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Two Simulated Spectral Databases of Lunar Regolith: Method, Validation, and Application. REMOTE SENSING 2022. [DOI: 10.3390/rs14020277] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
Our simulated lunar regolith spectra database, based on the Hapke AMSA radiative transfer model (RTM), is a large supplement to the limited number of lunar spectra data. By analyzing the multiple solutions and applicable scopes of the Hapke model by means of Newton interpolation and the least square optimization method, an improved method was found for the simulation of spectra, but it remained challenging to use to invert mineral abundance. Then, we simulated the spectra, mineral abundance, particle size and maturity of 57 mare and highland samples of the Lunar Soil Characterization Consortium (LSCC) in size groups of 10 µm, 10–20 µm and 20–45 µm. The simulated and measured spectra fit well with each other, with correlation coefficients greater than 0.99 and root mean square errors at a magnitude of 10-3. The parameters of mineral abundance, particle size and maturity are highly consistent with the measured values. Having confirmed the reliability of our simulation method, we analyzed the mechanism, reliability and applicability of the “spectral characteristic angle parameter” proposed by Lucey using the simulated spectral data of lunar regolith. Lucey’s method is only suitable for macro analysis of the entire moon, and the error is large when it is used for areas with high abundance of forsterite or ilmenite. In the spectral simulation of lunar regolith, olivine was subdivided into forsterite and fayalite, and the two end-members were mixed to approximately estimate the effect of the chemical composition of olivine on the spectra, which has been confirmed to be feasible.
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2
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Vaci Z, Day JMD, Paquet M, Ziegler K, Yin QZ, Dey S, Miller A, Agee C, Bartoschewitz R, Pack A. Olivine-rich achondrites from Vesta and the missing mantle problem. Nat Commun 2021; 12:5443. [PMID: 34521838 PMCID: PMC8440560 DOI: 10.1038/s41467-021-25808-9] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/04/2020] [Accepted: 07/19/2021] [Indexed: 11/09/2022] Open
Abstract
Mantles of rocky planets are dominantly composed of olivine and its high-pressure polymorphs, according to seismic data of Earth's interior, the mineralogy of natural samples, and modelling results. The missing mantle problem represents the paucity of olivine-rich material among meteorite samples and remote observation of asteroids, given how common differentiated planetesimals were in the early Solar System. Here we report the discovery of new olivine-rich meteorites that have asteroidal origins and are related to V-type asteroids or vestoids. Northwest Africa 12217, 12319, and 12562 are dunites and lherzolite cumulates that have siderophile element abundances consistent with origins on highly differentiated asteroidal bodies that experienced core formation, and with trace element and oxygen and chromium isotopic compositions associated with the howardite-eucrite-diogenite meteorites. These meteorites represent a step towards the end of the shortage of olivine-rich material, allowing for full examination of differentiation processes acting on planetesimals in the earliest epoch of the Solar System.
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Affiliation(s)
- Zoltan Vaci
- Institute of Meteoritics, University of New Mexico, Albuquerque, NM, USA.
- Department of Earth and Planetary Sciences, University of New Mexico, Albuquerque, NM, USA.
| | - James M D Day
- Scripps Institution of Oceanography, University of California San Diego, La Jolla, CA, USA
| | - Marine Paquet
- Scripps Institution of Oceanography, University of California San Diego, La Jolla, CA, USA
| | - Karen Ziegler
- Institute of Meteoritics, University of New Mexico, Albuquerque, NM, USA
- Department of Earth and Planetary Sciences, University of New Mexico, Albuquerque, NM, USA
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California Davis, Davis, CA, USA
| | - Supratim Dey
- Department of Earth and Planetary Sciences, University of California Davis, Davis, CA, USA
| | - Audrey Miller
- Department of Earth and Planetary Sciences, University of California Davis, Davis, CA, USA
| | - Carl Agee
- Institute of Meteoritics, University of New Mexico, Albuquerque, NM, USA
- Department of Earth and Planetary Sciences, University of New Mexico, Albuquerque, NM, USA
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Li S, Lucey PG, Fraeman AA, Poppe AR, Sun VZ, Hurley DM, Schultz PH. Widespread hematite at high latitudes of the Moon. SCIENCE ADVANCES 2020; 6:6/36/eaba1940. [PMID: 32917587 PMCID: PMC7467685 DOI: 10.1126/sciadv.aba1940] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 11/12/2019] [Accepted: 07/17/2020] [Indexed: 06/11/2023]
Abstract
Hematite (Fe2O3) is a common oxidization product on Earth, Mars, and some asteroids. Although oxidizing processes have been speculated to operate on the lunar surface and form ferric iron-bearing minerals, unambiguous detections of ferric minerals forming under highly reducing conditions on the Moon have remained elusive. Our analyses of the Moon Mineralogy Mapper data show that hematite, a ferric mineral, is present at high latitudes on the Moon, mostly associated with east- and equator-facing sides of topographic highs, and is more prevalent on the nearside than the farside. Oxygen delivered from Earth's upper atmosphere could be the major oxidant that forms lunar hematite. Hematite at craters of different ages may have preserved the oxygen isotopes of Earth's atmosphere in the past billions of years. Future oxygen isotope measurements can test our hypothesis and may help reveal the evolution of Earth's atmosphere.
