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Sample records for spirit gusev crater

  1. Textures of the soils and rocks at Gusev crater from Spirit's Microscopic Imager

    DEFF Research Database (Denmark)

    Herkenhoff, K.E.; Squyres, S.W.; Arvidson, R.

    2004-01-01

    The Microscopic Imager on the Spirit rover analyzed the textures of the soil and rocks at Gusev crater on Mars at a resolution of 100 micrometers. Weakly bound agglomerates of dust are present in the soil near the Columbia Memorial Station. Some of the brushed or abraded rock surfaces show igneous...

  2. Textures of the soils and rocks at Gusev crater from Spirit's Microscopic Imager

    DEFF Research Database (Denmark)

    Herkenhoff, K.E.; Squyres, S.W.; Arvidson, R.

    2004-01-01

    The Microscopic Imager on the Spirit rover analyzed the textures of the soil and rocks at Gusev crater on Mars at a resolution of 100 micrometers. Weakly bound agglomerates of dust are present in the soil near the Columbia Memorial Station. Some of the brushed or abraded rock surfaces show igneou...

  3. Mars exploration rover geologic traverse by the spirit rover in the plains of Gusev crater, Mars

    Science.gov (United States)

    Crumpler, L.S.; Squyres, S. W.; Arvidson, R. E.; Bell, J.F.; Blaney, D.; Cabrol, N.A.; Christensen, P.R.; DesMarais, D.J.; Farmer, J.D.; Fergason, R.; Golombek, M.P.; Grant, F.D.; Grant, J. A.; Greeley, R.; Hahn, B.; Herkenhoff, K. E.; Hurowitz, J.A.; Knudson, A.T.; Landis, G.A.; Li, R.; Maki, J.; McSween, H.Y.; Ming, D. W.; Moersch, J.E.; Payne, M.C.; Rice, J.W.; Richter, L.; Ruff, S.W.; Sims, M.; Thompson, S.D.; Tosca, N.; Wang, A.; Whelley, P.; Wright, S.P.; Wyatt, M.B.

    2005-01-01

    The Spirit rover completed a 2.5 km traverse across gently sloping plains on the floor of Gusev crater from its location on the outer rim of Bonneville crater to the lower slopes of the Columbia Hills, Mars. Using the Athena suite of instruments in a transect approach, a systematic series of overlapping panoramic mosaics, remote sensing observations, surface analyses, and trenching operations documented the lateral variations in landforms, geologic materials, and chemistry of the surface throughout the traverse, demonstrating the ability to apply the techniques of field geology by remote rover operations. Textures and shapes of rocks within the plains are consistent with derivation from impact excavation and mixing of the upper few meters of basaltic lavas. The contact between surrounding plains and crater ejecta is generally abrupt and marked by increases in clast abundance and decimeter-scale steps in relief. Basaltic materials of the plains overlie less indurated and more altered rock types at a time-stratigraphic contact between the plains and Columbia Hills that occurs over a distance of one to two meters. This implies that regional geologic contacts are well preserved and that Earth-like field geologic mapping will be possible on Mars despite eons of overturn by small impacts. ?? 2005 Geological Society of America.

  4. Use of Geochemistry Data Collected by the Mars Exploration Rover Spirit in Gusev Crater to Teach Geomorphic Zonation through Principal Components Analysis

    Science.gov (United States)

    Rodrigue, Christine M.

    2011-01-01

    This paper presents a laboratory exercise used to teach principal components analysis (PCA) as a means of surface zonation. The lab was built around abundance data for 16 oxides and elements collected by the Mars Exploration Rover Spirit in Gusev Crater between Sol 14 and Sol 470. Students used PCA to reduce 15 of these into 3 components, which,…

  5. Pancam multispectral imaging results from the Spirit Rover at Gusev Crater

    Science.gov (United States)

    Bell, J. F., III; Squyres, S. W.; Arvidson, R. E.; Arneson, H. M.; Bass, D.; Blaney, D.; Cabrol, N.; Calvin, W.; Farmer, J.; Farrand, W. H.; hide

    2004-01-01

    Panoramic Camera images at Gusev crater reveal a rock-strewn surface interspersed with high- to moderate-albedo fine-grained deposits occurring in part as drifts or in small circular swales or hollows. Optically thick coatings of fine-grained ferric iron-rich dust dominate most bright soil and rock surfaces. Spectra of some darker rock surfaces and rock regions exposed by brushing or grinding show near-infrared spectral signatures consistent with the presence of mafic silicates such as pyroxene or olivine. Atmospheric observations show a steady decline in dust opacity during the mission, and astronomical observations captured solar transits by the martian moons, Phobos and Deimos, as well as a view of Earth from the martian surface.

  6. Aqueous processes at Gusev crater inferred from physical properties of rocks and soils along the Spirit traverse

    Science.gov (United States)

    Cabrol, N.A.; Farmer, J.D.; Grin, E.A.; Ritcher, L.; Soderblom, L.; Li, R.; Herkenhoff, K.; Landis, G.A.; Arvidson, R. E.

    2006-01-01

    Gusev crater was selected as the landing site for Spirit on the basis of morphological evidence of long-lasting water activity, including possibly fluvial and lacustrine episodes. From the Columbia Memorial Station to the Columbia Hills, Spirit's traverse provides a journey back in time, from relatively recent volcanic plains showing little evidence for aqueous processes up to the older hills, where rock and soil composition are drastically different. For the first 156 sols, the only evidence of water action was weathering rinds, vein fillings, and soil crust cementation by salts. The trenches of Sols 112-145 marked the first significant findings of increased concentrations of sulfur and magnesium varying in parallel, suggesting that they be paired as magnesium-sulfate. Spirit's arrival at West Spur coincided with a shift in rock and soil composition with observations hinting at substantial amounts of water in Gusev's past. We used the Microscopic Imager data up to Sol 431 to analyze rock and soil properties and infer plausible types and magnitude of aqueous processes through time. We show the role played early by topography and structure. The morphology, texture, and deep alteration shown by the rocks in West Spur and the Columbia Hills Formation (CHF) suggest conditions that are not met in present-day Mars and required a wetter environment, which could have included transport of sulfur, chlorine, and bromine in water, vapor in volcanic gases, hydrothermal circulation, or saturation in a briny fluid containing the same elements. Changing conditions that might have affected flow circulation are suggested by different textural and morphological characteristics between the rocks in the CHF and those of the plains, with higher porosity proxy, higher void ratio, and higher water storage potential in the CHF. Soils were used to assess aqueous processes and water pathways in the top layers of modern soils. We conclude that infiltration might have become more difficult

  7. Magnetic Properties Experiments on the Mars exploration Rover Spirit at Gusev crater

    DEFF Research Database (Denmark)

    Bertelsen, Pernille; Goetz, W.; Madsen, M.B.

    2004-01-01

    The magnetic properties experiments are designed to help identify the magnetic minerals in the dust and rocks on Mars-and to determine whether liquid water was involved in the formation and alteration of these magnetic minerals. Almost all of the dust particles suspended in the martian atmosphere...... must contain ferrimagnetic minerals (such as maghemite or magnetite) in an amount of similar to2% by weight. The most magnetic fraction of the dust appears darker than the average dust. Magnetite was detected in the first two rocks ground by Spirit....

  8. Sands at Gusev Crater, Mars

    Science.gov (United States)

    Cabrol, Nathalie A.; Herkenhoff, Kenneth E.; Knoll, Andrew H.; Farmer, Jack D.; Arvidson, Raymond E.; Grin, E.A.; Li, Ron; Fenton, Lori; Cohen, B.; Bell, J.F.; Yingst, R. Aileen

    2014-01-01

    Processes, environments, and the energy associated with the transport and deposition of sand at Gusev Crater are characterized at the microscopic scale through the comparison of statistical moments for particle size and shape distributions. Bivariate and factor analyses define distinct textural groups at 51 sites along the traverse completed by the Spirit rover as it crossed the plains and went into the Columbia Hills. Fine-to-medium sand is ubiquitous in ripples and wind drifts. Most distributions show excess fine material, consistent with a predominance of wind erosion over the last 3.8 billion years. Negative skewness at West Valley is explained by the removal of fine sand during active erosion, or alternatively, by excess accumulation of coarse sand from a local source. The coarse to very coarse sand particles of ripple armors in the basaltic plains have a unique combination of size and shape. Their distribution display significant changes in their statistical moments within the ~400 m that separate the Columbia Memorial Station from Bonneville Crater. Results are consistent with aeolian and/or impact deposition, while the elongated and rounded shape of the grains forming the ripples, as well as their direction of origin, could point to Ma'adim Vallis as a possible source. For smaller particles on the traverse, our findings confirm that aeolian processes have dominated over impact and other processes to produce sands with the observed size and shape patterns across a spectrum of geologic (e.g., ripples and plains soils) and aerographic settings (e.g., wind shadows).

  9. Acid Sulfate Alteration in Gusev Crater, Mars

    Science.gov (United States)

    Morris, R. V.; Ming, D. W.; Catalano, J. G.

    2016-01-01

    The Mars Exploration Rover (MER) Spirit landed on the Gusev Crater plains west of the Columbia Hills in January, 2004, during the Martian summer (sol 0; sol = 1 Martian day = 24 hr 40 min). Spirit explored the Columbia Hills of Gusev Crater in the vicinity of Home Plate at the onset on its second winter (sol approximately 900) until the onset of its fourth winter (sol approximately 2170). At that time, Spirit became mired in a deposit of fined-grained and sulfate-rich soil with dust-covered solar panels and unfavorable pointing of the solar arrays toward the sun. Spirit has not communicated with the Earth since sol 2210 (January, 2011). Like its twin rover Opportunity, which landed on the opposite side of Mars at Meridiani Planum, Spirit has an Alpha Particle X-Ray Spectrometer (APXS) instrument for chemical analyses and a Moessbauer spectrometer (MB) for measurement of iron redox state, mineralogical speciation, and quantitative distribution among oxidation (Fe(3+)/sigma Fe) and coordination (octahedral versus tetrahedral) states and mineralogical speciation (e.g., olivine, pyroxene, ilmenite, carbonate, and sulfate). The concentration of SO3 in Gusev rocks and soils varies from approximately 1 to approximately 34 wt%. Because the APXS instrument does not detect low atomic number elements (e.g., H and C), major-element oxide concentrations are normalized to sum to 100 wt%, i.e., contributions of H2O, CO2, NO2, etc. to the bulk composition care not considered. The majority of Gusev samples have approximately 6 plus or minus 5 wt% SO3, but there is a group of samples with high SO3 concentrations (approximately 30 wt%) and high total iron concentrations (approximately 20 wt%). There is also a group with low total Fe and SO3 concentrations that is also characterized by high SiO2 concentrations (greater than 70 wt%). The trend labeled "Basaltic Soil" is interpreted as mixtures in variable proportions between unaltered igneous material and oxidized and SO3-rich basaltic

  10. Evidence of phyllosilicates in Wooly Patch, an altered rock encountered at West Spur, Columbia Hills, by the Spirit rover in Gusev crater, Mars

    Science.gov (United States)

    Wang, A.; Korotev, R.L.; Jolliff, B.L.; Haskin, L.A.; Crumpler, L.; Farrand, W. H.; Herkenhoff, K. E.; de Souza, Jr.; Kusack, A.G.; Hurowitz, J.A.; Tosca, N.J.

    2006-01-01

    On its traverse to Columbia Hills, the Mars Exploration Rover Spirit investigated an outcrop designated "Wooly Patch" that exhibited morphological, mineralogical, and geochemical characteristics at the extreme ends of ranges observed among rocks studied at West Spur, a westward projecting salient near the foot of the Columbia Hills, Gusev crater. The major-element composition and Fe-mineralogy, as determined by the Alpha-Particle X-ray Spectrometer and Mo??ssbauer Spectrometer, are inconsistent with any reasonable assemblage of basaltic minerals in that there is an excess of Si and Al. The combined data are best explained by the presence of 14-17% phyllosilicate minerals. Phyllosilicates that account for the composition and cation ratios include members of the kaolinite, serpentine, chlorite, and septechlorite groups. The potential existence of kaolinite-type Al-rich phyllosilicates within the Wooly Patch outcrop suggests a mildly acidic environment (pH 4-6) in the past and an open hydrologic system with good drainage conditions in the environment where these rocks were altered. Copyright 2006 by the American Geophysical Union.

  11. The Context of Carbonates in Gusev and Jezero Craters

    Science.gov (United States)

    Ruff, S. W.; Hamilton, V. E.

    2017-12-01

    Gusev and Jezero are Noachian-aged craters with evidence of a lake in early Mars history. Both are among three remaining candidates for the Mars 2020 rover mission, which is intended to collect and cache rock samples for possible future return to Earth. Gusev was explored by the Spirit rover from 2004 to 2010, revealing outcrops dubbed Comanche composed of olivine-rich volcanic tephra that hosts up to 30% Mg-Fe carbonate, clear evidence for the role of near-neutral pH fluids [1]. Jezero also displays evidence for olivine- and carbonate-bearing materials, likely Mg-carbonate based on orbital spectral observations [2]. In both craters, the carbonates occur in materials that are among the oldest stratigraphic units in each, perhaps an indication of more clement climatic conditions on early Mars compared to those that prevailed for most of its history. We are undertaking investigations of various rover-based and orbital measurements of the carbonates in Gusev to better understand their geologic context and origin. In doing so, the results shed light on carbonate occurrences in Jezero. The Comanche outcrops are contained in the Columbia Hills, which represent a kipuka or island of eroded older terrain fully encircled by lava flows, here with a crater retention age of 3.65 Ga (Fig. 1). In situ and orbital observations [3] demonstrate that carbonate-bearing outcrops extend beyond those visited by Spirit. The distinctive morphology and thermal inertia signature of these outcrops and their unaltered host rocks are recognizable in other kipukas on the floor of Gusev [4]. Carbonate also occurs in kipukas in Jezero (Fig. 2), but larger occurrences extend beyond the crater rim and in isolated places among the delta fan deposits [2]. The presence of carbonates outside of the crater suggests an origin unrelated to a former lake, unlike the Comanche carbonates, which may have arisen through evaporation of dilute brines from an ephemeral lake in Gusev [4]. In both cases, the clear

  12. Characterisation of the magnetic iron phases in Clovis Class rocks in Gusev crater from the MER Spirit Mössbauer spectrometer

    Science.gov (United States)

    Van Cromphaut, C.; de Resende, V. G.; De Grave, E.; Van Alboom, A.; Vandenberghe, R. E.; Klingelhöfer, G.

    2007-10-01

    Mössbauer backscattering spectra of eight Martian rocks, acquired by the MIMOS II spectrometer of Rover Spirit (MER-A) and containing goethite in addition to other iron minerals, have been selected for in-depth numerical analysis. Where feasible, different temperature windows for a given rock were considered. A novel calibration/folding procedure, exclusively based on the fitted positions of the eight prominent absorption lines in the transmission spectra of the reference target and not relying on the error signal of the MIMOS II spectrometer, has been developed. It is demonstrated that this procedure yields reliable and reasonably accurate values for the adjusted Mössbauer parameters of the respective spectra of the rock targets. These spectra are all composed of magnetically split components arising from hematite, magnetite and goethite phases, in addition to a ferrous and a ferric doublet that can be ascribed to the presence of Fe silicates, possibly glasses. It is argued that the Fe 3+ doublet has no significant contribution from superparamagnetic Fe-oxide particles. The hematite components reflect the coexistence of antiferromagnetic and weakly ferromagnetic spin states. In general the magnetite content in the selected rocks is low. The goethite subspectra are very broad and asymmetric and need to be described by a model-independent distribution of hyperfine fields. The as-such obtained parameter values indicate an average particle size of the order of 10 nm. For all examined rock spectra, the adjusted parameter values for the various Fe oxides are completely in line with those known for terrestrial (natural or synthetic) species.

  13. Hydrothermal origin of halogens at Home Plate, Gusev Crater

    Science.gov (United States)

    Schmidt, M.E.; Ruff, S.W.; McCoy, T.J.; Farrand, W. H.; Johnson, J. R.; Gellert, Ralf; Ming, D. W.; Morris, R.V.; Cabrol, N.; Lewis, K.W.; Schroeder, C.

    2008-01-01

    In the Inner Basin of the Columbia Hills, Gusev Crater is Home Plate, an 80 m platform of layered elastic rocks of the Barnhill class with microscopic and macroscopic textures, including a bomb sag, suggestive of a phreatomagmatic origin. We present data acquired by the Spirit Mars Exploration Rover by Alpha Particle X-Ray Spectrometer (APXS), Mo??ssbauer Spectrometer, Miniature Thermal Emission Spectrometer (Mini-TES), and Panoramic Camera (Pancam) for the Barnhill class rocks and nearby vesicular Irvine class basalts. In major element concentrations (e.g., SiO2, Al2O3, MgO, and FeO*), the two rock classes are similar, suggesting that they are derived from a similar magmatic source. The Barnhill class, however, has higher abundances of Cl, Br, Zn, and Ge with comparable SO3 to the Irvine basalts. Nanophase ferric oxide (np ox) and volcanic glass were detected in the Barnhill class rocks by Mo??ssbauer and Mini-TES, respectively, and imply greater alteration and cooling rates in the Barnhill than in the Irvine class rocks. The high volatile elements in the Barnhill class agree with volcanic textures that imply interaction with a briny groundwater during eruption and (or) by later alteration. Differences in composition between the Barnhill and Irvine classes allow the fingerprinting of a Na-Mg-Zn-Ge-Cl-Br (??Fe ?? Ca ?? CO2) brine with low S. Nearby sulfate salt soils of fumarolic origin may reflect fractionation of an acidic S-rich vapor during boiling of a hydrothermal brine at depth. Persistent groundwater was likely present during and after the formation of Home Plate. Copyright 2008 by the American Geophysical Union.

  14. Silica-Rich Soil in Gusev Crater

    Science.gov (United States)

    2007-01-01

    NASA's Mars Exploration Rover Spirit has found a patch of bright-toned soil so rich in silica that scientists propose water must have been involved in concentrating it. The silica-rich patch, informally named 'Gertrude Weise' after a player in the All-American Girls Professional Baseball League, was exposed when Spirit drove over it during the 1,150th Martian day, or sol, of Spirit's Mars surface mission (March 29, 2007). One of Spirit's six wheels no longer rotates, so it leaves a deep track as it drags through soil. Most patches of disturbed, bright soil that Spirit had investigated previously are rich in sulfur, but this one has very little sulfur and is about 90 percent silica. Spirit's panoramic camera imaged the bright patch through various filters on Sol 1,158 (April 6). This approximately true-color image combines images taken through three different filters. The track of disturbed soil is roughly 20 centimeters (8 inches) wide. Spirit's miniature thermal emission spectrometer, which can assess a target's mineral composition from a distance, examined the Gertrude Weise patch on Sol 1,172 (April 20). The indications it found for silica in the overturned soil prompted a decision to drive Spirit close enough to touch the soil with the alpha particle X-ray spectrometer, a chemical analyzer at the end of Spirit's robotic arm. The alpha particle X-ray spectrometer collected data about this target on sols 1,189 and 1,190 (May 8 and May 9) and produced the finding of approximately 90 percent silica. Silica is silicon dioxide. On Earth, it commonly occurs as the crystalline mineral quartz and is the main ingredient in window glass. The Martian silica at Gertrude Weise is non-crystalline, with no detectable quartz. In most cases, water is required to produce such a concentrated deposit of silica, according to members of the rover science team. One possible origin for the silica could have been interaction of soil with acidic steam produced by volcanic activity

  15. Characterization and petrologic interpretation of olivine-rich basalts at Gusev Crater, Mars

    Science.gov (United States)

    McSween, H.Y.; Wyatt, M.B.; Gellert, Ralf; Bell, J.F.; Morris, R.V.; Herkenhoff, K. E.; Crumpler, L.S.; Milam, K.A.; Stockstill, K.R.; Tornabene, L.L.; Arvidson, R. E.; Bartlett, P.; Blaney, D.; Cabrol, N.A.; Christensen, P.R.; Clark, B. C.; Crisp, J.A.; Des Marais, D.J.; Economou, T.; Farmer, J.D.; Farrand, W.; Ghosh, A.; Golombek, M.; Gorevan, S.; Greeley, R.; Hamilton, V.E.; Johnson, J. R.; Joliff, B.L.; Klingelhofer, G.; Knudson, A.T.; McLennan, S.; Ming, D.; Moersch, J.E.; Rieder, R.; Ruff, S.W.; Schrorder, C.; de Souza, P.A.; Squyres, S. W.; Wanke, H.; Wang, A.; Yen, A.; Zipfel, J.

    2006-01-01

    Rocks on the floor of Gusev crater are basalts of uniform composition and mineralogy. Olivine, the only mineral to have been identified or inferred from data by all instruments on the Spirit rover, is especially abundant in these rocks. These picritic basalts are similar in many respects to certain Martian meteorites (olivine-phyric shergottites). The olivine megacrysts in both have intermediate compositions, with modal abundances ranging up to 20-30%. Associated minerals in both include low-calcium and high-calcium pyroxenes, plagioclase of intermediate composition, iron-titanium-chromium oxides, and phosphate. These rocks also share minor element trends, reflected in their nickel-magnesium and chromium-magnesium ratios. Gusev basalts and shergottites appear to have formed from primitive magmas produced by melting an undepleted mantle at depth and erupted without significant fractionation. However, apparent differences between Gusev rocks and shergottites in their ages, plagioclase abundances, and volatile contents preclude direct correlation. Orbital determinations of global olivine distribution and compositions by thermal emission spectroscopy suggest that olivine-rich rocks may be widespread. Because weathering under acidic conditions preferentially attacks olivine and disguises such rocks beneath alteration rinds, picritic basalts formed from primitive magmas may even be a common component of the Martian crust formed during ancient and recent times. Copyright 2006 by the American Geophysical Union.

  16. Alkaline volcanic rocks from the Columbia Hills, Gusev crater, Mars

    Science.gov (United States)

    McSween, H.Y.; Ruff, S.W.; Morris, R.V.; Bell, J.F.; Herkenhoff, K.; Gellert, Ralf; Stockstill, K.R.; Tornabene, L.L.; Squyres, S. W.; Crisp, J.A.; Christensen, P.R.; McCoy, T.J.; Mittlefehldt, D. W.; Schmidt, M.

    2006-01-01

    Irvine, Backstay, and Wishstone are the type specimens for three classes of fine-grained or fragmental, relatively unaltered rocks with distinctive thermal emission spectra, found as float on the flanks of the Columbia Hills. Chemical analyses indicate that these rocks are mildly alkaline basalt, trachybasalt, and tephrite, respectively. Their mineralogy consists of Na- and K-rich feldspar(s), low- and high-Ca pyroxenes, ferroan olivine, Fe-Ti (and possibly Cr) oxides, phosphate, and possibly glass. The texture of Wishstone is consistent with a pyroclastic origin, whereas Irvine and Backstay are lavas or possibly dike rocks. Chemical compositions of these rocks plot on or near liquid lines of descent for most elements calculated for Adirondack class rocks (olivine-rich basalts from the Gusev plains) at various pressures from 0.1 to 1.0 GPa. We infer that Wishstone-, Backstay-, and Irvine-class magmas may have formed by fractionation of primitive, oxidized basaltic magma similar to Adirondack-class rocks. The compositions of all these rocks reveal that the Gusev magmatic province is alkaline, distinct from the subalkaline volcanic rocks thought to dominate most of the planet's surface. The fact that differentiated volcanic rocks were not encountered on the plains prior to ascending Husband Hill may suggest a local magma source for volcanism beneath Gusev crater. Copyright 2006 by the American Geophysical Union.

  17. Terrestrial analogues models based on MOURA magnetometer data. Application to Gusev crater and Apollinaris volcano

    Science.gov (United States)

    Díaz-Michelena, Marina; Cerdán, Miguel Felipe; Ramírez-Nicolás, María; Sánchez-Cano, Beatríz; Sánchez-Bayton, Marina; Kilian, Rolf

    2014-05-01

    models and on Earth surveys data. Furthermore, the Apollinaris volcano (Robinson, 1993) and the Gusev crater (Bertelsen, 2004) have been selected as the most appropriate edifices for the extrapolated analysis. They both belong to the Noachian period which comprise the needed characteristics described above. We aim to analyse if the magnetic measurements made on Earth with MOURA at specific crater structures can be reproduced on Mars with our model. References Moar, R. et al., 'Manicouagan and baie du nord projects Manicouagan reservoir, Quebec'; Technical Report, No. 733, 2004. Lorenz V., 'Maar-diatreme volcanoes, their formation and their setting in hard-rock or soft-rock environments'; Geolines, 15, 72-83, 2003. Grieve, R.A.F., 'Impact Structures in Canada'; Geological Association of Canada, 2006. Robinson M. S et al., 'Chronology, Eruption Duration, and Atmospheric Contribution of the Martian Volcano Apollinaris Patera', Icarus, Volume 104, Issue 2, August 1993, Pages 301-323, 1993. Bertelsen, P et al., 'Magnetic properties experiments on the Mars exploration rover Spirit at Gusev crater', Science Volume: 305 Issue: 5685 Pages: 827-829 (doi: 10.1126/science.1100112), August 6th, 2004.

