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  • Inorganic Chemistry  (3,890)
  • Lunar and Planetary Science and Exploration  (3,706)
  • LUNAR AND PLANETARY EXPLORATION
  • Landwirtschaft
  • Tectonics
  • Temperatur
  • 2000-2004  (3,940)
  • 1930-1934
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Years
Year
  • 1
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    In:  Tectonophysics, London, Institution of Mining and Metallurgy, vol. 391, no. 1-4, pp. 97-108, pp. 1869, (ISBN: 0-12-018847-3)
    Publication Date: 2004
    Keywords: Reflection seismics ; Refraction seismics ; Greece ; Sea seismics ; Tectonics ; Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Fault zone ; Clement
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  • 2
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    In:  Bulletin of the Seismological Society of America, Amsterdam, Univ. Tokyo, vol. 94, no. 1, pp. 326-333, pp. 2152, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Earthquake ; Aftershocks ; Tectonics ; Seismology ; BSSA
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  • 3
    Publication Date: 2004
    Keywords: Geol. aspects ; Tectonics ; Plate tectonics ; Subduction zone ; South ; America ; TP ; Suarez ; Herail ; Regnier ; Cruz
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  • 4
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    In:  Tectonophys., Stuttgart, Pergamon, vol. 388, no. 5, pp. 21-31, pp. 1244, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Velocity depth profile ; Geothermics ; Physical properties of rocks ; Tectonics ; China ; rheology, ; seismicity, ; strength ; profile ; composition
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  • 5
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    In:  Bull. Seism. Soc. Am., San Francisco, Pergamon, vol. 94, no. 3, pp. 880-896, pp. 1121, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Seismology ; Tectonics ; Seismicity ; BSSA
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  • 6
    Publication Date: 2004
    Keywords: Stress ; Fault plane solution, focal mechanism ; Inversion ; Tectonics ; Switzerland ; JGR
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  • 7
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    In:  J. Struct. Geol., Bonn, Inst. f. Theoret. Geodäsie, vol. 26, no. 12, pp. 2203-2209, pp. B01401, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Stress ; Stress measurements ; topography ; Tectonics
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  • 8
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    Conseil de l'Europe
    In:  Cahiers du Centre Européen de Géodynamique et de Séismologie, Luxembourg, Conseil de l'Europe, vol. 23, no. B11, pp. 111-123, pp. 1892
    Publication Date: 2004
    Keywords: Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Geodesy ; Tectonics
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  • 9
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    In:  Bull. Seism. Soc. Am., Luxembourg, Am. Soc. Mech. Eng., vol. 94, no. 3, pp. 930-939, pp. L12311, (ISBN 0-471-26610-8)
    Publication Date: 2004
    Keywords: Seismicity ; Tectonics ; BSSA
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  • 10
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    In:  Tectonophysics, Charleston, South Carolina, California Division of Mines San Francisco, vol. 391, no. 1-4, pp. 67-83, pp. L23602, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Geol. aspects ; Structural geology ; Tectonics ; basin ; Strike-slip ; Greece ; Fault zone ; Ocakoglu ; Demirbag ; Kuscu ; Alacati ; Doganbey ; Kusadasi
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  • 11
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    In:  Tectonophysics, Kyoto, AGU, vol. 391, no. 1-4, pp. 259-282, pp. L24302, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Structural geology ; NAF ; Tectonics ; Geol. aspects ; Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Fault zone ; Tueysuez ; Tuysuz
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  • 12
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    In:  Nature, Naples, AGU, vol. 427, no. 6975, pp. 624-627, pp. 1273, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Plate tectonics ; Subduction zone ; Tectonics
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  • 13
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    In:  Tectonophysics, Tokyo, Lawrence Livermore National Laboratory, vol. 381, no. 1-4, pp. 175-209, pp. L11604, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Tectonics ; Subduction zone ; Geol. aspects ; EUROPROBE (Geol. and Geophys. in eastern Europe) ; Ustaoemer ; Ustaomer ; Yigitbas
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  • 14
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    In:  Tectonophysics, Würzburg, Pergamon, vol. 381, no. 1-4, pp. 1-4, pp. B05S01, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Geol. aspects ; Structural geology ; Tectonics ; Review article ; EUROPROBE (Geol. and Geophys. in eastern Europe)
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  • 15
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    In:  Tectonophysics, London, AGU, vol. 391, no. 1-4, pp. 35-65, pp. B12310, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Tectonics ; Geol. aspects ; Greece
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  • 16
    Publication Date: 2004
    Keywords: Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Geodesy ; Global Positioning System ; China ; Tectonics ; Buergmann ; Burgmann
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  • 17
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    Birkhäuser
    In:  Zürich, 256 pp., Birkhäuser, vol. 106, pp. 503, (ISBN 0521537436)
    Publication Date: 2004
    Keywords: GeodesyY ; Tectonics ; Plate tectonics ; Seismicity ; Earthquake hazard ; Martin ; Davila ; Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Global Positioning System ; Seismology ; Gravimetry, Gravitation ; Paleomagnetism ; Geodesy ; PAG ; Udias
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  • 18
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    In:  Bulletin of the Seismological Society of America, Taipei, Elsevier, vol. 94, no. 1, pp. 99-116, pp. L07301, (ISBN: 0-12-018847-3)
    Publication Date: 2004
    Keywords: Seismicity ; Tectonics ; BSSA
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  • 19
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    In:  Earth planet. Sci. Lett., London, 416 pp., Geological Society, vol. 221, no. 1-4, pp. 91-101, pp. L18607, (ISBN 1-86239-117-3)
    Publication Date: 2004
    Keywords: Tectonics ; Geodesy ; Structural geology ; uplift ; EPSL
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  • 20
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    In:  Geophysical Journal International, London, 416 pp., Geological Society, vol. 156, no. 3, pp. 655-681, pp. L18607, (ISBN 1-86239-117-3)
    Publication Date: 2004
    Keywords: Velocity depth profile ; Fault zone ; Middle ; East ; Tectonics ; Plate tectonics ; Reflection seismics ; GJI ; Foerster ; Forster ; Goetze ; Gotze ; Jaeckel ; Jackel ; Oberhaensli ; Oberhansli ; Ruempker ; Rumpker
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  • 21
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    In:  Geology, Tokyo, Terra Scientific Publishing Company, vol. 32, no. 7, pp. 577-580, pp. B03302, (ISBN: 0534351875, 2nd edition)
    Publication Date: 2004
    Keywords: Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Geodesy ; InSAR ; Tectonics ; silent ; slow ; red ; Earthquake
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  • 22
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    In:  Geophys. Res. Lett., Warszawa, Pergamon, vol. 31, no. 11, pp. 837-843, pp. L11614, (ISBN: 0534351875, 2nd edition)
    Publication Date: 2004
    Keywords: Stress ; Seismicity ; Seismology ; Tectonics ; GRL ; no ; given ; name ; for ; Kalpna ; ! ; 7209 ; Seismology: ; Earthquake ; dynamics ; and ; mechanics ; 7230 ; Seismicity ; and ; seismotectonics ; 8123 ; Tectonophysics: ; Dynamics, ; seismotectonics ; 8164 ; Stresses--crust ; and ; lithosphere ; Asia
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  • 23
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    In:  Tectonophysics, Berlin, Inst. Electrical & Electronics Engineers, vol. 391, no. 1-4, pp. 11-34, pp. B04307, (ISBN: 0534351875, 2nd edition)
    Publication Date: 2004
    Keywords: Geol. aspects ; Tectonics ; Plate tectonics
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  • 24
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    In:  J. Geophys. Res., Charleston, South Carolina, California Division of Mines San Francisco, vol. 109, no. B11, pp. 339-349, pp. B11306, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Seismicity ; Tectonics ; Geodesy ; NAF ; Fault zone ; 7215 ; Seismology: ; Earthquake ; parameters ; 7209 ; Earthquake ; dynamics ; and ; mechanics ; 7230 ; Seismicity ; and ; seismotectonics ; JGR ; 7223 ; Seismic ; hazard ; assessment ; and ; prediction
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  • 25
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    In:  Tectonophys., Dordrecht, 89, vol. 379, no. 1-4, pp. 159-181, pp. TC5003, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Geol. aspects ; China ; Tectonics ; kinematics ; Seismicity ; Tomography ; GeodesyY ; Modelling
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  • 26
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    In:  Geophysical Journal International, Washington, D.C., AGU, vol. 156, no. 3, pp. 506-526, pp. 8011, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Tectonics ; Fault plane solution, focal mechanism ; Seismology ; Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Seismicity ; GJI
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  • 27
    Publication Date: 2004
    Keywords: Three dimensional ; Strength ; EUROPROBE (Geol. and Geophys. in eastern Europe) ; Modelling ; Subduction zone ; Tectonics ; Romania ; Gravimetry, Gravitation ; EPSL
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  • 28
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    In:  Tectonophysics, Kunming, China, D. Reidel Publishing Company, vol. 391, no. 1-4, pp. 203-237, pp. L09303, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Tectonics ; Geol. aspects ; Plate tectonics ; EAFZ ; Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Fault zone
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  • 29
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    Columbia University Press
    In:  New York, 384 pp., Columbia University Press, vol. 7, no. XVI:, pp. 227-235, (ISBN 0231-12739-1 hb, 0231127383 pb)
    Publication Date: 2004