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Affiliation(s)
- Shuai Li
- Hawai'i Institute of Geophysics and Planetology, University of Hawaii, Honolulu, HI 96822, USA.
| | - Paul G Lucey
- Hawai'i Institute of Geophysics and Planetology, University of Hawaii, Honolulu, HI 96822, USA
| | - Abigail A Fraeman
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Andrew R Poppe
- Space Sciences Laboratory, University of California at Berkeley, Berkeley, CA 94720, USA
| | - Vivian Z Sun
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Dana M Hurley
- Applied Physics Laboratory Johns Hopkins, Laurel, MD 20723, USA
| | - Peter H Schultz
- Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI 02912, USA
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An Empirical Model to Estimate Abundance of Nanophase Metallic Iron (npFe0) in Lunar Soils. REMOTE SENSING 2020. [DOI: 10.3390/rs12061047] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
Lunar soils gradually become mature when they are exposed to a space environment, and nanophase metallic iron (npFe0) generates within them. npFe0 significantly changes the optical properties of lunar soils and affects the interpretation of the remotely sensed data of the lunar surface. In this study, a correlation analysis was conducted between npFe0 abundance and reflectance spectra at short wavelengths for lunar soil samples in four size groups based on their spectral and compositional data, collected by the Lunar Soil Characterization Consortium (LSCC). Results show that 540 nm single scattering albedo (SSA) of lunar soils correlates well with their corresponding npFe0 abundance for each size group of lunar soil samples. However, it is poorly correlated with npFe0 abundance when all size groups were considered because of the strong interference from grain size variation of lunar soils. To minimize the effect of grain size, the correlation of npFe0 abundance with the spectral ratio of 540 nm/810 nm SSA of all size groups for LSCC samples was calculated and results show that a higher correlation existed between them (R2 = 0.91). This ratio can serve as a simple empirical model for estimating npFe0 abundance in lunar soils. However, bias could be introduced to the estimation result when lunar soils possess a high content of agglutinitic glass and ilmenite. Our future work will focus on improving the model’s performance for these lunar soils.
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Li S, Lucey PG, Milliken RE, Hayne PO, Fisher E, Williams JP, Hurley DM, Elphic RC. Direct evidence of surface exposed water ice in the lunar polar regions. Proc Natl Acad Sci U S A 2018; 115:8907-8912. [PMID: 30126996 PMCID: PMC6130389 DOI: 10.1073/pnas.1802345115] [Citation(s) in RCA: 212] [Impact Index Per Article: 35.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Water ice may be allowed to accumulate in permanently shaded regions on airless bodies in the inner solar system such as Mercury, the Moon, and Ceres [Watson K, et al. (1961) J Geophys Res 66:3033-3045]. Unlike Mercury and Ceres, direct evidence for water ice exposed at the lunar surface has remained elusive. We utilize indirect lighting in regions of permanent shadow to report the detection of diagnostic near-infrared absorption features of water ice in reflectance spectra acquired by the Moon Mineralogy Mapper [M (3)] instrument. Several thousand M (3) pixels (∼280 × 280 m) with signatures of water ice at the optical surface (depth of less than a few millimeters) are identified within 20° latitude of both poles, including locations where independent measurements have suggested that water ice may be present. Most ice locations detected in M (3) data also exhibit lunar orbiter laser altimeter reflectance values and Lyman Alpha Mapping Project instrument UV ratio values consistent with the presence of water ice and also exhibit annual maximum temperatures below 110 K. However, only ∼3.5% of cold traps exhibit ice exposures. Spectral modeling shows that some ice-bearing pixels may contain ∼30 wt % ice that is intimately mixed with dry regolith. The patchy distribution and low abundance of lunar surface-exposed water ice might be associated with the true polar wander and impact gardening. The observation of spectral features of H2O confirms that water ice is trapped and accumulates in permanently shadowed regions of the Moon, and in some locations, it is exposed at the modern optical surface.
