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Ferreira GW, Samulewski RB, Ivashita FF, Paesano A, Urbano A, Zaia DAM. Did Salts in Seawater Play an Important Role in the Adsorption of Molecules on Minerals in the Prebiotic Earth? The Case of the Adsorption of Thiocyanate onto Forsterite-91. ORIGINS LIFE EVOL B 2023; 53:127-156. [PMID: 37676558 DOI: 10.1007/s11084-023-09640-3] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/28/2023] [Accepted: 08/09/2023] [Indexed: 09/08/2023]
Abstract
Thiocyanate may have played as important a role as cyanide in the synthesis of several molecules. However, its concentration in the seas of the prebiotic Earth could have been very low. Thiocyanate was dissolved in two different seawaters: a) a composition that comes close to the seawater of the prebiotic Earth (seawater-B, Ca2+ and Cl-) and b) a seawater (seawater-A, Mg2+ and SO42-) that could be related to the seas of Mars and other moons in the solar system. In addition, forsterite-91 was a very common mineral on the prebiotic Earth and Mars. Two important results are reported in this work: 1) thiocyanate adsorbed onto forsterite-91 and 2) the amount of thiocyanate adsorbed, adsorption thermodynamic, and adsorption kinetic depend on the composition of the artificial seawater. For all experiments, the adsorption was thermodynamically favorable (ΔG < 0). The adsorption data fitted well in the Freundlich and Langmuir-Freundlich models. When dissolving thiocyanate in seawater 4.0-A-Gy and seawater 4.0-B-Gy, the adsorption of thiocyanate onto forsterite-91 was ruled by enthalpy and entropy, respectively. As shown by n values, the thiocyanate/foraterite-91 system is heterogeneous. For all kinetic data, the pseudo-first-order model presented the best fit. The constant rate for thiocyanate dissolved in seawater 4.0-A-Gy was twice that compared to thiocyanate dissolved in seawater 4.0-B-Gy or ultrapure-water. The interaction between thiocyanate and Fe2+ of forsterite-91 was with the nitrogen atom of thiocyanate. In the presence of thiocyanate, sulfate interacts with forsterite-91 as an inner-sphere surface complex, and without thiocyanate as an outer-sphere surface complex.
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Affiliation(s)
- Giulio Wilgner Ferreira
- Laboratório de Química Prebiótica-LQP, Departamento de Química, Universidade Estadual de Londrina, CEP 86057-970, Londrina, PR, Brazil
| | - Rafael Block Samulewski
- COLIQ - Coordenação de Licenciatura em Química, Universidade Tecnológica Federal do Paraná UTFPR Campus Apucarana, CEP 86812-460, Apucarana, PR, Brazil.
| | | | - Andrea Paesano
- Departamento de Física-CCE, Universidade Estadual de Maringá, 87020-900, Maringá, PR, Brazil
- Departamento de Física Teórica e Experimental, UFRN, Av. Sen. Salgado Filho, 3000, Lagoa Nova, 59078-970, Natal, RN, Brazil
| | - Alexandre Urbano
- Departamento de Física-CCE, Universidade Estadual de Londrina, CEP 86057-970, Londrina, PR, Brazil
| | - Dimas Augusto Morozin Zaia
- Laboratório de Química Prebiótica-LQP, Departamento de Química, Universidade Estadual de Londrina, CEP 86057-970, Londrina, PR, Brazil.
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2
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Chan DH, Wills JL, Tandy JD, Burchell MJ, Wozniakiewicz PJ, Alesbrook LS, Armes SP. Synthesis of Autofluorescent Phenanthrene Microparticles via Emulsification: A Useful Synthetic Mimic for Polycyclic Aromatic Hydrocarbon-Based Cosmic Dust. ACS APPLIED MATERIALS & INTERFACES 2023; 15:54039-54049. [PMID: 37944021 PMCID: PMC10685351 DOI: 10.1021/acsami.3c08585] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/14/2023] [Revised: 10/19/2023] [Accepted: 10/24/2023] [Indexed: 11/12/2023]
Abstract
Phenanthrene is the simplest example of a polycyclic aromatic hydrocarbon (PAH). Herein, we exploit its relatively low melting point (101 °C) to prepare microparticles from molten phenanthrene droplets by conducting high-shear homogenization in a 3:1 water/ethylene glycol mixture at 105 °C using poly(N-vinylpyrrolidone) as a non-ionic polymeric emulsifier. Scanning electron microscopy studies confirm that this protocol produces polydisperse phenanthrene microparticles with a spherical morphology: laser diffraction studies indicate a volume-average diameter of 25 ± 21 μm. Such projectiles are fired into an aluminum foil target at 1.87 km s-1 using a two-stage light gas gun. Interestingly, the autofluorescence exhibited by phenanthrene aids analysis of the resulting impact craters. More specifically, it enables assessment of the spatial distribution of any surviving phenanthrene in the vicinity of each crater. Furthermore, these phenanthrene microparticles can be coated with an ultrathin overlayer of polypyrrole, which reduces their autofluorescence. In principle, such core-shell microparticles should be useful for assessing the extent of thermal ablation that is likely to occur when they are fired into aerogel targets. Accordingly, polypyrrole-coated microparticles were fired into an aerogel target at 2.07 km s-1. Intact microparticles were identified at the end of carrot tracks and their relatively weak autofluorescence suggests that thermal ablation during aerogel capture did not completely remove the polypyrrole overlayer. Thus, these new core-shell microparticles appear to be useful model projectiles for assessing the extent of thermal processing that can occur in such experiments, which have implications for the capture of intact PAH-based dust grains originating from cometary tails or from plumes emanating from icy satellites (e.g., Enceladus) in future space missions.
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Affiliation(s)
- Derek
H. H. Chan
- Dainton
Building, Department of Chemistry, University
of Sheffield, Brook Hill, Sheffield, South
Yorkshire S3 7HF, U.K.
| | - Jessica L. Wills
- School
of Physics and Astronomy, University of
Kent, Canterbury, Kent CT2 7NH, U.K.
| | - Jon D. Tandy
- School
of Chemistry and Forensic Science, University
of Kent, Canterbury, Kent CT2 7NZ, U.K.
| | - Mark J. Burchell
- School
of Physics and Astronomy, University of
Kent, Canterbury, Kent CT2 7NH, U.K.
| | | | - Luke S. Alesbrook
- School
of Physics and Astronomy, University of
Kent, Canterbury, Kent CT2 7NH, U.K.
| | - Steven P. Armes
- Dainton
Building, Department of Chemistry, University
of Sheffield, Brook Hill, Sheffield, South
Yorkshire S3 7HF, U.K.
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3
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Nolan KC, Weiland A, Lepper BT, Aultman J, Murphy LR, Ruby BJ, Schwarz K, Davidson M, Wymer D, Everhart TD, Krus AM, McCoy TJ. Refuting the sensational claim of a Hopewell-ending cosmic airburst. Sci Rep 2023; 13:12910. [PMID: 37558779 PMCID: PMC10412550 DOI: 10.1038/s41598-023-39866-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/18/2022] [Accepted: 08/01/2023] [Indexed: 08/11/2023] Open
Affiliation(s)
- Kevin C Nolan
- Applied Anthropology Laboratories, College of Sciences and Humanities, Ball State University, Muncie, USA.
| | - Andrew Weiland
- Midwest Archaeological Center, National Park Service, Lincoln, USA
| | | | | | - Laura R Murphy
- Department of Sociology and Anthropology, Washburn University, Topeka, USA
| | - Bret J Ruby
- Hopewell Culture National Historic Park, National Park Service, Chillicothe, USA
| | | | - Matthew Davidson
- Department of Anthropology, University of Kentucky, Lexington, USA
| | - DeeAnne Wymer
- Susquehanna River Archaeological Center, Waverly, USA
| | - Timothy D Everhart
- Hopewell Culture National Historic Park, National Park Service, Chillicothe, USA
| | - Anthony M Krus
- Department of Anthropology and Sociology, University of South Dakota, Vermillion, USA
| | - Timothy J McCoy
- Curator of Meteorites, Smithsonian National Museum of Natural History, Washington, USA
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4
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Oba Y, Takano Y, Dworkin JP, Naraoka H. Ryugu asteroid sample return provides a natural laboratory for primordial chemical evolution. Nat Commun 2023; 14:3107. [PMID: 37253735 DOI: 10.1038/s41467-023-38518-1] [Citation(s) in RCA: 2] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Grants] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/24/2023] [Accepted: 05/04/2023] [Indexed: 06/01/2023] Open
Affiliation(s)
- Yasuhiro Oba
- Institute of Low Temperature Science (ILTS), Hokkaido University, N19W8 Kita-ku, Sapporo, 060-0819, Japan.
| | - Yoshinori Takano
- Biogeochemistry Research Center (BGC), Japan Agency for Marine-Earth Science and Technology (JAMSTEC), Natsushima, Yokosuka, 237-0061, Japan.
| | - Jason P Dworkin
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD, 20771, USA
| | - Hiroshi Naraoka
- Department of Earth and Planetary Sciences, Kyushu University, 744 Motooka, Nishi-ku, Fukuoka, 819-0395, Japan
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5
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Hoppe P, Rubin M, Altwegg K. A Comparison of Presolar Isotopic Signatures in Laboratory-Studied Primitive Solar System Materials and Comet 67P/Churyumov-Gerasimenko: New Insights from Light Elements, Halogens, and Noble Gases. SPACE SCIENCE REVIEWS 2023; 219:32. [PMID: 37251606 PMCID: PMC10209250 DOI: 10.1007/s11214-023-00977-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 01/30/2023] [Accepted: 05/08/2023] [Indexed: 05/31/2023]
Abstract
Comets are considered the most primitive planetary bodies in our Solar System. ESA's Rosetta mission to Jupiter family comet 67P/Churyumov-Gerasimenko (67P/CG) has provided a wealth of isotope data which expanded the existing data sets on isotopic compositions of comets considerably. In a previous paper (Hoppe et al. in Space Sci. Rev. 214:106, 2018) we reviewed the results for comet 67P/CG from the first four years of data reduction after arrival of Rosetta at the comet in August 2014 and discussed them in the context of respective meteorite data. Since then important new isotope data of several elements, among them the biogenic elements H, C, N, and O, for comet 67P/CG, the Tagish Lake meteorite, and C-type asteroid Ryugu became available which provide new insights into the formation conditions of small planetary bodies in the Solar System's earliest history. To complement the picture on comet 67P/CG and its context to other primitive Solar System materials, especially meteorites, that emerged from our previous paper, we review here the isotopic compositions of H, C, and N in various volatile molecules, of O in water and a suite of other molecules, of the halogens Cl and Br, and of the noble gas Kr in comet 67P/CG. Furthermore, we also review the H isotope data obtained in the refractory organics of the dust grains collected in the coma of 67P/CG. These data are compared with the respective meteoritic and Ryugu data and spectroscopic observations of other comets and extra-solar environments; Cl, Br, and Kr data are also evaluated in the context of a potential late supernova contribution, as suggested by the Si- and S-isotopic data of 67P/CG.
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Affiliation(s)
- Peter Hoppe
- Max Planck Institute for Chemistry, Hahn-Meitner-Weg 1, 55128 Mainz, Germany
| | - Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Kathrin Altwegg
- Center for Space and Habitability, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
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6
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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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7
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Tracing the Primordial Chemical Life of Glycine: A Review from Quantum Chemical Simulations. Int J Mol Sci 2022; 23:ijms23084252. [PMID: 35457069 PMCID: PMC9030215 DOI: 10.3390/ijms23084252] [Citation(s) in RCA: 6] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/14/2022] [Revised: 04/08/2022] [Accepted: 04/09/2022] [Indexed: 12/28/2022] Open
Abstract
Glycine (Gly), NH2CH2COOH, is the simplest amino acid. Although it has not been directly detected in the interstellar gas-phase medium, it has been identified in comets and meteorites, and its synthesis in these environments has been simulated in terrestrial laboratory experiments. Likewise, condensation of Gly to form peptides in scenarios resembling those present in a primordial Earth has been demonstrated experimentally. Thus, Gly is a paradigmatic system for biomolecular building blocks to investigate how they can be synthesized in astrophysical environments, transported and delivered by fragments of asteroids (meteorites, once they land on Earth) and comets (interplanetary dust particles that land on Earth) to the primitive Earth, and there react to form biopolymers as a step towards the emergence of life. Quantum chemical investigations addressing these Gly-related events have been performed, providing fundamental atomic-scale information and quantitative energetic data. However, they are spread in the literature and difficult to harmonize in a consistent way due to different computational chemistry methodologies and model systems. This review aims to collect the work done so far to characterize, at a quantum mechanical level, the chemical life of Gly, i.e., from its synthesis in the interstellar medium up to its polymerization on Earth.
