1
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Leone G, Tanaka HK. Igneous processes in the small bodies of the Solar System I. Asteroids and comets. iScience 2023; 26:107160. [PMID: 37534155 PMCID: PMC10391981 DOI: 10.1016/j.isci.2023.107160] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 08/04/2023] Open
Abstract
Igneous processes were quite widespread in the small bodies of the Solar System (SBSS) and were initially fueled by short-lived radioisotopes, the proto-Sun, impact heating, and differentiation heating. Once they finished, long-lived radioisotopes continued to warm the active bodies of the Earth, (possibly) Venus, and the cryovolcanism of Enceladus. The widespread presence of olivine and pyroxenes in planets and also in SBSS suggests that they were not necessarily the product of igneous processes and they might have been recycled from previous nebular processes or entrained in comets from interstellar space. The difference in temperature between the inner and the outer Solar System has clearly favored thermal annealing of the olivine close to the proto-Sun. Transport of olivine within the Solar System probably occurred also due to protostellar jets and winds but the entrainment in SBSS from interstellar space would overcome the requirement of initial turbulent regime in the protoplanetary nebula.
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Affiliation(s)
- Giovanni Leone
- Instituto de Investigación en Astronomía y Ciencias Planetarias, Universidad de Atacama, Chile
- Virtual Muography Institute, Global, Tokyo, Japan
| | - Hiroyuki K.M. Tanaka
- Virtual Muography Institute, Global, Tokyo, Japan
- International Muography Research Organization (MUOGRAPHIX), The University of Tokyo, Japan
- Earthquake Research Institute, The University of Tokyo, 1-1-1 Yayoi, Bunkyo, Tokyo 113-0032, Japan
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2
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Kelley MSP, Hsieh HH, Bodewits D, Saki M, Villanueva GL, Milam SN, Hammel HB. Spectroscopic identification of water emission from a main-belt comet. Nature 2023; 619:720-723. [PMID: 37187210 PMCID: PMC10371862 DOI: 10.1038/s41586-023-06152-y] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/16/2023] [Accepted: 04/28/2023] [Indexed: 05/17/2023]
Abstract
Main-belt comets are small Solar System bodies located in the asteroid belt that repeatedly exhibit comet-like activity (that is, dust comae or tails) during their perihelion passages, strongly indicating ice sublimation1,2. Although the existence of main-belt comets implies the presence of extant water ice in the asteroid belt, no gas has been detected around these objects despite intense scrutiny with the world's largest telescopes3. Here we present James Webb Space Telescope observations that clearly show that main-belt comet 238P/Read has a coma of water vapour, but lacks a significant CO2 gas coma. Our findings demonstrate that the activity of comet Read is driven by water-ice sublimation, and implies that main-belt comets are fundamentally different from the general cometary population. Whether or not comet Read experienced different formation circumstances or evolutionary history, it is unlikely to be a recent asteroid belt interloper from the outer Solar System. On the basis of these results, main-belt comets appear to represent a sample of volatile material that is currently unrepresented in observations of classical comets and the meteoritic record, making them important for understanding the early Solar System's volatile inventory and its subsequent evolution.
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Affiliation(s)
| | - Henry H Hsieh
- Planetary Science Institute, Tucson, AZ, USA
- Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan
| | - Dennis Bodewits
- Department of Physics, Auburn University, Edmund C. Leach Science Center, Auburn, AL, USA
| | - Mohammad Saki
- Department of Physics, Auburn University, Edmund C. Leach Science Center, Auburn, AL, USA
| | - Geronimo L Villanueva
- Solar System Exploration Division, NASA Goddard Space Flight Center, Code 690, Greenbelt, MD, USA
| | - Stefanie N Milam
- Solar System Exploration Division, NASA Goddard Space Flight Center, Code 690, Greenbelt, MD, USA
| | - Heidi B Hammel
- Association of Universities for Research in Astronomy, Washington, DC, USA
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3
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Juhas M. The World of Microorganisms. BRIEF LESSONS IN MICROBIOLOGY 2023:1-16. [DOI: 10.1007/978-3-031-29544-7_1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 09/02/2023]
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4
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Shi X, Castillo-Rogez J, Hsieh H, Hui H, Ip WH, Lei H, Li JY, Tosi F, Zhou L, Agarwal J, Barucci A, Beck P, Bagatin AC, Capaccioni F, Coates AJ, Cremonese G, Duffard R, Grande M, Jaumann R, Jones GH, Kallio E, Lin Y, Mousis O, Nathues A, Oberst J, Sierks H, Ulamec S, Wang M. GAUSS - genesis of asteroids and evolution of the solar system: A sample return mission to Ceres. EXPERIMENTAL ASTRONOMY 2021; 54:713-744. [PMID: 36915624 PMCID: PMC9998589 DOI: 10.1007/s10686-021-09800-1] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 07/30/2020] [Accepted: 09/23/2021] [Indexed: 06/18/2023]
Abstract
The goal of Project GAUSS (Genesis of Asteroids and evolUtion of the Solar System) is to return samples from the dwarf planet Ceres. Ceres is the most accessible candidate of ocean worlds and the largest reservoir of water in the inner Solar System. It shows active volcanism and hydrothermal activities in recent history. Recent evidence for the existence of a subsurface ocean on Ceres and the complex geochemistry suggest past habitability and even the potential for ongoing habitability. GAUSS will return samples from Ceres with the aim of answering the following top-level scientific questions: What is the origin of Ceres and what does this imply for the origin of water and other volatiles in the inner Solar System?What are the physical properties and internal structure of Ceres? What do they tell us about the evolutionary and aqueous alteration history of dwarf planets?What are the astrobiological implications of Ceres? Is it still habitable today?What are the mineralogical connections between Ceres and our current collections of carbonaceous meteorites?
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Affiliation(s)
- Xian Shi
- Max Planck Institute for Solar System Research, Göttingen, Germany
- Present Address: Shanghai Astronomical Observatory, Shanghai, China
| | | | | | - Hejiu Hui
- School of Earth Sciences and Engineering, Nanjing University, Nanjing, China
| | - Wing-Huen Ip
- Institute of Astronomy and Space Science, National Central University, Chung Li, Taiwan
| | - Hanlun Lei
- School of Astronomy and Space Science, Nanjing University, Nanjing, China
| | | | - Federico Tosi
- Istituto Nazionale di AstroFisica – Istituto di Astrofisica e Planetologia Spaziali (INAF-IAPS), Rome, Italy
| | - Liyong Zhou
- School of Astronomy and Space Science, Nanjing University, Nanjing, China
| | - Jessica Agarwal
- Max Planck Institute for Solar System Research, Göttingen, Germany
- Institute for Geophysics and Extraterrestrial Physics, Technical University Braunschweig, Braunschweig, Germany
| | - Antonella Barucci
- LESIA-Observatoire de Paris, Université PSL, CNRS, Université de Paris, Sorbonne Université, F-92195 Meudon, Principal Cedex, France
| | - Pierre Beck
- CNRS Institut de Planétologie et d’Astrophysique, Univ. Grenoble Alpes, Grenoble, France
| | - Adriano Campo Bagatin
- Universidad de Alicante, Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Alicante, Spain
| | - Fabrizio Capaccioni
- Istituto Nazionale di AstroFisica – Istituto di Astrofisica e Planetologia Spaziali (INAF-IAPS), Rome, Italy
| | - Andrew J. Coates
- Mullard Space Science Laboratory, University College London, Surrey, UK
| | | | - Rene Duffard
- Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain
| | | | - Ralf Jaumann
- Institute of Geological Sciences, Free University of Berlin, Berlin, Germany
| | - Geraint H. Jones
- Mullard Space Science Laboratory, University College London, Surrey, UK
| | - Esa Kallio
- School of Electrical Engineering, Aalto University, Aalto, Finland
| | - Yangting Lin
- Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | | | - Andreas Nathues
- Max Planck Institute for Solar System Research, Göttingen, Germany
| | - Jürgen Oberst
- DLR Institute of Planetary Research, Berlin, Germany
| | - Holger Sierks
- Max Planck Institute for Solar System Research, Göttingen, Germany
| | - Stephan Ulamec
- DLR Space Operations and Astronaut Training, Cologne, Germany
| | - Mingyuan Wang
- National Astronomical Observatory, Chinese Academy of Science, Beijing, China
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5
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Abstract
Ceres is the largest object in the main belt and it is also the most water-rich body in the inner solar system besides the Earth. The discoveries made by the Dawn Mission revealed that the composition of Ceres includes organic material, with a component of carbon globally present and also a high quantity of localized aliphatic organics in specific areas. The inferred mineralogy of Ceres indicates the long-term activity of a large body of liquid water that produced the alteration minerals discovered on its surface, including ammonia-bearing minerals. To explain the presence of ammonium in the phyllosilicates, Ceres must have accreted organic matter, ammonia, water and carbon present in the protoplanetary formation region. It is conceivable that Ceres may have also processed and transformed its own original organic matter that could have been modified by the pervasive hydrothermal alteration. The coexistence of phyllosilicates, magnetite, carbonates, salts, organics and a high carbon content point to rock–water alteration playing an important role in promoting widespread carbon occurrence.
