAs from CV and CO chondrites. GEOCHIMICA ET COSMOCHIMICA ACTA 2021; 293:544-574. [PMID: 34866644 PMCID: PMC8637496 DOI: 10.1016/j.gca.2020.09.036] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
Magnesium stable isotope ratios and minor element abundances of five olivine particles from comet 81P/Wild 2 were examined by secondary ion mass spectrometry (SIMS). Wild 2 olivine particles exhibit only small variations in δ25Mg values from -1.0 +0.4/-0.5 ‰ to 0.6 +0.5/- 0.6 ‰ (2σ). This variation can be simply explained by mass-dependent fractionation from Mg isotopic compositions of the Earth and bulk meteorites, suggesting that Wild 2 olivine particles formed in the chondritic reservoir with respect to Mg isotope compositions. We also determined minor element abundances, and O and Mg isotope ratios of olivine grains in amoeboid olivine aggregates (AOAs) from Kaba (CV3.1) and DOM 08006 (CO3.01) carbonaceous chondrites. Our new SIMS minor element data reveal uniform, low FeO contents of ~0.05 wt% among AOA olivines from DOM 08006, suggesting that AOAs formed at more reducing environments in the solar nebula than previously thought. Furthermore, the SIMS-derived FeO contents of the AOA olivines are consistently lower than those obtained by electron microprobe analyses (~1 wt% FeO), indicating possible fluorescence from surrounding matrix materials and/or Fe,Ni-metals in AOAs during electron microprobe analyses. For Mg isotopes, AOA olivines show more negative mass-dependent fractionation (-3.8 ± 0.5‰ ≤ δ25Mg ≤ -0.2 ± 0.3‰; 2σ) relative to Wild 2 olivines. Further, these Mg isotope variations are correlated with their host AOA textures. Large negative Mg isotope fractionations in olivine are often observed in pore-rich AOAs, while those in compact AOAs tend to have near-chondritic Mg isotopic compositions. These observations indicate that pore-rich AOAs preserved their gas-solid condensation histories, while compact AOAs experienced thermal processing in the solar nebula after their condensation and aggregation. Importantly, one 16O-rich Wild 2 LIME olivine particle (T77/F50) shows negative Mg isotope fractionation (δ25Mg = -0.8 ± 0.4‰, δ26Mg = -1.4 ± 0.9‰; 2σ) relative to bulk chondrites. Minor element abundances of T77/F50 are in excellent agreement with those of olivines from pore-rich AOAs in DOM 08006. The observed similarity in O and Mg isotopes, and minor element abundances suggest that T77/F50 formed in an environment similar to AOAs, probably near the proto-Sun, and then was transported to the Kuiper belt, where comet 81P/Wild 2 likely accreted.
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Affiliation(s)
- Kohei Fukuda
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Donald E. Brownlee
- Department of Astronomy, University of Washington, Seattle, WA 98195, USA
| | - David J. Joswiak
- Department of Astronomy, University of Washington, Seattle, WA 98195, USA
| | - Travis J. Tenner
- Chemistry Division, Nuclear and Radiochemistry, Los Alamos National Laboratory, MSJ514, Los Alamos, NM 87545, USA
| | - Makoto Kimura
- National Institute of Polar Research, Tokyo 190-8518, Japan
| | - Noriko T. Kita
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
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25
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Weiss BP, Bai XN, Fu RR. History of the solar nebula from meteorite paleomagnetism. SCIENCE ADVANCES 2021; 7:7/1/eaba5967. [PMID: 33523830 PMCID: PMC7775786 DOI: 10.1126/sciadv.aba5967] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/17/2019] [Accepted: 11/10/2020] [Indexed: 06/02/2023]
Abstract
We review recent advances in our understanding of magnetism in the solar nebula and protoplanetary disks (PPDs). We discuss the implications of theory, meteorite measurements, and astronomical observations for planetary formation and nebular evolution. Paleomagnetic measurements indicate the presence of fields of 0.54 ± 0.21 G at ~1 to 3 astronomical units (AU) from the Sun and ≳0.06 G at 3 to 7 AU until >1.22 and >2.51 million years (Ma) after solar system formation, respectively. These intensities are consistent with those predicted to enable typical astronomically observed protostellar accretion rates of ~10-8 M ⊙year-1, suggesting that magnetism played a central role in mass transport in PPDs. Paleomagnetic studies also indicate fields <0.006 G and <0.003 G in the inner and outer solar system by 3.94 and 4.89 Ma, respectively, consistent with the nebular gas having dispersed by this time. This is similar to the observed lifetimes of extrasolar protoplanetary disks.