    Description: Consequences of Asthenospheric Variability in Continental Rifting, by W. Roger Buck; Velocity Fields, Faulting and Strength on the Continents, by James Jackson; Low-Angle Normal Fault Mechanics and Crustal Strength, by Gary J. Axen; Depth-Dependent Lithospheric Stretching at Rifted Continental Margins, by Mark Davis and Nick Kusznir Limits of the Seismogenic Zone, by Larry J. Ruff; Controls on Subduction Thrust Earthquakes: Downdip Changes in Composition and State, by R.D. Hyndman; Thermo-Mechanical Models of Convergent Orogenesis: Thermal and Rheologic Dependence of Crustal Deformation, by Sean D. Willett and Daniel C. Pope; Structure of Large-Displacement, Strike-Slip Fault Zones in the Brittle Continental Crust, by F.M. Chester, J.S. Chester, D.L. Kirschner, S.E. Schulz and J.P. Evans; The Strength of the San Andres Fault: A Discussion by Christopher H. Scholz and Thomas C. Hanks; Deformation Behavior of Partially Molten Mantle Rocks, by YaQin Xu, M.E. Zimmerman and D.L. Kohlstedt; Relations Among Porosity, Permeability, and Deformation in Rocks at High Temperatures, by Brian Evans, Yves Bernable and Greg Hirth --- title suggested by Tikoff: A review of seismogenic behavior in different plate tectonic settings (and some partially molten mantle deformation experiments)
    Keywords: Rheology ; Fault zone ; SAF ; Subduction zone ; Rock mechanics ; Stress ; Strength ; Plate tectonics ; Tectonics ; Seismicity ; Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Physical properties of rocks ; Handbook of geophysics ; Strike-slip ; Dip-slip ; thrust ; convergent ; transcurrent ; divergent ; GFZ ; M ; 04.0414, ; 000268617
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  • 30
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    In:  Sozialministerium Baden-Württemberg, Stuttgart
    Publication Date: 2004
    Description: mit einem zusätzlichen Berichtsteil zur Sterblichkeit unter Bewohnern von Pflegeheimen während der Hitzewelle im August 2003 in Baden-Württemberg vom Landesgesundheitsamt Baden-Württemberg KATASTER-BESCHREIBUNG: unter Berücksichtigung des „Harvesting- Effektes“ etwa 1100 (900-1300) Hitzeopfer KATASTER-DETAIL:
    Keywords: Baden-Württemberg ; 2003 ; Umweltmedizin ; Temperatur
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  • 31
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    In:  Bulletin of the Seismological Society of America, Naples, AGU, vol. 94, no. 1, pp. 341-348, pp. 1273, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Peak ground velocity ; Strong motions ; basin ; rifting ; Tectonics ; Site amplification ; Seismology ; BSSA
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  • 32
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    In:  Journal of Geodynamics, Prague, Wiley, vol. 38, no. 1, pp. 19-55, pp. B09404, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Tectonics ; Geol. aspects ; Subduction zone ; JGD
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  • 33
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    In:  Tectonophysics, New York, Scientific American, vol. 391, no. 1-4, pp. 171-201, pp. B11404, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Geol. aspects ; Tectonics ; Modelling ; Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Alasehir ; Gordes ; Goerdes
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  • 34
    Publication Date: 2004
    Keywords: Earthquake ; Tectonics ; Source parameters ; Fault zone ; GRL
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  • 35
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    In:  J. Geophys. Res., Dordrecht, American Society of Civil Engineers, vol. B11, no. 5, pp. 1144-1154, pp. B11406, (ISSN: 1340-4202)
    Publication Date: 2004
    Keywords: Tectonics ; Plate tectonics ; Subduction zone ; back-arc ; Greece ; Hellenic ; JGR ; FROTH
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  • 36
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    In:  Eos, Trans., Am. Geophys. Un., Oxford and Edinburgh, Blackwell Scientific Publications, vol. 85, no. 49, pp. 521 & 529, pp. 1484, (ISBN: 0534351875, 2nd edition)
    Publication Date: 2004
    Keywords: Stress ; software ; Plate tectonics ; Tectonics ; Earthquake hazard ; data ; base ; Fault plane solution, focal mechanism ; Borehole breakouts ; quality ; World Stress Map (Project) ; Muller ; Mueller
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  • 37
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    In:  Proceedings of the IWAM04, Mizunami, Japan, Lawrence Livermore National Laboratory, vol. 339-350, no. S3-09, 6 pp., pp. 344, (ISBN 3-933346-037)
    Publication Date: 2004
    Keywords: Tectonics ; Aegean, ; active ; faulting ; and ; monitoring, ; current ; plate ; interactions, ; Dead-Sea ; fault, ; earthquake ; source ; mechanisms ; earthquake ; potential ; and ; risk ; eastern ; Mediterranean ; region, ; InSAR, ; Sea ; of ; Marmara, ; North ; and ; East ; Anatolian ; Fault ; Zones, ; sea-bottom, ; seismology, ; seismotectonics, ; seismic ; hazard, ; Fault zone ; NAF ; Crustal deformation (cf. Earthquake precursor: deformation or strain) ; Geol. aspects ; Seismicity ; Turkey ; Earthquake hazard ; Source
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  • 38
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    In:  Other Sources
    Publication Date: 2011-08-24
    Description: How will humans and robots cooperate in future planetary exploration? Are humans and robots fundamentally separate modes of exploration, or can humans and robots work together to synergistically explore the solar system? It is proposed that humans and robots can work together in exploring the planets by use of telerobotic operation to expand the function and usefulness of human explorers, and to extend the range of human exploration to hostile environments. Published by Elsevier Ltd.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Acta astronautica (ISSN 0094-5765); Volume 55; 12; 985-90
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  • 39
    Publication Date: 2011-08-24
    Description: During the period from March 13, 2002 to mid-September, 2002, six solar particle events (SPE) were observed by the MARIE instrument onboard the Odyssey Spacecraft in Martian Orbit. These events were observed also by the GOES 8 satellite in Earth orbit, and thus represent the first time that the same SPE have been observed at these separate locations. The characteristics of these SPE are examined, given that the active regions of the solar disc from which the event originated can usually be identified. The dose rates at Martian orbit are calculated, both for the galactic and solar components of the ionizing particle radiation environment. The dose rates due to galactic cosmic rays (GCR) agree well with the HZETRN model calculations. Published by Elsevier Ltd on behalf of COSPAR.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Advances in space research : the official journal of the Committee on Space Research (COSPAR); Volume 33; 12; 2215-8
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  • 40
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    In:  Other Sources
    Publication Date: 2011-08-24
    Description: No abstract available
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 305; 5689; 1414-5
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  • 41
    Publication Date: 2011-08-24
    Description: Extraterrestrial organic matter may have been chemically altered into forms more ameanable for prebiotic chemistry in the wake of a meteor after ablation. We measured the rate of cooling of the plasma in the meteor wake from the intensity decay just behind a meteoroid by freezing its motion in high frame-rate 1000 frames/s video images, with an intensified camera that has a short phosphor decay time. Though the resulting cooling rate was found to be lower than theoretically predicted, our calculations indicated that there would have been insufficient collisions to break apart large organic compounds before most reactive radicals and electrons were lost from the air plasma. Organic molecules delivered from space to the early Earth via meteors might therefore have survived in a chemically altered form. In addition, we discovered that relatively small meteoroids generated far-ultraviolet emission that is absorbed in the immediate environment of the meteoroid, which may chemically alter the atmosphere over a much larger region than previously recognized.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Astrobiology (ISSN 1531-1074); Volume 4; 1; 95-108
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  • 42
    Publication Date: 2011-08-24
    Description: We detected hydrogen Balmer-alpha (H(alpha)) emission in the spectra of bright meteors and investigated its potential use as a tracer for exogenous delivery of organic matter. We found that it is critical to observe the meteors with high enough spatial resolution to distinguish the 656.46 nm H(alpha) emission from the 657.46 nm intercombination line of neutral calcium, which was bright in the meteor afterglow. The H(alpha) line peak stayed in constant ratio to the atmospheric emissions of nitrogen during descent of the meteoroid. If all of the hydrogen originates in the Earth's atmosphere, the hydrogen atoms are expected to have been excited at T = 4400 K. In that case, we measured an H(2)O abundance in excess of 150 +/- 20 ppm at 80-90 km altitude (assuming local thermodynamic equilibrium in the air plasma). This compares with an expected 〈20 ppm from H(2)O in the gas phase. Alternatively, meteoric refractory organic matter (and water bound in meteoroid minerals) could have caused the observed H(alpha) emission, but only if the line is excited in a hot T approximately 10000 K plasma component that is unique to meteoric ablation vapor emissions such as Si(+). Assuming that the Si(+) lines of the Leonid spectrum would need the same hot excitation conditions, and a typical [H]/[C] = 1 in cometary refractory organics, we calculated an abundance ratio [C]/[Si] = 3.9 +/- 1.4 for the dust of comet 55P/Tempel-Tuttle. This range agreed with the value of [C]/[Si] = 4.4 measured for comet 1P/Halley dust. Unless there is 10 times more water vapor in the upper atmosphere than expected, we conclude that a significant fraction of the hydrogen atoms in the observed meteor plasma originated in the meteoroid.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Astrobiology (ISSN 1531-1074); Volume 4; 1; 123-34
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  • 43
    Publication Date: 2011-08-24
    Description: The Composite Infrared Spectrometer observed Jupiter in the thermal infrared during the swing-by of the Cassini spacecraft. Results include the detection of two new stratospheric species, the methyl radical and diacetylene, gaseous species present in the north and south auroral infrared hot spots; determination of the variations with latitude of acetylene and ethane, the latter a tracer of atmospheric motion; observations of unexpected spatial distributions of carbon dioxide and hydrogen cyanide, both considered to be products of comet Shoemaker-Levy 9 impacts; characterization of the morphology of the auroral infrared hot spot acetylene emission; and a new evaluation of the energetics of the northern auroral infrared hot spot.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 305; 5690; 1582-6