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6
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Laboratory Investigations Coupled to VIR/Dawn Observations to Quantify the Large Concentrations of Organic Matter on Ceres. MINERALS 2021. [DOI: 10.3390/min11070719] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 01/28/2023]
Abstract
Organic matter directly observed at the surface of an inner planetary body is quite infrequent due to the usual low abundance of such matter and the limitation of the infrared technique. Fortuitously, the Dawn mission has revealed, thanks to the Visible and InfraRed mapping spectrometer (VIR), large areas rich in organic matter at the surface of Ceres, near Ernutet crater. The origin of the organic matter and its abundance in association with minerals, as indicated by the low altitude VIR data, remains unclear, but multiple lines of evidence support an endogenous origin. Here, we report an experimental investigation to determine the abundance of the aliphatic carbon signature observed on Ceres. We produced relevant analogues containing ammoniated-phyllosilicates, carbonates, aliphatic carbons (coals), and magnetite or amorphous carbon as darkening agents, and measured their reflectance by infrared spectroscopy. Measurements of these organic-rich analogues were directly compared to the VIR spectra taken from different locations around Ernutet crater. We found that the absolute reflectance of our analogues is at least two orders of magnitude higher than Ceres, but the depths of absorption bands match nicely the ones of the organic-rich Ceres spectra. The choices of the different components are discussed in comparison with VIR data. Relative abundances of the components are extrapolated from the spectra and mixture composition, considering that the differences in reflectance level is mainly due to optical effects. Absorption bands of Ceres’ organic-rich spectra are best reproduced by around 20 wt.% of carbon (a third being aliphatic carbons), in association with around 20 wt.% of carbonates, 15 wt.% of ammoniated-phyllosilicate, 20 wt.% of Mg-phyllosilicates, and 25 wt.% of darkening agent. Results also highlight the pertinence to use laboratory analogues in addition to models for planetary surface characterization. Such large quantities of organic materials near Ernutet crater, in addition to the amorphous carbon suspected on a global scale, requires a concentration mechanism whose nature is still unknown but that could potentially be relevant to other large volatile-rich bodies.
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7
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Simon AA, Kaplan HH, Hamilton VE, Lauretta DS, Campins H, Emery JP, Barucci MA, DellaGiustina DN, Reuter DC, Sandford SA, Golish DR, Lim LF, Ryan A, Rozitis B, Bennett CA. Widespread carbon-bearing materials on near-Earth asteroid (101955) Bennu. Science 2020; 370:science.abc3522. [PMID: 33033153 DOI: 10.1126/science.abc3522] [Citation(s) in RCA: 40] [Impact Index Per Article: 10.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/20/2020] [Accepted: 08/27/2020] [Indexed: 11/02/2022]
Abstract
Asteroid (101955) Bennu is a dark asteroid on an Earth-crossing orbit that is thought to have assembled from the fragments of an ancient collision. We use spatially resolved visible and near-infrared spectra of Bennu to investigate its surface properties and composition. In addition to a hydrated phyllosilicate band, we detect a ubiquitous 3.4-micrometer absorption feature, which we attribute to a mix of organic and carbonate materials. The shape and depth of this absorption feature vary across Bennu's surface, spanning the range seen among similar main-belt asteroids. The distribution of the absorption feature does not correlate with temperature, reflectance, spectral slope, or hydrated minerals, although some of those characteristics correlate with each other. The deepest 3.4-micrometer absorptions occur on individual boulders. The variations may be due to differences in abundance, recent exposure, or space weathering.
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Affiliation(s)
- Amy A Simon
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA.
| | | | | | - Dante S Lauretta
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - Humberto Campins
- Department of Physics, University of Central Florida, Orlando, FL, USA
| | - Joshua P Emery
- Department of Astronomy and Planetary Sciences, Northern Arizona University, Flagstaff, AZ, USA
| | - M Antonietta Barucci
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, Université Paris Sciences et Lettres, Centre National de la Recherche Scientifique, Université de Paris, Sorbonne Université, Meudon, France
| | | | - Dennis C Reuter
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | | | - Dathon R Golish
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - Lucy F Lim
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Andrew Ryan
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - Benjamin Rozitis
- School of Physical Sciences, The Open University, Milton Keynes, UK
| | - Carina A Bennett
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
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8
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Kaplan HH, Lauretta DS, Simon AA, Hamilton VE, DellaGiustina DN, Golish DR, Reuter DC, Bennett CA, Burke KN, Campins H, Connolly HC, Dworkin JP, Emery JP, Glavin DP, Glotch TD, Hanna R, Ishimaru K, Jawin ER, McCoy TJ, Porter N, Sandford SA, Ferrone S, Clark BE, Li JY, Zou XD, Daly MG, Barnouin OS, Seabrook JA, Enos HL. Bright carbonate veins on asteroid (101955) Bennu: Implications for aqueous alteration history. Science 2020; 370:science.abc3557. [PMID: 33033155 DOI: 10.1126/science.abc3557] [Citation(s) in RCA: 47] [Impact Index Per Article: 11.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/20/2020] [Accepted: 09/24/2020] [Indexed: 11/02/2022]
Abstract
The composition of asteroids and their connection to meteorites provide insight into geologic processes that occurred in the early Solar System. We present spectra of the Nightingale crater region on near-Earth asteroid Bennu with a distinct infrared absorption around 3.4 micrometers. Corresponding images of boulders show centimeters-thick, roughly meter-long bright veins. We interpret the veins as being composed of carbonates, similar to those found in aqueously altered carbonaceous chondrite meteorites. If the veins on Bennu are carbonates, fluid flow and hydrothermal deposition on Bennu's parent body would have occurred on kilometer scales for thousands to millions of years. This suggests large-scale, open-system hydrothermal alteration of carbonaceous asteroids in the early Solar System.