  18. Mars Exploration Rover Pancam Multispectral Imaging of Rocks, Soils, and Dust at Gusev Crater and Meridiani Planum. Chapter 13

    Science.gov (United States)

    Bell, J. F., III; Calvin, W. M.; Farrand, W.; Greeley, R.; Johnson, J. R.; Jolliff, B.; Morris, R. V.; Sullivan, R. J.; Thompson, S.; Wang, A.; hide

    2007-01-01

    Multispectral imaging from the Panoramic Camera (Pancam) instruments on the Mars Exploration Rovers Spirit and Opportunity has provided important new insights about the geology and geologic history of the rover landing sites and traverse locations in Gusev crater and Meridiani Planum. Pancam observations from near-UV to near-IR wavelengths provide limited compositional and mineralogic constraints on the presence abundance, and physical properties of ferric- and ferrous-iron bearing minerals in rocks, soils, and dust at both sites. High resolution and stereo morphologic observations have also helped to infer some aspects of the composition of these materials at both sites. Perhaps most importantly, Pancam observations were often efficiently and effectively used to discover and select the relatively small number of places where in situ measurements were performed by the rover instruments, thus supporting and enabling the much more quantitative mineralogic discoveries made using elemental chemistry and mineralogy data. This chapter summarizes the major compositionally- and mineralogically-relevant results at Gusev and Meridiani derived from Pancam observations. Classes of materials encountered in Gusev crater include outcrop rocks, float rocks, cobbles, clasts, soils, dust, rock grindings, rock coatings, windblown drift deposits, and exhumed whitish/yellowish salty soils. Materials studied in Meridiani Planum include sedimentary outcrop rocks, rock rinds, fracture fills, hematite spherules, cobbles, rock fragments, meteorites, soils, and windblown drift deposits. This chapter also previews the results of a number of coordinated observations between Pancam and other rover-based and Mars-orbital instruments that were designed to provide complementary new information and constraints on the mineralogy and physical properties of martian surface materials.

  19. Temperature dependence of the quadrupole splitting of olivine and pyroxene from the Plains of Gusev Crater on Mars

    International Nuclear Information System (INIS)

    Agresti, David G.

    2012-01-01

    In the present work, we report application of simultaneous fitting procedures to Mössbauer data acquired on the Plains of Gusev Crater by the MIMOS II spectrometer on board the Mars Exploration Rover Spirit. Based on a quantitative measure of spectrum quality, the 34 best of the ∼126 spectra acquired on the Plains are grouped together for a single simultaneous fit with a common least-squares criterion. Fitted values for the quadrupole splitting (QS) of olivine (Ol) from 200 K to 260 K are shown to lie between reported trend lines for Fo50 and Fo30 olivine, with a temperature gradient of (−11.2 ± 1.2) × 10  − 4 mm/s/K, a nearly five-fold improvement in precision over the previously reported value, enabling extrapolation to QS(Ol) = (2.93 ± 0.01) mm/s at 295 K. QS of pyroxene fit as a single doublet exhibits a temperature gradient of (−7.3 ± 2.3) × 10  − 4 mm/s/K.

  20. Spectral Variability among Rocks in Visible and Near Infrared Multispectral Pancam Data Collected at Gusev Crater: Examinations using Spectral Mixture Analysis and Related Techniques

    Science.gov (United States)

    Farrand, W. H.; Bell, J. F., III; Johnson, J. R.; Squyres, S. W.; Soderblom, J.; Ming, D. W.

    2006-01-01

    Visible and Near Infrared (VNIR) multispectral observations of rocks made by the Mars Exploration Rover Spirit s Panoramic camera (Pancam) have been analysed using a spectral mixture analysis (SMA) methodology. Scenes have been examined from the Gusev crater plains into the Columbia Hills. Most scenes on the plains and in the Columbia Hills could be modeled as three endmember mixtures of a bright material, rock, and shade. Scenes of rocks disturbed by the rover s Rock Abrasion Tool (RAT) required additional endmembers. In the Columbia Hills there were a number of scenes in which additional rock endmembers were required. The SMA methodology identified relatively dust-free areas on undisturbed rock surfaces, as well as spectrally unique areas on RAT abraded rocks. Spectral parameters from these areas were examined and six spectral classes were identified. These classes are named after a type rock or area and are: Adirondack, Lower West Spur, Clovis, Wishstone, Peace, and Watchtower. These classes are discriminable based, primarily, on near-infrared (NIR) spectral parameters. Clovis and Watchtower class rocks appear more oxidized than Wishstone class rocks and Adirondack basalts based on their having higher 535 nm band depths. Comparison of the spectral parameters of these Gusev crater rocks to parameters of glass-dominated basaltic tuffs indicates correspondence between measurements of Clovis and Watchtower classes, but divergence for the Wishstone class rocks which appear to have a higher fraction of crystalline ferrous iron bearing phases. Despite a high sulfur content, the rock Peace has NIR properties resembling plains basalts.

  1. Geology of the Gusec cratered plains from the Spirit rover transverse

    Science.gov (United States)

    Golombek, M. P.; Crumpler, L. S.; Grant, J. A.; Greely, R.; Cabrol, N. A.; Parker, T. J.; Rice, J. W., Jr.; Ward, J. G.; Arvidson, R. E.; Moersch, J. E.; hide

    2006-01-01

    The cratered plains of Gusev traversed by Spirit are generally low-relief rocky plains dominated by impact and eolian processes. Ubiquitous shallow, soil-filled, circular depressions, called hollows, are modified impact craters. Rocks are dark, fine-grained basalts, and the upper 10 m of the cratered plains appears to be an impact-generated regolith developed over intact basalt flows. Systematic field observations across the cratered plains identified vesicular clasts and rare scoria similar to original lava flow tops, consistent with an upper inflated surface of lava flows with adjacent collapse depressions. Crater and hollow morphometry are consistent with most being secondaries. The size frequency distribution of rocks >0.1 m diameter generally follows exponential functions similar to other landing sites for total rock abundances of 5-35%. Systematic clast counts show that areas with higher rock abundance and more large rocks have higher thermal inertia. Plains with lower thermal inertia have fewer rocks and substantially more pebbles that are well sorted and evenly spaced, similar to a desert pavement or lag. Eolian bed forms (ripples and wind tails) have coarse surface lags, and many are dust covered and thus likely inactive. Deflation of the surface _5-25 cm likely exposed two-toned rocks and elevated ventifacts and transported fines into craters creating the hollows. This observed redistribution yields extremely slow average erosion rates of _0.03 nm/yr and argues for very little long-term net change of the surface and a dry and desiccating environment similar to today's since the Hesperian (or _3 Ga).

  2. The Alteration History of Clovis Class Rocks in Gusev Crater as Determined by Ti-Normalzed Mass Balance Analysis

    Science.gov (United States)

    Sutter, Brat; Ming, Douglas W.; Niles, P. B.; Golden, D. C.

    2012-01-01

    The West Spur Clovis class rocks in Gusev Crater are some of the most altered rocks in Gusev Crater and likely contain a mixed sulfate and phyllosilicate mineralogy [1,2]. The high S and Cl content of the Clovis rocks suggests that acidic vapors or fluids of H2SO4 and HCl reacted with the Clovis parent rock to form Ca, Mg,- sulfates, iron-oxyhydroxides and secondary aluminosilicates (approx.60 wt.%) of a poorly crystalline nature (e.g., allophane) [1]. Up to 14-17 wt.% phyllosilicates (e.g., kaolinite, chlorite, serpentine) are hypothesized to exist in the Clovis materials suggesting that Clovis parent materials while possibly exposed to acidic pHs were likely neutralized by basalt dissolution which resulted in mildly acidic pHs (4-6) [1, 2]. This work proposes that subsequent to the alteration of the Clovis rocks, alteration fluids became concentrated in ions resulting in the addition of silicate and salts. The objective of this work is to utilize Ti-normalized mass balance analysis to evaluate (1) mineral gains and losses and (2) elemental gains and losses in the Clovis rocks. Results of this work will be used evaluate the nature of geochemical conditions that affect phyllosilicate and sulfate formation at Gusev crater.

  3. Spectral variability among rocks in visible and near-infrared mustispectral Pancam data collected at Gusev crater: Examinations using spectral mixture analysis and related techniques

    Science.gov (United States)

    Farrand, W. H.; Bell, J.F.; Johnson, J. R.; Squyres, S. W.; Soderblom, J.; Ming, D. W.

    2006-01-01

    Visible and near-infrared (VNIR) multispectral observations of rocks made by the Mars Exploration Rover Spirit's Panoramic camera (Pancam) have been analyzed using a spectral mixture analysis (SMA) methodology. Scenes have been examined from the Gusev crater plains into the Columbia Hills. Most scenes on the plains and in the Columbia Hills could be modeled as three end-member mixtures of a bright material, rock, and shade. Scenes of rocks disturbed by the rover's Rock Abrasion Tool (RAT) required additional end-members. In the Columbia Hills, there were a number of scenes in which additional rock end-members were required. The SMA methodology identified relatively dust-free areas on undisturbed rock surfaces as well as spectrally unique areas on RAT abraded rocks. Spectral parameters from these areas were examined, and six spectral classes were identified. These classes are named after a type rock or area and are Adirondack, Lower West Spur, Clovis, Wishstone, Peace, and Watchtower. These classes are discriminable based, primarily, on near-infrared (NIR) spectral parameters. Clovis and Watchtower class rocks appear more oxidized than Wishstone class rocks and Adirondack basalts based on their having higher 535 nm band depths. Comparison of the spectral parameters of these Gusev crater rocks to parameters of glass-dominated basaltic tuffs indicates correspondence between measurements of Clovis and Watchtower classes but divergence for the Wishstone class rocks, which appear to have a higher fraction of crystalline ferrous iron-bearing phases. Despite a high sulfur content, the rock Peace has NIR properties resembling plains basalts. Copyright 2006 by the American Geophysical Union.

  4. High-Resolution Textures of Soils and Rocks at Gusev Crater and Meridiani Planum From the Mars Exploration Rover Microscopic Imagers

    Science.gov (United States)

    Herkenhoff, K. E.

    2004-12-01

    The Microscopic Imagers on the Spirit and Opportunity rovers have returned images of Mars with higher resolution than any previous camera system, allowing detailed petrographic and sedimentological studies of the rocks and soils at the Gusev and Meridiani landing sites. The Microscopic Imager (MI) is a fixed-focus camera mounted on the robotic arm of each Mars Exploration Rover (MER). The MI was designed to function like a geologist's hand lens, acquiring images at a scale of 31 microns/pixel over a broad spectral range (400-700 nm). The MI provides critical documentation of the constitution and texture of targets analyzed by the other MER in-situ instruments. The MI on the Spirit rover found weakly bound agglomerates of dust in the soil near the Columbia Memorial Station. Bedforms have coarser particles at their crests and finer grains in the troughs, like eolian ripples on Earth. Some of the brushed or abraded rock surfaces show igneous textures and evidence for alteration rinds, coatings, and veins consistent with secondary mineralization. The textures of rocks on the floor of Gusev crater are consistent with a volcanic origin and subsequent alteration and/or weathering by impact events, wind and possibly water. MI observations in the ''Columbia Hills'' are consistent with interpretations, based on syntheses of various MER data, that the rocks there are more altered than those on the floor of Gusev. The MI on the Opportunity rover has returned images of the Meridiani landing site that include evidence for both surface and ground water activity in Mars' ancient past. Soil particles imaged by the MI show constituents typical of windblown materials. The uppermost millimeter of some soils is weakly cemented, probably by salts precipitated from evaporating brines. Rock outcrops are laminated on a millimeter scale; image mosaics of cross-stratification suggest that some sediments were deposited by flowing water. Vugs in some outcrop faces are probably molds formed by

  5. Magnetic Properties Experiments on the Mars exploration Rover Spirit at Gusev crater

    DEFF Research Database (Denmark)

    Bertelsen, Pernille; Goetz, W.; Madsen, M.B.

    2004-01-01

    The magnetic properties experiments are designed to help identify the magnetic minerals in the dust and rocks on Mars-and to determine whether liquid water was involved in the formation and alteration of these magnetic minerals. Almost all of the dust particles suspended in the martian atmosphere...

  6. Weathering Profiles in Phosphorus-Rich Rocks at Gusev Crater, Mars, Suggest Dissolution of Phosphate Minerals into Potentially Habitable Near-Neutral Waters.

    Science.gov (United States)

    Adcock, Christopher T; Hausrath, Elisabeth M

    2015-12-01

    Abundant evidence indicates that significant surface and near-surface liquid water has existed on Mars in the past. Evaluating the potential for habitable environments on Mars requires an understanding of the chemical and physical conditions that prevailed in such aqueous environments. Among the geological features that may hold evidence of past environmental conditions on Mars are weathering profiles, such as those in the phosphorus-rich Wishstone-class rocks in Gusev Crater. The weathering profiles in these rocks indicate that a Ca-phosphate mineral has been lost during past aqueous interactions. The high phosphorus content of these rocks and potential release of phosphorus during aqueous interactions also make them of astrobiological interest, as phosphorus is among the elements required for all known life. In this work, we used Mars mission data, laboratory-derived kinetic and thermodynamic data, and data from terrestrial analogues, including phosphorus-rich basalts from Idaho, to model a conceptualized Wishstone-class rock using the reactive transport code CrunchFlow. Modeling results most consistent with the weathering profiles in Wishstone-class rocks suggest a combination of chemical and physical erosion and past aqueous interactions with near-neutral waters. The modeling results also indicate that multiple Ca-phosphate minerals are likely in Wishstone-class rocks, consistent with observations of martian meteorites. These findings suggest that Gusev Crater experienced a near-neutral phosphate-bearing aqueous environment that may have been conducive to life on Mars in the past. Mars-Gusev Crater-Wishstone-Reactive transport modeling-CrunchFlow-Aqueous interactions-Neutral pH-Habitability.

  7. Coatings and weathering rinds at Gusev crater, Mars, investigated by depth selective Moessbauer spectroscopy

    International Nuclear Information System (INIS)

    Fleischer, Iris; Klingelhoefer, Goestar; Schroeder, Christian; Rodionov, Daniel S.

    2008-01-01

    The miniaturised Moessbauer spectrometer (MIMOS II) is part of the scientific payload of the two Mars Exploration Rovers, 'Spirit' and 'Opportunity' (Klingelhoefer et al., J Geophys Res 108(E12), 2003). MIMOS II can obtain 14.4 keV γ-ray spectra and 6.4 keV X-ray spectra simultaneously in backscattering geometry. Comparing 6.4 keV and 14.4 keV spectra yields depth selective information about a sample and allows for the detection and characterization of thin coatings or weathering rinds. Laboratory measurements and a Monte Carlo simulation were used to study the influence of coatings of varying thickness and composition on backscattering Moessbauer spectra. The thickness of thin surface layers on natural samples can be estimated by comparing measured and the corresponding simulated spectra.

  8. Pancam Spectral Variations Across Home Plate: Bonestell Panorama, Gusev Crater, Mars

    Science.gov (United States)

    Johnson, J. R.; Bell, J. F.; Rice, M. S.; Farrand, W. H.; Schmidt, M. E.; Herkenhoff, K. E.; Wang, A.

    2008-12-01

    Visible/near-infrared color variations across the surface of the Home Plate (HP) structure were first observed by the Spirit Pancam multispectral camera using images acquired from the top of Husband Hill on sol 595, ~700m away from HP. Orbital imaging by the HiRISE camera on sol 1325 showed consistent color trends with Pancam in which the western edge of HP was "redder" than the "bluer" eastern portion. This suggested the eastern rim materials of HP are not as contaminated by airfall dust and/or are less oxidized. Pancam spectra of brushed rock targets indicate that western dust-free rock surfaces have higher 535nm band depths (consistent with higher Fe3+/Fe measured by the Mossbauer spectrometer), potentially caused by finely crystalline red hematite. The western rocks also exhibited less negative 601nm band depths than in the east, which could result from lower pyroxene/olivine ratios or the presence of goethite. The spectral variations across HP combined with in situ geochemical data around the rim suggest that the volcanic and/or hydrothermal nature of the HP system resulted in localized, high temperature events on the eastern side, compared to lower temperature alteration on the western side that produced greater amounts of nanophase ferric oxides. This hypothesis is being investigated using 13 band scenes acquired from Spirit's winter location on the northern rim of HP. Pancam began imaging on sol 1477 as part of an extensive mosaic (the "Bonestell Panorama"). Preliminary analyses confirm higher red/blue ratios along the western rim, but also redder regions on the eastern rim not as obvious in Sol 595 images. HiRISE acquired a color image of HP on Sol 1591 that shows less color variability on HP than the sol 1325 image. Dust fallout from the 2007 dust storm (sols 1240 to 1330) may be the cause of these temporal color variations. Additional analysis is required to determine whether surficial dust deposits are the dominant cause of the original color dichotomy

  9. VNIR Multispectral Observations of Rocks at Spirit of St. Louis Crater and Marathon Valley on Th Rim of Endeavour Crater Made by the Opportunity Rover Pancam

    Science.gov (United States)

    Farrand, W. H.; Johnson, J. R.; Bell, J. F., III; Mittlefehldt, D.W.

    2016-01-01

    The Mars Exploration Rover Opportunity has been exploring the western rim of the 22 km diameter Endeavour crater since August, 2011. Recently, Opportunity has reached a break in the Endeavour rim that the rover team has named Mara-thon Valley. This is the site where orbital observations from the MRO CRISM imaging spectrometer indicated the presence of iron smectites. On the outer western portion of Marathon Valley, Opportunity explored the crater-form feature dubbed Spirit of St. Louis (SoSL) crater. This presentation describes the 430 to 1009 nm (VNIR) reflectance, measured by the rover's Pancam, of rock units present both at Spirit of St. Louis and within Marathon Valley.

  10. Whirlwind Drama During Spirit's 496th Sol

    Science.gov (United States)

    2005-01-01

    This movie clip shows a dust devil growing in size and blowing across the plain inside Mars' Gusev Crater. The clip consists of frames taken by the navigation camera on NASA's Mars Exploration Rover Spirit during the morning of the rover's 496th martian day, or sol (May 26, 2005). Contrast has been enhanced for anything in the images that changes from frame to frame, that is, for the dust moved by wind.

  11. Curiosity at Gale Crater, Mars: Characterization and Analysis of the Rocknest Sand Shadow

    Science.gov (United States)

    Blake, D. F.; Morris, R. V.; Kocurek, G.; Morrison, S. M.; Downs, R. T.; Bish, D.; Ming, D. W.; Edgett, K. S.; Rubin, D.; Goetz, W.; Madsen, M. B.; Sullivan, R.; Gellert, R.; Campbell, I.; Treiman, A. H.; McLennan, S. M.; Yen, A. S.; Grotzinger, J.; Vaniman, D. T.; Chipera, S. J.; Achilles, C. N.; Rampe, E. B.; Sumner, D.; Meslin, P.-Y.; Maurice, S.; Forni, O.; Gasnault, O.; Fisk, M.; Schmidt, M.; Mahaffy, P.; Leshin, L. A.; Glavin, D.; Steele, A.; Freissinet, C.; Navarro-González, R.; Yingst, R. A.; Kah, L. C.; Bridges, N.; Lewis, K. W.; Bristow, T. F.; Farmer, J. D.; Crisp, J. A.; Stolper, E. M.; Des Marais, D. J.; Sarrazin, P.; Agard, Christophe; Alves Verdasca, José Alexandre; Anderson, Robert; Anderson, Ryan; Archer, Doug; Armiens-Aparicio, Carlos; Arvidson, Ray; Atlaskin, Evgeny; Atreya, Sushil; Aubrey, Andrew; Baker, Burt; Baker, Michael; Balic-Zunic, Tonci; Baratoux, David; Baroukh, Julien; Barraclough, Bruce; Bean, Keri; Beegle, Luther; Behar, Alberto; Bell, James; Bender, Steve; Benna, Mehdi; Bentz, Jennifer; Berger, Gilles; Berger, Jeff; Berman, Daniel; Blanco Avalos, Juan Jose; Blaney, Diana; Blank, Jen; Blau, Hannah; Bleacher, Lora; Boehm, Eckart; Botta, Oliver; Böttcher, Stephan; Boucher, Thomas; Bower, Hannah; Boyd, Nick; Boynton, Bill; Breves, Elly; Bridges, John; Brinckerhoff, William; Brinza, David; Brunet, Claude; Brunner, Anna; Brunner, Will; Buch, Arnaud; Bullock, Mark; Burmeister, Sönke; Cabane, Michel; Calef, Fred; Cameron, James; Cantor, Bruce; Caplinger, Michael; Rodríguez, Javier Caride; Carmosino, Marco; Blázquez, Isaías Carrasco; Charpentier, Antoine; Choi, David; Clark, Benton; Clegg, Sam; Cleghorn, Timothy; Cloutis, Ed; Cody, George; Coll, Patrice; Conrad, Pamela; Coscia, David; Cousin, Agnès; Cremers, David; Cros, Alain; Cucinotta, Frank; d'Uston, Claude; Davis, Scott; Day, Mackenzie; Juarez, Manuel de la Torre; DeFlores, Lauren; DeLapp, Dorothea; DeMarines, Julia; Dietrich, William; Dingler, Robert; Donny, Christophe; Drake, Darrell; Dromart, Gilles; Dupont, Audrey; Duston, Brian; Dworkin, Jason; Dyar, M. Darby; Edgar, Lauren; Edwards, Christopher; Edwards, Laurence; Ehlmann, Bethany; Ehresmann, Bent; Eigenbrode, Jen; Elliott, Beverley; Elliott, Harvey; Ewing, Ryan; Fabre, Cécile; Fairén, Alberto; Farley, Ken; Fassett, Caleb; Favot, Laurent; Fay, Donald; Fedosov, Fedor; Feldman, Jason; Feldman, Sabrina; Fitzgibbon, Mike; Flesch, Greg; Floyd, Melissa; Flückiger, Lorenzo; Fraeman, Abby; Francis, Raymond; François, Pascaline; Franz, Heather; French, Katherine Louise; Frydenvang, Jens; Gaboriaud, Alain; Gailhanou, Marc; Garvin, James; Geffroy, Claude; Genzer, Maria; Godber, Austin; Goesmann, Fred; Golovin, Dmitry; Gómez, Felipe Gómez; Gómez-Elvira, Javier; Gondet, Brigitte; Gordon, Suzanne; Gorevan, Stephen; Grant, John; Griffes, Jennifer; Grinspoon, David; Guillemot, Philippe; Guo, Jingnan; Gupta, Sanjeev; Guzewich, Scott; Haberle, Robert; Halleaux, Douglas; Hallet, Bernard; Hamilton, Vicky; Hardgrove, Craig; Harker, David; Harpold, Daniel; Harri, Ari-Matti; Harshman, Karl; Hassler, Donald; Haukka, Harri; Hayes, Alex; Herkenhoff, Ken; Herrera, Paul; Hettrich, Sebastian; Heydari, Ezat; Hipkin, Victoria; Hoehler, Tori; Hollingsworth, Jeff; Hudgins, Judy; Huntress, Wesley; Hurowitz, Joel; Hviid, Stubbe; Iagnemma, Karl; Indyk, Steve; Israël, Guy; Jackson, Ryan; Jacob, Samantha; Jakosky, Bruce; Jensen, Elsa; Jensen, Jaqueline Kløvgaard; Johnson, Jeffrey; Johnson, Micah; Johnstone, Steve; Jones, Andrea; Jones, John; Joseph, Jonathan; Jun, Insoo; Kahanpää, Henrik; Kahre, Melinda; Karpushkina, Natalya; Kasprzak, Wayne; Kauhanen, Janne; Keely, Leslie; Kemppinen, Osku; Keymeulen, Didier; Kim, Myung-Hee; Kinch, Kjartan; King, Penny; Kirkland, Laurel; Koefoed, Asmus; Köhler, Jan; Kortmann, Onno; Kozyrev, Alexander; Krezoski, Jill; Krysak, Daniel; Kuzmin, Ruslan; Lacour, Jean Luc; Lafaille, Vivian; Langevin, Yves; Lanza, Nina; Lasue, Jeremie; Le Mouélic, Stéphane; Lee, Ella Mae; Lee, Qiu-Mei; Lees, David; Lefavor, Matthew; Lemmon, Mark; Lepinette Malvitte, Alain; Léveillé, Richard; Lewin-Carpintier, Éric; Li, Shuai; Lipkaman, Leslie; Little, Cynthia; Litvak, Maxim; Lorigny, Eric; Lugmair, Guenter; Lundberg, Angela; Lyness, Eric; Maki, Justin; Malakhov, Alexey; Malespin, Charles; Malin, Michael; Mangold, Nicolas; Manning, Heidi; Marchand, Geneviève; Marín Jiménez, Mercedes; Martín García, César; Martin, Dave; Martin, Mildred; Martínez-Frías, Jesús; Martín-Soler, Javier; Martín-Torres, F. Javier; Mauchien, Patrick; McAdam, Amy; McCartney, Elaina; McConnochie, Timothy; McCullough, Emily; McEwan, Ian; McKay, Christopher; McNair, Sean; Melikechi, Noureddine; Meyer, Michael; Mezzacappa, Alissa; Miller, Hayden; Miller, Kristen; Milliken, Ralph; Minitti, Michelle; Mischna, Michael; Mitrofanov, Igor; Moersch, Jeff; Mokrousov, Maxim; Molina Jurado, Antonio; Moores, John; Mora-Sotomayor, Luis; Morookian, John Michael; Mueller-Mellin, Reinhold; Muller, Jan-Peter; Muñoz Caro, Guillermo; Nachon, Marion; Navarro López, Sara; Nealson, Kenneth; Nefian, Ara; Nelson, Tony; Newcombe, Megan; Newman, Claire; Newsom, Horton; Nikiforov, Sergey; Niles, Paul; Nixon, Brian; Dobrea, Eldar Noe; Nolan, Thomas; Oehler, Dorothy; Ollila, Ann; Olson, Timothy; Owen, Tobias; Pablo, Hernández; Paillet, Alexis; Pallier, Etienne; Palucis, Marisa; Parker, Timothy; Parot, Yann; Patel, Kiran; Paton, Mark; Paulsen, Gale; Pavlov, Alex; Pavri, Betina; Peinado-González, Verónica; Pepin, Robert; Peret, Laurent; Perez, Rene; Perrett, Glynis; Peterson, Joe; Pilorget, Cedric; Pinet, Patrick; Pla-García, Jorge; Plante, Ianik; Poitrasson, Franck; Polkko, Jouni; Popa, Radu; Posiolova, Liliya; Pradler, Irina; Prats, Benito; Prokhorov, Vasily; Purdy, Sharon Wilson; Raaen, Eric; Radziemski, Leon; Rafkin, Scot; Ramos, Miguel; Raulin, François; Ravine, Michael; Reitz, Günther; Rennó, Nilton; Rice, Melissa; Richardson, Mark; Robert, François; Rodriguez Manfredi, José Antonio; Romeral-Planelló, Julio J.; Rowland, Scott; Saccoccio, Muriel; Salamon, Andrew; Sandoval, Jennifer; Sanin, Anton; Sans Fuentes, Sara Alejandra; Saper, Lee; Sautter, Violaine; Savijärvi, Hannu; Schieber, Juergen; Schmidt, Walter; Scholes, Daniel; Schoppers, Marcel; Schröder, Susanne; Sebastian Martinez, Eduardo; Sengstacken, Aaron; Shterts, Ruslan; Siebach, Kirsten; Siili, Tero; Simmonds, Jeff; Sirven, Jean-Baptiste; Slavney, Susie; Sletten, Ronald; Smith, Michael; Sobrón Sánchez, Pablo; Spanovich, Nicole; Spray, John; Squyres, Steven; Stack, Katie; Stalport, Fabien; Stein, Thomas; Stern, Jennifer; Stewart, Noel; Stipp, Susan Louise Svane; Stoiber, Kevin; Sucharski, Bob; Summons, Roger; Sun, Vivian; Supulver, Kimberley; Sutter, Brad; Szopa, Cyril; Tate, Christopher; Teinturier, Samuel; ten Kate, Inge Loes; Thomas, Peter; Thompson, Lucy; Tokar, Robert; Toplis, Mike; Torres Redondo, Josefina; Trainer, Melissa; Tretyakov, Vladislav; Urqui-O'Callaghan, Roser; Van Beek, Jason; Van Beek, Tessa; VanBommel, Scott; Varenikov, Alexey; Vasavada, Ashwin; Vasconcelos, Paulo; Vicenzi, Edward; Vostrukhin, Andrey; Voytek, Mary; Wadhwa, Meenakshi; Ward, Jennifer; Webster, Chris; Weigle, Eddie; Wellington, Danika; Westall, Frances; Wiens, Roger Craig; Wilhelm, Mary Beth; Williams, Amy; Williams, Joshua; Williams, Rebecca; Williams, Richard B.; Wilson, Mike; Wimmer-Schweingruber, Robert; Wolff, Mike; Wong, Mike; Wray, James; Wu, Megan; Yana, Charles; Zeitlin, Cary; Zimdar, Robert; Zorzano Mier, María-Paz

