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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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2
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Leone G, Tanaka HK. Igneous processes in the small bodies of the Solar System I. Asteroids and comets. iScience 2023; 26:107160. [PMID: 37534155 PMCID: PMC10391981 DOI: 10.1016/j.isci.2023.107160] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 08/04/2023] Open
Abstract
Igneous processes were quite widespread in the small bodies of the Solar System (SBSS) and were initially fueled by short-lived radioisotopes, the proto-Sun, impact heating, and differentiation heating. Once they finished, long-lived radioisotopes continued to warm the active bodies of the Earth, (possibly) Venus, and the cryovolcanism of Enceladus. The widespread presence of olivine and pyroxenes in planets and also in SBSS suggests that they were not necessarily the product of igneous processes and they might have been recycled from previous nebular processes or entrained in comets from interstellar space. The difference in temperature between the inner and the outer Solar System has clearly favored thermal annealing of the olivine close to the proto-Sun. Transport of olivine within the Solar System probably occurred also due to protostellar jets and winds but the entrainment in SBSS from interstellar space would overcome the requirement of initial turbulent regime in the protoplanetary nebula.
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Affiliation(s)
- Giovanni Leone
- Instituto de Investigación en Astronomía y Ciencias Planetarias, Universidad de Atacama, Chile
- Virtual Muography Institute, Global, Tokyo, Japan
| | - Hiroyuki K.M. Tanaka
- Virtual Muography Institute, Global, Tokyo, Japan
- International Muography Research Organization (MUOGRAPHIX), The University of Tokyo, Japan
- Earthquake Research Institute, The University of Tokyo, 1-1-1 Yayoi, Bunkyo, Tokyo 113-0032, Japan
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3
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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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4
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Lykawka PS, Ito T. Terrestrial planet and asteroid belt formation by Jupiter-Saturn chaotic excitation. Sci Rep 2023; 13:4708. [PMID: 36973305 PMCID: PMC10042868 DOI: 10.1038/s41598-023-30382-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/21/2022] [Accepted: 02/21/2023] [Indexed: 03/29/2023] Open
Abstract
The terrestrial planets formed by accretion of asteroid-like objects within the inner solar system's protoplanetary disk. Previous works have found that forming a small-mass Mars requires the disk to contain little mass beyond ~ 1.5 au (i.e., the disk mass was concentrated within this boundary). The asteroid belt also holds crucial information about the origin of such a narrow disk. Several scenarios may produce a narrow disk. However, simultaneously replicating the four terrestrial planets and the inner solar system properties remains elusive. Here, we found that chaotic excitation of disk objects generated by a near-resonant configuration of Jupiter-Saturn can create a narrow disk, allowing the formation of the terrestrial planets and the asteroid belt. Our simulations showed that this mechanism could typically deplete a massive disk beyond ~ 1.5 au on a 5-10 Myr timescale. The resulting terrestrial systems reproduced the current orbits and masses of Venus, Earth and Mars. Adding an inner region disk component within ~ 0.8-0.9 au allowed several terrestrial systems to simultaneously form analogues of the four terrestrial planets. Our terrestrial systems also frequently satisfied additional constraints: Moon-forming giant impacts occurring after a median ~ 30-55 Myr, late impactors represented by disk objects formed within 2 au, and effective water delivery during the first 10-20 Myr of Earth's formation. Finally, our model asteroid belt explained the asteroid belt's orbital structure, small mass and taxonomy (S-, C- and D/P-types).
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Affiliation(s)
| | - Takashi Ito
- Center for Computational Astrophysics, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo, 181-8588, Japan
- Planetary Exploration Research Center, Chiba Institute of Technology, 2-17-1 Tsudanuma, Narashino, Chiba, 275-0016, Japan
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5
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Nie NX, Wang D, Torrano ZA, Carlson RW, O'D Alexander CM, Shahar A. Meteorites have inherited nucleosynthetic anomalies of potassium-40 produced in supernovae. Science 2023; 379:372-376. [PMID: 36701465 DOI: 10.1126/science.abn1783] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/27/2023]
Abstract
Meteorites record processes that occurred before and during the formation of the Solar System in the form of nucleosynthetic anomalies: isotopic compositions that differ from the Solar System patterns. Nucleosynthetic anomalies are rarely seen in volatile elements such as potassium at bulk meteorite scale. We measured potassium isotope ratios in 32 meteorites and identified nucleosynthetic anomalies in the isotope potassium-40. The anomalies are larger and more variable in carbonaceous chondrite (CC) meteorites than in noncarbonaceous (NC) meteorites, indicating that CCs inherited more material produced in supernova nucleosynthesis. The potassium-40 anomaly of Earth is close to that of the NCs, implying that Earth's potassium was mostly delivered by NCs.