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8
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Yamagishi A, Hashimoto H, Yano H, Imai E, Tabata M, Higashide M, Okudaira K. Four-Year Operation of Tanpopo: Astrobiology Exposure and Micrometeoroid Capture Experiments on the JEM Exposed Facility of the International Space Station. ASTROBIOLOGY 2021; 21:1461-1472. [PMID: 34449271 DOI: 10.1089/ast.2020.2430] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
The Tanpopo experiment was the first Japanese astrobiology mission on board the International Space Station. It included exposure experiments of microbes and organic compounds as well as a capture experiment of hypervelocity impacting microparticles. We deployed three Exposure Panels, each consisting of 20 Exposure Units that contained microbes, organic compounds, an alanine UV dosimeter or an ionizing radiation dosimeter. The three Exposure Panels were situated on the zenith face of the Exposed Experiment Handrail Attachment Mechanism (ExHAM) that was pointing in zenith direction toward space, which was attached on a handrail of the Japanese Experiment Module (Kibo) Exposed Facility (JEM-EF) outside the International Space Station. The three Exposure Panels were one by one retrieved and returned to the ground after approximately 1, 2, and 3 years of exposure to the space environment. Capture Panels, each of which contained one or two blocks of amorphous silica aerogel, were exposed to collect hypervelocity impact microparticles. Possible captured particles may include micrometeoroids, human-made orbital debris, and natural terrestrial particles. Each year, Capture Panels containing from 11 to 12 aerogel blocks were attached to the three faces of the ExHAM (pointing to zenith, ram, and port); they remained in place for about 1 year and were then returned to the laboratory. This process was repeated three times, in total, during 2015-2018. Additional exposure of a Capture Panel facing ram was conducted between 2018 and 2019. Once the aerogel blocks were returned to the laboratory, they were encapsulated in dedicated transparent plastic cases and optically inspected by a specially designed microscopic system. Once located and recorded, hypervelocity impact signatures were excavated one by one and distributed for further detailed analyses. The apparatus, operation, and environmental factors of all the Tanpopo experiments are summarized in this article.
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Affiliation(s)
- Akihiko Yamagishi
- School of Life Sciences, Tokyo University of Pharmacy and Life Sciences, Hachioji, Tokyo, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa, Japan
| | - Hirofumi Hashimoto
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa, Japan
| | - Hajime Yano
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa, Japan
| | - Eiichi Imai
- Department of Bioengineering, Nagaoka University of Technology, Kamitomioka, Nagaoka, Niigata, Japan
| | - Makoto Tabata
- Department of Physics, Chiba University, Chiba, Japan
| | - Masumi Higashide
- Research and Development Directorate, Japan Aerospace Exploration Agency (JAXA), Chofu, Tokyo, Japan
| | - Kyoko Okudaira
- Aizu Research Center for Space Informatics (ARC-Space), The University of Aizu, Aizuwakamatsu, Fukushima, Japan
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9
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Yamagishi A, Yokobori SI, Kobayashi K, Mita H, Yabuta H, Tabata M, Higashide M, Yano H. Scientific Targets of Tanpopo: Astrobiology Exposure and Micrometeoroid Capture Experiments at the Japanese Experiment Module Exposed Facility of the International Space Station. ASTROBIOLOGY 2021; 21:1451-1460. [PMID: 34449275 DOI: 10.1089/ast.2020.2426] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
The Tanpopo experiment was the first Japanese astrobiology mission on board the Japanese Experiment Module Exposed Facility on the International Space Station (ISS). The experiments were designed to address two important astrobiological topics, panspermia and the chemical evolution process toward the generation of life. These experiments also tested low-density aerogel and monitored the microdebris environment around low Earth orbit. The following six subthemes were identified to address these goals: (1) Capture of microbes in space: Estimation of the upper limit of microbe density in low Earth orbit; (2) Exposure of microbes in space: Estimation of the survival time course of microbes in the space environment; (3) Capture of cosmic dust on the ISS and analysis of organics: Detection of the possible presence of organic compounds in cosmic dust; (4) Alteration of organic compounds in space environments: Evaluation of decomposition time courses of organic compounds in space; (5) Space verification of the Tanpopo hyper-low-density aerogel: Durability and particle-capturing capability of aerogel; (6) Monitoring of the number of space debris: Time-dependent change in space debris environment. Subthemes 1 and 2 address the panspermia hypothesis, whereas 3 and 4 address the chemical evolution. The last two subthemes contribute to space technology development. Some of the results have been published previously or are included in this issue. This article summarizes the current status of the Tanpopo experiments.
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Affiliation(s)
- Akihiko Yamagishi
- School of Life Sciences, Tokyo University of Pharmacy and Life Sciences, Hachioji, Tokyo, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa, Japan
| | - Shin-Ichi Yokobori
- School of Life Sciences, Tokyo University of Pharmacy and Life Sciences, Hachioji, Tokyo, Japan
| | - Kensei Kobayashi
- Department of Chemistry, Yokohama National University, Hodogayaku, Yokohama, Japan
| | - Hajime Mita
- Department of Life, Environment and Applied Chemistry, Faculty of Engineering, Fukuoka Institute of Technology, Higashiku, Fukuoka, Japan
| | - Hikaru Yabuta
- Department of Earth and Planetary Systems Science, Hiroshima University, Hiroshima, Japan
| | - Makoto Tabata
- Department of Physics, Chiba University, Chiba, Japan
| | - Masumi Higashide
- Research and Development Directorate, Japan Aerospace Exploration Agency, Chofu, Tokyo, Japan
| | - Hajime Yano
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa, Japan
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10
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Method for detecting and quantitating capture of organic molecules in hypervelocity impacts. MethodsX 2021; 8:101239. [PMID: 34434762 PMCID: PMC8374173 DOI: 10.1016/j.mex.2021.101239] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/11/2020] [Accepted: 01/18/2021] [Indexed: 11/26/2022] Open
Abstract
Enceladus is a prime candidate in the solar system for in-depth astrobiological studies searching for habitability and life because it has a liquid water ocean with significant organic content and ongoing cryovolcanic activity. The presence of ice plumes that jet up through fissures in the ice crust covering the sub-surface ocean, enables remote sampling and in-situ analysis via a fly-by mission. However, capture and transport of organic materials to organic analyzers presents distinctive challenges as it is unknown whether, and to what extent, organic molecules imbedded in ice particles can be captured and survive hypervelocity impacts. This manuscript provides a fluorescence microscopic method to parametrically determine the amount of an organic fluorescent tracer dye, Pacific Blue™ (PB) deposited on a metallic surface. This method can be used to measure the capture and survival outcomes of terrestrial hypervelocity impact experiments where an ice projectile labeled with Pacific Blue impacts a soft metal surface. This work is an important step in the advancement of instruments like the Enceladus Organic Analyzer for detecting biosignatures in an Enceladus plume fly-by mission. An apparatus consisting of a substrate humidification shroud coupled with an epifluorescence microscope with CCD detector is developed to measure the intensity of quantitatively deposited Pacific Blue droplets under controlled humidity. Calibration curves are produced that relate the integrated fluorescence intensity of humidified PB droplets on metal foils to the number of PB molecules deposited. To demonstrate the utility of this method, our calibrations are used to analyze and quantitate organic capture and survival (up to 11% capture efficiency) following ice particle impacts at a velocity of 1.7 km/s on an aluminum substrate.
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11
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Gaylor MO, Miro P, Vlaisavljevich B, Kondage AAS, Barge LM, Omran A, Videau P, Swenson VA, Leinen LJ, Fitch NW, Cole KL, Stone C, Drummond SM, Rageth K, Dewitt LR, González Henao S, Karanauskus V. Plausible Emergence and Self Assembly of a Primitive Phospholipid from Reduced Phosphorus on the Primordial Earth. ORIGINS LIFE EVOL B 2021; 51:185-213. [PMID: 34279769 DOI: 10.1007/s11084-021-09613-4] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/26/2021] [Accepted: 06/19/2021] [Indexed: 11/28/2022]
Abstract
How life arose on the primitive Earth is one of the biggest questions in science. Biomolecular emergence scenarios have proliferated in the literature but accounting for the ubiquity of oxidized (+ 5) phosphate (PO43-) in extant biochemistries has been challenging due to the dearth of phosphate and molecular oxygen on the primordial Earth. A compelling body of work suggests that exogenous schreibersite ((Fe,Ni)3P) was delivered to Earth via meteorite impacts during the Heavy Bombardment (ca. 4.1-3.8 Gya) and there converted to reduced P oxyanions (e.g., phosphite (HPO32-) and hypophosphite (H2PO2-)) and phosphonates. Inspired by this idea, we review the relevant literature to deduce a plausible reduced phospholipid analog of modern phosphatidylcholines that could have emerged in a primordial hydrothermal setting. A shallow alkaline lacustrine basin underlain by active hydrothermal fissures and meteoritic schreibersite-, clay-, and metal-enriched sediments is envisioned. The water column is laden with known and putative primordial hydrothermal reagents. Small system dimensions and thermal- and UV-driven evaporation further concentrate chemical precursors. We hypothesize that a reduced phospholipid arises from Fischer-Tropsch-type (FTT) production of a C8 alkanoic acid, which condenses with an organophosphinate (derived from schreibersite corrosion to hypophosphite with subsequent methylation/oxidation), to yield a reduced protophospholipid. This then condenses with an α-amino nitrile (derived from Strecker-type reactions) to form the polar head. Preliminary modeling results indicate that reduced phospholipids do not aggregate rapidly; however, single layer micelles are stable up to aggregates with approximately 100 molecules.
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Affiliation(s)
- Michael O Gaylor
- Department of Chemistry, Dakota State University, Madison, SD, 57042, USA.
| | - Pere Miro
- Department of Chemistry, University of South Dakota, Vermillion, SD, 57069, USA
| | - Bess Vlaisavljevich
- Department of Chemistry, University of South Dakota, Vermillion, SD, 57069, USA
| | | | - Laura M Barge
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, 91109, USA
| | - Arthur Omran
- School of Geosciences, University of South Florida, Tampa, FL, 33620, USA.,Department of Chemistry, University of North Florida, Jacksonville, FL, 32224, USA
| | - Patrick Videau
- Department of Biology, Southern Oregon University, Ashland, OR, 97520, USA.,Bayer Crop Science, Chesterfield, MO, 63017, USA
| | - Vaille A Swenson
- Department of Chemistry, Dakota State University, Madison, SD, 57042, USA.,Department of Molecular Medicine, Mayo Clinic, Rochester, MN, 55905, USA
| | - Lucas J Leinen
- Department of Chemistry, Dakota State University, Madison, SD, 57042, USA
| | - Nathaniel W Fitch
- Department of Chemistry, Dakota State University, Madison, SD, 57042, USA
| | - Krista L Cole
- Department of Chemistry, Dakota State University, Madison, SD, 57042, USA
| | - Chris Stone
- Department of Biology, Southern Oregon University, Ashland, OR, 97520, USA
| | - Samuel M Drummond
- Department of Chemistry, Dakota State University, Madison, SD, 57042, USA
| | - Kayli Rageth
- Department of Chemistry, Dakota State University, Madison, SD, 57042, USA
| | - Lillian R Dewitt
- Department of Chemistry, Dakota State University, Madison, SD, 57042, USA
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12
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Breakup of a long-period comet as the origin of the dinosaur extinction. Sci Rep 2021; 11:3803. [PMID: 33589634 PMCID: PMC7884440 DOI: 10.1038/s41598-021-82320-2] [Citation(s) in RCA: 9] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/25/2020] [Accepted: 01/18/2021] [Indexed: 11/08/2022] Open
Abstract
The origin of the Chicxulub impactor, which is attributed as the cause of the K/T mass extinction event, is an unsolved puzzle. The background impact rates of main-belt asteroids and long-period comets have been previously dismissed as being too low to explain the Chicxulub impact event. Here, we show that a fraction of long-period comets are tidally disrupted after passing close to the Sun, each producing a collection of smaller fragments that cross the orbit of Earth. This population could increase the impact rate of long-period comets capable of producing Chicxulub impact events by an order of magnitude. This new rate would be consistent with the age of the Chicxulub impact crater, thereby providing a satisfactory explanation for the origin of the impactor. Our hypothesis explains the composition of the largest confirmed impact crater in Earth's history as well as the largest one within the last million years. It predicts a larger proportion of impactors with carbonaceous chondritic compositions than would be expected from meteorite falls of main-belt asteroids.
