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  • 1
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    Constraints on olivine-rich rock types on the Moon as observed by Diviner and M3: Implications for the formation of the lunar crust (2016)
    Wiley
    Details
    Publication Date: 2016-06-28
    Description: We place upper limits on lunar olivine abundance using mid infrared (5-25 µm) (MIR) data from the Lunar Reconnaissance Orbiter Diviner Lunar Radiometer Experiment (Diviner) along with effective emissivity spectra of mineral mixtures in a simulated lunar environment. Olivine-bearing, pyroxene-poor lithologies have been identified on the lunar surface with visible-near infrared (VNIR) observations. Since the Kaguya Spectral Profiler (SP) VNIR survey of olivine-rich regions [ Yamamoto et al ., 2010] is the most complete to date, we focus this work on exposures identified by that study. We first confirmed the locations with VNIR data from the Moon Mineralogy Mapper (M 3 ) instrument. We then developed a Diviner olivine index from our laboratory data which, along with M 3 and Lunar Reconnaissance Orbiter Camera (LROC) wide angle camera (WAC) data, was used to select the geographic area over which Diviner emissivity data were extracted. We calculate upper limits on olivine abundance for these areas using laboratory emissivity spectra of anorthite-forsterite mixtures acquired under lunar-like conditions. We find that these exposures have widely varying olivine content. In addition, after applying an albedo-based space weathering correction to the Diviner data, we find that none of the areas are unambiguously consistent with concentrations of forsterite exceeding 90 wt%, in contrast to the higher abundance estimates derived from VNIR data.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 2
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    Particle Size Effects on Mid‐IR Spectra of Lunar Analog Minerals in a Simulated Lunar Environment (2019)
    Wiley
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    Publication Date: 2019
    Description: Abstract Mid‐infrared spectroscopic analysis of the Moon and other airless bodies requires a full accounting of spectral variation due to the unique thermal environment in airless body regoliths and the substantial differences between spectra acquired under airless body conditions and those measured in an ambient environment on Earth. Because there exists a thermal gradient within the upper 100s of microns of lunar regolith, the data acquired by the Diviner Lunar Radiometer Experiment are not isothermal with wavelength. While this complication has been previously identified, its effect on other known variables that contribute to spectral variation, such as particle size and porosity, have yet to be well characterized in the laboratory. Here we examine the effect of particle size on mid‐infrared spectra of silicates common to the Moon measured within a simulated lunar environment chamber. Under simulated lunar conditions, decreasing particle size is shown to enhance the spectral contrast of the Reststrahlen bands and transparency features, as well as shift the location of the Christiansen feature to longer wavelengths. This study shows that these variations are detectable at Diviner spectral resolution, and emphasizes the need for simulated environment laboratory datasets, as well as hyperspectral mid‐infrared instruments on future missions to airless bodies.
    Print ISSN: 2169-9097
    Electronic ISSN: 2169-9100
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 3
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    Chloride-bearing materials in the southern highlands of Mars (2008)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2008-03-22
    Description: Chlorides commonly precipitate during the evaporation of surface water or groundwater and during volcanic outgassing. Spectrally distinct surface deposits consistent with chloride-bearing materials have been identified and mapped using data from the 2001 Mars Odyssey Thermal Emission Imaging System. These deposits are found throughout regions of low albedo in the southern highlands of Mars. Geomorphologic evidence from orbiting imagery reveals these deposits to be light-toned relative to their surroundings and to be polygonally fractured. The deposits are small (〈 approximately 25 km(2)) but globally widespread, occurring in middle to late Noachian terrains with a few occurrences in early Hesperian terrains. The identification of chlorides in the ancient southern highlands suggests that near-surface water was available and widespread in early Martian history.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Osterloo, M M -- Hamilton, V E -- Bandfield, J L -- Glotch, T D -- Baldridge, A M -- Christensen, P R -- Tornabene, L L -- Anderson, F S -- New York, N.Y. -- Science. 2008 Mar 21;319(5870):1651-4. doi: 10.1126/science.1150690.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Hawaii Institute of Geophysics and Planetology, University of Hawaii, 1680 East-West Road, Honolulu, HI 96822, USA. osterloo@higp.hawaii.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18356522" target="_blank"〉PubMed〈/a〉