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Affiliation(s)
- H H Kaplan
- NASA Goddard Space Flight Center, Greenbelt, MD, USA. .,Southwest Research Institute, Boulder, CO, USA
| | - D S Lauretta
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - A A Simon
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | | | - D N DellaGiustina
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - D R Golish
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - D C Reuter
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - C A Bennett
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - K N Burke
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - H Campins
- Department of Physics, University of Central Florida, Orlando, FL, USA
| | - H C Connolly
- Department of Geology, School of Earth and Environment, Rowan University, Glassboro, NJ, USA.,Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - J P Dworkin
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - J P Emery
- Department of Astronomy and Planetary Sciences, Northern Arizona University, Flagstaff, AZ, USA
| | - D P Glavin
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - T D Glotch
- Department of Geosciences, Stony Brook University, Stony Brook, NY, USA
| | - R Hanna
- Jackson School of Geosciences, University of Texas, Austin, TX, USA
| | - K Ishimaru
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - E R Jawin
- Smithsonian Institution National Museum of Natural History, Washington, DC, USA
| | - T J McCoy
- Smithsonian Institution National Museum of Natural History, Washington, DC, USA
| | - N Porter
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - S A Sandford
- NASA Ames Research Center, Mountain View, CA, USA
| | - S Ferrone
- Department of Physics and Astronomy, Ithaca College, Ithaca, NY, USA
| | - B E Clark
- Department of Physics and Astronomy, Ithaca College, Ithaca, NY, USA
| | - J-Y Li
- Planetary Science Institute, Tucson, AZ, USA
| | - X-D Zou
- Planetary Science Institute, Tucson, AZ, USA
| | - M G Daly
- Centre for Research in Earth and Space Science, York University, Toronto, Ontario, Canada
| | - O S Barnouin
- John Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - J A Seabrook
- Centre for Research in Earth and Space Science, York University, Toronto, Ontario, Canada
| | - H L Enos
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
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9
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Poch O, Istiqomah I, Quirico E, Beck P, Schmitt B, Theulé P, Faure A, Hily-Blant P, Bonal L, Raponi A, Ciarniello M, Rousseau B, Potin S, Brissaud O, Flandinet L, Filacchione G, Pommerol A, Thomas N, Kappel D, Mennella V, Moroz L, Vinogradoff V, Arnold G, Erard S, Bockelée-Morvan D, Leyrat C, Capaccioni F, De Sanctis MC, Longobardo A, Mancarella F, Palomba E, Tosi F. Ammonium salts are a reservoir of nitrogen on a cometary nucleus and possibly on some asteroids. Science 2020; 367:367/6483/eaaw7462. [PMID: 32165559 DOI: 10.1126/science.aaw7462] [Citation(s) in RCA: 17] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/21/2019] [Revised: 10/11/2019] [Accepted: 02/14/2020] [Indexed: 11/02/2022]
Abstract
The measured nitrogen-to-carbon ratio in comets is lower than for the Sun, a discrepancy which could be alleviated if there is an unknown reservoir of nitrogen in comets. The nucleus of comet 67P/Churyumov-Gerasimenko exhibits an unidentified broad spectral reflectance feature around 3.2 micrometers, which is ubiquitous across its surface. On the basis of laboratory experiments, we attribute this absorption band to ammonium salts mixed with dust on the surface. The depth of the band indicates that semivolatile ammonium salts are a substantial reservoir of nitrogen in the comet, potentially dominating over refractory organic matter and more volatile species. Similar absorption features appear in the spectra of some asteroids, implying a compositional link between asteroids, comets, and the parent interstellar cloud.
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Affiliation(s)
- Olivier Poch
- Université Grenoble Alpes, Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France.
| | - Istiqomah Istiqomah
- Université Grenoble Alpes, Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France
| | - Eric Quirico
- Université Grenoble Alpes, Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France
| | - Pierre Beck
- Université Grenoble Alpes, Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France.,Institut Universitaire de France (IUF), Paris, France
| | - Bernard Schmitt
- Université Grenoble Alpes, Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France
| | - Patrice Theulé
- Aix-Marseille Université, CNRS, Centre National d'Etudes Spatiales (CNES), Laboratoire d'Astrophysique de Marseille (LAM), Marseille, France
| | - Alexandre Faure
- Université Grenoble Alpes, Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France
| | - Pierre Hily-Blant
- Université Grenoble Alpes, Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France
| | - Lydie Bonal
- Université Grenoble Alpes, Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France
| | - Andrea Raponi
- Istituto di Astrofisica e Planetologia Spaziali (IAPS), Istituto Nazionale di Astrofisica (INAF), 00133 Rome, Italy
| | - Mauro Ciarniello
- Istituto di Astrofisica e Planetologia Spaziali (IAPS), Istituto Nazionale di Astrofisica (INAF), 00133 Rome, Italy
| | - Batiste Rousseau
- Université Grenoble Alpes, Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France
| | - Sandra Potin
- Université Grenoble Alpes, Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France
| | - Olivier Brissaud
- Université Grenoble Alpes, Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France
| | - Laurène Flandinet
- Université Grenoble Alpes, Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France
| | - Gianrico Filacchione
- Istituto di Astrofisica e Planetologia Spaziali (IAPS), Istituto Nazionale di Astrofisica (INAF), 00133 Rome, Italy
| | - Antoine Pommerol
- Physikalisches Institut, Sidlerstrasse 5, University of Bern, CH-3012 Bern, Switzerland
| | - Nicolas Thomas
- Physikalisches Institut, Sidlerstrasse 5, University of Bern, CH-3012 Bern, Switzerland
| | - David Kappel
- Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam, Germany.,Institute for Planetary Research, German Aerospace Center (DLR), 12489 Berlin, Germany
| | - Vito Mennella
- Istituto Nazionale di Astrofisica (INAF)-Osservatorio Astronomico di Capodimonte, Napoli, Italy
| | - Lyuba Moroz
- Institute for Planetary Research, German Aerospace Center (DLR), 12489 Berlin, Germany
| | - Vassilissa Vinogradoff
- CNRS, Aix-Marseille Université, Laboratoire Physique des Interactions Ioniques et Moléculaires (PIIM), Unité Mixte de Recherche (UMR) CNRS 7345, 13397 Marseille, France
| | - Gabriele Arnold
- Institute for Planetary Research, German Aerospace Center (DLR), 12489 Berlin, Germany
| | - Stéphane Erard
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris, Université Paris Sciences et Lettres (PSL), CNRS, Sorbonne Université, Université de Paris, 92195 Meudon, France
| | - Dominique Bockelée-Morvan
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris, Université Paris Sciences et Lettres (PSL), CNRS, Sorbonne Université, Université de Paris, 92195 Meudon, France
| | - Cédric Leyrat
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris, Université Paris Sciences et Lettres (PSL), CNRS, Sorbonne Université, Université de Paris, 92195 Meudon, France
| | - Fabrizio Capaccioni
- Istituto di Astrofisica e Planetologia Spaziali (IAPS), Istituto Nazionale di Astrofisica (INAF), 00133 Rome, Italy
| | - Maria Cristina De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali (IAPS), Istituto Nazionale di Astrofisica (INAF), 00133 Rome, Italy
| | - Andrea Longobardo
- Istituto di Astrofisica e Planetologia Spaziali (IAPS), Istituto Nazionale di Astrofisica (INAF), 00133 Rome, Italy.,Dipartimento di Scienze e Tecnologie (DIST), Università Parthenope, 80143 Napoli, Italy
| | - Francesca Mancarella
- Dipartimento di Matematica e Fisica "E. De Giorgi," Università del Salento, Lecce, Italy
| | - Ernesto Palomba
- Istituto di Astrofisica e Planetologia Spaziali (IAPS), Istituto Nazionale di Astrofisica (INAF), 00133 Rome, Italy
| | - Federico Tosi
- Istituto di Astrofisica e Planetologia Spaziali (IAPS), Istituto Nazionale di Astrofisica (INAF), 00133 Rome, Italy
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Abstract
Recent dynamical analyses suggest that some Jupiter family comets (JFCs) may originate in the main asteroid belt instead of the outer solar system. This possibility is particularly interesting given evidence that icy main-belt objects are known to be present in the Themis asteroid family. We report results from dynamical analyses specifically investigating the possibility that icy Themis family members could contribute to the observed population of JFCs. Numerical integrations show that such dynamical evolution is indeed possible via a combination of eccentricity excitation apparently driven by the nearby 2:1 mean-motion resonance with Jupiter, gravitational interactions with planets other than Jupiter, and the Yarkovsky effect. We estimate that, at any given time, there may be tens of objects from the Themis family on JFC-like orbits with the potential to mimic active JFCs from the outer solar system, although not all, or even any, may necessarily be observably active. We find that dynamically evolved Themis family objects on JFC-like orbits have semimajor axes between 3.15 au and 3.40 au for the vast majority of their time on such orbits, consistent with the strong role that the 2:1 mean-motion resonance with Jupiter likely plays in their dynamical evolution. We conclude that a contribution from the Themis family to the active JFC population is plausible, although further work is needed to better characterize this contribution.
