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  • Lunar and Planetary Science and Exploration  (1,839)
  • Waves
  • 2005-2009  (1,855)
  • 1950-1954  (12)
  • 1935-1939  (7)
  • 1925-1929
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  • 1
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    Massachusetts Institute of Technology and Woods Hole Oceanographic Institution
    Publication Date: 2022-05-25
    Description: Submitted to the Joint Program in Physical Oceanography in partial fulfillment of the requirements for the degree of Doctor of Philosophy at the Massachusetts Institute of Technology and the Woods Hole Oceanographic Institution September 2006
    Description: Ocean surface infragravity waves (periods from 20 to 200 s) observed along the southern California coast are shown to be sensitive to the bottom topography of the shelf region, where propagation is linear, and of the nearshore region, where nonlinearity is important. Infragravity waves exchange energy with swell and wind waves (periods from 5 to 20 s) via conservative nonlinear interactions that approach resonance with decreasing water depth. Consistent with previous results, it is shown here that as waves shoal into water less than a few meters deep, energy is transfered from swell to infragravity waves. In addition, it is shown here that the apparent dissipation of infragravity energy observed in the surfzone is the result of nonlinear energy transfers from infragravity waves back to swell and wind waves. The energy transfers are sensitive to the shallow water bottom topography. On nonplanar beach profiles the transfers, and thus the amount of infragravity energy available for reflection from the shoreline, change with the tide, resulting in the tidal modulation of infragravity energy observed in bottom-pressure records on the continental shelf. The observed wave propagation over the shelf topography is dominated by refraction, and the observed partial reflection from, and transmission across, a steep-walled submarine canyon is consistent with long-wave theory. A generalized regional model incorporating these results predicts the observed infragravity wave amplitudes over variable bottom topography.
    Description: Support from the Office of Naval Research (Coastal Geosciences Program, N00014-02-10145), the National Science Foundation (Physical Oceanography, OCE-0115850),
    Keywords: Waves ; Ocean bottom
    Repository Name: Woods Hole Open Access Server
    Type: Thesis
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  • 2
    Publication Date: 2022-05-26
    Description: Wave power spectra from four waverider buoys on the New England Shelf and wind velocity records from three of those buoys and a fixed platform were analyzed. The data span the period from May 1987 through August 1988. Time series plots of significant wave height, mean wave period and modal (peak) period and distribution histograms of significant wave height, mean frequency and modal frequency are presented for the two buoys nearest to Martha's Vineyard. Time series plots of wind speed and vector velocity and distribution histograms of speed and direction are plotted for one buoy and the platform. For all stations, monthly and seasonal mean and extreme values of significant wave height, mean and modal wave periods, wind speed and mean weighted and unweighted values of wind direction are provided in tabular form. Five and ten year extreme wave height predictions are also calculated.
    Description: Funding was provided by the Office of Naval Research through contract Number N00014-86-K-0715 under the University Research Initiative Program.
    Keywords: Wind ; Waves ; Statistics
    Repository Name: Woods Hole Open Access Server
    Type: Technical Report
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  • 3
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    Massachusetts Institute of Technology and Woods Hole Oceanographic Institution
    Publication Date: 2022-05-26
    Description: Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy at the Massachusetts Institute of Technology and the Woods Hole Oceanographic Institution September, 1970
    Description: A series of laboratory experiments were conducted in a glass wave tank to investigate the propagation of internal gravity waves up a sloping bottom in a fluid with constant Brunt-Vaisala frequency. Measurements of the wave motion in the fluid interior were primarily taken with electrical conductivity probes; measurements in the boundary layer were made with dye streaks and neutrally buoyant particles. The results indicate that, outside of the breaking zone, the amplitude and horizontal wave number of the high-frequency waves increase lineariy with decreasing depth; this is shown to agree with existing linear, inviscid solutions. A zone of breaking or runup is induced by these high-frequency waves well upslope. Shadowgraph observations show that, if the wave characteristics are coincident, or nearly so, with the bottom slope, the upslope propagation of the low-frequency waves causes a line of regularly spaced vortices to form along the slope. Subsequent mixing in the vortex cells creates thin horizontal laminae that are more homogeneous than the adjacent layers. These laminae slowly penetrate the fluid interior, creating a step-like vertical density structure. Available linear theoretical solutions for the velocity in the viscous boundary layer, determined to be valid for certain experimental conditions, are used to develop a criterion for incipient motion of bottom sediment induced by shoaling internal waves. The maximum sediment sizes that can be placed into motion, according to this criterion, are larger than certain mean sediment sizes on the continental margin off New England. This suggests that internal waves might induce initial sediment movement. Speculation about the geological effects of breaking and vortex instabilities is also given. These processes, not definitely measured in the field as yet, might also be conducive to sediment movement.
    Description: This work was supported by the Office of Naval Research.
    Keywords: Sediment transport ; Waves
    Repository Name: Woods Hole Open Access Server
    Type: Thesis
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  • 4
    Publication Date: 2022-05-26
    Description: This paper is not subject to U.S. copyright. The definitive version was published in Continental Shelf Research 24 (2004): 1397-1419, doi:10.1016/j.csr.2004.02.010.
    Description: The fringing coral reef off the south coast of Molokai, Hawaii is currently being studied as part of a US Geological Survey (USGS) multi-disciplinary project that focuses on geologic and oceanographic processes that affect coral reef systems. For this investigation, four instrument packages were deployed across the fringing coral reef during the summer of 2001 to understand the processes governing fine-grained terrestrial sediment suspension on the shallow reef flat (h=1 m) and its advection across the reef crest and onto the deeper fore reef. The time–series measurements suggest the following conceptual model of water and fine-grained sediment transport across the reef: Relatively cool, clear water flows up onto the reef flat during flooding tides. At high tide, more deep-water wave energy is able to propagate onto the reef flat and larger Trade wind-driven waves can develop on the reef flat, thereby increasing sediment suspension. Trade wind-driven surface currents and wave breaking at the reef crest cause setup of water on the reef flat, further increasing the water depth and enhancing the development of depth-limited waves and sediment suspension. As the tide ebbs, the water and associated suspended sediment on the reef flat drains off the reef flat and is advected offshore and to the west by Trade wind- and tidally- driven currents. Observations on the fore reef show relatively high turbidity throughout the water column during the ebb tide. It therefore appears that high suspended sediment concentrations on the deeper fore reef, where active coral growth is at a maximum, are dynamically linked to processes on the muddy, shallow reef flat.
    Keywords: Coral reefs ; Waves ; Tides ; Suspended sediment ; Sediment flux ; Cross-shore transport
    Repository Name: Woods Hole Open Access Server
    Type: Article
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  • 5
    Publication Date: 2022-05-26
    Description: This paper is not subject to U.S. copyright. The definitive version was published in Marine Geology 264 (2009): 140-151, doi:10.1016/j.margeo.2009.05.002.
    Description: Oceanographic measurements and sediment samples were collected during the summer of 2006 as part of a multi-year study of coastal circulation and the fate of terrigenous sediment on coral reefs in Hanalei Bay, Kauai. The goal of this study was to better understand sediment dynamics in a coral reef-lined embayment where winds, ocean surface waves, and river floods are important processes. During a summer period that was marked by two wave events and one river flood, we documented significant differences in sediment trap collection rates and the composition, grain size, and magnitude of sediment transported in the bay. Sediment trap collection rates were well correlated with combined wave-current near-bed shear stresses during the non-flood periods but were not correlated during the flood. The flood's delivery of fine-grained sediment to the bay initially caused high turbidity and sediment collection rates off the river mouth but the plume dispersed relatively quickly. Over the next month, the flood deposit was reworked by mild waves and currents and the fine-grained terrestrial sediment was advected around the bay and collected in sediment traps away from the river mouth, long after the turbid surface plume was gone. The reworked flood deposits, due to their longer duration of influence and proximity to the seabed, appear to pose a greater long-term impact to benthic coral reef communities than the flood plumes themselves. The results presented here display how spatial and temporal differences in hydrodynamic processes, which result from variations in reef morphology and orientation, cause substantial variations in the deposition, residence time, resuspension, and advection of both reef-derived and fluvial sediment over relatively short spatial scales in a coral reef embayment.