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13
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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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14
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Hu JY, Dauphas N, Tissot FLH, Yokochi R, Ireland TJ, Zhang Z, Davis AM, Ciesla FJ, Grossman L, Charlier BLA, Roskosz M, Alp EE, Hu MY, Zhao J. Heating events in the nascent solar system recorded by rare earth element isotopic fractionation in refractory inclusions. SCIENCE ADVANCES 2021; 7:7/2/eabc2962. [PMID: 33523962 PMCID: PMC7787488 DOI: 10.1126/sciadv.abc2962] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/16/2020] [Accepted: 11/16/2020] [Indexed: 05/31/2023]
Abstract
Equilibrium condensation of solar gas is often invoked to explain the abundance of refractory elements in planets and meteorites. This is partly motivated, by the observation that the depletions in both the least and most refractory rare earth elements (REEs) in meteoritic group II calcium-aluminum-rich inclusions (CAIs) can be reproduced by thermodynamic models of solar nebula condensation. We measured the isotopic compositions of Ce, Nd, Sm, Eu, Gd, Dy, Er, and Yb in eight CAIs to test this scenario. Contrary to expectation for equilibrium condensation, we find light isotope enrichment for the most refractory REEs and more subdued isotopic variations for the least refractory REEs. This suggests that group II CAIs formed by a two-stage process involving fast evaporation of preexisting materials, followed by near-equilibrium recondensation. The calculated time scales are consistent with heating in events akin to FU Orionis- or EX Lupi-type outbursts of eruptive pre-main-sequence stars.
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Affiliation(s)
- J Y Hu
- Origins Laboratory, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA.
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - N Dauphas
- Origins Laboratory, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - F L H Tissot
- Origins Laboratory, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
- The Isotoparium, Division of Geological and Planetary Sciences, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USA
| | - R Yokochi
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - T J Ireland
- Origins Laboratory, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
- Department of Earth and Environment, Boston University, 685 Commonwealth Avenue, Boston, MA 02215, USA
| | - Z Zhang
- Origins Laboratory, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - A M Davis
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - F J Ciesla
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - L Grossman
- Department of the Geophysical Sciences, Enrico Fermi Institute, Chicago Center for Cosmochemistry, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA
| | - B L A Charlier
- School of Geography, Earth and Environmental Sciences, Victoria University of Wellington, Wellington 6140, New Zealand
| | - M Roskosz
- IMPMC, CNRS, UMR 7590, Sorbonne Universités, Université Pierre et Marie Curie, Muséum National d'Histoire Naturelle, CP 52, 57 rue Cuvier, Paris F-75231, France
| | - E E Alp
- Advanced Photon Source, Argonne National Laboratory, 9700 South Cass Avenue, Argonne, IL 60439, USA
| | - M Y Hu
- Advanced Photon Source, Argonne National Laboratory, 9700 South Cass Avenue, Argonne, IL 60439, USA
| | - J Zhao
- Advanced Photon Source, Argonne National Laboratory, 9700 South Cass Avenue, Argonne, IL 60439, USA
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15
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Zellner NEB, McCaffrey VP, Butler JHE. Cometary Glycolaldehyde as a Source of pre-RNA Molecules. ASTROBIOLOGY 2020; 20:1377-1388. [PMID: 32985898 DOI: 10.1089/ast.2020.2216] [Citation(s) in RCA: 11] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/11/2023]
Abstract
Over 200 molecules have been detected in multiple extraterrestrial environments, including glycolaldehyde (C2(H2O)2, GLA), a two-carbon sugar precursor that has been detected in regions of the interstellar medium. Its recent in situ detection on the nucleus of comet 67P/Churyumov-Gerasimenko and through remote observations in the comae of others provides tantalizing evidence that it is common on most (if not all) comets. Impact experiments conducted at the Experimental Impact Laboratory at NASA's Johnson Space Center have shown that samples of GLA and GLA mixed with montmorillonite clays can survive impact delivery in the pressure range of 4.5 to 25 GPa. Extrapolated to amounts of GLA observed on individual comets and assuming a monotonic impact rate in the first billion years of Solar System history, these experimental results show that up to 1023 kg of cometary GLA could have survived impact delivery, with substantial amounts of threose, erythrose, glycolic acid, and ethylene glycol also produced or delivered. Importantly, independent of the profile of the impact flux in the early Solar System, comet delivery of GLA would have provided (and may continue to provide) a reservoir of starting material for the formose reaction (to form ribose) and the Strecker reaction (to form amino acids). Thus, comets may have been important delivery vehicles for starting molecules necessary for life as we know it.
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Affiliation(s)
| | | | - Jayden H E Butler
- Department of Physics, Albion College, Albion, Michigan, USA
- Department of Physics, California State University - Los Angeles, Los Angeles, California, USA
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16
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Rubin M, Engrand C, Snodgrass C, Weissman P, Altwegg K, Busemann H, Morbidelli A, Mumma M. On the Origin and Evolution of the Material in 67P/Churyumov-Gerasimenko. SPACE SCIENCE REVIEWS 2020; 216:102. [PMID: 32801398 PMCID: PMC7392949 DOI: 10.1007/s11214-020-00718-2] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/09/2019] [Accepted: 07/03/2020] [Indexed: 06/02/2023]
Abstract
Primitive objects like comets hold important information on the material that formed our solar system. Several comets have been visited by spacecraft and many more have been observed through Earth- and space-based telescopes. Still our understanding remains limited. Molecular abundances in comets have been shown to be similar to interstellar ices and thus indicate that common processes and conditions were involved in their formation. The samples returned by the Stardust mission to comet Wild 2 showed that the bulk refractory material was processed by high temperatures in the vicinity of the early sun. The recent Rosetta mission acquired a wealth of new data on the composition of comet 67P/Churyumov-Gerasimenko (hereafter 67P/C-G) and complemented earlier observations of other comets. The isotopic, elemental, and molecular abundances of the volatile, semi-volatile, and refractory phases brought many new insights into the origin and processing of the incorporated material. The emerging picture after Rosetta is that at least part of the volatile material was formed before the solar system and that cometary nuclei agglomerated over a wide range of heliocentric distances, different from where they are found today. Deviations from bulk solar system abundances indicate that the material was not fully homogenized at the location of comet formation, despite the radial mixing implied by the Stardust results. Post-formation evolution of the material might play an important role, which further complicates the picture. This paper discusses these major findings of the Rosetta mission with respect to the origin of the material and puts them in the context of what we know from other comets and solar system objects.
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Affiliation(s)
- Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Cécile Engrand
- CNRS/IN2P3, IJCLab, Université Paris-Saclay, 91405 Orsay Cedex, France
| | - Colin Snodgrass
- Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9 3HJ UK
| | | | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Henner Busemann
- Institute of Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | | | - Michael Mumma
- NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, 20771 MD USA
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17
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Potapov A, Jäger C, Henning T. Ice Coverage of Dust Grains in Cold Astrophysical Environments. PHYSICAL REVIEW LETTERS 2020; 124:221103. [PMID: 32567895 DOI: 10.1103/physrevlett.124.221103] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/24/2020] [Revised: 04/14/2020] [Accepted: 05/01/2020] [Indexed: 06/11/2023]
Abstract
Surface processes on cosmic solids in cold astrophysical environments lead to gas-phase depletion and molecular complexity. Most astrophysical models assume that the molecular ice forms a thick multilayer substrate, not interacting with the dust surface. In contrast, we present experimental results demonstrating the importance of the surface for porous grains. We show that cosmic dust grains may be covered by a few monolayers of ice only. This implies that the role of dust surface structure, composition, and reactivity in models describing surface processes in cold interstellar, protostellar, and protoplanetary environments has to be reevaluated.
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Affiliation(s)
- Alexey Potapov
- Laboratory Astrophysics Group of the Max Planck Institute for Astronomy at the Friedrich Schiller University Jena, Institute of Solid State Physics, Helmholtzweg 3, 07743 Jena, Germany
| | - Cornelia Jäger
- Laboratory Astrophysics Group of the Max Planck Institute for Astronomy at the Friedrich Schiller University Jena, Institute of Solid State Physics, Helmholtzweg 3, 07743 Jena, Germany
| | - Thomas Henning
- Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
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18
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Chan QHS, Stroud R, Martins Z, Yabuta H. Concerns of Organic Contamination for Sample Return Space Missions. SPACE SCIENCE REVIEWS 2020; 216:56. [PMID: 32624626 PMCID: PMC7319412 DOI: 10.1007/s11214-020-00678-7] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 06/27/2019] [Accepted: 04/23/2020] [Indexed: 06/11/2023]
Abstract
Analysis of organic matter has been one of the major motivations behind solar system exploration missions. It addresses questions related to the organic inventory of our solar system and its implication for the origin of life on Earth. Sample return missions aim at returning scientifically valuable samples from target celestial bodies to Earth. By analysing the samples with the use of state-of-the-art analytical techniques in laboratories here on Earth, researchers can address extremely complicated aspects of extra-terrestrial organic matter. This level of detailed sample characterisation provides the range and depth in organic analysis that are restricted in spacecraft-based exploration missions, due to the limitations of the on-board in-situ instrumentation capabilities. So far, there are four completed and in-process sample return missions with an explicit mandate to collect organic matter: Stardust and OSIRIS-REx missions of NASA, and Hayabusa and Hayabusa2 missions of JAXA. Regardless of the target body, all sample return missions dedicate to minimise terrestrial organic contamination of the returned samples, by applying various degrees or strategies of organic contamination mitigation methods. Despite the dedicated efforts in the design and execution of contamination control, it is impossible to completely eliminate sources of organic contamination. This paper aims at providing an overview of the successes and lessons learned with regards to the identification of indigenous organic matter of the returned samples vs terrestrial contamination.
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Affiliation(s)
- Queenie Hoi Shan Chan
- Planetary and Space Sciences, School of Physical Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA UK
- Present Address: Department of Earth Sciences, Royal Holloway University of London, Egham Surrey, TW20 0EX UK
| | - Rhonda Stroud
- Code 6360, Naval Research Laboratory, Washington, DC 20375 USA
| | - Zita Martins
- Centro de Química Estrutural, Departamento de Engenharia Química, Instituto Superior Técnico (IST), Universidade de Lisboa, Avenida Rovisco Pais 1, 1049-001 Lisbon, Portugal
| | - Hikaru Yabuta
- Department of Earth and Planetary Systems Science, Hiroshima University, 1-3-1 Kagamiyama, Hiroshima, 739-8526 Japan
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19
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Larsen K, Wielandta D, Schillera M, Krot A, Bizzarro M. Episodic formation of refractory inclusions in the Solar System and their presolar heritage. EARTH AND PLANETARY SCIENCE LETTERS 2020; 535:116088. [PMID: 34334802 PMCID: PMC7611424 DOI: 10.1016/j.epsl.2020.116088] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
Refractory inclusions [Ca-Al-rich Inclusions (CAIs) and Amoeboid Olivine Aggregates (AOAs)] in primitive meteorites are the oldest Solar System solids. They formed in the hot inner protoplanetary disk and, as such, provide insights into the earliest disk dynamics and physicochemical processing of the dust and gas that accreted to form the Sun and its planetary system. Using the short-lived 26Al to 26Mg decay system, we show that bulk refractory inclusions in CV (Vigarano-type) and CR (Renazzo-type) carbonaceous chondrites captured at least two distinct 26Al-rich (26Al/27Al ratios of ~5 × 10-5) populations of refractory inclusions characterized by different initial 26Mg/24Mg isotope compositions (μ26Mg*0). Another 26Al-poor CAI records an even larger μ26Mg*0 deficit. This suggests that formation of refractory inclusions was punctuated and recurrent, possibly associated with episodic outbursts from the accreting proto-Sun lasting as short as <8000 yr. Our results support a model in which refractory inclusions formed close to the hot proto-Sun and were subsequently redistributed to the outer disk, beyond the orbit of Jupiter, plausibly via stellar outflows with progressively decreasing transport efficiency. We show that the magnesium isotope signatures in refractory inclusions mirrors the presolar grain record, demonstrating a mutual exclusivity between 26Al enrichments and large nucleosynthetic Mg isotope effects. This suggests that refractory inclusions formed by incomplete thermal processing of presolar dust, thereby inheriting a diluted signature of their isotope systematics. As such, they record snapshots in the progressive sublimation of isotopically anomalous presolar carriers through selective thermal processing of young dust components from the proto-Solar molecular cloud. We infer that 26Al-rich refractory inclusions incorporated 26Al-rich dust which formed <5 Myr prior to our Sun, whereas 26Al-poor inclusions (such as FUN- and PLAC-type CAIs) incorporated >10 Myr old dust.