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11
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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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12
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Zhu C, Crandall PB, Gillis-Davis JJ, Ishii HA, Bradley JP, Corley LM, Kaiser RI. Untangling the formation and liberation of water in the lunar regolith. Proc Natl Acad Sci U S A 2019; 116:11165-11170. [PMID: 31110011 PMCID: PMC6561281 DOI: 10.1073/pnas.1819600116] [Citation(s) in RCA: 31] [Impact Index Per Article: 6.2] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
The source of water (H2O) and hydroxyl radicals (OH), identified on the lunar surface, represents a fundamental, unsolved puzzle. The interaction of solar-wind protons with silicates and oxides has been proposed as a key mechanism, but laboratory experiments yield conflicting results that suggest that proton implantation alone is insufficient to generate and liberate water. Here, we demonstrate in laboratory simulation experiments combined with imaging studies that water can be efficiently generated and released through rapid energetic heating like micrometeorite impacts into anhydrous silicates implanted with solar-wind protons. These synergistic effects of solar-wind protons and micrometeorites liberate water at mineral temperatures from 10 to 300 K via vesicles, thus providing evidence of a key mechanism to synthesize water in silicates and advancing our understanding on the origin of water as detected on the Moon and other airless bodies in our solar system such as Mercury and asteroids.
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Affiliation(s)
- Cheng Zhu
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822
- W. M. Keck Laboratory in Astrochemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822
| | - Parker B Crandall
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822
- W. M. Keck Laboratory in Astrochemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822
| | - Jeffrey J Gillis-Davis
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822
| | - Hope A Ishii
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822
| | - John P Bradley
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822
| | - Laura M Corley
- Hawai'i Institute of Geophysics and Planetology, University of Hawai'i at Mānoa, Honolulu, HI 96822
| | - Ralf I Kaiser
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822;
- W. M. Keck Laboratory in Astrochemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822
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13
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Noun M, Baklouti D, Brunetto R, Borondics F, Calligaro T, Dionnet Z, Le Sergeant d'Hendecourt L, Nsouli B, Ribaud I, Roumie M, Della-Negra S. A Mineralogical Context for the Organic Matter in the Paris Meteorite Determined by A Multi-Technique Analysis. Life (Basel) 2019; 9:E44. [PMID: 31151218 PMCID: PMC6617381 DOI: 10.3390/life9020044] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/30/2019] [Revised: 05/17/2019] [Accepted: 05/25/2019] [Indexed: 11/25/2022] Open
Abstract
This study is a multi-technique investigation of the Paris carbonaceous chondrite directly applied on two selected 500 × 500 µm² areas of a millimetric fragment, without any chemical extraction. By mapping the partial hydration of the amorphous silicate phase dominating the meteorite sample matrix, infrared spectroscopy gave an interesting glimpse into the way the fluid may have circulated into the sample and partially altered it. The TOF-SIMS in-situ analysis allowed the studying and mapping of the wide diversity of chemical moieties composing the meteorite organic content. The results of the combined techniques show that at the micron scale, the organic matter was always spatially associated with the fine-grained and partially-hydrated amorphous silicates and to the presence of iron in different chemical states. These systematic associations, illustrated in previous studies of other carbonaceous chondrites, were further supported by the identification by TOF-SIMS of cyanide and/or cyanate salts that could be direct remnants of precursor ices that accreted with dust during the parent body formation, and by the detection of different metal-containing large organic ions. Finally, the results obtained emphasized the importance of studying the specific interactions taking place between organic and mineral phases in the chondrite matrix, in order to investigate their role in the evolution story of primitive organic matter in meteorite parent bodies.
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Affiliation(s)
- Manale Noun
- Institut de Physique Nucléaire d'Orsay, UMR 8608, CNRS/IN2P3, Université Paris-Sud, Université Paris-Saclay, F-91406 Orsay, France.
- Lebanese Atomic Energy Commission, NCSR, Beirut 11-8281, Lebanon.
| | - Donia Baklouti
- Institut d'Astrophysique Spatiale, UMR 8617, CNRS/Université Paris-Sud, Université Paris-Saclay, bâtiment 121, Université Paris-Sud, 91405 Orsay CEDEX, France.
| | - Rosario Brunetto
- Institut d'Astrophysique Spatiale, UMR 8617, CNRS/Université Paris-Sud, Université Paris-Saclay, bâtiment 121, Université Paris-Sud, 91405 Orsay CEDEX, France.
| | - Ferenc Borondics
- Synchrotron Soleil, L'Orme des Merisiers, BP48, Saint Aubin, 91192 Gif sur Yvette CEDEX, France.
| | - Thomas Calligaro
- Centre de Recherche et de Restauration des musées de France, UMR 171, Palais du Louvre, 75001 Paris, France.
- PSL Research University, Institut de Recherche Chimie Paris, Chimie ParisTech, CNRS UMR 8247, 75005 Paris, France.
| | - Zélia Dionnet
- Institut d'Astrophysique Spatiale, UMR 8617, CNRS/Université Paris-Sud, Université Paris-Saclay, bâtiment 121, Université Paris-Sud, 91405 Orsay CEDEX, France.
- Università degli Studi di Napoli Parthenope, Dip. di Scienze e Tecnologie, CDN IC4, I-80143 Naples, Italy.
| | - Louis Le Sergeant d'Hendecourt
- Institut d'Astrophysique Spatiale, UMR 8617, CNRS/Université Paris-Sud, Université Paris-Saclay, bâtiment 121, Université Paris-Sud, 91405 Orsay CEDEX, France.
- Université Aix-Marseille, Laboratoire de Physique des Interactions Ioniques et Moléculaires (PIIM), UMR CNRS 7345, F-13397 Marseille, France.
| | - Bilal Nsouli
- Lebanese Atomic Energy Commission, NCSR, Beirut 11-8281, Lebanon.
| | - Isabelle Ribaud
- Institut de Physique Nucléaire d'Orsay, UMR 8608, CNRS/IN2P3, Université Paris-Sud, Université Paris-Saclay, F-91406 Orsay, France.
| | - Mohamad Roumie
- Lebanese Atomic Energy Commission, NCSR, Beirut 11-8281, Lebanon.
| | - Serge Della-Negra
- Institut de Physique Nucléaire d'Orsay, UMR 8608, CNRS/IN2P3, Université Paris-Sud, Université Paris-Saclay, F-91406 Orsay, France.
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14
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Kitazato K, Milliken RE, Iwata T, Abe M, Ohtake M, Matsuura S, Arai T, Nakauchi Y, Nakamura T, Matsuoka M, Senshu H, Hirata N, Hiroi T, Pilorget C, Brunetto R, Poulet F, Riu L, Bibring JP, Takir D, Domingue DL, Vilas F, Barucci MA, Perna D, Palomba E, Galiano A, Tsumura K, Osawa T, Komatsu M, Nakato A, Arai T, Takato N, Matsunaga T, Takagi Y, Matsumoto K, Kouyama T, Yokota Y, Tatsumi E, Sakatani N, Yamamoto Y, Okada T, Sugita S, Honda R, Morota T, Kameda S, Sawada H, Honda C, Yamada M, Suzuki H, Yoshioka K, Hayakawa M, Ogawa K, Cho Y, Shirai K, Shimaki Y, Hirata N, Yamaguchi A, Ogawa N, Terui F, Yamaguchi T, Takei Y, Saiki T, Nakazawa S, Tanaka S, Yoshikawa M, Watanabe S, Tsuda Y. The surface composition of asteroid 162173 Ryugu from Hayabusa2 near-infrared spectroscopy. Science 2019; 364:272-275. [PMID: 30890589 DOI: 10.1126/science.aav7432] [Citation(s) in RCA: 40] [Impact Index Per Article: 8.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/26/2018] [Accepted: 03/07/2019] [Indexed: 11/02/2022]
Abstract
The near-Earth asteroid 162173 Ryugu, the target of the Hayabusa2 sample-return mission, is thought to be a primitive carbonaceous object. We report reflectance spectra of Ryugu's surface acquired with the Near-Infrared Spectrometer (NIRS3) on Hayabusa2, to provide direct measurements of the surface composition and geological context for the returned samples. A weak, narrow absorption feature centered at 2.72 micrometers was detected across the entire observed surface, indicating that hydroxyl (OH)-bearing minerals are ubiquitous there. The intensity of the OH feature and low albedo are similar to thermally and/or shock-metamorphosed carbonaceous chondrite meteorites. There are few variations in the OH-band position, which is consistent with Ryugu being a compositionally homogeneous rubble-pile object generated from impact fragments of an undifferentiated aqueously altered parent body.
