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  • 1
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    The Sustainability of Habitability on Terrestrial Planets: Insights, Questions, and Needed Measurements from Mars for Understanding the Evolution of Earth-like Worlds (2016)
    Wiley
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    Publication Date: 2016-09-17
    Description: With the advent of exoplanetary astronomy and the ongoing discovery of terrestrial-type planets around other stars, our own solar system becomes a key testing ground for ideas about what factors control planetary evolution. In particular, what allows a planet to be both within a potentially habitable zone and sustain habitability over long geologic time, are crucial issues. In this regard, Mars is uniquely suited, providing the solar system's longest record of the interplay of the physical and chemical processes relevant to habitability on an accessible rocky planet with an atmosphere and hydrosphere. Here we review current understanding and update the timeline of key processes in early Mars history. We then draw on knowledge of exoplanets and the other solar system terrestrial planets to identify 6 broad questions of high importance to the development and sustaining of habitability (unprioritized): (1) Is small planetary size fatal? (2) How do magnetic fields influence atmospheric evolution? (3) To what extent does starting composition dictate subsequent evolution, including redox processes and the availability of water and organics? (4) Does early bombardment during an era of higher impact flux have a net deleterious or beneficial influence? (5) How do planetary climates respond to stellar evolution, e.g., sustaining early liquid water in spite of a faint young sun? (6) How important are the timescales of climate forcing and their dynamical drivers? Finally, we suggest crucial Mars measurements (unprioritized) to address these questions: (1) in situ petrology at multiple units/sites; (2) continued quantification of volatile reservoirs and new isotopic measurements of H, C, N, O, S, Cl, and noble gases in rocks that sample multiple stratigraphic sections; (3) radiometric age dating of units in stratigraphic sections and from key volcanic and impact units; (4) higher resolution measurements of heat flux, subsurface structure, and magnetic field anomalies coupled with absolute age dating. The unique dataset recording the evolution of early Mars will feed forward to understanding divergent evolutionary paths of the Earth, Venus, and thousands of small rocky extrasolar planets yet to be discovered.
    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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    Mineralogy and chemistry of altered Icelandic basalts: Application to clay mineral detection and understanding aqueous environments on Mars (2012)
    Wiley
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    Publication Date: 2012-10-13
    Description: We used a suite of techniques, including those emulating compositional data sets obtained from Mars orbit and obtainable at the Mars surface, to examine aqueous alteration of basaltic rocks from Iceland as a mineralogic and geochemical analog for Noachian environments on Mars. A sample suite was collected for laboratory measurement of (1) whole-rock visible/near-infrared (VNIR) reflectance and thermal infrared (TIR) emission spectra; (2) VNIR and TIR reflectance spectra of particle-size separates derived from the bulk rock and from materials extracted from fractures/vesicles; (3) X-ray diffraction (XRD) patterns for determination of quantitative modal mineralogy; (4) major element chemistry using flux fusion of whole-rock powders; and (5) electron microprobe analyses of minerals in thin sections. Conclusions about aqueous alteration can be influenced by technique. For these basalts, whole-rock chemical data showed scant evidence for chemical fractionation, but TIR, VNIR, and XRD measurements identified distinctive assemblages of hydrous silicate minerals, differing by sample. XRD provided the most complete and accurate quantitative determination of sample mineralogy. However, VNIR spectroscopy was the technique most useful for determining composition of low-abundance smectite clays, and TIR spectroscopy was the most useful for recognizing hydrated silicates in thin surface coatings. High spatial resolution mineralogical and chemical data sets were useful for understanding the texture and distribution of alteration products and variations in fluid chemistry. No single approach provides a complete assessment of the environment of alteration, demonstrating the importance of employing multiple, synergistic mineralogical and geochemical techniques and instruments in exploration of rock strata from aqueous paleoenvironments on Mars.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
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  • 3
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    Low temperature aqueous alteration of basalt: Mineral assemblages of Deccan basalts and implications for Mars (2012)