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  • 44
    Publication Date: 2011-08-24
    Description: Thermal infrared spectra of the martian atmosphere taken by the Miniature Thermal Emission Spectrometer (Mini-TES) were used to determine the atmospheric temperatures in the planetary boundary layer and the column-integrated optical depth of aerosols. Mini-TES observations show the diurnal variation of the martian boundary layer thermal structure, including a near-surface superadiabatic layer during the afternoon and an inversion layer at night. Upward-looking Mini-TES observations show warm and cool parcels of air moving through the Mini-TES field of view on a time scale of 30 seconds. The retrieved dust optical depth shows a downward trend at both sites.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 306; 5702; 1750-3
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  • 45
    Publication Date: 2011-08-24
    Description: The 2001 Mars Odyssey spacecraft was launched towards Mars on April 7, 2001. Onboard the spacecraft is the Martian radiation environment experiment (MARIE), which is designed to measure the background radiation environment due to galactic cosmic rays (GCR) and solar protons in the 20-500 MeV/n energy range. We present an approach for developing a space radiation-shielding model of the spacecraft that includes the MARIE instrument in the current mapping phase orientation. A discussion is presented describing the development and methodology used to construct the shielding model. For a given GCR model environment, using the current MARIE shielding model and the high-energy particle transport codes, dose rate values are compared with MARIE measurements during the early mapping phase in Mars orbit. The results show good agreement between the model calculations and the MARIE measurements as presented for the March 2002 dataset. c2003 COSPAR. Published by Elsevier Ltd. All rights reserved.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Advances in space research : the official journal of the Committee on Space Research (COSPAR); Volume 33; 12; 2219-21
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  • 46
    Publication Date: 2011-08-24
    Description: Space radiation presents a hazard to astronauts, particularly those journeying outside the protective influence of the geomagnetosphere. Crews on future missions to Mars will be exposed to the harsh radiation environment of deep space during the transit between Earth and Mars. Once on Mars, they will encounter radiation that is only slightly reduced, compared to free space, by the thin Martian atmosphere. NASA is obliged to minimize, where possible, the radiation exposures received by astronauts. Thus, as a precursor to eventual human exploration, it is necessary to measure the Martian radiation environment in detail. The MARIE experiment, aboard the 2001 Mars Odyssey spacecraft, is returning the first data that bear directly on this problem. Here we provide an overview of the experiment, including introductory material on space radiation and radiation dosimetry, a description of the detector, model predictions of the radiation environment at Mars, and preliminary dose-rate data obtained at Mars. c2003 COSPAR. Published by Elsevier Ltd. All rights reserved.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Advances in space research : the official journal of the Committee on Space Research (COSPAR); Volume 33; 12; 2204-10
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  • 47
    Publication Date: 2011-08-24
    Description: Discussions of future human expeditions into the solar system generally focus on whether the next explorers ought to go to the Moon or to Mars. The only mission scenario developed in any detail within NASA is an expedition to Mars with a 500-day stay at the surface. The technological capabilities and the operational experience base required for such a mission do not now exist nor has any self-consistent program plan been proposed to acquire them. In particular, the lack of an Abort-to-Earth capability implies that critical mission systems must perform reliably for 3 years or must be maintainable and repairable by the crew. As has been previously argued, a well-planned program of human exploration of the Moon would provide a context within which to develop the appropriate technologies because a lunar expedition incorporates many of the operational elements of a Mars expedition. Initial lunar expeditions can be carried out at scales consistent with the current experience base but can be expanded in any or all operational phases to produce an experience base necessary to successfully and safely conduct human exploration of Mars. Published by Elsevier Ltd.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Acta astronautica (ISSN 0094-5765); Volume 55; 3-9; 773-80
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  • 48
    Publication Date: 2011-08-24
    Description: Mission scenarios outside the Earth's protective magnetic shield are being studied. Included are high usage assets in the near-Earth environment for casual trips, for research, and for commercial/operational platforms, in which career exposures will be multi-mission determined over the astronaut's lifetime. The operational platforms will serve as launching points for deep space exploration missions, characterized by a single long-duration mission during the astronaut's career. The exploration beyond these operational platforms will include missions to planets, asteroids, and planetary satellites. The interplanetary environment is evaluated using convective diffusion theory. Local environments for each celestial body are modeled by using results from the most recent targeted spacecraft, and integrated into the design environments. Design scenarios are then evaluated for these missions. The underlying assumptions in arriving at the model environments and their impact on mission exposures within various shield materials will be discussed. Published by Elsevier Ltd on behalf of COSPAR.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Advances in space research : the official journal of the Committee on Space Research (COSPAR); Volume 34; 6; 1281-7
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  • 49
    Publication Date: 2011-08-24
    Description: Meteoroids that dominate the Earth's extraterrestrial mass influx (50-300 microm size range) may have contributed a unique blend of exogenous organic molecules at the time of the origin of life. Such meteoroids are so large that most of their mass is ablated in the Earth's atmosphere. In the process, organic molecules are decomposed and chemically altered to molecules differently from those delivered to the Earth's surface by smaller (〈50 microm) micrometeorites and larger (〉10 cm) meteorites. The question addressed here is whether the organic matter in these meteoroids is fully decomposed into atoms or diatomic compounds during ablation. If not, then the ablation products made available for prebiotic organic chemistry, and perhaps early biology, might have retained some memory of their astrophysical nature. To test this hypothesis we searched for CN emission in meteor spectra in an airborne experiment during the 2001 Leonid meteor storm. We found that the meteor's light-emitting air plasma, which included products of meteor ablation, contained less than 1 CN molecule for every 30 meteoric iron atoms. This contrasts sharply with the nitrogen/iron ratio of 1:1.2 in the solid matter of comet 1P/Halley. Unless the nitrogen content or the abundance of complex organic matter in the Leonid parent body, comet 55P/Tempel-Tuttle, differs from that in comet 1P/Halley, it appears that very little of that organic nitrogen decomposes into CN molecules during meteor ablation in the rarefied flow conditions that characterize the atmospheric entry of meteoroids approximately 50 microm-10 cm in size. We propose that the organics of such meteoroids survive instead as larger compounds.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Astrobiology (ISSN 1531-1074); Volume 4; 1; 67-79
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  • 50
    Publication Date: 2011-08-24
    Description: The speed and mass dependence of meteor air plasma temperatures is perhaps the most important data needed to understand how small meteoroids chemically change the ambient atmosphere in their path and enrich the ablated meteoric organic matter with oxygen. Such chemistry can play an important role in creating prebiotic compounds. The excitation conditions in various air plasma emissions were measured from high-resolution optical spectra of Leonid storm meteors during NASA's Leonid Multi-Instrument Aircraft Campaign. This was the first time a sufficient number and range of temperature measurements were obtained to search for meteoroid mass and speed dependencies. We found slight increases in temperature with decreasing altitude, but otherwise nearly constant values for meteoroids with speeds between 35 and 72 km/s and masses between 10(-5) g and 1 g. We conclude that faster and more massive meteoroids produce a larger emission volume, but not a higher air plasma temperature. We speculate that the meteoric plasma may be in multiphase equilibrium with the ambient atmosphere, which could mean lower plasma temperatures in a CO(2)-rich early Earth atmosphere.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Astrobiology (ISSN 1531-1074); Volume 4; 1; 81-94
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  • 51
    Publication Date: 2011-08-24
    Description: We report the discovery of the N(2)(+) A-X Meinel band in the 780-840 nm meteor emission from two Leonid meteoroids that were ejected less than 1000 years ago by comet 55P/Tempel-Tuttle. Our analysis indicates that the N(2)(+) molecule is at least an order of magnitude less abundant than expected, possibly as a result of charge transfer reactions with meteoric metal atoms. This new band was found while searching for rovibrational transitions in the X(2)Pi electronic ground state of OH (the OH Meinel band), a potential tracer of water bound to minerals in cometary matter. The electronic A-X transition of OH has been identified in other Leonid meteors. We did not detect this OH Meinel band, which implies that the excited A state is not populated by thermal excitation but by a mechanism that directly produces OH in low vibrational levels of the excited A(2)Sigma state. Ultraviolet dissociation of atmospheric or meteoric water vapor is such a mechanism, as is the possible combustion of meteoric organics.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Astrobiology (ISSN 1531-1074); Volume 4; 1; 109-21
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  • 52
    Publication Date: 2011-08-24