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Affiliation(s)
- Nicole X Nie
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Da Wang
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA.,International Center for Planetary Science, College of Earth Sciences, Chengdu University of Technology, 610059 Chengdu, China
| | - Zachary A Torrano
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Richard W Carlson
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Conel M O'D Alexander
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Anat Shahar
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
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6
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King AJ, Daly L, Rowe J, Joy KH, Greenwood RC, Devillepoix HA, Suttle MD, Chan QH, Russell SS, Bates HC, Bryson JF, Clay PL, Vida D, Lee MR, O’Brien Á, Hallis LJ, Stephen NR, Tartèse R, Sansom EK, Towner MC, Cupak M, Shober PM, Bland PA, Findlay R, Franchi IA, Verchovsky AB, Abernethy FA, Grady MM, Floyd CJ, Van Ginneken M, Bridges J, Hicks LJ, Jones RH, Mitchell JT, Genge MJ, Jenkins L, Martin PE, Sephton MA, Watson JS, Salge T, Shirley KA, Curtis RJ, Warren TJ, Bowles NE, Stuart FM, Di Nicola L, Györe D, Boyce AJ, Shaw KM, Elliott T, Steele RC, Povinec P, Laubenstein M, Sanderson D, Cresswell A, Jull AJ, Sýkora I, Sridhar S, Harrison RJ, Willcocks FM, Harrison CS, Hallatt D, Wozniakiewicz PJ, Burchell MJ, Alesbrook LS, Dignam A, Almeida NV, Smith CL, Clark B, Humphreys-Williams ER, Schofield PF, Cornwell LT, Spathis V, Morgan GH, Perkins MJ, Kacerek R, Campbell-Burns P, Colas F, Zanda B, Vernazza P, Bouley S, Jeanne S, Hankey M, Collins GS, Young JS, Shaw C, Horak J, Jones D, James N, Bosley S, Shuttleworth A, Dickinson P, McMullan I, Robson D, Smedley AR, Stanley B, Bassom R, McIntyre M, Suttle AA, Fleet R, Bastiaens L, Ihász MB, McMullan S, Boazman SJ, Dickeson ZI, Grindrod PM, Pickersgill AE, Weir CJ, Suttle FM, Farrelly S, Spencer I, Naqvi S, Mayne B, Skilton D, Kirk D, Mounsey A, Mounsey SE, Mounsey S, Godfrey P, Bond L, Bond V, Wilcock C, Wilcock H, Wilcock R. The Winchcombe meteorite, a unique and pristine witness from the outer solar system. SCIENCE ADVANCES 2022; 8:eabq3925. [PMID: 36383648 PMCID: PMC9668287 DOI: 10.1126/sciadv.abq3925] [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: 04/05/2022] [Accepted: 10/20/2022] [Indexed: 06/16/2023]
Abstract
Direct links between carbonaceous chondrites and their parent bodies in the solar system are rare. The Winchcombe meteorite is the most accurately recorded carbonaceous chondrite fall. Its pre-atmospheric orbit and cosmic-ray exposure age confirm that it arrived on Earth shortly after ejection from a primitive asteroid. Recovered only hours after falling, the composition of the Winchcombe meteorite is largely unmodified by the terrestrial environment. It contains abundant hydrated silicates formed during fluid-rock reactions, and carbon- and nitrogen-bearing organic matter including soluble protein amino acids. The near-pristine hydrogen isotopic composition of the Winchcombe meteorite is comparable to the terrestrial hydrosphere, providing further evidence that volatile-rich carbonaceous asteroids played an important role in the origin of Earth's water.