    Keywords: Chemical Precipitation ; *Chlorides ; Extraterrestrial Environment ; *Mars ; Time ; *Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 4
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    Highly silicic compositions on the Moon (2010)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2010-09-18
    Description: Using data from the Diviner Lunar Radiometer Experiment, we show that four regions of the Moon previously described as "red spots" exhibit mid-infrared spectra best explained by quartz, silica-rich glass, or alkali feldspar. These lithologies are consistent with evolved rocks similar to lunar granites in the Apollo samples. The spectral character of these spots is distinct from surrounding mare and highlands material and from regions composed of pure plagioclase feldspar. The variety of landforms associated with the silicic spectral character suggests that both extrusive and intrusive silicic magmatism occurred on the Moon. Basaltic underplating is the preferred mechanism for silicic magma generation, leading to the formation of extrusive landforms. This mechanism or silicate liquid immiscibility could lead to the formation of intrusive bodies.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Glotch, Timothy D -- Lucey, Paul G -- Bandfield, Joshua L -- Greenhagen, Benjamin T -- Thomas, Ian R -- Elphic, Richard C -- Bowles, Neil -- Wyatt, Michael B -- Allen, Carlton C -- Donaldson Hanna, Kerri -- Paige, David A -- New York, N.Y. -- Science. 2010 Sep 17;329(5998):1510-3. doi: 10.1126/science.1192148.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geosciences, Stony Brook University, Stony Brook, NY, USA. tglotch@notes.cc.sunysb.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20847267" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 5
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    Global silicate mineralogy of the Moon from the Diviner lunar radiometer (2010)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2010-09-18
    Description: We obtained direct global measurements of the lunar surface using multispectral thermal emission mapping with the Lunar Reconnaissance Orbiter Diviner Lunar Radiometer Experiment. Most lunar terrains have spectral signatures that are consistent with known lunar anorthosite and basalt compositions. However, the data have also revealed the presence of highly evolved, silica-rich lunar soils in kilometer-scale and larger exposures, expanded the compositional range of the anorthosites that dominate the lunar crust, and shown that pristine lunar mantle is not exposed at the lunar surface at the kilometer scale. Together, these observations provide compelling evidence that the Moon is a complex body that has experienced a diverse set of igneous processes.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Greenhagen, Benjamin T -- Lucey, Paul G -- Wyatt, Michael B -- Glotch, Timothy D -- Allen, Carlton C -- Arnold, Jessica A -- Bandfield, Joshua L -- Bowles, Neil E -- Donaldson Hanna, Kerri L -- Hayne, Paul O -- Song, Eugenie -- Thomas, Ian R -- Paige, David A -- New York, N.Y. -- Science. 2010 Sep 17;329(5998):1507-9. doi: 10.1126/science.1192196.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA. benjamin.t.greenhagen@jpl.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20847266" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 6
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    Initial results from the Mini-TES experiment in Gusev Crater from the Spirit Rover (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-08-07