    Description: The results of a study of the ion-molecule reactions of N(+), N(2)(+), and HCN(+) with methane, acetylene, and ethylene are reported. These studies were performed using the FA-SIFT at the University of Canterbury. The reactions studied here are important to understanding the ion chemistry in Titan's atmosphere. N(+) and N(2)(+) are the primary ions formed by photo-ionization and electron impact in Titan's ionosphere and drive Titan's ion chemistry. It is therefore very important to know how these ions react with the principal trace neutral species in Titan's atmosphere: Methane, acetylene, and ethylene. While these reactions have been studied before the product channels have been difficult to define as several potential isobaric products make a definitive answer difficult. Mass overlap causes difficulties in making unambiguous species assignments in these systems. Two discriminators have been used in this study to resolve the mass overlap problem. They are deuterium labeling and also the differences in reactivities of each isobar with various neutral reactants. Several differences have been found from the products in previous work. The HCN(+) ion is important in both Titan's atmosphere and in the laboratory.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Journal of the American Society for Mass Spectrometry (ISSN 1044-0305); Volume 15; 8; 1148-55
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  • 53
    Publication Date: 2004-10-05
    Description: The space environment above the icy surface of Europa is a source of radio noise in this frequency range from natural sources in the Jovian magnetosphere. The ionospheric and magnetospheric plasma environment of Europa affects propagation of transmitted and return signals between the spacecraft and the solid surface in a frequency-dependent manner. The ultimate resolution of the subsurface sounding measurements will be determined, in part, by a capability to mitigate these effects. We discuss an integrated multi-frequency approach to active radio sounding of the Europa ionospheric and local magnetospheric environments, based on operational experience from the Radio Plasma Imaging @PI) experiment on the IMAGE spacecraft in Earth orbit, in support of the subsurface measurement objectives.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Europa's Icy Shell: Past, Present, and Future; 48; LPI-Contrib-1195
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  • 54
    Publication Date: 2004-10-05
    Description: We use several independent constraints on the number of ecliptic comets to estimate impact cratering rates on the Jupiter moons. The impact rate on Jupiter by 1.5-km diameter ecliptic comets is currently NY(d 〉 1.5km) = 0.005(+0.006)(-0.003) per annum. Asteroids and long period comets are currently unimportant. The size-number distribution of ecliptic comets smaller than 20 km is inferred from size-number distributions of impact craters on Europa, Ganymede, and Triton. For comets bigger than 50 km we use the size-number distribution of Kuiper Belt Objects. The overview of the impact rate at Jupiter in general and at Europa in particular are given. These impact rates imply cratering rates on Europa of 0.5 per Ma per 10(exp 6) sq km for impact craters bigger than 1 km, and of 0.015 per Ma per 10(exp 6) sq km for impact craters bigger than 20 km. The latter corresponds to an average recurrence time of 2.2 Ma for 20 km craters. The best current estimates for the number of 20 km craters on Europa appear to range between about twelve to thirty. This implies that the average age of Europa's surface is between 30 and 70 Ma. The average density of craters with diameter greater than 1 km on well-mapped swaths on Europa is 30 per 10(exp 6) sq km. The corresponding nominal surface age would be 60 Ma. These two estimates are not truly independent because we have used size-number distribution of the Europan craters to help generate the size-number distribution of comets. The uncertainty of the best estimate - call it 42 Ma for specificity - is at least a factor of 3.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Europa's Icy Shell: Past, Present, and Future; 98-99; LPI-Contrib-1195
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  • 55
    Publication Date: 2011-08-24
    Description: The charged particle spectrum for nuclei from protons to neon, (charge Z=10) was observed during the cruise phase and orbit around Mars by the MARIE charged particle spectrometer on the Odyssey spacecraft. The cruise data were taken between April 23, 2001 and mid-August 2001. The Mars orbit data were taken March 5, 2002 through May 2002 and are scheduled to continue until August 2004. Charge peaks are clearly separated for charges up to Z=10. Especially prominent are the carbon and oxygen peaks, with boron and nitrogen also clearly visible. Although heavy ions are much less abundant than protons in the cosmic ray environment, it is important to determine their abundances because their ionization energy losses (proportional to Z2) are far more dangerous to humans and to instruments. Thus the higher charged nuclei make a significant contribution to dose and dose equivalent received in space. Results of the charged particle spectrum measurements will be reported. c2003 COSPAR. Published by Elsevier Ltd. All rights reserved.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Advances in space research : the official journal of the Committee on Space Research (COSPAR); Volume 33; 12; 2211-4
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  • 56
    Publication Date: 2011-08-24
    Description: We interpret the nucleus properties and jet activity from the Stardust spacecraft imaging and the onboard dust monitoring system data. Triangulation of 20 jets shows that 2 emanate from the nucleus dark side and 16 emanate from sources that are on slopes where the Sun's elevation is greater than predicted from the fitted triaxial ellipsoid. Seven sources, including five in the Mayo depression, coincide with relatively bright surface spots. Fitting the imaged jets, the spikelike temporal distribution of dust impacts indicates that the spacecraft crossed thin, densely populated sheets of particulate ejecta extending from small sources on the rotating nucleus, consistent with an emission cone model.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 304; 5678; 1769-74
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  • 57
    facet.materialart.
    Unknown
    In:  CASI
    Publication Date: 2013-08-31
    Description: This special bibliography includes the extraction, processing, and utilization of lunar, planetary, and asteroid resources; mining and excavation equipment, oxygen and propellant production; and in situ resource utilization.
    Keywords: Lunar and Planetary Science and Exploration
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  • 58
    facet.materialart.
    Unknown
    In:  CASI
    Publication Date: 2013-08-31
    Description: This custom bibliography from the NASA Scientific and Technical Information Program lists a sampling of records found in the NASA Aeronautics and Space Database. The scope of this topic includes technologies for ultimately enabling us to "cut the cord" with Earth for space logistics. This area of focus is one of the enabling technologies as defined by NASA s Report of the President s Commission on Implementation of United States Space Exploration Policy, published in June 2004.
    Keywords: Lunar and Planetary Science and Exploration
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  • 59
    Publication Date: 2013-08-31
    Description: Knowledge of the trapping mechanisms and diffusion characteristics of solar-wind implanted isotopes in the minerals of the lunar regolith will enable the optimization of the processes to extract solar wind gases from regolith particles. Extraction parameters include the temperature and duration of extraction, particle size, and gas yield. Diffusion data will increase the efficiency and profitability of future mining ventures. This data will also assist in optimizing the evaluations of various potential mining sites based on remote sensing data. For instance, if magnesian ilmenite (Mg,Fel.,Ti03) is found to retain He better than stoichiometric ilmenite (FeTi03), remote sensing data for Mg could be considered in addition to Ti and maturity data. The context of the currently discussed work is the mining of helium-3 for potential use as a fuel for fusion energy generation. However, the potential resources deposited by the solar wind include hydrogen (and derived water), helium-4, nitrogen and carbon. Implantation experiments such as those performed for helium isotopes in ilmenite are important for the optimized extraction of these additional resources. These experiments can easily be reproduced for most elements or isotopes of interest.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Space Resources Roundtable VI; 28; LPI-Contrib-1224
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  • 60
    Publication Date: 2013-08-31
    Description: The Mars Global Surveyor spacecraft has completed two Mars years in nearly circular polar orbit at a nominal altitude of 400 km. The Mars crust is at least an order of magnitude more intensely magnetized than that of the Earth, and intriguing in both its global distribution and geometric properties. Measurements of the vector magnetic field have been used to map the magnetic field of crustal origin to high accuracy. This most recent map is assembled from 〉 2 full years of MGS night-side observations, and uses along-track filtering to greatly reduce noise due to external field variations. Additional information is included in the original extended abstract.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Hemispheres Apart: The Origin and Modification of The Martian Crustal Dichotomy; 11-12; LPI-Contrib-1213
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  • 61
    Publication Date: 2013-08-31
    Description: The Martian dichotomy divides the smooth, northern lowlands from the rougher southern highlands. The northern lowlands are largely free of magnetic anomalies, while the majority of the significant magnetic anomalies are located in the southern highlands. An elevation change of 2-4 km is typical across the dichotomy, and is up to 6 km locally. We examine a part of the dichotomy that is likely to preserve the early history of the dichotomy as it is relatively unaffected by major impacts and erosion. This study contains three parts: 1) the geologic history, which is summarized below and detailed in McGill et al., 2) the study of the gravity and magnetic field to better constrain the subsurface structure and history of the magnetic field (this abstract), and 3) modeling of the relaxation of this area. Our overall goal is to place constraints on formation models of the dichotomy by constraining lithospheric properties. Initial results for the analysis of the geology, gravity, and magnetic field studies are synthesized in Smrekar et al..