    Wiley
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    Publication Date: 2012-09-18
    Description: Al-rich phyllosilicates (kaolinite, montmorillonite) have been found in layers overlying Fe/Mg-smectites on Mars, and it has been suggested that this stratigraphy formed through in situ leaching at the surface, similar to terrestrial weathering profiles. We are investigating the remotely sensed signatures of this type of weathering using ten samples from a vertical section of altered Deccan basalts and four samples collected nearby as an analog for leaching resulting in Al-rich phyllosilicate over Fe/Mg-smectite stratigraphies. Samples were analyzed with reflectance spectroscopy from 0.28 to 25.0 μm, inductively coupled plasma atomic emission spectrometry for 10 major element concentrations (Al, Ca, Fe, K, Mg, Mn, Na, P, Si, Ti), loss on ignition for volatiles, x-ray diffraction (XRD) for mineralogies, and Mössbauer spectroscopy for Fe redox state. Spectra of basalt samples were dominated by Fe2+ crystal field transitions with weak alteration bands near 1.4 and/or 1.9 μm. Reststrahlen bands in mid-infrared showed the convolution of plagioclase and pyroxene features typical of basalts. Saprolite samples were incompletely leached, and their spectra were dominated by complex Al- and Fe/Mg-bearing smectite clays and retained no original mafic signatures. XRD and Mössbauer detected pyroxene and plagioclase not visible by reflectance spectroscopy in some saprolite samples. Zeolites were present throughout the saprolite. The laterite was the most leached horizon, and all analyses showed kaolinite and iron oxide assemblages. This kaolinite and hematite association would be expected if kaolinite on Mars formed through leaching under conditions similar to those on Earth and has implications for abundant freshwater on the Martian surface.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
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  • 4
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    Compositional variability of the Marius Hills volcanic complex from the Moon Mineralogy Mapper (M3) (2011)
    Wiley
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    Publication Date: 2011-05-12
    Description: Using the Moon Mineralogy Mapper(M3), we examine the Marius Hills volcanic complex for the first time from 0.46 to 2.97 μm. The integrated band depth at 1 μm separates the mare basalts on the plateau in two units: (1) a strong 1 μm band unit of localized lava flows within the plateau that has similar olivine-rich signatures to those of the nearby Oceanus Procellarum and (2) a weaker 1 μm band unit that characterizes most of the basalts of the plateau, which is interpreted as having a high-calcium pyroxene signature. Domes and cones within the complex belong to the high-calcium pyroxene plateau unit and are associated with the weakest 1 μm band observed on the plateau. This difference could be the result of higher silica content, more opaque minerals, and/or a weaker olivine content of the magma. Finally, the floor of Marius crater has one of the strongest olivine-rich signatures of the entire Marius Hills complex. These compositional differences are indicative of the long and complex volcanic history of the region. The first episode started before the emplacement of the surrounding basalts of the plateau and produced the high-calcium pyroxene flows present on the plateau and their associated domes and cones. The second episode occurred concurrently or slightly after the emplacement of the adjacent Procellarum basalts and produced the olivine-rich basalts seen within the plateau, outside the plateau, and in Marius crater. If the olivine content of the lava flows increases with time, the olivine-rich region on the floor of Marius crater may represent one of the latest episodes of volcanism exposed on the Marius Hills complex.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
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  • 5
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    Global Assessment of Pure Crystalline Plagioclase across the Moon and Implications for the Evolution of the Primary Crust (2014)
    Wiley
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    Publication Date: 2014-05-02
    Description: Recent advancements in visible- to near- infrared orbital measurements of the lunar surface have allowed have allowed the character and extent of the primary anorthositic crust to be studied at unprecedented spatial and spectral resolutions. Here we assess the lunar primary anorthositic crust in global context using a spectral parameter tool for Moon Mineralogy Mapper (M 3 ) data to identify and map Fe-bearing, crystalline plagioclase based on its diagnostic 1.25  μ m absorption band. This allows plagioclase-dominated rocks, specifically anorthosites, to be unambiguously identified as well as distinguished from lithologies with minor to trace amounts of mafic minerals. Low spatial resolution global mosaics and high spatial resolution individual data strips