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Towards In-Situ Geochemical Analysis of Planetary Rocks and Soils by Laser Ablation/Ionisation Time-of-Flight Mass Spectrometry. UNIVERSE 2022. [DOI: 10.3390/universe8080410] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
Spectroscopic instruments were a part of payloads on orbiter and lander missions and delivered vast data sets to explore minerals, elements and molecules on air-less rocky planets, asteroids and comets on global and local scales. To answer current space science questions, the chemical composition of planetary rocks and soils at grain scale is required, as well as measurements of element (isotope) concentrations down to the part per million or lower. Only mass spectrometric methods equipped with laser sampling ion sources can deliver the necessary information. Laser sampling techniques can reduce the dimensions of the investigated sample material down to micrometre scale, allowing for the composition analysis of grain-sized objects or thin mineral layers with sufficiently high spatial resolution, such that important geological processes can be recognised and studied as they progressed in time. We describe the performance characteristics, when applied to meteorite and geological samples, of a miniaturised laser ablation/ionisation mass spectrometer (named LMS) system that has been developed in our group. The main advantages of the LMS instrument over competing techniques are illustrated by examples of high spatial (lateral and vertical) resolution studies in different meteorites, terrestrial minerals and fossil-like structures in ancient rocks for most elements of geochemical interest. Top-level parameters, such as dimension, weight, and power consumption of a possible flight design of the LMS system are presented as well.
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Jenniskens P, Gabadirwe M, Yin QZ, Proyer A, Moses O, Kohout T, Franchi F, Gibson RL, Kowalski R, Christensen EJ, Gibbs AR, Heinze A, Denneau L, Farnocchia D, Chodas PW, Gray W, Micheli M, Moskovitz N, Onken CA, Wolf C, Devillepoix HAR, Ye Q, Robertson DK, Brown P, Lyytinen E, Moilanen J, Albers J, Cooper T, Assink J, Evers L, Lahtinen P, Seitshiro L, Laubenstein M, Wantlo N, Moleje P, Maritinkole J, Suhonen H, Zolensky ME, Ashwal L, Hiroi T, Sears DW, Sehlke A, Maturilli A, Sanborn ME, Huyskens MH, Dey S, Ziegler K, Busemann H, Riebe MEI, Meier MMM, Welten KC, Caffee MW, Zhou Q, Li QL, Li XH, Liu Y, Tang GQ, McLain HL, Dworkin JP, Glavin DP, Schmitt-Kopplin P, Sabbah H, Joblin C, Granvik M, Mosarwa B, Botepe K. The impact and recovery of asteroid 2018 LA. METEORITICS & PLANETARY SCIENCE 2021; 56:844-893. [PMID: 34295141 PMCID: PMC7611328 DOI: 10.1111/maps.13653] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/22/2021] [Accepted: 03/23/2021] [Indexed: 06/13/2023]
Abstract
The June 2, 2018, impact of asteroid 2018 LA over Botswana is only the second asteroid detected in space prior to impacting over land. Here, we report on the successful recovery of meteorites. Additional astrometric data refine the approach orbit and define the spin period and shape of the asteroid. Video observations of the fireball constrain the asteroid's position in its orbit and were used to triangulate the location of the fireball's main flare over the Central Kalahari Game Reserve. 23 meteorites were recovered. A consortium study of eight of these classifies Motopi Pan as a HED polymict breccia derived from howardite, cumulate and basaltic eucrite, and diogenite lithologies. Before impact, 2018 LA was a solid rock of ~156 cm diameter with high bulk density ~2.85 g/cm3, a relatively low albedo pv ~ 0.25, no significant opposition effect on the asteroid brightness, and an impact kinetic energy of ~0.2 kt. The orbit of 2018 LA is consistent with an origin at Vesta (or its Vestoids) and delivery into an Earth-impacting orbit via the v6 resonance. The impact that ejected 2018 LA in an orbit towards Earth occurred 22.8 ± 3.8 Ma ago. Zircons record a concordant U-Pb age of 4563 ± 11 Ma and a consistent 207Pb/206Pb age of 4563 ± 6 Ma. A much younger Pb-Pb phosphate resetting age of 4234 ± 41 Ma was found. From this impact chronology, we discuss what is the possible source crater of Motopi Pan and the age of Vesta's Veneneia impact basin.
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Affiliation(s)
- Peter Jenniskens
- SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA
- NASA Ames Research Center, Moffett Field, CA 94035, USA
| | - Mohutsiwa Gabadirwe
- Botswana Geoscience Institute, Plot 11566, Khama 1 Avenue, Private Bag 0014, Lobatse, Botswana
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California Davis, One Shields Avenue, CA 95616, USA
| | - Alexander Proyer
- Botswana International University of Science and Technology, Private Bag 16, Palapye, Botswana
| | - Oliver Moses
- University of Botswana, Okavango Research Institute, Private Bag 285, Maun, Botswana
| | - Tomas Kohout
- Department of Geosciences and Geography, University of Helsinki, P. O. Box 64, FI-00014 Helsinki, Finland
- Ursa Finnish Fireball Network, Kopernikuksentie 1, FI-00130 Helsinki, Finland
| | - Fulvio Franchi
- Botswana International University of Science and Technology, Private Bag 16, Palapye, Botswana
| | - Roger L. Gibson
- School of Geosciences, University of the Witwatersrand, P.O. WITS, Johannesburg 2050, South Africa
| | - Richard Kowalski
- Catalina Sky Survey, Lunar & Planetary Laboratory, The University of Arizona, 1629 E University Blvd., Tucson, AZ 85721, USA
| | - Eric J. Christensen
- Catalina Sky Survey, Lunar & Planetary Laboratory, The University of Arizona, 1629 E University Blvd., Tucson, AZ 85721, USA
| | - Alex R. Gibbs
- Catalina Sky Survey, Lunar & Planetary Laboratory, The University of Arizona, 1629 E University Blvd., Tucson, AZ 85721, USA
| | - Aren Heinze
- ATLAS, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822-1839, USA
| | - Larry Denneau
- ATLAS, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822-1839, USA
| | - Davide Farnocchia
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - Paul W. Chodas
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - William Gray
- Project Pluto, 168 Ridge Road, Bowdoinham, ME 04008, USA
| | - Marco Micheli
- ESA NEO Coordination Centre, Largo Galileo Galilei 1, I-00044, Frascati, Italy
| | - Nick Moskovitz
- Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff, AZ 86001, USA
| | - Christopher A. Onken
- Research School of Astronomy and Astrophysics, The Australian National University, Canberra ACT 2611, Australia
| | - Christian Wolf
- Research School of Astronomy and Astrophysics, The Australian National University, Canberra ACT 2611, Australia
| | | | - Quanzhi Ye
- Department of Astronomy, University of Maryland, College Park, MD 20742, USA
- Division of Physics, Mathematics and Astronomy, Caltech, Pasadena, CA 91125, USA
| | - Darrel K. Robertson
- NASA Ames Research Center, Asteroid Threat Assessment Project, Mail Stop 239-1, Moffett Field, CA 94035, USA
| | - Peter Brown
- Centre for Planetary Science and Exploration, Western University, London, Ontario, N6A 5B7, Canada
| | - Esko Lyytinen
- Ursa Finnish Fireball Network, Kopernikuksentie 1, FI-00130 Helsinki, Finland
| | - Jarmo Moilanen
- Ursa Finnish Fireball Network, Kopernikuksentie 1, FI-00130 Helsinki, Finland
| | - Jim Albers
- SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA
| | - Tim Cooper
- Astronomical Society of Southern Africa, Suite 617, Private Bag X043, Benoni 1500, South Africa
| | - Jelle Assink
- Royal Dutch Meteorological Institute, R&D Seismology and Acoustics, P. O. Box 201, NL-3730 AE De Bilt, The Netherlands
| | - Läslo Evers
- Royal Dutch Meteorological Institute, R&D Seismology and Acoustics, P. O. Box 201, NL-3730 AE De Bilt, The Netherlands