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Affiliation(s)
- K.K. Larsen
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
| | - D. Wielandta
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
| | - M. Schillera
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
| | - A.N. Krot
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
- Hawai’i Institute of Geophysics and Planetology, University of Hawai’i at Manoa, HI 96822, USA
| | - M. Bizzarro
- Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Copenhagen DK-1350, Denmark
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20
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New JS, Mathies RA, Price MC, Cole MJ, Golozar M, Spathis V, Burchell MJ, Butterworth AL. Characterizing organic particle impacts on inert metal surfaces: Foundations for capturing organic molecules during hypervelocity transits of Enceladus plumes. METEORITICS & PLANETARY SCIENCE 2020; 55:465-479. [PMID: 32362737 PMCID: PMC7188319 DOI: 10.1111/maps.13448] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/18/2019] [Accepted: 01/08/2020] [Indexed: 05/23/2023]
Abstract
The presence and accessibility of a sub-ice-surface saline ocean at Enceladus, together with geothermal activity and a rocky core, make it a compelling location to conduct further, in-depth, astrobiological investigations to probe for organic molecules indicative of extraterrestrial life. Cryovolcanic plumes in the south polar region of Enceladus enable the use of remote in situ sampling and analysis techniques. However, efficient plume sampling and the transportation of captured organic materials to an organic analyzer present unique challenges for an Enceladus mission. A systematic study, accelerating organic ice-particle simulants into soft inert metal targets at velocities ranging 0.5-3.0 km s-1, was carried out using a light gas gun to explore the efficacy of a plume capture instrument. Capture efficiency varied for different metal targets as a function of impact velocity and particle size. Importantly, organic chemical compounds remained chemically intact in particles captured at speeds up to ~2 km s-1. Calibration plots relating the velocity, crater, and particle diameter were established to facilitate future ice-particle impact experiments where the size of individual ice particles is unknown.
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Affiliation(s)
- J. S. New
- Space Sciences LaboratoryUniversity of CaliforniaBerkeley7 Gauss WayBerkeleyCalifornia94720USA
- School of Physical SciencesUniversity of KentCanterburyKentCT2 7NHUK
| | - R. A. Mathies
- Space Sciences LaboratoryUniversity of CaliforniaBerkeley7 Gauss WayBerkeleyCalifornia94720USA
- Department of ChemistryUniversity of CaliforniaBerkeleyCalifornia94720USA
| | - M. C. Price
- School of Physical SciencesUniversity of KentCanterburyKentCT2 7NHUK
| | - M. J. Cole
- School of Physical SciencesUniversity of KentCanterburyKentCT2 7NHUK
| | - M. Golozar
- Space Sciences LaboratoryUniversity of CaliforniaBerkeley7 Gauss WayBerkeleyCalifornia94720USA
- Department of ChemistryUniversity of CaliforniaBerkeleyCalifornia94720USA
| | - V. Spathis
- School of Physical SciencesUniversity of KentCanterburyKentCT2 7NHUK
| | - M. J. Burchell
- School of Physical SciencesUniversity of KentCanterburyKentCT2 7NHUK
| | - A. L. Butterworth
- Space Sciences LaboratoryUniversity of CaliforniaBerkeley7 Gauss WayBerkeleyCalifornia94720USA
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21
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Rubin M, Engrand C, Snodgrass C, Weissman P, Altwegg K, Busemann H, Morbidelli A, Mumma M. On the Origin and Evolution of the Material in 67P/Churyumov-Gerasimenko. SPACE SCIENCE REVIEWS 2020. [PMID: 32801398 DOI: 10.1007/s11214-019-0625-7] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/15/2023]
Abstract
Primitive objects like comets hold important information on the material that formed our solar system. Several comets have been visited by spacecraft and many more have been observed through Earth- and space-based telescopes. Still our understanding remains limited. Molecular abundances in comets have been shown to be similar to interstellar ices and thus indicate that common processes and conditions were involved in their formation. The samples returned by the Stardust mission to comet Wild 2 showed that the bulk refractory material was processed by high temperatures in the vicinity of the early sun. The recent Rosetta mission acquired a wealth of new data on the composition of comet 67P/Churyumov-Gerasimenko (hereafter 67P/C-G) and complemented earlier observations of other comets. The isotopic, elemental, and molecular abundances of the volatile, semi-volatile, and refractory phases brought many new insights into the origin and processing of the incorporated material. The emerging picture after Rosetta is that at least part of the volatile material was formed before the solar system and that cometary nuclei agglomerated over a wide range of heliocentric distances, different from where they are found today. Deviations from bulk solar system abundances indicate that the material was not fully homogenized at the location of comet formation, despite the radial mixing implied by the Stardust results. Post-formation evolution of the material might play an important role, which further complicates the picture. This paper discusses these major findings of the Rosetta mission with respect to the origin of the material and puts them in the context of what we know from other comets and solar system objects.
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Affiliation(s)
- Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Cécile Engrand
- CNRS/IN2P3, IJCLab, Université Paris-Saclay, 91405 Orsay Cedex, France
| | - Colin Snodgrass
- Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9 3HJ UK
| | | | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Henner Busemann
- Institute of Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | | | - Michael Mumma
- NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, 20771 MD USA
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22
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Glavin DP, Burton AS, Elsila JE, Aponte JC, Dworkin JP. The Search for Chiral Asymmetry as a Potential Biosignature in our Solar System. Chem Rev 2019; 120:4660-4689. [DOI: 10.1021/acs.chemrev.9b00474] [Citation(s) in RCA: 88] [Impact Index Per Article: 17.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/07/2023]
Affiliation(s)
- Daniel P. Glavin
- NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, United States
| | - Aaron S. Burton
- NASA Johnson Space Center, Houston, Texas 77058, United States
| | - Jamie E. Elsila
- NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, United States
| | - José C. Aponte
- NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, United States
- Catholic University of America, Washington, D.C. 20064, United States
| | - Jason P. Dworkin
- NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, United States
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23
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COHEN BA, SZALAY JR, RIVKIN AS, RICHARDSON JA, KLIMA RL, ERNST CM, CHABOT NL, STERNOVSKY Z, HORÁNYI M. Using dust shed from asteroids as microsamples to link remote measurements with meteorite classes. METEORITICS & PLANETARY SCIENCE 2019; 54:2046-2066. [PMID: 32256026 PMCID: PMC7120990 DOI: 10.1111/maps.13348] [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: 07/30/2018] [Accepted: 05/30/2019] [Indexed: 06/11/2023]
Abstract
Given the compositional diversity of asteroids, and their distribution in space, it is impossible to consider returning samples from each one to establish their origin. However, the velocity and molecular composition of primary minerals, hydrated silicates, and organic materials can be determined by in situ dust detector instruments. Such instruments could sample the cloud of micrometer-scale particles shed by asteroids to provide direct links to known meteorite groups without returning the samples to terrestrial laboratories. We extend models of the measured lunar dust cloud from LADEE to show that the abundance of detectable impact-generated microsamples around asteroids is a function of the parent body radius, heliocentric distance, flyby distance, and speed. We use Monte Carlo modeling to show that several tens to hundreds of particles, if randomly ejected and detected during a flyby, would be a sufficient number to classify the parent body as an ordinary chondrite, basaltic achondrite, or other class of meteorite. Encountering and measuring microsamples shed from near-Earth and Main Belt asteroids, coupled with complementary imaging and multispectral measurements, could accomplish a thorough characterization of small, airless bodies.
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Affiliation(s)
- B. A. COHEN
- NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA
| | - J. R. SZALAY
- Princeton University, Princeton, New Jersey 08544, USA
| | - A. S. RIVKIN
- Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland 20723, USA
| | - J. A. RICHARDSON
- NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA
| | - R. L. KLIMA
- Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland 20723, USA
| | - C. M. ERNST
- Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland 20723, USA
| | - N. L. CHABOT
- Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland 20723, USA
| | - Z. STERNOVSKY
- LASP, University of Colorado, Boulder, Colorado 80303, USA
- Smead Aerospace Sciences, University of Colorado, Boulder, Colorado 80309, USA
| | - M. HORÁNYI
- LASP, University of Colorado, Boulder, Colorado 80303, USA
- Physics Department, University of Colorado, Boulder, Colorado 80309, USA
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24
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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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25
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Gainsforth Z, Westphal AJ, Butterworth AL, Jilly-Rehak CE, Brownlee DE, Joswiak D, Ogliore RC, Zolensky ME, Bechtel HA, Ebel DS, Huss GR, Sandford SA, White AJ. Fine-grained Material Associated with a Large Sulfide returned from Comet 81P/Wild 2. METEORITICS & PLANETARY SCIENCE 2019; 54:1069-1091. [PMID: 31080342 PMCID: PMC6505703 DOI: 10.1111/maps.13265] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/25/2018] [Accepted: 01/27/2019] [Indexed: 06/09/2023]
Abstract
In a consortium analysis of a large particle captured from the coma of comet 81P/Wild 2 by the Stardust spacecraft, we report the discovery of a field of fine-grained material (FGM) in contact with a large sulfide particle. The FGM was partially located in an embayment in the sulfide. As a consequence, some of the FGM appears to have been protected from damage during hypervelocity capture in aerogel. Some of the FGM particles are indistinguishable in their characteristics from common components of chondritic-porous interplanetary dust particles (CP-IDPs), including glass with embedded metals and sulfides (GEMS) and equilibrated aggregates (EAs). The sulfide exhibits surprising Ni-rich lamellae, which may indicate that this particle experienced a long-duration heating event after its formation but before incorporation into Wild 2.
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Affiliation(s)
- Z. Gainsforth
- Space Sciences Laboratory, University of California, Berkeley, CA 94720
| | - A. J. Westphal
- Space Sciences Laboratory, University of California, Berkeley, CA 94720
| | - A. L. Butterworth
- Space Sciences Laboratory, University of California, Berkeley, CA 94720
| | - C. E. Jilly-Rehak
- Space Sciences Laboratory, University of California, Berkeley, CA 94720
| | - D. E. Brownlee
- Dept. of Astronomy, University of Washington, Seattle, WA 98195
| | - D. Joswiak
- Dept. of Astronomy, University of Washington, Seattle, WA 98195
| | - R. C. Ogliore
- Department of Physics, Washington University in St. Louis, St. Louis, MO, 63117
| | | | - H. A. Bechtel
- Advanced Light Source, Lawrence Berkeley Laboratory, Berkeley, CA 94720
| | - D. S. Ebel
- Dept. Earth Planet. Sci., American Museum Natural History, NY, NY 10024
| | - G. R. Huss
- University of Hawai’i at Manoa, Honolulu, HI 96822
| | | | - A. J. White
- Dept. Astro. and Planet. Sci., University of Colorado, Boulder, CO 80309
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26
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Electrochirogenesis: The Possible Role of Low-Energy Spin-Polarized Electrons in Creating Homochirality. Symmetry (Basel) 2019. [DOI: 10.3390/sym11040528] [Citation(s) in RCA: 10] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/01/2023] Open
Abstract
Electrochirogenesis deals with the induction of chirality by polarized electrons of which those with low energy (<15 eV) are seen to be the most effective. Possible sources of such electrons in the prebiotic universe are discussed and several examples where chiral induction by these electrons have been demonstrated are given. Finally, some possible scenarios where electrochirogenesis could have played a role in forming a chiral imbalance in a prebiotic setting have been speculated on and some possible future areas of research proposed.