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Affiliation(s)
- Benjamin P Weiss
- Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA.
| | - Xue-Ning Bai
- Institute for Advanced Study and Department of Astronomy, Tsinghua University, Beijing, China.
| | - Roger R Fu
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA, USA
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26
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Vollmer C, Leitner J, Kepaptsoglou D, Ramasse QM, King AJ, Schofield PF, Bischoff A, Araki T, Hoppe P. A primordial 15N-depleted organic component detected within the carbonaceous chondrite Maribo. Sci Rep 2020; 10:20251. [PMID: 33219224 PMCID: PMC7679378 DOI: 10.1038/s41598-020-77190-z] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/04/2020] [Accepted: 11/06/2020] [Indexed: 11/09/2022] Open
Abstract
We report on the detection of primordial organic matter within the carbonaceous chondrite Maribo that is distinct from the majority of organics found in extraterrestrial samples. We have applied high-spatial resolution techniques to obtain C-N isotopic compositions, chemical, and structural information of this material. The organic matter is depleted in 15N relative to the terrestrial value at around δ15N ~ -200‰, close to compositions in the local interstellar medium. Morphological investigations by electron microscopy revealed that the material consists of µm- to sub-µm-sized diffuse particles dispersed within the meteorite matrix. Electron energy loss and synchrotron X-ray absorption near-edge structure spectroscopies show that the carbon functional chemistry is dominated by aromatic and C=O bonding environments similar to primordial organics from other carbonaceous chondrites. The nitrogen functional chemistry is characterized by C-N double and triple bonding environments distinct from what is usually found in 15N-enriched organics from aqueously altered carbonaceous chondrites. Our investigations demonstrate that Maribo represents one of the least altered CM chondrite breccias found to date and contains primordial organic matter, probably originating in the interstellar medium.
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Affiliation(s)
- Christian Vollmer
- Institut für Mineralogie, Westfälische Wilhelms-Universität, Corrensstr. 24, 48149, Münster, Germany.
| | - Jan Leitner
- Particle Chemistry Department, Max Planck Institute for Chemistry, Hahn-Meitner-Weg 1, 55128, Mainz, Germany
| | - Demie Kepaptsoglou
- SuperSTEM Laboratory, Keckwick Lane, Daresbury, WA4 4AD, UK.,Jeol Nanocentre and Department of Physics, University of York, Heslington, YO10 5DD, UK
| | - Quentin M Ramasse
- SuperSTEM Laboratory, Keckwick Lane, Daresbury, WA4 4AD, UK.,School of Chemical and Process Engineering and School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK
| | - Ashley J King
- Planetary Materials Group, Department of Earth Sciences, Natural History Museum, London, SW7 5BD, UK
| | - Paul F Schofield
- Planetary Materials Group, Department of Earth Sciences, Natural History Museum, London, SW7 5BD, UK
| | - Addi Bischoff
- Institut für Planetologie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Str. 10, 48149, Münster, Germany
| | | | - Peter Hoppe
- Particle Chemistry Department, Max Planck Institute for Chemistry, Hahn-Meitner-Weg 1, 55128, Mainz, Germany
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27
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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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28
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Vance SD, Melwani Daswani M. Serpentinite and the search for life beyond Earth. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2020; 378:20180421. [PMID: 31902342 DOI: 10.1098/rsta.2018.0421] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 11/27/2019] [Indexed: 06/10/2023]
Abstract