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Affiliation(s)
- K Kitazato
- The University of Aizu, Fukushima, Japan.
| | | | - T Iwata
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan.,The Graduate University for Advanced Studies (SOKENDAI), Kanagawa, Japan
| | - M Abe
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan.,The Graduate University for Advanced Studies (SOKENDAI), Kanagawa, Japan
| | - M Ohtake
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan.,The Graduate University for Advanced Studies (SOKENDAI), Kanagawa, Japan
| | | | - T Arai
- Ashikaga University, Tochigi, Japan
| | - Y Nakauchi
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | | | - M Matsuoka
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - H Senshu
- Chiba Institute of Technology, Chiba, Japan
| | - N Hirata
- The University of Aizu, Fukushima, Japan
| | - T Hiroi
- Brown University, Providence, RI, USA
| | - C Pilorget
- Institut d'Astrophysique Spatial, Université Paris-Sud, Orsay, France
| | - R Brunetto
- Institut d'Astrophysique Spatial, Université Paris-Sud, Orsay, France
| | - F Poulet
- Institut d'Astrophysique Spatial, Université Paris-Sud, Orsay, France
| | - L Riu
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - J-P Bibring
- Institut d'Astrophysique Spatial, Université Paris-Sud, Orsay, France
| | - D Takir
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX, USA
| | | | - F Vilas
- Planetary Science Institute, Tucson, AZ, USA
| | - M A Barucci
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris, Meudon, France
| | - D Perna
- Osservatorio Astronomico di Roma, Istituto Nazionale di Astrofisica (INAF), Monte Porzio Catone, Italy.,Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris, Meudon, France
| | - E Palomba
- Istituto di Astrofisica e Planetologia Spaziali, INAF, Roma, Italy
| | - A Galiano
- Istituto di Astrofisica e Planetologia Spaziali, INAF, Roma, Italy
| | - K Tsumura
- Tohoku University, Sendai, Japan.,Tokyo City University, Tokyo, Japan
| | - T Osawa
- Japan Atomic Energy Agency, Ibaraki, Japan
| | - M Komatsu
- The Graduate University for Advanced Studies (SOKENDAI), Kanagawa, Japan
| | - A Nakato
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - T Arai
- Chiba Institute of Technology, Chiba, Japan
| | - N Takato
- National Astronomical Observatory of Japan, Tokyo, Japan.,The Graduate University for Advanced Studies (SOKENDAI), Kanagawa, Japan
| | - T Matsunaga
- National Institute for Environmental Studies, Ibaraki, Japan
| | - Y Takagi
- Aichi Toho University, Nagoya, Japan
| | - K Matsumoto
- National Astronomical Observatory of Japan, Tokyo, Japan.,The Graduate University for Advanced Studies (SOKENDAI), Kanagawa, Japan
| | - T Kouyama
- National Institute of Advanced Industrial Science and Technology, Tokyo, Japan
| | - Y Yokota
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan.,Kochi University, Kochi, Japan
| | - E Tatsumi
- The University of Tokyo, Tokyo, Japan
| | - N Sakatani
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - Y Yamamoto
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan.,The Graduate University for Advanced Studies (SOKENDAI), Kanagawa, Japan
| | - T Okada
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan.,The University of Tokyo, Tokyo, Japan
| | - S Sugita
- The University of Tokyo, Tokyo, Japan
| | - R Honda
- Kochi University, Kochi, Japan
| | - T Morota
- Nagoya University, Nagoya, Japan
| | | | - H Sawada
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - C Honda
- The University of Aizu, Fukushima, Japan
| | - M Yamada
- Chiba Institute of Technology, Chiba, Japan
| | | | | | - M Hayakawa
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - K Ogawa
- Kobe University, Kobe, Japan
| | - Y Cho
- The University of Tokyo, Tokyo, Japan
| | - K Shirai
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - Y Shimaki
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | | | - A Yamaguchi
- National Institute of Polar Research, Tokyo, Japan.,The Graduate University for Advanced Studies (SOKENDAI), Kanagawa, Japan
| | - N Ogawa
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - F Terui
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - T Yamaguchi
- Mitsubishi Electric Corporation, Kanagawa, Japan
| | - Y Takei
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - T Saiki
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - S Nakazawa
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - S Tanaka
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan.,The Graduate University for Advanced Studies (SOKENDAI), Kanagawa, Japan
| | - M Yoshikawa
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan.,The Graduate University for Advanced Studies (SOKENDAI), Kanagawa, Japan
| | - S Watanabe
- Nagoya University, Nagoya, Japan.,Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan
| | - Y Tsuda
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Japan.,The Graduate University for Advanced Studies (SOKENDAI), Kanagawa, Japan
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15
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Hamilton VE, Simon AA, Christensen PR, Reuter DC, Clark BE, Barucci MA, Bowles NE, Boynton WV, Brucato JR, Cloutis EA, Connolly HC, Hanna KLD, Emery JP, Enos HL, Fornasier S, Haberle CW, Hanna RD, Howell ES, Kaplan HH, Keller LP, Lantz C, Li JY, Lim LF, McCoy TJ, Merlin F, Nolan MC, Praet A, Rozitis B, Sandford SA, Schrader DL, Thomas CA, Zou XD, Lauretta DS. Evidence for widespread hydrated minerals on asteroid (101955) Bennu. NATURE ASTRONOMY 2019; 3:332-340. [PMID: 31360777 PMCID: PMC6662227 DOI: 10.1038/s41550-019-0722-2] [Citation(s) in RCA: 46] [Impact Index Per Article: 9.2] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/29/2019] [Accepted: 02/12/2019] [Indexed: 05/18/2023]
Abstract
Early spectral data from the Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) mission reveal evidence for abundant hydrated minerals on the surface of near-Earth asteroid (101955) Bennu in the form of a near-infrared absorption near 2.7 μm and thermal infrared spectral features that are most similar to those of aqueously altered CM carbonaceous chondrites. We observe these spectral features across the surface of Bennu, and there is no evidence of substantial rotational variability at the spatial scales of tens to hundreds of meters observed to date. In the visible and near-infrared (0.4 to 2.4 μm) Bennu's spectrum appears featureless and with a blue (negative) slope, confirming previous ground-based observations. Bennu may represent a class of objects that could have brought volatiles and organic chemistry to Earth.