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Affiliation(s)
- Shuai Li
- Department of Geology and Geophysics, University of Hawaii, Honolulu, HI 96822;
- Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI 02912
| | - Paul G Lucey
- Department of Geology and Geophysics, University of Hawaii, Honolulu, HI 96822
| | - Ralph E Milliken
- Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI 02912
| | - Paul O Hayne
- Department of Astrophysical & Planetary Sciences, University of Colorado Boulder, Boulder, CO 80309
| | - Elizabeth Fisher
- Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI 02912
| | - Jean-Pierre Williams
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA 90095
| | - Dana M Hurley
- Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723
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Formation of lunar swirls by magnetic field standoff of the solar wind. Nat Commun 2015; 6:6189. [PMID: 25650225 DOI: 10.1038/ncomms7189] [Citation(s) in RCA: 53] [Impact Index Per Article: 5.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/19/2013] [Accepted: 01/02/2015] [Indexed: 11/08/2022] Open
Abstract
Lunar swirls are high-albedo markings on the Moon that occur in both mare and highland terrains; their origin remains a point of contention. Here, we use data from the Lunar Reconnaissance Orbiter Diviner Lunar Radiometer to support the hypothesis that the swirls are formed as a result of deflection of the solar wind by local magnetic fields. Thermal infrared data from this instrument display an anomaly in the position of the silicate Christiansen Feature consistent with reduced space weathering. These data also show that swirl regions are not thermophysically anomalous, which strongly constrains their formation mechanism. The results of this study indicate that either solar wind sputtering and implantation are more important than micrometeoroid bombardment in the space-weathering process, or that micrometeoroid bombardment is a necessary but not sufficient process in space weathering, which occurs on airless bodies throughout the solar system.
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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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8
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Taylor LA, Pieters C, Patchen A, Taylor DHS, Morris RV, Keller LP, McKay DS. Mineralogical and chemical characterization of lunar highland soils: Insights into the space weathering of soils on airless bodies. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003427] [Citation(s) in RCA: 69] [Impact Index Per Article: 4.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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9
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Milliken RE, Mustard JF, Poulet F, Jouglet D, Bibring JP, Gondet B, Langevin Y. Hydration state of the Martian surface as seen by Mars Express OMEGA: 2. H2O content of the surface. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002853] [Citation(s) in RCA: 84] [Impact Index Per Article: 4.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Ralph E. Milliken
- Department of Geological Sciences; Brown University; Providence Rhode Island USA
| | - John F. Mustard
- Department of Geological Sciences; Brown University; Providence Rhode Island USA
| | | | - Denis Jouglet
- Institut d'Astrophysique Spatiale (IAS); Orsay Cedex France
| | | | | | - Yves Langevin
- Institut d'Astrophysique Spatiale (IAS); Orsay Cedex France
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10
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Noble SK, Pieters CM, Hiroi T, Taylor LA. Using the modified Gaussian model to extract quantitative data from lunar soils. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002721] [Citation(s) in RCA: 31] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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11