- Delft University of Technology, Department of Geoscience and Engineering, P. O. Box 5048, NL-2600 GA Delft, the Netherlands
| | - Panu Lahtinen
- Ursa Finnish Fireball Network, Kopernikuksentie 1, FI-00130 Helsinki, Finland
| | - Lesedi Seitshiro
- Botswana International University of Science and Technology, Private Bag 16, Palapye, Botswana
| | - Matthias Laubenstein
- Gran Sasso National Laboratory, National Institute for Nuclear Physics, Via G. Acitelli 22, I-67100 Assergi, Italy
| | - Nggie Wantlo
- Botswana Geoscience Institute, Plot 11566, Khama 1 Avenue, Private Bag 0014, Lobatse, Botswana
| | - Phemo Moleje
- Botswana Geoscience Institute, Plot 11566, Khama 1 Avenue, Private Bag 0014, Lobatse, Botswana
| | - Joseph Maritinkole
- Botswana Geoscience Institute, Plot 11566, Khama 1 Avenue, Private Bag 0014, Lobatse, Botswana
| | - Heikki Suhonen
- University of Helsinki, Department of Physics, P. O. Box 64, FI-00014 Helsinki, Finland
| | | | - Lewis Ashwal
- School of Geosciences, University of the Witwatersrand, P.O. WITS, Johannesburg 2050, South Africa
| | - Takahiro Hiroi
- Brown University, Reflectance Experiment Laboratory, Department of Earth, Environmental and Planetary Science, Providence, RI 02912, USA
| | - Derek W. Sears
- NASA Ames Research Center / Bay Area Environmental Research Institute, Mail Stop 245-3, Moffett Field, CA 94035, USA
| | - Alexander Sehlke
- NASA Ames Research Center / Bay Area Environmental Research Institute, Mail Stop 245-3, Moffett Field, CA 94035, USA
| | - Alessandro Maturilli
- Institute for Planetary Research, German Aerospace Center DLR, Rutherfordstrasse 2, D-12489 Berlin-Adlershof, Germany
| | - Matthew E. Sanborn
- Department of Earth and Planetary Sciences, University of California Davis, One Shields Avenue, CA 95616, USA
| | - Magdalena H. Huyskens
- Department of Earth and Planetary Sciences, University of California Davis, One Shields Avenue, CA 95616, USA
| | - Supratim Dey
- Department of Earth and Planetary Sciences, University of California Davis, One Shields Avenue, CA 95616, USA
| | - Karen Ziegler
- University of New Mexico, Institute of Meteoritics, 221 Yale Blvd NE, 331 Northrop Hall, Albuquerque, NM 87131, USA
| | - Henner Busemann
- Institute of Geochemistry and Petrology, ETH Zürich, Clausiusstrasse 25, CH-8092 Zürich, Switzerland
| | - My E. I. Riebe
- Institute of Geochemistry and Petrology, ETH Zürich, Clausiusstrasse 25, CH-8092 Zürich, Switzerland
| | - Matthias M. M. Meier
- Naturmuseum St. Gallen, Rorschacher Strasse 263, CH-9016 St. Gallen, Switzerland
| | - Kees C. Welten
- University of California Berkeley, Space Science Laboratory, Berkeley, CA 94720, USA
| | - Marc W. Caffee
- Purdue University, Dept. Physics and Astronomy, 525 Northwestern Avenue, West Lafayette, IN 47907, USA
| | - Qin Zhou
- National Astronomical Observatories, Beijing, Chinese Academy of Sciences, Beijing 100012, China
| | - Qiu-Li Li
- National Astronomical Observatories, Beijing, Chinese Academy of Sciences, Beijing 100012, China
| | - Xian-Hua Li
- State Key Laboratory of Lithospheric Evolution, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, China
| | - Yu Liu
- State Key Laboratory of Lithospheric Evolution, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, China
| | - Guo-Qiang Tang
- State Key Laboratory of Lithospheric Evolution, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, China
| | - Hannah L. McLain
- Catholic University of America, Department of Chemistry, 620 Michigan Ave, N.E., Washington, DC 20064, USA
- NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, MD 20771, USA
| | - Jason P. Dworkin
- NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, MD 20771, USA
| | - Daniel P. Glavin
- NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, MD 20771, USA
| | - Philippe Schmitt-Kopplin
- Helmholtz Zentrum München, Research Unit Analytical BioGeoChemistry, Ingolstädter Landstr. 1, D-85764 Neuherberg, Germany
- Technische Universität München, Analytical Food Chemistry, D-85354 Freising-Weihenstephan, Germany
| | - Hassan Sabbah
- IRAP, Université de Toulouse, CNRS, CNES, Université de Toulouse (UPS), F-31028 Toulouse Cedex 4, France
| | | | - Mikael Granvik
- University of Helsinki, Department of Physics, P. O. Box 64, FI-00014 Helsinki, Finland
- Asteroid Engineering Laboratory, Onboard Space Systems, Lulea University of Technology, Box 848, S-981 28 Kiruna, Sweden
| | - Babutsi Mosarwa
- Botswana National Museum, 161 Queens Rd., Gaborone, Botswana
| | - Koketso Botepe
- Botswana Geoscience Institute, Plot 11566, Khama 1 Avenue, Private Bag 0014, Lobatse, Botswana
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Burbine TH, Greenwood RC. Exploring the Bimodal Solar System via Sample Return from the Main Asteroid Belt: The Case for Revisiting Ceres. SPACE SCIENCE REVIEWS 2020; 216:59. [PMID: 32624627 PMCID: PMC7319314 DOI: 10.1007/s11214-020-00671-0] [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: 07/24/2019] [Accepted: 04/07/2020] [Indexed: 06/11/2023]
Abstract
Sample return from a main-belt asteroid has not yet been attempted, but appears technologically feasible. While the cost implications are significant, the scientific case for such a mission appears overwhelming. As suggested by the "Grand Tack" model, the structure of the main belt was likely forged during the earliest stages of Solar System evolution in response to migration of the giant planets. Returning samples from the main belt has the potential to test such planet migration models and the related geochemical and isotopic concept of a bimodal Solar System. Isotopic studies demonstrate distinct compositional differences between samples believed to be derived from the outer Solar System (CC or carbonaceous chondrite group) and those that are thought to be derived from the inner Solar System (NC or non-carbonaceous group). These two groups are separated on relevant isotopic variation diagrams by a clear compositional gap. The interface between these two regions appears to be broadly coincident with the present location of the asteroid belt, which contains material derived from both groups. The Hayabusa mission to near-Earth asteroid (NEA) (25143) Itokawa has shown what can be learned from a sample-return mission to an asteroid, even with a very small amount of sample. One scenario for main-belt sample return involves a spacecraft launching a projectile that strikes an object and flying through the debris cloud, which would potentially allow multiple bodies to be sampled if a number of projectiles are used on different asteroids. Another scenario is the more traditional method of landing on an asteroid to obtain the sample. A significant range of main-belt asteroids are available as targets for a sample-return mission and such a mission would represent a first step in mineralogically and isotopically mapping the asteroid belt. We argue that a sample-return mission to the asteroid belt does not necessarily have to return material from both the NC and CC groups to viably test the bimodal Solar System paradigm, as material from the NC group is already abundantly available for study. Instead, there is overwhelming evidence that we have a very incomplete suite of CC-related samples. Based on our analysis, we advocate a dedicated sample-return mission to the dwarf planet (1) Ceres as the best means of further exploring inherent Solar System variation. Ceres is an ice-rich world that may be a displaced trans-Neptunian object. We almost certainly do not have any meteorites that closely resemble material that would be brought back from Ceres. The rich heritage of data acquired by the Dawn mission makes a sample-return mission from Ceres logistically feasible at a realistic cost. No other potential main-belt target is capable of providing as much insight into the early Solar System as Ceres. Such a mission should be given the highest priority by the international scientific community.