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Affiliation(s)
- V. E. Hamilton
- Department of Space Studies, Southwest Research Institute, Boulder, CO, USA
| | - A. A. Simon
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - P. R. Christensen
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | - D. C. Reuter
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - B. E. Clark
- Department of Physics and Astronomy, Ithaca College, Ithaca, NY, USA
| | | | - N. E. Bowles
- Department of Atmospheric, Oceanic and Planetary Physics, University of Oxford, Oxford, UK
| | - W. V. Boynton
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - J. R. Brucato
- INAF-Astrophysical Observatory of Arcetri, Firenze, Italy
| | - E. A. Cloutis
- Department of Geography, University of Winnipeg, Winnipeg, Canada
| | - H. C. Connolly
- Department of Geology, Rowan University, Glassboro, NJ, USA
| | - K. L. Donaldson Hanna
- Department of Atmospheric, Oceanic and Planetary Physics, University of Oxford, Oxford, UK
| | - J. P. Emery
- Department of Earth and Planetary Science, University of Tennessee, Knoxville, TN, USA
| | - H. L. Enos
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | | | - C. W. Haberle
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | - R. D. Hanna
- Jackson School of Geosciences, University of Texas, Austin, TX, USA
| | - E. S. Howell
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - H. H. Kaplan
- Department of Space Studies, Southwest Research Institute, Boulder, CO, USA
| | - L. P. Keller
- ARES, NASA Johnson Space Center, Houston, TX USA
| | - C. Lantz
- Institut d’Astrophysique Spatiale, CNRS/Université Paris Sud, Orsay, France
| | - J.-Y. Li
- Planetary Science Institute, Tucson, AZ, USA
| | - L. F. Lim
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - T. J. McCoy
- Smithsonian Institution, National Museum of Natural History, Washington, D.C., USA
| | - F. Merlin
- LESIA, Observatoire de Paris, France
| | - M. C. Nolan
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - A. Praet
- LESIA, Observatoire de Paris, France
| | - B. Rozitis
- Planetary and Space Sciences, The Open University, Milton Keynes, UK
| | | | - D. L. Schrader
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | - C. A. Thomas
- Department of Physics and Astronomy, Northern Arizona University, Flagstaff, AZ, USA
| | - X.-D. Zou
- Planetary Science Institute, Tucson, AZ, USA
| | - D. S. Lauretta
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
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16
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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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17
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De Sanctis MC, Ammannito E, McSween HY, Raponi A, Marchi S, Capaccioni F, Capria MT, Carrozzo FG, Ciarniello M, Fonte S, Formisano M, Frigeri A, Giardino M, Longobardo A, Magni G, McFadden LA, Palomba E, Pieters CM, Tosi F, Zambon F, Raymond CA, Russell CT. Localized aliphatic organic material on the surface of Ceres. Science 2017; 355:719-722. [PMID: 28209893 DOI: 10.1126/science.aaj2305] [Citation(s) in RCA: 132] [Impact Index Per Article: 18.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/16/2016] [Accepted: 01/17/2017] [Indexed: 11/02/2022]
Abstract
Organic compounds occur in some chondritic meteorites, and their signatures on solar system bodies have been sought for decades. Spectral signatures of organics have not been unambiguously identified on the surfaces of asteroids, whereas they have been detected on cometary nuclei. Data returned by the Visible and InfraRed Mapping Spectrometer on board the Dawn spacecraft show a clear detection of an organic absorption feature at 3.4 micrometers on dwarf planet Ceres. This signature is characteristic of aliphatic organic matter and is mainly localized on a broad region of ~1000 square kilometers close to the ~50-kilometer Ernutet crater. The combined presence on Ceres of ammonia-bearing hydrated minerals, water ice, carbonates, salts, and organic material indicates a very complex chemical environment, suggesting favorable environments to prebiotic chemistry.
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Affiliation(s)
- M C De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - E Ammannito
- Earth Planetary and Space Sciences, University of California-Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA.,Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - H Y McSween
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996-1410, USA
| | - A Raponi
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - S Marchi
- Southwest Research Institute, Boulder, CO 80302, USA.,Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - F Capaccioni
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M T Capria
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - F G Carrozzo
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M Ciarniello
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - S Fonte
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M Formisano
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - A Frigeri
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M Giardino
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - A Longobardo
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - G Magni
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - L A McFadden
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - E Palomba
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - C M Pieters
- Brown University, Department of Earth, Environmental, and Planetary Sciences, Providence, RI 02912, USA
| | - F Tosi
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - F Zambon
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - C A Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA
| | - C T Russell
- Earth Planetary and Space Sciences, University of California-Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
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Pizzarello S, Shock E. Carbonaceous Chondrite Meteorites: the Chronicle of a Potential Evolutionary Path between Stars and Life. ORIGINS LIFE EVOL B 2017; 47:249-260. [PMID: 28078499 DOI: 10.1007/s11084-016-9530-1] [Citation(s) in RCA: 20] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/31/2016] [Accepted: 11/01/2016] [Indexed: 10/20/2022]
Abstract
The biogenic elements, H, C, N, O, P and S, have a long cosmic history, whose evolution can still be observed in diverse locales of the known universe, from interstellar clouds of gas and dust, to pre-stellar cores, nebulas, protoplanetary discs, planets and planetesimals. The best analytical window into this cosmochemical evolution as it neared Earth has been provided so far by the small bodies of the Solar System, some of which were not significantly altered by the high gravitational pressures and temperatures that accompanied the formation of larger planets and may carry a pristine record of early nebular chemistry. Asteroids have delivered such records, as their fragments reach the Earth frequently and become available for laboratory analyses. The Carbonaceous Chondrite meteorites (CC) are a group of such fragments with the further distinction of containing abundant organic materials with structures as diverse as kerogen-like macromolecules and simpler compounds with identical counterparts in Earth's biosphere. All have revealed a lineage to cosmochemical synthetic regimes. Several CC show that asteroids underwent aqueous alteration of their minerals or rock metamorphism but may yet yield clues to the reactivity of organic compounds during parent-body processes, on asteroids as well as larger ocean worlds and planets. Whether the exogenous delivery by meteorites held an advantage in Earth's molecular evolution remains an open question as many others regarding the origins of life are. Nonetheless, the natural samples of meteorites allow exploring the physical and chemical processes that might have led to a selected chemical pool amenable to the onset of life. Graphical Abstract ᅟ.
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Affiliation(s)
- Sandra Pizzarello
- School of Molecular Sciences, Arizona State University, Tempe, AZ, 85287-1604, USA.
| | - Everett Shock
- School of Molecular Sciences, Arizona State University, Tempe, AZ, 85287-1604, USA
- School of Earth & Space Exploration, Arizona State University, Tempe, AZ, 85218, USA
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Alexander CMO. The origin of inner Solar System water. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2017; 375:20150384. [PMID: 28416723 PMCID: PMC5394251 DOI: 10.1098/rsta.2015.0384] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 09/05/2016] [Indexed: 05/23/2023]
Abstract
Of the potential volatile sources for the terrestrial planets, the CI and CM carbonaceous chondrites are closest to the planets' bulk H and N isotopic compositions. For the Earth, the addition of approximately 2-4 wt% of CI/CM material to a volatile-depleted proto-Earth can explain the abundances of many of the most volatile elements, although some solar-like material is also required. Two dynamical models of terrestrial planet formation predict that the carbonaceous chondrites formed either in the asteroid belt ('classical' model) or in the outer Solar System (5-15 AU in the Grand Tack model). To test these models, at present the H isotopes of water are the most promising indicators of formation location because they should have become increasingly D-rich with distance from the Sun. The estimated initial H isotopic compositions of water accreted by the CI, CM, CR and Tagish Lake carbonaceous chondrites were much more D-poor than measured outer Solar System objects. A similar pattern is seen for N isotopes. The D-poor compositions reflect incomplete re-equilibration with H2 in the inner Solar System, which is also consistent with the O isotopes of chondritic water. On balance, it seems that the carbonaceous chondrites and their water did not form very far out in the disc, almost certainly not beyond the orbit of Saturn when its moons formed (approx. 3-7 AU in the Grand Tack model) and possibly close to where they are found today.This article is part of the themed issue 'The origin, history and role of water in the evolution of the inner Solar System'.