    2013-09-01

    The Rocknest aeolian deposit is similar to aeolian features analyzed by the Mars Exploration Rovers (MERs) Spirit and Opportunity. The fraction of sand Mars instrument and of the fine-grained nanophase oxide component first described from basaltic soils analyzed by MERs. The similarity between soils and aeolian materials analyzed at Gusev Crater, Meridiani Planum, and Gale Crater implies locally sourced, globally similar basaltic materials or globally and regionally sourced basaltic components deposited locally at all three locations.

  12. Wind-driven particle mobility on Mars: Insights from Mars Exploration Rover observations at "El Dorado" and surroundings at Gusev Crater

    Science.gov (United States)

    Sullivan, R.; Arvidson, R.; Bell, J.F.; Gellert, Ralf; Golombek, M.; Greeley, R.; Herkenhoff, K.; Johnson, J.; Thompson, S.; Whelley, P.; Wray, J.

    2008-01-01

    The ripple field known as 'El Dorado' was a unique stop on Spirit's traverse where dust-raising, active mafic sand ripples and larger inactive coarse-grained ripples interact, illuminating several long-standing issues of Martian dust mobility, sand mobility, and the origin of transverse aeolian ridges. Strong regional wind events endured by Spirit caused perceptible migration of ripple crests in deposits SSE of El Dorado, erasure of tracks in sandy areas, and changes to dust mantling the site. Localized thermal vortices swept across El Dorado, leaving paths of reduced dust but without perceptibly damaging nearly cohesionless sandy ripple crests. From orbit, winds responsible for frequently raising clay-sized dust into the atmosphere do not seem to significantly affect dunes composed of (more easily entrained) sand-sized particles, a long-standing paradox. This disparity between dust mobilization and sand mobilization on Mars is due largely to two factors: (1) dust occurs on the surface as fragile, low-density, sand-sized aggregates that are easily entrained and disrupted, compared with clay-sized air fall particles; and (2) induration of regolith is pervasive. Light-toned bed forms investigated at Gusev are coarse-grained ripples, an interpretation we propose for many of the smallest linear, light-toned bed forms of uncertain origin seen in high-resolution orbital images across Mars. On Earth, wind can organize bimodal or poorly sorted loose sediment into coarse-grained ripples. Coarse-grained ripples could be relatively common on Mars because development of durable, well-sorted sediments analogous to terrestrial aeolian quartz sand deposits is restricted by the lack of free quartz and limited hydraulic sediment processing. Copyright 2008 by the American Geophysical Union.

  13. Silica-rich deposits and hydrated minerals at Gusev Crater, Mars: Vis-NIR spectral characterization and regional mapping

    Science.gov (United States)

    Rice, M.S.; Bell, J.F.; Cloutis, E.A.; Wang, A.; Ruff, S.W.; Craig, M.A.; Bailey, D.T.; Johnson, J. R.; De Souza, P.A.; Farrand, W. H.

    2010-01-01

    The Mars Exploration Rover (MER) Spirit has discovered surprisingly high concentrations of amorphous silica in soil and nodular outcrops in the Inner Basin of the Columbia Hills. In Pancam multispectral observations, we find that an absorption feature at the longest Pancam wavelength (1009 nm) appears to be characteristic of these silica-rich materials; however, spectral analyses of amorphous silica suggest that the ???1009 nm spectral feature is not a direct reflection of their silica-rich nature. Based on comparisons with spectral databases, we hypothesize that the presence of H2O or OH, either free (as water ice), adsorbed or bound in a mineral structure, is responsible for the spectral feature observed by Pancam. The Gertrude Weise soil, which is nearly pure opaline silica, may have adsorbed water cold-trapped on mineral grains. The origin of the ???1009 nm Pancam feature observed in the silica-rich nodular outcrops may result from the presence of additional hydrated minerals (specific sulfates, halides, chlorides, sodium silicates, carbonates or borates). Using the ???1009 nm feature with other spectral parameters as a "hydration signature" we have mapped the occurrence of hydrated materials along the extent of Spirit's traverse across the Columbia Hills from West Spur to Home Plate (sols 155-1696). We have also mapped this hydration signature across large panoramic images to understand the regional distribution of materials that are spectrally similar to the silica-rich soil and nodular outcrops. Our results suggest that hydrated materials are common in the Columbia Hills. ?? 2009 Elsevier Inc.

  14. Comparison of some Phoenix and gusev soil types

    DEFF Research Database (Denmark)

    Walter..[], Goetz; Hviid, S.F.; Madsen, Morten Bo

    2010-01-01

    The comparison of soil particles at the Phoenix landing site and in Gusev Crater provides clues on their origin and global distribution. Some unusual Phoenix particles are possibly of (more) local origin, as they appear to be absent in Gusev dunes....

  15. Gusev Rocks Solidified from Lava (3-D)

    Science.gov (United States)

    2006-01-01

    In recent weeks, as NASA's Mars Exploration Rover Spirit has driven through the basin south of 'Husband Hill,' it has been traversing mainly sand and dune deposits. This week, though, Spirit has been maneuvering along the edge of an arc-shaped feature called 'Lorre Ridge' and has encountered some spectacular examples of basaltic rocks with striking textures. This panoramic camera (Pancam) image shows a group of boulders informally named 'FuYi.' These basaltic rocks were formed by volcanic processes and may be a primary constituent of Lorre Ridge and other interesting landforms in the basin. Spirit first encountered basalts at its landing site two years ago, on a vast plain covered with solidified lava that appeared to have flowed across Gusev Crater. Later, basaltic rocks became rare as Spirit climbed Husband Hill. The basaltic rocks that Spirit is now seeing are interesting because they exhibit many small holes or vesicles, similar to some kinds of volcanic rocks on Earth. Vesicular rocks form when gas bubbles are trapped in lava flows and the rock solidifies around the bubbles. When the gas escapes, it leaves holes in the rock. The quantity of gas bubbles in rocks on Husband Hill varies considerably; some rocks have none and some, such as several here at FuYi, are downright frothy. The change in textures and the location of the basalts may be signs that Spirit is driving along the edge of a lava flow. This lava may be the same as the basalt blanketing the plains of Spirit's landing site, or it may be different. The large size and frothy nature of the boulders around Lorre Ridge might indicate that eruptions once took place at the edge of the lava flow, where the lava interacted with the rocks of the basin floor. Scientists hope to learn more as Spirit continues to investigate these rocks. As Earth approaches the Chinese New Year (The Year of the Dog), the Athena science team decided to use nicknames representing Chinese culture and geography to identify rocks and

  16. Gusev Rocks Solidified from Lava (False Color)

    Science.gov (United States)

    2006-01-01

    In recent weeks, as NASA's Mars Exploration Rover Spirit has driven through the basin south of 'Husband Hill,' it has been traversing mainly sand and dune deposits. This week, though, Spirit has been maneuvering along the edge of an arc-shaped feature called 'Lorre Ridge' and has encountered some spectacular examples of basaltic rocks with striking textures. This panoramic camera (Pancam) image shows a group of boulders informally named 'FuYi.' These basaltic rocks were formed by volcanic processes and may be a primary constituent of Lorre Ridge and other interesting landforms in the basin. Spirit first encountered basalts at its landing site two years ago, on a vast plain covered with solidified lava that appeared to have flowed across Gusev Crater. Later, basaltic rocks became rare as Spirit climbed Husband Hill. The basaltic rocks that Spirit is now seeing are interesting because they exhibit many small holes or vesicles, similar to some kinds of volcanic rocks on Earth. Vesicular rocks form when gas bubbles are trapped in lava flows and the rock solidifies around the bubbles. When the gas escapes, it leaves holes in the rock. The quantity of gas bubbles in rocks on Husband Hill varies considerably; some rocks have none and some, such as several here at FuYi, are downright frothy. The change in textures and the location of the basalts may be signs that Spirit is driving along the edge of a lava flow. This lava may be the same as the basalt blanketing the plains of Spirit's landing site, or it may be different. The large size and frothy nature of the boulders around Lorre Ridge might indicate that eruptions once took place at the edge of the lava flow, where the lava interacted with the rocks of the basin floor. Scientists hope to learn more as Spirit continues to investigate these rocks. As Earth approaches the Chinese New Year (The Year of the Dog), the Athena science team decided to use nicknames representing Chinese culture and geography to identify rocks and

  17. Distinguishing Endogenic and Impact Craters Using Depth to Diameter Ratios and Circularities

    Science.gov (United States)

    Dorsey, R. J.; Greeley, R.

    2011-03-01

    Based on concerns for surface age dating, morphometric data from the McCartys Flow, New Mexico, was compared to craters in the Colombia Hills area in Gusev Crater, Mars, to distinguish impact craters from volcanic craters in lava flows.

  18. Initial Results on the Mineralogy and Geochemistry of the Mar Exploration Rover Gusev Landing Site

    Science.gov (United States)

    Christensen, P. R.

    2004-05-01

    The Spirit rover has investigated the geochemistry and mineralogy of the Gusev crater site using in situ Alpha Proton X-Ray, Mossbauer, visible, and infrared spectroscopy. The Gusev site is covered with angular to sub-rounded rocks that are typically less than 1 m in maximum dimension. More than 90 percent of these rocks are dark-toned, with the remainder being lighter-toned rocks that may predominantly be dark rocks with a thin (10's of microns) coating of easily removed fines. APXS analysis has been obtained of a rock (Adirondack) following the removal by grinding of the surface dust and the upper few mm of the rock surface. These data give a modal mineralogy corresponding to olivine basalt. High quality Mini-TES data have not been obtained of a completely dust-free rock surface. The Mini-TES data of Adirondack do show long wavelength (15-25 microns) absorptions due to olivine of composition ~Fo60. All of the rocks observed are very compositionally homogeneous in the Mini-TES spectra. These findings are consistent with the detection of olivine-bearing basalt at this site from orbital TES infrared spectroscopy. Mossbauer spectra of Adirondack show the presence of forsteritic olivine and magnetite, with possible pyroxene. The soils at Gusev are a mixture of reddish fine-grained to sandy materials, granular-sized particles that occur in ripple forms, and minor pebbles. Mini-TES spectra of the soil show an excellent match to the TES spectra of high-albedo, fine-grained material found in regional bright regions that is interpreted to be windblown dust. This agreement suggests at least the uppermost layer of the soil at Gusev has been accumulated from airfall dust. By analogy with prior analysis of TES data these materials contain several percent carbonate, minor bound water, and a framework silicate interpreted to be either feldspar or zeolite. APXS spectra show similar oxide abundances to those determined for the Pathfinder site, except for higher MgO, and lower

  19. Gusev Rocks Solidified from Lava (Approximate True Color)

    Science.gov (United States)

    2006-01-01

    In recent weeks, as NASA's Mars Exploration Rover Spirit has driven through the basin south of 'Husband Hill,' it has been traversing mainly sand and dune deposits. This week, though, Spirit has been maneuvering along the edge of an arc-shaped feature called 'Lorre Ridge' and has encountered some spectacular examples of basaltic rocks with striking textures. This panoramic camera (Pancam) image shows a group of boulders informally named 'FuYi.' These basaltic rocks were formed by volcanic processes and may be a primary constituent of Lorre Ridge and other interesting landforms in the basin. Spirit first encountered basalts at its landing site two years ago, on a vast plain covered with solidified lava that appeared to have flowed across Gusev Crater. Later, basaltic rocks became rare as Spirit climbed Husband Hill. The basaltic rocks that Spirit is now seeing are interesting because they exhibit many small holes or vesicles, similar to some kinds of volcanic rocks on Earth. Vesicular rocks form when gas bubbles are trapped in lava flows and the rock solidifies around the bubbles. When the gas escapes, it leaves holes in the rock. The quantity of gas bubbles in rocks on Husband Hill varies considerably; some rocks have none and some, such as several here at FuYi, are downright frothy. The change in textures and the location of the basalts may be signs that Spirit is driving along the edge of a lava flow. This lava may be the same as the basalt blanketing the plains of Spirit's landing site, or it may be different. The large size and frothy nature of the boulders around Lorre Ridge might indicate that eruptions once took place at the edge of the lava flow, where the lava interacted with the rocks of the basin floor. Scientists hope to learn more as Spirit continues to investigate these rocks. As Earth approaches the Chinese New Year (The Year of the Dog), the Athena science team decided to use nicknames representing Chinese culture and geography to identify rocks and

  20. Multispectral Imaging Results from the Mars Exploration Rover Gusev and Meridiani Landing Sites

    Science.gov (United States)

    Bell, J. F., III; Athena Science

    2004-11-01

    Multispectral images from 400 to 1000 nm from the Mars Exploration Rover Spirit and Opportunity Pancams have provided new information on the morphology, physical properties, and mineralogy of rocks and soils at Gusev and Meridiani and have played a critical role in helping to choose specific targets for detailed compositional analyses using the rovers' arm instruments. Images within the Gusev plains reveal a rock-strewn surface interspersed with moderate- to high-albedo fine-grained deposits occurring in part as drifts or in small circular hollows. Optically thick coverings or coatings of fine-grained ferric-rich dust dominate most bright soil and rock surfaces. Spectra of some darker rock surfaces show near-IR signatures consistent with mafic silicates like pyroxene or olivine. Imaging in the Columbia Hills reveals evidence for outcrop, layered materials, and a different style of physical and/or chemical weathering of some rocks than in the plains. At Meridiani, images within Eagle crater and in the plains during the traverse to Endurance crater reveal a low-albedo, generally flat and rock-free surface. Outcrops of higher-albedo, red, laminated rocks are observed within and around small craters, riftlike cracks in the plains, and well into Endurance crater. Fine-grained materials include dark ferrous-Fe rich basaltic sand, angular rock clasts, bright dust, and mm-size, low- and high-albedo spherical granules (spherules) that occur within and near the bright outcrop. Spectra of the low-albedo sand, small rock clasts, and one larger dark rock found on the plains show near-IR signatures consistent with the presence of pyroxene or olivine. Spectra of the dark spherules are consistent with the presence of crystalline ferric oxides/oxyhydroxides, supporting their interpretation as concretions. Bright spherule spectra are consistent with dark spherules covered or coated by nanocrystalline ferric-rich dust. Spectra of the laminated outcrop materials indicate the presence

  1. 'McMurdo' Panorama from Spirit's 'Winter Haven'

    Science.gov (United States)

    2006-01-01

    This 360-degree view, called the 'McMurdo' panorama, comes from the panoramic camera (Pancam) on NASA's Mars Exploration Rover Spirit. From April through October 2006, Spirit has stayed on a small hill known as 'Low Ridge.' There, the rover's solar panels are tilted toward the sun to maintain enough solar power for Spirit to keep making scientific observations throughout the winter on southern Mars. This view of the surroundings from Spirit's 'Winter Haven' is presented in approximately true color. Oct. 26, 2006, marks Spirit's 1,000th sol of what was planned as a 90-sol mission. (A sol is a Martian day, which lasts 24 hours, 39 minutes, 35 seconds). The rover has lived through the most challenging part of its second Martian winter. Its solar power levels are rising again. Spring in the southern hemisphere of Mars will begin in early 2007. Before that, the rover team hopes to start driving Spirit again toward scientifically interesting places in the 'Inner Basin' and 'Columbia Hills' inside Gusev crater. The McMurdo panorama is providing team members with key pieces of scientific and topographic information for choosing where to continue Spirit's exploration adventure. The Pancam began shooting component images of this panorama during Spirit's sol 814 (April 18, 2006) and completed the part shown here on sol 932 (Aug. 17, 2006). The panorama was acquired using all 13 of the Pancam's color filters, using lossless compression for the red and blue stereo filters, and only modest levels of compression on the remaining filters. The overall panorama consists of 1,449 Pancam images and represents a raw data volume of nearly 500 megabytes. It is thus the largest, highest-fidelity view of Mars acquired from either rover. Additional photo coverage of the parts of the rover deck not shown here was completed on sol 980 (Oct. 5 , 2006). The team is completing the processing and mosaicking of those final pieces of the panorama, and that image will be released on the Web shortly

  2. 'McMurdo' Panorama from Spirit's 'Winter Haven' (False Color)

    Science.gov (United States)

    2006-01-01

    This 360-degree view, called the 'McMurdo' panorama, comes from the panoramic camera (Pancam) on NASA's Mars Exploration Rover Spirit. From April through October 2006, Spirit has stayed on a small hill known as 'Low Ridge.' There, the rover's solar panels are tilted toward the sun to maintain enough solar power for Spirit to keep making scientific observations throughout the winter on southern Mars. This view of the surroundings from Spirit's 'Winter Haven' is presented in exaggerated color to enhance color differences among rocks, soils and sand. Oct. 26, 2006, marks Spirit's 1,000th sol of what was planned as a 90-sol mission. (A sol is a Martian day, which lasts 24 hours, 39 minutes, 35 seconds). The rover has lived through the most challenging part of its second Martian winter. Its solar power levels are rising again. Spring in the southern hemisphere of Mars will begin in early 2007. Before that, the rover team hopes to start driving Spirit again toward scientifically interesting places in the 'Inner Basin' and 'Columbia Hills' inside Gusev crater. The McMurdo panorama is providing team members with key pieces of scientific and topographic information for choosing where to continue Spirit's exploration adventure. The Pancam began shooting component images of this panorama during Spirit's sol 814 (April 18, 2006) and completed the part shown here on sol 932 (Aug. 17, 2006). The panorama was acquired using all 13 of the Pancam's color filters, using lossless compression for the red and blue stereo filters, and only modest levels of compression on the remaining filters. The overall panorama consists of 1,449 Pancam images and represents a raw data volume of nearly 500 megabytes. It is thus the largest, highest-fidelity view of Mars acquired from either rover. Additional photo coverage of the parts of the rover deck not shown here was completed on sol 980 (Oct. 5 , 2006). The team is completing the processing and mosaicking of those final pieces of the panorama

  3. 'McMurdo' Panorama from Spirit's 'Winter Haven' (Color Stereo)

    Science.gov (United States)

    2006-01-01

    [figure removed for brevity, see original site] Left-eye view of a stereo pair for PIA01905 [figure removed for brevity, see original site] Right-eye view of a stereo pair for PIA01905 This 360-degree view, called the 'McMurdo' panorama, comes from the panoramic camera (Pancam) on NASA's Mars Exploration Rover Spirit. From April through October 2006, Spirit has stayed on a small hill known as 'Low Ridge.' There, the rover's solar panels are tilted toward the sun to maintain enough solar power for Spirit to keep making scientific observations throughout the winter on southern Mars. This view of the surroundings from Spirit's 'Winter Haven' is presented as a stereo anaglyph to show the scene three-dimensionally when viewed through red-blue glasses (with the red lens on the left). Oct. 26, 2006, marks Spirit's 1,000th sol of what was planned as a 90-sol mission. (A sol is a Martian day, which lasts 24 hours, 39 minutes, 35 seconds). The rover has lived through the most challenging part of its second Martian winter. Its solar power levels are rising again. Spring in the southern hemisphere of Mars will begin in early 2007. Before that, the rover team hopes to start driving Spirit again toward scientifically interesting places in the 'Inner Basin' and 'Columbia Hills' inside Gusev crater. The McMurdo panorama is providing team members with key pieces of scientific and topographic information for choosing where to continue Spirit's exploration adventure. The Pancam began shooting component images of this panorama during Spirit's sol 814 (April 18, 2006) and completed the part shown here on sol 932 (Aug. 17, 2006). The panorama was acquired using all 13 of the Pancam's color filters, using lossless compression for the red and blue stereo filters, and only modest levels of compression on the remaining filters. The overall panorama consists of 1,449 Pancam images and represents a raw data volume of nearly 500 megabytes. It is thus the largest, highest-fidelity view of Mars