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27
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Ishii HA. Comparison of GEMS in Interplanetary Dust Particles and GEMS-like Objects in a Stardust Impact Track in Aerogel. METEORITICS & PLANETARY SCIENCE 2019; 54:202-219. [PMID: 30713419 PMCID: PMC6350812 DOI: 10.1111/maps.13182] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/25/2018] [Accepted: 07/06/2018] [Indexed: 06/09/2023]
Abstract
Comet 81P/Wild 2 dust, the first comet sample of known provenance, was widely expected to resemble anhydrous chondritic porous (CP) interplanetary dust particles (IDPs). GEMS, distinctly characteristic of CP IDPs, have yet to be unambiguously identified in the Stardust mission samples despite claims of likely candidates. One such candidate is Stardust impact track 57 "Febo" in aerogel, which contains fine-grained objects texturally and compositionally similar to GEMS. Their position adjacent the terminal particle suggests that they may be indigenous, fine-grained, cometary material, like that in CP IDPs, shielded by the terminal particle from damage during deceleration from hypervelocity. Darkfield imaging and multi-detector energy-dispersive x-ray mapping were used to compare GEMS-like-objects in the Febo terminal particle with GEMS in an anhydrous, chondritic IDP. GEMS in the IDP are within 3× CI (solar) abundances for major and minor elements. In the Febo GEMS-like objects, Mg and Ca are systematically and strongly depleted relative to CI; S and Fe are somewhat enriched; and Au, a known aerogel contaminant is present, consistent with ablation, melting, abrasion and mixing of the SiOx aerogel with crystalline Fe-sulfide and minor enstatite, high-Ni sulfide and augite identified by elemental mapping in the terminal particle. Thus, GEMS-like objects in "caches" of fine-grained debris abutting terminal particles are most likely deceleration debris packed in place during particle transit through the aerogel.
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Affiliation(s)
- Hope A Ishii
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA
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28
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Hoppe P, Rubin M, Altwegg K. Presolar Isotopic Signatures in Meteorites and Comets: New Insights from the Rosetta Mission to Comet 67P/Churyumov-Gerasimenko. SPACE SCIENCE REVIEWS 2018; 214:106. [PMID: 37265997 PMCID: PMC10229468 DOI: 10.1007/s11214-018-0540-3] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/28/2017] [Accepted: 08/20/2018] [Indexed: 06/01/2023]
Abstract
Comets are considered the most primitive planetary bodies in our Solar System, i.e., they should have best preserved the solid components of the matter from which our Solar System formed. ESA's recent Rosetta mission to Jupiter family comet 67P/Churyumov-Gerasimenko (67P/CG) has provided a wealth of isotope data which expanded the existing data sets on isotopic compositions of comets considerably. In this paper we review our current knowledge on the isotopic compositions of H, C, N, O, Si, S, Ar, and Xe in primitive Solar System materials studied in terrestrial laboratories and how the Rosetta data acquired with the ROSINA (Rosetta Orbiter Sensor for Ion and Neutral Analysis) and COSIMA (COmetary Secondary Ion Mass Analyzer) mass spectrometer fit into this picture. The H, Si, S, and Xe isotope data of comet 67P/CG suggest that this comet might be particularly primitive and might have preserved large amounts of unprocessed presolar matter. We address the question whether the refractory Si component of 67P/CG contains a presolar isotopic fingerprint from a nearby Type II supernova (SN) and discuss to which extent C and O isotope anomalies originating from presolar grains should be observable in dust from 67P/CG. Finally, we explore whether the isotopic fingerprint of a potential late SN contribution to the formation site of 67P/CG in the solar nebula can be seen in the volatile component of 67P/CG.
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Affiliation(s)
- Peter Hoppe
- Max Planck Institute for Chemistry, Hahn-Meitner-Weg 1, 55128 Mainz, Germany
| | - Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
- Center for Space and Habitability, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
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29
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Levasseur-Regourd AC, Agarwal J, Cottin H, Engrand C, Flynn G, Fulle M, Gombosi T, Langevin Y, Lasue J, Mannel T, Merouane S, Poch O, Thomas N, Westphal A. Cometary Dust. SPACE SCIENCE REVIEWS 2018; 214:64. [PMID: 35095119 PMCID: PMC8793767 DOI: 10.1007/s11214-018-0496-3] [Citation(s) in RCA: 12] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/13/2017] [Accepted: 03/16/2018] [Indexed: 05/15/2023]
Abstract
This review presents our understanding of cometary dust at the end of 2017. For decades, insight about the dust ejected by nuclei of comets had stemmed from remote observations from Earth or Earth's orbit, and from flybys, including the samples of dust returned to Earth for laboratory studies by the Stardust return capsule. The long-duration Rosetta mission has recently provided a huge and unique amount of data, obtained using numerous instruments, including innovative dust instruments, over a wide range of distances from the Sun and from the nucleus. The diverse approaches available to study dust in comets, together with the related theoretical and experimental studies, provide evidence of the composition and physical properties of dust particles, e.g., the presence of a large fraction of carbon in macromolecules, and of aggregates on a wide range of scales. The results have opened vivid discussions on the variety of dust-release processes and on the diversity of dust properties in comets, as well as on the formation of cometary dust, and on its presence in the near-Earth interplanetary medium. These discussions stress the significance of future explorations as a way to decipher the formation and evolution of our Solar System.
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Affiliation(s)
- Anny-Chantal Levasseur-Regourd
- Sorbonne Université; UVSQ; CNRS/INSU; Campus Pierre et Marie Curie, BC 102, 4 place Jussieu, F-75005 Paris, France, Tel.: + 33 144274875,
| | - Jessica Agarwal
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg, 3, D-37077, Göttingen, Germany
| | - Hervé Cottin
- Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA), UMR CNRS 7583, Université Paris-Est Créteil et Université Paris Diderot, Institut Pierre Simon Laplace, 94000 Créteil, France
| | - Cécile Engrand
- Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), CNRS/IN2P3 Université Paris Sud - UMR 8609, Université Paris-Saclay, Bâtiment 104, 91405 Orsay Campus, France
| | - George Flynn
- SUNY-Plattsburgh, 101 Broad St, Plattsburgh, NY 12901, United States
| | - Marco Fulle
- INAF - Osservatorio Astronomico, Via Tiepolo 11, 34143 Trieste Italy
| | - Tamas Gombosi
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI 48109, USA
| | - Yves Langevin
- Institut dAstrophysique Spatiale (IAS), CNRS/Université Paris Sud, Bâtiment 121, 91405 Orsay France
| | - Jérémie Lasue
- IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
| | - Thurid Mannel
- Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria; Physics Institute, University of Graz, Universitätsplatz 5, 8010 Graz, Austria
| | - Sihane Merouane
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg, 3, D-37077, Göttingen, Germany
| | - Olivier Poch
- Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
| | - Nicolas Thomas
- Physikalisches Institut, Universität Bern, Sidlerstrasse 5, 3012, Bern, Switzerland
| | - Andrew Westphal
- Space Sciences Laboratory, U.C. Berkeley, Berkeley, California 94720-7450 USA
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Rimola A, Trigo-Rodríguez JM, Martins Z. Interaction of organic compounds with chondritic silicate surfaces. Atomistic insights from quantum chemical periodic simulations. Phys Chem Chem Phys 2018; 19:18217-18231. [PMID: 28682400 DOI: 10.1039/c7cp03504g] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
The interaction of 14 different probe organic molecules with the crystalline (010) forsterite Mg2SiO4 surface has been studied at quantum chemical level by means of B3LYP-D2* periodic simulations. The probe molecules are representatives of the class of soluble organic compounds found in carbonaceous meteorites, namely: aliphatic and aromatic hydrocarbons, alcohols, carbonyl compounds, amines, amides, nitrogen heterocycles, carboxylic and hydroxycarboxylic acids, sulfonic and phosphonic acids, amino acids, and carbohydrates. With the exception of the aliphatic and aromatic hydrocarbons, the interaction takes place mainly between the O and N electron donor atoms of the molecules and the outermost Mg surface cations, and/or by hydrogen bonds of H atoms of the molecules with O surface atoms. Dispersion also contributes to the final interaction energies. Each surface/molecule complex has also been characterized by computing its harmonic vibrational spectrum, in which the most significant frequency perturbations caused by the surface interaction are described. With the calculated interaction energies, a trend of the intrinsic affinity of the probe molecules with the silicate surface has been obtained. However, this affinity scale does not correlate with the experimental abundances of the class of compounds found in the Murchison meteorite. A brief discussion of this lack of correlation and the factors that can help us to understand the abundances is provided.
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Affiliation(s)
- Albert Rimola
- Departament de Química, Universitat Autònoma de Barcelona, 08193 Bellaterra, Spain.
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O'D Alexander CM, McKeegan KD, Altwegg K. Water Reservoirs in Small Planetary Bodies: Meteorites, Asteroids, and Comets. SPACE SCIENCE REVIEWS 2018; 214:36. [PMID: 30842688 PMCID: PMC6398961 DOI: 10.1007/s11214-018-0474-9] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/10/2018] [Accepted: 01/11/2018] [Indexed: 06/09/2023]
Abstract
Asteroids and comets are the remnants of the swarm of planetesimals from which the planets ultimately formed, and they retain records of processes that operated prior to and during planet formation. They are also likely the sources of most of the water and other volatiles accreted by Earth. In this review, we discuss the nature and probable origins of asteroids and comets based on data from remote observations, in situ measurements by spacecraft, and laboratory analyses of meteorites derived from asteroids. The asteroidal parent bodies of meteorites formed ≤4 Ma after Solar System formation while there was still a gas disk present. It seems increasingly likely that the parent bodies of meteorites spectroscopically linked with the E-, S-, M- and V-type asteroids formed sunward of Jupiter's orbit, while those associated with C- and, possibly, D-type asteroids formed further out, beyond Jupiter but probably not beyond Saturn's orbit. Comets formed further from the Sun than any of the meteorite parent bodies, and retain much higher abundances of interstellar material. CI and CM group meteorites are probably related to the most common C-type asteroids, and based on isotopic evidence they, rather than comets, are the most likely sources of the H and N accreted by the terrestrial planets. However, comets may have been major sources of the noble gases accreted by Earth and Venus. Possible constraints that these observations can place on models of giant planet formation and migration are explored.
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Affiliation(s)
- Conel M O'D Alexander
- Dept. Terrestrial Magnetism, Carnegie Institution for Science, 5241 Broad Branch Road NW, Washington, DC 20015, USA. . Tel. (202) 478 8478
| | - Kevin D McKeegan
- Department of Earth, Planetary, and Space Sciences, University of California-Los Angeles, Los Angeles, CA 90095-1567, USA.
| | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland.
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Jones GH, Knight MM, Fitzsimmons A, Taylor MGGT. Cometary science after Rosetta. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2017; 375:rsta.2017.0001. [PMID: 28554982 PMCID: PMC5454231 DOI: 10.1098/rsta.2017.0001] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 03/20/2017] [Indexed: 05/31/2023]
Abstract
The European Space Agency's Rosetta mission ended operations on 30 September 2016 having spent over 2 years in close proximity to its target comet, 67P/Churyumov-Gerasimenko. Shortly before this, in summer 2016, a discussion meeting was held to examine how the results of the mission could be framed in terms of cometary and solar system science in general. This paper provides a brief history of the Rosetta mission, and gives an overview of the meeting and the contents of this associated special issue.This article is part of the themed issue 'Cometary science after Rosetta'.