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Affiliation(s)
- Conel M O'D Alexander
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road NW, Washington, DC 20015, USA
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20
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Abstract
The Dawn spacecraft finds evidence for organic material and water ice on Ceres
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Affiliation(s)
- Michael Küppers
- European Space Astronomy Center, European Space Agency, Camino bajo del Castillo S/N, Madrid, Spain
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21
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Capaccioni F, Coradini A, Filacchione G, Erard S, Arnold G, Drossart P, De Sanctis MC, Bockelee-Morvan D, Capria MT, Tosi F, Leyrat C, Schmitt B, Quirico E, Cerroni P, Mennella V, Raponi A, Ciarniello M, McCord T, Moroz L, Palomba E, Ammannito E, Barucci MA, Bellucci G, Benkhoff J, Bibring JP, Blanco A, Blecka M, Carlson R, Carsenty U, Colangeli L, Combes M, Combi M, Crovisier J, Encrenaz T, Federico C, Fink U, Fonti S, Ip WH, Irwin P, Jaumann R, Kuehrt E, Langevin Y, Magni G, Mottola S, Orofino V, Palumbo P, Piccioni G, Schade U, Taylor F, Tiphene D, Tozzi GP, Beck P, Biver N, Bonal L, Combe JP, Despan D, Flamini E, Fornasier S, Frigeri A, Grassi D, Gudipati M, Longobardo A, Markus K, Merlin F, Orosei R, Rinaldi G, Stephan K, Cartacci M, Cicchetti A, Giuppi S, Hello Y, Henry F, Jacquinod S, Noschese R, Peter G, Politi R, Reess JM, Semery A. Cometary science. The organic-rich surface of comet 67P/Churyumov-Gerasimenko as seen by VIRTIS/Rosetta. Science 2015; 347:aaa0628. [PMID: 25613895 DOI: 10.1126/science.aaa0628] [Citation(s) in RCA: 266] [Impact Index Per Article: 29.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The VIRTIS (Visible, Infrared and Thermal Imaging Spectrometer) instrument on board the Rosetta spacecraft has provided evidence of carbon-bearing compounds on the nucleus of the comet 67P/Churyumov-Gerasimenko. The very low reflectance of the nucleus (normal albedo of 0.060 ± 0.003 at 0.55 micrometers), the spectral slopes in visible and infrared ranges (5 to 25 and 1.5 to 5% kÅ(-1)), and the broad absorption feature in the 2.9-to-3.6-micrometer range present across the entire illuminated surface are compatible with opaque minerals associated with nonvolatile organic macromolecular materials: a complex mixture of various types of carbon-hydrogen and/or oxygen-hydrogen chemical groups, with little contribution of nitrogen-hydrogen groups. In active areas, the changes in spectral slope and absorption feature width may suggest small amounts of water-ice. However, no ice-rich patches are observed, indicating a generally dehydrated nature for the surface currently illuminated by the Sun.
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Affiliation(s)
- F Capaccioni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy.
| | - A Coradini
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - G Filacchione
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - S Erard
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - G Arnold
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - P Drossart
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - M C De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - D Bockelee-Morvan
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - M T Capria
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - F Tosi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - C Leyrat
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - B Schmitt
- Université Grenoble Alpes, CNRS, Institut de Planétologie et d'Astrophysique de Grenoble, Grenoble, France
| | - E Quirico
- Université Grenoble Alpes, CNRS, Institut de Planétologie et d'Astrophysique de Grenoble, Grenoble, France
| | - P Cerroni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - V Mennella
- Osservatorio di Capodimonte, INAF, Napoli, Italy
| | - A Raponi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - M Ciarniello
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - T McCord
- Bear Fight Institute, Winthrop, WA 98862, USA
| | - L Moroz
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - E Palomba
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - E Ammannito
- University of California, Los Angeles, Los Angeles, CA 90095, USA
| | - M A Barucci
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - G Bellucci
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - J Benkhoff
- European Space Agency (ESA), European Space Research and Technology Centre (ESTEC), Noordwijk, Netherlands
| | - J P Bibring
- Institut d'Astrophysique Spatial, CNRS, Orsay, France
| | - A Blanco
- Dipartimento di Matematica e Fisica "Ennio De Giorgi," Università del Salento, Italy
| | - M Blecka
- Space Research Centre, Polish Academy of Sciences, Warsaw, Poland
| | - R Carlson
- NASA Jet Propulsion Laboratory, Pasadena, CA 91109, USA
| | - U Carsenty
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - L Colangeli
- European Space Agency (ESA), European Space Research and Technology Centre (ESTEC), Noordwijk, Netherlands
| | - M Combes
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - M Combi
- Space Physics Research Laboratory, The University of Michigan, Ann Arbor, MI 48109, USA
| | - J Crovisier
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - T Encrenaz
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | | | - U Fink
- Lunar Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - S Fonti
- Dipartimento di Matematica e Fisica "Ennio De Giorgi," Università del Salento, Italy
| | - W H Ip
- National Central University, Taipei, Taiwan
| | - P Irwin
- Departement of Physics, Oxford University, Oxford, UK
| | - R Jaumann
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany. Free University of Berlin, Institute of Geosciences, Malteserstraße 74-100, Building Haus A, 12249 Berlin, Germany
| | - E Kuehrt
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - Y Langevin
- Institut d'Astrophysique Spatial, CNRS, Orsay, France
| | - G Magni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - S Mottola
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - V Orofino
- Dipartimento di Matematica e Fisica "Ennio De Giorgi," Università del Salento, Italy
| | - P Palumbo
- Università "Parthenope," Napoli, Italy
| | - G Piccioni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - U Schade
- Helmholtz-Zentrum Berlin für Materialien und Energie, Berlin, Germany
| | - F Taylor
- Departement of Physics, Oxford University, Oxford, UK
| | - D Tiphene
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - G P Tozzi
- Osservatorio Astrofisico di Arcetri, INAF, Firenze, Italy
| | - P Beck
- Université Grenoble Alpes, CNRS, Institut de Planétologie et d'Astrophysique de Grenoble, Grenoble, France
| | - N Biver
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - L Bonal
- Université Grenoble Alpes, CNRS, Institut de Planétologie et d'Astrophysique de Grenoble, Grenoble, France
| | - J-Ph Combe
- Bear Fight Institute, Winthrop, WA 98862, USA
| | - D Despan
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - E Flamini
- Agenzia Spaziale Italiana, Rome, Italy
| | - S Fornasier
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - A Frigeri
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - D Grassi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - M Gudipati
- NASA Jet Propulsion Laboratory, Pasadena, CA 91109, USA. Institute for Physical Science and Technology, University of Maryland, College Park, MD 20742, USA
| | - A Longobardo
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - K Markus
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - F Merlin
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - R Orosei
- Istituto di Radioastronomia, INAF, Bologna, Italy
| | - G Rinaldi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - K Stephan
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - M Cartacci
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - A Cicchetti
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - S Giuppi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - Y Hello
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - F Henry
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - S Jacquinod
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - R Noschese
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - G Peter
- Institut für Optische Sensorsysteme, DLR, Berlin, Germany
| | - R Politi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - J M Reess
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - A Semery
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
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22
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Solar System evolution from compositional mapping of the asteroid belt. Nature 2014; 505:629-34. [PMID: 24476886 DOI: 10.1038/nature12908] [Citation(s) in RCA: 33] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/10/2013] [Accepted: 11/22/2013] [Indexed: 11/09/2022]
Abstract
Advances in the discovery and characterization of asteroids over the past decade have revealed an unanticipated underlying structure that points to a dramatic early history of the inner Solar System. The asteroids in the main asteroid belt have been discovered to be more compositionally diverse with size and distance from the Sun than had previously been known. This implies substantial mixing through processes such as planetary migration and the subsequent dynamical processes.
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23
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Localized sources of water vapour on the dwarf planet (1) Ceres. Nature 2014; 505:525-7. [PMID: 24451541 DOI: 10.1038/nature12918] [Citation(s) in RCA: 229] [Impact Index Per Article: 22.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/23/2013] [Accepted: 11/26/2013] [Indexed: 11/08/2022]
Abstract
The 'snowline' conventionally divides Solar System objects into dry bodies, ranging out to the main asteroid belt, and icy bodies beyond the belt. Models suggest that some of the icy bodies may have migrated into the asteroid belt. Recent observations indicate the presence of water ice on the surface of some asteroids, with sublimation a potential reason for the dust activity observed on others. Hydrated minerals have been found on the surface of the largest object in the asteroid belt, the dwarf planet (1) Ceres, which is thought to be differentiated into a silicate core with an icy mantle. The presence of water vapour around Ceres was suggested by a marginal detection of the photodissociation product of water, hydroxyl (ref. 12), but could not be confirmed by later, more sensitive observations. Here we report the detection of water vapour around Ceres, with at least 10(26) molecules being produced per second, originating from localized sources that seem to be linked to mid-latitude regions on the surface. The water evaporation could be due to comet-like sublimation or to cryo-volcanism, in which volcanoes erupt volatiles such as water instead of molten rocks.