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Affiliation(s)
- Thomas H. Burbine
- Department of Astronomy, Mount Holyoke College, South Hadley, MA 01075 USA
| | - Richard C. Greenwood
- Planetary and Space Sciences, School of Physical Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA UK
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Zhang AC, Kawasaki N, Bao H, Liu J, Qin L, Kuroda M, Gao JF, Chen LH, He Y, Sakamoto N, Yurimoto H. Evidence of metasomatism in the interior of Vesta. Nat Commun 2020; 11:1289. [PMID: 32157094 PMCID: PMC7064581 DOI: 10.1038/s41467-020-15049-7] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/05/2018] [Accepted: 02/10/2020] [Indexed: 11/09/2022] Open
Abstract
Diogenites are a group of meteorites that are derived from the interior of the largest protoplanet Vesta. They provide a unique opportunity to understanding together the internal structure and dynamic evolution of this protoplanet. Northwest Africa (NWA) 8321 was suggested to be an unbrecciated noritic diogenite meteorite, which is confirmed by our oxygen and chromium isotopic data. Here, we find that olivine in this sample has been partly replaced by orthopyroxene, troilite, and minor metal. The replacement texture of olivine is unambiguous evidence of sulfur-involved metasomatism in the interior of Vesta. The presence of such replacement texture suggests that in NWA 8321, the olivine should be of xenolith origin while the noritic diogenite was derived from partial melting of pre-existing rocks and had crystallized in the interior of Vesta. The post-Rheasilvia craters in the north-polar region on Vesta could be the potential source for NWA 8321.
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Affiliation(s)
- Ai-Cheng Zhang
- State Key Laboratory for Mineral Deposits Research and School of Earth Sciences and Engineering, Nanjing University, Nanjing, 210023, China.
- CAS Center for Excellence in Comparative Planetology, Hefei, China.
| | - Noriyuki Kawasaki
- Department of Natural History Sciences, Hokkaido University, Sapporo, 060-0810, Japan
| | - Huiming Bao
- Department of Geology & Geophysics, Louisiana State University, Baton Rouge, LA, 70803, USA
- International Center for Isotope Effects Research, Nanjing University, Nanjing, 210023, China
- School of Earth Sciences and Engineering, Nanjing University, Nanjing, 210023, China
| | - Jia Liu
- CAS Center for Excellence in Comparative Planetology, Hefei, China
- CAS Key Laboratory of Crust-Mantle Materials and Environment, University of Science and Technology of China, Hefei, 230026, China
| | - Liping Qin
- CAS Center for Excellence in Comparative Planetology, Hefei, China
- CAS Key Laboratory of Crust-Mantle Materials and Environment, University of Science and Technology of China, Hefei, 230026, China
| | - Minami Kuroda
- Department of Natural History Sciences, Hokkaido University, Sapporo, 060-0810, Japan
| | - Jian-Feng Gao
- State Key Laboratory of Ore Deposit Geochemistry, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang, 550081, China
| | - Li-Hui Chen
- State Key Laboratory for Mineral Deposits Research and School of Earth Sciences and Engineering, Nanjing University, Nanjing, 210023, China
- CAS Center for Excellence in Comparative Planetology, Hefei, China
| | - Ye He
- State Key Laboratory for Mineral Deposits Research and School of Earth Sciences and Engineering, Nanjing University, Nanjing, 210023, China
| | - Naoya Sakamoto
- Isotope Imaging Laboratory, Creative Research Institution, Hokkaido University, Sapporo, 001-0021, Japan
| | - Hisayoshi Yurimoto
- Department of Natural History Sciences, Hokkaido University, Sapporo, 060-0810, Japan
- Isotope Imaging Laboratory, Creative Research Institution, Hokkaido University, Sapporo, 001-0021, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Kanagawa, 252-5210, Japan
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The Effect of Jupiter's Formation on the Distribution of Refractory Elements and Inclusions in Meteorites. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4365/aad95f] [Citation(s) in RCA: 115] [Impact Index Per Article: 19.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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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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Herd CDK, Moser DE, Tait K, Darling JR, Shaulis BJ, McCoy TJ. Crystallization of Baddeleyite in Basaltic Rocks from Mars, and Comparisons with the Earth, Moon, and Vesta. MICROSTRUCTURAL GEOCHRONOLOGY 2017. [DOI: 10.1002/9781119227250.ch6] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/12/2022]
Affiliation(s)
- Christopher D. K. Herd
- Department of Earth and Atmospheric Sciences; University of Alberta; Edmonton Alberta Canada
| | - Desmond E. Moser
- Department of Earth Sciences; University of Western Ontario; London Ontario Canada
| | - Kimberly Tait
- Department of Natural History; Royal Ontario Museum; Toronto Ontario Canada
| | - James R. Darling
- School of Earth and Environmental Sciences; University of Portsmouth; Portsmouth UK
| | - Barry J. Shaulis
- Department of Geosciences; University of Arkansas; Fayetteville Arkansas USA
| | - Timothy J. McCoy
- Department of Mineral Sciences; National Museum of Natural History, Smithsonian Institution; Washington District of Columbia USA
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Hallis LJ. D/H ratios of the inner Solar System. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2017; 375:rsta.2015.0390. [PMID: 28416726 PMCID: PMC5394254 DOI: 10.1098/rsta.2015.0390] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 10/12/2016] [Indexed: 05/23/2023]
Abstract
The original hydrogen isotope (D/H) ratios of different planetary bodies may indicate where each body formed in the Solar System. However, geological and atmospheric processes can alter these ratios through time. Over the past few decades, D/H ratios in meteorites from Vesta and Mars, as well as from S- and C-type asteroids, have been measured. The aim of this article is to bring together all previously published data from these bodies, as well as the Earth, in order to determine the original D/H ratio for each of these inner Solar System planetary bodies. Once all secondary processes have been stripped away, the inner Solar System appears to be relatively homogeneous in terms of water D/H, with the original water D/H ratios of Vesta, Mars, the Earth, and S- and C-type asteroids all falling between δD values of -100‰ and -590‰. This homogeneity is in accord with the 'Grand tack' model of Solar System formation, where giant planet migration causes the S- and C-type asteroids to be mixed within 1 AU to eventually form the terrestrial planets.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)
- L J Hallis
- School of Geographical and Earth Sciences, Gregory Building, University of Glasgow, Glasgow G12 8QQ, UK
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Sarafian AR, Hauri EH, McCubbin FM, Lapen TJ, Berger EL, Nielsen SG, Marschall HR, Gaetani GA, Righter K, Sarafian E. Early accretion of water and volatile elements to the inner Solar System: evidence from angrites. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2017; 375:20160209. [PMID: 28416730 PMCID: PMC5394258 DOI: 10.1098/rsta.2016.0209] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 01/19/2017] [Indexed: 05/23/2023]
Abstract
Inner Solar System bodies are depleted in volatile elements relative to chondrite meteorites, yet the source(s) and mechanism(s) of volatile-element depletion and/or enrichment are poorly constrained. The timing, mechanisms and quantities of volatile elements present in the early inner Solar System have vast implications for diverse processes, from planetary differentiation to the emergence of life. We report major, trace and volatile-element contents of a glass bead derived from the D'Orbigny angrite, the hydrogen isotopic composition of this glass bead and that of coexisting olivine and silicophosphates, and the 207Pb-206Pb age of the silicophosphates, 4568 ± 20 Ma. We use volatile saturation models to demonstrate that the angrite parent body must have been a major body in the early inner Solar System. We further show via mixing calculations that all inner Solar System bodies accreted volatile elements with carbonaceous chondrite H and N isotope signatures extremely early in Solar System history. Only a small portion (if any) of comets and gaseous nebular H species contributed to the volatile content of the inner Solar System bodies.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)