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Arvidson RE, Poulet F, Morris RV, Bibring JP, Bell JF, Squyres SW, Christensen PR, Bellucci G, Gondet B, Ehlmann BL, Farrand WH, Fergason RL, Golombek M, Griffes JL, Grotzinger J, Guinness EA, Herkenhoff KE, Johnson JR, Klingelhöfer G, Langevin Y, Ming D, Seelos K, Sullivan RJ, Ward JG, Wiseman SM, Wolff M. Nature and origin of the hematite-bearing plains of Terra Meridiani based on analyses of orbital and Mars Exploration rover data sets. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002728] [Citation(s) in RCA: 131] [Impact Index Per Article: 7.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- R. E. Arvidson
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - F. Poulet
- Institut d'Astrophysique Spatiale; Université Paris-Sud; Orsay France
| | | | - J.-P. Bibring
- Institut d'Astrophysique Spatiale; Université Paris-Sud; Orsay France
| | - J. F. Bell
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - S. W. Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - P. R. Christensen
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - G. Bellucci
- Istituto di Fisica dello Spazio Interplanetario; Istituto Nazionale di Astrofisica; Rome Italy
| | - B. Gondet
- Institut d'Astrophysique Spatiale; Université Paris-Sud; Orsay France
| | - B. L. Ehlmann
- School of Geography and Environment; University of Oxford; Oxford UK
| | | | - R. L. Fergason
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - M. Golombek
- Jet Propulsion Laboratory; Pasadena California USA
| | - J. L. Griffes
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - J. Grotzinger
- Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
| | - E. A. Guinness
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | | | | | - G. Klingelhöfer
- Institut für Anorganische und Analytische Chemie; Johannes Gutenberg-Universität; Mainz Germany
| | - Y. Langevin
- Institut d'Astrophysique Spatiale; Université Paris-Sud; Orsay France
| | - D. Ming
- NASA Johnson Space Center; Houston Texas USA
| | - K. Seelos
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - R. J. Sullivan
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - J. G. Ward
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - S. M. Wiseman
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - M. Wolff
- Space Science Institute; Boulder Colorado USA
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Wilcox BB, Lucey PG, Gillis JJ. Mapping iron in the lunar mare: An improved approach. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2005je002512] [Citation(s) in RCA: 41] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Anand M, Taylor LA, Nazarov MA, Shu J, Mao HK, Hemley RJ. Space weathering on airless planetary bodies: clues from the lunar mineral hapkeite. Proc Natl Acad Sci U S A 2004; 101:6847-51. [PMID: 15118081 PMCID: PMC406430 DOI: 10.1073/pnas.0401565101] [Citation(s) in RCA: 80] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Physical and chemical reactions occurring as a result of the high-velocity impacts of meteorites and micrometeorites and of cosmic rays and solar-wind particles are major causes of space weathering on airless planetary bodies, such as the Moon, Mercury, and asteroids. These weathering processes are responsible for the formation of their regolith and soil. We report here the natural occurrence of the mineral hapkeite, a Fe2Si phase, and other associated Fe-Si phases (iron-silicides) in a regolith breccia clast of a lunar highland meteorite. These Fe-Si phases are considered to be a direct product of impact-induced, vapor-phase deposition in the lunar soil, all part of space weathering. We have used an in situ synchrotron energy-dispersive, single-crystal x-ray diffraction technique to confirm the crystal structure of hapkeite as similar to the structure of synthetic Fe2Si. This mineral, hapkeite, is named after Bruce Hapke of the University of Pittsburgh, who predicted the presence and importance of vapor-deposited coatings on lunar soil grains some 30 years ago. We propose that this mineral and other Fe-Si phases are probably more common in the lunar regolith than previously thought and are directly related to the formation of vapor-deposited, nanophase elemental iron in the lunar soils.
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Affiliation(s)
- Mahesh Anand
- Planetary Geosciences Institute, Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996, USA.