Hydrogen from serpentinization is a source of chemical energy for some life forms on Earth. It is a potential fuel for life in the subsurface of Mars and in the icy ocean worlds in the outer solar system. Serpentinization is also implicated in life's origin. Planetary exploration offers a way to investigate such theories by characterizing and ultimately searching for life in geochemical settings that no longer exist on Earth. At present, much of the current context of serpentinization on other worlds relies on inference from modelling and studies on Earth. While there is evidence from orbital spectral imaging and martian meteorites that serpentinization has occurred on Mars, the extent and duration of that activity has not been constrained. Similarly, ongoing serpentinization might explain hydrogen found in the ocean of Saturn's tiny moon Enceladus, but this raises questions about how long such activity has persisted. Titan's hydrocarbon-rich atmosphere may derive from ancient or present-day serpentinization at the bottom of its ocean. In Europa, volcanism or serpentinization may provide hydrogen as a redox couple to oxygen generated at the moon's surface. We assess the potential extent of serpentinization in the solar system's wet and rocky worlds, assuming that microfracturing from thermal expansion anisotropy sets an upper limit on the percolation depth of surface water into the rocky interiors. In this bulk geophysical model, planetary cooling from radiogenic decay implies the infiltration of water to greater depths through time, continuing to the present. The serpentinization of this newly exposed rock is assessed as a significant source of global hydrogen. Comparing the computed hydrogen and surface-generated oxygen delivered to Europa's ocean reveals redox fluxes similar to Earth's. Planned robotic exploration missions to other worlds can aid in understanding the planetary context of serpentinization, testing the predictions herein. This article is part of a discussion meeting issue 'Serpentinite in the Earth System'.
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Affiliation(s)
- S D Vance
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8001, USA
| | - M Melwani Daswani
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8001, USA
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29
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Tenner TJ, Nakashima D, Ushikubo T, Tomioka N, Kimura M, Weisberg MK, Kita NT. Extended chondrule formation intervals in distinct physicochemical environments: Evidence from Al-Mg isotope systematics of CR chondrite chondrules with unaltered plagioclase. GEOCHIMICA ET COSMOCHIMICA ACTA 2019; 260:133-160. [PMID: 32255837 PMCID: PMC7121246 DOI: 10.1016/j.gca.2019.06.023] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
Al-Mg isotope systematics of twelve FeO-poor (type I) chondrules from CR chondrites Queen Alexandra Range 99177 and Meteorite Hills 00426 were investigated by secondary ion mass spectrometry (SIMS). Five chondrules with Mg#'s of 99.0 to 99.2 and Δ17O of -4.2‰ to -5.3‰ have resolvable excess 26Mg. Their inferred (26Al/27Al)0 values range from (3.5 ± 1.3) × 10‒6 to (6.0 ± 3.9) × 10‒6. This corresponds to formation times of 2.2 (-0.5/+1.1) Myr to 2.8 (‒0.3/+0.5) Myr after CAIs, using a canonical (26Al/27Al)0 of 5.23 × 10-5, and assuming homogeneously distributed 26Al that yielded a uniform initial 26Al/27Al in the Solar System. Seven chondrules lack resolvable excess 26Mg. They have lower Mg#'s (94.2 to 98.7) and generally higher Δ17O (-0.9‰ to -4.9‰) than chondrules with resolvable excess 26Mg. Their inferred (26Al/27Al)0 upper limits range from 1.3 × 10‒6 to 3.2 × 10‒6, corresponding to formation >2.9 to >3.7 Myr after CAIs. Al-Mg isochrons depend critically on chondrule plagioclase, and several characteristics indicate the chondrule plagioclase is unaltered: (1) SIMS 27Al/24Mg depth profile patterns match those from anorthite standards, and SEM/EDS of chondrule SIMS pits show no foreign inclusions; (2) transmission electron microscopy (TEM) reveals no nanometer-scale micro-inclusions and no alteration due to thermal metamorphism; (3) oxygen isotopes of chondrule plagioclase match those of coexisting olivine and pyroxene, indicating a low extent of thermal metamorphism; and (4) electron microprobe data show chondrule plagioclase is anorthite-rich, with excess structural silica and high