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Affiliation(s)
- Geraint H Jones
- Mullard Space Science Laboratory, University College London, Dorking, Surrey, UK
- The Centre for Planetary Sciences at UCL/Birkbeck, Gower Street, London, UK
| | | | - Alan Fitzsimmons
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast, UK
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Marty B, Altwegg K, Balsiger H, Bar-Nun A, Bekaert DV, Berthelier JJ, Bieler A, Briois C, Calmonte U, Combi M, De Keyser J, Fiethe B, Fuselier SA, Gasc S, Gombosi TI, Hansen KC, Hässig M, Jäckel A, Kopp E, Korth A, Le Roy L, Mall U, Mousis O, Owen T, Rème H, Rubin M, Sémon T, Tzou CY, Waite JH, Wurz P. Xenon isotopes in 67P/Churyumov-Gerasimenko show that comets contributed to Earth's atmosphere. Science 2017; 356:1069-1072. [DOI: 10.1126/science.aal3496] [Citation(s) in RCA: 131] [Impact Index Per Article: 18.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/05/2016] [Accepted: 05/03/2017] [Indexed: 11/02/2022]
Affiliation(s)
- B. Marty
- Centre de Recherches Pétrographiques et Géochimiques, CNRS, Université de Lorraine, 15 rue Notre Dame des Pauvres, BP 20, 54501 Vandoeuvre lès Nancy, France
| | - K. Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Center for Space and Habitability, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - H. Balsiger
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - A. Bar-Nun
- Department of Geoscience, Tel Aviv University, Ramat Aviv, Tel Aviv, Israel
| | - D. V. Bekaert
- Centre de Recherches Pétrographiques et Géochimiques, CNRS, Université de Lorraine, 15 rue Notre Dame des Pauvres, BP 20, 54501 Vandoeuvre lès Nancy, France
| | - J.-J. Berthelier
- Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Institut Pierre Simon Laplace, CNRS, Université Pierre et Marie Curie, 4 Avenue de Neptune, 94100 Saint-Maur, France
| | - A. Bieler
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, USA
| | - C. Briois
- Laboratoire de Physique et Chimie de l’Environnement et de l’Espace (LPC2E), UMR 6115 CNRS–Université d’Orléans, France
| | - U. Calmonte
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - M. Combi
- Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, USA
| | - J. De Keyser
- Koninklijk Belgisch Instituut voor Ruimte-Aeronomie/Institut Royal d’Aéronomie Spatiale de Belgique (BIRA-IASB), Ringlaan 3, B-1180 Brussels, Belgium
| | - B. Fiethe
- Institute of Computer and Network Engineering (IDA), Technische Universität Braunschweig, Hans-Sommer-Straße 66, D-38106 Braunschweig, Germany
| | - S. A. Fuselier
- Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA
| | - S. Gasc
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - T. I. Gombosi
- Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, USA
| | - K. C. Hansen
- Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, USA
| | - M. Hässig
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA
| | - A. Jäckel
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - E. Kopp
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - A. Korth
- Max-Planck-Institut für Sonnensystemforschung (MPS), Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - L. Le Roy
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - U. Mall
- Max-Planck-Institut für Sonnensystemforschung (MPS), Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - O. Mousis
- Laboratoire d’Astrophysique de Marseille, CNRS, Aix Marseille Université, 13388 Marseille, France
| | - T. Owen
- Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA
| | - H. Rème
- Institut de Recherche en Astrophysique et Planétologie, CNRS, Université Paul Sabatier, Observatoire Midi-Pyrénées, 9 Avenue du Colonel Roche, 31028 Toulouse Cedex 4, France
| | - M. Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - T. Sémon
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - C.-Y. Tzou
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - J. H. Waite
- Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA
| | - P. Wurz
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
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Defouilloy C, Nakashima D, Joswiak DJ, Brownlee DE, Tenner TJ, Kita NT. Origin of crystalline silicates from Comet 81P/Wild 2: Combined study on their oxygen isotopes and mineral chemistry. EARTH AND PLANETARY SCIENCE LETTERS 2017; 465:145-154. [PMID: 30705461 PMCID: PMC6350803 DOI: 10.1016/j.epsl.2017.02.045] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
In order to explore the link between comet 81P/Wild 2 and materials in primitive meteorites, seven particles 5 to 15 μm in diameter from comet 81P/Wild 2 have been analyzed for their oxygen isotope ratios using a secondary ion mass spectrometer. Most particles are single minerals consisting of olivine or pyroxene with Mg# higher than 85, which are relatively minor in 81P/Wild 2 particles (~1/3 of the 16O-poor cluster). Four particles extracted from Track 149 are 16O-poor and show Δ17O (= δ17O - 0.52 × δ18O) values from -2%0 to +1%0, similar to previous studies, while one enstatite (En99) particle shows lower Δ17O value of -7±4%o (2σ). This compositional range has not been reported among 16O-poor particles in 81P/Wild 2, but is commonly observed among chondrules in carbonaceous chondrites and in particular in CR chondrites. The distribution in Δ17O indicates that 16O-poor 81P/Wild 2 particles are most similar to chondrules (and their fragments) in the CR chondrites and Tagish Lake-like WIS91600 chondrite chondrule silicate grains, which indicates that they likely come from a reservoir with similar dust/ice ratios as CR chondrites and WIS91600. However, differences in the Mg# distribution imply that the 81P/Wild 2 reservoir was comparatively more oxidized, with a higher dust enrichment. Two nearly pure enstatite grains from track 172 are significantly enriched in 16O, with δ18O values of -51.2 ± 1.5%0 (2σ) and -43.0 ± 1.3% (2σ), respectively, and Δ17O values of -22.3 ± 1.9% (2σ) and -21.3 ± 2.3%0 (2σ), respectively. They are the first 16O-rich pyroxenes found among 81P/Wild 2 particles, with similar Δ17O values to those of 16O-rich low-iron, manganese-enriched (LIME) olivine and CAI (calcium and aluminum-rich inclusions) -like particles from 81P/Wild 2. The major element and oxygen isotopic compositions of the pyroxenes are similar to those of enstatite in amoeboid olivine aggregates (AOAs) in primitive chondrites, in which 16O-rich pyroxenes have previously been found, and thus suggest a condensation origin.
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Affiliation(s)
- Céline Defouilloy
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Daisuke Nakashima
- Division of Earth and Planetary Materials Science, Tohoku University, Miyagi 980-8578, Japan
| | - David J. Joswiak
- Department of Astronomy, University of Washington, Seattle, WA 98195, USA
| | - Donald E. Brownlee
- Department of Astronomy, University of Washington, Seattle, WA 98195, USA
| | - Travis J. Tenner
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
| | - Noriko T. Kita
- WiscSIMS, Department of Geoscience, University of Wisconsin-Madison, Madison, WI 53706, USA
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Liquid metal technology of synthesis of AlOOH anisotropic nanostructured aerogel. NUCLEAR ENERGY AND TECHNOLOGY 2017. [DOI: 10.1016/j.nucet.2017.03.008] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/17/2022] Open
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37
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Hibbert R, Cole M, Price M, Burchell M. The Hypervelocity Impact Facility at the University of Kent: Recent Upgrades and Specialized Capabilities. ACTA ACUST UNITED AC 2017. [DOI: 10.1016/j.proeng.2017.09.775] [Citation(s) in RCA: 11] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
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39
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Maynard-Casely HE. ‘Peaks in space’ – crystallography in planetary science: past impacts and future opportunities. CRYSTALLOGR REV 2016. [DOI: 10.1080/0889311x.2016.1242127] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/20/2022]
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40
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Aggregate dust particles at comet 67P/Churyumov-Gerasimenko. Nature 2016; 537:73-5. [PMID: 27582221 DOI: 10.1038/nature19091] [Citation(s) in RCA: 120] [Impact Index Per Article: 15.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/17/2015] [Accepted: 07/06/2016] [Indexed: 11/08/2022]
Abstract
Comets are thought to preserve almost pristine dust particles, thus providing a unique sample of the properties of the early solar nebula. The microscopic properties of this dust played a key part in particle aggregation during the formation of the Solar System. Cometary dust was previously considered to comprise irregular, fluffy agglomerates on the basis of interpretations of remote observations in the visible and infrared and the study of chondritic porous interplanetary dust particles that were thought, but not proved, to originate in comets. Although the dust returned by an earlier mission has provided detailed mineralogy of particles from comet 81P/Wild, the fine-grained aggregate component was strongly modified during collection. Here we report in situ measurements of dust particles at comet 67P/Churyumov-Gerasimenko. The particles are aggregates of smaller, elongated grains, with structures at distinct sizes indicating hierarchical aggregation. Topographic images of selected dust particles with sizes of one micrometre to a few tens of micrometres show a variety of morphologies, including compact single grains and large porous aggregate particles, similar to chondritic porous interplanetary dust particles. The measured grain elongations are similar to the value inferred for interstellar dust and support the idea that such grains could represent a fraction of the building blocks of comets. In the subsequent growth phase, hierarchical agglomeration could be a dominant process and would produce aggregates that stick more easily at higher masses and velocities than homogeneous dust particles. The presence of hierarchical dust aggregates in the near-surface of the nucleus of comet 67P also provides a mechanism for lowering the tensile strength of the dust layer and aiding dust release.
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41
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High-molecular-weight organic matter in the particles of comet 67P/Churyumov-Gerasimenko. Nature 2016; 538:72-74. [PMID: 27602514 DOI: 10.1038/nature19320] [Citation(s) in RCA: 27] [Impact Index Per Article: 3.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/06/2016] [Accepted: 07/15/2016] [Indexed: 11/08/2022]
Abstract
The presence of solid carbonaceous matter in cometary dust was established by the detection of elements such as carbon, hydrogen, oxygen and nitrogen in particles from comet 1P/Halley. Such matter is generally thought to have originated in the interstellar medium, but it might have formed in the solar nebula-the cloud of gas and dust that was left over after the Sun formed. This solid carbonaceous material cannot be observed from Earth, so it has eluded unambiguous characterization. Many gaseous organic molecules, however, have been observed; they come mostly from the sublimation of ices at the surface or in the subsurface of cometary nuclei. These ices could have been formed from material inherited from the interstellar medium that suffered little processing in the solar nebula. Here we report the in situ detection of solid organic matter in the dust particles emitted by comet 67P/Churyumov-Gerasimenko; the carbon in this organic material is bound in very large macromolecular compounds, analogous to the insoluble organic matter found in the carbonaceous chondrite meteorites. The organic matter in meteorites might have formed in the interstellar medium and/or the solar nebula, but was almost certainly modified in the meteorites' parent bodies. We conclude that the observed cometary carbonaceous solid matter could have the same origin as the meteoritic insoluble organic matter, but suffered less modification before and/or after being incorporated into the comet.
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Luthra A, Ravi A, Li S, Nystrom SV, Thompson Z, Coe JV. Dust Library of Plasmonically Enhanced Infrared Spectra of Individual Respirable Particles. APPLIED SPECTROSCOPY 2016; 70:1546-1554. [PMID: 27440136 DOI: 10.1177/0003702816653126] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/29/2015] [Accepted: 03/04/2016] [Indexed: 06/06/2023]
Abstract
This work characterizes collections of infrared spectra of individual dust particles of ∼4 µm size that were obtained from three very different environments: our lab air, a home air filter, and the 11 September 2001 World Trade Center event. Particle collection was done either directly from the air or by placing dust powder from various samples directly on the plasmonic mesh with 5 µm square holes as air is pumped through the mesh. This arrangement enables the recording of "scatter-free" infrared absorption spectra of individual particles of size comparable to the probing wavelengths whose vibrational signatures are otherwise dominated by scattering and dispersive line shape distortions. The spectra are sensitive to the amounts of various infrared active components and analysis using a Mie-Bruggeman model for mixed composition particles provides volume fractions of the components. Inhalation of dust particles of ∼4 µm size has significant health consequences as these are among the largest inhaled into people's lungs. The chemical composition of ∼4 µm respirable particles is of great interest from health, atmospheric, and environmental perspectives as different environments may pose different hazards and spectroscopic challenges.