    Description: The Miniature Thermal Emission Spectrometer (Mini-TES) on Spirit has studied the mineralogy and thermophysical properties at Gusev crater. Undisturbed soil spectra show evidence for minor carbonates and bound water. Rocks are olivinerich basalts with varying degrees of dust and other coatings. Dark-toned soils observed on disturbed surfaces may be derived from rocks and have derived mineralogy (+/-5 to 10%) of 45% pyroxene (20% Ca-rich pyroxene and 25% pigeonite), 40% sodic to intermediate plagioclase, and 15% olivine (forsterite 45% +/-5 to 10). Two spectrally distinct coatings are observed on rocks, a possible indicator of the interaction of water, rock, and airfall dust. Diurnal temperature data indicate particle sizes from 40 to 80 microm in hollows to approximately 0.5 to 3 mm in soils.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Christensen, P R -- Ruff, S W -- Fergason, R L -- Knudson, A T -- Anwar, S -- Arvidson, R E -- Bandfield, J L -- Blaney, D L -- Budney, C -- Calvin, W M -- Glotch, T D -- Golombek, M P -- Gorelick, N -- Graff, T G -- Hamilton, V E -- Hayes, A -- Johnson, J R -- McSween, H Y Jr -- Mehall, G L -- Mehall, L K -- Moersch, J E -- Morris, R V -- Rogers, A D -- Smith, M D -- Squyres, S W -- Wolff, M J -- Wyatt, M B -- New York, N.Y. -- Science. 2004 Aug 6;305(5685):837-42.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geological Sciences, Arizona State University, Tempe, AZ 85287, USA. phil.christensen@asu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15297667" target="_blank"〉PubMed〈/a〉
    Keywords: Carbonates ; Geologic Sediments ; Interferometry ; Iron Compounds ; Magnesium Compounds ; *Mars ; *Minerals ; Oxides ; Silicates ; Spectrum Analysis ; Temperature ; Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 7
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    Spectroscopic identification of carbonate minerals in the martian dust (2003)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2003-08-23
    Description: Thermal infrared spectra of the martian surface indicate the presence of small concentrations (approximately 2 to 5 weight %) of carbonates, specifically dominated by magnesite (MgCO3). The carbonates are widely distributed in the martian dust, and there is no indication of a concentrated source. The presence of small concentrations of carbonate minerals in the surface dust and in martian meteorites can sequester several bars of atmospheric carbon dioxide and may have been an important sink for a thicker carbon dioxide atmosphere in the martian past.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Bandfield, Joshua L -- Glotch, Timothy D -- Christensen, Philip R -- New York, N.Y. -- Science. 2003 Aug 22;301(5636):1084-7.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geological Sciences, Arizona State University, Tempe, AZ 85287-6305, USA. joshband@asu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/12934004" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Atmospheric Pressure ; Carbon Dioxide ; Carbonates/*analysis ; Extraterrestrial Environment ; Geologic Sediments ; Magnesium/*analysis ; *Mars ; Meteoroids ; Minerals/*analysis ; Particle Size ; Silicates/analysis ; Spectrophotometry, Infrared ; Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 8
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    Soils of Eagle crater and Meridiani Planum at the Opportunity Rover landing site (2004)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2004-12-04
    Description: The soils at the Opportunity site are fine-grained basaltic sands mixed with dust and sulfate-rich outcrop debris. Hematite is concentrated in spherules eroded from the strata. Ongoing saltation exhumes the spherules and their fragments, concentrating them at the surface. Spherules emerge from soils coated, perhaps from subsurface cementation, by salts. Two types of vesicular clasts may represent basaltic sand sources. Eolian ripples, armored by well-sorted hematite-rich grains, pervade Meridiani Planum. The thickness of the soil on the plain is estimated to be about a meter. The flatness and thin cover suggest that the plain may represent the original sedimentary surface.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Soderblom, L A -- Anderson, R C -- Arvidson, R E -- Bell, J F 3rd -- Cabrol, N A -- Calvin, W -- Christensen, P R -- Clark, B C -- Economou, T -- Ehlmann, B L -- Farrand, W H -- Fike, D -- Gellert, R -- Glotch, T D -- Golombek, M P -- Greeley, R -- Grotzinger, J P -- Herkenhoff, K E -- Jerolmack, D J -- Johnson, J R -- Jolliff, B -- Klingelhofer, G -- Knoll, A H -- Learner, Z A -- Li, R -- Malin, M C -- McLennan, S M -- McSween, H Y -- Ming, D W -- Morris, R V -- Rice, J W Jr -- Richter, L -- Rieder, R -- Rodionov, D -- Schroder, C -- Seelos, F P 4th -- Soderblom, J M -- Squyres, S W -- Sullivan, R -- Watters, W A -- Weitz, C M -- Wyatt, M B -- Yen, A -- Zipfel, J -- New York, N.Y. -- Science. 2004 Dec 3;306(5702):1723-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉U.S. Geological Survey, Flagstaff, AZ 86001, USA. lsoderblom@usgs.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15576606" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Ferric Compounds ; Geologic Sediments ; *Mars ; Minerals ; Silicates ; Spacecraft ; Spectrum Analysis ; Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 9