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Lawrence DJ, Feldman WC, Elphic RC, Little RC, Prettyman TH, Maurice S, Lucey PG, Binder AB. Iron abundances on the lunar surface as measured by the Lunar Prospector gamma-ray and neutron spectrometers. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2001je001530] [Citation(s) in RCA: 176] [Impact Index Per Article: 8.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- D. J. Lawrence
- Space and Atmospheric Sciences; Los Alamos National Laboratory; Los Alamos New Mexico USA
| | - W. C. Feldman
- Space and Atmospheric Sciences; Los Alamos National Laboratory; Los Alamos New Mexico USA
| | - R. C. Elphic
- Space and Atmospheric Sciences; Los Alamos National Laboratory; Los Alamos New Mexico USA
| | - R. C. Little
- Diagnostic Applications, Los Alamos National Laboratory; Los Alamos New Mexico USA
| | - T. H. Prettyman
- Space and Atmospheric Sciences; Los Alamos National Laboratory; Los Alamos New Mexico USA
| | - S. Maurice
- Observatoire Midi-Pyrénées; Toulouse France
| | - P. G. Lucey
- Hawai'i Institute of Geophysics and Planetology; University of Hawaii; Honolulu Hawaii USA
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16
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Taylor LA, Pieters CM, Keller LP, Morris RV, McKay DS. Lunar Mare Soils: Space weathering and the major effects of surface-correlated nanophase Fe. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001402] [Citation(s) in RCA: 227] [Impact Index Per Article: 9.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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18
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Hood LL, Zakharian A, Halekas J, Mitchell DL, Lin RP, Acuña MH, Binder AB. Initial mapping and interpretation of lunar crustal magnetic anomalies using Lunar Prospector magnetometer data. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001366] [Citation(s) in RCA: 157] [Impact Index Per Article: 6.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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19
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Starukhina L. Water detection on atmosphereless celestial bodies: Alternative explanations of the observations. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001307] [Citation(s) in RCA: 70] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Veverka J, Robinson M, Thomas P, Murchie S, Bell JF, Izenberg N, Chapman C, Harch A, Bell M, Carcich B, Cheng A, Clark B, Domingue D, Dunham D, Farquhar R, Gaffey MJ, Hawkins E, Joseph J, Kirk R, Li H, Lucey P, Malin M, Martin P, McFadden L, Merline WJ, Miller JK. NEAR at eros: imaging and spectral results. Science 2000; 289:2088-97. [PMID: 11000105 DOI: 10.1126/science.289.5487.2088] [Citation(s) in RCA: 200] [Impact Index Per Article: 8.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Eros is a very elongated (34 kilometers by 11 kilometers by 11 kilometers) asteroid, most of the surface of which is saturated with craters smaller than 1 kilometer in diameter. The largest crater is 5.5 kilometers across, but there is a 10-kilometer saddle-like depression with attributes of a large degraded crater. Surface lineations, both grooves and ridges, are prominent on Eros; some probably exploit planes of weakness produced by collisions on Eros and/or its parent body. Ejecta blocks (30 to 100 meters across) are abundant but not uniformly distributed over the surface. Albedo variations are restricted to the inner walls of certain craters and may be related to downslope movement of regolith. On scales of 200 meters to 1 kilometer, Eros is more bland in terms of color variations than Gaspra or Ida. Spectra (800 to 2500 nanometers) are consistent with an ordinary chondrite composition for which the measured mean density of 2.67 +/- 0.1 grams per cubic centimeter implies internal porosities ranging from about 10 to 30 percent.
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Affiliation(s)
- J Veverka
- Space Sciences Building, Cornell University, Ithaca, NY 14853, USA. Department of Geological Sciences, Northwestern University, 309 Locy Hall, Evanston, IL 60208, USA. Applied Physics Laboratory, Johns Hopkins University, 1110 Johns Hopkins Road, L
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Le Mouélic S, Langevin Y, Erard S, Pinet P, Chevrel S, Daydou Y. Discrimination between maturity and composition of lunar soils from integrated Clementine UV-visible/near-infrared data: Application to the Aristarchus Plateau. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001196] [Citation(s) in RCA: 64] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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23
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Pinet PC, Shevchenko VV, Chevrel SD, Daydou Y, Rosemberg C. Local and regional lunar regolith characteristics at Reiner Gamma Formation: Optical and spectroscopic properties from Clementine and Earth-based data. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001086] [Citation(s) in RCA: 65] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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24
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Dukes CA, Baragiola RA, McFadden LA. Surface modification of olivine by H+and He+bombardment. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/98je02820] [Citation(s) in RCA: 85] [Impact Index Per Article: 3.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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25
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Binzel RP, Bus SJ, Burbine TH, Sunshine JM. Spectral Properties of Near-Earth Asteroids: Evidence for Sources of Ordinary Chondrite Meteorites. Science 1996; 273:946-8. [PMID: 8688076 DOI: 10.1126/science.273.5277.946] [Citation(s) in RCA: 111] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/01/2023]
Abstract
Although ordinary chondrite (OC) meteorites dominate observed falls, the identification of near-Earth and main-belt asteroid sources has remained elusive. Telescopic measurements of 35 near-Earth asteroids ( approximately3 kilometers in diameter) revealed six that have visible wavelength spectra similar to laboratory spectra of OC meteorites. Near-Earth asteroids were found to have spectral properties that span the range between the previously separated domains of OC meteorites and the most common (S class) asteroids, suggesting a link. This range of spectral properties could arise through a diversity of mineralogies and regolith particle sizes, as well as through a time-dependent surface weathering process.