covering more than 650 targeted craters were analyzed to identify and map the mineralogy of spectrally pure regions as small as ~400 meters in size. Spectrally pure plagioclase is identified in approximately 450 targets located across the lunar surface. Diviner thermal infrared (TIR) data is analyzed for 37 of these nearly monomineralic regions in order to understand the compositional variability of plagioclase (An#) in these areas. The average Christiansen feature (CF) value for each spectrally pure region is estimated using new laboratory measurements of a well-characterized anorthite (An 96 ) sample. Diviner TIR results suggests that the plagioclase composition across the lunar highlands is relatively uniform, highly calcium (An ≥96 ), and consistent with plagioclase compositions found in the ferroan anorthosites (An 94-98 ). Our results confirm that spectrally pure anorthosite is widely distributed across the lunar surface and most exposures of the ancient anorthositic crust are concentrated in regions of thicker crust surrounding impact basins on the lunar near- and far-sides. In addition, the scale of the impact basins and the global nature and distribution of pure plagioclase requires a coherent zone of anorthosite of similar composition in the lunar crust supporting its formation from a single differentiation event involving a magma ocean. Our identifications of pure anorthosite combined with the GRAIL crustal thickness model suggest that pure anorthosite is currently observed at a range of crustal thickness values between 9 and 63 km and that the primary anorthositic crust must have been at least 30 km thick.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
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  • 6
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    Laboratory emissivity measurements of the plagioclase solid solution series under varying environmental conditions (2012)
    Wiley
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    Publication Date: 2012-11-08
    Description: New laboratory thermal infrared emissivity measurements of the plagioclase solid solution series over the 1700 ∼ 400 cm−1 (6–25 μm) spectral range are presented. Thermal infrared (TIR) spectral changes for fine-particulate samples (0–25 μm) are characterized for the first time under different laboratory environmental conditions: ambient (terrestrial-like), half-vacuum (Mars-like), vacuum, and vacuum with cooled chamber (lunar-like). Under all environmental conditions the Christiansen Feature (CF) is observed to vary in a systematic way with Na-rich end-member (albite) having a CF position at the highest wave number (shortest wavelength) and the Ca-rich end-member (anorthite) having a CF position with the lowest wave number (longest wavelength). As pressure decreases to 
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    Topics: Geosciences , Physics
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  • 7
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    Hydrated silicate minerals on Mars observed by the Mars Reconnaissance Orbiter CRISM instrument (2008)
    Nature Publishing Group (NPG)
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    Publication Date: 2008-07-18
    Description: Phyllosilicates, a class of hydrous mineral first definitively identified on Mars by the OMEGA (Observatoire pour la Mineralogie, L'Eau, les Glaces et l'Activitie) instrument, preserve a record of the interaction of water with rocks on Mars. Global mapping showed that phyllosilicates are widespread but are apparently restricted to ancient terrains and a relatively narrow range of mineralogy (Fe/Mg and Al smectite clays). This was interpreted to indicate that phyllosilicate formation occurred during the Noachian (the earliest geological era of Mars), and that the conditions necessary for phyllosilicate formation (moderate to high pH and high water activity) were specific to surface environments during the earliest era of Mars's history. Here we report results from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) of phyllosilicate-rich regions. We expand the diversity of phyllosilicate mineralogy with the identification of kaolinite, chlorite and illite or muscovite, and a new class of hydrated silicate (hydrated silica). We observe diverse Fe/Mg-OH phyllosilicates and find that smectites such as nontronite and saponite are the most common, but chlorites are also present in some locations. Stratigraphic relationships in the Nili Fossae region show olivine-rich materials overlying phyllosilicate-bearing units, indicating the cessation of aqueous alteration before emplacement of the olivine-bearing unit. Hundreds of detections of Fe/Mg phyllosilicate in rims, ejecta and central peaks of craters in the southern highland Noachian cratered terrain indicate excavation of altered crust from depth. We also find phyllosilicate in sedimentary deposits clearly laid by water. These results point to a rich diversity of Noachian environments conducive to habitability.