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Affiliation(s)
- Ashley J. King
- Natural History Museum, London SW7 5BD, UK
- System for Capture of Asteroid and Meteorite Paths (SCAMP), UK
- UK Fireball Alliance (UKFAll), UK
| | - Luke Daly
- UK Fireball Alliance (UKFAll), UK
- University of Glasgow, Glasgow G12 8QQ, UK
- University of Oxford, Oxford OX1 3AN, UK
- University of Sydney, Sydney 2006, NSW, Australia
- UK Fireball Network (UKFN), UK
| | - James Rowe
- System for Capture of Asteroid and Meteorite Paths (SCAMP), UK
- UK Fireball Alliance (UKFAll), UK
| | - Katherine H. Joy
- UK Fireball Alliance (UKFAll), UK
- The University of Manchester, Manchester M13 9PL, UK
| | | | | | - Martin D. Suttle
- Natural History Museum, London SW7 5BD, UK
- UK Fireball Network (UKFN), UK
- The Open University, Milton Keynes MK7 6AA, UK
| | - Queenie H. S. Chan
- The Open University, Milton Keynes MK7 6AA, UK
- Royal Holloway, University of London, Egham TW20 0EX, UK
| | | | | | | | | | - Denis Vida
- Western University, London N6A 3K7, Canada
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | - Finlay M. Stuart
- Scottish Universities Environmental Research Centre (SUERC), East Kilbride G75 0QF, UK
| | - Luigia Di Nicola
- Scottish Universities Environmental Research Centre (SUERC), East Kilbride G75 0QF, UK
| | - Domokos Györe
- Scottish Universities Environmental Research Centre (SUERC), East Kilbride G75 0QF, UK
- Isomass Scientific Inc., Calgary T2H 3A9, Canada
| | - Adrian J. Boyce
- Scottish Universities Environmental Research Centre (SUERC), East Kilbride G75 0QF, UK
| | | | | | | | | | | | - David Sanderson
- Scottish Universities Environmental Research Centre (SUERC), East Kilbride G75 0QF, UK
| | - Alan Cresswell
- Scottish Universities Environmental Research Centre (SUERC), East Kilbride G75 0QF, UK
| | - Anthony J. T. Jull
- University of Arizona, Tucson, AZ 85721, USA
- Institute for Nuclear Research, Debrecen, Hungary
| | - Ivan Sýkora
- Comenius University, Bratislava 842 48, Slovakia
| | | | | | | | - Catherine S. Harrison
- Natural History Museum, London SW7 5BD, UK
- The University of Manchester, Manchester M13 9PL, UK
| | - Daniel Hallatt
- University of Kent, Canterbury CT2 7NH, UK
- Université de Lille, Lille 59000, France
| | | | | | | | | | | | - Caroline L. Smith
- Natural History Museum, London SW7 5BD, UK
- University of Glasgow, Glasgow G12 8QQ, UK
| | | | | | | | | | | | | | | | - Richard Kacerek
- UK Fireball Alliance (UKFAll), UK
- UK Meteor Observation Network (UKMON), UK
| | | | - Francois Colas
- Observatoire de Paris, Paris 75014, France
- Fireball Recovery and InterPlanetary Recovery (FRIPON), France
| | - Brigitte Zanda
- Fireball Recovery and InterPlanetary Recovery (FRIPON), France
- Muséum National d’Histoire Naturelle, Paris 75005, France
| | - Pierre Vernazza
- Fireball Recovery and InterPlanetary Recovery (FRIPON), France
- Aix-Marseille Université, Marseille 13007, France
| | - Sylvain Bouley
- Fireball Recovery and InterPlanetary Recovery (FRIPON), France
- Université Paris-Saclay, Orsay 91405, France
| | - Simon Jeanne
- Observatoire de Paris, Paris 75014, France
- Fireball Recovery and InterPlanetary Recovery (FRIPON), France
| | | | - Gareth S. Collins
- UK Fireball Alliance (UKFAll), UK
- Imperial College London, London SW7 2BP, UK
| | - John S. Young
- UK Fireball Network (UKFN), UK
- University of Cambridge, Cambridge CB2 3EQ, UK
| | - Clive Shaw
- UK Fireball Network (UKFN), UK
- University of Cambridge, Cambridge CB2 3EQ, UK
| | - Jana Horak