    Keywords: Coral reefs ; Winds ; Waves ; Currents ; Sediment traps ; Sedimentation ; USA ; Hawaii ; Kauai
    Repository Name: Woods Hole Open Access Server
    Type: Article
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  • 6
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    In:  Gerlands Beiträge zur Geophysik, Milano, Gustav Fischer, vol. 45, no. 3, pp. 280-360, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1935
    Keywords: Waves ; Seismology ; Review article
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  • 7
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    In:  Gerlands Beiträge zur Geophysik, Milano, Gustav Fischer, vol. 47, no. 3, pp. 73-131, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1936
    Keywords: Waves ; Seismology ; Review article
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  • 8
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    In:  Geophysics, Milano, California Institute of Technology Pasadena, vol. 15, no. 6, pp. 156, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1950
    Keywords: Waves ; Velocity analysis ; Seismology
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  • 9
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    In:  Bull. Geol. Soc. Am., Milano, California Institute of Technology Pasadena, vol. 62, no. 6, pp. 1528, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1951
    Keywords: Travel time ; Waves ; Nuclear explosion
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  • 10
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    In:  Trans., Am. Geophys. Union, Milano, California Institute of Technology Pasadena, vol. 33, no. 6, pp. 427-431, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1952
    Keywords: Waves ; Seismometer ; Seismology ; EOS
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  • 11
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    In:  Trans., Am. Geophys. Union, Milano, California Institute of Technology Pasadena, vol. 33, no. 6, pp. 573-584, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1952
    Keywords: Waves ; SV waves ; Shear waves ; Seismology ; SH waves ; EOS
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  • 12
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    In:  Bull. Geol. Soc. Am., Los Angeles California, 1 p., California Institute of Technology Pasadena, vol. 63, no. 6, pp. 1353, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1952
    Keywords: Surface waves ; Waves ; Seismology ; Shear waves
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  • 13
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    In:  Trans., Am. Geophys. Union, Milano, California Institute of Technology Pasadena, vol. 32, no. 6, pp. 373-390, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1951
    Keywords: Waves ; earth Core ; Seismology ; P-waves ; EOS
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  • 14
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    In:  Geophys. Res. Lett., Luxembourg, Conseil de l'Europe, vol. 32, no. 1, pp. 760-768, pp. L01306, (ISSN: 1340-4202)
    Publication Date: 2005
    Keywords: Rheology ; Wave propagation ; Modelling ; Waves ; Attenuation ; GRL
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  • 15
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    In:  Zeitschrift für Geophysik, Jena, Gustav Fischer, vol. 2, no. 3, pp. 260-266, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1926
    Keywords: Waves ; Acoustics
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  • 16
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    In:  Die Naturwissenschaften, Jena, Gustav Fischer, vol. 14, no. 3, pp. 338-342, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1926
    Keywords: Waves ; Meteorology ; Acoustics
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  • 17
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    In:  Nature, Milano, Gustav Fischer, vol. 141, no. 6, pp. 371, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1938
    Keywords: Waves ; Seismology ; earth Core
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  • 18
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    In:  Month. Notices Royal astr. Soc., Geophys. Suppl., Milano, Gustav Fischer, vol. 4, no. 6, pp. 363-372, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1938
    Keywords: Waves ; earth Core ; P-waves ; Diffraction
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  • 19
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    In:  Bull. Seism. Soc. Am., Oxford and Edinburgh, Blackwell Scientific Publications, vol. 43, no. 11, pp. 17-34, pp. L23301, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1953
    Keywords: Surface waves ; Dispersion ; Layers ; Waves ; Modelling ; Synthetic seismograms ; BSSA ; FROTH ; HPH
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  • 20
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    In:  Geophys., Oxford and Edinburgh, Blackwell Scientific Publications, vol. 18, no. 5, pp. 871-893, pp. B09408, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1953
    Keywords: Waves ; Refraction seismics ; Head waves
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  • 21
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    In:  Geophys. Res. Lett., Kyoto, AGU, vol. 33, no. 7, pp. 627-638, pp. L07305, (ISSN: 1340-4202)
    Publication Date: 2006
    Keywords: Strong motions ; Site amplification ; Earthquake engineering, engineering seismology ; Earthquake risk ; Fault zone ; SAF ; USA ; Love-waves ; basin ; guided ; Waves ; Modelling ; GRL ; 7212 ; Seismology: ; Earthquake ; ground ; motions ; and ; engineering ; seismology ; 7260 ; Theory ; 7290 ; Seismology: ; Computational ; seismology
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  • 22
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    In:  J. appl. Phys., London, AGU, vol. 21, no. 2, pp. 89-93, pp. L10304, (ISSN: 1340-4202)
    Publication Date: 1950
    Keywords: Wavelet processing ; Layers ; Waves ; Modelling ; Thomson-Haskell ; Synthetic seismograms
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  • 23
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    In:  Bull. Am. Meteor. Soc., Beijing, Pergamon, vol. 20, no. 3-4, pp. 421-426, pp. 1246
    Publication Date: 1939
    Keywords: Waves ; Electromagnetic methods/phenomena ; Instruments ; Meteorology
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  • 24
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    In:  Eos Trans. AGU, Warszawa, Inst. Electrical & Electronics Engineers, vol. 86, no. 35, pp. 317 & 320, pp. 2121, (ISBN: 0534351875, 2nd edition)
    Publication Date: 2005
    Description: Infrasound arrays in the Pacific and Indian oceans that are part of the International Monitoring System (IMS) of the Comprehensive Nuclear Test Ban Treaty (CTBT) recorded distinct signatures associated with the 26 December 2004 Sumatra earthquake (M9, http://earthquake.usgs.gov/) and tsunami. Although the radiation of infrasound from large continental earthquakes is established [e.g., Le Pichon et al., 2003], the results presented in the present article indicate that islands undergoing significant surface displacements from submarine earthquakes can produce infrasound. Far more intriguing is the possibility that the initiation and propagation of a tsunami may produce low-frequency sound near the source as well as along coastlines and basins. Since distant sound effectively propagates at ~300 m/s and tsunamis propagate at ~200 m/s, precursory sound could potentially be used as a discriminant for tsunami genesis
    Keywords: Tsunami(s) ; Acoustics ; Waves ; Earthquake ; Banda ; Aceh ; Indonesia ; Garces ; Pichon ; 4564 ; Oceanography: ; Physical: ; Tsunamis ; and ; storm ; surges ; 7209 ; Seismology: ; Earthquake ; dynamics ; 9805 ; General ; or ; Miscellaneous: ; Instruments ; useful ; in ; three ; or ; more ; fields
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  • 25
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    In:  J. Geophys. Res., Karlsruhe, 3-4, vol. 110, no. B10, pp. 870-881, pp. B10302, (ISBN: 0534351875, 2nd edition)
    Publication Date: 2005
    Keywords: Channel waves ; Fault zone ; trapped ; Waves ; Inhomogeneity ; Subduction zone ; Intensity ; Site amplification ; Seismology ; JGR
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  • 26
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    In:  Trans., Am. Geophys. Union, Los Angeles California, 1 p., California Institute of Technology Pasadena, vol. 34, no. 6, pp. 161-173, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1953
    Keywords: Micro seismicity ; Waves ; Seismology ; Meteorology ; NOISE ; EOS
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  • 27
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    In:  Gerlands Beiträge zur Geophysik, Milano, Gustav Fischer, vol. 54, no. 6, pp. 94-136, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1939
    Keywords: Waves ; Seismology ; Review article
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  • 28
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    In:  Zeitschrift für Physik, Leipzig, Birkhäuser Verlag, vol. 38, no. 5, pp. 803, pp. L15S17, (ISBN: 0-12-018847-3)
    Publication Date: 1926
    Keywords: physics ; Scattering ; Waves ; quantum ; mechanics
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  • 29
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    In:  Physikalische Zeitschrift, Milano, Gustav Fischer, vol. 30, no. 3, pp. 230-231, pp. L24306, (ISBN: 0534351875, 2nd edition)
    Publication Date: 1929
    Keywords: Seismology ; Elasticity ; Waves ; Inelastic ; Fluids
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  • 30
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    In:  Geophys. Res. Lett., Philadelphia, 4, vol. 32, no. 4, pp. 1063-1066, pp. L04302, (ISSN: 1340-4202)
    Publication Date: 2005
    Keywords: Stress ; Seismicity ; Dynamic ; Waves ; Aftershocks ; Friction ; Fault zone ; Physical properties of rocks ; Omori ; GRL ; 7209 ; Seismology: ; Earthquake ; dynamics ; (1242) ; 7223 ; Earthquake ; interaction, ; forecasting, ; and ; prediction ; (1217, ; 1242) ; 7230 ; Seismicity ; and ; tectonics ; (1207, ; 1217, ; 1240, ; 1242) ; 7260 ; Theory
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  • 31
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    In:  Geophys. Res. Lett., Veldhoven, Kluwer, vol. 33, no. 18, pp. 101-108, pp. L18305, (ISSN: 1340-4202)
    Publication Date: 2006
    Keywords: Seismology ; period ; 500 ; s ; (The Earth's free) oscillations ; Surface waves ; Waves ; Earthquake ; Indonesia ; Banda ; Aceh ; GRL ; 7215 ; Seismology: ; Earthquake ; source ; observations ; (1240) ; 7209 ; Earthquake ; dynamics ; (1242) ; 7230 ; Seismicity ; and ; tectonics ; (1207, ; 1217, ; 1240, ; 1242) ; 7255 ; Surface ; waves ; and ; free ; oscillations