  4. 'McMurdo' Panorama from Spirit's 'Winter Haven' (Stereo)

    Science.gov (United States)

    2006-01-01

    This 360-degree view, called the 'McMurdo' panorama, comes from the panoramic camera (Pancam) on NASA's Mars Exploration Rover Spirit. From April through October 2006, Spirit has stayed on a small hill known as 'Low Ridge.' There, the rover's solar panels are tilted toward the sun to maintain enough solar power for Spirit to keep making scientific observations throughout the winter on southern Mars. This view of the surroundings from Spirit's 'Winter Haven' is presented as a stereo anaglyph to show the scene three-dimensionally when viewed through red-blue glasses (with the red lens on the left). Oct. 26, 2006, marks Spirit's 1,000th sol of what was planned as a 90-sol mission. (A sol is a Martian day, which lasts 24 hours, 39 minutes, 35 seconds). The rover has lived through the most challenging part of its second Martian winter. Its solar power levels are rising again. Spring in the southern hemisphere of Mars will begin in early 2007. Before that, the rover team hopes to start driving Spirit again toward scientifically interesting places in the 'Inner Basin' and 'Columbia Hills' inside Gusev crater. The McMurdo panorama is providing team members with key pieces of scientific and topographic information for choosing where to continue Spirit's exploration adventure. The Pancam began shooting component images of this panorama during Spirit's sol 814 (April 18, 2006) and completed the part shown here on sol 932 (Aug. 17, 2006). The panorama was acquired using all 13 of the Pancam's color filters, using lossless compression for the red and blue stereo filters, and only modest levels of compression on the remaining filters. The overall panorama consists of 1,449 Pancam images and represents a raw data volume of nearly 500 megabytes. It is thus the largest, highest-fidelity view of Mars acquired from either rover. Additional photo coverage of the parts of the rover deck not shown here was completed on sol 980 (Oct. 5 , 2006). The team is completing the processing and

  5. Spirit Hits a Home Run

    Science.gov (United States)

    2006-01-01

    This week, NASA's Mars Exploration Rover Spirit arrived at 'Home Plate,' a feature that, when seen from orbit, looks like the home plate of a baseball diamond. Home Plate is a roughly circular feature about 80 meters (260 feet) in diameter that might be an old impact crater or volcanic feature. The Spirit team has been eager to get to Home Plate and has been enjoying distant views of the feature and a curious 'bathtub ring' of light-colored materials along its edges. The team has pushed the rover hard to get here before the deep Martian winter sets in. After scientists had identified Home Plate from orbit, they had many theories about what it could be and what they might see. But when Spirit's panoramic camera (Pancam) took this and other images, the science team was stunned. This Pancam image is of an outcrop nicknamed 'Barnhill' and surrounding rocks on the north side of Home Plate, showing the most spectacular layering that Spirit has seen. Pancam and microscopic imager views of the layers in the rocks reveal a range of grain sizes and textures that change from the lower to the upper part of the outcrop. This may help scientists figure out how the material was emplaced. Spirit is also conducting work with its arm instruments to figure out the chemistry and mineralogy of the rocks. Scientists have several hypotheses about what Home Plate could be, including features made by volcanoes and impact craters, and ways that water could have played a role. They are busy trying to figure out what the data from Spirit is really telling us. As Spirit works at Home Plate during February, the science team is choosing informal names for rocks from the great players and managers of the Negro Leagues of baseball. This outcrop, 'Barnhill,' is informally named for David Barnhill, the ace of the New York Cubans' pitching staff during the early 1940s. He compiled an 18-3 record in 1941 and defeated Satchel Paige in the 1942 East-West all-star game. Other rocks in the area are

  6. Sancti Spirit

    Directory of Open Access Journals (Sweden)

    Torroja, Eduardo

    1962-02-01

    Full Text Available Mucho más alto que el último pueblo del valle, a 1.500 metros de altitud, las aguas del San Nicolau, cansadas de saltar cascadas, se detienen a lo largo de unos pocos kilómetros, entreteniéndose en suaves meandros antes de volver a precipitarse en otra cascada mayor. La nieve cubre esa región la mayor parte del año, y en los meses de verano es lugar delicioso para el excursionista y el pescador de truchas. Sólo las tormentas bruscas, violentas y breves llegan con frecuencia a turbar la paz de su reposo en aquel edén. Puede cobijarse entonces bajo la media naranja del refugio, orientada a sotavento; y mientras pasa el aguacero, contemplar sus frescos inspirados por el nombre del lugar: Sancti Spirit.

  7. Aqueous Alteration of Endeavour Crater Rim Apron Rocks

    Science.gov (United States)

    Mittlefehldt, David W.; Ming, Douglas W.; Gellert, Ralf; Clark, Benton C.; Morris, Richard V.; Yen, Albert S.; Arvidson, Raymond E.; Crumpler, Larry S.; Farrand, William H.; Grant, John A.; hide

    2014-01-01

    Mars Exploration Rover Opportunity is exploring Noachian age rocks of the rim of 22 km diameter Endeavour crater. Overlying the pre-impact lithologies and rim breccias is a thin apron of fine-grained sediments, the Grasberg fm, forming annuli on the lower slopes of rim segments. Hesperian Burns fm sandstones overly the Grasberg fm. Grasberg rocks have major element compositions that are distinct from Burns fm sandstones, especially when comparing interior compositions exposed by the Rock Abrasion Tool. Grasberg rocks are also different from Endeavour rim breccias, but have general compositional similarities to them. Grasberg sediments are plausibly fine-grained materials derived from the impact breccias. Veins of CaSO4 transect Grasberg fm rocks demonstrating post-formation aqueous alteration. Minor/trace elements show variations consistent with mobilization by aqueous fluids. Grasberg fm rocks have low Mn and high Fe/Mn ratios compared to the other lithologies. Manganese likely was mobilized and removed from the Grasberg host rock by redox reactions. We posit that Fe2+ from acidic solutions associated with formation of the Burns sulfate-rich sandstones acted as an electron donor to reduce more oxidized Mn to Mn2+. The Fe contents of Grasberg rocks are slightly higher than in other rocks suggesting precipitation of Fe phases in Grasberg materials. Pancam spectra show that Grasberg rocks have a higher fraction of ferric oxide minerals than other Endeavour rim rocks. Solutions transported Mn2+ into the Endeavour rim materials and oxidized and/or precipitated it in them. Grasberg has higher contents of the mobile elements K, Zn, Cl, and Br compared to the rim materials. Similar enrichments of mobile elements were measured by the Spirit APXS on West Spur and around Home Plate in Gusev crater. Enhancements in these elements are attributed to interactions of hydrothermal acidic fluids with the host rocks. Interactions of fluids with the Grasberg fm postdate the genesis

  8. Filled Craters

    Science.gov (United States)

    2006-01-01

    11 May 2006 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows adjacent impact craters located north-northwest of the Acheron Fossae region of Mars. The two craters are of similar size and formed by meteor impacts. However, one is much more filled than the other, indicating that it is older. The surface of the material in the older, partially-filled crater has a texture similar to the crater's surroundings. The southern (bottom) crater is bowl-shaped and is also partially-filled, however, the filling material seems to be limited to the southern half of the crater. Location near: 44.6oN, 128.4oW Image width: 3 km (1.9 mi) Illumination from: lower left Season: Northern Winter

  9. Secondary Craters

    Science.gov (United States)

    2005-01-01

    7 October 2005 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a cluster of craters in far western Arabia Terra. The crater cluster is oriented along a line that runs nearly east-west (left-right) across the scene. Clusters of craters positioned along a line like this are secondary craters -- that is, they formed as the result of a much larger meteor, asteroid, or cometary impact somewhere else in the region. These craters do not form from the object that impacted Mars to form the larger, primary crater; these are the product of the impact of the rocks and debris thrown out by the larger impact. Location near: 14.9oN, 19.3oW Image width: width: 3 km (1.9 mi) Illumination from: lower left Season: Northern Autumn

  10. Lonely Crater

    Science.gov (United States)

    2005-01-01

    24 December 2005 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a full-resolution (1.5 meters/5 feet per pixel) view of an old meteor impact crater, somewhat filled with sediment. This crater is located near a larger crater, Newcomb, in far northern Noachis Terra. Location near: 22.1oS, 1.1oW Image width: 1 km (0.6 mi) Illumination from: upper left Season: Southern Spring

  11. Exhumed Craters

    Science.gov (United States)

    2004-01-01

    5 July 2004 Burial and exhumation is a theme that repeats itself, all over the surface of Mars. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows several north mid-latitude meteor impact craters with bouldery ejecta deposits. Each of the craters was once buried and later exhumed. Mesas on the floors of these craters are remnants of the materials that once filled and covered them. The craters are located near 39.7oN, 206.0oW. The image covers an area about 3 km (1.9 mi) wide; sunlight illuminates the scene from the lower left.

  12. Buried Crater

    Science.gov (United States)

    2004-01-01

    29 September 2004 The circular feature in this Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image is the location of a buried impact crater in southern Noachis Terra near 55.4oS, 325.1oW. The image covers an area about 3 km (1.9 mi) across; thus the crater is roughly 2 km in diameter, or twice the size of the famous Meteor Crater in northern Arizona. A visitor to the Arizona Crater would be quite impressed by the height of its raised rims and the depth of and distance across its bowl, relative to a person. At the human scale It is challenging to imagine a crater twice that size that has been filled and buried by sediment and debris, yet the crater shown here is simply an example. On Mars, craters over 100 km in diameter have been buried, and some have been exhumed. This image is illuminated by sunlight from the upper left.

  13. Impact Crater

    Science.gov (United States)

    2006-01-01

    16 January 2006 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows an impact crater, roughly the size of the famous Meteor Crater in northern Arizona, U.S.A., in western Elysium Planitia. Light-toned, windblown ripples of sediment have accumulated in subtle troughs and in the lee -- the downwind side -- of the crater. Location near: 28.4oN, 247.9oW Image width: 3 km (1.9 mi) Illumination from: lower left Season: Northern Winter

  14. Fresh Crater

    Science.gov (United States)

    2004-01-01

    30 July 2004 This full-resolution (1.5 meters, 5 feet, per pixel) Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a fairly small, fresh meteor impact crater in far southeastern Arabia Terra. The crater's bowl, rim, and ejecta exhibit numerous boulders. The image covers an area about 3 km (1.9 mi) wide and is located near 6.9oS, 317.1oW. Sunlight illuminates the terrain from the left.

  15. Impact cratering

    Indian Academy of Sciences (India)

    In addition, further improvement of our understanding of the physico–chemical and geological processes fundamental to the impact cratering process is required for reliable numerical modeling of the process, and also for the correlation of impact magnitude and environmental effects. Over the last few decades, impact ...

  16. Asymmetric Crater

    Science.gov (United States)

    2004-01-01

    [figure removed for brevity, see original site] Released 18 December 2003Asymmetric craters such as the one in the center of this image are fairly rare. The more typical symmetric craters are formed when meteors impact a surface over a wide range of angles. Only very low impact angles (within 15o of horizontal) result in asymmetric structures such as this one. The bilateral symmetry of the ejecta, like two wings on either side of the elliptical crater, is typical of oblique impacts. The small crater downrange from the main crater could have been caused by the impactor breaking apart before impact or possibly a 'decapitation' of the impactor as it hit with the 'head' traveling farther to form the smaller structure.Image information: VIS instrument. Latitude -8.5, Longitude 227.5 East (132.5 West). 19 meter/pixel resolution.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

  17. Galle Crater

    Science.gov (United States)

    2002-01-01

    (Released 19 June 2002) The Science This image is of part of Galle Crater, located at 51.9S, 29.5W. This image was taken far enough south and late enough into the southern hemisphere fall to catch observe water ice clouds partially obscuring the surface. The most striking aspect of the surface is the dissected layered unit to the left in the image. Other areas also appear to have layering, but they are either more obscured by clouds or are less well defined on the surface. The layers appear to be mostly flat lying and layer boundaries appear as topographic lines would on a map, but there are a few areas where it appears that these layers have been deformed to some level. Other areas of the image contain rugged, mountainous terrain as well as a separate pitted terrain where the surface appears to be a separate unit from the mountains and the layered terrain. The Story Galle Crater is officially named after a German astronomer who, in 1846, was the first to observe the planet Neptune. It is better known, however, as the 'Happy Face Crater.' The image above focuses on too small an area of the crater to see its beguiling grin, but you can catch the rocky line of a 'half-smile' in the context image to the right (to the left of the red box). While water ice clouds make some of the surface harder to see, nothing detracts from the fabulous layering at the center left-hand edge of the image. If you click on the above image, the scalloped layers almost look as if a giant knife has swirled through a landscape of cake frosting. These layers, the rugged, mountains near them, and pits on the surface (upper to middle section of the image on the right-hand side) all create varying textures on the crater floor. With such different features in the same place, geologists have a lot to study to figure out what has happened in the crater since it formed.

  18. Centrifuge impact cratering experiment 5

    Science.gov (United States)

    1984-01-01

    Transient crates motions, cratering flow fields, crates dynamics, determining impact conditions from total crater welt, centrifuge quarter-space cratering, and impact cratering mechanics research is documented.

  19. Multispectral VNIR Observations by the Opportunity Rover Pancam of Multiple Episodes of Aqueous Alteration in Marathon Valley, Endeavour Crater, Mars

    Science.gov (United States)

    Farrand, William H.; Bell, James F., III; Johnson, Jeffrey R.; Arvidson, Raymond E.; Mittlefehldt, David W.; Ruff, Steven W.; Rice, Melissa S.

    2016-01-01

    Since early 2015, the Mars Exploration Rover Opportunity has been exploring the break in the rim of Endeavour Crater dubbed Marathon Valley by the rover team. Marathon Valley was identified by orbital hyperspectral data from the MRO CRISM as having a relatively strong spectral feature in the 2.3 micrometer region indicative of an Mg or Fe-OH combination overtone absorption band indicative of smectite clay. Earlier in its mission, Opportunity examined the Matijevic Hill region on the more northerly Cape York crater rim segment and found evidence for smectite clays in a stratigraphically lower, pre-impact formed unit dubbed the Matijevic formation. However, the smectite exposures in Marathon Valley appear to be associated with the stratigraphically higher Shoemaker formation impact breccia. Evidence for alteration in this unit in Marathon Valley is provided by Pancam multispectral observations in the 430 to 1010 nm visible/near infrared (VNIR) spectral range. Sinuous troughs ("red zones") contain fragmented cobbles and pebbles displaying higher blue-to-red slopes, moderately higher 535 nm band depths, elevated 754 to 934 nm, and negative 934 to 1009 nm slopes. The lack of an absorption at 864 to 904 nm indicates the lack of crystalline red hematite in these red zones, but likely an enrichment in nanophase ferric oxides. The negative 934 to 1009 nm slope is potentially indicative of the presence of adsorbed or structurally bound water. A scuff in a red zone near the southern wall of Marathon Valley uncovered light-toned soils and a pebble with an 803 to 864 nm absorption resembling that of light-toned Fe-sulfate bearing soils uncovered by the Spirit rover in the Columbia Hills of Gusev crater. APXS chemical measurements indicated enrichments of Mg and S in the scuff soils and the pebble, Joseph Field, with the strongest 803 nm band- consistent with Mg and Fe sulfates. The presence of Fe and Mg sulfates can be interpreted as evidence of a potentially later episode of

  20. SPIRIT 2013 Statement

    DEFF Research Database (Denmark)

    Chan, An-Wen; Tetzlaff, Jennifer M; Altman, Douglas G

    2013-01-01

    The protocol of a clinical trial serves as the foundation for study planning, conduct, reporting, and appraisal. However, trial protocols and existing protocol guidelines vary greatly in content and quality. This article describes the systematic development and scope of SPIRIT (Standard Protocol......; it does not prescribe how to design or conduct a trial. By providing guidance for key content, the SPIRIT recommendations aim to facilitate the drafting of high-quality protocols. Adherence to SPIRIT would also enhance the transparency and completeness of trial protocols for the benefit of investigators...

  1. Cutting Craters

    Science.gov (United States)

    2003-01-01

    [figure removed for brevity, see original site] Released 12 November 2003The rims of two old and degraded impact craters are intersected by a graben in this THEMIS image taken near Mangala Fossa. Yardangs and low-albedo wind streaks are observed at the top of the image as well as interesting small grooves on the crater floor. The origin of these enigmatic grooves may be the result of mud or lava and volatile interactions. Variable surface textures observed in the bottom crater floor are the result of different aged lava flows.Image information: VIS instrument. Latitude -15.2, Longitude 219.2 East (140.8 West). 19 meter/pixel resolution.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

  2. Crater Copernicus

    Science.gov (United States)

    1999-01-01

    HUBBLE SHOOTS THE MOON in a change of venue from peering at the distant universe, NASA's Hubble Space Telescope has taken a look at Earth's closest neighbor in space, the Moon. Hubble was aimed at one of the Moon's most dramatic and photogenic targets, the 58 mile-wide (93 km) impact crater Copernicus. The image was taken while the Space Telescope Imaging Spectrograph(STIS) was aimed at a different part of the moon to measure the colors of sunlight reflected off the Moon. Hubble cannot look at the Sun directly and so must use reflected light to make measurements of the Sun's spectrum. Once calibrated by measuring the Sun's spectrum, the STIS can be used to study how the planets both absorb and reflect sunlight.(upper left)The Moon is so close to Earth that Hubble would need to take a mosaic of 130 pictures to cover the entire disk. This ground-based picture from Lick Observatory shows the area covered in Hubble's photomosaic with the WideField Planetary Camera 2..(center)Hubble's crisp bird's-eye view clearly shows the ray pattern of bright dust ejected out of the crater over one billion years ago, when an asteroid larger than a mile across slammed into the Moon. Hubble can resolve features as small as 600 feet across in the terraced walls of the crater, and the hummock-like blanket of material blasted out by the meteor impact.(lower right)A close-up view of Copernicus' terraced walls. Hubble can resolve features as small as 280 feet across.

  3. Degraded Crater

    Science.gov (United States)

    2004-01-01

    21 October 2004 Near the center of this Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image lies the degraded remnants of an old meteor impact crater. The terrain in which it occurs is a heavily eroded, north middle-latitude surface. The image is located in the fretted terrains north of Arabia Terra near 41.3oN, 305.8oW. The image covers an area about 3 km (1.9 mi) wide and sunlight illuminates the scene from the lower left.

  4. Exhuming Craters

    Science.gov (United States)

    2005-01-01

    30 July 2005 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a wind-eroded landscape in the Amazonis Mensa region of far western Tharsis. Two meteor impact craters that formed in -- and then were buried by -- rock are now found in a state of partial-exhumation from within the wind-eroded material. Location near: 2.0oN, 147.3oW Image width: width: 3 km (1.9 mi) Illumination from: lower left Season: Northern Autumn

  5. Discerning the Spirits

    DEFF Research Database (Denmark)

    Pedersen, Else Marie Wiberg

    2007-01-01

    This response to Swedish scholar Jayne Svenungsson's keynote on the return of spirituality sets off by agreeing in general to her thesis that there is a return of spirituality - or rather a return of the Spirit. But whilst Svenungsson in her paper endeavours to see the return of spirituality...

  6. INCULCATING ENTREPRENEURIAL SPIRIT THROUGH ...

    African Journals Online (AJOL)

    JONATHAN

    this paper advocates the use and teaching of indigenous languages (Igbo) not only from primary and post-primary level ... process of inculcating entrepreneurial spirit should start at the elementary school level through ... productively in their indigenous languages and posits that, "A Scientific impetus or technology acquired ...

  7. Martian Meteor Crater

    Science.gov (United States)

    2004-01-01

    20 February 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a fairly young meteor impact crater on Mars that is about the same size ( 1 kilometer; 0.62 miles) as the famous Meteor Crater in northern Arizona, U.S.A. Like the Arizona crater, boulders of ejected bedrock can be seen on the crater's ejecta blanket and in the crater itself. This crater is located in the Aethiopis region of Mars near 4.7oN, 224.1oW. Sunlight illuminates the scene from the lower left.

  8. Dome craters on Ganymede

    International Nuclear Information System (INIS)

    Moore, J.M.; Malin, M.C.

    1987-01-01

    Voyager observations reveal impact craters on Ganymede that are characterized by the presence of broad, high albedo, topographic domes situated within a central pit. Fifty-seven craters with central domes were identified in images covering approx. 50% of the surface. Owing to limitations in resolution, and viewing and illumination angles, the features identified are most likely a subset of dome craters. The sample appears to be sufficiently large to infer statistically meaningful trends. Dome craters appear to fall into two distinct populations on plots of the ratio of dome diameter to crater rim diameter, large-dome craters and small-dome craters. The two classes are morphologically distinct from one another. In general, large dome craters show little relief and their constituent landforms appear subdued with respect to fresh craters. The physical attributes of small-dome craters are more sharply defined, a characteristic they share with young impact craters of comparable size observed elsewhere in the solar system. Both types of dome craters exhibit central pits in which the dome is located. As it is difficult to produce domes by impact and/or erosional processes, an endogenic origin for the domes is reasonably inferred. Several hypotheses for their origin are proposed. These hypotheses are briefly reviewed

  9. Impact craters on Titan

    Science.gov (United States)

    Wood, Charles A.; Lorenz, Ralph; Kirk, Randy; Lopes, Rosaly; Mitchell, Karl; Stofan, Ellen; ,

    2010-01-01

    Five certain impact craters and 44 additional nearly certain and probable ones have been identified on the 22% of Titan's surface imaged by Cassini's high-resolution radar through December 2007. The certain craters have morphologies similar to impact craters on rocky planets, as well as two with radar bright, jagged rims. The less certain craters often appear to be eroded versions of the certain ones. Titan's craters are modified by a variety of processes including fluvial erosion, mass wasting, burial by dunes and submergence in seas, but there is no compelling evidence of isostatic adjustments as on other icy moons, nor draping by thick atmospheric deposits. The paucity of craters implies that Titan's surface is quite young, but the modeled age depends on which published crater production rate is assumed. Using the model of Artemieva and Lunine (2005) suggests that craters with diameters smaller than about 35 km are younger than 200 million years old, and larger craters are older. Craters are not distributed uniformly; Xanadu has a crater density 2-9 times greater than the rest of Titan, and the density on equatorial dune areas is much lower than average. There is a small excess of craters on the leading hemisphere, and craters are deficient in the north polar region compared to the rest of the world. The youthful age of Titan overall, and the various erosional states of its likely impact craters, demonstrate that dynamic processes have destroyed most of the early history of the moon, and that multiple processes continue to strongly modify its surface. The existence of 24 possible impact craters with diameters less than 20 km appears consistent with the Ivanov, Basilevsky and Neukum (1997) model of the effectiveness of Titan's atmosphere in destroying most but not all small projectiles.

  10. Degraded Crater Rim

    Science.gov (United States)

    2002-01-01

    (Released 3 May 2002) The Science The eastern rim of this unnamed crater in Southern Arabia Terra is very degraded (beaten up). This indicates that this crater is very ancient and has been subjected to erosion and subsequent bombardment from other impactors such as asteroids and comets. One of these later (younger) craters is seen in the upper right of this image superimposed upon the older crater rim material. Note that this smaller younger crater rim is sharper and more intact than the older crater rim. This region is also mantled with a blanket of dust. This dust mantle causes the underlying topography to take on a more subdued appearance. The Story When you think of Arabia, you probably think of hot deserts and a lot of profitable oil reserves. On Mars, however, Southern Arabia Terra is a cold place of cratered terrain. This almost frothy-looking image is the badly battered edge of an ancient crater, which has suffered both erosion and bombardment from asteroids, comets, or other impacting bodies over the long course of its existence. A blanket of dust has also settled over the region, which gives the otherwise rugged landscape a soft and more subdued appearance. The small, round crater (upper left) seems almost gemlike in its setting against the larger crater ring. But this companionship is no easy romance. Whatever formed the small crater clearly whammed into the larger crater rim at some point, obliterating part of its edge. You can tell the small crater was formed after the first and more devastating impact, because it is laid over the other larger crater. How much younger is the small one? Well, its rim is also much sharper and more intact, which gives a sense that it is probably far more youthful than the very degraded, ancient crater.