- System for Capture of Asteroid and Meteorite Paths (SCAMP), UK
- UK Fireball Alliance (UKFAll), UK
- Amgueddfa Cymru—National Museum Wales, Cardiff CF10 3NP, UK
| | - Dave Jones
- UK Meteor Observation Network (UKMON), UK
| | | | | | | | | | | | - Derek Robson
- UK Meteor Observation Network (UKMON), UK
- NEMETODE Network, UK
| | - Andrew R. D. Smedley
- System for Capture of Asteroid and Meteorite Paths (SCAMP), UK
- UK Fireball Alliance (UKFAll), UK
- The University of Manchester, Manchester M13 9PL, UK
| | | | - Richard Bassom
- UK Meteor Observation Network (UKMON), UK
- Global Meteor Network (GMN)
| | - Mark McIntyre
- UK Fireball Alliance (UKFAll), UK
- UK Meteor Observation Network (UKMON), UK
- Global Meteor Network (GMN)
| | | | | | | | | | - Sarah McMullan
- UK Fireball Alliance (UKFAll), UK
- UK Fireball Network (UKFN), UK
- Imperial College London, London SW7 2BP, UK
| | - Sarah J. Boazman
- European Space Research and Technology Centre (ESTEC), Keplerlaan 1, 2201 AZ Noordwijk, Netherlands
| | | | | | - Annemarie E. Pickersgill
- University of Glasgow, Glasgow G12 8QQ, UK
- Scottish Universities Environmental Research Centre (SUERC), East Kilbride G75 0QF, UK
| | | | | | | | | | | | - Ben Mayne
- Toucan Energy Ltd., London SE1 4PG, UK
| | | | - Dan Kirk
- Toucan Energy Ltd., London SE1 4PG, UK
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7
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Hopp T, Dauphas N, Abe Y, Aléon J, O'D Alexander CM, Amari S, Amelin Y, Bajo KI, Bizzarro M, Bouvier A, Carlson RW, Chaussidon M, Choi BG, Davis AM, Di Rocco T, Fujiya W, Fukai R, Gautam I, Haba MK, Hibiya Y, Hidaka H, Homma H, Hoppe P, Huss GR, Ichida K, Iizuka T, Ireland TR, Ishikawa A, Ito M, Itoh S, Kawasaki N, Kita NT, Kitajima K, Kleine T, Komatani S, Krot AN, Liu MC, Masuda Y, McKeegan KD, Morita M, Motomura K, Moynier F, Nakai I, Nagashima K, Nesvorný D, Nguyen A, Nittler L, Onose M, Pack A, Park C, Piani L, Qin L, Russell SS, Sakamoto N, Schönbächler M, Tafla L, Tang H, Terada K, Terada Y, Usui T, Wada S, Wadhwa M, Walker RJ, Yamashita K, Yin QZ, Yokoyama T, Yoneda S, Young ED, Yui H, Zhang AC, Nakamura T, Naraoka H, Noguchi T, Okazaki R, Sakamoto K, Yabuta H, Abe M, Miyazaki A, Nakato A, Nishimura M, Okada T, Yada T, Yogata K, Nakazawa S, Saiki T, Tanaka S, Terui F, Tsuda Y, Watanabe SI, Yoshikawa M, Tachibana S, Yurimoto H. Ryugu's nucleosynthetic heritage from the outskirts of the Solar System. SCIENCE ADVANCES 2022; 8:eadd8141. [PMID: 36264823 DOI: 10.1126/sciadv.add8141] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/16/2023]
Abstract
Little is known about the origin of the spectral diversity of asteroids and what it says about conditions in the protoplanetary disk. Here, we show that samples returned from Cb-type asteroid Ryugu have Fe isotopic anomalies indistinguishable from Ivuna-type (CI) chondrites, which are distinct from all other carbonaceous chondrites. Iron isotopes, therefore, demonstrate that Ryugu and CI chondrites formed in a reservoir that was different from the source regions of other carbonaceous asteroids. Growth and migration of the giant planets destabilized nearby planetesimals and ejected some inward to be implanted into the Main Belt. In this framework, most carbonaceous chondrites may have originated from regions around the birthplaces of Jupiter and Saturn, while the distinct isotopic composition of CI chondrites and Ryugu may reflect their formation further away in the disk, owing their presence in the inner Solar System to excitation by Uranus and Neptune.
