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      • Record: found
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      On the origin and evolution of the asteroid Ryugu: A comprehensive geochemical perspective

      research-article
      Author(s): *1 , † , *1 , *1 , *1 , *1 , *1 , *1 , *1 , *1 , *1 , *1 , *1 , *1 , *1 , *1 , *2 , *3 , *4 , *3 , *3 , *5 , *3 , *3 , *3 , *6 , *3 , *6 , *3 , *3 , *3 , *3 , *5 , *3 , *6 , *5 , *7 , *3 , *6 , *3 , *3 , *3 , *3 , *3 , *8 , *3 , *3 , *8 , *9 , *10 , *9 , *3 , *3 , *11 , *12 , *3 , *3 , *4 , *3 , *3 , *7 , *9 , *13 , *3 , *14 , *15 , *3 , *3 , *16 , *3 , *13 , *13 , *3 , *17 , *3 , *18 , *3 , *8 , *11 , *3 , *3 , *19 , *3 , *7 , *3 , *3 , *8 , *3 , *3 , *3 , *4 , *20 , *5 , *21 , *3 , *22 , *3 , *7 , *7 , *3 , *3 , *3 , *3 , *3 , *3 , *4 , *11 , *3 , *16 , *3 , *5
      Publication date (Print):
      Journal: Proceedings of the Japan Academy. Series B, Physical and Biological Sciences
      Publisher: The Japan Academy
      Keywords: sample return, Hayabusa2, Ryugu, interstellar medium, protosolar nebula, comprehensive analysis

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          There is no author summary for this article yet. Authors can add summaries to their articles on ScienceOpen to make them more accessible to a non-specialist audience.

          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 δ 18O, Δ 17O, and ε 54Cr 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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          Interpretation of Raman spectra of disordered and amorphous carbon

          A. C. Ferrari, J. Robertson (2000)
          Physical Review B, 61(20), 14095-14107
          Article 0 comments Cited 2063 times – based on 0 reviews     Review now
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            Origin of the cataclysmic Late Heavy Bombardment period of the terrestrial planets.

            R. Gomes, H. Levison, K Tsiganis … (2005)
            The petrology record on the Moon suggests that a cataclysmic spike in the cratering rate occurred approximately 700 million years after the planets formed; this event is known as the Late Heavy Bombardment (LHB). Planetary formation theories cannot naturally account for an intense period of planetesimal bombardment so late in Solar System history. Several models have been proposed to explain a late impact spike, but none of them has been set within a self-consistent framework of Solar System evolution. Here we propose that the LHB was triggered by the rapid migration of the giant planets, which occurred after a long quiescent period. During this burst of migration, the planetesimal disk outside the orbits of the planets was destabilized, causing a sudden massive delivery of planetesimals to the inner Solar System. The asteroid belt was also strongly perturbed, with these objects supplying a significant fraction of the LHB impactors in accordance with recent geochemical evidence. Our model not only naturally explains the LHB, but also reproduces the observational constraints of the outer Solar System.
            Article 0 comments Cited 683 times – based on 0 reviews     Review now
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              Origin of the orbital architecture of the giant planets of the Solar System.

              K Tsiganis, R. Gomes, A MORBIDELLI … (2005)
              Planetary formation theories suggest that the giant planets formed on circular and coplanar orbits. The eccentricities of Jupiter, Saturn and Uranus, however, reach values of 6 per cent, 9 per cent and 8 per cent, respectively. In addition, the inclinations of the orbital planes of Saturn, Uranus and Neptune take maximum values of approximately 2 degrees with respect to the mean orbital plane of Jupiter. Existing models for the excitation of the eccentricity of extrasolar giant planets have not been successfully applied to the Solar System. Here we show that a planetary system with initial quasi-circular, coplanar orbits would have evolved to the current orbital configuration, provided that Jupiter and Saturn crossed their 1:2 orbital resonance. We show that this resonance crossing could have occurred as the giant planets migrated owing to their interaction with a disk of planetesimals. Our model reproduces all the important characteristics of the giant planets' orbits, namely their final semimajor axes, eccentricities and mutual inclinations.
              Article 0 comments Cited 632 times – based on 0 reviews     Review now
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                Author and article information