  11. Large Crater Clustering tool

    Science.gov (United States)

    Laura, Jason; Skinner, James A.; Hunter, Marc A.

    2017-08-01

    In this paper we present the Large Crater Clustering (LCC) tool set, an ArcGIS plugin that supports the quantitative approximation of a primary impact location from user-identified locations of possible secondary impact craters or the long-axes of clustered secondary craters. The identification of primary impact craters directly supports planetary geologic mapping and topical science studies where the chronostratigraphic age of some geologic units may be known, but more distant features have questionable geologic ages. Previous works (e.g., McEwen et al., 2005; Dundas and McEwen, 2007) have shown that the source of secondary impact craters can be estimated from secondary impact craters. This work adapts those methods into a statistically robust tool set. We describe the four individual tools within the LCC tool set to support: (1) processing individually digitized point observations (craters), (2) estimating the directional distribution of a clustered set of craters, back projecting the potential flight paths (crater clusters or linearly approximated catenae or lineaments), (3) intersecting projected paths, and (4) intersecting back-projected trajectories to approximate the local of potential source primary craters. We present two case studies using secondary impact features mapped in two regions of Mars. We demonstrate that the tool is able to quantitatively identify primary impacts and supports the improved qualitative interpretation of potential secondary crater flight trajectories.

  12. An Embarrassment of Spirits: Spirits, Hauntology and Democracy in Indonesia

    DEFF Research Database (Denmark)

    Bubandt, Nils Ole

    2014-01-01

    Kyai Muzakkin is the spiritual leader of a Koranic school (pesantren) in East Java that he claims is the only pesantren in the world that is attended entirely by spirits (jin). Kyai Muzakkin is also the founder of an anti-corruption NGO. In 2009, he gained national notoriety and infamy when he...... combined his vocational interest in spirits and anti-corruption and sent a thousand spirits to Jakarta to protect the supporters of the Indonesian president at an anti-corruption rally. The introduction of spirits into the increasingly ‘occult’ Indonesian politics of 2009 was as apt as it was embarrassing...... effects....

  13. Developing students’ entrepreneurial spirit

    Directory of Open Access Journals (Sweden)

    Grădinaru, E.

    2012-01-01

    Full Text Available This paper contains a research study about the necessity to develop the entrepreneurial spirit in universities and how students could be involved in such initiatives. A qualitative research based on three focus groups was conducted, having as main objective to identify students’ opinions regarding the initiative to develop an on-line magazine for students and young people. The results reveal that students prefer the online media to the traditional ones and the pilot numbers of the magazine received good appreciations. A business plan for the future development of the magazine is also presented.

  14. X-ray Diffraction Results from Mars Science Laboratory: Mineralogy of Rocknest at Gale Crater

    Science.gov (United States)

    Bish, D. L.; Blake, D. F.; Vaniman, D. T.; Chipera, S. J.; Morris, R. V.; Ming, D. W.; Treiman, A. H.; Sarrazin, P.; Morrison, S. M.; Downs, R. T.; Achilles, C. N.; Yen, A. S.; Bristow, T. F.; Crisp, J. A.; Morookian, J. M.; Farmer, J. D.; Rampe, E. B.; Stolper, E. M.; Spanovich, N.; Achilles, Cherie; Agard, Christophe; Verdasca, José Alexandre Alves; Anderson, Robert; Anderson, Ryan; Archer, Doug; Armiens-Aparicio, Carlos; Arvidson, Ray; Atlaskin, Evgeny; Atreya, Sushil; Aubrey, Andrew; Baker, Burt; Baker, Michael; Balic-Zunic, Tonci; Baratoux, David; Baroukh, Julien; Barraclough, Bruce; Bean, Keri; Beegle, Luther; Behar, Alberto; Bell, James; Bender, Steve; Benna, Mehdi; Bentz, Jennifer; Berger, Gilles; Berger, Jeff; Berman, Daniel; Bish, David; Blake, David F.; Avalos, Juan J. Blanco; Blaney, Diana; Blank, Jen; Blau, Hannah; Bleacher, Lora; Boehm, Eckart; Botta, Oliver; Böttcher, Stephan; Boucher, Thomas; Bower, Hannah; Boyd, Nick; Boynton, Bill; Breves, Elly; Bridges, John; Bridges, Nathan; Brinckerhoff, William; Brinza, David; Bristow, Thomas; Brunet, Claude; Brunner, Anna; Brunner, Will; Buch, Arnaud; Bullock, Mark; Burmeister, Sönke; Cabane, Michel; Calef, Fred; Cameron, James; Campbell, John "Iain"; Cantor, Bruce; Caplinger, Michael; Rodríguez, Javier Caride; Carmosino, Marco; Blázquez, Isaías Carrasco; Charpentier, Antoine; Chipera, Steve; Choi, David; Clark, Benton; Clegg, Sam; Cleghorn, Timothy; Cloutis, Ed; Cody, George; Coll, Patrice; Conrad, Pamela; Coscia, David; Cousin, Agnès; Cremers, David; Crisp, Joy; Cros, Alain; Cucinotta, Frank; d'Uston, Claude; Davis, Scott; Day, Mackenzie "Kenzie"; Juarez, Manuel de la Torre; DeFlores, Lauren; DeLapp, Dorothea; DeMarines, Julia; DesMarais, David; Dietrich, William; Dingler, Robert; Donny, Christophe; Downs, Bob; Drake, Darrell; Dromart, Gilles; Dupont, Audrey; Duston, Brian; Dworkin, Jason; Dyar, M. Darby; Edgar, Lauren; Edgett, Kenneth; Edwards, Christopher; Edwards, Laurence; Ehlmann, Bethany; Ehresmann, Bent; Eigenbrode, Jen; Elliott, Beverley; Elliott, Harvey; Ewing, Ryan; Fabre, Cécile; Fairén, Alberto; Farley, Ken; Farmer, Jack; Fassett, Caleb; Favot, Laurent; Fay, Donald; Fedosov, Fedor; Feldman, Jason; Feldman, Sabrina; Fisk, Marty; Fitzgibbon, Mike; Flesch, Greg; Floyd, Melissa; Flückiger, Lorenzo; Forni, Olivier; Fraeman, Abby; Francis, Raymond; François, Pascaline; Franz, Heather; Freissinet, Caroline; French, Katherine Louise; Frydenvang, Jens; Gaboriaud, Alain; Gailhanou, Marc; Garvin, James; Gasnault, Olivier; Geffroy, Claude; Gellert, Ralf; Genzer, Maria; Glavin, Daniel; Godber, Austin; Goesmann, Fred; Goetz, Walter; Golovin, Dmitry; Gómez, Felipe Gómez; Gómez-Elvira, Javier; Gondet, Brigitte; Gordon, Suzanne; Gorevan, Stephen; Grant, John; Griffes, Jennifer; Grinspoon, David; Grotzinger, John; Guillemot, Philippe; Guo, Jingnan; Gupta, Sanjeev; Guzewich, Scott; Haberle, Robert; Halleaux, Douglas; Hallet, Bernard; Hamilton, Vicky; Hardgrove, Craig; Harker, David; Harpold, Daniel; Harri, Ari-Matti; Harshman, Karl; Hassler, Donald; Haukka, Harri; Hayes, Alex; Herkenhoff, Ken; Herrera, Paul; Hettrich, Sebastian; Heydari, Ezat; Hipkin, Victoria; Hoehler, Tori; Hollingsworth, Jeff; Hudgins, Judy; Huntress, Wesley; Hurowitz, Joel; Hviid, Stubbe; Iagnemma, Karl; Indyk, Steve; Israël, Guy; Jackson, Ryan; Jacob, Samantha; Jakosky, Bruce; Jensen, Elsa; Jensen, Jaqueline Kløvgaard; Johnson, Jeffrey; Johnson, Micah; Johnstone, Steve; Jones, Andrea; Jones, John; Joseph, Jonathan; Jun, Insoo; Kah, Linda; Kahanpää, Henrik; Kahre, Melinda; Karpushkina, Natalya; Kasprzak, Wayne; Kauhanen, Janne; Keely, Leslie; Kemppinen, Osku; Keymeulen, Didier; Kim, Myung-Hee; Kinch, Kjartan; King, Penny; Kirkland, Laurel; Kocurek, Gary; Koefoed, Asmus; Köhler, Jan; Kortmann, Onno; Kozyrev, Alexander; Krezoski, Jill; Krysak, Daniel; Kuzmin, Ruslan; Lacour, Jean Luc; Lafaille, Vivian; Langevin, Yves; Lanza, Nina; Lasue, Jeremie; Le Mouélic, Stéphane; Lee, Ella Mae; Lee, Qiu-Mei; Lees, David; Lefavor, Matthew; Lemmon, Mark; Malvitte, Alain Lepinette; Leshin, Laurie; Léveillé, Richard; Lewin-Carpintier, Éric; Lewis, Kevin; Li, Shuai; Lipkaman, Leslie; Little, Cynthia; Litvak, Maxim; Lorigny, Eric; Lugmair, Guenter; Lundberg, Angela; Lyness, Eric; Madsen, Morten; Mahaffy, Paul; Maki, Justin; Malakhov, Alexey; Malespin, Charles; Malin, Michael; Mangold, Nicolas; Manhes, Gérard; Manning, Heidi; Marchand, Geneviève; Jiménez, Mercedes Marín; García, César Martín; Martin, Dave; Martin, Mildred; Martínez-Frías, Jesús; Martín-Soler, Javier; Martín-Torres, F. Javier; Mauchien, Patrick; Maurice, Sylvestre; McAdam, Amy; McCartney, Elaina; McConnochie, Timothy; McCullough, Emily; McEwan, Ian; McKay, Christopher; McLennan, Scott; McNair, Sean; Melikechi, Noureddine; Meslin, Pierre-Yves; Meyer, Michael; Mezzacappa, Alissa; Miller, Hayden; Miller, Kristen; Milliken, Ralph; Ming, Douglas; Minitti, Michelle; Mischna, Michael; Mitrofanov, Igor; Moersch, Jeff; Mokrousov, Maxim; Jurado, Antonio Molina; Moores, John; Mora-Sotomayor, Luis; Morookian, John Michael; Morris, Richard; Morrison, Shaunna; Mueller-Mellin, Reinhold; Muller, Jan-Peter; Caro, Guillermo Muñoz; Nachon, Marion; López, Sara Navarro; Navarro-González, Rafael; Nealson, Kenneth; Nefian, Ara; Nelson, Tony; Newcombe, Megan; Newman, Claire; Newsom, Horton; Nikiforov, Sergey; Niles, Paul; Nixon, Brian; Dobrea, Eldar Noe; Nolan, Thomas; Oehler, Dorothy; Ollila, Ann; Olson, Timothy; Owen, Tobias; Hernández, Miguel Ángel de Pablo; Paillet, Alexis; Pallier, Etienne; Palucis, Marisa; Parker, Timothy; Parot, Yann; Patel, Kiran; Paton, Mark; Paulsen, Gale; Pavlov, Alex; Pavri, Betina; Peinado-González, Verónica; Pepin, Robert; Peret, Laurent; Perez, Rene; Perrett, Glynis; Peterson, Joe; Pilorget, Cedric; Pinet, Patrick; Pla-García, Jorge; Plante, Ianik; Poitrasson, Franck; Polkko, Jouni; Popa, Radu; Posiolova, Liliya; Posner, Arik; Pradler, Irina; Prats, Benito; Prokhorov, Vasily; Purdy, Sharon Wilson; Raaen, Eric; Radziemski, Leon; Rafkin, Scot; Ramos, Miguel; Rampe, Elizabeth; Raulin, François; Ravine, Michael; Reitz, Günther; Rennó, Nilton; Rice, Melissa; Richardson, Mark; Robert, François; Robertson, Kevin; Manfredi, José Antonio Rodriguez; Romeral-Planelló, Julio J.; Rowland, Scott; Rubin, David; Saccoccio, Muriel; Salamon, Andrew; Sandoval, Jennifer; Sanin, Anton; Fuentes, Sara Alejandra Sans; Saper, Lee; Sarrazin, Philippe; Sautter, Violaine; Savijärvi, Hannu; Schieber, Juergen; Schmidt, Mariek; Schmidt, Walter; Scholes, Daniel "Dan"; Schoppers, Marcel; Schröder, Susanne; Schwenzer, Susanne; Martinez, Eduardo Sebastian; Sengstacken, Aaron; Shterts, Ruslan; Siebach, Kirsten; Siili, Tero; Simmonds, Jeff; Sirven, Jean-Baptiste; Slavney, Susie; Sletten, Ronald; Smith, Michael; Sánchez, Pablo Sobrón; Spanovich, Nicole; Spray, John; Squyres, Steven; Stack, Katie; Stalport, Fabien; Steele, Andrew; Stein, Thomas; Stern, Jennifer; Stewart, Noel; Stipp, Susan Louise Svane; Stoiber, Kevin; Stolper, Ed; Sucharski, Bob; Sullivan, Rob; Summons, Roger; Sumner, Dawn; Sun, Vivian; Supulver, Kimberley; Sutter, Brad; Szopa, Cyril; Tan, Florence; Tate, Christopher; Teinturier, Samuel; ten Kate, Inge; Thomas, Peter; Thompson, Lucy; Tokar, Robert; Toplis, Mike; Redondo, Josefina Torres; Trainer, Melissa; Treiman, Allan; Tretyakov, Vladislav; Urqui-O'Callaghan, Roser; Van Beek, Jason; Van Beek, Tessa; VanBommel, Scott; Vaniman, David; Varenikov, Alexey; Vasavada, Ashwin; Vasconcelos, Paulo; Vicenzi, Edward; Vostrukhin, Andrey; Voytek, Mary; Wadhwa, Meenakshi; Ward, Jennifer; Webster, Chris; Weigle, Eddie; Wellington, Danika; Westall, Frances; Wiens, Roger Craig; Wilhelm, Mary Beth; Williams, Amy; Williams, Joshua; Williams, Rebecca; Williams, Richard B. "Mouser"; Wilson, Mike; Wimmer-Schweingruber, Robert; Wolff, Mike; Wong, Mike; Wray, James; Wu, Megan; Yana, Charles; Yen, Albert; Yingst, Aileen; Zeitlin, Cary; Zimdar, Robert; Mier, María-Paz Zorzano

    2013-09-01

    The Mars Science Laboratory rover Curiosity scooped samples of soil from the Rocknest aeolian bedform in Gale crater. Analysis of the soil with the Chemistry and Mineralogy (CheMin) x-ray diffraction (XRD) instrument revealed plagioclase (~An57), forsteritic olivine (~Fo62), augite, and pigeonite, with minor K-feldspar, magnetite, quartz, anhydrite, hematite, and ilmenite. The minor phases are present at, or near, detection limits. The soil also contains 27 ± 14 weight percent x-ray amorphous material, likely containing multiple Fe3+- and volatile-bearing phases, including possibly a substance resembling hisingerite. The crystalline component is similar to the normative mineralogy of certain basaltic rocks from Gusev crater on Mars and of martian basaltic meteorites. The amorphous component is similar to that found on Earth in places such as soils on the Mauna Kea volcano, Hawaii.

  15. Filled/Eroded Craters

    Science.gov (United States)

    2005-01-01

    14 October 2005 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows rugged terrain in northern Arabia Terra. The circular features are the remains of old meteor impact craters -- either the eroded remnants of the interiors of craters, or the remains of craters that were filled by layered material. The martian bedrock has craters of all sizes and states of erosion interbedded with its layered materials. Location near: 31.4oN, 299.0oW Image width: width: 3 km (1.9 mi) Illumination from: lower left Season: Northern Winter

  16. The Spirit of Logotherapy

    Directory of Open Access Journals (Sweden)

    Stephen J. Costello

    2015-12-01

    Full Text Available The aim of this paper is to adduce the meaning of Viktor Frankl’s logotherapy and existential analysis—the spirit of logotherapy—in the two-fold sense of its core teachings, as well as its emphasis on the spiritual dimension of the human person. Firstly, I situate Frankl’s tri-dimensional ontology—his philosophical anthropology—within a Platonic perspective, asserting that it was Plato who first gave us a picture and model of mental health which he based on the harmony of the disparate parts of the personality—the aim to become One instead of Many, which finds a modern parallel in Viktor Frankl’s logotherapy, which likewise stresses the importance of inner wholeness (an anthropological oneness despite our ontological differences. Classical Greek philosophers all pointed to the Logos as source of order—to the horizon of meaning-potentials, so I visit the various understandings of this term from the pre-Socratics to Frankl, albeit briefly, to avoid semantic confusion in what is to follow. I then discuss in some detail the exact meaning that logos/spirit has in Frankl’s philosophical conceptualisations. Disorders of logos may be seen in various psychopathologies and pnemopathologies which I go on to consider, highlighting the differences between various terms that are commonly left unclarified. Next, I adumbrate the differences between psychotherapy and logotherapy, which ultimately revolves around the difference between instincts and spirit before demarcating the boundaries between religion (as salvation and logotherapy (as sanity. The question I pose next is: what exactly constitutes the spiritual in logotherapy, as in life? An example is given to concretise the conceptual considerations previously elucidated before drawing on another distinction, that between “ultimate meaning” and “the meaning of the moment”. The paper concludes with a brief excursus into the work of Ken Wilber by way of enabling us to appreciate and

  17. Buried Craters of Utopia

    Science.gov (United States)

    2003-01-01

    MGS MOC Release No. MOC2-365, 19 May 2003Beneath the northern plains of Mars are numerous buried meteor impact craters. One of the most heavily-cratered areas, although buried, occurs in Utopia Planitia, as shown in this Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image. The history of Mars is complex; impact craters provide a tool by which to understand some of that history. In this case, a very ancient, cratered surface was thinly-buried by younger material that is not cratered at all. This area is near 48.1oN, 228.2oW; less than 180 km (112 mi) west of the Viking 2 lander site. Sunlight illuminates the scene from the lower left.

  18. Exhuming South Polar Crater

    Science.gov (United States)

    2004-01-01

    7 February 2004 The large, circular feature in this image is an old meteor impact crater. The crater is larger than the 3 kilometers-wide (1.9 miles-wide) Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image, thus only part of the crater is seen. The bright mesas full of pits and holes--in some areas resembling swiss cheese--are composed of frozen carbon dioxide. In this summertime view, the mesa slopes and pit walls are darkened as sunlight causes some of the ice to sublime away. At one time in the past, the crater shown here may have been completely covered with carbon dioxide ice, but, over time, it has been exhumed as the ice sublimes a little bit more each summer. The crater is located near 86.8oS, 111.6oW. Sunlight illuminates this scene from the upper left.

  19. Arabia Crater Cluster

    Science.gov (United States)

    2004-01-01

    27 May 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a portion of a large field of small craters clustered together in northeastern Arabia Terra. Crater clusters usually result from the secondary impact of debris thrown from a much larger impact or from the break-up and impact of fragments of a large meteor. Each crater has subsequently been partially filled by material that erodes to form a rugged crater floor surface, and the general appearance of each crater has been somewhat eroded and modified, as well. The image is located near 34.7oN, 314.7oW, and covers an area about 3 km (1.9 mi) across. Sunlight illuminates the scene from the lower left.

  20. SPIRIT 2013 explanation and elaboration

    DEFF Research Database (Denmark)

    Chan, An-Wen; Tetzlaff, Jennifer M; Gøtzsche, Peter C

    2013-01-01

    (Standard Protocol Items: Recommendations for Interventional Trials). The SPIRIT Statement provides guidance in the form of a checklist of recommended items to include in a clinical trial protocol. This SPIRIT 2013 Explanation and Elaboration paper provides important information to promote full...... understanding of the checklist recommendations. For each checklist item, we provide a rationale and detailed description; a model example from an actual protocol; and relevant references supporting its importance. We strongly recommend that this explanatory paper be used in conjunction with the SPIRIT Statement...

  1. Search for magnetic minerals in Martian rocks: Overview of the Rock Abrasion Tool (RAT) magnet investigation on Spirit and Opportunity

    DEFF Research Database (Denmark)

    Goetz, W.; Leer, K.; Gunnlaugsson, H.P.

    2008-01-01

    indicates the presence of a strongly ferrimagnetic phase in outcrops, such as magnetite or an altered version of magnetite. However, the evidence is weaker than in the case of Spirit. According to data from the a particle X-ray spectrometer (APXS) and the Mossbauer spectrometer (MB), the Eagle crater...

  2. Education and entrepreneurial spirit

    Directory of Open Access Journals (Sweden)

    Paul Marinescu

    2015-12-01

    Full Text Available The attitude of a man is influenced by the quality of education. Too often we use to exclusively impute to the system the educational problems of individuals and groups. It is necessary to look lucidly and to identify the role of family, civil society and individuals in education. Exercising leadership means continuously learning and, therefore, it is difficult to separate the educational dynamics from the team evolution at organizational level. The training of individuals occurs in variable contexts that they create or in which they are involved. From the leadership perspective, education is also a problem of assuming responsibilities. The set of values that outlines a social behaviour imposes also disclaimers. In such context, disclaimers can define the understanding of the efficient use of resources in favour of the group and not in one’s own interest. Hence, the management lesson for those who will be prepared to lead begins. That’s how the practical management and leadership lessons can contribute to the creation of complex personalities. Leaders and managers define a reality in which education plays a central role. Therefore, selfeducation becomes a must because it will impose the development of the spirit of initiative and the selection of those having both potential and skills to become leaders, managers and entrepreneurs. We can say that it is imperative to move on from “the game of chance” to the real performance standards in training tomorrow’s decision-makers.

  3. Library Spirit and Genius Loci

    DEFF Research Database (Denmark)

    Dahlkild, Nan

    2009-01-01

    The architecture and design of Nyborg Public Library in the light of the concepts "Library Spirit" and "Genius Loci", related to contemporary social and cultural movements, the development of the early welfare state and the "Scandinavian Style".......The architecture and design of Nyborg Public Library in the light of the concepts "Library Spirit" and "Genius Loci", related to contemporary social and cultural movements, the development of the early welfare state and the "Scandinavian Style"....

  4. Mars Gusts Blow Toward Spirit

    Science.gov (United States)

    2005-01-01

    This movie clip shows several gusts and whirlwinds carrying dust as they move toward NASA's Mars Exploration Rover Spirit. It consists of frames taken by the navigation camera on Spirit during the afternoon of the rover's 501st martian day, or sol (May 31, 2005). The camera was facing into the wind. Contrast has been enhanced for anything in the images that changes from frame to frame, that is, for the dust moved by wind.

  5. Venus - Crater Aurelia

    Science.gov (United States)

    1990-01-01

    This Magellan image shows a complex crater, 31.9 kilometers (20 miles) in diameter with a circular rim, terraced walls, and central peaks, located at 20.3 degrees north latitude and 331.8 degrees east longitude. Several unusual features are evidenced in this image: large dark surface up range from the crater; lobate flows emanating from crater ejecta, and very radar-bright ejecta and floor. Aurelia has been proposed to the International Astronomical Union, Subcommittee of Planetary Nomenclature as a candidate name. Aurelia is the mother of Julius Caesar.

  6. Crater in Utopia

    Science.gov (United States)

    2004-01-01

    23 March 2004 Craters of the martian northern plains tend to be somewhat shallow because material has filled them in. Their ejecta blankets, too, are often covered by younger materials. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows an example--a crater in Utopia Planitia near 43.7oN, 227.3oW. Erosion has roughened some of the surfaces of the material that filled the crater and covered its ejecta deposit. The picture covers an area about 3 km (1.9 mi) across. Sunlight illuminates the scene from the lower left.

  7. Solis Planum Craters

    Science.gov (United States)

    2005-01-01

    15 January 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows several meteor impact craters on Solis Planum. The second-largest crater in this scene is relatively young and fresh, exhibiting arrayed ejecta pattern and numerous boulders near its raised rim. The image covers an area about 3 km (1.9 mi) wide and is illuminated by sunlight from the upper left. The craters are located near 19.8oS, 85.5oW.

  8. Crater with Streak

    Science.gov (United States)

    2004-01-01

    6 November 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a small meteor impact crater (approximately the size of the famous Meteor Crater in northern Arizona) with a bright wind streak on its west (left) side. Generally, winds blowing from the east (right) have stripped away bright dust everywhere but in the lee of the crater. These landforms are located in eastern Kasei Valles near 25.1oN, 60.8oW. The picture covers an area about 3 km (1.9 mi) wide. Sunlight illuminates the scene from the left/lower left.