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Affiliation(s)
- Timo Hopp
- Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Nicolas Dauphas
- Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Yoshinari Abe
- Graduate School of Engineering Materials Science and Engineering, Tokyo Denki University, Tokyo 120-8551, Japan
| | - Jérôme Aléon
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Sorbonne Université, Museum National d'Histoire Naturelle, CNRS UMR 7590, IRD, 75005 Paris, France
| | - Conel M O'D Alexander
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Sachiko Amari
- McDonnell Center for the Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, USA
- Geochemical Research Center, The University of Tokyo, Tokyo 113-0033, Japan
| | - Yuri Amelin
- Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, GD 510640, China
| | - Ken-Ichi Bajo
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Martin Bizzarro
- Centre for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Copenhagen K 1350, Denmark
| | - Audrey Bouvier
- Bayerisches Geoinstitut, Universität Bayreuth, Bayreuth 95447, Germany
| | - Richard W Carlson
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - Marc Chaussidon
- Université Paris Cité, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Byeon-Gak Choi
- Department of Earth Science Education, Seoul National University, Seoul 08826, Republic of Korea
| | - Andrew M Davis
- Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, IL 60637, USA
| | - Tommaso Di Rocco
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Wataru Fujiya
- Faculty of Science, Ibaraki University, Mito 310-8512, Japan
| | - Ryota Fukai
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Ikshu Gautam
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Makiko K Haba
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Yuki Hibiya
- Department of General Systems Studies, The University of Tokyo, Tokyo 153-0041, Japan
- Research Center for Advanced Science and Technology, The University of Tokyo, Tokyo 153-8904, Japan
| | - Hiroshi Hidaka
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Hisashi Homma
- Osaka Application Laboratory, SBUWDX, Rigaku Corporation, Osaka 569-1146, Japan
| | - Peter Hoppe
- Max Planck Institute for Chemistry, Mainz 55128, Germany
| | - Gary R Huss
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - Kiyohiro Ichida
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Tsuyoshi Iizuka
- Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - Trevor R Ireland
- School of Earth and Environmental Sciences, The University of Queensland, St. Lucia, QLD 4072, Australia
| | - Akira Ishikawa
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Motoo Ito
- Kochi Institute for Core Sample Research, JAMSTEC, Kochi 783-8502, Japan
| | - Shoichi Itoh
- Department of Earth and Planetary Sciences, Kyoto University, Kyoto 606-8502, Japan
| | - Noriyuki Kawasaki
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Noriko T Kita
- Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Kouki Kitajima
- Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Thorsten Kleine
- Max Planck Institute for Solar System Research, 37077 Göttingen, Germany
| | - Shintaro Komatani
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Alexander N Krot
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - Ming-Chang Liu
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
- Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
| | - Yuki Masuda
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Kevin D McKeegan
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Mayu Morita
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | | | - Frédéric Moynier
- Université Paris Cité, Institut de physique du globe de Paris, CNRS, 75005 Paris, France
| | - Izumi Nakai
- Thermal Analysis, Rigaku Corporation, Tokyo 196-8666, Japan
| | - Kazuhide Nagashima
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
| | - David Nesvorný
- Department of Space Studies, Southwest Research Institute, Boulder, CO 80302, USA
| | - Ann Nguyen
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
| | - Larry Nittler
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Morihiko Onose
- Analytical Technology Division, Horiba Techno Service Co. Ltd., Kyoto 601-8125, Japan
| | - Andreas Pack
- Faculty of Geosciences and Geography, University of Göttingen, Göttingen D-37077, Germany
| | - Changkun Park
- Division of Earth-System Sciences, Korea Polar Research Institute, Incheon 21990, Korea
| | - Laurette Piani
- Centre de Recherches Pétrographiques et Géochimiques, CNRS-Université de Lorraine, 54500 Nancy, France
| | - Liping Qin