- Adam R Sarafian
- Massachusetts Institute of Technology - Woods Hole Oceanographic Institution Joint Program in Oceanography/Applied Ocean Science and Engineering, Cambridge, MA 02139, USA
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
- NIRVANA Laboratories, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
| | - Erik H Hauri
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA
| | | | - Thomas J Lapen
- Department of Earth and Atmospheric Sciences, University of Houston, Houston, TX 77204, USA
| | - Eve L Berger
- GeoControl Systems Inc., Jacobs JETS Contract, NASA JSC, Houston, TX, USA
| | - Sune G Nielsen
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
- NIRVANA Laboratories, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
| | - Horst R Marschall
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
- Goethe Universität Frankfurt, Institut für Geowissenschaften, Altenhöferallee 1, 60438 Frankfurt am Main, Germany
| | - Glenn A Gaetani
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
| | - Kevin Righter
- NASA JSC, Mailcode XI2, 2101 NASA Parkway, Houston, TX 77058, USA
| | - Emily Sarafian
- Massachusetts Institute of Technology - Woods Hole Oceanographic Institution Joint Program in Oceanography/Applied Ocean Science and Engineering, Cambridge, MA 02139, USA
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
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10
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Pieters CM, Noble SK. Space Weathering on Airless Bodies. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2016; 121:1865-1884. [PMID: 29862145 PMCID: PMC5975224 DOI: 10.1002/2016je005128] [Citation(s) in RCA: 26] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/26/2023]
Abstract
Space weathering refers to alteration that occurs in the space environment with time. Lunar samples, and to some extent meteorites, have provided a benchmark for understanding the processes and products of space weathering. Lunar soils are derived principally from local materials but have accumulated a range of optically active opaque particles (OAOpq) that include nanophase metallic iron on/in rims formed on individual grains (imparting a red slope to visible and near-infrared reflectance) and larger iron particles (which darken across all wavelengths) such as are often found within the interior of recycled grains. Space weathering of other anhydrous silicate bodies, such as Mercury and some asteroids, produce different forms and relative abundance of OAOpq particles depending on the particular environment. If the development of OAOpq particles is minimized (such as at Vesta), contamination by exogenic material and regolith mixing become the dominant space weathering processes. Volatile-rich bodies and those composed of abundant hydrous minerals (dwarf planet Ceres, many dark asteroids, outer solar system satellites) are affected by space weathering processes differently than the silicate bodies of the inner solar system. However, the space weathering products of these bodies are currently poorly understood and the physics and chemistry of space weathering processes in different environments are areas of active research.
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Affiliation(s)
- Carle M Pieters
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI 02912
| | - Sarah K Noble
- Planetary Science Division, NASA Headquarters, Washington DC, 20546, one: 202-358-2492
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Abstract
A sample of 359 minor planets with available colorimetric, spectropnotometric, thermal-radiometric, and/or polarimetrie data are classified into broadly defined compositional types C (carbonaceous), S (silicaceous), M (metal-rich), E (metal-free; enstatite?), O (ordinary-chondritic?), T (Trojan; unidentified composition), and U (unclassifiable; none of the above).The small asteroids in Mars- or earth-crossing orbits are almost invariably of type S or O. For the main belt between 2.2 and 3.5 AU., distributions of the various types over diameter and orbital parameters are derived with corrections for observational selection bias. For 560 main-belt asteroids with diameters >50 km, 76% are of type C, 16% of type S, 5% M, and 3% of other types. The S objects become progressively less common with distance. The shapes of the diammeter-frequency relations for primitive (C) and evolved (S + M) types are statistically indistinguishable, both showing a change of slope at 160-km diameter.While large asteroids avoid the Kirkwood gaps more strongly than small ones, we find no significant gap-related anomalies in the relative frequencies of compositional types. Thus most of the observational basis for models in which primitive and evolved asteroids respond differently to collisional evolution has been removed.
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12
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Abstract
Curves of polarization are available at present for asteroids Vesta, Ceres, Pallas, Iris, Flora, and Icarus. These curves are compared with those of the satellites of Jupiter and Mercury, the Moon, and Mars. Laboratory simulations had already proved that the Moon's surface behaves like a powder of pulverized basalts; the recent confirmation by direct exploration is proving the significance of the method for remote determination of the surface properties of celestial bodies. The simulation of the Martian surface is found on small grained powders oxidized by ferreous limonite or goethite. New laboratory measurements were conducted to prepare the simulation of the asteroidal surfaces. Samples of the lunar surface returned to Earth provide impact-generated regolith and bare rocks superficially pitted and etched by impacts of the types suggested to be found on asteroidal surfaces; they were analyzed polarimetrically.Preliminary interpretations show that Vesta departs significantly from the other asteroids and cannot be covered by frost deposits or by aggregate cosmic dusts; a regolith-type surface generated by impacts or a coating of cohesive grains is indicated.Ceres, Pallas, and Iris are darker, and their polarizations do not suggest a pure regolithic surface, but cohesive grains or aggregates of dust are indicated.Icarus is 108 times smaller in mass; its polarization authorizes a fluffy, loosely aggregated dust deposit; however, a cometary model with stones embedded in ice is perhaps not ruled out on the basis of the present data.The way in which deep-space missions near the asteroidal belt can improve these results is discussed.
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13
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Abstract
Near infrared spectrophotometry has vastly increased our knowledge of the composition and structure of asteroids, satellites and planetary surfaces over the past ten years. In this article we will attempt to summarize the most recent comprehensive results. We will emphasize the interpretations and present only examples of the data.
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14
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Sarafian AR, Nielsen SG, Marschall HR, McCubbin FM, Monteleone BD. Early solar system. Early accretion of water in the inner solar system from a carbonaceous chondrite-like source. Science 2014; 346:623-6. [PMID: 25359971 DOI: 10.1126/science.1256717] [Citation(s) in RCA: 103] [Impact Index Per Article: 10.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Determining the origin of water and the timing of its accretion within the inner solar system is important for understanding the dynamics of planet formation. The timing of water accretion to the inner solar system also has implications for how and when life emerged on Earth. We report in situ measurements of the hydrogen isotopic composition of the mineral apatite in eucrite meteorites, whose parent body is the main-belt asteroid 4 Vesta. These measurements sample one of the oldest hydrogen reservoirs in the solar system and show that Vesta contains the same hydrogen isotopic composition as that of carbonaceous chondrites. Taking into account the old ages of eucrite meteorites and their similarity to Earth's isotopic ratios of hydrogen, carbon, and nitrogen, we demonstrate that these volatiles could have been added early to Earth, rather than gained during a late accretion event.