  9. Magma genesis at Gale Crater: Evidence for Pervasive Mantle Metasomatism

    Science.gov (United States)

    Filiberto, J.

    2017-12-01

    Basaltic rocks have been analyzed at Gale Crater with a larger range in bulk chemistry than at any other landing site [1]. Therefore, the rocks may have experienced significantly different formation conditions than those experienced by magmas at Gusev Crater or Meridiani Planum. Specifically, the rocks at Gale Crater have higher potassium than other Martian rocks, with a potential analog of the Nakhlite parental magma, and are consistent with forming from a metasomatized mantle source [2-4]. Mantle metasomatism would not only affect the bulk chemistry but mantle melting conditions, as metasomatism fluxes fluids into the source region. Here I will combine differences in bulk chemistry between Martian basalts to calculate formation conditions in the interior and investigate if the rocks at Gale Crater experienced magma genesis conditions consistent with metasomatism - lower temperatures and pressures of formation. To calculate average formation conditions, I rely on experimental results, where available, and silica-activity and Mg-exchange thermometry calculations for all other compositions following [5, 6]. The results show that there is a direct correlation between the calculated mantle potential temperature and the K/Ti ratio of Gale Crater rocks. This is consistent with fluid fluxed metasomatism introducing fluids to the system, which depressed the melting temperature and fluxed K but not Ti to the system. Therefore, all basalts at Gale Crater are consistent with forming from a metasomatized mantle source, which affected not only the chemistry of the basalts but also the formation conditions. References: [1] Cousin A. et al. (2017) Icarus. 288: 265-283. [2] Treiman A.H. et al. (2016) Journal of Geophysical Research: Planets. 121: 75-106. [3] Treiman A.H. and Medard E. (2016) Geological Society of America Abstracts with Programs. 48: doi: 10.1130/abs/2016AM-285851. [4] Schmidt M.E. et al. (2016) Geological Society of America Abstracts with Programs. 48: doi: 10

  10. Ganymede Crater Database

    Data.gov (United States)

    National Aeronautics and Space Administration — This web page leads to a database of images and information about the 150 major impact craters on Ganymede and is updated semi-regularly based on continuing analysis...

  11. Venus Crater Database

    Data.gov (United States)

    National Aeronautics and Space Administration — This web page leads to a database of images and information about the 900 or so impact craters on the surface of Venus by diameter, latitude, and name.

  12. Small, Bouldery Crater

    Science.gov (United States)

    2004-01-01

    30 April 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a relatively young impact crater located in southeastern Arabia Terra near 4.8oN, 313.9oW. It is about 1 kilometer (about six tenths of a mile) in diameter, roughly the size of the famous Meteor Crater in northern Arizona, U.S.A. Indeed, the Arizona crater may once have looked very similar to this, but erosion on Earth has been more vigorous than on the modern Mars. Large boulders, many of them bigger than a typical house, can be seen in the ejecta blanket and on the crater floor. Fine, bright dust, common throughout Arabia Terra, has thinly mantled all but the steepest slopes. The image is illuminated by sunlight from the left/upper left. The picture covers an area about 3 km (1.9 mi) across.

  13. Craters and Layers

    Science.gov (United States)

    2006-01-01

    11 March 2006 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows some typical relations between impact craters and light-toned, layered rock on Mars. The larger circular feature at the north (top) end of the image marks the location of a filled, buried crater on intermountain terrain north of Hellas Planitia. The larger crater at the southeast (lower right) corner formed by meteor impact into the layered material in which the buried crater is encased. The layered rock, in this case, has a light tone similar to the sedimentary rocks being explored by the Mars Exploration Rover, Opportunity, thousands of kilometers away in Sinus Meridiani. Location near: 24.9oS, 299.3oW Image width: 3 km (1.9 mi) Illumination from: upper left Season: Southern Summer

  14. Callisto Crater Database

    Data.gov (United States)

    National Aeronautics and Space Administration — This web page leads to a database of images and information about the 150 major impact craters on Callisto and is updated semi-regularly based on continuing analysis...

  15. Comparisons of Unconsolidated Sediments Analyzed by APXS (MSL-Curiosity) within Gale Crater, Mars: Soils, Sands of the Barchan and Linear Dunes of the Active Bagnold Dune Field, and Ripple-field Sands.

    Science.gov (United States)

    Thompson, L. M.; O'Connell-Cooper, C.; Spray, J. G.; Gellert, R.; Boyd, N. I.; Desouza, E.

    2017-12-01

    The MSL-APXS has analyzed a variety of unconsolidated sediments within the Gale impact crater, including soils, sands from barchan [High, Namib dunes], and linear dunes [Nathan Bridges, Mount Desert dunes], within the active Bagnold dune field, and sands from two smaller ripple fields ("mega-ripples"). The Gale "soils" (unsorted, unconsolidated sediments, ranging from fine-grained particles (including dust) to coarser "pebbly" material [>2 mm]), are, to a large degree, similar to Martian basaltic soils quantified by APXS, at Gusev crater (MER-A_Spirit) and Meridiani Planum (MER-B_Opportunity). Some local contributions are indicated by, for example, the enriched K levels (relative to a martian average basaltic soil [ABS]) within coarser Gale soil samples, and a Cr, Mn, Fe enrichment within finer-grained samples. Sands (grain size 62 µm to 2 mm) of the Bagnold dunes, generally, exhibit elevated Mg and Ni, indicating enrichment from olivine and pyroxene, but depleted S, Cl and Zn, indicating high activity levels and low dust. Compositional differences, related both to position within a dune (i.e., crest versus off-crest sand), and type of dune (linear versus barchan), are identified. Off-crest sands have Na, Al, Si, K, P contents similar to (or slightly depleted, relative to) the ABS, enrichment in Mg, and low dust content, whilst crest sands contain very high Mg and Ni (relative to the ABS), low felsic elemental concentrations and very low dust content. Cr is significantly enriched (and, to a lesser degree, Mn, Fe, Ti) in the off-crest sands of the linear dunes. In contrast, barchan dunes off-crest sands have Cr, Mn, Fe, and Ti abundances similar to those in the Gale soils. Additionally, Ni concentrations in barchan dunes off-crest sands are enriched relative to the linear dunes. Analyses from a small, isolated "mega-ripple" reveal a composition similar to that of the Gale soils, including a high dust content. The second mega-ripple, within a larger ripple field, is

  16. Multivariate analyses of crater parameters and the classification of craters

    Science.gov (United States)

    Siegal, B. S.; Griffiths, J. C.

    1974-01-01

    Multivariate analyses were performed on certain linear dimensions of six genetic types of craters. A total of 320 craters, consisting of laboratory fluidization craters, craters formed by chemical and nuclear explosives, terrestrial maars and other volcanic craters, and terrestrial meteorite impact craters, authenticated and probable, were analyzed in the first data set in terms of their mean rim crest diameter, mean interior relief, rim height, and mean exterior rim width. The second data set contained an additional 91 terrestrial craters of which 19 were of experimental percussive impact and 28 of volcanic collapse origin, and which was analyzed in terms of mean rim crest diameter, mean interior relief, and rim height. Principal component analyses were performed on the six genetic types of craters. Ninety per cent of the variation in the variables can be accounted for by two components. Ninety-nine per cent of the variation in the craters formed by chemical and nuclear explosives is explained by the first component alone.

  17. The Geochemical Alteration History of Clovis Class Rocks in Gusev Crater as Determined by Ti-Normailized Mass Balance Analysis

    Science.gov (United States)

    Sutter, B.; Ming, D. W.; Niles, P. B.; Golden, D. C.

    2012-03-01

    Clovis rocks were exposed to high aqueous activity that resulted in the loss of 20-65% of pyroxene and feldspar, which was followed by periods of lower aqueous activity that allowed for Mg, Si, Ca, S, and Cl additions.

  18. Integrating Principles Underlying Ancestral Spirits Belief in ...

    African Journals Online (AJOL)

    , associated with ancestral spirits and its use as powerful therapeutic agent for influencing behavior or lifestyle changes. Explanatory models of attachment to ancestral spirits by living descendants are first discussed, followed by a discussion ...

  19. Presidendi preemia said Urmas Kokassaar, Terje Varul, Heli Adamovitš ja Mihhail Gusev / Eve Kruuse

    Index Scriptorium Estoniae

    Kruuse, Eve, 1959-

    2009-01-01

    Vabariigi Presidendi Kultuurirahastu hariduspreemia pälvisid Tartu Ülikooli loodus- ja tehnoloogiateaduskonna loodusteadusliku hariduse keskuse bioloogia didaktika lektor ning Hugo Treffneri gümnaasiumi bioloogia ja keemia süvaõppega loodussuuna bioloogiaõpetaja Urmas Kokassaar, Kolga keskkooli eesti keele ja kirjanduseõpetaja Terje Varul ning Narva lasteaia "Päikene" juhataja Heli Adamovitš. Reaalteaduste eripreemia pälvis Tallinna Tõnismäe Reaalkooli matemaatikaõpetaja Mihhail Gusev

  20. Spirit Boxes: Expressions of Culture.

    Science.gov (United States)

    DeMuro, Ted

    1984-01-01

    After studying the culture and art of the ancient civilizations of South America, Mesopotamia, Greece, and Egypt, secondary level art students made spirit boxes as expressions of the various cultures. How to make the boxes and how to prepare the face molds are described. (RM)

  1. The Spirit of the Teacher

    Science.gov (United States)

    Smith, Olynda

    2013-01-01

    "The real preparation for education is a study of one's self. The training of the teacher who is to help life is something far more than a learning of ideas. It includes the training of character, it is a preparation of the spirit."--Maria Montessori". It is common knowledge among Montessorians that spiritual preparation was…

  2. Northern Plains Buried Craters

    Science.gov (United States)

    2004-01-01

    22 December 2003This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows three circular features on the martian northern plains near 70.7oN, 311.7oW. These circular features are the locations of meteor impact craters that have been buried beneath the plains. Much of the northern plains shares this story, in which thousands of old craters have been filled or partially filled and then thinly buried beneath textured plains. The picture covers an area 3 km (1.9 mi) wide. Sunlight illuminates the scene from the lower left.

  3. CHINCHIRISI: THE PHENOMENON OF "SPIRIT CHILDREN ...

    African Journals Online (AJOL)

    CHINCHIRISI: THE PHENOMENON OF "SPIRIT CHILDREN" AMONG. THE NANKANI OF NORTHERN GHANA1. Rose Ma7y Amenga-Etego*. Abstract. The identity of the 'spirit child' may be ambiguous, but 'its'place in the experiences and in explaining the intricacies between the human nature and the spirit world remains ...

  4. 27 CFR 30.41 - Bulk spirits.

    Science.gov (United States)

    2010-04-01

    ... shall be determined by reference to Table 4. However, in the case of spirits which contain solids in... ascertaining the wine gallons per pound of the spirits and multiplying the wine gallons per pound by the weight...) and dividing the result by 100. The wine gallons per pound of spirits containing solids in excess of...

  5. Thirteen Iron Meteorites Found at Gale Crater, Meridiani Planum, and Gusev Crater — Exogenic Witnesses to Weathering Processes Near the Martian Equator

    Science.gov (United States)

    Ashley, J.

    2014-12-01

    At least 20 meteorites and meteorite candidates have now been found by science teams at three Mars rover landing sites, all within 15 degrees of the martian equator. Thirteen of these are iron meteorites, comprising 65% of the population — an order of magnitude greater abundance than found among witnessed iron falls in Earth-based collections (~6%). Chondritic meteorites, which comprise some 86% of Earth-based falls, are conspicuously absent from the Mars inventory. The reasons for this disproportion may involve a) post-fall environmental resistance differences favoring iron survivability; b) fragmentation from impact shock (and possibly internal weathering stresses associated with oxide production in desert environments [1]); combined with c) selection biases arising from residual chondritic fragments appearing less conspicuous. Impact features along rover traverses often show evidence of dark materials likely to be impactor fragments [e.g., 2], which could represent the missing chondritic fraction. The reactivity of reduced (metallic) iron to aqueous alteration, combined with the near equatorial and widely distributed locations of these rocks, makes them particularly useful to the assessment of climate models arguing for geologically recent ice at the martian equator. Exposure histories involving alternating wind/water cycles are imprinted on several Meridiani irons, for example [3]. Evidence for oxide coating removal demonstrates the current epoch to be one of coating destruction, not production, showing that atmospheric exposure alone is insufficient to produce the coating. Cavernous weathering is likely associated with acidic corrosion, while evidence of aeolian scouring is found in Widmanstätten patterns, sharp-crested scallops, regmaglypt enlargement, and abundant pitting. Further study of these features could help constrain wind direction and velocity during epochs of sculpting [e.g., 4], and assist in exposure age estimation. References: [1] Ashley J. W. and M. A. Velbel (2000), MAPS, v. 35 no. 5 Supplement, p. A22. [2] Golombek et al., (2010) J. Geophys. Res., 115, E00F08, doi:10.1029/2010JE003628. [3] Ashley J. W. et al., (2011) J. Geophys. Res., 116, E00F20, doi:10.1029/2010JE003672. [4] Greeley R. et al., (2002) J. Geophys. Res., 107, E1, 5005, doi : 10.1029/2000JE001481.

  6. Secrets of the Wabar craters

    Science.gov (United States)

    Wynn, Jeffrey C.; Shoemaker, Eugene M.

    1997-01-01

    Focuses on the existence of craters in the Empty Quarter of Saudi Arabia created by the impact of meteors in early times. Mars Pathfinder and Mars Global Surveyor's encounter with impact craters; Elimination of craters in the Earth's surface by the action of natural elements; Impact sites' demand for careful scientific inspections; Location of the impact sites.

  7. Marte Valles Crater 'Island'

    Science.gov (United States)

    2004-01-01

    10 April 2004 Marte Valles is an outflow channel system that straddles 180oW longitude between the region south of Cerberus and far northwestern Amazonis. The floor of the Marte valleys have enigmatic platy flow features that some argue are formed by lava, others suggest they are remnants of mud flows. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows an island created in the middle of the main Marte Valles channel as fluid---whether lava or mud---flowed past two older meteor impact craters. The craters are located near 21.5oN, 175.3oW. The image covers an area about 3 km (1.9 mi) across. Sunlight illuminates the scene from the lower left.

  8. Crater in Marte Vallis

    Science.gov (United States)

    2003-01-01

    MGS MOC Release No. MOC2-566, 6 December 2003This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a streamlined tail-pointing toward the upper right (northeast)--in the lee of a meteor impact crater in Marte Vallis, a large valley and channel complex southeast and east of the Elysium volcanic region. The fluid that went through Marte Vallis, whether water, mud, lava, or otherwise, created this form as it moved from the lower left (southwest) toward the upper right. The crater is located near 19.0oN, 174.9oW. The image covers an area 3 km (1.9 mi) wide and is illuminated from the left.

  9. Northern Plains 'Crater'

    Science.gov (United States)

    2004-01-01

    10 December 2004 The lower left (southwest) corner of this Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows the location of a somewhat filled and buried meteor impact crater on the northern plains of Mars. The dark dots are boulders. A portion of a similar feature is seen in the upper right (northeast) corner of the image. This picture, showing landforms (including the odd mound north/northeast of the crater) that are typical of the martian northern lowland plains, was obtained as part of the MGS MOC effort to support the search for a landing site for the Phoenix Mars Scout lander. Phoenix will launch in 2007 and land on the northern plains in 2008. This image is located near 68.0oN, 227.4oW, and covers an area approximately 3 km (1.9 mi) wide. The scene is illuminated by sunlight from the lower left.

  10. Pair of Craters

    Science.gov (United States)

    2005-01-01

    14 July 2005 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a 1.5 meters per pixel (5 ft/pixel) view of a pair of small meteor impact craters in the Arena Colles region of Mars, located north of Isidis Planitia. Location near: 22.7oN, 278.5oW Image width: width: 3 km (1.9 mi) Illumination from: lower left Season: Northern Autumn

  11. Cracked Plain, Buried Craters

    Science.gov (United States)

    2004-01-01

    4 September 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a cracked plain in western Utopia Planitia. The three circular crack patterns indicate the location of three buried meteor impact craters. These landforms are located near 41.9oN, 275.9oW. The image covers an area approximately 3 km (1.9 mi) across. Sunlight illuminates this scene from the lower left.

  12. Wind Streak and Crater

    Science.gov (United States)

    2004-01-01

    23 February 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a wind streak developed in the lee of a meteor impact crater in western Daedalia Planum. The dominant winds responsible for the streak blew from the bottom/lower right (southeast). The image is located near 9.9oS, 144.9oW. Sunlight illuminates the scene from the lower left; the picture covers an area 3 km (1.9 mi) wide.

  13. Crater in Arabia

    Science.gov (United States)

    2004-01-01

    28 October 2004 This high resolution Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a small meteor impact crater with bouldery ejecta in the Arabia Terra region of Mars. The image is located near 11.9oN, 342.2oW. The 300 meter scale bar is about 328 yards long. Sunlight illuminates the scene from the upper left.

  14. Iturralde Crater, Bolivia

    Science.gov (United States)

    2002-01-01

    NASA scientists will venture into an isolated part of the Bolivian Amazon to try and uncover the origin of a 5 mile (8 kilometer) diameter crater there known as the Iturralde Crater. Traveling to this inhospitable forest setting, the Iturralde Crater Expedition 2002 will seek to determine if the unusual circular crater was created by a meteor or comet. Organized by Dr. Peter Wasilewski of NASA's Goddard Space Flight Center, Greenbelt, Md., the Iturralde Crater Expedition 2002 will be led by Dr. Tim Killeen of Conservation International, which is based in Bolivia. Killeen will be assisted by Dr. Compton Tucker of Goddard. The team intends to collect and analyze rocks and soil, look for glass particles that develop from meteor impacts and study magnetic properties in the area to determine if the Iturralde site was indeed created by a meteor.This image was acquired on June 29, 2001 by the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) on NASA's Terra satellite. With its 14 spectral bands from the visible to the thermal infrared wavelength region, and its high spatial resolution of 15 to 90 meters (about 50 to 300 feet), ASTER will image Earth for the next 6 years to map and monitor the changing surface of our planet.ASTER is one of five Earth-observing instruments launched December 18, 1999, on NASA's Terra satellite. The instrument was built by Japan's Ministry of Economy, Trade and Industry. A joint U.S./Japan science team is responsible for validation and calibration of the instrument and the data products.The broad spectral coverage and high spectral resolution of ASTER will provide scientists in numerous disciplines with critical information for surface mapping, and monitoring dynamic conditions and temporal change. Example applications are: monitoring glacial advances and retreats; monitoring potentially active volcanoes; identifying crop stress; determining cloud morphology and physical properties; wetlands evaluation; thermal pollution

  15. Formation of Craters in Sand

    Directory of Open Access Journals (Sweden)

    Vanissra Boonyaleepun

    2007-06-01

    Full Text Available The diameter of craters formed by spheres of varying mass dropped into sand at low speed was studied. The relationship between the diameter of the crater formed and the kinetic energy of the projectile at impact was found to be of the same general form as that for planetary meteor craters. The relationship is shown to be a power law with exponent 0.17.

  16. The Spirit of Public Service

    DEFF Research Database (Denmark)

    Hassall Thomsen, Line Hassall; Willig, Ida

    Research on public service broadcasting tends to highlight norms and values at the strategic level. This paper explores ‘public service’ as an institutional logic guiding the everyday practice of journalists. The theoretical framework draws on Pierre Bourdieus’ field theory and recent works...... on cultural production and news work. Through fieldwork and interviews with Danish and British reporters/editors from DR 1, TV 2, BBC 1 and ITV we identify three components of a strong public service spirit present in the journalist’s understanding of the self: mass audience orientation, democratic...

  17. 27 CFR 24.232 - Gauge of spirits.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Gauge of spirits. 24.232... OF THE TREASURY LIQUORS WINE Spirits § 24.232 Gauge of spirits. (a) If the spirits to be used are in... the proof of the spirits and the quantity used by volume gauge or by weight. Upon completion of the...

  18. Crater Highlands, Tanzania

    Science.gov (United States)

    2006-01-01

    The Shuttle Radar Topography Mission (SRTM), flown aboard Space Shuttle Endeavour in February 2000, acquired elevation measurements for nearly all of Earth's landmass between 60oN and 56oS latitudes. For many areas of the world SRTM data provide the first detailed three-dimensional observation of landforms at regional scales. SRTM data were used to generate this view of the Crater Highlands along the East African Rift in Tanzania. Landforms are depicted with colored height and shaded relief, using a vertical exaggeration of 2X and a southwestwardly look direction. Lake Eyasi is depicted in blue at the top of the image, and a smaller lake occurs in Ngorongoro Crater. Near the image center, elevations peak at 3648 meters (11,968 feet) at Mount Loolmalasin, which is south of Ela Naibori Crater. Kitumbeine (left) and Gelai (right) are the two broad mountains rising from the rift lowlands. Mount Longido is seen in the lower left, and the Meto Hills are in the right foreground. Tectonics, volcanism, landslides, erosion and deposition -- and their interactions -- are all very evident in this view. The East African Rift is a zone of spreading between the African (on the west) and Somali (on the east) crustal plates. Two branches of the rift intersect here in Tanzania, resulting in distinctive and prominent landforms. One branch trends nearly parallel the view and includes Lake Eyasi and the very wide Ngorongoro Crater. The other branch is well defined by the lowlands that trend left-right across the image (below center, in green). Volcanoes are often associated with spreading zones where magma, rising to fill the gaps, reaches the surface and builds cones. Craters form if a volcano explodes or collapses. Later spreading can fracture the volcanoes, which is especially evident on Kitumbeine and Gelai Mountains (left and right, respectively, lower center). The Crater Highlands rise far above the adjacent savannas, capture moisture from passing air masses, and host rain

  19. Polygons and Craters

    Science.gov (United States)

    2005-01-01

    3 September 2005 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows polygons enhanced by subliming seasonal frost in the martian south polar region. Polygons similar to these occur in frozen ground at high latitudes on Earth, suggesting that perhaps their presence on Mars is also a sign that there is or once was ice in the shallow subsurface. The circular features are degraded meteor impact craters. Location near: 72.2oS, 310.3oW Image width: width: 3 km (1.9 mi) Illumination from: upper left Season: Southern Spring

  20. Layers in Crater Wall

    Science.gov (United States)

    2004-01-01

    22 January 2004 This January 2004 Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows three distinct bands of layered material exposed in the wall of a south, middle-latitude meteor impact crater wall. Talus--debris shed from erosion of the wall--has piled up on the slopes below the layered outcrop. This picture is located near 45.5oS, 85.9oW, and covers an area 3 km (1.9 mi) wide. Sunlight illuminates the scene from the right/lower right.

  1. Themes in Spirit Possession in Ugandan Christianity

    African Journals Online (AJOL)

    Rob and Jean

    theorisation of the world in order to understand and affect it. Key words: Spirit Possession; .... about twenty-five minutes in, the music changed, beginning to slow and quieten. As it did so, the songs of the .... other stories that are passed on in discussions (such as the memory of spirits living Lake. Victoria or tales of armies of ...

  2. Renewing the Spirit of the Liberal Arts

    Science.gov (United States)

    Noddings, Nel

    2013-01-01

    The spirit of the liberal arts has been undermined by overspecialization, and it has been further damaged by the increase in emphasis on the economic purpose of education. The spirit might be renewed by using the aims of the liberal arts to develop every course we teach.

  3. Crater density differences: Exploring regional resurfacing, secondary crater populations, and crater saturation equilibrium on the moon

    Science.gov (United States)

    Povilaitis, R Z; Robinson, M S; van der Bogert, C H; Hiesinger, Harald; Meyer, H M; Ostrach, Lillian

    2017-01-01

    The global population of lunar craters >20 km in diameter was analyzed by Head et al., (2010) to correlate crater distribution with resurfacing events and multiple impactor populations. The work presented here extends the global crater distribution analysis to smaller craters (5–20 km diameters, n = 22,746). Smaller craters form at a higher rate than larger craters and thus add granularity to age estimates of larger units and can reveal smaller and younger areas of resurfacing. An areal density difference map generated by comparing the new dataset with that of Head et al., (2010) shows local deficiencies of 5–20 km diameter craters, which we interpret to be caused by a combination of resurfacing by the Orientale basin, infilling of intercrater plains within the nearside highlands, and partial mare flooding of the Australe region. Chains of 5–30 km diameter secondaries northwest of Orientale and possible 8–22 km diameter basin secondaries within the farside highlands are also distinguishable. Analysis of the new database indicates that craters 57–160 km in diameter across much of the lunar highlands are at or exceed relative crater densities of R = 0.3 or 10% geometric saturation, but nonetheless appear to fit the lunar production function. Combined with the observation that small craters on old surfaces can reach saturation equilibrium at 1% geometric saturation (Xiao and Werner, 2015), this suggests that saturation equilibrium is a size-dependent process, where large craters persist because of their resistance to destruction, degradation, and resurfacing.

