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  • 1
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    Uncertainties in the shock devolatilization of hydrated minerals: A nontronite case study (2013)
    Wiley
    Details
    Publication Date: 2013-09-20
    Description: [1]  Controlled recovery of hydrated minerals subjected to planar shock loading is challenging because of the large difference in shock impedance between the natural samples and the engineering materials used as the recovery capsules. Significant differences in recovery capsule design confound straightforward interpretation of existing data on shock modification of hydrated minerals. We present x-ray diffraction and infrared spectroscopy results from new shock recovery experiments experiments on nontronite (a smectite clay observed on Mars) and identify major issues in the interpretation of recovered samples. Previous work assumes that the first shock pressure step in a ring-up configuration is the most important factor in the interpretation of shock modification. By comparing the x-ray diffraction and infrared spectroscopy data from experiments with similar first shock steps but significantly different final shock states, we show that one cannot simply interpret the recovered samples based upon the first shock pressure step. This work demonstrates the need for a deeper understanding of the thermodynamics of ring-up experiments in order to be able to interpret the results in terms of an equivalent single shock loading pressure for planetary applications. In this work we also show that venting of the samples does not matter significantly at low pressures but may be important at high pressures. We have developed a recovery method and validation test that allows us to address the major issues and technical tradeoffs with shock recovery experiments on volatile materials.
    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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    The Stratigraphy and Evolution of Lower Mt. Sharp from Spectral, Morphological, and Thermophysical Orbital Datasets (2016)
    Wiley
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    Publication Date: 2016-09-01
    Description: We have developed a refined geologic map and stratigraphy for lower Mt. Sharp using coordinated analyses of new spectral, thermophysical, and morphologic orbital data products. The Mt. Sharp group consists of seven relatively planar units delineated by differences in texture, mineralogy, and thermophysical properties. These units are (1-3) three spatially adjacent units in the Murray formation which contain a variety of secondary phases and are distinguishable by thermal inertia and albedo differences, (4) a phyllosilicate-bearing unit, (5) a hematite-capped ridge unit, (6) a unit associated with material having a strongly sloped spectral signature at visible-near infrared wavelengths, and (7) a layered sulfate unit. The Siccar Point group consists of the Stimson formation and two additional units that unconformably overlie the Mt. Sharp group. All Siccar Point group units are distinguished by higher thermal inertia values and record a period of substantial deposition and exhumation that followed the deposition and exhumation of the Mt. Sharp group. Several spatially extensive silica deposits associated with veins and fractures show late stage silica enrichment within lower Mt. Sharp was pervasive. At least two laterally extensive hematitic deposits are present at different stratigraphic intervals, and both are geometrically conformable with lower Mt. Sharp strata. The occurrence of hematite at multiple stratigraphic horizons suggests redox interfaces were widespread in space and/or in time, and future measurements by the Mars Science Laboratory Curiosity rover will provide further insights into the depositional settings of these and other mineral phases.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 3
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    Columbus crater and other possible groundwater-fed paleolakes of Terra Sirenum, Mars (2011)
    Wiley
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    Publication Date: 2011-01-05
    Description: Columbus crater in the Terra Sirenum region of the Martian southern highlands contains light-toned layered deposits with interbedded sulfate and phyllosilicate minerals, a rare occurrence on Mars. Here we investigate in detail the morphology, thermophysical properties, mineralogy, and stratigraphy of these deposits; explore their regional context; and interpret the crater's aqueous history. Hydrated mineral-bearing deposits occupy a discrete ring around the walls of Columbus crater and are also exposed beneath younger materials, possibly lava flows, on its floor. Widespread minerals identified in the crater include gypsum, polyhydrated and monohydrated Mg/Fe-sulfates, and kaolinite; localized deposits consistent with montmorillonite, Fe/Mg-phyllosilicates, jarosite, alunite, and crystalline ferric oxide or hydroxide are also detected. Thermal emission spectra suggest abundances of these minerals in the tens of percent range. Other craters in northwest Terra Sirenum also contain layered deposits and Al/Fe/Mg-phyllosilicates, but sulfates have so far been found only in Columbus and Cross craters. The region's intercrater plains contain scattered exposures of Al-phyllosilicates and one isolated mound with opaline silica, in addition to more common Fe/Mg-phyllosilicates with chlorides. A Late Noachian age is estimated for the aqueous deposits in Columbus, coinciding with a period of inferred groundwater upwelling and evaporation, which (according to model results reported here) could have formed evaporites in Columbus and other craters in Terra Sirenum. Hypotheses for the origin of these deposits include groundwater cementation of crater-filling sediments and/or direct precipitation from subaerial springs or in a deep (∼900 m) paleolake. Especially under the deep lake scenario, which we prefer, chemical gradients in Columbus crater may have created a habitable environment at this location on early Mars.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 4