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  • 32
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    J. A. Barth
    In:  Professional Paper, Handbuch der physikalischen und technischen Mechanik, Bd. III, Leipzig, J. A. Barth, vol. 3, no. VIIa, pp. 387-420, (ISBN: 3-540-23712-7)
    Publication Date: 1927
    Keywords: Seismology ; Seismicity ; Waves
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  • 33
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    Springer
    In:  Professional Paper, Landolt Börnstein (6. Edition) III. Band: Astronomie und Geophysik, Berlin, Springer, vol. 7, no. XVI:, pp. 375-384, (ISBN: 3-540-23712-7)
    Publication Date: 1952
    Keywords: Seismology ; Waves
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  • 34
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    In:  Bull. Seism. Soc. Am., Tokyo, Railway Tech. Res. Inst., vol. 44, no. 4, pp. 39-56, pp. L06615, (ISSN: 1340-4202)
    Publication Date: 1954
    Keywords: Waves ; Seismology ; earth Core ; Travel time ; BSSA
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  • 35
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    In:  J. Geophys. Res., Luxembourg, Deutsche Geophys. Gesellschaft, vol. 110, no. B11, pp. 703-710, pp. B11307, (ISSN: 1340-4202)
    Publication Date: 2005
    Keywords: Wave propagation ; Waves ; Modelling ; Elasticity ; porosity ; Fluids ; Anisotropy ; JGR ; anisotropic ; poroelastic ; (APE) ; solid ; Biot's ; theory ; phase ; velocity ; attenuation ; 3285 ; Mathematical ; Geophysics: ; Wave ; propagation ; (0689, ; 2487, ; 4275, ; 4455, ; 6934) ; 5102 ; Physical ; Properties ; of ; Rocks: ; Acoustic ; properties ; 5144 ; Wave ; attenuation ; 7203 ; Seismology: ; Body ; waves ; 7260 ; Theory
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  • 36
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    In:  Geophys. Res. Lett., Taipei, EGS, vol. 32, no. 20, pp. 183-194, pp. L20303, (ISSN: 1340-4202)
    Publication Date: 2005
    Keywords: Seismology ; Location ; Waves ; Electromagnetic methods/phenomena ; GRL ; 0689 ; Electromagnetics: ; Wave ; propagation ; (2487, ; 3285, ; 4275, ; 4455, ; 6934) ; 5109 ; Physical ; Properties ; of ; Rocks: ; Magnetic ; and ; electrical ; properties ; (0925) ; 6914 ; Radio ; Science: ; Electromagnetic ; noise ; and ; interference ; 7223 ; Seismology: ; Earthquake ; interaction, ; forecasting, ; and ; prediction ; (1217, ; 1242)
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  • 37
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    Gauthier-Villars
    In:  Paris, Gauthier-Villars, vol. 3, no. 3, pp. 275-291, (ISBN 0-415-24328-9 (hb), 0-203-47128-8 (pb))
    Publication Date: 1939
    Keywords: Waves ; Refraction seismics ; Reflection seismics
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  • 38
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    Bornträger
    In:  Professional Paper, Handbuch der Geophysik, Volume 4: Erdbeben (finished), 12 + 1202 S., Berlin, Bornträger, vol. 3, no. VIIa, pp. 1-150, (ISBN: 3-540-23712-7)
    Publication Date: 1929
    Keywords: Review article ; Seismology ; Waves ; Wave propagation
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  • 39
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    In:  J. Geophys. Res., New York, Scientific American, vol. 111, no. B4, pp. 799-815, pp. B04305, (ISSN: 1340-4202)
    Publication Date: 2006
    Keywords: Wave propagation ; Waves ; Finite difference method ; Modelling ; TWO ; Inhomogeneity ; Scattering ; Born ; RTT ; Monte ; Carlo ; Energy (of earthquakes) ; JGR ; 7203 ; Seismology: ; Body ; waves ; 7260 ; Seismology: ; Theory ; 7290 ; Computational ; seismology
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  • 40
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    Elsevier
    In:  Amsterdam, 652 pp., Elsevier, vol. 39, no. XVI:, pp. 227-235, (0-444-51955-6)
    Publication Date: 2005
    Keywords: Seismics (controlled source seismology) ; Applied geophysics ; Wave propagation ; plane ; spherical ; and ; cylindrical ; Waves ; in ; isotropic ; and ; transversely ; isotropic ; solids, ; liquid-solid ; models, ; and ; media ; with ; cylindrical ; inclusions ; (boreholes) ; Textbook of geophysics
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  • 41
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    AGU
    In:  Washington, D.C., 280 pages, AGU, vol. 81A and 81B, no. 22, pp. 65-70, (ISBN 0-87590-422-X)
    Publication Date: 2005
    Keywords: Seismology ; Seismic arrays ; Data analysis / ~ processing ; Ray seismics ; Synthetic seismograms ; Modelling ; Wave propagation ; Waves ; Earth model, also for more shallow analyses ! ; Physical properties of rocks ; Broad-band
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  • 42
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    Bornträger
    In:  Professional Paper, Lehrbuch der Geophysik, Berlin, 6 + 1017 pp., Bornträger, vol. 3, no. VIIa, pp. 308-353, (ISBN: 3-540-23712-7)
    Publication Date: 1926
    Keywords: Waves ; TIDES
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  • 43
    Publication Date: 2011-08-24
    Description: The Cassini Titan Radar Mapper imaged about 1% of Titan's surface at a resolution of approximately 0.5 kilometer, and larger areas of the globe in lower resolution modes. The images reveal a complex surface, with areas of low relief and a variety of geologic features suggestive of dome-like volcanic constructs, flows, and sinuous channels. The surface appears to be young, with few impact craters. Scattering and dielectric properties are consistent with porous ice or organics. Dark patches in the radar images show high brightness temperatures and high emissivity and are consistent with frozen hydrocarbons.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 308; 5724; 970-4
    Format: text
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  • 44
    Publication Date: 2011-08-24
    Description: The mineralogical and elemental compositions of the martian soil are indicators of chemical and physical weathering processes. Using data from the Mars Exploration Rovers, we show that bright dust deposits on opposite sides of the planet are part of a global unit and not dominated by the composition of local rocks. Dark soil deposits at both sites have similar basaltic mineralogies, and could reflect either a global component or the general similarity in the compositions of the rocks from which they were derived. Increased levels of bromine are consistent with mobilization of soluble salts by thin films of liquid water, but the presence of olivine in analysed soil samples indicates that the extent of aqueous alteration of soils has been limited. Nickel abundances are enhanced at the immediate surface and indicate that the upper few millimetres of soil could contain up to one per cent meteoritic material.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Nature (ISSN 0028-0836); Volume 436; 7047; 49-54
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  • 45
    Publication Date: 2011-08-26
    Description: To explain the much higher denudation rates and valley network development on early Mars (more than approximately 3.6 Gyr ago), most investigators have invoked either steady state warm/wet (Earthlike) or cold/dry (modern Mars) end-member paleoclimates. Here we discuss evidence that highland gradation was prolonged, but generally slow and possibly ephemeral during the Noachian Period, and that the immature valley networks entrenched during a brief terminal epoch of more erosive fluvial activity in the late Noachian to early Hesperian. Observational support for this interpretation includes (1) late-stage breaching of some enclosed basins that had previously been extensively modified, but only by internal erosion and deposition; (2) deposition of pristine deltas and fans during a late stage of contributing valley entrenchment; (3) a brief, erosive response to base level decline (which was imparted as fretted terrain developed by a suite of processes unrelated to surface runoff) in fluvial valleys that crosscut the highland-lowland boundary scarp; and (4) width/contributing area relationships of interior channels within valley networks, which record significant late-stage runoff production with no evidence of recovery to lower-flow conditions. This erosion appears to have ended abruptly, as depositional landforms generally were not entrenched with declining base level in crater lakes. A possible planetwide synchronicity and common cause to the late-stage fluvial activity are possible but remain uncertain. This increased activity of valley networks is offered as a possible explanation for diverse features of highland drainage basins, which were previously cited to support competing warm, wet and cold, dry paleoclimate scenarios.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Journal of Geophysical Research; Vol. 110
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  • 46
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    Publication Date: 2011-08-24
    Description: The NASA STARDUST mission collected thousands of particles from Comet Wild 2 that are now being studied by two hundred scientists around the world. The spacecraft captured the samples during a close flyby of the comet in 2004 and returned them to Earth with a dramatic entry into the atmosphere early in 2006. The precious cargo of comet dust is being studied to determine new information about the origin of the Sun and planets. The comet formed at the edge of the solar system, beyond the orbit of Neptune, and is a sample of the material from which the solar system was formed. One of the most dramatic early findings from the mission was that a comet that formed in the coldest place in the solar system contained minerals that formed in the hottest place in the solar system. The comet samples are telling stories of fire and ice and they providing fascinating and unexpected information about our origins.
    Keywords: Lunar and Planetary Science and Exploration
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  • 47
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    Publication Date: 2011-08-24
    Description: Many ideas have been proposed for the origin of the Moon, but only one has stood the test of time: During the formation of Earth, about 4.5 billion years ago, our planet was hit by a projectile the size of Mars, leading to a close-in disk of molten material in earth orbit. From this material, our Moon formed in about a thousand years. I will explain how the properties of the Moon can be explained by this model and why the alternative ideas are either incorrect or highly improbable. I will also talk about some new developments in this area that come from a consideration of chemistry and isotopic measurements. Finally. I will talk about what we don't know and why the Moon is still an interesting place for further exploration.