MgO, consistent with such plagioclase from other petrologic type 3.00-3.05 chondrites. We conclude that the resolvable (26Al/27Al)0 variabilities among chondrules studied are robust, corresponding to a formation interval of at least 1.1 Myr. Using relationships between chondrule (26Al/27Al)0, Mg#, and Δ17O, we interpret spatial and temporal features of dust, gas, and H2O ice in the FeO-poor chondrule-forming environment. Mg# ≥ 99, Δ17O ~-5‰ chondrules with resolvable excess 26Mg initially formed in an environment that was relatively anhydrous, with a dust-to-gas ratio of ~100×. After these chondrules formed, we interpret a later influx of 16O-poor H2O ice into the environment, and that dust-to-gas ratios expanded (100× to 300×). This led to the later formation of more oxidized Mg# 94-99 chondrules with higher Δ17O (-5‰ to -1‰), with low (26Al/27Al)0, and hence no resolvable excess 26Mg. We refine the mean CR chondrite chondrule formation age via mass balance, by considering that Mg# ≥ 99 chondrules generally have resolved positive (26Al/27Al)0 and that Mg# < 99 chondrules generally have no resolvable excess 26Mg, implying lower (26Al/27Al)0. We obtain a mean chondrule formation age of 3.8 ± 0.3 Myr after CAIs, which is consistent with Pb-Pb and Hf-W model ages of CR chondrite chondrule aggregates. Overall, this suggests most CR chondrite chondrules formed immediately before parent body accretion.
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Affiliation(s)
- Travis J Tenner
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
- Chemistry Division, Nuclear and Radiochemistry, Los Alamos National Laboratory, MSJ514, Los Alamos, NM 87545, USA
| | - Daisuke Nakashima
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
- Department of Earth and Planetary Material Sciences, Faculty of Science, Tohoku University, Aoba, Sendai, Miyagi 980-8578, Japan
| | - Takayuki Ushikubo
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
- Kochi Institute for Core Sample Research, Japan Agency for Marine-Earth Science and Technology (JAMSTEC), 200 Monobe Otsu, Nankoku, Kochi 783-8502, Japan
| | - Naotaka Tomioka
- Kochi Institute for Core Sample Research, Japan Agency for Marine-Earth Science and Technology (JAMSTEC), 200 Monobe Otsu, Nankoku, Kochi 783-8502, Japan
| | - Makoto Kimura
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
- National Institute of Polar Research, Tokyo 190-8518, Japan
| | - Michael K Weisberg
- Kingsborough Community College and Graduate Center, The City University of New York, 2001 Oriental Boulevard, Brooklyn, NY 11235-2398, USA
- American Museum of Natural History, Central Park West at 79 Street, New York, NY, 10024-5192, USA
| | - Noriko T Kita
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
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30
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Hertwig AT, Makoto K, Ushikubo T, Defouilloy C, Kita NT. The 26Al- 26Mg systematics of FeO-rich chondrules from Acfer 094: two chondrule generations distinct in age and oxygen isotope ratios. GEOCHIMICA ET COSMOCHIMICA ACTA 2019; 253:111-126. [PMID: 32214432 PMCID: PMC7094794 DOI: 10.1016/j.gca.2019.02.020] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
The 26Al-26Mg ages of FeO-rich (type II) chondrules from Acfer 094, one of the least thermally metamorphosed carbonaceous chondrites, were determined by SIMS analysis of plagioclase and olivine/pyroxene using a radio frequency (RF) plasma oxygen ion source. In combination with preexisting 26Al-26Mg ages of FeO-poor (type I) chondrules, the maximum range of formation ages recorded in chondrules from a single meteorite is determined to help provide constraints on models of material transport in the proto-planetary disk. We also report new SIMS oxygen three-isotope analyses of type II chondrules in Acfer 094. All but one of the plagioclase analyses show resolvable excesses in 26Mg and isochron regressions yield initial 26Al/27Al ratios of type II chondrules that range from (3.62 ± 0.86) × 10-6 to (9.3 ± 1.1) × 10-6, which translates to formation ages between 2.71 -0.22/+0.28 Ma and 1.75 -0.11/+0.12 Ma after CAI. This overall range is