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Hemispheres Apart: The Origin and Modification of The Martian Crustal Dichotomy; 60-61; LPI-Contrib-1213
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  • 62
    Publication Date: 2013-08-31
    Description: Linear negative gravity anomalies in Acidalia Planitia along the eastern edge of Tempe Terra and along the northern edge of Arabia Terra have been noted in Mars Global Surveyor gravity fields. Once proposed to represent buried fluvial channels, it is now believed that these gravity troughs mainly arise from partial compensation of the hemispheric dichotomy topographic scarp. A recent inversion for crustal structure finds that mantle compensation of the scarp is offset from the present-day topographic expression of the dichotomy boundary. The offset suggests that erosion or other forms of mass wasting occurred after lithosphere thickened and no longer accomodated topographic change through viscous relaxation.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Hemispheres Apart: The Origin and Modification of The Martian Crustal Dichotomy; 46-47; LPI-Contrib-1213
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  • 63
    Publication Date: 2013-08-31
    Description: MOLA data have revealed a large population of "Quasi-Circular Depressions" (QCDs) with little or no visible expression in image data. These likely buried impact basins have important implications for the age of the lowland crust, how that compares with original highland crust, and when and how the crustal dichotomy may have formed. The buried lowlands are of Early Noachian age, likely slightly younger than the buried highlands but older than the exposed (visible) highland surface. A depopulation of large visible basins at diameters 800 to 1300 km suggests some global scale event early in martian history, maybe related to the formation of the lowlands andor the development of Tharsis. A suggested early disappearance of the global magnetic field can be placed within a temporal sequence of formation of the very largest impact basins. The global field appears to have disappeared at about the time the lowlands formed. It seems likely the topographic crustal dichotomy was produced very early in martian history by processes which operated very quickly. This and the preservation of large relic impact basins in the north- em hemisphere, which themselves can account for the lowland topography, suggest that large impacts played the major role in the origin Mars fundamental crustal feature.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Hemispheres Apart: The Origin and Modification of The Martian Crustal Dichotomy; 19-20; LPI-Contrib-1213
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  • 64
    Publication Date: 2013-08-31
    Description: The Martian dichotomy is a global feature separating the northern and southern hemispheres. The 3.5 - 4 Gyr old feature is manifested by a topographic difference of 2-6 km and crustal thickness difference of approx. 15 - 30 km between the two hemispheres. In the Ismenius region, sections of the boundary are characterized by a single scarp with a slope of approx. 20 deg. - 23 deg. and are believed to be among the most well preserved parts of the dichotomy boundary. The origin of the dichotomy is unknown. Endogenic hypotheses do not predict the steep slopes (scarps) of the dichotomy boundary. Exogenic models for forming the northern lowlands by impact cratering, associate the scarps along the dichotomy boundary with craters' rims, but are not globally consistent with the topography and gravity. In order to better understand the origin of the Martian dichotomy, it is necessary to know if the steep scarps along the boundary represent the original shape of the dichotomy. Smrekar et al. presented evidence showing that the boundary scarp in Ismenius is a fault along which the highland crust was down faulted. We test whether the relaxation process could produce faulting along the dichotomy boundary and examine the crustal and mantle conditions that would allow for faulting to occur within 1 Gyr and preserve the long wavelength topography over another 3 Gyr. We approach the problem by a combination of numerical and semi-analytical modeling. We test different viscosity profiles and crustal thicknesses by comparing our modeled magnitude, location and timing of plastic strain and displacements to detailed geologic observations in the Ismenius region.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Hemispheres Apart: The Origin and Modification of The Martian Crustal Dichotomy; 21-22; LPI-Contrib-1213
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  • 65
    Publication Date: 2013-08-31
    Description: Despite research by numerous geologists and geo- physicists, the age and origin of the martian crustal dichotomy remain uncertain. Models for the origin of this dichotomy involve single or multiple impact, mantle megaplumes, primordial crustal asymmetry, and plate tectonics. Most of these models imply a Noachian age for the dichotomy. A major problem common to all genetic models is the difficulty separating the features resulting from the primary cause for the dichotomy from features due to younger fault- ing, impact cratering, volcanism, deposition, and erosion. highlands (the dichotomy boundary) approximates a small circle that ranges in latitude from about -10 deg. in Elysium Planitia to about +45 deg. north of Arabia Terra. For much of its length the boundary is characterized by relatively steep scarps separating highland plateau to the south from lowland plains to the north, generally with a complex transition zone on the lowland side of these scarps. These scarps are almost certainly due to normal faulting. The type fretted terrain, which defines the boundary in north-central Arabia Terra, also is characterized by scarps but has under- gone a more complex history of faulting and dissection [13]. In some places, notably in the Acidalia Planitia region, the dichotomy boundary is gradational. In the Tharsis region the boundary is obscured by younger volcanics.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Hemispheres Apart: The Origin and Modification of The Martian Crustal Dichotomy; 42-43; LPI-Contrib-1213
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  • 66
    Publication Date: 2017-10-02
    Description: High-resolution topographic data from the Mars Orbiter Laser Altimeter (MOLA), and imagery from the Mars Orbiter Camera (MOC) and the Thermal Emission Imaging System (THEMIS) allow for the first accurate assessment of lava flow directions relative to topographic slopes in the Tharsis region. Tharisis has long been recognized as the dominant tectonic and volcanic province on the planet, with a complex geologic history. In this study, lava flow directions on Daedalia Planum, Syria Planum, Tempe Terra, and near the Tharsis Montes are compared with MOLA topographic contours to look for deviations of flow directions from the local slope direction. The topographic deviations identified in this study are likely due to Tharsis tectonic deformation that has modified the regional topography subsequent to the emplacement of the flows, and can be used to model the mechanisms and magnitudes of relatively recent tectonism in the region. A similar approach was used to identify possible post-flow tectonic subsidence on the Snake River Plain in Idaho.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life; LPI-Contrib-1211
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  • 67
    Publication Date: 2017-10-02
    Description: Tumbleweed is a wind-propelled long-range vehicle based on well-developed and tested technology, instrumented to perform surveys Mars analog environments for habitability and suitable for a variety of missions on Mars. Tumbleweeds are light-weight and relatively inexpensive, making it very attractive for multiple deployments or piggy-backing on a larger mission. Tumbleweeds with rigid structures are also being developed for similar applications. Modeling and testing have shown that a 6 meter diameter Tumbleweed is capable of climbing 25 hills, traveling over 1 meter diameter boulders, and ranging over a thousand kilometers. Tumbleweeds have a potential payload capability of about 10 kilograms with approximately 10-20 Watts of power. Stopping for science investigations can also be accomplished using partial deflation or other braking mechanisms. Surveys for Astrobiology and other applications of tumbleweeds are shown.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life; LPI-Contrib-1211
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  • 68
    Publication Date: 2017-10-02
    Description: A climatic optimum? The often strong contrast between the pristine and degraded Noachian channels and craters might be due to a gradual climatic change superimposed upon an episode of mantling associated with early Hesperian volcanism. On the other hand, one or more episodes of volcanism or large impacts could have induced global warming and produced a relatively short-lived optimum for precipitation and runoff. The rapid cutoff of fluvial activity following the development of the later pristine fluvial features is consistent with this scenario. We discuss the changing style of erosion in the highlands during the Noachian and early Hesperian in a companion abstract to this workshop. Here we review the some of the morphologic evidence for a possible Noachian-Hesperian (N-H) climate optimum.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life; LPI-Contrib-1211
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  • 69
    Publication Date: 2017-10-02
    Description: The first images returned by the Mariner 7 spacecraft of the Martian surface showed a landscape heavily scared by impacts. Mariner 9 imaging revealed geomorphic features including valley networks and outflow channels that suggest liquid water once flowed at the surface of Mars. Further evidence for water erosion and surface modification has come from the Viking Spacecraft, Mars Pathfinder, Mars Global Surveyor's (MGS) Mars Orbiter Camera (MOC), and Mars Odyssey's THEMIS instrument. In addition to network channels, this evidence includes apparent paleolake beds, fluvial fans and sedimentary layers. The estimated erosion rates necessary to explain the observed surface morphologies present a conundrum. The rates of erosion appear to be highest when the early sun was fainter and only 75% as luminous as it is today. All of this evidence points to a very different climate than what exists on Mars today. The most popular paradigm for the formation of the valley networks is that Mars had at one time a warm (T average 〉 273), wetter and stable climate. Possible warming mechanisms have included increased surface pressures, carbon dioxide clouds and trace greenhouse gasses. Yet to date climate models have not been able to produce a continuously warm and wet early Mars. The rates of erosion appear to correlate with the rate at which Mars was impacted thus an alternate possibility is transient warm and wet conditions initiated by large impacts. It is widely accepted that even relatively small impacts (approx. 10 km) have altered the past climate of Earth to such an extent as to cause mass extinctions. Mars has been impacted with a similar distribution of objects. The impact record at Mars is preserved in the abundance of observable craters on it surface. Impact induced climate change must have occurred on Mars.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life; LPI-Contrib-1211
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  • 70
    Publication Date: 2017-10-02
    Description: Previous in-situ measurements of soil-like materials on the surface of Mars, in particular during the on-going Mars Exploration Rover missions, have shown complex relationships between composition, exposure to the surface environment, texture, and local rocks. In particular, a diversity in both compositional and physical properties could be established that is interpreted to be diagnostic of the complex geologic history of the martian surface layer. Physical and chemical properties vary laterally and vertically, providing insight into the composition of rocks from which soils derive, and environmental conditions that led to soil formation. They are central to understanding whether habitable environments existed on Mars in the distant past. An instrument the Mole for Soil Compositional Studies and Sampling (MOCSS) - is proposed to allow repeated access to subsurface regolith on Mars to depths of up to 1.5 meters for in-situ measurements of elemental composition and of physical and thermophysical properties, as well as for subsurface sample acquisition. MOCSS is based on the compact PLUTO (PLanetary Underground TOol) Mole system developed for the Beagle 2 lander and incorporates a small X-ray fluorescence spectrometer within the Mole which is a new development. Overall MOCSS mass is approximately 1.4 kilograms. Taken together, the MOCSS science data support to decipher the geologic history at the landing site as compositional and textural stratigraphy if they exist - can be detected at a number of places if the MOCSS were accommodated on a rover such as MSL. Based on uncovered stratigraphy, the regional sequence of depositional and erosional styles can be constrained which has an impact on understanding the ancient history of the Martian near-surface layer, considering estimates of Mars soil production rates of 0.5... 1.0 meters per billion years on the one hand and Mole subsurface access capability of approximately 1.5 meters. An overview of the MOCSS, XRS instrument accomodation and the impact that these instruments have on Mars science is discussed.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life; LPI-Contrib-1211
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  • 71
    Publication Date: 2017-10-02
    Description: Aqueous environments on early Mars were probably relatively short-lived and localized, as evidenced by the lack of abundant secondary minerals detected by the TES instrument. In order to better understand the aqueous history of early Mars we need to be able to interpret the evidence preserved in secondary minerals formed during these aqueous events. Carbonate minerals, in particular, are important secondary minerals for interpreting past aqueous environments as illustrated by the carbonates preserved in ALH84001. Carbonates formed in short-lived, dynamic aqueous events often preserve kinetic rather than equilibrium chemical and isotopic processes, and predicting the behavior of such systems is facilitated by empirical data.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life; LPI-Contrib-1211
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  • 72
    Publication Date: 2017-10-02
    Description: Hesperian and Amazonian plains units cover the northern lowlands but little is known about what this surface covers. Models for the creation of the lowlands and the dichotomy boundary implement mechanisms which vary from internal processes, such as plate tectonics or first-order mantle convection, to external processes, such as a single large impact or multiple impacts. Different models require different time scales for low-land formation; determining the age of the buried low-land surface would help constrain the formation models. The Mars Orbiting Laser Altimeter (MOLA) has yielded a high-precision, topographic gridded data set that reveals the presence of Quasi-Circular Depressions (QCDs) in both the southern highlands and the northern lowlands. Most of these roughly circular depressions have no corresponding visible structural feature on the surface. It is proposed that these QCDs are the surface representation of buried impact craters. Based on this assumption, cumulative number vs. diameter curves were constructed, which placed the age of the buried surface of the northern lowlands in the Early or pre-Noachian. A Noachian basement is supported by the remnants of large craters and multi-ring basins discovered in earlier research, but the QCDs provide the first evidence of this for the entire lowland. Constraining the age of the basement floor to the earliest Noachian, however, would require that the process that formed the northern lowlands either occurred in the early Noachian or involves removal of material from the bottom of the crust without destroying the previously formed craters to achieve the modeled crustal thinning. But can we establish that the QCDs do in fact represent buried impact craters, and thus validate an Early Noachian age for the buried lowland floor?