    Keywords: Lunar and Planetary Science and Exploration
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  • 48
    Publication Date: 2011-08-24
    Description: Radio Doppler data from the Galileo spacecraft's encounter with Amalthea, one of Jupiter's small inner moons, on 5 November 2002 yield a mass of (2.08 +/- 0.15) x 10(18) kilograms. Images of Amalthea from two Voyager spacecraft in 1979 and Galileo imaging between November 1996 and June 1997 yield a volume of (2.43 +/- 0.22) x 10(6) cubic kilometers. The satellite thus has a density of 857 +/- 99 kilograms per cubic meter. We suggest that Amalthea is porous and composed of water ice, as well as rocky material, and thus formed in a cold region of the solar system, possibly not at its present location near Jupiter.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 308; 5726; 1291-3
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  • 49
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    Publication Date: 2011-08-24
    Description: The Cassini Orbiter spacecraft first skimmed through the tenuous upper atmosphere of Titan on 26 October 2004. This moon of Saturn is unique in our solar system, with a dense nitrogen atmosphere that is cold enough in places to rain methane, the feedstock for the atmospheric chemistry that produces hydrocarbons, nitrile compounds, and Titan's orange haze. The data returned from this flyby supply new information on the magnetic field and plasma environment around Titan, expose new facets of the dynamics and chemistry of Titan's atmosphere, and provide the first glimpses of what appears to be a complex, fluid-processed, geologically young Titan surface.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 308; 5724; 969-70
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  • 50
    Publication Date: 2005-04-25
    Description: Near-Earth asteroids are important exploration targets since they provide clues to the evolution of the solar system. They are also of interest since they present a clear danger to Earth. Our mission objective is to image the internal structure of two NEOs using radio reflection tomography (RRT) in order to explore the record of asteroid origin and impact evolution, and to test the fundamental hypothesis that some NEOs are rubble piles rather than consolidated bodies. Our mission s RRT technique is analogous to doing a CAT scan of the asteroid from orbit. Closely sampled radar echoes are processed to yield volumetric maps of mechanical and compositional boundaries, and to measure interior material dielectric properties. The RRT instrument is a radar that operates at 5 and 15 MHz with two 30-m (tip-to-tip) dipole antennas that are used in a cross-dipole configuration. The radar transmitter and receiver electronics have heritage from JPL's MARSIS contribution to Mars Express, and the antenna is similar to systems used in IMAGE and LACE missions. The 5-MHz channel is designed to penetrate greater than 1 km of basaltic rock, and 15-MHz penetrates a few hundred meters or more. In addition to RRT volumetric imaging, we use redundant color cameras to explore the surface expressions of unit boundaries, in order to relate interior radar imaging to what is observable from spacecraft imaging and from Earth. The camera also yields stereo color imaging for geology and RRT-related compositional analysis. Gravity and high fidelity geodesy are used to explore how interior structure is expressed in shape, density, mass distribution and spin. Ion thruster propulsion is utilized by Deep Interior to enable tomographic radar mapping of multiple asteroids. Within the Discovery AO scheduling parameters we identify two targets, S-type 1999 ND43 (approximately 500 m diameter) and V-type 3908 Nyx (approximately 1 km), asteroids whose compositions bracket the diversity of solar system materials that we are likely to encounter, from undifferentiated to highly evolved. The 5-15 MHz radar is capable of probing more primitive bodies (e.g. comets or C-types) that may be available given other launch schedules. 5 MHz radar easily penetrates, with the required SNR , greater than 1 km of basalt (a good analog for Nyx). Basalt has a greater loss tangent than expected for most asteroids, although iron-rich M-types are probably not appropriate targets. 15 MHz radar penetrates the outer approximately 100 m of rocky 1 km asteroids and the deep interiors of comets. Laboratory studies of the most common NE0 materials expected (S-, C- and V-type meteorite analogs) will commence in 2005.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Radar Investigations of Planetary and Terrestrial Environments; 71; LPI-Contrib-1231
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  • 51
    Publication Date: 2005-04-25
    Description: There are numerous challenges in successfully implementing and interpreting planetary ground penetrating radar (GPR) measurements. Many are due to substantial uncertainties in the target ground parameters and the intervening medium (i.e., the ionosphere). These uncertainties generate a compelling need for meaningful quantitative simulation of the planetary GPR problem. An accurate numerical model would enable realistic numerical GPR simulations using parameter regimes much broader than are possible in laboratory or field experiments. Parameters such as source bandwidth and power, surface and subsurface features, and ionospheric profiles could be rapidly iterated to understand their impact on GPR performance and the reliable interpretation of GPR data.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Radar Investigations of Planetary and Terrestrial Environments; 79; LPI-Contrib-1231
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  • 52
    Publication Date: 2005-08-22
    Description: Attempts to match the E asteroids with enstatite-rich meteorites universally conclude that the aubrites or enstatite chondrites are natural candidates, and accordingly conclude that E asteroids as a class are very water-poor. Accordingly, the highly reduced nature of typical enstatite-rich meteorites suggests that aqueous alteration was an improbable process on any E asteroid. However, there are spectroscopic observations of several E-class asteroids that suggest the presence there of hydrated phases. Examination of the Kaidun meteorite reveals the true situation.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Oxygen in Asteroids and Meteorites; LPI-Contrib-1267
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  • 53
    Publication Date: 2011-08-24
    Description: An interplanetary dust particle contains a submicrometer crystalline silicate aggregate of probable supernova origin. The grain has a pronounced enrichment in 18O/16O (13 times the solar value) and depletions in 17O/16O (one-third solar) and 29Si/28Si (〈0.8 times solar), indicative of formation from a type II supernova. The aggregate contains olivine (forsterite 83) grains 〈100 nanometers in size, with microstructures that are consistent with minimal thermal alteration. This unusually iron-rich olivine grain could have formed by equilibrium condensation from cooling supernova ejecta if several different nucleosynthetic zones mixed in the proper proportions. The supernova grain is also partially encased in nitrogen-15-rich organic matter that likely formed in a presolar cold molecular cloud.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 309; 5735; 737-41
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  • 54
    Publication Date: 2011-08-24
    Description: We quantified eight parent volatiles (H2O, C2H6, HCN, CO, CH3OH, H2CO, C2H2, and CH4) in the Jupiter-family comet Tempel 1 using high-dispersion infrared spectroscopy in the wavelength range 2.8 to 5.0 micrometers. The abundance ratio for ethane was significantly higher after impact, whereas those for methanol and hydrogen cyanide were unchanged. The abundance ratios in the ejecta are similar to those for most Oort cloud comets, but methanol and acetylene are lower in Tempel 1 by a factor of about 2. These results suggest that the volatile ices in Tempel 1 and in most Oort cloud comets originated in a common region of the protoplanetary disk.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 310; 5746; 270-4
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  • 55
    Publication Date: 2011-08-24
    Description: We report data from the Cassini radio and plasma wave instrument during the approach and first orbit at Saturn. During the approach, radio emissions from Saturn showed that the radio rotation period is now 10 hours 45 minutes 45 k 36 seconds, about 6 minutes longer than measured by Voyager in 1980 to 1981. In addition, many intense impulsive radio signals were detected from Saturn lightning during the approach and first orbit. Some of these have been linked to storm systems observed by the Cassini imaging instrument. Within the magnetosphere, whistler-mode auroral hiss emissions were observed near the rings, suggesting that a strong electrodynamic interaction is occurring in or near the rings.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science; Volume 307; 1255-1259
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  • 56
    Publication Date: 2011-08-24
    Description: Stratospheric temperatures on Saturn imply a strong decay of the equatorial winds with altitude. If the decrease in winds reported from recent Hubble Space Telescope images is not a temporal change, then the features tracked must have been at least 130 kilometers higher than in earlier studies. Saturn's south polar stratosphere is warmer than predicted from simple radiative models. The C/H ratio on Saturn is seven times solar, twice Jupiter's. Saturn's ring temperatures have radial variations down to the smallest scale resolved (100 kilometers). Diurnal surface temperature variations on Phoebe suggest a more porous regolith than on the jovian satellites.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 307; 5713; 1247-51
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  • 57
    Publication Date: 2013-08-31
    Description: The Mars Exploration Rovers Spirit and Opportunity investigated numerous craters since landing in Gusev crater (14.569degS, 175.473degE) and Meridiani Planum (1.946degS, 354.473degE) over the first 400 sols of their missions [1-4]. Craters at both sites are simple structures and vary in size and preservation state. Comparing observed and expected pristine morphology and using process-specific gradational signatures around terrestrial craters as a template [5-7] allows distinguishing gradation processes whose relative importance fundamentally differs from those responsible for most crater modification on the Earth.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on The Role of Volatile and Atmospheres on Martian Impact Craters; 42-43; LPI-Contrib-1273
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  • 58
    Publication Date: 2013-08-31
    Description: The Mars Exploration Rovers have provided a field geologist's perspective of impact craters in various states of degradation along their traverses at Gusev crater and Meridiani Planum. This abstract will describe the craters observed and changes to the craters that constrain the erosion rates and the climate [l]. Changes to craters on the plains of Gusev argue for a dry and desiccating environment since the Late Hesperian in contrast to the wet and likely warm environment in the Late Noachian at Meridiani in which the sulfate evaporites were deposited in salt-water playas or sabkhas.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on The Role of Volatile and Atmospheres on Martian Impact Craters; 40-41; LPI-Contrib-1273
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  • 59
    Publication Date: 2013-08-31
    Description: We present the results of the complete survey of Martian alluvial fans from 0-30 S, initiated by Moore and Howard. Nineteen impact craters contain alluvial fans. They are regionally grouped into three distinct areas. We present our initial results regarding their distribution and orientation in order to understand what controls their formation. Since alluvial fans are formed by water transport of sediment, these features record wetter episodes of Martian climate. In addition, their enigmatic distribution (in regional groups and in some craters, but not similar adjacent ones) needs to be understood, to see how regional geology, topographic characteristics, and/or climate influence their formation and distribution.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on The Role of Volatile and Atmospheres on Martian Impact Craters; LPI-Contrib-1273
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  • 60
    Publication Date: 2013-08-31
    Description: Evidence for the presence of liquid water early in Mars history continues to accumulate. The most recent evidence for liquid water being pervasive early in Mars history is the discoveries of sulfate and gypsum layers by the Mars Exploration Rovers and Mars Express. However, the presence of liquid water at the surface very early in Mars history presents a conundrum. The early sun was most likely approximately 75% fainter than it is today. About 65-70 degrees of greenhouse warming is needed to bring surface temperatures to the melting point of water. To date climate models have not been able to produce a continuously warm and wet early Mars. This may be a good thing as there is morphological and mineralogical evidence that the warm and wet period had to be relatively short and episodic. 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 (approximately 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: Workshop on The Role of Volatile and Atmospheres on Martian Impact Craters; LPI-Contrib-1273
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  • 61
    Publication Date: 2013-08-31
    Description: The martian southern highlands contain impact craters that display pristine to degraded morphologies, and preserve a record of degradation that can be attributed to fluvial, eolian, mass wasting, volcanic and impact-related processes. However, the relative degree of modification by these processes and the amounts of material contributed to crater interiors are not well constrained. Impact craters (D〉10 km) within Terra Cimmeria (0deg-60degS, 190deg-240degW), Terra Tyrrhena (0deg-30degS, 260deg-310degW) and Noachis Terra (20deg-50degS, 310deg-340degW) are being examined to better understand the degradational history and evolution of highland terrains. The following scientific objectives will be accomplished. 1) Determine the geologic processes that modified impact craters (and surrounding highland terrains). 2) Determine the sources (e.g. fluvial, lacustrine, eolian, mass wasting, volcanic, impact melt) and relative amounts of material composing crater interior deposits. 3) Document the relationships between impact crater degradation and highland fluvial systems. 4) Determine the spatial and temporal relationships between degradational processes on local and regional scales. And 5) develop models of impact crater (and highland) degradation that can be applied to these and other areas of the martian highlands. The results of this study will be used to constrain the geologic, hydrologic and climatic evolution of Mars and identify environments in which subsurface water might be present or evidence for biologic activity might be preserved.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on The Role of Volatile and Atmospheres on Martian Impact Craters; 77-78; LPI-Contrib-1273
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  • 62
    Publication Date: 2013-08-31
    Description: Impact craters on Mars have served as catchments for channel-eroding surface fluids, and hundreds of examples of candidate paleolakes are documented [1,2] (see Figure 1). Because these features show similarity to terrestrial shorelines, wave action has been hypothesized as the geomorphic agent responsible for the generation of these features [3]. Recent efforts have examined the potential for shoreline formation by wind-driven waves, in order to turn an important but controversial idea into a quantitative, falsifiable hypothesis. These studies have concluded that significant wave-action shorelines are unlikely to have formed commonly within craters on Mars, barring Earth-like weather for approx.1000 years [4,5,6].