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Mustard, John F -- Murchie, S L -- Pelkey, S M -- Ehlmann, B L -- Milliken, R E -- Grant, J A -- Bibring, J-P -- Poulet, F -- Bishop, J -- Dobrea, E Noe -- Roach, L -- Seelos, F -- Arvidson, R E -- Wiseman, S -- Green, R -- Hash, C -- Humm, D -- Malaret, E -- McGovern, J A -- Seelos, K -- Clancy, T -- Clark, R -- Marais, D D -- Izenberg, N -- Knudson, A -- Langevin, Y -- Martin, T -- McGuire, P -- Morris, R -- Robinson, M -- Roush, T -- Smith, M -- Swayze, G -- Taylor, H -- Titus, T -- Wolff, M -- England -- Nature. 2008 Jul 17;454(7202):305-9. doi: 10.1038/nature07097. Epub 2008 Jul 16.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geological Sciences, Brown University, Providence, Rhode Island 02912, USA. john_mustard@brown.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18633411" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
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  • 8
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    Phyllosilicate diversity and past aqueous activity revealed at Mawrth Vallis, Mars (2008)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2008-08-09
    Description: Observations by the Mars Reconnaissance Orbiter/Compact Reconnaissance Imaging Spectrometer for Mars in the Mawrth Vallis region show several phyllosilicate species, indicating a wide range of past aqueous activity. Iron/magnesium (Fe/Mg)-smectite is observed in light-toned outcrops that probably formed via aqueous alteration of basalt of the ancient cratered terrain. This unit is overlain by rocks rich in hydrated silica, montmorillonite, and kaolinite that may have formed via subsequent leaching of Fe and Mg through extended aqueous events or a change in aqueous chemistry. A spectral feature attributed to an Fe2+ phase is present in many locations in the Mawrth Vallis region at the transition from Fe/Mg-smectite to aluminum/silicon (Al/Si)-rich units. Fe2+-bearing materials in terrestrial sediments are typically associated with microorganisms or changes in pH or cations and could be explained here by hydrothermal activity. The stratigraphy of Fe/Mg-smectite overlain by a ferrous phase, hydrated silica, and then Al-phyllosilicates implies a complex aqueous history.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Bishop, Janice L -- Dobrea, Eldar Z Noe -- McKeown, Nancy K -- Parente, Mario -- Ehlmann, Bethany L -- Michalski, Joseph R -- Milliken, Ralph E -- Poulet, Francois -- Swayze, Gregg A -- Mustard, John F -- Murchie, Scott L -- Bibring, Jean-Pierre -- New York, N.Y. -- Science. 2008 Aug 8;321(5890):830-3. doi: 10.1126/science.1159699.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉SETI Institute and NASA Ames Research Center, Mountain View, CA 94043, USA. jbishop@seti.org〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18687963" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Iron/analysis ; Magnesium/analysis ; *Mars ; Silicates/*analysis ; 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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    Olivine and pyroxene diversity in the crust of Mars (2005)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2005-02-19
    Description: Data from the Observatoire pour la Mineralogie, l'Eau, les Glaces, et l'Activite (OMEGA) on the Mars Express spacecraft identify the distinct mafic, rock-forming minerals olivine, low-calcium pyroxene (LCP), and high-calcium pyroxene (HCP) on the surface of Mars. Olivine- and HCP-rich regions are found in deposits that span the age range of geologic units. However, LCP-rich regions are found only in the ancient Noachian-aged units, which suggests that melts for these deposits were derived from a mantle depleted in aluminum and calcium. Extended dark regions in the northern plains exhibit no evidence of strong mafic absorptions or absorptions due to hydrated materials.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Mustard, J F -- Poulet, F -- Gendrin, A -- Bibring, J-P -- Langevin, Y -- Gondet, B -- Mangold, N -- Bellucci, G -- Altieri, F -- New York, N.Y. -- Science. 2005 Mar 11;307(5715):1594-7. Epub 2005 Feb 17.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Geological Sciences, Brown University, Providence, RI 02912, USA. john_mustard@brown.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15718427" target="_blank"〉PubMed〈/a〉
    Keywords: Absorption ; Atmosphere ; Calcium ; Extraterrestrial Environment ; Geologic Sediments ; *Iron Compounds ; *Magnesium Compounds ; *Mars ; *Minerals ; *Silicates ; Spacecraft ; Spectroscopy, Near-Infrared ; Spectrum Analysis ; 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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  • 10
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    All about Mars (1993)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 1993-05-21
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Mustard, J F -- New York, N.Y. -- Science. 1993 May 21;260(5111):1174-5.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17806357" 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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