    Keywords: Lunar and Planetary Science and Exploration
    Type: Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life; LPI-Contrib-1211
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  • 73
    Publication Date: 2017-10-02
    Description: MOLA data have revealed a large population of "Quasi-Circular Depressions" (QCDs) with little or no visible expression in image data. These likely buried impact basins have important implications for the age of the lowland crust, how that compares with original highland crust, and when and how the crustal dichotomy may have formed. The buried lowlands are of Early Noachian age, likely slightly younger than the buried highlands but older than the exposed (visible) highland surface. A depopulation of large visible basins at diameters 800 to 1300 km suggests some global scale event early in martian history, maybe related to the formation of the lowlands and/or the development of Tharsis. A suggested early disappearance of the global magnetic field can be placed within a temporal sequence of formation of the very largest impact basins. The global field appears to have disappeared at about the time the lowlands formed. It seems likely the topographic crustal dichotomy was produced very early in martian history by processes which operated very quickly. Thus there appears to have been a northern lowland throughout nearly all of martian history, predating the last of the really large impacts (Hellas, Argyre and Isidis) and their likely very significant environmental consequences.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life; LPI-Contrib-1211
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  • 74
    Publication Date: 2017-10-02
    Description: Different-sized bodies of water have been proposed to have occurred episodically in the lowlands of Mars throughout the planet's history, largely related to major stages of development of Tharsis and/or orbital obliquity. These water bodies range from large oceans in the Noachian-Early Hesperian, to a minor sea in the Late Hesperian, and dispersed lakes during the Amazonian. To evaluate the more recent discoveries regarding the oceanic possibility, here we perform a comprehensive analysis of the evolution of water on Mars, including: 1. Geological assessment of proposed shorelines; 2. A volumetric approximation to the plains-filing proposed oceans; 3. Geochemistry of the oceans and derived mineralogies; 4. Post-oceanic (i.e., Amazonian) evolution of the shorelines; and 5. Ultimate water evolution on Mars.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Second Conference on Early Mars: Geologic Hydrologic, and Climatic Evolution and the Implications for Life; LPI-Contrib-1211
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  • 75
    Publication Date: 2017-10-02
    Description: Global data sets returned by the Mars Global Surveyor (MGS), Mars Odyssey, and Mars Express spacecraft and recent analyses of Martian meteorites suggest that most of the major geological events of Martian history occurred within the first billion years of solar system formation. This period was a time of heavy impact bombardment of the inner solar system, a process that strongly overprinted much of the Martian geological record from that time. Geophysical signatures nonetheless remain from that period in the Martian crust, and several geochemical tracers of early events are found in Martian meteorites. Collectively, these observations provide insight into the earliest era in Martian history when the conditions favoring life were best satisfied.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life; LPI-Contrib-1211
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  • 76
    Publication Date: 2018-06-08
    Keywords: Lunar and Planetary Science and Exploration
    Type: 2004 IEEE Aerospace Conference; Big Sky, MT; United States
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  • 77
    Publication Date: 2018-06-08
    Description: The NASA Discovery Stardust spacecraft flew by the main belt asteroid 5535 Annefrank at a distance of 3100 km and a speed of 7.4 km/s in November 2002 to test the encounter sequence developed for its primary science target, the comet 81P/Wild2. During this testing, over 70 images of Annefrank were obtained, taken over a phase angle range from 40 to 140 degrees.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Journal of Geophysical Research; Volume 109
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  • 78
    Publication Date: 2018-06-11
    Description: There is appreciable evidence for a significant hydrocarbon ocean on the surface of Titan. However, it has long been appreciated that tidal dissipation within a putative hydrocarbon ocean on Titan easily yields an orbital eccentricity damping time e which is short compared to the age of the solar system. Unless Titan s present eccentricity (e = 0.0288) were acquired recently, it requires that either: the ocean has a configuration which limits dissipation, or some mechanism exists which effectively maintains the eccentricity against dissipative damping. We argue for the latter. Specifically, the proximity of Jupiter and Saturn to a 5:2 mean motion resonance may provide a sufficient excitation source, and thereby effectively remove dynamical constraints on the dissipation and configuration of the Titan ocean.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Io, with a Dash of Titan; LPI-Contrib-1197
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  • 79
    Publication Date: 2018-06-11
    Description: We have begun work to prepare for producing controlled 2001 Mars Odyssey THEMIS infrared (IR) and visible (VIS) global mosaics of Mars. This effort is being coordinated with colleagues from Arizona State University and on the THEMIS team who plan to address radiometric issues in making such mosaics. We are concentrating on geometric issues. Several areas of investigation are now in progress, including: a) characterizing the absolute pointing accuracy of THEMIS images; b) investigating whether automatic tie point matching algorithms could be used to provide connections between overlapping THEMIS images; c) developing algorithms to allow for the photogrammetric (bundle) adjustment of the THEMIS IR (line scanner) camera images. Our primary goal in this pilot study effort will be to make several test control THEMIS mosaics and better determine which methods could be used, which require development, and what level of effort is required, in order to make large regional or global controlled THEMIS mosaics.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars: New Methods and Techniques; LPI-Contrib-1197
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  • 80
    Publication Date: 2018-06-11
    Description: The Mars Exploration Rover (MER) panoramic camera system (Pancam) has provided surface-based multispectral image data with unprecedented spatial and radiometric fidelity. The spectral coverage of the camera system allows for the discrimination of important Fe2+ and Fe3+ bearing minerals expected to occur on the Martian surface . This paper explores the spatially coherent and structurally consistent spectral variability present at both the Spirit and Opportunity landing sites using multidimensional analysis of representative Pancam multispectral scenes.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Missions; LPI-Contrib-1197
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  • 81
    Publication Date: 2018-06-11
    Description: Selection of the Mars Exploration Rover (MER) landing sites took place over a three year period in which engineering constraints were identified, 155 possible sites were downselected to the final two, surface environments and safety considerations were developed, and the potential science return at the sites was considered. Landing sites in Gusev crater and Meridiani Planum were selected because they appeared acceptably safe for MER landing and roving and had strong morphologic and mineralogical indicators of liquid water in their past and thus appeared capable of addressing the science objectives of the MER missions, which are to determine the aqueous, climatic, and geologic history of sites on Mars where conditions may have been favorable to the preservation of evidence of possible pre-biotic or biotic processes. Engineering constraints important to the selection included: latitude (10 N-15 S) for maximum solar power; elevation (〈-1.3 km) for sufficient atmosphere to slow the lander; low horizontal winds, shear and turbulence in the last few kilometers to minimize horizontal velocity; low 10-m scale slopes to reduce airbag spinup and bounce; moderate rock abundance to reduce abrasion or stroke-out of the airbags; and a radar-reflective, load-bearing and trafficable surface safe for landing and roving that is not dominated by fine-grained dust. In selecting the MER landing sites these engineering constraints were addressed via comprehensive evaluation of surface and atmospheric characteristics from existing remote sensing data and models as well as targeted orbital information acquired from Mars Global Surveyor and Mars Odyssey. This evaluation resulted in a number of predictions of the surface characteristics of the sites, which are tested in this abstract. Relating remote sensing signatures to surface characteristics at landing sites allows these sites to be used as ground truth for the orbital data, is essential for selecting and validating landing sites for future missions, and is required for correctly interpreting the surfaces and materials globally present on Mars.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Missions; LPI-Contrib-1197
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  • 82
    Publication Date: 2018-06-11
    Description: The Athena science payload on the Mars Exploration Rovers (MER) includes the Microscopic Imager (MI). The MI is a fixed-focus camera mounted on an extendable arm, the Instrument Deployment Device (IDD). The MI acquires images at a spatial resolution of 30 microns/pixel over a broad spectral range (400 - 700 nm). The MI uses the same electronics design as the other MER cameras but its optics yield a field of view of 31 x 31 mm across a 1024 x 1024 pixel CCD image. The MI acquires images using only solar or skylight illumination of the target surface. A contact sensor is used to place the MI slightly closer to the target surface than its best focus distance (about 69 mm), allowing concave surfaces to be imaged in good focus. Coarse focusing (approx. 2 mm precision) is achieved by moving the IDD away from a rock target after contact is sensed. The MI optics are protected from the Martian environment by a retractable dust cover. This cover includes a Kapton window that is tinted orange to restrict the spectral bandpass to 500 - 700 nm, allowing crude color information to be obtained by acquiring images with the cover open and closed. The MI science objectives, instrument design and calibration, operation, and data processing were described by Herkenhoff et al. Initial results of the MI experiment on both MER rovers ('Spirit' and 'Opportunity') are described below.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Missions; LPI-Contrib-1197