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on The Role of Volatile and Atmospheres on Martian Impact Craters; LPI-Contrib-1273
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  • 63
    Publication Date: 2013-04-10
    Description: This presentation reviews the International Lunar Network (ILN) mission, a cooperative effort designed to coordinate individual lunar landers in a geophysical network on the lunar surface. The presentation also includes information on the geophysical network, mission operations, and recent accomplishments.
    Keywords: Lunar and Planetary Science and Exploration
    Type: M09-0817 , NLSI Lunar Science Forum; 21-23 Jul. 2009; Moffett Field, CA; United States
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  • 64
    Publication Date: 2013-08-31
    Description: Many regions of the martian surface are covered by fine-grained materials emplaced by volcanic, fluvial, or aeolian processes. These mantling deposits likely hide ancient channel systems (particularly at smaller scale lengths) and volcanic, impact, glacial, or shoreline features. Synthetic aperture radar (SAR) offers the capability to probe meters below the surface, with imaging resolution in the 10 s of m range, to reveal the buried terrain and enhance our understanding of Mars geologic and climate history. This presentation focuses on the practical applications of a Mars orbital SAR, methods for polarimetric and interferometric radar studies, and examples of such techniques for Mars-analog sites on the Moon and Earth.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Radar Investigations of Planetary and Terrestrial Environments; 25-26; LPI-Contrib-1231
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  • 65
    Publication Date: 2013-08-31
    Description: Radar interferometry is rapidly becoming one of the major applications of radar systems in Earth orbit. So far the 2000 flight of the Shuttle Radar Topographic Mission (SRTM) is the only dedicated U.S. radar to be flown for the collection of interferometric data, but enough has been learned from this mission and from the use of foreign partner radars (ERS-1/2, Radarsat, ENIVISAT and JERS-1) for the potential planetary applications of this technique to be identified. A recent workshop was organized by the Jet Propulsion Laboratory and the Southern California Earthquake Center (SCEC), and was held at Oxnard, CA, from October 20th - 22nd, 2004. At this meeting, the major interest was in terrestrial radar systems, but approx. 20 or the approx. 250 attendees also discussed potential applications of interferometric radar for the terrestrial planets. The primary foci were for the detection of planetary water, the search for active tectonism and volcanism and the improved topographic mapping. This abstract provides a summary of these planetary discussions at the Oxnard meeting.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Workshop on Radar Investigations of Planetary and Terrestrial Environments; 56-57; LPI-Contrib-1231
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  • 66
    Publication Date: 2013-08-29
    Description: To date, manned space flight has maintained the locus of control for the mission on the ground. Mission control performs tasks such as activity planning, system health management, resource allocation, and astronaut health monitoring. Future exploration missions require the locus of control to shift to on-board due light speed constraints and potential loss of communication. The lunar campaign must begin to utilize a shared control approach to validate and understand the limitations of the technology allowing astronauts to oversee and direct aspects of operation that require timely decision making. Crew-centered Operations require a system-level approach that integrates multiple technologies together to allow a crew-prime concept of operations. This paper will provide an overview of the driving mission requirements, highlighting the limitations of existing approaches to mission operations and identifying the critical technologies necessary to enable a crew-centered mode of operations. The paper will focus on the requirements, trade spaces, and concepts for fulfillment of this capability. The paper will provide a broad overview of relevant technologies including: Activity Planning and Scheduling; System Monitoring; Repair and Recovery; Crew Work Practices.
    Keywords: Lunar and Planetary Science and Exploration
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  • 67
    Publication Date: 2013-08-29
    Description: The 1/14/04 USA Space Exploratiofltilization Initiative invites all Space-faring Nations, all Space User Groups in Science, Space Entrepreneuring, Advocates of Robotic and Human Space Exploration, Space Tourism and Colonization Promoters, etc., to join an International Space Partnership. With more Space-faring Nations and Space User Groups each year, such a Partnership would require Multi-year (35 yr.-45 yr.) Space Mission Planning. With each Nation and Space User Group demanding priority for its missions, one needs a methodology for obiectively selecting the best mission sequences to be added annually to this 45 yr. Moving Space Mission Plan. How can this be done? Planners have suggested building a Reusable, Sustainable, Space Transportation Infrastructure (RSSn) to increase Mission synergism, reduce cost, and increase scientific and societal returns from this Space Initiative. Morgenthaler and Woodcock presented a Paper at the 55th IAC, Vancouver B.C., Canada, entitled Constrained Optimization Models For Optimizing Multi - Year Space Programs. This Paper showed that a Binary Integer Programming (BIP) Constrained Optimization Model combined with the NASA ATLAS Cost and Space System Operational Parameter Estimating Model has the theoretical capability to solve such problems. IAA Commission III, Space Technology and Space System Development, in its ACADEMY DAY meeting at Vancouver, requested that the Authors and NASA experts find several Space Exploration Architectures (SEAS), apply the combined BIP/ATLAS Models, and report the results at the 56th Fukuoka IAC. While the mathematical Model is in Ref.[2] this Paper presents the Application saga of that effort.
    Keywords: Lunar and Planetary Science and Exploration
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  • 68
    Publication Date: 2019-04-04
    Description: The lunar surface is covered with a thick layer of sub-micron/micron size dust grains formed by meteoritic impact over billions of years. The fine dust grains are levitated and transported on the lunar surface, as indicated by the transient dust clouds observed over the lunar horizon during the Apollo 17 mission. Theoretical models suggest that the dust grains on the lunar surface are charged by the solar UV radiation as well as the solar wind. Even without any physical activity, the dust grains are levitated by electrostatic fields and transported away from the surface in the near vacuum environment of the Moon. The current dust charging and levitation models, however, do not fully explain the observed phenomena. Since the abundance of dust on the Moon s surface with its observed adhesive characteristics has the potential of severe impact on human habitat and operations and lifetime of a variety of equipment, it is necessary to investigate the charging properties and the lunar dust phenomena in order to develop appropriate mitigating strategies. Photoelectric emission induced by the solar UV radiation with photon energies higher than the work function of the grain materials is recognized to be the dominant process for charging of the lunar dust, and requires measurements of the photoelectric yields to determine the charging and equilibrium potentials of individual dust grains. In this paper, we present the first laboratory measurements of the photoelectric efficiencies and yields of individual sub-micron/micron size dust grains selected from sample returns of Apollo 17, and Luna 24 missions, as well as similar size dust grains from the JSC-1 simulants. The measurements were made on a laboratory facility based on an electrodynamic balance that permits a variety of experiments to be conducted on individual sub-micron/micron size dust grains in simulated space environments. The photoelectric emission measurements indicate grain size dependence with the yield increasing by an order of magnitude for grains of sub-micron to several micron size radii, at which it reaches asymptotic values. The yield for large size grains is found to be more than an order of magnitude higher than the bulk measurements on lunar fines reported in the literature.