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Affiliation(s)
- Antriksh Luthra
- Department of Chemistry and Biochemistry, The Ohio State University, USA Department of Mechanical and Aerospace Engineering, The Ohio State University, USA
| | - Aruna Ravi
- Department of Chemistry and Biochemistry, The Ohio State University, USA Department of Electrical and Computer Engineering, The Ohio State University, USA
| | - Sirui Li
- Department of Chemistry and Biochemistry, The Ohio State University, USA
| | - Steven V Nystrom
- Department of Chemical Engineering, The Ohio State University, USA
| | | | - James V Coe
- Department of Chemistry and Biochemistry, The Ohio State University, USA
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Domagal-Goldman SD, Wright KE, Adamala K, Arina de la Rubia L, Bond J, Dartnell LR, Goldman AD, Lynch K, Naud ME, Paulino-Lima IG, Singer K, Walther-Antonio M, Abrevaya XC, Anderson R, Arney G, Atri D, Azúa-Bustos A, Bowman JS, Brazelton WJ, Brennecka GA, Carns R, Chopra A, Colangelo-Lillis J, Crockett CJ, DeMarines J, Frank EA, Frantz C, de la Fuente E, Galante D, Glass J, Gleeson D, Glein CR, Goldblatt C, Horak R, Horodyskyj L, Kaçar B, Kereszturi A, Knowles E, Mayeur P, McGlynn S, Miguel Y, Montgomery M, Neish C, Noack L, Rugheimer S, Stüeken EE, Tamez-Hidalgo P, Imari Walker S, Wong T. The Astrobiology Primer v2.0. ASTROBIOLOGY 2016; 16:561-653. [PMID: 27532777 PMCID: PMC5008114 DOI: 10.1089/ast.2015.1460] [Citation(s) in RCA: 46] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/23/2015] [Accepted: 06/06/2016] [Indexed: 05/09/2023]
Affiliation(s)
- Shawn D Domagal-Goldman
- 1 NASA Goddard Space Flight Center , Greenbelt, Maryland, USA
- 2 Virtual Planetary Laboratory , Seattle, Washington, USA
| | - Katherine E Wright
- 3 University of Colorado at Boulder , Colorado, USA
- 4 Present address: UK Space Agency, UK
| | - Katarzyna Adamala
- 5 Department of Genetics, Cell Biology and Development, University of Minnesota , Minneapolis, Minnesota, USA
| | | | - Jade Bond
- 7 Department of Physics, University of New South Wales , Sydney, Australia
| | | | | | - Kennda Lynch
- 10 Division of Biological Sciences, University of Montana , Missoula, Montana, USA
| | - Marie-Eve Naud
- 11 Institute for research on exoplanets (iREx) , Université de Montréal, Montréal, Canada
| | - Ivan G Paulino-Lima
- 12 Universities Space Research Association , Mountain View, California, USA
- 13 Blue Marble Space Institute of Science , Seattle, Washington, USA
| | - Kelsi Singer
- 14 Southwest Research Institute , Boulder, Colorado, USA
| | | | - Ximena C Abrevaya
- 16 Instituto de Astronomía y Física del Espacio (IAFE) , UBA-CONICET, Ciudad Autónoma de Buenos Aires, Argentina
| | - Rika Anderson
- 17 Department of Biology, Carleton College , Northfield, Minnesota, USA
| | - Giada Arney
- 18 University of Washington Astronomy Department and Astrobiology Program , Seattle, Washington, USA
| | - Dimitra Atri
- 13 Blue Marble Space Institute of Science , Seattle, Washington, USA
| | | | - Jeff S Bowman
- 19 Lamont-Doherty Earth Observatory, Columbia University , Palisades, New York, USA
| | | | | | - Regina Carns
- 22 Polar Science Center, Applied Physics Laboratory, University of Washington , Seattle, Washington, USA
| | - Aditya Chopra
- 23 Planetary Science Institute, Research School of Earth Sciences, Research School of Astronomy and Astrophysics, The Australian National University , Canberra, Australia
| | - Jesse Colangelo-Lillis
- 24 Earth and Planetary Science, McGill University , and the McGill Space Institute, Montréal, Canada
| | | | - Julia DeMarines
- 13 Blue Marble Space Institute of Science , Seattle, Washington, USA
| | | | - Carie Frantz
- 27 Department of Geosciences, Weber State University , Ogden, Utah, USA
| | - Eduardo de la Fuente
- 28 IAM-Departamento de Fisica, CUCEI , Universidad de Guadalajara, Guadalajara, México
| | - Douglas Galante
- 29 Brazilian Synchrotron Light Laboratory , Campinas, Brazil
| | - Jennifer Glass
- 30 School of Earth and Atmospheric Sciences, Georgia Institute of Technology , Atlanta, Georgia , USA
| | | | | | - Colin Goldblatt
- 33 School of Earth and Ocean Sciences, University of Victoria , Victoria, Canada
| | - Rachel Horak
- 34 American Society for Microbiology , Washington, DC, USA
| | | | - Betül Kaçar
- 36 Harvard University , Organismic and Evolutionary Biology, Cambridge, Massachusetts, USA
| | - Akos Kereszturi
- 37 Research Centre for Astronomy and Earth Sciences , Hungarian Academy of Sciences, Budapest, Hungary
| | - Emily Knowles
- 38 Johnson & Wales University , Denver, Colorado, USA
| | - Paul Mayeur
- 39 Rensselaer Polytechnic Institute , Troy, New York, USA
| | - Shawn McGlynn
- 40 Earth Life Science Institute, Tokyo Institute of Technology , Tokyo, Japan
| | - Yamila Miguel
- 41 Laboratoire Lagrange, UMR 7293, Université Nice Sophia Antipolis , CNRS, Observatoire de la Côte d'Azur, Nice, France
| | | | - Catherine Neish
- 43 Department of Earth Sciences, The University of Western Ontario , London, Canada
| | - Lena Noack
- 44 Royal Observatory of Belgium , Brussels, Belgium
| | - Sarah Rugheimer
- 45 Department of Astronomy, Harvard University , Cambridge, Massachusetts, USA
- 46 University of St. Andrews , St. Andrews, UK
| | - Eva E Stüeken
- 47 University of Washington , Seattle, Washington, USA
- 48 University of California , Riverside, California, USA
| | | | - Sara Imari Walker
- 13 Blue Marble Space Institute of Science , Seattle, Washington, USA
- 50 School of Earth and Space Exploration and Beyond Center for Fundamental Concepts in Science, Arizona State University , Tempe, Arizona, USA
| | - Teresa Wong
- 51 Department of Earth and Planetary Sciences, Washington University in St. Louis , St. Louis, Missouri, USA
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Kawaguchi Y, Yokobori SI, Hashimoto H, Yano H, Tabata M, Kawai H, Yamagishi A. Investigation of the Interplanetary Transfer of Microbes in the Tanpopo Mission at the Exposed Facility of the International Space Station. ASTROBIOLOGY 2016; 16:363-76. [PMID: 27176813 DOI: 10.1089/ast.2015.1415] [Citation(s) in RCA: 19] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/25/2023]
Abstract
UNLABELLED The Tanpopo mission will address fundamental questions on the origin of terrestrial life. The main goal is to test the panspermia hypothesis. Panspermia is a long-standing hypothesis suggesting the interplanetary transport of microbes. Another goal is to test the possible origin of organic compounds carried from space by micrometeorites before the terrestrial origin of life. To investigate the panspermia hypothesis and the possible space origin of organic compounds, we performed space experiments at the Exposed Facility (EF) of the Japanese Experiment Module (JEM) of the International Space Station (ISS). The mission was named Tanpopo, which in Japanese means dandelion. We capture any orbiting microparticles, such as micrometeorites, space debris, and terrestrial particles carrying microbes as bioaerosols, by using blocks of silica aerogel. We also test the survival of microbial species and organic compounds in the space environment for up to 3 years. The goal of this review is to introduce an overview of the Tanpopo mission with particular emphasis on the investigation of the interplanetary transfer of microbes. The Exposed Experiment Handrail Attachment Mechanism with aluminum Capture Panels (CPs) and Exposure Panels (EPs) was exposed on the EF-JEM on May 26, 2015. The first CPs and EPs will be returned to the ground in mid-2016. Possible escape of terrestrial microbes from Earth to space will be evaluated by investigating the upper limit of terrestrial microbes by the capture experiment. Possible mechanisms for transfer of microbes over the stratosphere and an investigation of the effect of the microbial cell-aggregate size on survivability in space will also be discussed. KEY WORDS Panspermia-Astrobiology-Low-Earth orbit. Astrobiology 16, 363-376.
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Affiliation(s)
- Yuko Kawaguchi
- 1 Institute of Space and Astronautical Science , Japan Aerospace Exploration Agency (ISAS/JAXA), Sagamihara, Japan
- 2 School of Life Sciences, Tokyo University of Pharmacy and Life Sciences , Hachioji, Tokyo, Japan
| | - Shin-Ichi Yokobori
- 2 School of Life Sciences, Tokyo University of Pharmacy and Life Sciences , Hachioji, Tokyo, Japan
| | - Hirofumi Hashimoto
- 1 Institute of Space and Astronautical Science , Japan Aerospace Exploration Agency (ISAS/JAXA), Sagamihara, Japan
| | - Hajime Yano
- 1 Institute of Space and Astronautical Science , Japan Aerospace Exploration Agency (ISAS/JAXA), Sagamihara, Japan
| | - Makoto Tabata
- 3 Graduate School of Science, Chiba University , Chiba-shi, Japan
| | - Hideyuki Kawai
- 3 Graduate School of Science, Chiba University , Chiba-shi, Japan
| | - Akihiko Yamagishi
- 2 School of Life Sciences, Tokyo University of Pharmacy and Life Sciences , Hachioji, Tokyo, Japan
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45
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Demir S, Brune N, Van Humbeck J, Mason JA, Plakhova T, Wang S, Tian G, Minasian SG, Tyliszczak T, Yaita T, Kobayashi T, Kalmykov SN, Shiwaku H, Shuh DK, Long JR. Extraction of Lanthanide and Actinide Ions from Aqueous Mixtures Using a Carboxylic Acid-Functionalized Porous Aromatic Framework. ACS CENTRAL SCIENCE 2016; 2:253-65. [PMID: 27163056 PMCID: PMC4850516 DOI: 10.1021/acscentsci.6b00066] [Citation(s) in RCA: 48] [Impact Index Per Article: 6.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/06/2016] [Indexed: 05/04/2023]
Abstract
Porous aromatic frameworks (PAFs) incorporating a high concentration of acid functional groups possess characteristics that are promising for use in separating lanthanide and actinide metal ions, as required in the treatment of radioactive waste. These materials have been shown to be indefinitely stable to concentrated acids and bases, potentially allowing for multiple adsorption/stripping cycles. Additionally, the PAFs combine exceptional features from MOFs and inorganic/activated carbons giving rise to tunable pore surfaces and maximum chemical stability. Herein, we present a study of the adsorption of selected metal ions, Sr(2+), Fe(3+), Nd(3+), and Am(3+), from aqueous solutions employing a carbon-based porous aromatic framework, BPP-7 (Berkeley Porous Polymer-7). This material displays high metal loading capacities together with excellent adsorption selectivity for neodymium over strontium based on Langmuir adsorption isotherms and ideal adsorbed solution theory (IAST) calculations. Based in part upon X-ray absorption spectroscopy studies, the stronger adsorption of neodymium is attributed to multiple metal ion and binding site interactions resulting from the densely functionalized and highly interpenetrated structure of BPP-7. Recyclability and combustibility experiments demonstrate that multiple adsorption/stripping cycles can be completed with minimal degradation of the polymer adsorption capacity.
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Affiliation(s)
- Selvan Demir
- Department of Chemistry and Department of
Chemical and Biomolecular Engineering, University
of California, Berkeley, California 94720, United States
- Chemical Sciences Division, Materials Sciences
Division,
and Advanced Light
Source, Lawrence Berkeley National Laboratory, Berkeley, California 94720, United States
| | - Nicholas
K. Brune
- Department of Chemistry and Department of
Chemical and Biomolecular Engineering, University
of California, Berkeley, California 94720, United States
- Chemical Sciences Division, Materials Sciences
Division,
and Advanced Light
Source, Lawrence Berkeley National Laboratory, Berkeley, California 94720, United States
| | - Jeffrey
F. Van Humbeck
- Department of Chemistry and Department of
Chemical and Biomolecular Engineering, University
of California, Berkeley, California 94720, United States
| | - Jarad A. Mason
- Department of Chemistry and Department of
Chemical and Biomolecular Engineering, University
of California, Berkeley, California 94720, United States
| | - Tatiana
V. Plakhova
- Chemical Sciences Division, Materials Sciences
Division,
and Advanced Light
Source, Lawrence Berkeley National Laboratory, Berkeley, California 94720, United States
- Chemistry
Department, Lomonosov Moscow State University, Leninskie Gory, Moscow 11991, Russia
| | - Shuao Wang
- Department of Chemistry and Department of
Chemical and Biomolecular Engineering, University
of California, Berkeley, California 94720, United States
- Chemical Sciences Division, Materials Sciences
Division,
and Advanced Light
Source, Lawrence Berkeley National Laboratory, Berkeley, California 94720, United States
| | - Guoxin Tian
- Chemical Sciences Division, Materials Sciences
Division,
and Advanced Light
Source, Lawrence Berkeley National Laboratory, Berkeley, California 94720, United States
- Radiochemistry
Department, China Institute of Atomic Energy, Beijing 102413, China
| | - Stefan G. Minasian
- Chemical Sciences Division, Materials Sciences
Division,
and Advanced Light
Source, Lawrence Berkeley National Laboratory, Berkeley, California 94720, United States
| | - Tolek Tyliszczak
- Chemical Sciences Division, Materials Sciences
Division,
and Advanced Light
Source, Lawrence Berkeley National Laboratory, Berkeley, California 94720, United States
| | - Tsuyoshi Yaita
- Actinide
Chemistry Group, Energy and Environment Science Division, Quantum
Beam Science Center, Japan Atomic Energy
Agency, 1-1-1 Kouto,
Sayo-cho, Sayo-gun, Hyogo 679-5148, Japan
| | - Tohru Kobayashi
- Actinide
Chemistry Group, Energy and Environment Science Division, Quantum
Beam Science Center, Japan Atomic Energy
Agency, 1-1-1 Kouto,
Sayo-cho, Sayo-gun, Hyogo 679-5148, Japan
| | - Stepan N. Kalmykov
- Chemistry
Department, Lomonosov Moscow State University, Leninskie Gory, Moscow 11991, Russia
| | - Hideaki Shiwaku
- Actinide
Chemistry Group, Energy and Environment Science Division, Quantum
Beam Science Center, Japan Atomic Energy
Agency, 1-1-1 Kouto,
Sayo-cho, Sayo-gun, Hyogo 679-5148, Japan
| | - David K. Shuh
- Chemical Sciences Division, Materials Sciences
Division,
and Advanced Light
Source, Lawrence Berkeley National Laboratory, Berkeley, California 94720, United States
| | - Jeffrey R. Long
- Department of Chemistry and Department of
Chemical and Biomolecular Engineering, University
of California, Berkeley, California 94720, United States
- Chemical Sciences Division, Materials Sciences
Division,
and Advanced Light
Source, Lawrence Berkeley National Laboratory, Berkeley, California 94720, United States
- E-mail:
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Pätzold M, Andert T, Hahn M, Asmar SW, Barriot JP, Bird MK, Häusler B, Peter K, Tellmann S, Grün E, Weissman PR, Sierks H, Jorda L, Gaskell R, Preusker F, Scholten F. A homogeneous nucleus for comet 67P/Churyumov-Gerasimenko from its gravity field. Nature 2016; 530:63-5. [PMID: 26842054 DOI: 10.1038/nature16535] [Citation(s) in RCA: 222] [Impact Index Per Article: 27.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/27/2015] [Accepted: 12/10/2015] [Indexed: 11/09/2022]
Abstract
Cometary nuclei consist mostly of dust and water ice. Previous observations have found nuclei to be low-density and highly porous bodies, but have only moderately constrained the range of allowed densities because of the measurement uncertainties. Here we report the precise mass, bulk density, porosity and internal structure of the nucleus of comet 67P/Churyumov-Gerasimenko on the basis of its gravity field. The mass and gravity field are derived from measured spacecraft velocity perturbations at fly-by distances between 10 and 100 kilometres. The gravitational point mass is GM = 666.2 ± 0.2 cubic metres per second squared, giving a mass M = (9,982 ± 3) × 10(9) kilograms. Together with the current estimate of the volume of the nucleus, the average bulk density of the nucleus is 533 ± 6 kilograms per cubic metre. The nucleus appears to be a low-density, highly porous (72-74 per cent) dusty body, similar to that of comet 9P/Tempel 1. The most likely composition mix has approximately four times more dust than ice by mass and two times more dust than ice by volume. We conclude that the interior of the nucleus is homogeneous and constant in density on a global scale without large voids. The high porosity seems to be an inherent property of the nucleus material.