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Affiliation(s)
- Adam R Sarafian
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA.
| | - Sune G Nielsen
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
| | - Horst R Marschall
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA. Department of Earth and Planetary Sciences, American Museum of Natural History, New York, NY 10024, USA. School of Earth Sciences, University of Bristol, Bristol BS8 1RJ, UK
| | - Francis M McCubbin
- Institute of Meteoritics, University of New Mexico, Albuquerque, NM 87131, USA
| | - Brian D Monteleone
- Department of Geology and Geophysics, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
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15
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Clenet H, Jutzi M, Barrat JA, Asphaug EI, Benz W, Gillet P. A deep crust–mantle boundary in the asteroid 4 Vesta. Nature 2014; 511:303-6. [DOI: 10.1038/nature13499] [Citation(s) in RCA: 48] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/18/2014] [Accepted: 04/16/2014] [Indexed: 11/09/2022]
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16
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The formation of jupiter, the jovian early bombardment and the delivery of water to the asteroid belt: the case of (4) vesta. Life (Basel) 2014; 4:4-34. [PMID: 25370027 PMCID: PMC4187151 DOI: 10.3390/life4010004] [Citation(s) in RCA: 17] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/01/2013] [Revised: 12/26/2013] [Accepted: 01/16/2014] [Indexed: 11/17/2022] Open
Abstract
The asteroid (4) Vesta, parent body of the Howardite-Eucrite-Diogenite meteorites, is one of the first bodies that formed, mostly from volatile-depleted material, in the Solar System. The Dawn mission recently provided evidence that hydrated material was delivered to Vesta, possibly in a continuous way, over the last 4 Ga, while the study of the eucritic meteorites revealed a few samples that crystallized in presence of water and volatile elements. The formation of Jupiter and probably its migration occurred in the period when eucrites crystallized, and triggered a phase of bombardment that caused icy planetesimals to cross the asteroid belt. In this work, we study the flux of icy planetesimals on Vesta during the Jovian Early Bombardment and, using hydrodynamic simulations, the outcome of their collisions with the asteroid. We explore how the migration of the giant planet would affect the delivery of water and volatile materials to the asteroid and we discuss our results in the context of the geophysical and collisional evolution of Vesta. In particular, we argue that the observational data are best reproduced if the bulk of the impactors was represented by 1-2 km wide planetesimals and if Jupiter underwent a limited (a fraction of au) displacement.
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Jutzi M, Asphaug E, Gillet P, Barrat JA, Benz W. The structure of the asteroid 4 Vesta as revealed by models of planet-scale collisions. Nature 2013; 494:207-10. [PMID: 23407535 DOI: 10.1038/nature11892] [Citation(s) in RCA: 77] [Impact Index Per Article: 7.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/24/2012] [Accepted: 01/04/2013] [Indexed: 11/09/2022]
Abstract
Asteroid 4 Vesta seems to be a major intact protoplanet, with a surface composition similar to that of the HED (howardite-eucrite-diogenite) meteorites. The southern hemisphere is dominated by a giant impact scar, but previous impact models have failed to reproduce the observed topography. The recent discovery that Vesta's southern hemisphere is dominated by two overlapping basins provides an opportunity to model Vesta's topography more accurately. Here we report three-dimensional simulations of Vesta's global evolution under two overlapping planet-scale collisions. We closely reproduce its observed shape, and provide maps of impact excavation and ejecta deposition. Spiral patterns observed in the younger basin Rheasilvia, about one billion years old, are attributed to Coriolis forces during crater collapse. Surface materials exposed in the north come from a depth of about 20 kilometres, according to our models, whereas materials exposed inside the southern double-excavation come from depths of about 60-100 kilometres. If Vesta began as a layered, completely differentiated protoplanet, then our model predicts large areas of pure diogenites and olivine-rich rocks. These are not seen, possibly implying that the outer 100 kilometres or so of Vesta is composed mainly of a basaltic crust (eucrites) with ultramafic intrusions (diogenites).
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Affiliation(s)
- M Jutzi
- Physics Institute, Space Research and Planetary Sciences, Center for Space and Habitability, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland.
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18
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Pieters CM, Ammannito E, Blewett DT, Denevi BW, De Sanctis MC, Gaffey MJ, Le Corre L, Li JY, Marchi S, McCord TB, McFadden LA, Mittlefehldt DW, Nathues A, Palmer E, Reddy V, Raymond CA, Russell CT. Distinctive space weathering on Vesta from regolith mixing processes. Nature 2012; 491:79-82. [PMID: 23128227 DOI: 10.1038/nature11534] [Citation(s) in RCA: 105] [Impact Index Per Article: 8.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/17/2012] [Accepted: 08/20/2012] [Indexed: 11/09/2022]
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19
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Dark material on Vesta from the infall of carbonaceous volatile-rich material. Nature 2012; 491:83-6. [PMID: 23128228 DOI: 10.1038/nature11561] [Citation(s) in RCA: 139] [Impact Index Per Article: 11.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/16/2012] [Accepted: 08/29/2012] [Indexed: 11/09/2022]
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20
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Abstract
The progression from astronomical observation to geochemical analysis epitomizes advancements in planetary exploration.
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Affiliation(s)
- Richard P Binzel
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA.
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21
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Denevi BW, Blewett DT, Buczkowski DL, Capaccioni F, Capria MT, De Sanctis MC, Garry WB, Gaskell RW, Le Corre L, Li JY, Marchi S, McCoy TJ, Nathues A, O’Brien DP, Petro NE, Pieters CM, Preusker F, Raymond CA, Reddy V, Russell CT, Schenk P, Scully JEC, Sunshine JM, Tosi F, Williams DA, Wyrick D. Pitted Terrain on Vesta and Implications for the Presence of Volatiles. Science 2012; 338:246-9. [DOI: 10.1126/science.1225374] [Citation(s) in RCA: 86] [Impact Index Per Article: 7.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- B. W. Denevi
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - D. T. Blewett
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - D. L. Buczkowski
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - F. Capaccioni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy
| | - M. T. Capria
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy
| | - M. C. De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy
| | - W. B. Garry
- Planetary Science Institute, Tucson, AZ, USA
| | | | - L. Le Corre
- Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany
| | - J.-Y. Li
- Planetary Science Institute, Tucson, AZ, USA
- University of Maryland, College Park, MD, USA
| | - S. Marchi
- NASA Lunar Science Institute, Boulder, CO, USA
| | - T. J. McCoy
- National Museum of Natural History, Smithsonian Institution, Washington, DC, USA
| | - A. Nathues
- Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany
| | | | - N. E. Petro
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | | | - F. Preusker
- Deutsches Zentrum fur Luft- und Raumfahrt (DLR), Institute of Planetary Research, Berlin, Germany
| | - C. A. Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - V. Reddy
- Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany
- University of North Dakota, Grand Forks, ND, USA
| | | | - P. Schenk
- Lunar and Planetary Institute, Houston, TX, USA
| | | | | | - F. Tosi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy
| | | | - D. Wyrick
- Southwest Research Institute, San Antonio, TX, USA
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22
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Adams JB. Visible and near-infrared diffuse reflectance spectra of pyroxenes as applied to remote sensing of solid objects in the solar system. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb079i032p04829] [Citation(s) in RCA: 509] [Impact Index Per Article: 42.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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23
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24
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Prettyman TH, Mittlefehldt DW, Yamashita N, Lawrence DJ, Beck AW, Feldman WC, McCoy TJ, McSween HY, Toplis MJ, Titus TN, Tricarico P, Reedy RC, Hendricks JS, Forni O, Le Corre L, Li JY, Mizzon H, Reddy V, Raymond CA, Russell CT. Elemental mapping by Dawn reveals exogenic H in Vesta's regolith. Science 2012; 338:242-6. [PMID: 22997135 DOI: 10.1126/science.1225354] [Citation(s) in RCA: 186] [Impact Index Per Article: 15.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Using Dawn's Gamma Ray and Neutron Detector, we tested models of Vesta's evolution based on studies of howardite, eucrite, and diogenite (HED) meteorites. Global Fe/O and Fe/Si ratios are consistent with HED compositions. Neutron measurements confirm that a thick, diogenitic lower crust is exposed in the Rheasilvia basin, which is consistent with global magmatic differentiation. Vesta's regolith contains substantial amounts of hydrogen. The highest hydrogen concentrations coincide with older, low-albedo regions near the equator, where water ice is unstable. The young, Rheasilvia basin contains the lowest concentrations. These observations are consistent with gradual accumulation of hydrogen by infall of carbonaceous chondrites--observed as clasts in some howardites--and subsequent removal or burial of this material by large impacts.