    Keywords: Lunar and Planetary Science and Exploration
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  • 69
    Publication Date: 2017-10-02
    Description: The composition of material condensed in the outer solar system is very dependent on the state of carbon and oxygen in the solar or circumplanetary nebula, since oxygen is the dominant solid-forming element in a solar composition gas (in the form of silicates and water ice), and carbon is about half as abundant. Past discussions of solid material formed in these regions have focused on differences expected between material formed near giant planets where carbon is generally expected to be in the reduced, CH4, form and material formed in the outer protoplanetary solar nebula where CO is believed to be the dominant form [1]. The composition and expected density of these materials are quite sensitive to the C and O solar abundances in all these models. We discuss here the effects of recently suggested modifications to solar abundances on the interpretation of the mean densities for satellites in the Saturn system.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 10; LPI-Contrib-1234-Pt-10
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  • 70
    Publication Date: 2017-10-02
    Description: The Panoramic Cameras (Pancam) on the Spirit and Opportunity Mars Exploration Rovers have acquired multispectral reflectance observations of rocks and soils at different incidence, emission, and phase angles that will be used for photometric modeling of surface materials. Phase angle coverage at both sites extends from approx. 0 deg. to approx. 155 deg.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 10; LPI-Contrib-1234-Pt-10
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  • 71
    Publication Date: 2017-10-02
    Description: The seven known Martian nakhlites are Nakhla, Lafayette, Governador Valadares, and four recent finds from hot and cold deserts: MIL03346 from the Transantarctic Mountains, a paired group from the Yamato Mountains (Y000593, Y000749, and Y000802, and two from Morocco (NWA998 and NWA817. Radiometric ages (Sm-Nd, Rb-Sr, U-Pb, and Ar-Ar) for the first three nakhlites, along with Chassigny, fall in the range of 1.19-1.37 Gyr and may suggest a common formation age. These meteorites also show very similar cosmic-ray (space) exposure ages, suggesting a single ejection event from Mars. The ages for nakhlites are different from those of Martian shergottites, whose radiometric ages vary by nearly a factor of three (approx. 165-475 Myr) and whose space exposure ages vary over a factor of approx. 20. Shergottite ages suggest that multiple locations on the Martian surface have been sampled, whereas nakhlite data imply sampling of only one Mars surface location. Because older Martian surfaces are expected to be more abundant, it seems surprising that all nakhlites would represent only one Martian impact event. To address this issue, we are measuring the (39)Ar-(40)Ar ages of Y-000593, NWA-998, Nakhla, and MIL-03346, and the space (CRE) exposure age of NWA998. Additional information is included in the original extended abstract.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 7; LPI-Contrib-1234-Pt-7
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  • 72
    Publication Date: 2017-10-02
    Description: We modeled the solar phase curves of the moon at a series of wavelengths using the full disk telescopic observations [1]. We endeavored to keep the database self-contained, that is, to use the values derived for the solar magnitude and phase curves of the disk-integrated [1]. These observations were made in a suite of 10 narrowband filters between 0.315 microns and 1.06 microns, and in the broad band Johnson UBV filters, as part of a larger program to obtain photoelectric photometry of the larger planets. Two aspects of the lunar observations are unique. First, the observations cover phase angles from 6deg through 120deg. More importantly, the observers used a special 20-mm diameter f/15 fused quartz lens constructed solely for this purpose. The lens reduced the whole lunar image in the focal plane to a size comparable to the planets observed as part of the same program. This image was fed directly into the photometer. Thus, these observations constitute the only existing set of phase curves of the entire lunar disk over a range of wavelengths. Table 1 lists the values of the Hapke model parameters which fit the data. Figure 1 is an example of the model fits to the data.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 4; LPI-Contrib-1234-Pt-4
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  • 73
    Publication Date: 2017-10-02
    Description: Introduction: An overarching geologic theory, GEOMARS, coherently explains many otherwise anomalous aspects of the geological history of Mars. Premises for a theory of martian geologic evolution include: (1) Mars is a water-rich terrestrial planet, (2) terrestrial planets should evolve through progressive stages of dynamical history (accretion, differentiation, tectonism) and mantle convection (magma ocean, plate tectonism, stagnant lid), and (3) the early history of Earth affords an analogue to the evolution of Mars. The theory describes the following major stages of evolution for Mars (from oldest to youngest): Stage 1 - shortly after accretion, Mars differentiates to a liquid metallic core, a mantle boundary (MBL) of high-pressure silicate mineral phases, upper mantle, magma ocean, thin komatiic crust, and convecting steam atmosphere; Stage 2- Mars cools to condense its steam atmosphere and transform its mode of mantle convection to plate tectonism; subduction of waterrich oceanic crust initiates arc volcanism and transfers water, carbonates and sulfates to the mantle; Stage 3 - the core dynamo initiates, and the associated magnetosphere leads to conditions conducive to the development of near-surface life and photosynthetic production of oxygen; Stage 4 - accretion of thickened, continental crust and subduction of hydrated oceanic crust to the mantle boundary layer and lower mantle of Mars occurs; Stage 5 - the core dynamo stops during Noachian heavy bombardment while plate tectonism continues; Stage 6 - initiation of the Tharsis superplume (approx. between 4.0 and 3.8Ga) occurs, and Stage 7 - the superlume phase (stagnant-lid regime) of martian planetary evolution with episodic phases of volcanism and water outflows continues into the present. The GEOMARS Theory is testable through a multidisciplinary approach, including utilizing GRS-based information. Based on a synthesis of published geologic, paleohydrologic, topographic, geophysical, spectral, and elemental information, we have defined geologic provinces that represent significant windows into the geological evolution of Mars, unfolding the GEOMARS Theory and forming the basis for interpreting GRS data.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 4; LPI-Contrib-1234-Pt-4
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  • 74
    Publication Date: 2017-10-02
    Description: The first of two relatively close Iapetus flybys in Cassini's primary mission occured on Dec 31, 2004 18:49 UTC near apoapsis from orbit "B" to "C" at an altitude of approximately 123,400 km over the northern leading hemisphere, resulting in a minimum pixel scale of 740 m for the ISS narrow angle camera (NAC). Data revealed details of a greater than 1300-km-long ridge that had been discovered just one week earlier in optical navigation images. Individual mountains within the western part of the ridge reach heights of approximately 20 km over surrounding terrain. The data set provides constraints on the origin of the albedo dichotomy. It appears very likely that the dark material is overlying an ice crust, but no evidence for emplacement of dark material via surface flows is apparent. Instead, signs for dark-material emplacement through processes that included ballistic transportation are visible. No bright-floor ("punch-through") craters have been found on the dark hemisphere. The ridge discovery may revive the idea of an endogenic origin of the dark side.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 4; LPI-Contrib-1234-Pt-4
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  • 75
    Publication Date: 2017-10-02
    Description: To better understand the behavior of the Mars CO2 ice seasonal polar caps, and in particular interpret the the Mars Express Omega observations of the recession of the northern seasonal cap, we present some simulations of the Martian Climate/CO2 cycle/ water cycle as modeled by the Laboratoire de Meteorologie Dynamique (LMD) global climate model.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 6; LPI-Contrib-1234-Pt-6
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  • 76
    Publication Date: 2017-10-02
    Description: Introduction: The Mars Global Surveyor spacecraft has completed three 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 [1], and intriuging in both its global distribution and geometric properties [2,3,4,5]. We present here a new map of the magnetic field with an order of magnitude increased sensitivity to crustal magnetization. The map is assembled from 〉 2 full years of MGS night-side observations. The increased sensitivity and spatial resolution afforded by this new map invites geologic interpretation akin to that here-to-for reserved for aeromagnetic and ship surveys on Earth.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 3; LPI-Contrib-1234-Pt-3
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  • 77
    Publication Date: 2017-10-02
    Description: The Murchison and Murray meteorites are the best-characterized carbonaceous meteorites with respect to organic chemistry and are generally used as references for organic compounds in extraterrestrial material. Among the classes of organic compounds found in these meteorites are amino acids, carboxylic acids, hydroxy acids, purines, and pyrimidines. Such compounds, important in contemporary biochemistry, are thought to have been delivered to the early Earth in asteroids and comets and may have played a role in early life and/or the origin of life. Absent among (today's) critically important biological compounds reported in carbonaceous meteorites are keto acids, i.e., pyruvic acid, acetoacetic acid, and higher homologs. These compounds are key intermediates in such critical processes as glycolysis and the citric acid cycle. In this study several individual meteoritic keto acids were identified by gas chromatography-mass spectrometry (GC-MS) (see figure below). All compounds were identified as their trimethylsilyl (TMS), isopropyl ester (ISP), and tert-butyldimethylsilyl (tBDMS) derivatives. In general, the compounds follow the abiotic synthesis pattern of other known meteorite classes of organic compounds [1,2]: a general decrease in abundance with increasing carbon number within a class of compounds and many, if not all, possible isomers present at a given carbon number. The majority of the shown compounds was positively identified by comparison of their mass spectra to commercially available standards or synthesized standards.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 3; LPI-Contrib-1234-Pt-3
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  • 78
    Publication Date: 2017-10-02
    Description: LAP 02205 is a 1.2 kg lunar mare basalt meteorite found in the Lap Paz ice field of Antarctica in 2002 [1]. Four similar meteorites were also found within the same region [1] and all five have a combined mass of 1.9 kg (LAP 02224, LAP 02226, LAP 02436 and LAP 03632, hereafter called the LAP meteorites). The LAP meteorites all contain a similar texture, mineral assemblage, and composition. A lunar origin for these samples comes from O isotopic data for LAP 02205 [1], Fe/Mn ratios of pyroxenes [1-5], and the presence of distinct lunar mineralogy such as Fe metal and baddeleyite. The LAP meteorites may represent an area of the Moon, which has never been sampled by Apollo missions, or by other lunar meteorites. The data from this study will be used to compare the LAP meteorites to Apollo mare basalts and lunar basaltic meteorites, and will ultimately help to constrain their origin.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 3; LPI-Contrib-1234-Pt-3