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Affiliation(s)
- M Pätzold
- Rheinisches Institut für Umweltforschung an der Universität zu Köln, Abteilung Planetenforschung, 50931 Köln, Germany
| | - T Andert
- Institut für Raumfahrttechnik und Weltraumnutzung, Universität der Bundeswehr München, 85577 Neubiberg, Germany
| | - M Hahn
- Rheinisches Institut für Umweltforschung an der Universität zu Köln, Abteilung Planetenforschung, 50931 Köln, Germany
| | - S W Asmar
- Jet Propulsion Laboratory, Caltech, Pasadena, California 91109, USA
| | - J-P Barriot
- Université de la Polynésie Francaise, Faaa, Tahiti
| | - M K Bird
- Rheinisches Institut für Umweltforschung an der Universität zu Köln, Abteilung Planetenforschung, 50931 Köln, Germany
| | - B Häusler
- Institut für Raumfahrttechnik und Weltraumnutzung, Universität der Bundeswehr München, 85577 Neubiberg, Germany
| | - K Peter
- Rheinisches Institut für Umweltforschung an der Universität zu Köln, Abteilung Planetenforschung, 50931 Köln, Germany
| | - S Tellmann
- Rheinisches Institut für Umweltforschung an der Universität zu Köln, Abteilung Planetenforschung, 50931 Köln, Germany
| | - E Grün
- Max-Planck-Institut für Kernphysik, 69117 Heidelberg, Germany
| | - P R Weissman
- Planetary Science Institute, 1700 East Fort Lowell Suite 106, Tucson, Arizona 85719, USA
| | - H Sierks
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - L Jorda
- Laboratoire d'Astrophysique de Marseille, 13388 Marseille, France
| | - R Gaskell
- Planetary Science Institute, 1700 East Fort Lowell Suite 106, Tucson, Arizona 85719, USA
| | - F Preusker
- Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt (DLR) Berlin-Adlershof, 12489 Berlin, Germany
| | - F Scholten
- Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt (DLR) Berlin-Adlershof, 12489 Berlin, Germany
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47
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Isotopic evidence for primordial molecular cloud material in metal-rich carbonaceous chondrites. Proc Natl Acad Sci U S A 2016; 113:2011-6. [PMID: 26858438 DOI: 10.1073/pnas.1518183113] [Citation(s) in RCA: 118] [Impact Index Per Article: 14.8] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
The short-lived (26)Al radionuclide is thought to have been admixed into the initially (26)Al-poor protosolar molecular cloud before or contemporaneously with its collapse. Bulk inner Solar System reservoirs record positively correlated variability in mass-independent (54)Cr and (26)Mg*, the decay product of (26)Al. This correlation is interpreted as reflecting progressive thermal processing of in-falling (26)Al-rich molecular cloud material in the inner Solar System. The thermally unprocessed molecular cloud matter reflecting the nucleosynthetic makeup of the molecular cloud before the last addition of stellar-derived (26)Al has not been identified yet but may be preserved in planetesimals that accreted in the outer Solar System. We show that metal-rich carbonaceous chondrites and their components have a unique isotopic signature extending from an inner Solar System composition toward a (26)Mg*-depleted and (54)Cr-enriched component. This composition is consistent with that expected for thermally unprocessed primordial molecular cloud material before its pollution by stellar-derived (26)Al. The (26)Mg* and (54)Cr compositions of bulk metal-rich chondrites require significant amounts (25-50%) of primordial molecular cloud matter in their precursor material. Given that such high fractions of primordial molecular cloud material are expected to survive only in the outer Solar System, we infer that, similarly to cometary bodies, metal-rich carbonaceous chondrites are samples of planetesimals that accreted beyond the orbits of the gas giants. The lack of evidence for this material in other chondrite groups requires isolation from the outer Solar System, possibly by the opening of disk gaps from the early formation of gas giants.
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49
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Mandt K, Mousis O, Marty B, Cavalié T, Harris W, Hartogh P, Willacy K. Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites. SPACE SCIENCE REVIEWS 2015; 197:297-342. [PMID: 31105346 PMCID: PMC6525011 DOI: 10.1007/s11214-015-0161-z] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
Comets play a dual role in understanding the formation and evolution of the solar system. First, the composition of comets provides information about the origin of the giant planets and their moons because comets formed early and their composition is not expected to have evolved significantly since formation. They, therefore serve as a record of conditions during the early stages of solar system formation. Once comets had formed, their orbits were perturbed allowing them to travel into the inner solar system and impact the planets. In this way they contributed to the volatile inventory of planetary atmospheres. We review here how knowledge of comet composition up to the time of the Rosetta mission has contributed to understanding the formation processes of the giant planets, their moons and small icy bodies in the solar system. We also discuss how comets contributed to the volatile inventories of the giant and terrestrial planets.
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Affiliation(s)
- K.E. Mandt
- Southwest Research Institute, San Antonio, TX, USA
| | - O. Mousis
- Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388, Marseille, France
| | - B. Marty
- CRPG-CNRS, Nancy-Université, Vandoeuvre-lès-Nancy, France
| | - T. Cavalié
- Max Planck Institute for Solar System Research, Göttingen, Germany
| | - W. Harris
- University of Arizona, Tucson, AZ, USA
| | - P. Hartogh
- Max Planck Institute for Solar System Research, Göttingen, Germany
| | - K. Willacy
- Jet Propulsion Laboratory, Pasadena, CA, USA
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50
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Biele J, Ulamec S, Maibaum M, Roll R, Witte L, Jurado E, Muñoz P, Arnold W, Auster HU, Casas C, Faber C, Fantinati C, Finke F, Fischer HH, Geurts K, Güttler C, Heinisch P, Herique A, Hviid S, Kargl G, Knapmeyer M, Knollenberg J, Kofman W, Kömle N, Kührt E, Lommatsch V, Mottola S, Pardo de Santayana R, Remetean E, Scholten F, Seidensticker KJ, Sierks H, Spohn T. COMETARY SCIENCE. The landing(s) of Philae and inferences about comet surface mechanical properties. Science 2015; 349:aaa9816. [PMID: 26228158 DOI: 10.1126/science.aaa9816] [Citation(s) in RCA: 190] [Impact Index Per Article: 21.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Philae lander, part of the Rosetta mission to investigate comet 67P/Churyumov-Gerasimenko, was delivered to the cometary surface in November 2014. Here we report the precise circumstances of the multiple landings of Philae, including the bouncing trajectory and rebound parameters, based on engineering data in conjunction with operational instrument data. These data also provide information on the mechanical properties (strength and layering) of the comet surface. The first touchdown site, Agilkia, appears to have a granular soft surface (with a compressive strength of 1 kilopascal) at least ~20 cm thick, possibly on top of a more rigid layer. The final landing site, Abydos, has a hard surface.
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Affiliation(s)
- Jens Biele
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Stephan Ulamec
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Michael Maibaum
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Reinhard Roll
- Max-Planck-Institut für Sonnensystemforschung (MPS), Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Lars Witte
- DLR/Institut für Raumfahrtsysteme, Robert Hooke-Straße 7, 28359 Bremen, Germany
| | - Eric Jurado
- Centre National d'Études Spatiales, 18 Avenue Édouard Belin, 31400 Toulouse, France
| | - Pablo Muñoz
- European Space Agency/European Space Operations Centre (ESA/ESOC), Robert-Bosch-Straße 5, 64293 Darmstadt, Germany. Grupo Mecánica de Vuelo at ESA/ESOC - GMV Robert-Bosch-Straße 5, 64293 Darmstadt, Germany
| | - Walter Arnold
- 1. Physikalisches Institut, Georg August Universität, 37077 Göttingen, Germany; permanent address: Department of Materials Science, Saarland University, 66123 Saarbrücken, Germany
| | - Hans-Ulrich Auster
- Institut für Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig Mendelssohnstrasse 3, 38106 Braunschweig, Germany
| | - Carlos Casas
- European Space Agency/European Space Operations Centre (ESA/ESOC), Robert-Bosch-Straße 5, 64293 Darmstadt, Germany. Grupo Mecánica de Vuelo at ESA/ESOC - GMV Robert-Bosch-Straße 5, 64293 Darmstadt, Germany
| | - Claudia Faber
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | - Cinzia Fantinati
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Felix Finke
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Hans-Herbert Fischer
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Koen Geurts
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Carsten Güttler
- Max-Planck-Institut für Sonnensystemforschung (MPS), Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Philip Heinisch
- Institut für Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig Mendelssohnstrasse 3, 38106 Braunschweig, Germany
| | - Alain Herique
- Université Grenoble Alpes and CNRS, Institut de Planétologie et d'Astrophysique de Grenoble, F-38000 Grenoble, France
| | - Stubbe Hviid
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | - Günter Kargl
- Institut für Weltraumforschung (IWF) Graz, Austria Austrian Academy of Sciences, Space Research Institute, Schmiedlstraße 6, 8042 Graz, Austria
| | - Martin Knapmeyer
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | - Jörg Knollenberg
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | - Wlodek Kofman
- Université Grenoble Alpes and CNRS, Institut de Planétologie et d'Astrophysique de Grenoble, F-38000 Grenoble, France
| | - Norbert Kömle
- Institut für Weltraumforschung (IWF) Graz, Austria Austrian Academy of Sciences, Space Research Institute, Schmiedlstraße 6, 8042 Graz, Austria
| | - Ekkehard Kührt
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | - Valentina Lommatsch
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Stefano Mottola
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | - Ramon Pardo de Santayana
- European Space Agency/European Space Operations Centre (ESA/ESOC), Robert-Bosch-Straße 5, 64293 Darmstadt, Germany. Grupo Mecánica de Vuelo at ESA/ESOC - GMV Robert-Bosch-Straße 5, 64293 Darmstadt, Germany
| | - Emile Remetean
- Centre National d'Études Spatiales, 18 Avenue Édouard Belin, 31400 Toulouse, France
| | - Frank Scholten
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | | | - Holger Sierks
- Max-Planck-Institut für Sonnensystemforschung (MPS), Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Tilman Spohn
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
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