                Journal
                Journal ID (nlm-ta): Proc Jpn Acad Ser B Phys Biol Sci
                Journal ID (iso-abbrev): Proc Jpn Acad Ser B Phys Biol Sci
                Journal ID (publisher-id): PJAB
                Title: Proceedings of the Japan Academy. Series B, Physical and Biological Sciences
                Publisher: The Japan Academy (Tokyo, Japan )
                ISSN (Print): 0386-2208
                ISSN (Electronic): 1349-2896
                Publication date (Print): 10 June 2022
                Volume: 98
                Issue: 6
                Pages: 227-282
                Affiliations
                [*1 ]The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Tottori, Japan.
                [*2 ]Department of Information and Basic Science, Nagoya City University, Nagoya, Aichi, Japan.
                [*3 ]Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan.
                [*4 ]The Graduate University for Advanced Studies (SOKENDAI), Hayama, Kanagawa, Japan.
                [*5 ]Graduate School of Science, The University of Tokyo, Tokyo, Japan.
                [*6 ]Marine Works Japan, Ltd., Yokosuka, Kanagawa, Japan.
                [*7 ]Planetary Exploration Research Center (PERC), Chiba Institute of Technology, Narashino, Chiba, Japan.
                [*8 ]Graduate School of Science, Kobe University, Kobe, Hyogo, Japan.
                [*9 ]Faculty of Computer Science and Engineering, The University of Aizu, Aizu-Wakamatsu, Fukushima, Japan.
                [*10 ]Faculty of Science and Technology, Kochi University, Kochi, Japan.
                [*11 ]Research and Development Directorate, JAXA, Sagamihara, Kanagawa, Japan.
                [*12 ]Department of Physics and Astronomy, Seoul National University, Seoul, Korea.
                [*13 ]National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan.
                [*14 ]Observatoire de Paris, Meudon, France.
                [*15 ]Faculty of Engineering, Kindai University, Higashi-Hiroshima, Hiroshima, Japan.
                [*16 ]Graduate School of Environmental Studies, Nagoya University, Nagoya, Aichi, Japan.
                [*17 ]Faculty of Science, Niigata University, Niigata, Japan.
                [*18 ]JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan.
                [*19 ]College of Science, Rikkyo University, Tokyo, Japan.
                [*20 ]The University of Tokyo, Kashiwa, Chiba, Japan.
                [*21 ]Instituto de Astrofisica de Canarias, University of La Laguna, Tenerife, Spain.
                [*22 ]Faculty of Engineering, Kanagawa Institute of Technology, Atsugi, Kanagawa, Japan.
                Author notes
                [# ]

                the deceased.

                [⁑ ]

                Present address: Toyo University, Tokyo, Japan.

                [‡ ]

                Present address: Japan Patent Office, Tokyo, Japan.

                [† ]Correspondence should be addressed to: E. Nakamura, The Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, 827 Yamada, Misasa, Tottori 682-0193, Japan (e-mail: eizonak@ 123456gmail.com ).

                (Edited by Ikuo KUSHIRO, M.J.A.; Communicated by Yoshio FUKAO, M.J.A.)

                Article
                Publisher ID: pjab-98-227
                DOI: 10.2183/pjab.98.015
                PMC ID: 9246647
                PubMed ID: 35691845
                SO-VID: d755aacd-7352-43fb-8942-4be9352a577f
                Copyright © © 2022 The Author(s).
                License:

                Published under the terms of the CC BY-NC license https://creativecommons.org/licenses/by-nc/4.0/.

                History
                Date received : 31 January 2022
                Date accepted : 6 May 2022
                Categories
                Subject: Original Article

                ScienceOpen disciplines: Life sciences
                Keywords: sample return,hayabusa2,ryugu,interstellar medium,protosolar nebula,comprehensive analysis
                Data availability:
                ScienceOpen disciplines: Life sciences
                Keywords: sample return, hayabusa2, ryugu, interstellar medium, protosolar nebula, comprehensive analysis

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