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  • 79
    Publication Date: 2017-10-02
    Description: The STARDUST sample return capsule is anticipated to provide 500-1000 cometary particles 15 m in size. These were collected during the 340 km flyby of Comet P/Wild-2 and impacted the aerogel collection medium at a relative velocity of approx. 6.1 /kms. Hypervelocity impact studies suggest that some fraction of the original organic inventory of collected particles ought to remain intact, although there is likely to be a significant amount of devolatilization and disassociation of the lower mass organic fraction.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 3; LPI-Contrib-1234-Pt-3
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  • 80
    Publication Date: 2017-10-02
    Description: Addressable Reconfigurable Technology (ART) based structures: Mission Concepts based on Addressable Reconfigurable Technology (ART), originally studied for future ANTS (Autonomous Nanotechnology Swarm) Space Architectures, are now being developed as rovers for nearer term use in lunar and planetary surface exploration. The architecture is based on the reconfigurable tetrahedron as a building block. Tetrahedra are combined to form space-filling networks, shaped for the required function. Basic structural components are highly modular, addressable arrays of robust nodes (tetrahedral apices) from which highly reconfigurable struts (tetrahedral edges), acting as supports or tethers, are efficiently reversibly deployed/stowed, transforming and reshaping the structures as required.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 3; LPI-Contrib-1234-Pt-3
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  • 81
    Publication Date: 2017-10-02
    Description: Introduction: The observed Springtime (Ls approx. 200) surface albedo in the Martian southern polar region is shown in Figure 1. In general, the hemisphere west of Hellas is marked by relatively high values of surface albedo. In contrast, the hemisphere east of Hellas contains extensive regions of very low surface albedo. One of the brightest features within the western hemisphere is the South Pole Residual Cap (SPRC). The dark region, which dominates the eastern hemisphere, is the "Cryptic" region[1]. The nature of the SPRC has been the source of considerable debate since its identification as CO2 ice by the Viking spacecraft. Two fundamental questions still exist regarding the SPRC s formation, location and stability. First, why is the SPRC offset from the geographic pole? There are no local topographic features or surface properties that can account for the offset in the SPRC. Second, does the SPRC represent a large or a small reservoir of CO2? If the former, then it could possibly buffer the surface pressure. If the latter, then the SPRC may not survive every year.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 3; LPI-Contrib-1234-Pt-3
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  • 82
    Publication Date: 2017-10-02
    Description: We model the interior of Rhea based on observational constraints and the results from geodynamical models available in the literature. Ten main types of models are defined, depending on the presence or absence of a high-pressure ice layer (ice II), and the extent of separation of the rock component from the volatiles. We present degree-two gravity components computed for each of these models in order to assess which properties of the interior are likely to be inferred from Cassini radio science measurements scheduled on November 26, 2005.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 3; LPI-Contrib-1234-Pt-3
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  • 83
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    In:  CASI
    Publication Date: 2017-10-02
    Description: The early bombardment revealed in the larger impact craters and basins on the moon was a major planetary process that affected all bodies in the inner solar system, including the Earth and Mars. Understanding the nature and timing of this bombardment is a fundamental planetary problem. The surface density of lunar impact craters within a given size range on a given lunar surface is a measure of the age of that surface relative to other lunar surfaces. When crater densities are combined with absolute radiometric ages determined on lunar rocks returned to Earth, the flux of large lunar impactors through time can be estimated. These studies suggest that the flux of impactors producing craters greater than 1 km in diameter has been approximately constant over the past approx. 3 Gyr. However, prior to 3.0 - 3.5 Gyr the impactor flux was much larger and defines an early bombardment period. Unfortunately, no lunar surface feature older than approx. 4 Gyr is accurately dated, and the surface density of craters are saturated in most of the lunar highlands. This means that such data cannot define the impactor flux between lunar formation and approx. 4 Gyr ago.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 2; LPI-Contrib-1234-Pt-2
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  • 84
    Publication Date: 2017-10-02
    Description: The debate about fossil life on Mars includes the origin of magnetites of specific sizes and habits in the siderite-rich portions of the carbonate spheres in ALH 84001 [1,2]. Specifically [2] were able to demonstrate that inorganic synthesis of these compositionally zoned spheres from aqueous solutions of variable ion-concentrations is possible. They further demonstrated the formation of magnetite from siderite upon heating at 550 C under a Mars-like CO2-rich atmosphere according to 3FeCO3 = Fe3O4 + 2CO2 + CO [3] and they postulated that the carbonates in ALH 84001 were heated to these temperatures by some shock event. The average shock pressure for ALH 84001, substantially based on the refractive index of diaplectic feldspar glasses [3,4,5] is some 35-40 GPa and associated temperatures are some 300-400 C [4]. However, some of the feldspar is melted [5], requiring local deviations from this average as high as 45-50 GPa. Indeed, [5] observes the carbonates in ALH 84001 to be melted locally, requiring pressures in excess of 60 GPa and temperatures 〉 600 C. Combining these shock studies with the above inorganic synthesis of zoned carbonates it seems possible to produce the ALH 84001 magnetites by the shock-induced decomposition of siderite.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 2; LPI-Contrib-1234-Pt-2
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  • 85
    Publication Date: 2017-10-02
    Description: Methane has been detected in the martian atmosphere at a concentration of approximately 10 ppb. The lifetime of such methane against decomposition by solar radiation is approximately 300 years, strongly suggesting that methane is currently being released to the atmosphere. By analogy to Earth, possible methane sources on Mars include active volcanism, hot springs, frozen methane clathrates, thermally-matured sedimentary organic matter, and extant microbial metabolism. The discovery of any one of these sources would revolutionize our understanding of Mars.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 1; LPI-Contrib-1234-Pt-1
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  • 86
    Publication Date: 2017-10-02
    Description: Results are presented from the Cassini radio and plasma wave instrument during the approach and first few orbits around Saturn. During the approach the intensity modulation of Saturn Kilometric Radiation (SKR) showed that the radio rotation period of Saturn has increased to 10 hr 45 min plus or minus 36 sec, about 6 min longer than measured by Voyager in 1980-81. Also, many intense impulsive radio signals called Saturn Electrostatic Discharges (SEDs) were detected from saturnian lightning, starting as far as 1.08 AU from Saturn, much farther than terrestrial lightning can be detected from Earth. Some of the SED episodes have been linked to cloud systems observed in Saturn s atmosphere by the Cassini imaging system. Within the magnetosphere plasma wave emissions have been used to construct an electron density profile through the inner region of the magnetosphere. With decreasing radial distance the electron density increases gradually to a peak of about 100 per cubic centimeter near the outer edge of the A ring, and then drops precipitously to values as low as .03 per cubic centimeter over the rings. Numerous nearly monochromatic whistler-mode emissions were observed as the spacecraft passed over the rings that are believed to be produced by meteoroid impacts on the rings. Whistlermode emissions, similar to terrestrial auroral hiss were also observed over the rings, indicating that an electrodynamic interaction, similar to auroral particle acceleration, may be occurring in or near the rings. During the Titan flybys Langmuir probe and plasma wave measurements provided observations of the density and temperature in Titan's ionosphere.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 7; LPI-Contrib-1234-Pt-7
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  • 87
    Publication Date: 2017-10-02
    Description: The valley networks found on the slopes of Martian volcanoes represent an interesting subset of the Martian valley networks. Not only do the volcanoes constrain the possible geologic settings, they also provide a window into Martian valley development through time, as the volcanoes formed throughout the geologic history of Mars. Here I take another look at this intriguing subset of networks by revisiting conclusions reached in my earlier studies using the Viking imagery and the valleys on Hawaii as an analog. I then examine more recent datasets.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 7; LPI-Contrib-1234-Pt-7
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  • 88
    Publication Date: 2017-10-02
    Description: Mars Exploration Rover Opportunity discovered sedimentary dirty evaporites in Meridiani Planum that were deposited in salt-water playas or sabkhas in the Noachian, roughly coeval with a variety of geomorphic indicators (valley networks, degraded craters and highly eroded terrain) of a possible early warmer and wetter environment. In contrast, the cratered plains of Gusev that Spirit has traversed (exclusive of the Columbia Hills) have been dominated by impact and eolian processes and a gradation history that argues for a dry and desiccating environment since the Late Hesperian. This paper reviews the surficial geology and gradation history of the plains in Gusev crater as observed along the traverse by Spirit that supports this climate change from the two landing sites on Mars.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 7; LPI-Contrib-1234-Pt-7
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  • 89
    Publication Date: 2017-10-02
    Description: The Huygens Probe descended through Titan s atmosphere on January 14, 2005. The Descent Imager/Spectral Radiometer (DISR) instrument made optical measurements which constrain the nature and vertical distribution and of the aerosols in the atmosphere.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 4; LPI-Contrib-1234-Pt-4
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  • 90
    Publication Date: 2017-10-02