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Affiliation(s)
- RP Binzel
- R. P. Binzel, S. J. Bus, T. H. Burbine, Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA. J. M. Sunshine, Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, and Science Applications International Corporation, 4501 Daly Drive, Chantilly, VA 22021, USA
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Bishop JL, Koeberl C, Kralik C, Fröschl H, Englert PA, Andersen DW, Pieters CM, Wharton RA. Reflectance spectroscopy and geochemical analyses of Lake Hoare sediments, Antarctica: implications for remote sensing of the Earth and Mars. GEOCHIMICA ET COSMOCHIMICA ACTA 1996; 60:765-785. [PMID: 11539146 DOI: 10.1016/0016-7037(95)00432-7] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
Visible to infrared reflectance spectroscopic analyses (0.3-25 micromoles) have been performed on sediments from the Dry Valleys region of Antarctica. Sample characterization for these sediments includes extensive geochemical analyses and X-ray diffraction (XRD). The reflectance spectra and XRD indicate major amounts of quartz, feldspar, and pyroxene in these samples and lesser amounts of carbonate, mica, chlorite, amphibole, illite, smectite, and organic matter. Calcite is the primary form of carbonate present in these Lake Hoare sediments based on the elemental abundances and spectroscopic features. The particle size distribution of the major and secondary components influences their detection in mixtures and this sensitivity to particle size is manifested differently in the "volume scattering" and "surface scattering" infrared regions. The Christiansen feature lies between these two spectral regimes and is influenced by the spectral properties of both regions. For these mixtures the Christiansen feature was found to be dependent on physical parameters, such as particle size and sample texture, as well as the mineralogy. Semiquantitative spectroscopic detection of calcite and organic material has been tested in these quartz- and feldspar-rich sediments. The relative spectral band depths due to organics and calcite correlate in general with the wt% C from organic matter and carbonate. The amounts of organic matter and carbonate present correlate with high Br and U abundances and high Ca and Sr abundances, respectively. Variation in the elemental abundances was overall minimal, which is consistent with a common sedimentary origin for the forty-two samples studied here from Lake Hoare.
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Affiliation(s)
- J L Bishop
- DLR, Institute for Planetary Exploration, Rudower Chausee, Berlin, Germany
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Fischer EM, Pieters CM. Lunar surface aluminum and iron concentration from Galileo solid state imaging data, and the mixing of mare and highland materials. ACTA ACUST UNITED AC 1995. [DOI: 10.1029/95je02359] [Citation(s) in RCA: 36] [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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Pieters CM, Staid MI, Fischer EM, Tompkins S, He G. A Sharper View of Impact Craters from Clementine Data. Science 1994; 266:1844-8. [PMID: 17737078 DOI: 10.1126/science.266.5192.1844] [Citation(s) in RCA: 119] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The ultraviolet-visible camera on the Clementine spacecraft obtained high-spatial resolution images of the moon in five spectral channels. Impact craters mapped with these multispectral images show a scale of lithologic diversity that varies with crater size and target stratigraphy. Prominent lithologic variations (feldspathic versus basaltic) occur within the south wall of Copernicus (93 kilometers in diameter) on the scale of 1 to 2 kilometers. Lithologic diversity at Tycho (85 kilometers in diameter) is less apparent at this scale, although the impact melt of these two large craters is remarkably similar in this spectral range. The lunar surface within and around the smaller crater Giordano Bruno (22 kilometers in diameter) is largely dominated by the mixing of freshly excavated material with surrounding older soils derived from a generally similar feldspathic lithology.
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Hiroi T, Pieters CM. Estimation of grain sizes and mixing ratios of fine powder mixtures of common geologic minerals. ACTA ACUST UNITED AC 1994. [DOI: 10.1029/94je00841] [Citation(s) in RCA: 62] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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