  4. APXS-derived chemistry of the Bagnold dune sands: Comparisons with Gale Crater soils and the global Martian average

    Science.gov (United States)

    O'Connell-Cooper, C. D.; Spray, J. G.; Thompson, L. M.; Gellert, R.; Berger, J. A.; Boyd, N. I.; Desouza, E. D.; Perrett, G. M.; Schmidt, M.; VanBommel, S. J.

    2017-12-01

    We present Alpha-Particle X-ray Spectrometer (APXS) data for the active Bagnold dune field within the Gale impact crater (Mars Science Laboratory (MSL) mission). We derive an APXS-based average basaltic soil (ABS) composition for Mars based on past and recent data from the MSL and Mars Exploration Rover (MER) missions. This represents an update to the Taylor and McLennan (2009) average Martian soil and facilitates comparison across Martian data sets. The active Bagnold dune field is compositionally distinct from the ABS, with elevated Mg, Ni, and Fe, suggesting mafic mineral enrichment and uniformly low levels of S, Cl, and Zn, indicating only a minimal dust component. A relationship between decreasing grain size and increasing felsic content is revealed. The Bagnold sands possess the lowest S/Cl of all Martian unconsolidated materials. Gale soils exhibit relatively uniform major element compositions, similar to Meridiani Planum and Gusev Crater basaltic soils (MER missions). However, they show minor enrichments in K, Cr, Mn, and Fe, which may signify a local contribution. The lithified eolian Stimson Formation within the Gale impact crater is compositionally similar to the ABS and Bagnold sands, which provide a modern analogue for these ancient eolian deposits. Compilation of APXS-derived soil data reveals a generally homogenous global composition for Martian soils but one that can be locally modified due to past or extant geologic processes that are limited in both space and time.

  5. Orson Welles Crater Dunes

    Science.gov (United States)

    2004-01-01

    [figure removed for brevity, see original site] Released 14 April 2004 The Odyssey spacecraft has completed a full Mars year of observations of the red planet. For the next several weeks the Image of the Day will look back over this first mars year. It will focus on four themes: 1) the poles - with the seasonal changes seen in the retreat and expansion of the caps; 2) craters - with a variety of morphologies relating to impact materials and later alteration, both infilling and exhumation; 3) channels - the clues to liquid surface flow; and 4) volcanic flow features. While some images have helped answer questions about the history of Mars, many have raised new questions that are still being investigated as Odyssey continues collecting data as it orbits Mars. This daytime VIS image was collected on November 13, 2003 during the southern summer season in Orson Welles Crater. Image information: VIS instrument. Latitude -0, Longitude 313.4 East (46.6 West). 19 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly

  6. Spirit Beside 'Home Plate,' Sol 1809

    Science.gov (United States)

    2009-01-01

    NASA Mars Exploration Rover Spirit used its navigation camera to take the images assembled into this 120-degree view southward after a short drive during the 1,809th Martian day, or sol, of Spirit's mission on the surface of Mars (February 3, 2009). Spirit had driven about 2.6 meters (8.5 feet) that sol, continuing a clockwise route around a low plateau called 'Home Plate.' In this image, the rocks visible above the rovers' solar panels are on the slope at the northern edge of Home Plate. This view is presented as a cylindrical projection with geometric seam correction.

  7. Spirit's Surroundings on 'West Spur,' Sol 305

    Science.gov (United States)

    2005-01-01

    This 360-degree panorama shows the terrain surrounding NASA's Mars Exploration Rover Spirit as of the rover's 305th martian day, or sol, (Nov. 11, 2004). At that point, Spirit was climbing the 'West Spur' of the 'Columbia Hills.' The rover had just finished inspecting a rock called 'Lutefisk' and was heading uphill toward an area called 'Machu Picchu.' Spirit used its navigational camera to take the images combined into this mosaic. The rover's location when the images were taken is catalogued as the mission's site 89, position 205. The view is presented here as a cylindrical projection with geometric seam correction.

  8. Basalt-trachybasalt samples in Gale Crater, Mars

    International Nuclear Information System (INIS)

    Edwards, Peter H.; Anderson, Ryan B.; Dyar, Darby

    2017-01-01

    The ChemCam instrument on the Mars Science Laboratory (MSL) rover, Curiosity, observed numerous igneous float rocks and conglomerate clasts, reported previously. A new statistical analysis of single-laser-shot spectra of igneous targets observed by ChemCam shows a strong peak at ~55 wt% SiO 2 and 6 wt% total alkalis, with a minor secondary maximum at 47–51 wt% SiO 2 and lower alkali content. The centers of these distributions, together with the rock textures, indicate that many of the ChemCam igneous targets are trachybasalts, Mg# = 27 but with a secondary concentration of basaltic material, with a focus of compositions around Mg# = 54. We suggest that all of these igneous rocks resulted from low-pressure, olivine-dominated fractionation of Adirondack (MER) class-type basalt compositions. This magmatism has subalkaline, tholeiitic affinities. The similarity of the basalt endmember to much of the Gale sediment compositions in the first 1000 sols of the MSL mission suggests that this type of Fe-rich, relatively low-Mg#, olivine tholeiite is the dominant constituent of the Gale catchment that is the source material for the fine-grained sediments in Gale. The similarity to many Gusev igneous compositions suggests that it is a major constituent of ancient Martian magmas, and distinct from the shergottite parental melts thought to be associated with Tharsis and the Northern Lowlands. Finally, the Gale Crater catchment sampled a mixture of this tholeiitic basalt along with alkaline igneous material, together giving some analogies to terrestrial intraplate magmatic provinces.

  9. 27 CFR 19.998 - Transfer in bond of spirits.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Transfer in bond of spirits. 19.998 Section 19.998 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE... spirits plants. Spirits (not including spirits produced from petroleum, natural gas, or coal) may be...

  10. 27 CFR 19.99 - Spirits in customs custody.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Spirits in customs custody. 19.99 Section 19.99 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU... Conveyance of Spirits Or Wines on Plant Premises § 19.99 Spirits in customs custody. Spirits in customs...

  11. Physicochemical and Sensorial Characterization of Honey Spirits.

    Science.gov (United States)

    Anjos, Ofélia; Frazão, David; Caldeira, Ilda

    2017-07-27

    Distilled spirits are usually made from fermented sugar-based materials, such as wines or fermented fruits, but other products can be used, namely berries or honey. In this work, an evaluation of honey spirits is done based on its physicochemical and sensory characteristics. Fourteen honey spirit samples of different brands of honey spirit were purchased at the market and from artisan Portuguese producers. Several analytical determinations, namely alcoholic strength, dry matter, density, total acidity, chromatic characteristics, methanol, acetaldehyde, ethyl acetate and higher alcohols were done to characterize all samples. The results pointed out several differences in physicochemical composition of samples. In general, these drinks are characterized by an alcohol strength between 37.4% and 53.0% and a low methanol content, quite null for most samples. Samples with higher ethanol content corresponded to the artisanal samples. Significant differences ( p drink, which has gained market value.

  12. Raves, psychosis, and spirit healing.

    Science.gov (United States)

    Seeman, Mary V

    2010-07-01

    This paper reflects the intersection of three cultures: the rave (all night dance party and use of the drug, Ecstasy) culture; the ward culture of an inpatient psychiatric program for First Episode Psychosis; the spirit healing culture of the Philippines. All three intersected in Toronto, Canada in the mid 1990s, as illustrated by the clinical case of a 19-year-old university student who was hospitalized with symptoms of drug-induced psychosis. Her initial treatment was not successful and presented dilemmas for the treating staff. Transfer to a second psychiatric facility that permitted attendance at a traditional Filipino healing ceremony resulted in a cure, with no recurrence 10 years later. According to James Dow's 1986 formulation, the components of the key spiritual healing session paralleled the very elements the young woman had sought by participating in raves, an activity that was problematic because it led to family displeasure. Whereas attendance at a rave triggered illness, the healing session, sanctioned by her family and taking place in their midst, resulted in healing.

  13. Geology of Lofn Crater, Callisto

    Science.gov (United States)

    Greeley, Ronald; Heiner, Sarah; Klemaszewski, James E.

    2001-01-01

    Lofn crater is a 180-km-diameter impact structure in the southern cratered plains of Callisto and is among the youngest features seen on the surface. The Lofn area was imaged by the Galileo spacecraft at regional-scale resolutions (875 m/pixel), which enable the general geology to be investigated. The morphology of Lofn crater suggests that (1) it is a class of impact structure intermediate between complex craters and palimpsests or (2) it formed by the impact of a projectile which fragmented before reaching the surface, resulting in a shallow crater (even for Callisto). The asymmetric pattern of the rim and ejecta deposits suggests that the impactor entered at a low angle from the northwest. The albedo and other characteristics of the ejecta deposits from Lofn also provide insight into the properties of the icy lithosphere and subsurface configuration at the time of impact. The "target" for the Lofn impact is inferred to have included layered materials associated with the Adlinda multiring structure northwest of Loh and ejecta deposits from the Heimdall crater area to the southeast. The Lofn impact might have penetrated through these materials into a viscous substrate of ductile ice or possibly liquid water. This interpretation is consistent with models of the current interior of Callisto based on geophysical information obtained from the Galileo spacecraft.

  14. A Tale of 3 Craters

    Science.gov (United States)

    2004-01-01

    11 November 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image captures some of the complexity of the martian upper crust. Mars does not simply have an impact-cratered surface, it's upper crust is a cratered volume. Over time, older craters on Mars have been eroded, filled, buried, and in some cases exhumed and re-exposed at the martian surface. The crust of Mars is layered to depths of 10 or more kilometers, and mixed in with the layered bedrock are a variety of ancient craters with diameters ranging from a few tens of meters (a few tens of yards) to several hundred kilometers (more than one or two hundred miles). The picture shown here captures some of the essence of the layered, cratered volume of the upper crust of Mars in a very simple form. The image shows three distinct circular features. The smallest, in the lower right quarter of the image, is a meteor crater surrounded by a mound of material. This small crater formed within a layer of bedrock that once covered the entire scene, but today is found only in this small remnant adjacent to the crater. The intermediate-sized crater, west (left) of the small one, formed either in the next layer down--that is, below the layer in which the small crater formed--or it formed in some layers that are now removed, but was big enough to penetrate deeply into the rock that is near the surface today. The largest circular feature in the image, in the upper right quarter of the image, is still largely buried. It formed in layers of rock that are below the present surface. Erosion has brought traces of its rim back to the surface of Mars. This picture is located near 50.0oS, 77.8oW, and covers an area approximately 3 km (1.9 mi) across. Sunlight illuminates this October 2004 image from the upper left.

  15. Test-field for evaluation of laboratory craters using a Crater Shape-based interpolation crater detection algorithm and comparison with Martian and Lunar impact craters

    Science.gov (United States)

    Salamunićcar, Goran; Lončarić, Sven; Vinković, Dejan; Vučina, Damir; Gomerčić, Mladen; Pehnec, Igor; Vojković, Marin; Hercigonja, Tomislav

    2012-10-01

    Impact craters are some of the most abundant geological features on most lunar and planetary bodies, providing insight into the history and physical processes that shaped their surface. It is therefore not surprising that extensive research has been done in the past on laboratory craters, as well as on crater detection algorithms (CDAs). No prior work has investigated how CDAs can assist in the research of laboratory craters, nor has an alternative formal method for evaluation of the similarity between laboratory and real impact craters been proposed. The result of this work is a test-field for evaluation of laboratory craters which includes: (1) a procedure for creation of explosion-induced laboratory craters in stone powder surfaces; (2) a method for 3D scanning of laboratory craters using a GOM-ATOS-I 3D scanner; (3) a new method for emplacement of laboratory craters into the topography of a planetary body; (4) a new method for objective evaluation of laboratory craters which utilizes the CDA, the Turing test, and a new measure of similarity between laboratory and real craters; and (5) a possibility of accompanying manual evaluation of laboratory craters using 2D topographical profiles. The successful verification of the proposed test-field, using Martian and Lunar global DEMs and local high-resolution DEMs, confirmed possibilities for the proposed scientific investigations of real impact craters using laboratory craters as proxies. This cost-effective approach also promises affordable accessibility for introductory physics and astronomy laboratories.

  16. Alumina+Silica+/-Germanium Alteration in Smectite-Bearing Marathon Valley, Endeavour Crater Rim, Mars

    Science.gov (United States)

    Mittlefehldt, D. W.; Gellert, R.; Van Bommel, S.; Arvidson, R. E.; Clark, B. C.; Ming, D. W.; Schroeder, C.; Yen, A. S.; Fox, V. K.; Farrand, W. H.; hide

    2016-01-01

    Mars Exploration Rover Opportunity has been exploring Mars for 12+ years, and is presently investigating the geology of a western rim segment of 22 kilometers diameter, Noachian- aged Endeavour crater. The Alpha Particle X-ray Spectrometer has determined the compositions of a pre-impact lithology, the Matijevic fm., and polymict impact breccias ejected from the crater, the Shoemaker fm. Opportunity is now investigating a region named Marathon Valley that cuts southwest-northeast through the central portion of the rim segment and provides a window into the lower stratigraphic record. (Geographic names used here are informal.) At the head of Marathon Valley, referred to here as Upper Marathon Valley, is a shallow, ovoid depression approximately 25×35 millimeters in size, named Spirit of Saint Louis. Layering inside Spirit of Saint Louis appears continuous with the Upper Marathon Valley rocks outside, indicating they are coeval. Spirit of Saint Louis is partly bounded by approximately 10-20 centimeters wide zone containing reddish altered rocks (red zone). Red zones also form prominent curvilinear features in Marathon Valley. Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) spectra provide evidence for a really extensive Fe-Mg smectite in the Marathon Valley region, indicating distinct styles of aqueous alteration. The CRISM detections of smectites are based on metal-OH absorptions at approximately 2.3 and 2.4 micron that are at least two times the background noise level.

  17. Spirit Near 'Stapledon' on Sol 1802 (Polar)

    Science.gov (United States)

    2009-01-01

    NASA Mars Exploration Rover Spirit used its navigation camera for the images assembled into this full-circle view of the rover's surroundings during the 1,802nd Martian day, or sol, (January 26, 2009) of Spirit's mission on the surface of Mars. North is at the top. This view is presented as a polar projection with geometric seam correction. Spirit had driven down off the low plateau called 'Home Plate' on Sol 1782 (January 6, 2009) after spending 12 months on a north-facing slope on the northern edge of Home Plate. The position on the slope (at about the 9-o'clock position in this view) tilted Spirit's solar panels toward the sun, enabling the rover to generate enough electricity to survive its third Martian winter. Tracks at about the 11-o'clock position of this panorama can be seen leading back to that 'Winter Haven 3' site from the Sol 1802 position about 10 meters (33 feet) away. For scale, the distance between the parallel wheel tracks is about one meter (40 inches). Where the receding tracks bend to the left, a circular pattern resulted from Spirit turning in place at a soil target informally named 'Stapledon' after William Olaf Stapledon, a British philosopher and science-fiction author who lived from 1886 to 1950. Scientists on the rover team suspected that the soil in that area might have a high concentration of silica, resembling a high-silica soil patch discovered east of Home Plate in 2007. Bright material visible in the track furthest to the right was examined with Spirit's alpha partical X-ray spectrometer and found, indeed, to be rich in silica. The team laid plans to drive Spirit from this Sol 1802 location back up onto Home Plate, then southward for the rover's summer field season.

  18. the spirit of the body of christ: the holy spirit's indwelling in the church

    African Journals Online (AJOL)

    presence of Christ who indwells his body. ..... 12:12). Both belong intrinsically together. They are one and the same God in action. Now that Christ is in heaven, his Spirit is his own presence on earth and we must view the Spirit in this perspective: no ..... Christians are called to celebrate the Eucharist, in memory of the death.

  19. Silica-Rich Soil Found by Spirit

    Science.gov (United States)

    2007-01-01

    NASA's Mars Exploration Rover Spirit has found a patch of bright-toned soil so rich in silica that scientists propose water must have been involved in concentrating it. The silica-rich patch, informally named 'Gertrude Weise' after a player in the All-American Girls Professional Baseball League, was exposed when Spirit drove over it during the 1,150th Martian day, or sol, of Spirit's Mars surface mission (March 29, 2007). One of Spirit's six wheels no longer rotates, so it leaves a deep track as it drags through soil. Most patches of disturbed, bright soil that Spirit had investigated previously are rich in sulfur, but this one has very little sulfur and is about 90 percent silica. This image is a approximately true-color composite of three images taken through different filters by Spirit's panoramic camera on Sol 1,187 (May 6). The track of disturbed soil is roughly 20 centimeters (8 inches) wide. Spirit's miniature thermal emission spectrometer, which can assess a target's mineral composition from a distance, examined the Gertrude Weise patch on Sol 1,172 (April 20). The indications it found for silica in the overturned soil prompted a decision to drive Spirit close enough to touch the soil with the alpha particle X-ray spectrometer, a chemical analyzer at the end of Spirit's robotic arm. The alpha particle X-ray spectrometer collected data about this target on sols 1,189 and 1,190 (May 8 and May 9) and produced the finding of approximately 90 percent silica. Silica is silicon dioxide. On Earth, it commonly occurs as the crystalline mineral quartz and is the main ingredient in window glass. The Martian silica at Gertrude Weise is non-crystalline, with no detectable quartz. In most cases, water is required to produce such a concentrated deposit of silica, according to members of the rover science team. One possible origin for the silica could have been interaction of soil with acidic steam produced by volcanic activity. Another could have been from water in a hot

  20. Spirit Does a 'Jig' at Laguna Hollow

    Science.gov (United States)

    2004-01-01

    This front hazard-avoidance image taken by the Mars Exploration Rover Spirit on sol 45 shows Spirit in its new location after a drive totaling about 20 meters (65.6 feet). The circular depression that Spirit is in, dubbed 'Laguna Hollow,' was most likely formed by a small impact.Scientists were interested in reaching Laguna Hollow because of the location's abundance of very fine, dust-like soil. The fine material could be atmospheric dust that has settled into the depression, or a salt-based material that causes crusts in the soils and coating on rocks. Either way, scientists hope to be able to characterize the material and broaden their understanding of this foreign world.To help scientists get a better look at the variations in the fine-grained dust at different depths, controllers commanded Spirit to 'jiggle' its wheels in the soil before backing away to a distance that allows the area to be reached with the robotic arm. Spirit will likely spend part of sol 46 analyzing this area with the instruments on its robotic arm.

  1. Spirit Begins Drive Around Home Plate

    Science.gov (United States)

    2009-01-01

    The hazard avoidance camera on the front of NASA's Mars Exploration Rover Spirit took this image after a drive by Spirit on the 1,829th Martian day, or sol, of Spirit's mission on the surface of Mars (Feb. 24, 2009). On Sol 1829, Spirit drove 6.29 meters (21 feet) northwestward, away from the northern edge of the low plateau called 'Home Plate.' The track dug by the dragged right-front wheel as the rover drove backward is visible in this image, receding toward the southeast. Rock layers of the northern slope of Home Plate are visible in the upper right portion of the image. In sols prior to 1829, the rover team had been trying to maneuver Spirit to climb onto the northern edge of Home Plate, ready to drive southward across the top of the plateau toward science destinations south of Home Plate. The Sol 1829 drive was the first move of a revised strategy to circle at least partway around Home Plate on the trek toward the sites south of the plateau.

  2. Impact Crater in Coastal Patagonia

    Science.gov (United States)

    D'Antoni, Hector L; Lasta, Carlos A.; Condon, Estelle (Technical Monitor)

    2000-01-01

    Impact craters are geological structures attributed to the impact of a meteoroid on the Earth's (or other planet's) surface (Koeberl and Sharpton. 1999). The inner planets of the solar system as well as other bodies such as our moon show extensive meteoroid impacts (Gallant 1964, French 1998). Because of its size and gravity, we may assume that the Earth has been heavily bombarded but weathering and erosion have erased or masked most of these features. In the 1920's, a meteor crater (Mark 1987) was identified in Arizona and to this first finding the identification of a large number of impact structures on Earth followed (Hodge 1994). Shock metamorphic effects are associated with meteorite impact craters. Due to extremely high pressures, shatter cones are produced as well as planar features in quartz and feldspar grains, diaplectic glass and high-pressure mineral phases such as stishovite (French 1998).

  3. View Ahead After Spirit's Sol 1861 Drive

    Science.gov (United States)

    2009-01-01

    NASA's Mars Exploration Rover Spirit used its navigation camera to take the images combined into this 210-degree view of the rover's surroundings during the 1,861st to 1,863rd Martian days, or sols, of Spirit's surface mission (March 28 to 30, 2009). The center of the scene is toward the south-southwest. East is on the left. West-northwest is on the right. The rover had driven 22.7 meters (74 feet) southwestward on Sol 1861 before beginning to take the frames in this view. The drive brought Spirit past the northwestern corner of Home Plate. In this view, the western edge of Home Plate is on the portion of the horizon farthest to the left. A mound in middle distance near the center of the view is called 'Tsiolkovsky' and is about 40 meters (about 130 feet) from the rover's position. This view is presented as a cylindrical projection with geometric seam correction.

  4. Size-Frequency Distribution of Small Lunar Craters: Widening with Degradation and Crater Lifetime

    Science.gov (United States)

    Ivanov, B. A.

    2018-01-01

    The review and new measurements are presented for depth/diameter ratio and slope angle evolution during small ( D impact craters aging (degradation). Comparative analysis of available data on the areal cratering density and on the crater degradation state for selected craters, dated with returned Apollo samples, in the first approximation confirms Neukum's chronological model. The uncertainty of crater retention age due to crater degradational widening is estimated. The collected and analyzed data are discussed to be used in the future updating of mechanical models for lunar crater aging.

  5. The self-secondary crater population of the Hokusai crater on Mercury

    Science.gov (United States)

    Xiao, Zhiyong; Prieur, Nils C.; Werner, Stephanie C.

    2016-07-01

    Whether or not self-secondaries dominate small crater populations on continuous ejecta deposits and floors of fresh impact craters has long been a controversy. This issue potentially affects the age determination technique using crater statistics. Here the self-secondary crater population on the continuous ejecta deposits of the Hokusai crater on Mercury is unambiguously recognized. Superposition relationships show that this population was emplaced after both the ballistic sedimentation of excavation flows and the subsequent veneering of impact melt, but it predated the settlement and solidification of melt pools on the crater floor. Fragments that formed self-secondaries were launched via impact spallation with large angles. Complex craters on the Moon, Mercury, and Mars probably all have formed self-secondaries populations. Dating young craters using crater statistics on their continuous ejecta deposits can be misleading. Impact melt pools are less affected by self-secondaries. Overprint by subsequent crater populations with time reduces the predominance of self-secondaries.

  6. Life and death in Kardecist Spiritism

    Directory of Open Access Journals (Sweden)

    Maria Laura Viveiros de Castro Cavalcanti

    2006-01-01

    Full Text Available The paper analyses from an anthropological perspective how Brazilian Spiritism resignifies the current notions of life and death, comparing the notion of reincarnation with the Christian and Catholic notion of purgatory. The search for understanding of the processes of identity construction in this religious system leads to the examination of the notions of reincarnation, karma, evolution, mediumship and probation, which are central to Kardecian cosmology. With this active set of notions, Spiritism proposes a rich set of perspectives about the self, and simultaneously graduates and softens the otherness of death.

  7. Revisiting the crater of doom

    Science.gov (United States)

    de Régules, Sergio

    2015-09-01

    The Chicxulub impact structure in Mexico is widely believed to be the site of the asteroid impact that allegedly killed the dinosaurs. As Sergio de Régules reports, scientists are now preparing to glean from it new insights into crater formation, materials science and the mechanisms of mass extinction.

  8. Key Recent Scientific Results from the Opportunity Rover's Exploration of Cape Tribulation, Endeavour Crater, Mars

    Science.gov (United States)

    Arvidson, R. E.; Squyres, S. W.; Gellert, R.; Herkenhoff, K. E.; Mittlefehldt, D. W.; Crumpler, L. S.; McLennan, S. M.; Farrand, W. H.; Jolliff, B. L.; Morris, R. V.