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    Mineralogy at Meridiani Planum from the Mini-TES Experiment on the Opportunity Rover (2004)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2004-12-04
    Description: The Miniature Thermal Emission Spectrometer (Mini-TES) on Opportunity investigated the mineral abundances and compositions of outcrops, rocks, and soils at Meridiani Planum. Coarse crystalline hematite and olivine-rich basaltic sands were observed as predicted from orbital TES spectroscopy. Outcrops of aqueous origin are composed of 15 to 35% by volume magnesium and calcium sulfates [a high-silica component modeled as a combination of glass, feldspar, and sheet silicates (approximately 20 to 30%)], and hematite; only minor jarosite is identified in Mini-TES spectra. Mini-TES spectra show only a hematite signature in the millimeter-sized spherules. Basaltic materials have more plagioclase than pyroxene, contain olivine, and are similar in inferred mineral composition to basalt mapped from orbit. Bounce rock is dominated by clinopyroxene and is close in inferred mineral composition to the basaltic martian meteorites. Bright wind streak material matches global dust. Waterlain rocks covered by unaltered basaltic sands suggest a change from an aqueous environment to one dominated by physical weathering.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Christensen, P R -- Wyatt, M B -- Glotch, T D -- Rogers, A D -- Anwar, S -- Arvidson, R E -- Bandfield, J L -- Blaney, D L -- Budney, C -- Calvin, W M -- Fallacaro, A -- Fergason, R L -- Gorelick, N -- Graff, T G -- Hamilton, V E -- Hayes, A G -- Johnson, J R -- Knudson, A T -- McSween, H Y Jr -- Mehall, G L -- Mehall, L K -- Moersch, J E -- Morris, R V -- Smith, M D -- Squyres, S W -- Ruff, S W -- Wolff, M J -- New York, N.Y. -- Science. 2004 Dec 3;306(5702):1733-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geological Sciences, Arizona State University, Tempe, AZ 85287, USA. phil.christensen@asu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15576609" target="_blank"〉PubMed〈/a〉
    Keywords: Calcium Sulfate ; Extraterrestrial Environment ; Ferric Compounds ; Geologic Sediments ; Iron Compounds ; Magnesium Compounds ; Magnesium Sulfate ; *Mars ; *Minerals ; Silicates ; Spacecraft ; Sulfates ; Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 10
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    The geology and astrobiology of McLaughlin Crater, Mars: an ancient lacustrine basin containing turbidites, mudstones and serpentinites (2019)
    Wiley
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    Publication Date: 2019
    Description: Abstract McLaughlin Crater is a 92 km‐diameter complex crater that formed on Mars ~4 billion years ago. The resulting basin was the site of a large (~3000 km2), deep (~500 m), voluminous (~1500 km3) Martian lake c.a. 3.8 Ga. While there is strong evidence that 100s of lakes have existed on Mars at some point during the same time period, the geology of McLaughlin Crater is extraordinary for a number of reasons. Detailed spectral analyses show that the deep water sediments include detrital inputs of olivine and pyroxene, but the lake‐floor sediments include lithologies with abundant Fe‐rich, Mg‐bearing smectite, serpentine‐rich deposits and ferrihydrite. For astrobiologists, this site provides a treasure trove of high‐priority targets. Serpentinization reactions are thought to have played a key role in abiogenesis on Earth and within McLaughlin Crater, deposits of subterranean and probably sub‐lacustrine serpentinites are well preserved. In addition, delta sequences are well exposed throughout the east side of the basin; such deposits are endorsed by some as the highest priority targets for preservation of organics on Mars. Yet, deep water turbidites, which might have flowed through hydrothermal environments may be the most intriguing aspect of this geology. Such rapid sedimentation could have sequestered and preserved any potential organic materials for future exploration by a rover.
    Print ISSN: 2169-9097
    Electronic ISSN: 2169-9100
    Topics: Geosciences , Physics
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