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  • 83
    Publication Date: 2018-06-11
    Description: The purpose of this paper is to report the 'early returns' on the physical properties of soil units and rocks at the MER landing sites. Because we are still very early in the mission at Meridiani Planum, results from the Gusev Crater Landing Site are emphasized here.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Missions; LPI-Contrib-1197
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  • 84
    Publication Date: 2018-06-11
    Description: The Viking and the Mars Exploration Rover missions observed that the surface of Mars is encrusted by a thinly cemented layer tagged as "duricrust". A hypothesis to explain the formation of duricrust on Mars should address not only the potential mechanisms by which these materials become cemented, but also the textural and compositional components of cemented Martian soils. Elemental analyzes at five sites on Mars show that these soils have sulfur content of up to 4%, and chlorine content of up to 1%. This is consistent with the presence of sulfates and halides as mineral cements. . For comparison, the rock "Adirondack" at the MER site, after the exterior layer was removed, had nearly five times lower sulfur and chlorine content , and the Martian meteorites have ten times lower sulfur and chlorine content, showing that the soil is highly enriched in the saltforming elements compared with rock.Here we propose two alternative models to account for the origin of these crusts, each requiring the action of transient liquid water films to mediate adhesion and cementation of grains. Two alternative versions of the transient water hypothesis are offered, a top down hypothesis that emphasizes the surface deposition of frost, melting and downward migration of liquid water and a bottom up alternative that proposes the presence of interstitial ice/brine, with the upward capillary migration of liquid water.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Missions; LPI-Contrib-1197
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  • 85
    Publication Date: 2018-06-11
    Description: Localization of the two Mars Exploration Rovers involved three independent approaches to place the landers with respect to the surface of Mars and to refine the location of those points on the surface with the Mars control net: 1) Track the spacecraft through entry, descent, and landing, then refine the final roll stop position by radio tracking and comparison to images taken during descent; 2) Locate features on the horizon imaged by the two rovers and compare them to the MOC and THEMIS VIS images, and the DIMES images on the two MER landers; and 3) 'Check' and refine locations by acquisition of MOC 1.5 meter and 50 cm/pixel images.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Missions; LPI-Contrib-1197
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  • 86
    Publication Date: 2018-06-11
    Description: This report casts the initial results of the traverse and science investigations by the Mars Exploration Rover (MER) Spirit at Gusev crater [1] in terms of data sets commonly used in field geologic investigations: Local mapping of geologic features, analyses of selected samples, and their location within the local map, and the regional context of the field traverse in terms of the larger geologic and physiographic region. These elements of the field method are represented in the MER characterization of the Gusev traverse by perspective-based geologic/morphologic maps, the placement of the results from Mossbauer, APXS, Microscopic Imager, Mini-TES and Pancam multispectral studies in context within this geologic/ morphologic map, and the placement of the overall traverse in the context of narrow-angle MOC (Mars Orbiter Camera) and descent images. A major campaign over a significance fraction of the mission will be the first robotic traverse of the ejecta from a Martian impact crater along an approximate radial from the crater center. The Mars Exploration Rovers have been conceptually described as 'robotic field geologists', that is, a suite of instruments with mobility that enables far-field traverses to multiple sites located within a regional map/image base at which in situ analyses may be done. Initial results from MER, where the field geologic method has been used throughout the initial course of the investigation, confirm that this field geologic model is applicable for remote planetary surface exploration. The field geologic method makes use of near-field geologic characteristics ('outcrops') to develop an understanding of the larger geologic context through continuous loop of rational steps focused on real-time hypothesis identification and testing. This poster equates 'outcrops' with the locations of in situ investigations and 'regional context' with the geology over distance of several kilometers. Using this fundamental field geologic method, we have identified the basic local geologic materials on the floor of Gusev at this site, their compositions and likely lithologies, origins, processes that have modified these materials, and their potential significance in the interpretation of the regional geology both spatially and temporally.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Missions; LPI-Contrib-1197
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  • 87
    Publication Date: 2018-06-11
    Description: For the first time in history a Moessbauer spectrometer was placed on the surface of another planet. The miniaturized Moessbauer spectrometer MIMOS II is part of the Athena payload of NASA's twin Mars Exploration Rovers (MER) Spirit,and Opportunity. It determines the Fe-bearing mineralogy of Martian soils and rocks at the Rovers respective landing sites, Gusev crater and Meridiani Planum. First results of soil and rock measurements at both landing sites confirm a generally basaltic composition of Martian surface materials.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Missions; LPI-Contrib-1197
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  • 88
    Publication Date: 2018-06-11
    Description: Newly developed APXS (Alpha Particle X-Ray Spectrometers) are part of the Athena payload of the Mars Exploration Rovers Spirit and Opportunity [1]. The APXS determines the chemical composition of soils and rocks along the traverse of the two rovers. Spirit and Opportunity operate at Gusev Crater and Meridiani Planum, respectively. First results of soil X-ray spectra at both landing sites support the hypothesis of a global homogenization of the soil by large dust storms and impact processes in the northern and southern hemisphere.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Missions; LPI-Contrib-1197
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  • 89
    Publication Date: 2018-06-11
    Description: Spirit landed in a flat plain in Gusev crater with local undulations at meters scales generated by ridges covered with blocks, some of them looking rounded. Several, flat-topped, mesas are visible in the far field in direction of Ma adim Vallis. A set of north/south oriented hills reaches approximately 150 m elevation to the east of the landing site (LS). A dipping brighter unit with possibly some scarps is associated with it. This setting could be consistent with layering observed on the MOC images of the hills, local exposure of material with variable dust cover, or deflated or allochtonous material. Numerous small depressions are visible from LS referred to as "Columbia Memorial Station"* (CMS). Floors are partially filled with finer-grained, high albedo material. At least one of them, nicknamed "Sleepy Hollow"* (approximately 30 m diameter) may be an eroded secondary impact crater. It is unclear if they can all be related to small impact structures. Some of them are elongated and aligned with the ridges. The morphology of rocks and soil at this Gusev Crater is presented. Evidence of dynamic aeolian action along this Crater is also discussed.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Missions; LPI-Contrib-1197
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  • 90
    Publication Date: 2018-06-11
    Description: Recently, nebular shock waves have become one of the leading candidates for explaining the presence of chondrules in primitive meteorites. While shocks have been shown to be capable of explaining many of the features of chondrules, a major problem with the theory is that the source of the shocks remains unidentified. Among the suggested sources of the shocks are bow shocks created by supersonic planetesimals in the nebula. Recently, we studied the structure of the shocks that would form around such supersonic planetesimals. We found that particles that encountered the shocks at distances greater than 2 planetesimal radii from the planetesimal would cool too quickly to form the textures observed in chondrules. While the region of the shock far away from the planetesimal may not allow chondrules to form, the region closer in has not been studied in detail. In this work we consider the dynamical and thermal evolution of particles that encounter supersonic planetesimals in this region.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Origin of Planetary Systems; LPI-Contrib-1197
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  • 91
    Publication Date: 2018-06-11
    Description: High-resolution topographic data for Mars from the Mars Orbiter Laser Altimeter (MOLA), and imagery from the Mars Orbiter Camera (MOC) and the Thermal Emission Imaging System (THEMIS) allow for the first accurate assessment of lava flow directions relative to topographic slopes in the Tharsis region. Tharisis has long been recognized as the dominant tectonic and volcanic province on the planet, with a complex geologic history. In this study, lava flow directions on Daedalia Planum, Syria Planum, Tempe Terra, and near the Tharsis Montes are compared with MOLA topographic contours to look for deviations of flow directions from the local slope direction. The topographic deviations identified in this study are likely due to Tharsis tectonic deformation that has modified the regional topography subsequent to the emplacement of the flows, and can be used to model the mechanisms and magnitudes of relatively recent tectonism in the region. A similar approach was used to identify possible postflow tectonic subsidence on the Snake River Plain in Idaho.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Volcanology and Tectonics; LPI-Contrib-1197
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  • 92
    Publication Date: 2018-06-11