- Deep Space Exploration Laboratory/CAS Key Laboratory of Crust-Mantle Materials and Environments, University of Science and Technology of China, Hefei 230026, China
| | - Sara S Russell
- Department of Earth Sciences, Natural History Museum, London SW7 5BD, UK
| | - Naoya Sakamoto
- Isotope Imaging Laboratory, Hokkaido University, Sapporo 001-0021, Japan
| | - Maria Schönbächler
- Institute for Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | - Lauren Tafla
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Haolan Tang
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
- University of Science and Technology of China, Hefei, China
| | - Kentaro Terada
- Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan
| | - Yasuko Terada
- Spectroscopy and Imaging Division, Japan Synchrotron Radiation Research Institute, Hyogo 679-5198, Japan
| | - Tomohiro Usui
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Sohei Wada
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
| | - Meenakshi Wadhwa
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Richard J Walker
- Department of Geology, University of Maryland, College Park, MD 20742, USA
| | - Katsuyuki Yamashita
- Graduate School of Natural Science and Technology, Okayama University, Okayama 700-8530, Japan
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California Davis, Davis, CA 95616, USA
| | - Tetsuya Yokoyama
- Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Tokyo 152-8551, Japan
| | - Shigekazu Yoneda
- Department Science and Engineering, National Museum of Nature and Science, Tsukuba 305-0005, Japan
| | - Edward D Young
- Department of Earth, Planetary, and Space Sciences, UCLA, Los Angeles, CA 90095, USA
| | - Hiroharu Yui
- Department of Chemistry, Tokyo University of Science, Tokyo 162-8601, Japan
| | - Ai-Cheng Zhang
- School of Earth Sciences and Engineering, Nanjing University, Nanjing 210023, China
| | - Tomoki Nakamura
- Department of Earth Science, Tohoku University, Sendai 980-8578, Japan
| | - Hiroshi Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Takaaki Noguchi
- Kochi Institute for Core Sample Research, JAMSTEC, Kochi 783-8502, Japan
| | - Ryuji Okazaki
- Department of Earth and Planetary Sciences, Kyushu University, Fukuoka 819-0395, Japan
| | - Kanako Sakamoto
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Hikaru Yabuta
- Earth and Planetary Systems Science Program, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - Masanao Abe
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Akiko Miyazaki
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Aiko Nakato
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Masahiro Nishimura
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Tatsuaki Okada
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Toru Yada
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Kasumi Yogata
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoru Nakazawa
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Takanao Saiki
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Satoshi Tanaka
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Fuyuto Terui
- Graduate School of Engineering, Kanagawa Institute of Technology, Atsugi 243-0292, Japan
| | - Yuichi Tsuda
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Sei-Ichiro Watanabe
- Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan
| | - Makoto Yoshikawa
- Institute of Space and Astronautical Science/JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan
| | - Shogo Tachibana
- UTokyo Organization for Planetary and Space Science, University of Tokyo, Tokyo 113-0033, Japan
| | - Hisayoshi Yurimoto
- Department of Natural History Sciences, Hokkaido University, Sapporo 001-0021, Japan
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8
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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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9
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Formation of Comets. UNIVERSE 2022. [DOI: 10.3390/universe8070381] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/04/2022]
Abstract
Questions regarding how primordial or pristine the comets of the solar system are have been an ongoing controversy. In this review, we describe comets’ physical evolution from dust and ice grains in the solar nebula to the contemporary small bodies in the outer solar system. This includes the phases of dust agglomeration, the formation of planetesimals, their thermal evolution and the outcomes of collisional processes. We use empirical evidence about comets, in particular from the Rosetta Mission to comet 67P/Churyumov–Gerasimenko, to draw conclusions about the possible thermal and collisional evolution of comets.