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Affiliation(s)
- Thomas H Prettyman
- Planetary Science Institute, 1700 East Fort Lowell, Suite 106, Tucson, AZ 85719-2395, USA.
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25
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Johnson TV, Fanale FP. Optical properties of carbonaceous chondrites and their relationship to asteroids. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb078i035p08507] [Citation(s) in RCA: 218] [Impact Index Per Article: 18.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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26
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Walker D, Stolper EM, Hays JF. A numerical treatment of melt/solid segregation: Size of the eucrite parent body and stability of the terrestrial low-velocity zone. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb083ib12p06005] [Citation(s) in RCA: 72] [Impact Index Per Article: 6.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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27
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28
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Greenberger RN, Mustard JF, Kumar PS, Dyar MD, Breves EA, Sklute EC. Low temperature aqueous alteration of basalt: Mineral assemblages of Deccan basalts and implications for Mars. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2012je004127] [Citation(s) in RCA: 31] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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29
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Michel T, Eugster O. Primitive xenon in diogenites and plutonium-244-fission xenon ages of a diogenite, a howardite, and eucrites. ACTA ACUST UNITED AC 2012. [DOI: 10.1111/j.1945-5100.1994.tb00772.x] [Citation(s) in RCA: 27] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/30/2022]
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30
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31
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De Sanctis MC, Ammannito E, Capria MT, Tosi F, Capaccioni F, Zambon F, Carraro F, Fonte S, Frigeri A, Jaumann R, Magni G, Marchi S, McCord TB, McFadden LA, McSween HY, Mittlefehldt DW, Nathues A, Palomba E, Pieters CM, Raymond CA, Russell CT, Toplis MJ, Turrini D. Spectroscopic characterization of mineralogy and its diversity across Vesta. Science 2012; 336:697-700. [PMID: 22582257 DOI: 10.1126/science.1219270] [Citation(s) in RCA: 216] [Impact Index Per Article: 18.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The mineralogy of Vesta, based on data obtained by the Dawn spacecraft's visible and infrared spectrometer, is consistent with howardite-eucrite-diogenite meteorites. There are considerable regional and local variations across the asteroid: Spectrally distinct regions include the south-polar Rheasilvia basin, which displays a higher diogenitic component, and equatorial regions, which show a higher eucritic component. The lithologic distribution indicates a deeper diogenitic crust, exposed after excavation by the impact that formed Rheasilvia, and an upper eucritic crust. Evidence for mineralogical stratigraphic layering is observed on crater walls and in ejecta. This is broadly consistent with magma-ocean models, but spectral variability highlights local variations, which suggests that the crust can be a complex assemblage of eucritic basalts and pyroxene cumulates. Overall, Vesta mineralogy indicates a complex magmatic evolution that led to a differentiated crust and mantle.
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Affiliation(s)
- M C De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy.
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32
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Schenk P, O'Brien DP, Marchi S, Gaskell R, Preusker F, Roatsch T, Jaumann R, Buczkowski D, McCord T, McSween HY, Williams D, Yingst A, Raymond C, Russell C. The geologically recent giant impact basins at Vesta's south pole. Science 2012; 336:694-7. [PMID: 22582256 DOI: 10.1126/science.1223272] [Citation(s) in RCA: 173] [Impact Index Per Article: 14.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
Abstract
Dawn's global mapping of Vesta reveals that its observed south polar depression is composed of two overlapping giant impact features. These large basins provide exceptional windows into impact processes at planetary scales. The youngest, Rheasilvia, is 500 kilometers wide and 19 kilometers deep and finds its nearest morphologic analog among large basins on low-gravity icy satellites. Extensive ejecta deposits occur, but impact melt volume is low, exposing an unusual spiral fracture pattern that is likely related to faulting during uplift and convergence of the basin floor. Rheasilvia obliterated half of another 400-kilometer-wide impact basin, Veneneia. Both basins are unexpectedly young, roughly 1 to 2 billion years, and their formation substantially reset Vestan geology and excavated sufficient volumes of older compositionally heterogeneous crustal material to have created the Vestoids and howardite-eucrite-diogenite meteorites.
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Affiliation(s)
- Paul Schenk
- Lunar and Planetary Institute, Houston, TX 77058, USA.
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33
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Marchi S, McSween HY, O'Brien DP, Schenk P, De Sanctis MC, Gaskell R, Jaumann R, Mottola S, Preusker F, Raymond CA, Roatsch T, Russell CT. The violent collisional history of asteroid 4 Vesta. Science 2012; 336:690-4. [PMID: 22582255 DOI: 10.1126/science.1218757] [Citation(s) in RCA: 187] [Impact Index Per Article: 15.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Vesta is a large differentiated rocky body in the main asteroid belt that accreted within the first few million years after the formation of the earliest solar system solids. The Dawn spacecraft extensively imaged Vesta's surface, revealing a collision-dominated history. Results show that Vesta's cratering record has a strong north-south dichotomy. Vesta's northern heavily cratered terrains retain much of their earliest history. The southern hemisphere was reset, however, by two major collisions in more recent times. We estimate that the youngest of these impact structures, about 500 kilometers across, formed about 1 billion years ago, in agreement with estimates of Vesta asteroid family age based on dynamical and collisional constraints, supporting the notion that the Vesta asteroid family was formed during this event.
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Affiliation(s)
- S Marchi
- NASA Lunar Science Institute, Boulder, CO, USA.
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34
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Russell CT, Raymond CA, Coradini A, McSween HY, Zuber MT, Nathues A, De Sanctis MC, Jaumann R, Konopliv AS, Preusker F, Asmar SW, Park RS, Gaskell R, Keller HU, Mottola S, Roatsch T, Scully JEC, Smith DE, Tricarico P, Toplis MJ, Christensen UR, Feldman WC, Lawrence DJ, McCoy TJ, Prettyman TH, Reedy RC, Sykes ME, Titus TN. Dawn at Vesta: testing the protoplanetary paradigm. Science 2012; 336:684-6. [PMID: 22582253 DOI: 10.1126/science.1219381] [Citation(s) in RCA: 37] [Impact Index Per Article: 3.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Dawn spacecraft targeted 4 Vesta, believed to be a remnant intact protoplanet from the earliest epoch of solar system formation, based on analyses of howardite-eucrite-diogenite (HED) meteorites that indicate a differentiated parent body. Dawn observations reveal a giant basin at Vesta's south pole, whose excavation was sufficient to produce Vesta-family asteroids (Vestoids) and HED meteorites. The spatially resolved mineralogy of the surface reflects the composition of the HED meteorites, confirming the formation of Vesta's crust by melting of a chondritic parent body. Vesta's mass, volume, and gravitational field are consistent with a core having an average radius of 107 to 113 kilometers, indicating sufficient internal melting to segregate iron. Dawn's results confirm predictions that Vesta differentiated and support its identification as the parent body of the HEDs.
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Affiliation(s)
- C T Russell
- Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA 90095-1567, USA.