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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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  • 5
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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
    Published by American Association for the Advancement of Science (AAAS)
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  • 6
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    In situ radiometric and exposure age dating of the martian surface (2013)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2013-12-11
    Description: We determined radiogenic and cosmogenic noble gases in a mudstone on the floor of Gale Crater. A K-Ar age of 4.21 +/- 0.35 billion years represents a mixture of detrital and authigenic components and confirms the expected antiquity of rocks comprising the crater rim. Cosmic-ray-produced (3)He, (21)Ne, and (36)Ar yield concordant surface exposure ages of 78 +/- 30 million years. Surface exposure occurred mainly in the present geomorphic setting rather than during primary erosion and transport. Our observations are consistent with mudstone deposition shortly after the Gale impact or possibly in a later event of rapid erosion and deposition. The mudstone remained buried until recent exposure by wind-driven scarp retreat. Sedimentary rocks exposed by this mechanism may thus offer the best potential for organic biomarker preservation against destruction by cosmic radiation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Farley, K A -- Malespin, C -- Mahaffy, P -- Grotzinger, J P -- Vasconcelos, P M -- Milliken, R E -- Malin, M -- Edgett, K S -- Pavlov, A A -- Hurowitz, J A -- Grant, J A -- Miller, H B -- Arvidson, R -- Beegle, L -- Calef, F -- Conrad, P G -- Dietrich, W E -- Eigenbrode, J -- Gellert, R -- Gupta, S -- Hamilton, V -- Hassler, D M -- Lewis, K W -- McLennan, S M -- Ming, D -- Navarro-Gonzalez, R -- Schwenzer, S P -- Steele, A -- Stolper, E M -- Sumner, D Y -- Vaniman, D -- Vasavada, A -- Williford, K -- Wimmer-Schweingruber, R F -- MSL Science Team -- New York, N.Y. -- Science. 2014 Jan 24;343(6169):1247166. doi: 10.1126/science.1247166. Epub 2013 Dec 9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/24324273" target="_blank"〉PubMed〈/a〉
    Keywords: Biomarkers/analysis/chemistry ; *Cosmic Radiation ; *Evolution, Planetary ; *Exobiology ; Extraterrestrial Environment/*chemistry ; Geologic Sediments ; Isotopes/analysis/chemistry ; *Mars ; Noble Gases/*analysis ; Organic Chemicals/analysis/chemistry ; Radiation Dosage ; Radiometric Dating ; Surface Properties
    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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    Mineralogy of a mudstone at Yellowknife Bay, Gale crater, Mars (2013)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2013-12-11
    Description: Sedimentary rocks at Yellowknife Bay (Gale crater) on Mars include mudstone sampled by the Curiosity rover. The samples, John Klein and Cumberland, contain detrital basaltic minerals, calcium sulfates, iron oxide or hydroxides, iron sulfides, amorphous material, and trioctahedral smectites. The John Klein smectite has basal spacing of ~10 angstroms, indicating little interlayer hydration. The Cumberland smectite has basal spacing at both ~13.2 and ~10 angstroms. The larger spacing suggests a partially chloritized interlayer or interlayer magnesium or calcium facilitating H2O retention. Basaltic minerals in the mudstone are similar to those in nearby eolian deposits. However, the mudstone has far less Fe-forsterite, possibly lost with formation of smectite plus magnetite. Late Noachian/Early Hesperian or younger age indicates that clay mineral formation on Mars extended beyond Noachian time.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Vaniman, D T -- Bish, D L -- Ming, D W -- Bristow, T F -- Morris, R V -- Blake, D F -- Chipera, S J -- Morrison, S M -- Treiman, A H -- Rampe, E B -- Rice, M -- Achilles, C N -- Grotzinger, J P -- McLennan, S M -- Williams, J -- Bell, J F 3rd -- Newsom, H E -- Downs, R T -- Maurice, S -- Sarrazin, P -- Yen, A S -- Morookian, J M -- Farmer, J D -- Stack, K -- Milliken, R E -- Ehlmann, B L -- Sumner, D Y -- Berger, G -- Crisp, J A -- Hurowitz, J A -- Anderson, R -- Des Marais, D J -- Stolper, E M -- Edgett, K S -- Gupta, S -- Spanovich, N -- MSL Science Team -- New York, N.Y. -- Science. 2014 Jan 24;343(6169):1243480. doi: 10.1126/science.1243480. Epub 2013 Dec 9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Planetary Science Institute, Tucson, AZ 85719, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/24324271" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment/*chemistry ; Ferrosoferric Oxide/analysis/chemistry ; Geologic Sediments/analysis/*chemistry ; *Mars ; Minerals/analysis/*chemistry ; Silicates/analysis/chemistry ; Silicon Compounds/analysis/chemistry