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10
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Sossi PA, Stotz IL, Jacobson SA, Morbidelli A, O’Neill HS. Stochastic accretion of the Earth. NATURE ASTRONOMY 2022; 6:951-960. [PMID: 35971330 PMCID: PMC7613298 DOI: 10.1038/s41550-022-01702-2] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 11/03/2021] [Accepted: 05/06/2022] [Indexed: 06/15/2023]
Abstract
Chondritic meteorites are thought to be representative of the material that formed the Earth. However, the Earth is depleted in volatile elements in a manner unlike that in any chondrite, and yet these elements retain chondritic isotope ratios. Here we use N-body simulations to show that the Earth did not form from chondrites, but rather by stochastic accretion of many precursor bodies whose variable compositions reflect the temperatures at which they formed. Earth's composition is reproduced when initial temperatures of planetesimal- to embryo-sized bodies are set by disk accretion rates of (1.08±0.17)×10-7 solar masses/yr, although they may be perturbed by 26Al heating on bodies formed at different times. Our model implies that a heliocentric gradient in composition was present in the protoplanetary disc and that planetesimals formed rapidly within ~1 Myr, in accord with radiometric volatile depletion ages of the Earth.
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Affiliation(s)
- Paolo A. Sossi
- Institute of Geochemistry and Petrology, ETH Zürich, CH-8092, Zürich, Switzerland
| | - Ingo L. Stotz
- Institut für Geophysik, Ludwig-Maximilians Universität Münich, Münich, Germany
| | - Seth A. Jacobson
- Department of Earth and Environmental Sciences, Michigan State University, East Lansing, MI 48824, USA
| | - 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
| | - Hugh St.C. O’Neill
- School of Earth, Atmosphere and Environment, Monash University, Melbourne, VIC 3800, Australia
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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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Brennan MC, Fischer RA, Nimmo F, O’Brien DP. Timing of Martian Core Formation from Models of Hf-W Evolution Coupled with N-body Simulations. GEOCHIMICA ET COSMOCHIMICA ACTA 2022; 316:295-308. [PMID: 34866645 PMCID: PMC8637548 DOI: 10.1016/j.gca.2021.09.022] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
Determining how and when Mars formed has been a long-standing challenge for planetary scientists. The size and orbit of Mars are difficult to reproduce in classical simulations of planetary accretion, and this has inspired models of inner solar system evolution that are tuned to produce Mars-like planets. However, such models are not always coupled to geochemical constraints. Analyses of Martian meteorites using the extinct hafnium-tungsten (Hf-W) radioisotopic system, which is sensitive to the timing of core formation, have indicated that the Martian core formed within a few million years of the start of the solar system itself. This has been interpreted to suggest that, unlike Earth's protracted accretion, Mars grew to its modern size very rapidly. These arguments, however, generally rely on simplified growth histories for Mars. Here, we combine likely accretionary histories from a large number of N-body simulations with calculations of metal-silicate partitioning and Hf-W isotopic evolution during core formation to constrain the range of conditions that could have produced Mars. We find that there is no strong correlation between the final masses or orbits of simulated Martian analogs and their 182W anomalies, and that it is readily possible to produce Mars-like Hf-W isotopic compositions for a variety of accretionary conditions. The Hf-W signature of Mars is very sensitive to the oxygen fugacity (fO2) of accreted material because the metal-silicate partitioning behavior of W is strongly dependent on redox conditions. The average fO2 of Martian building blocks must fall in the range of 1.3-1.6 log units below the iron-wüstite buffer to produce a Martian mantle with the observed Hf/W ratio. Other geochemical properties (such as sulfur content) also influence Martian 182W signatures, but the timing of accretion is a more important control. We find that while Mars must have accreted most of its mass within ~5 million years of solar system formation to reproduce the Hf-W isotopic constraints, it may have continued growing afterwards for over 50 million years. There is a high probability of simultaneously matching the orbit, mass, and Hf-W signature of Mars even in cases of prolonged accretion if giant impactor cores were poorly equilibrated and merged directly with the proto-Martian core.
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Affiliation(s)
- Matthew C. Brennan
- Department of Earth and Planetary Sciences, Harvard University (20 Oxford Street, Cambridge, MA 02138, USA)
| | - Rebecca A. Fischer
- Department of Earth and Planetary Sciences, Harvard University (20 Oxford Street, Cambridge, MA 02138, USA)
| | - Francis Nimmo
- Department of Earth and Planetary Sciences, University of California Santa Cruz (1156 High Street, Santa Cruz, CA 95064, USA)
| | - David P. O’Brien
- Planetary Science Institute (1700 East Fort Lowell, Tucson, AZ 85719-2395, USA)
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13
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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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14
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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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