    Description: Determination of atmospheric and surface elemental and molecular composition of various solar system bodies is essential to the development of a firm understanding of the origin and evolution of the solar system. Furthermore, such data is needed to address the intriguing question of whether or not life exists or once existed elsewhere in the Solar System. As such, these measurements are among the primary scientific goals of NASA s current and future planetary missions. In recent years, significant progress toward both miniaturization and field portability of in situ analytical separation and detection devices have been made with future planetary explorations in mind. However, despite all these advances, accurate in situ identification of atmospheric and surface compounds remains a big challenge. In response to that we are developing various hardware and software tools which would enable us to uniquely identify species of interest in a complex chemical environment.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 4; LPI-Contrib-1234-Pt-4
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  • 91
    Publication Date: 2017-10-02
    Description: The Composite Infrared Spectrometer (CIRS) is a remote-sensing Fourier Transform Spectrometer on the Cassini orbiter that measures thermal radiation over two decades in wavenumber, from 10 to 1400 /cm (1 mm to 7 microns), with a spectral resolution that can be set from 0.5 to 15.5 /cm. The far infrared portion of the spectrum (10-600 /cm) is measured with a polarizing interferometer having thermopile detectors with a common 4-mrad field of view. The middle infrared portion is measured with a traditional Michelson interferometer having two focal planes (600-1100 /cm, 1100-1400 cm). Each focal plane is composed of a 1x10 array of HgCdTe detectors, each detector having a 0.3-mrad field of view. More complete descriptions of the instrument and investigation are given in and. A brief description of the first results from observations through the Saturn orbital insertion period can be found in.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 6; LPI-Contrib-1234-Pt-6
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  • 92
    Publication Date: 2017-10-02
    Description: Several teams have recently reported the detection of methane in the Martian atmosphere [1-3]. Although the detection is at the limit of the instrument capacities, one of the most surprising findings by some of these teams is the apparent strong spatial variations observed in spite of the fact that a gas like methane was expected to have a relatively long lifetime in the Martian atmosphere and thus be well mixed. To better quantitatively understand how such spatial variations can form on Mars, we have performed multiple realistic 3D general circulation model simulations in which gases with different sources, lifetime or sinks are released and transported in the Martian atmosphere.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 6; LPI-Contrib-1234-Pt-6
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  • 93
    Publication Date: 2017-10-02
    Description: Introduction: The meteorite record contains several examples of minerals that would not persist if allowed to come to equilibrium with a cooling gas of solar composition. This includes all minerals in CAIs and AOAs. Their survival is generally ascribed to physical removal of the object from the gas (isolation into a large parent object, or ejection by a stellar wind), but could also result from outward radial diffusion into cooler regions, which we discuss here. Accretion of CAIs into planetesimals has also been relied on to preserve them against loss into the sun. However, this suggestion faces several objections. Simple outward diffusion in turbulence has recently been modeled in some detail, and can preserve CAIs against loss into the sun [2]. Naturally, outward radial diffusion in turbulence is slower than immediate ejection by a stellar wind, which occurs on an orbital timescale. Here we ask whether these different transport mechanisms can be distinguished by nonequilibrium mineralogy, which provides a sort of clock. Our application here is to one aspect of CAI mineralogy - the Wark-Lovering rims (WLR); even more specifically, to alteration of one layer in the WLR sequence from melilite (Mel) to anorthite (An).
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 3; LPI-Contrib-1234-Pt-3
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  • 94
    Publication Date: 2017-10-02
    Description: Hellas basin, the largest well-preserved impact structure on the Martian surface, is Mars deepest depositional sink and has long been recognized as a source for global dust storms. The basin and surrounding highlands span a wide range in latitude and elevation, exhibit landforms shaped by a diversity of geologic processes, and preserve exposures of Noachian, Hesperian, and Amazonian units. Geologically contemporaneous volcanism and volatile-driven activity in the circum-Hellas highlands provide resources for potential Martian life. Hellas is a geologically significant region for evaluating volatile abundance, distribution and cycling and changes in surface conditions on Mars. Current work integrates geologic studies of the basin floor and east rim using Viking Orbiter, Mars Global Surveyor, and Mars Odyssey datasets to provide a synthesis of the history of volatiles in the region.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 3; LPI-Contrib-1234-Pt-3
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  • 95
    Publication Date: 2017-10-02
    Description: Introduction: The water-content of Martian magmas is a topic of debate among researchers. Some Martian basalts are characterized with melt inclusions of biotite, apatite and amphibole; phases typically associated with hydration reactions on Earth [1-3]. However, the H-content of melt inclusions from these basalts is low, and bulk-rock H2O-contents range from a meager 0.013 to 0.035 wt. % in Shergotty [4]. Nonetheless, researchers note that low present-day water contents do not preclude a once hydrous past [5]. Since light lithophile elements (LLE), such as Li and B, partition into aqueous fluids at T 〉 350 C, workers proposed that Li-B depletions in pyroxene rims of Nakhlite and Shergottite basalts reflect the loss of several weight percent water from Martian magmas during crystallization [6]. Since similar depletions were observed in pyroxene rims from completely dry lunar basalts, it is likely that alternative mechanisms also contribute to the distribution of elements such as Li and B [7]. Given that many Martian basalts have experienced considerable shock pressures (15-45 GPa), it is possible that shock and subsequent thermal metamorphism may have influenced the volatile element records of these basalts [8]. In order to better understand the distribution of Li and B, we are studying the effects of crystal chemistry, shock pressure, and thermal metamorphism in pyroxenes from lunar basalts. Below, we discuss results from experimentally shocked and thermally metamorphosed Apollo 11, 10017 (A-11) and Apollo 17, 75035 (A-17) basalts.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 3; LPI-Contrib-1234-Pt-3
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  • 96
    Publication Date: 2017-10-02
    Description: We surveyed the characteristic of non-organized soils at Gusev crater at microscale and macroscale in four main traverse regions: (1) Landing site to Bonneville crater; (2) Bonneville to West Spur; (3) the West Spur region; and (4) the Columbia Hills up to sol 363. Non-organized soils are defined as soils traversed by Spirit that do not include drifts, ripples, or dunes.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 3; LPI-Contrib-1234-Pt-3
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  • 97
    Publication Date: 2017-10-02
    Description: We are engaged in a NASA Vision Mission study, called Palmer Quest after the American Antarctic explorer Nathaniel Palmer, to assess the presence of life and evaluate the habitability of the basal domain of the Mars polar caps. We address this goal through four objectives: 1. Determine the presence of amino acids, nutrients, and geochemical heterogeneity in the ice sheet. 2. Quantify and characterize the provenance of the amino acids in Mars ice. 3. Assess the stratification of outcropped units for indications of habitable zones. 4. Determine the accumulation of ice, mineralogic material, and amino acids in Mars ice caps over the present epoch. Because of the defined scientific goal for the vision mission, the Palmer Quest focus is astrobiological; however, the results of the study make us optimistic that aggressive multi-platform in-situ missions that address a wide range of objectives, such as climate change, can be supported by variations of the approach used on this mission. Mission Overview: The Palmer Quest baseline
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 3; LPI-Contrib-1234-Pt-3
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  • 98
    Publication Date: 2017-10-02
    Description: Inspection of the interior of the Genesis science canister after recovery in Utah, and subsequently at JSC, revealed a darkening on the aluminum canister shield and other canister components. There has been no such observation of film contamination on the collector surfaces, and preliminary spectroscopic ellipsometry measurements support the theory that the films observed on the anodized aluminum components do not appear on the collectors to any significant extent. The Genesis Science Team has made an effort to characterize the thickness and composition of the brown stain and to determine if it is associated with molecular outgassing.Detailed examination of the surfaces within the Genesis science canister reveals that the brown contamination is observed to varying degrees, but only on surfaces exposed in space to the Sun and solar wind hydrogen. In addition, the materials affected are primarily composed of anodized aluminum. A sharp line separating the sun and shaded portion of the thermal closeout panel is shown. This piece was removed from a location near the gold foil collector within the canister. Future plans include a reassembly of the canister components to look for large-scale patterns of contamination within the canister to aid in revealing the root cause.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 2; LPI-Contrib-1234-Pt-2
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  • 99
    Publication Date: 2017-10-02
    Description: The Mars Rover-missions demonstrate that there are accessible Martian sulfate deposits (evaporites) [1]. These sedimentary rocks could indicate influence of past or present biotic processes even in the absence of traces of extraterrestrial life. We evaluate the potential of the analysis of mass independent isotope fractionation of oxygen in sulfate as a biosignature.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 2; LPI-Contrib-1234-Pt-2
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    Publication Date: 2017-10-02
    Description: The Cassini Imaging Science System (ISS) has been returning images of Titan, along with other Saturnian satellites. Images taken through the 938 nm methane window see down to Titan's surface. One of the purposes of the Cassini mission is to investigate possible fluid cycling on Titan. Lemniscate features shown recently and radar evidence of surface flow prompted us to consider theoretically the creation by methane fluid flow of streamlined forms on Titan. This follows work by other groups in theoretical consideration of fluid motion on Titan's surface.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 2; LPI-Contrib-1234-Pt-2
    Format: application/pdf
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