indistinguishable from that determined for type I chondrules in Acfer 094. The initial 26Al/27Al ratio of the oldest type II chondrule is resolved from that of all other type II chondrules in Acfer 094. Importantly, the oldest type I chondrule and the oldest type II chondrule in Acfer 094 possess within analytical error indistinguishable initial 26Al/27Al ratios and Δ17O values of ~0‰. Ages and oxygen isotope ratios clearly set these two chondrules apart from all other chondrules in Acfer 094. It is therefore conceivable that the formation region of these two chondrules differs from that of other chondrules and in turn suggests that Acfer 094 contains two distinct chondrule generations.
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Affiliation(s)
- Andreas T Hertwig
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Kimura Makoto
- National Institute of Polar Research, Meteorite Research Center, Midoricho 10-3, Tachikawa, Tokyo 190-8518, Japan
| | - Takayuki Ushikubo
- Kochi Institute for Core Sample Research, JAMSTEC, 200 Monobe-otsu, Nankoku, Kochi 783-8502 Japan
| | - Céline Defouilloy
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Noriko T Kita
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
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31
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Contributions from Accreted Organics to Titan’s Atmosphere: New Insights from Cometary and Chondritic Data. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/aaf561] [Citation(s) in RCA: 26] [Impact Index Per Article: 5.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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32
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33
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Schrader DL, Fu RR, Desch SJ, Davidson J. The background temperature of the protoplanetary disk within the first four million years of the Solar System. EARTH AND PLANETARY SCIENCE LETTERS 2018; 504:30-37. [PMID: 31708587 PMCID: PMC6839690 DOI: 10.1016/j.epsl.2018.09.030] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
The background temperature of the protoplanetary disk is a fundamental but poorly constrained parameter that strongly influences a wide range of conditions and processes in the early Solar System, including the widespread process(es) by which chondrules originate. Chondrules, mm-scale objects composed primarily of silicate minerals, were formed in the protoplanetary disk almost entirely during the first four million years of Solar System history but their formation mechanism(s) are poorly understood. Here we present new constraints on the sub-silicate solidus cooling rates of chondrules at <873 K (600°C) using the compositions of sulfide minerals. We show that chondrule cooling rates remained relatively rapid (~100 to 101 K/hr) between 873 and 503 K, which implies a protoplanetary disk background temperature of <503 K (230°C) and is consistent with many models of chondrule formation by shocks in the solar nebula, potentially driven by the formation of Jupiter and/or planetary embryos, as the chondrule formation mechanism. This protoplanetary disk background temperature rules out current sheets and resulting short-circuit instabilities as the chondrule formation mechanism. More detailed modeling of chondrule cooling histories in impacts is required to fully evaluate impacts as a chondrule formation model. These results motivate further theoretical work to understand the expected thermal evolution of chondrules at ≤873 K under a variety of chondrule formation scenarios.
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Affiliation(s)
- Devin L. Schrader
- Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, 781 East Terrace Road, Tempe, AZ 85287
| | - Roger R. Fu
- Department of Earth and Planetary Sciences, Harvard University, 20 Oxford St. Cambridge, MA 02138
| | - Steven J. Desch
- School of Earth and Space Exploration, Arizona State University, PO Box 871404, Tempe, AZ 85287
| | - Jemma Davidson
- Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, 781 East Terrace Road, Tempe, AZ 85287
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