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35
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Jaumann R, Williams DA, Buczkowski DL, Yingst RA, Preusker F, Hiesinger H, Schmedemann N, Kneissl T, Vincent JB, Blewett DT, Buratti BJ, Carsenty U, Denevi BW, De Sanctis MC, Garry WB, Keller HU, Kersten E, Krohn K, Li JY, Marchi S, Matz KD, McCord TB, McSween HY, Mest SC, Mittlefehldt DW, Mottola S, Nathues A, Neukum G, O’Brien DP, Pieters CM, Prettyman TH, Raymond CA, Roatsch T, Russell CT, Schenk P, Schmidt BE, Scholten F, Stephan K, Sykes MV, Tricarico P, Wagner R, Zuber MT, Sierks H. Vesta’s Shape and Morphology. Science 2012; 336:687-90. [PMID: 22582254 DOI: 10.1126/science.1219122] [Citation(s) in RCA: 195] [Impact Index Per Article: 16.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- R. Jaumann
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
- Freie Universität Berlin, Planetary Sciences, Germany
| | | | - D. L. Buczkowski
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - R. A. Yingst
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - F. Preusker
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - H. Hiesinger
- Westfälische Wilhelms-Universität Münster, Germany
| | | | - T. Kneissl
- Freie Universität Berlin, Planetary Sciences, Germany
| | - J. B. Vincent
- Max Planck Institute for Solar System Research (MPS), Katlenburg-Lindau, Germany
| | - D. T. Blewett
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - B. J. Buratti
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - U. Carsenty
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - B. W. Denevi
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - M. C. De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Roma, Italy
| | - W. B. Garry
- Planetary Science Institute, Tucson, AZ 85719, USA
| | | | - E. Kersten
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - K. Krohn
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - J.-Y. Li
- University of Maryland, College Park, MD 20742, USA
| | - S. Marchi
- National Aeronautics and Space Administration (NASA) Lunar Science Institute, Boulder, CO 80309, USA
| | - K. D. Matz
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | | | - H. Y. McSween
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996, USA
| | - S. C. Mest
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - D. W. Mittlefehldt
- Astromaterials Research Office, NASA Johnson Space Center, Houston, TX 77058, USA
| | - S. Mottola
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - A. Nathues
- Max Planck Institute for Solar System Research (MPS), Katlenburg-Lindau, Germany
| | - G. Neukum
- Freie Universität Berlin, Planetary Sciences, Germany
| | | | - C. M. Pieters
- Brown University, Planetary Geosciences Department, Providence, RI 02912, USA
| | | | - C. A. Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - T. Roatsch
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - C. T. Russell
- Institute of Geophysics and Planetary Physics, University of California Los Angeles (UCLA), Los Angeles, CA 90095, USA
| | - P. Schenk
- Lunar and Planetary Institute, Houston, TX 77058, USA
| | - B. E. Schmidt
- Institute for Geophysics, University of Texas, Austin, TX 78712, USA
| | - F. Scholten
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - K. Stephan
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - M. V. Sykes
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - P. Tricarico
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - R. Wagner
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - M. T. Zuber
- Massachusetts Institute of Technology, Cambridge, MA 02139,USA
| | - H. Sierks
- Max Planck Institute for Solar System Research (MPS), Katlenburg-Lindau, Germany
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Reddy V, Nathues A, Le Corre L, Sierks H, Li JY, Gaskell R, McCoy T, Beck AW, Schröder SE, Pieters CM, Becker KJ, Buratti BJ, Denevi B, Blewett DT, Christensen U, Gaffey MJ, Gutierrez-Marques P, Hicks M, Keller HU, Maue T, Mottola S, McFadden LA, McSween HY, Mittlefehldt D, O’Brien DP, Raymond C, Russell C. Color and Albedo Heterogeneity of Vesta from Dawn. Science 2012; 336:700-4. [PMID: 22582258 DOI: 10.1126/science.1219088] [Citation(s) in RCA: 152] [Impact Index Per Article: 12.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Vishnu Reddy
- Max Planck Institute for Solar System Research, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
- Department of Space Studies, University of North Dakota, Grand Forks, ND 58202, USA
| | - Andreas Nathues
- Max Planck Institute for Solar System Research, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
| | - Lucille Le Corre
- Max Planck Institute for Solar System Research, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
| | - Holger Sierks
- Max Planck Institute for Solar System Research, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
| | - Jian-Yang Li
- Department of Astronomy, University of Maryland, College Park, MD 20742, USA
| | - Robert Gaskell
- Planetary Science Institute, 1700 East Fort Lowell, Suite 106, Tucson, AZ 85719, USA
| | - Timothy McCoy
- Department of Mineral Sciences, Smithsonian National Museum of Natural History, 10th and Constitution NW, Washington, DC 20560–0119, USA
| | - Andrew W. Beck
- Department of Mineral Sciences, Smithsonian National Museum of Natural History, 10th and Constitution NW, Washington, DC 20560–0119, USA
| | - Stefan E. Schröder
- Max Planck Institute for Solar System Research, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
| | - Carle M. Pieters
- Department of Geological Sciences, Brown University, Providence, RI 02912, USA
| | - Kris J. Becker
- Astrogeology Science Center, U.S. Geological Survey, Flagstaff, AZ 86001, USA
| | - Bonnie J. Buratti
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - Brett Denevi
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - David T. Blewett
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - Ulrich Christensen
- Max Planck Institute for Solar System Research, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
| | - Michael J. Gaffey
- Department of Space Studies, University of North Dakota, Grand Forks, ND 58202, USA
| | - Pablo Gutierrez-Marques
- Max Planck Institute for Solar System Research, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
| | - Michael Hicks
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - Horst Uwe Keller
- Institut für Geophysik und extraterrestrische Physik, TU Braunschweig Mendelssohnstrasse 3, DE 38106 Braunschweig, Germany
| | - Thorsten Maue
- Max Planck Institute for Solar System Research, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
| | - Stefano Mottola
- Deutsches Zentrum für Luft und Raumfahrt (DLR)–German Aerospace Center, Institute of Planetary Research, Rutherfordstrasse 2, D-12489 Berlin, Germany
| | - Lucy A. McFadden
- NASA/Goddard Space Flight Center, Mail Code 160, Greenbelt, MD 20771, USA
| | - Harry Y. McSween
- Department of Earth and Planetary Sciences, University of Tennessee, 1412 Circle Drive, Knoxville, TN 37996–1410, USA
| | - David Mittlefehldt
- Astromaterials Research Office, NASA Johnson Space Center, Mail Code KR, Houston, TX 77058, USA
| | - David P. O’Brien
- Planetary Science Institute, 1700 East Fort Lowell, Suite 106, Tucson, AZ 85719, USA
| | - Carol Raymond
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - Christopher Russell
- Institute of Geophysics and Planetary Physics, University of California Los Angeles, Los Angeles, CA 90024–1567, USA
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Binzel RP, Xu S. Chips off of Asteroid 4 Vesta: Evidence for the Parent Body of Basaltic Achondrite Meteorites. Science 2010; 260:186-91. [PMID: 17807177 DOI: 10.1126/science.260.5105.186] [Citation(s) in RCA: 543] [Impact Index Per Article: 38.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
For more than two decades, asteroid 4 Vesta has been debated as the source for the eucrite, diogenite, and howardite classes of basaltic achondrite meteorites. Its basaltic achondrite spectral properties are unlike those of other large main-belt asteroids. Telescopic measurements have revealed 20 small (diameters </= 10 kilometers) main-belt asteroids that have distinctive optical reflectance spectral features similar to those of Vesta and eucrite and diogenite meteorites. Twelve have orbits that are similar to Vesta's and were previously predicted to be dynamically associated with Vesta. Eight bridge the orbital space between Vesta and the 3:1 resonance, a proposed source region for meteorites. These asteroids are most probably multikilometer-sized fragments excavated from Vesta through one or more impacts. The sizes, ejection velocities of 500 meters per second, and proximity of these fragments to the 3:1 resonance establish Vesta as a dynamically viable source for eucrite, diogenite, and howardite meteorites.
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Abstract
Minerals partly composing the surfaces of 14 asteroids are determined by using asteroid reflectance spectra and optical properties of meteorites and other materials. Individual electronic absorption features are identified in the asteroids' spectra. The energies, relative strengths, and shapes of these features are interpreted by using laboratory and theoretical studies. Analysis of the initial 14 asteroid reflectance spectra indicates the presence of the following types of surface materials: six carbonaceous chondrite-like; two stony-iron-like (metal/silicate approximately 1); one iron meteorite-like; one basaltic achondrite-like; and four silicate-metal assemblages (metal/silicate approximately 0.25). These results support the conclusion that the asteroid belt is a source of at least some meteoritic material, and they show a relation between certain asteroids and certain classes of meteoritcs.