    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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    Orbital identification of carbonate-bearing rocks on Mars (2008)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2008-12-20
    Description: Geochemical models for Mars predict carbonate formation during aqueous alteration. Carbonate-bearing rocks had not previously been detected on Mars' surface, but Mars Reconnaissance Orbiter mapping reveals a regional rock layer with near-infrared spectral characteristics that are consistent with the presence of magnesium carbonate in the Nili Fossae region. The carbonate is closely associated with both phyllosilicate-bearing and olivine-rich rock units and probably formed during the Noachian or early Hesperian era from the alteration of olivine by either hydrothermal fluids or near-surface water. The presence of carbonate as well as accompanying clays suggests that waters were neutral to alkaline at the time of its formation and that acidic weathering, proposed to be characteristic of Hesperian Mars, did not destroy these carbonates and thus did not dominate all aqueous environments.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Ehlmann, Bethany L -- Mustard, John F -- Murchie, Scott L -- Poulet, Francois -- Bishop, Janice L -- Brown, Adrian J -- Calvin, Wendy M -- Clark, Roger N -- Marais, David J Des -- Milliken, Ralph E -- Roach, Leah H -- Roush, Ted L -- Swayze, Gregg A -- Wray, James J -- New York, N.Y. -- Science. 2008 Dec 19;322(5909):1828-32. doi: 10.1126/science.1164759.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geological Sciences, Brown University, Providence, RI02912, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19095939" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Iron Compounds ; *Magnesium ; Magnesium Compounds ; *Mars ; Silicates ; Spacecraft ; 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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  • 9
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    Temporal and spatial variability of lunar hydration as observed by the Deep Impact spacecraft (2009)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2009-09-26
    Description: The Moon is generally anhydrous, yet the Deep Impact spacecraft found the entire surface to be hydrated during some portions of the day. Hydroxyl (OH) and water (H2O) absorptions in the near infrared were strongest near the North Pole and are consistent with 〈0.5 weight percent H2O. Hydration varied with temperature, rather than cumulative solar radiation, but no inherent absorptivity differences with composition were observed. However, comparisons between data collected 1 week (a quarter lunar day) apart show a dynamic process with diurnal changes in hydration that were greater for mare basalts (approximately 70%) than for highlands (approximately 50%). This hydration loss and return to a steady state occurred entirely between local morning and evening, requiring a ready daytime source of water-group ions, which is consistent with a solar wind origin.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sunshine, Jessica M -- Farnham, Tony L -- Feaga, Lori M -- Groussin, Olivier -- Merlin, Frederic -- Milliken, Ralph E -- A'Hearn, Michael F -- New York, N.Y. -- Science. 2009 Oct 23;326(5952):565-8. doi: 10.1126/science.1179788. Epub 2009 Sep 24.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉University of Maryland, College Park, MD 20742, USA. jess@astro.umd.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19779149" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; *Hydroxyl Radical ; *Moon ; Spacecraft ; Spectrum Analysis ; Sunlight ; Temperature ; Time Factors ; *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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    WATER AND CHLORINE CONTENT IN THE MARTIAN SOIL ALONG THE FIRST 1900 METERS OF THE CURIOSITY ROVER TRAVERSE AS ESTIMATED BY THE DAN INSTRUMENT (2014)
    Wiley
    Details
    Publication Date: 2014-06-22
    Description: The presence of hydrated phases in the soil and near-surface bedrock of Gale Crater is thought to be direct evidence for water-rock interaction in the crater in the ancient past. Layered sediments over the Gale Crater floor are thought to have formed in past epochs due to sediment transport, accumulation, and cementation through interaction with fluids, and the observed strata of water-bearing minerals record the history of these episodes. The first data analysis of the DAN investigation onboard the Curiosity rover is presented for 154 individual points of active mode measurements along 1900 meters of the traverse over the first 361 sols in Gale crater. It is found that a model of constant water content within subsurface should be rejected for practically all tested points, whereas a two-layer model with different water contents in each layer is supported by the data. A so-called direct two-layer model (water content increasing with depth) yields acceptable fits for odometry ranges between 0 – 455 meters and beyond 638 meters. The mean water (H 2 O) abundances of the top and bottom layers vary from 1.5 to 1.7 wt% and from 2.2 to 3.3 wt%, respectively, while at some tested spots the water content is estimated to be as high as ~5 wt%. The data for odometry range 455 – 638 meters support an inverse two-layer model (water content decreasing with depth), with an estimated mean water abundance of 2.1 ± 0.1 wt% and 1.4 ± 0.04 wt% in the top and bottom layers, respectively.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
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