    Description: Mars Orbiter Laser Altimeter (MOLA) data allows insight to Martian features in great detail, revealing numerous small shields in the Tempe region, consisting of low profiles and a prominent summit caps . Terrestrial examples of this shield morphology are found on the Eastern Snake River Plain (ESRP), Idaho. This plains-style volcanism [2] allows an analog to Martian volcanism based on topographic manifestations of volcanic processes . Recent studies link the slope and morphology of Martian volcanoes to eruptive process and style . The ESRP, a 400km long, 100km wide depression, is host to hundreds of tholeiitic basalt shields, which have low-profiles built up over short eruptive periods of a few months or years . Many of these smaller scale shields (basal diameters rarely exceed 5km) display morphology similar to the volcanoes in the Tempe region of Mars . Morphological variations within these tholeiitic shields are beautifully illustrated in their profiles.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Volcanology and Tectonics; LPI-Contrib-1197
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  • 93
    Publication Date: 2018-06-11
    Description: Channelized lava flows on Mars and the Earth often feature levees and collateral margins that change in volume along the path of the flow. Consistent with field observations of terrestrial flows, this suggests that the rate of levee formation varies with distance and other factors. Previous models have assumed a constant rate of levee growth, specified by a single parameter, lambda. The rate of levee formation for lava flows is a good indicator of the mass eruption rate and rheology of the flow. Insight into levee formation will help us better understand whether or not the effusion rate was constant during an eruption, and once local topography is considered, allows us to look at cooling and/or rheology changes downslope. Here we present a more realistic extension of the levee formation model that treats the rate of levee growth as a function of distance along the flow path. We show how this model can be used with a terrestrial flow and a long lava flow on Mars. The key statement of the new formulation is the rate of transfer from the active component to the levees (or other passive components) through an element dx along the path of the flow. This volumetric transfer equation is presented.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Volcanology and Tectonics; LPI-Contrib-1197
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  • 94
    Publication Date: 2018-06-11
    Description: CEPS has undertaken an extended study of long lava flows on the terrestrial planets, their location, morphology, and potential modes of emplacement. As part of this ongoing investigation, we have concentrated on a single large flow in Tharsis, with noted similarities to several terrestrial analogs. An impressive series of lava flows emerges from the topographic saddle between Ascraeus and Pavonis Mons. The most prominent of these (hereafter referred to as the 'Saddle Flow') has distinct margins that can be traced for over 480 km in the Viking images, although its exact source cannot be identified. A multimodal approach is utilized in the examination of the Saddle Flow, including image interpretation (VIKING and THEMIS, MOLA topographic analysis and flow profiling, downflow behavior statistical analysis, rheologic modeling, and GIS modeling and integration.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Volcanology and Tectonics; LPI-Contrib-1197
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  • 95
    Publication Date: 2018-06-11
    Description: The determination of oxidation conditions for basaltic magmas derived by the melting of planetary mantles is critical to our understanding of the nature and evolution of planetary interiors. Yet, these determinations are compromised in terrestrial and especially extraterrestrial basalts by our analytical and computational methods for estimating oxygen fugacity (fO2). For example, mineralogical barometers (1, 2) can be reduced in effectiveness by subsolidus re-equilibration of mineral assemblages, inversion of mineralogical data to melt characteristics, and deviations of the natural mineral compositions from ideal thermodynamic parameters.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Special Session: Oxygen in the Solar System, II; LPI-Contrib-1197
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  • 96
    Publication Date: 2018-06-11
    Description: The issue of whether martian magmas are wet or dry is an important one. The answer to this basic question has profound consequences for how we think about Mars as a planet. Recently, several lines of evidence have been presented that collectively suggest that shergottite parent magmas were once wet. These include: (i) phase equilibria studies that indicate that the Shergotty parent magma required ~2 wt.% water in order to be co-saturated with both pigeonite and augite, (ii) reverse zoning of light lithophile elements (Li and B) in shergottite pyroxenes, suggesting the exsolution and removal of an aqueous fluid, and (iii) measurement of D/H ratios in SNC minerals that are much lower than atmospheric, suggesting that there may be juvenile (primordial) mantle water. Below I will review the evidence for the diametrically opposite case, that shergottite magmas were effectively dry (〈〈 1 wt.% H2O).
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Martian Meteorites: Hot and Steamy; LPI-Contrib-1197
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  • 97
    Publication Date: 2018-06-11
    Description: The Antarctic Research Center of the Japanese National Institute of Polar Research (NIPR) recently announced the discovery of a new Martian shergottite, Y98(0459). This sample is a member of the subgroup of basaltic shergottites that contain abundant olivine phenocrysts, and are thus olivine- phyric. Y98 may have special significance among the basaltic shergottites because (1) it appears to have been the most magnesian Martian magma yet found, and thus can provide valuable clues to magma petrogenesis on Mars; (2) it contains no late-crystallizing phases, but instead contains approx. 30% interstitial glass, which can provide unambiguous incompatible element patterns of the parent melt; and (3) it carries an LREE-depleted signature similar to QUE 94201, whose isotopic characteristics are the most primitive of all basaltic shergottites.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Martian Meteorites: Hot and Steamy; LPI-Contrib-1197
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  • 98
    Publication Date: 2018-06-11
    Description: Y980459 was found near the Minami-Yamato Nunataks, Antarctica in 1998 and was recently classified as an olivine-bearing shergottite. It petrographically resembles many other olivine-phyric shergottites mostly found in hot deserts, e.g. DaG476/489, SaU005/094, Dohfar 019, NWA 1068/1110, NWA 1195 and EETA 79001 lith.A. However, Y980459 is unique among these meteorites in several respects. It is apparently very fresh and only weakly shocked. Also, it completely lacks plagioclase, but contains abundant residual volcanic glass. This group of olivine-phyric shergottites is characterized by variable crystallization ages from approx.172 Ma to approx.575 Ma and ejection ages from approx.1 Ma to approx.20 Ma. They probably represent volcanic melts originated from the deep Martian mantle. We performed Rb-Sr and Sm-Nd isotopic analyses on Y980459 to determine its crystallization age and compared its age and isotopic signatures with those obtained from other olivine-phyric shergottites and QUE 94201, the other Antarctic olivine-free shergottite. QUE 94201 and some olivine-phyric shergottites e.g. DaG, SaU, Doh and EETA lith A have similar depleted-LREE patterns and are herein referred to as depleted shergottites. A petrogenetic model correlating depleted shergottites and nakhlites is also proposed. Preliminary Rb-Sr and Sm-Nd isotopic data for Y980459 were presented earlier at the NIPR, Japan, in 2003.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Martian Meteorites: Hot and Steamy; LPI-Contrib-1197
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  • 99
    Publication Date: 2018-06-11
    Description: Recently, several basaltic shergottites have been found that include magnesian olivines as a major minerals. These have been called olivinephyric shergottites. Yamato 980459, which is a new martian meteorite recovered from the Antarctica by the Japanese Antarctic expedition, is one of them. This meteorite is different from other olivine-phyric shergottites in several key features and will give us important clues to understand crystallization of martian meteorites and the evolution of Martian magma.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Martian Meteorites: Hot and Steamy; LPI-Contrib-1197
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  • 100
    Publication Date: 2018-06-11
    Description: Martian meteorite ALH84001 carbonates preserve large and variable microscale isotopic compositions, which in some way reflect their formation environment. These measurements show large variations (〉20%) in the carbon and oxygen isotopic compositions of the carbonates on a 10-20 micron scale that are correlated with chemical composition. However, the utilization of these data sets for interpreting the formation conditions of the carbonates is complex due to lack of suitable terrestrial analogs and the difficulty of modeling under non-equilibrium conditions. Thus, the mechanisms and processes are largely unknown that create and preserve large microscale isotopic variations in carbonate minerals. Experimental tests of the possible environments and mechanisms that lead to large microscale isotopic variations can help address these concerns. One possible mechanism for creating large carbon isotopic variations in carbonates involves the freezing of water. Carbonates precipitate during extensive CO2 degassing that occurs during the freezing process as the fluid s decreasing volume drives CO2 out. This rapid CO2 degassing results in a kinetic isotopic fractionation where the CO2 gas has a much lighter isotopic composition causing an enrichment of 13C in the remaining dissolved bicarbonate. This study seeks to determine the suitability of cryogenically formed carbonates as analogs to ALH84001 carbonates. Specifically, our objective is to determine how accurately models using equilibrium fractionation factors approximate the isotopic compositions of cryogenically precipitated carbonates. This includes determining the accuracy of applying equilibrium fractionation factors during a kinetic process, and determining how isotopic variations in the fluid are preserved in microscale variations in the precipitated carbonates.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Martian Meteorites: Hot and Steamy; LPI-Contrib-1197
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