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McCord TB, McFadden LA, Russell CT, Sotin C, Thomas PC. Ceres, Vesta, and Pallas: Protoplanets, not asteroids. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006eo100002] [Citation(s) in RCA: 21] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Thomas PC, Parker JW, McFadden LA, Russell CT, Stern SA, Sykes MV, Young EF. Differentiation of the asteroid Ceres as revealed by its shape. Nature 2005; 437:224-6. [PMID: 16148926 DOI: 10.1038/nature03938] [Citation(s) in RCA: 239] [Impact Index Per Article: 12.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/22/2005] [Accepted: 06/10/2005] [Indexed: 11/08/2022]
Abstract
The accretion of bodies in the asteroid belt was halted nearly 4.6 billion years ago by the gravitational influence of the newly formed giant planet Jupiter. The asteroid belt therefore preserves a record of both this earliest epoch of Solar System formation and variation of conditions within the solar nebula. Spectral features in reflected sunlight indicate that some asteroids have experienced sufficient thermal evolution to differentiate into layered structures. The second most massive asteroid--4 Vesta--has differentiated to a crust, mantle and core. 1 Ceres, the largest and most massive asteroid, has in contrast been presumed to be homogeneous, in part because of its low density, low albedo and relatively featureless visible reflectance spectrum, similar to carbonaceous meteorites that have suffered minimal thermal processing. Here we show that Ceres has a shape and smoothness indicative of a gravitationally relaxed object. Its shape is significantly less flattened than that expected for a homogeneous object, but is consistent with a central mass concentration indicative of differentiation. Possible interior configurations include water-ice-rich mantles over a rocky core.
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Affiliation(s)
- P C Thomas
- Center for Radiophysics and Space Research, Cornell University, Ithaca, New York 14853, USA.
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Cloutis EA. Pyroxene reflectance spectra: Minor absorption bands and effects of elemental substitutions. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2001je001590] [Citation(s) in RCA: 52] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Hiroi T, Zolensky ME, Pieters CM. The Tagish Lake meteorite: a possible sample from a D-type asteroid. Science 2001; 293:2234-6. [PMID: 11520950 DOI: 10.1126/science.1063734] [Citation(s) in RCA: 177] [Impact Index Per Article: 7.7] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
Abstract
A new type of carbonaceous chondrite, the Tagish Lake meteorite, exhibits a reflectance spectrum similar to spectra observed from the D-type asteroids, which are relatively abundant in the outer solar system beyond the main asteroid belt and have been inferred to be more primitive than any known meteorite. Until the Tagish Lake fall, these asteroids had no analog in the meteorite collections. The Tagish Lake meteorite is a carbon-rich (4 to 5 weight %), aqueously altered carbonaceous chondrite and contains high concentrations of presolar grains and carbonate minerals, which is consistent with the expectation that the D-type asteroids were originally made of primitive materials and did not experience any extensive heating.
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Affiliation(s)
- T Hiroi
- Department of Geological Sciences, Brown University, Providence, RI 02912, USA.
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Lazzaro D, Michtchenko T, Carvano JM, Binzel RP, Bus SJ, Burbine TH, Mothe-Diniz T, Florczak M, Angeli CA, Harris AW. Discovery of a basaltic asteroid in the outer main belt. Science 2000; 288:2033-5. [PMID: 10856214 DOI: 10.1126/science.288.5473.2033] [Citation(s) in RCA: 97] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Visible and near-infrared spectroscopic observations of the asteroid 1459 Magnya indicate that it has a basaltic surface. Magnya is at 3. 15 astronomical units (AU) from the sun and has no known dynamical link to any family, to any nearby large asteroid, or to asteroid 4 Vesta at 2.36 AU, which is the only other known large basaltic asteroid. We show that the region of the belt around Magnya is densely filled by mean-motion resonances, generating slow orbital diffusion processes and providing a potential mechanism for removing other basaltic fragments that may have been created on the same parent body as Magnya. Magnya may represent a rare surviving fragment from a larger, differentiated planetesimal that was disrupted long ago.
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Affiliation(s)
- D Lazzaro
- Observatorio Nacional, Departamento de Astrofisica, Rua Gal. Jose Cristino 77, 20921-400 Rio de Janeiro, Brazil. Instituto Astronomico e Geofisico, Universidade de Sao Paulo, Av. Miguel Stefano 4200, 04301-904 Sao Paulo, Brazil. De
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Thomas PC, Binzel RP, Gaffey MJ, Storrs AD, Wells EN, Zellner BH. Impact Excavation on Asteroid 4 Vesta: Hubble Space Telescope Results. Science 1997. [DOI: 10.1126/science.277.5331.1492] [Citation(s) in RCA: 252] [Impact Index Per Article: 9.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Peter C. Thomas
- P. C. Thomas, Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA
- R. P. Binzel, Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
- M. J. Gaffey, Department of Earth and Environmental Sciences, Rensselaer Polytechnic Institute, Troy, NY 12181, USA
- A. D. Storrs, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
- E. N. Wells, Astronomy Programs, Computer Sciences Corporation, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - Richard P. Binzel
- P. C. Thomas, Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA
- R. P. Binzel, Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
- M. J. Gaffey, Department of Earth and Environmental Sciences, Rensselaer Polytechnic Institute, Troy, NY 12181, USA
- A. D. Storrs, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
- E. N. Wells, Astronomy Programs, Computer Sciences Corporation, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - Michael J. Gaffey
- P. C. Thomas, Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA
- R. P. Binzel, Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
- M. J. Gaffey, Department of Earth and Environmental Sciences, Rensselaer Polytechnic Institute, Troy, NY 12181, USA
- A. D. Storrs, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
- E. N. Wells, Astronomy Programs, Computer Sciences Corporation, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - Alex D. Storrs
- P. C. Thomas, Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA
- R. P. Binzel, Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
- M. J. Gaffey, Department of Earth and Environmental Sciences, Rensselaer Polytechnic Institute, Troy, NY 12181, USA
- A. D. Storrs, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
- E. N. Wells, Astronomy Programs, Computer Sciences Corporation, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - Eddie N. Wells
- P. C. Thomas, Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA
- R. P. Binzel, Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
- M. J. Gaffey, Department of Earth and Environmental Sciences, Rensselaer Polytechnic Institute, Troy, NY 12181, USA
- A. D. Storrs, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
- E. N. Wells, Astronomy Programs, Computer Sciences Corporation, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - Benjamin H. Zellner
- P. C. Thomas, Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA
- R. P. Binzel, Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
- M. J. Gaffey, Department of Earth and Environmental Sciences, Rensselaer Polytechnic Institute, Troy, NY 12181, USA
- A. D. Storrs, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
- E. N. Wells, Astronomy Programs, Computer Sciences Corporation, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
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Pieters CM, Fischer EM, Rode O, Basu A. Optical effects of space weathering: The role of the finest fraction. ACTA ACUST UNITED AC 1993. [DOI: 10.1029/93je02467] [Citation(s) in RCA: 239] [Impact Index Per Article: 7.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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49
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Cloutis EA, Gaffey MJ. Pyroxene spectroscopy revisited: Spectral-compositional correlations and relationship to geothermometry. ACTA ACUST UNITED AC 1991. [DOI: 10.1029/91je02512] [Citation(s) in RCA: 310] [Impact Index Per Article: 9.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Abstract
Infrared absorption spectra of a low-albedo water-rich asteroid appear to show a weak 3.4-micrometer carbon-hydrogen stretching mode band, which suggests the presence of hydrocarbons on asteroid 130 Elektra. The organic extract from the primitive carbonaceous chondritic Murchison meteorite shows similar spectral bands.
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