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24
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Evaporating asteroid. Nature 2014; 505:487-8. [DOI: 10.1038/505487a] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
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Bennett CJ, Pirim C, Orlando TM. Space-Weathering of Solar System Bodies: A Laboratory Perspective. Chem Rev 2013; 113:9086-150. [DOI: 10.1021/cr400153k] [Citation(s) in RCA: 107] [Impact Index Per Article: 9.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
Affiliation(s)
- Chris J. Bennett
- Department of Chemistry & Biochemistry, Georgia Institute of Technology, 901 Atlantic Drive, Atlanta, Georgia 30332, United States
| | - Claire Pirim
- Department of Chemistry & Biochemistry, Georgia Institute of Technology, 901 Atlantic Drive, Atlanta, Georgia 30332, United States
| | - Thomas M. Orlando
- Department of Chemistry & Biochemistry, Georgia Institute of Technology, 901 Atlantic Drive, Atlanta, Georgia 30332, United States
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Muñoz Caro GM, Dartois E. Prebiotic chemistry in icy grain mantles in space. An experimental and observational approach. Chem Soc Rev 2013; 42:2173-85. [PMID: 23340705 DOI: 10.1039/c2cs35425j] [Citation(s) in RCA: 15] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
A compendium of different solid carbonaceous materials detected in space is presented, focussing on the search for organic matter of prebiotic interest. This journey takes us from the carbon grains likely formed in the atmospheres of evolved stars to organic grain mantles made from ice processing thought to be present in dense interstellar clouds and circumstellar regions, making a stop in solar system objects that could have delivered organic species to the early Earth. The most abundant carbon materials detected to date in space appear to be of little biological relevance. On the other hand, organic refractory residues, made in the laboratory from UV-photoprocessing followed by warm-up of interstellar ice analogs, are a hydrocarbon material rich in O and N containing chemical compounds that could act as initiators of prebiotic chemistry. A similar material might be present in dust grains inside dense clouds or circumstellar regions, some comets, and as a minor component in carbonaceous chondrites. We use infrared spectroscopy as a tool to spot organic refractory matter in various space environments. The delivery of organic materials via comets, (micro-) meteorites, and interplanetary dust particles to the primitive Earth might have contributed as a starting material for prebiotic chemistry. To test this hypothesis, it is first essential to characterize the composition of exogenous organic matter.
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Affiliation(s)
- Guillermo M Muñoz Caro
- Centro de Astrobiología, INTA-CSIC, Ctra. de Ajalvir, km 4, Torrejón de Ardoz, 28850 Madrid, Spain.
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27
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Role of proton ordering in adsorption preference of polar molecule on ice surface. Proc Natl Acad Sci U S A 2012; 109:13177-81. [PMID: 22837403 DOI: 10.1073/pnas.1206879109] [Citation(s) in RCA: 29] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Adsorption of polar monomers on ice surface, relevant to the physical/chemical reaction in ice clouds as well as growth of ice, remains an open issue partially due to the unusual surface characteristics with protons at the top layer of ice. Using first-principle calculations, we explore the adsorption properties of ice surface in terms of a surface proton order parameter, which characterizes the inhomogeneity of the dangling atoms on ice surface. We show that, due to an effective electric field created by dangling OH bonds and lone pairs of water molecules not only directly neighboring but also further away from the adsorbed polar molecule on the ice surface, the adsorption energy of polar monomer on ice surface exhibits large variance and a strong correlation with the proton order parameter of ice surface. Our results about the positive correlation between the inhomogeneity of ice surface and adsorption energies suggest that the physical/chemical reactions as well as the growth of ice may prefer to occur firstly on surfaces with larger proton order parameter.
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Castro-Chavez F. Most Used Codons per Amino Acid and per Genome in the Code of Man Compared to Other Organisms According to the Rotating Circular Genetic Code. ACTA ACUST UNITED AC 2011; 9. [PMID: 22997484 DOI: 10.14704/nq.2011.9.4.500] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 12/31/2022]
Abstract
My previous theoretical research shows that the rotating circular genetic code is a viable tool to make easier to distinguish the rules of variation applied to the amino acid exchange; it presents a precise and positional bio-mathematical balance of codons, according to the amino acids they codify. Here, I demonstrate that when using the conventional or classic circular genetic code, a clearer pattern for the human codon usage per amino acid and per genome emerges. The most used human codons per amino acid were the ones ending with the three hydrogen bond nucleotides: C for 12 amino acids and G for the remaining 8, plus one codon for arginine ending in A that was used approximately with the same frequency than the one ending in G for this same amino acid (plus *). The most used codons in man fall almost all the time at the rightmost position, clockwise, ending either in C or in G within the circular genetic code. The human codon usage per genome is compared to other organisms such as fruit flies (Drosophila melanogaster), squid (Loligo pealei), and many others. The biosemiotic codon usage of each genomic population or 'Theme' is equated to a 'molecular language'. The C/U choice or difference, and the G/A difference in the third nucleotide of the most used codons per amino acid are illustrated by comparing the most used codons per genome in humans and squids. The human distribution in the third position of most used codons is a 12-8-2, C-G-A, nucleotide ending signature, while the squid distribution in the third position of most used codons was an odd, or uneven, distribution in the third position of its most used codons: 13-6-3, U-A-G, as its nucleotide ending signature. These findings may help to design computational tools to compare human genomes, to determine the exchangeability between compatible codons and amino acids, and for the early detection of incompatible changes leading to hereditary diseases.
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Abundant ammonia in primitive asteroids and the case for a possible exobiology. Proc Natl Acad Sci U S A 2011; 108:4303-6. [PMID: 21368183 DOI: 10.1073/pnas.1014961108] [Citation(s) in RCA: 70] [Impact Index Per Article: 5.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Carbonaceous chondrites are asteroidal meteorites that contain abundant organic materials. Given that meteorites and comets have reached the Earth since it formed, it has been proposed that the exogenous influx from these bodies provided the organic inventories necessary for the emergence of life. The carbonaceous meteorites of the Renazzo-type family (CR) have recently revealed a composition that is particularly enriched in small soluble organic molecules, such as the amino acids glycine and alanine, which could support this possibility. We have now analyzed the insoluble and the largest organic component of the CR2 Grave Nunataks (GRA) 95229 meteorite and found it to be of more primitive composition than in other meteorites and to release abundant free ammonia upon hydrothermal treatment. The findings appear to trace CR2 meteorites' origin to cosmochemical regimes where ammonia was pervasive, and we speculate that their delivery to the early Earth could have fostered prebiotic molecular evolution.
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Yang B, Jewitt D. IDENTIFICATION OF MAGNETITE IN B-TYPE ASTEROIDS. THE ASTRONOMICAL JOURNAL 2010; 140:692-698. [DOI: 10.1088/0004-6256/140/3/692] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 09/01/2023]
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Water ice and organics on the surface of the asteroid 24 Themis. Nature 2010; 464:1320-1. [PMID: 20428164 DOI: 10.1038/nature09029] [Citation(s) in RCA: 274] [Impact Index Per Article: 19.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/21/2009] [Accepted: 02/24/2010] [Indexed: 11/09/2022]
Abstract
It has been suggested that Earth's current supply of water was delivered by asteroids, some time after the collision that produced the Moon (which would have vaporized any of the pre-existing water). So far, no measurements of water ice on asteroids have been made, but its presence has been inferred from the comet-like activity of several small asteroids, including two members of the Themis dynamical family. Here we report infrared spectra of the asteroid 24 Themis which show that ice and organic compounds are not only present on its surface but also prevalent. Infrared spectral differences between it and other asteroids make 24 Themis unique so far, and our identification of ice and organics agrees with independent results that rule out other compounds as possible sources of the observed spectral structure. The widespread presence of surface ice on 24 Themis is somewhat unexpected because of the relatively short lifetime of exposed ice at this distance ( approximately 3.2 au) from the Sun. Nevertheless, there are several plausible sources, such as a subsurface reservoir that brings water to the surface through 'impact gardening' and/or sublimation.
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Asteroid ice hints at rocky start to life on Earth. Nature 2010. [DOI: 10.1038/news.2010.207] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
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