    2015-12-01

    The Opportunity Rover is in its 11th year of exploration, currently exploring the Cape Tribulation rim segment of the ~22 km wide Noachian Endeavour Crater and its tilted and fractured outcrops. A key target for Opportunity's measurements has been the Spirit of Saint Louis crater (SoSL), which is ~25 m wide, oval in plan view, shallow, flat-floored, and has a slightly raised rim. SoSL crater is surrounded by an apron of bright, polygonally-shaped outcrops and is superimposed on a gentle swale in Cape Tribulation. Rocks in a thin reddish zone on the rim are enriched in hematite, Si, and Ge, and depleted in Fe, relative to surrounding rocks. Apron rocks include an outcrop also enriched in Si and Ge, and slightly depleted in Fe. In general rocks in the crater and apron have elevated S levels relative to Shoemaker formation breccias, tracking values observed in the Cook Haven (gentle swale superimposed on Murray Ridge and site of Opportunity's 5th winter site) and the Hueytown fracture (running perpendicular to Cape Tribulation) outcrops. SoSL crater lies just to the west of Marathon Valley, a key target for exploration by Opportunity because five separate CRISM observations indicate the presence of Fe/Mg smectites on the upper valley floor. Opportunity data show that low relief, relatively bright, wind-scoured outcrops dominate the valley floor where not covered by scree and soil shed from surrounding walls. Initial reconnaissance shows that the outcrops are breccias with compositions similar to the typical SoSL crater apron and floor rocks, although only the very upper portion of the valley has been explored as of August 2015. Pervasive but modest aqueous alteration of Endeavour's rim is implied by the combination of CRISM and Opportunity data, providing insight into early aqueous processes dominated in this location by relatively low water to rock ratios, and at least in part associated with enhanced fluid flow along fractures.

  9. 27 CFR 27.120 - Persons authorized to receive distilled spirits imported in bulk.

    Science.gov (United States)

    2010-04-01

    ... SPIRITS, WINES, AND BEER Importation of Distilled Spirits In Bulk § 27.120 Persons authorized to receive distilled spirits imported in bulk. Distilled spirits imported in bulk (i.e., in containers having a...

  10. 27 CFR 24.233 - Addition of spirits to wine.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Addition of spirits to wine. 24.233 Section 24.233 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU, DEPARTMENT OF THE TREASURY LIQUORS WINE Spirits § 24.233 Addition of spirits to wine. (a) Prior to the addition of spirits. Wine will be placed...

  11. George Peabody and the Spirit of America.

    Science.gov (United States)

    Parker, Franklin

    1994-01-01

    One of a collection of articles on philanthropist George Peabody tells the story of two bronze doors made by sculptor Louis Amateis for the U.S. Capitol. The doors include a panel entitled Apotheosis of America that captures Amateis' vision of the spirit of America and includes the figures of George Peabody and other historic personages. (SM)

  12. Science-its Philosophy and Spirit

    Indian Academy of Sciences (India)

    Home; Journals; Resonance – Journal of Science Education; Volume 1; Issue 7. Science - its Philosophy and Spirit. Hermann Bondi. Reflections Volume 1 Issue 7 July 1996 pp 82-95. Fulltext. Click here to view fulltext PDF. Permanent link: http://www.ias.ac.in/article/fulltext/reso/001/07/0082-0095. Author Affiliations.

  13. Methanol levels in methylated spirit drinking alcoholics.

    Science.gov (United States)

    Caldwell, K

    1986-10-08

    On three different occasions, blood samples sent to this laboratory from the accident and emergency department were found to contain potentially toxic amounts of methanol (30, 34 and 41 mmol/l) during analysis for ethanol by a gas chromatographic method. It is suggested that the simultaneous determination of both alcohols may be clinically important in methylated spirit drinking alcoholics.

  14. The Teacher as an Archetype of Spirit

    Science.gov (United States)

    Mayes, Clifford

    2002-01-01

    Many images of the teacher in the current literature on teaching and teacher reflectivity can be seen as aspects of the Jungian image of the teacher as an archetype of spirit. These images--the teacher as philosopher, prophet, Zen master, and priest--correspond to what I call dialogical, civic, ontological and incarnational spirituality,…

  15. Physics issues of a proposed program, SPIRIT

    International Nuclear Information System (INIS)

    Ji, Hantao; Yamada, Masaaki

    2000-01-01

    Physics issues of the proposed program, SPIRIT (Self-organized Plasma with Induction, Reconnection, and Induction Techniques) are discussed. The main purpose of this program is to explore the physics of global stability and sustainment of compact toroids, including FRC (field reversed configuration) as well as low-aspect-ratio RFP (reversed field pinch), spheromak and spherical torus. (author)

  16. Europe's crisis : unification without a unifying spirit

    NARCIS (Netherlands)

    Margriet Krijtenburg

    2011-01-01

    What is happening to the EU? Following Schuman’s line of thought we can see that the crisis is linked with the lack of a European spirit among member states, together with the lack of a moral order as the guiding principle for European policies – including in the field of finance. It is the speed of

  17. Blocky craters: implications about the lunar megaregolith

    International Nuclear Information System (INIS)

    Thompson, T.W.; Roberts, W.J.; Hartmann, W.K.; Shorthill, R.W.; Zisk, S.H.

    1979-01-01

    Radar, infrared, and photogeologic properties of lunar craters have been studied to determine whether there is a systematic difference in blocky craters between the maria and terrae and whether this difference may be due to a deep megaregolith of pulverized material forming the terra surface, as opposed to a layer of semi-coherent basalt flows forming the mare surface. Some 1310 craters from about 4 to 100 km diameter have been catalogued as radar and/or infrared anomalies. In addition, a study of Apollo Orbital Photography confirmed that the radar and infrared anomalies are correlated with blocky rubble around the crater. Analysis of the radar and infrared data indicated systematic terra-mare differences. Fresh terra craters smaller than 12 km were less likely to be infrared and radar anomalies than comparable mare craters: but terra and mare craters larger than 12 km had similar infrared and radar signatures. Also, there are many terra craters which are radar bright but not infrared anomalies. The authors interpretation of these data is that while the maria are rock layers (basaltic flow units) where craters eject boulder fields, the terrae are covered by relatively pulverized megaregolith at least 2 km deep, where craters eject less rocky rubble. Blocky rubble, either in the form of actual rocks or partly consolidated blocks, contributes to the radar and infrared signatures of the crater. However, aging by impacts rapidly destroys these effects, possibly through burial by secondary debris or by disintegration of the blocks themselves, especially in terra regions. (Auth.)

  18. Klubi "Spirit" = Club Spirit / Hanno Soans ; tõlk. Liisi Ojamaa

    Index Scriptorium Estoniae

    Soans, Hanno, 1974-

    2000-01-01

    Eesti klubikultuurist 1990-ndatel. Klubi "Spirit" kujundusest. Sisearhitektid Tarmo Piirmets, Martti Siimann. Arhitekt Jüri Irik Arhitektuuribüroost Ehala & Irik. Projekt ja klubi valmis 2000. Flaierid kujundas Aadam Kaarma. 10 ill. Vaated, korruste plaanid

  19. On shaping of craters at ion bombardment

    International Nuclear Information System (INIS)

    Kalinichenko, A.I.; Perepelkin, S.S.; Strel'nitskij, V.E.

    2013-01-01

    Effect of plasticity and surface tension of metal on form and size of crater produced by heavy low-energy ion is theoretically investigated. Crater is approximated by an axially-symmetrical hollow. The hollow is characterized by known volume and two radii which specify curvatures of both bottom and peripheral parts of crater. Radii of curvature are determined by equality of surface tension forces and elastic reaction of metal. Equations for crater depth and diameter as well as for coefficient of increase of free surface ? due to crater and droplet formation are derived. Dependences of crater form and size on yield strength and surface tension coefficient of metal are analyzed. Influence of specified characteristics on possibility of droplet sputtering and nanometer-sized craters formation at ion bombardment of metals is shown.

  20. 27 CFR 19.65 - Experimental distilled spirits plants.

    Science.gov (United States)

    2010-04-01

    ... spirits plants. 19.65 Section 19.65 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU, DEPARTMENT OF THE TREASURY LIQUORS DISTILLED SPIRITS PLANTS Administrative and Miscellaneous Provisions Activities Not Subject to This Part § 19.65 Experimental distilled spirits plants. The...

  1. 27 CFR 19.67 - Spirits produced in industrial processes.

    Science.gov (United States)

    2010-04-01

    ... industrial processes. 19.67 Section 19.67 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND... Miscellaneous Provisions Activities Not Subject to This Part § 19.67 Spirits produced in industrial processes. (a) Applicability. (1) Persons who produce spirits in industrial processes (including spirits...

  2. 27 CFR 19.984 - Record of spirits received.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Record of spirits received. 19.984 Section 19.984 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU, DEPARTMENT OF THE TREASURY LIQUORS DISTILLED SPIRITS PLANTS Distilled Spirits For Fuel Use Accounting for...

  3. Two Spirit: Counseling Native American Gay, Lesbian, and Bisexual People.

    Science.gov (United States)

    Garrett, Michael Tlanusta; Barret, Bob

    2003-01-01

    The cultural world of the Two Spirit, the traditional role of Native individuals believed to possess both male and female spirit, is explored in both "old ways" and current-day experiences. Cultural beliefs and meanings around sexual identity are discussed from a Native perspective with recommendations for counseling Two Spirit clients.…

  4. 27 CFR 27.31 - Warehouse receipts covering distilled spirits.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Warehouse receipts... BEER Dealer Registration and Recordkeeping § 27.31 Warehouse receipts covering distilled spirits. The sale of warehouse receipts for distilled spirits is equivalent to the sale of distilled spirits...

  5. 27 CFR 31.47 - Warehouse receipts covering spirits.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Warehouse receipts... Part Certain Organizations, Agencies, and Persons § 31.47 Warehouse receipts covering spirits. The sale of warehouse receipts for distilled spirits is equivalent to the sale of distilled spirits...

  6. Crater Degradation on Mercury: A Global Perspective

    Science.gov (United States)

    Kinczyk, M. J.; Byrne, P. K.; Prockter, L. M.; Susorney, H. C. M.; Chapman, C. R.; Barnouin, O. S.

    2017-12-01

    On geologic timescales, initially fresh craters are subjected to many weathering mechanisms. Whereas water and wind are, or were, effective erosive mechanisms such as on Earth and Mars, micrometeorite bombardment and modification due to subsequent impacts are the dominant processes that degrade craters and crater rays on airless bodies like the Moon and Mercury. Classifying craters based on their state of degradation can help determine the relative ages of landforms proximal to, and crosscut by, these craters. However, this method is most effective when used together with statistical analysis of crater distributions. Pre-MESSENGER degradation classification schemes lacked sufficient detail to be consistently applied to craters of various sizes and morphological types—despite evidence suggesting that the ejecta deposits of large basins persist much longer than those of smaller craters, for instance—yet broad assumptions have been made regarding the correlation of crater class to the planet's time-stratigraphic sequence. Moreover, previous efforts to categorize craters by degradation state have either been restricted to regional study sites or applied only to a subset of crater age or size. As a result, numerous interpretations of crater degradation state persist for Mercury, challenging a complete understanding of this process on the innermost planet. We report on the first global survey of crater degradation on Mercury. By modifying an established 5-class scheme, we have systematically applied a rigorous set of criteria to all craters ≥40 km in diameter on the planet. These criteria include the state and morphology of crater deposits separately (e.g., rim, floor, wall, ejecta) and degradation classes were assigned as the collection of these individual attributes. This approach yields a consistent classification of craters of different sizes. Our results provide the first comprehensive assessment of how craters of various states of degradation are distributed

  7. Effect of spirit irradiation with 60Co gamma-rays

    International Nuclear Information System (INIS)

    Gwardys, S.

    1975-01-01

    A few sorts of spirit were irradiated with a dose of 1 or 5 Mrad of 60 Co gamma-rays. Then the chemical composition of spirits was investigated. It was found that as a result of irradiation the content of acids, esters, acetal aldehydes and methanol increases, while the strength of higher alcohols decreases slightly. The changes of compounds content in particular spirits are dependent on radiation doses and chemical composition before irradiation. It was also discovered that spirit irradiation causes decrease or even disappearance of characteristic - for given spirits - maxima of UV absorption. (Z.M.)

  8. Impact Craters: Size-Dependent Degration Rates

    Science.gov (United States)

    Ravi, S.; Mahanti, P.; Meyer, H. M.; Robinson, M. S.

    2017-12-01

    From superposition relations, Shoemaker and Hackman (1) devised the lunar geologic timescale with Copernican and Eratosthenian as the most recent periods. Classifying craters into the two periods is key to understanding impactor flux and regolith maturation rates over the last 3 Ga. Both Copernican and Eratosthenian craters exhibit crisp morphologies (sharp rims, steep slopes), however, only the former exhibit high reflectance rays and ejecta (1). Based on the Optical Maturity Parameter (OMAT; 2), Grier et al. (3) classified 50 fresh craters (D >20 km) into 3 categories - young (OMAT >0.22), intermediate, and old (OMAT 10) were identified (4) from a catalogue of 11,875 craters (5). In this work; we compare two size ranges (D: 5 km - 10 km and 10 km to 15 km) of 177 Copernican craters based on the average OMAT, measured near the crater rim (3). OMAT is measured at the crater rim (as opposed to further away from the crater) to minimize the influence of spatial variation of OMAT (6) in our investigation. We found that OMAT values are typically lower for smaller craters (5km age, craters with higher d/D value (morphologically fresher) should have higher OMAT, but this is not the case. We propose that quicker loss of OMAT (over time) for smaller craters compared to decrease in d/D with crater ageing, is responsible for the observed decreased OMAT for smaller craters. (1) Shoemaker and Hackman, 1962 (2) Lucey et al., 2000 (3) Grier et al., 2001 (4) Ravi et al., 2016 (5) Reinhold et al., 2015 (6) Mahanti et al., 2016

  9. Gullies in Crater in Hellas

    Science.gov (United States)

    2003-01-01

    MGS MOC Release No. MOC2-571, 11 December 2003This October 2003 Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows gullies cut into debris on the southeast-facing wall of an old meteor impact crater in southeastern Hellas Planitia. This view is located near 44.5oS, 277.0oW. The 200 meter scale bar is approximately 656 feet across; the picture is illuminated from the upper left.

  10. The SPIRIT Telescope Initiative: six years on

    Science.gov (United States)

    Luckas, Paul

    2017-06-01

    Now in its sixth year of operation, the SPIRIT initiative remains unique in Australia, as a robust web-enabled robotic telescope initiative funded for education and outreach. With multiple modes of operation catering for a variety of usage scenarios and a fully supported education program, SPIRIT provides free access to contemporary astronomical tools for students and educators in Western Australia and beyond. The technical solution itself provides an excellent model for low cost robotic telescope installations, and the education program has evolved over time to include a broad range of student experiences-from engagement activities to authentic science. This paper details the robotic telescope solution, student interface and educational philosophy, summarises achievements and lessons learned and examines the possibilities for future enhancement including spectroscopy.

  11. Decolonizing Education: Nourishing the Learning Spirit

    Directory of Open Access Journals (Sweden)

    Jennifer Brant

    2014-10-01

    Full Text Available As an emerging Indigenous scholar completing a mainstream doctoral program, I was immediately drawn to the work of Marie Battiste. Her work inspires my commitment to approach my degree as a decolonizing journey that nourishes my own learning spirit. Battiste (1998 captures the paradox of mainstream education as it is experienced by Aboriginal students. As she pointed out while Aboriginal students are looking to liberate themselves and their communities through education, they are faced with a strenuous curriculum that does not “mirror” them. As a result, students experience a “fragmented existence” (p. 24. This has indeed been my experience. Her recent book, Decolonizing Education: Nourishing the Learning Spirit expresses the tensions Indigenous learners face in all levels of mainstream education. These are the very tensions I personally experienced throughout the entirety of my educational experience as I have attempted to secure my own space and sense of place as a student and now aspiring professor.

  12. Volatile congeners in strong alcoholic fruit spirits

    OpenAIRE

    Kostik, Vesna; Memeti, Shaban; Bauer, Biljana

    2013-01-01

    The aim of our study was to identify and quantitatively analyze alcohol volatile congeners in different types of spirits from the domestic producers in order to evaluate their quality according to the Official Regulation. A total of 100 samples of three different types of grape brandies (lozova rakia, komova rakia and vinjak) and 30 samples of plum brandies obtained from seven domestic producers were analyzed on the content of ethanol, ethyl acetate, methanol, i-propanol, n- propanol, i-bu...

  13. Spirit of place: Bridging the 'epistemological gap'

    Science.gov (United States)

    Dudley, Nickola B. N.

    My work explores the psychological gap between humans and nature. Also how humanity is a parcel of nature and that the philosophy of spirit of place can create oneness through imagery, describing the landscape while also encompassing the 'larger frame' within the aesthetic. These transcendental moments connect with not only the landscape but to earth as a spiritual entity. My work is a response to the landscape and these moments.

  14. Clustered impacts - Experiments and implications. [cratering mechanics

    Science.gov (United States)

    Schultz, P. H.; Gault, D. E.

    1985-01-01

    The characteristics of impact by clusters of projectiles are experimentally studied by launching grouped projectiles of aluminum shot, steel shot, iron filings, and sand. Cratering efficiency is considered as a function of a dimensionless parameter related to projectile size and impact velocity. The effects of different target and projectile densities on cratering efficiency are examined. Crater morphology is addressed by considering a typical example, reviewing the systematics between cluster dispersion and crater morphology for vertical impacts, and examining oblique angle impacts which have relevance for planetary secondary cratering processes. These results are compared with impacts by single bodies with different strengths. The evolution of the ejecta plume for clustered impacts is compared to that for single-body impacts for vertical and oblique impacts from 1.3 to 1.8 km/s. The experimental results are discussed in the context of planetary surface processes, emphasizing processes in an atmosphere-free environment and secondary impact cratering.

  15. Spirit Beside 'Home Plate,' Sol 1809 (Stereo)

    Science.gov (United States)

    2009-01-01

    [figure removed for brevity, see original site] Left-eye view of a color stereo pair for PIA11803 [figure removed for brevity, see original site] Right-eye view of a color stereo pair for PIA11803 NASA Mars Exploration Rover Spirit used its navigation camera to take the images assembled into this stereo, 120-degree view southward after a short drive during the 1,809th Martian day, or sol, of Spirit's mission on the surface of Mars (February 3, 2009). By combining images from the left-eye and right-eye sides of the navigation camera, the view appears three-dimensional when viewed through red-blue glasses with the red lens on the left. Spirit had driven about 2.6 meters (8.5 feet) that sol, continuing a clockwise route around a low plateau called 'Home Plate.' In this image, the rocks visible above the rovers' solar panels are on the slope at the northern edge of Home Plate. This view is presented as a cylindrical-perspective projection with geometric seam correction.

  16. Defrosting of Russell Crater Dunes

    Science.gov (United States)

    2007-01-01

    These two images (at right) were acquired by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) 39 days apart at 19:10 UTC (2:10 PM EST) on December 28, 2006 (upper right) and at 20:06 UTC (3:06 PM EST) on February 5, 2007 (lower right). These CRISM data were acquired in 544 colors covering the wavelength range from 0.36-3.92 micrometers, and show features as small as 20 meters (about 65 feet) across. Both images are false color composites of bands at 2.5, 1.5, and 1.25 micrometers, and are nearly centered at the same location, 54.875oS, 12.919oE (upper right) and 54.895oS, 12.943oE (lower right). Each image is approximately 11 kilometers (7 miles) across at its narrowest. These are part of a series of images capturing the evolution of carbon dioxide frost on the surface of the dunes in Russell Crater. Russell Crater is one of many craters in the southern highland region of Mars that contain large areas of sand dunes. The sand in these dunes has accumulated over a very long time period -- perhaps millions of years -- as wind blows over the highland terrain, picking up sand in some places and depositing in others. The topography of the craters forces the wind to blow up and over the crater rims, and the wind often isn't strong enough to keep the tiny grains suspended. This makes the sand fall to the ground and gradually pile up, and over time the surface breezes shape the sand into ripples and dunes. A similar process is at work at the Great Sand Dunes National Park and Preserve in Colorado, USA. The above left image shows a THEMIS daytime infrared mosaic of Russell Crater and the location of its (approximately) 30-kilometer wide dune field in the northeastern quadrant of the crater floor. Superposed on this view and shown enlarged at the upper right is CRISM image FRT000039DF. This CRISM image was acquired during the late Martian southern winter (solar longitude = 157.7o), and the bright blue in this false color composite indicates the presence of

  17. What Really Happened to Earth's Older Craters?

    Science.gov (United States)

    Bottke, William; Mazrouei, Sara; Ghent, Rebecca; Parker, Alex

    2017-10-01

    Most assume the Earth’s crater record is heavily biased, with erosion/tectonics destroying older craters. This matches expectations, but is it actually true? To test this idea, we compared Earth’s crater record, where nearly all D ≥ 20 km craters are ages were computed using a new method employing LRO-Diviner temperature data. Large lunar rocks have high thermal inertia and remain warm through the night relative to the regolith. Analysis shows young craters with numerous meter-sized fragments are easy to pick out from older craters with eroded fragments. Moreover, an inverse relationship between rock abundance (RA) and crater age exists. Using measured RA values, we computed ages for 111 rocky craters with D ≥ 10 km that formed between 80°N and 80°S over the last 1 Gyr.We found several surprising results. First, the production rate of D ≥ 10 km lunar craters increased by a factor of 2.2 [-0.9, +4.4; 95% confidence limits] over the past 250 Myr compared to the previous 750 Myr. Thus, the NEO population is higher now than it has been for the last billion years. Second, the size and age distributions of lunar and terrestrial craters for D ≥ 20 km over the last 650 Myr have similar shapes. This implies that crater erasure must be limited on stable terrestrial terrains; in an average sense, for a given region, the Earth either keeps all or loses all of its D ≥ 20 craters at the same rate, independent of size. It also implies the observed deficit of large terrestrial craters between 250-650 Myr is not preservation bias but rather reflects a distinctly lower impact flux. We predict 355 ± 86 D ≥ 20 km craters formed on Earth over the last 650 Myr. Only 38 ± 6 are known, so the ratio, 10.7 ± 3.1%, is a measure of the Earth’s surface that is reasonably stable to large crater formation over 650 Myr. If erosion had dominated, the age distribution of terrestrial craters would be strongly skewed toward younger ages, which is not observed. We predict

  18. SPIRIT GUSJIGANG KUDUS DAN TANTANGAN GLOBALISASI EKONOMI

    Directory of Open Access Journals (Sweden)

    Muhamad Mustaqim

    2015-03-01

    Full Text Available THE SPIRIT OF GUSJIGANG KUDUS AND THE ECONOMIC GLOBALIZATION CHALLENGES. This paper intends to reveal the role of  Gusjigang business spirituality in facing the global economy. Kudus society known to have unique typology in business and learning, it is known as “Gusjigang”, it stands for the good, recite the Qur’an, and trade. Studies on the relationship between spirituality and business have been conducted a lot, but the study of the ethical spirit that focuses on business behavior of Muslim community in the context of  the trend of  economic globalization would still limited. The unique format and typology resulting from this study is expected to be a new concept for the development of Islamic economics and business at a different time and space in the future. In general, the results of this study came to the conclusion that Gusjigang spirit as glokalitas in business behavior. Glokalitas is a local moral value that is expected to become a universal character. This universal value if applied in the free competition, it will generate business behavior which always brings the perpetrators to goodness. Keywords: Gusjigang, Globalization, Economics. Tulisan ini bermaksud mengungkap peran spiritualitas bisnis Gusjigang dalam menghadapi ekonomi global. Masyarakat Kudus dikenal memiliki tipologi unik dalam berbisnis dan belajar, yang dikenal dengan istilah “Gusjigang”, kepanjangan dari bagus, ngaji, dan dagang. Kajian tentang hubungan antara spiritualitas dan perilaku bisnis memang sudah banyak dilakukan, tetapi kajian tentang spirit etik yang berfokus pada perilaku bisnis masyarakat Muslim konteksnya dengan kecenderungan globalisasi ekonomi kiranya masih terbatas. Format dan tipologi unik yang dihasilkan dari kajian ini diharapkan mampu menjadi konsep baru untuk pengembangan ekonomi dan bisnis Islam pada ruang dan waktu yang berbeda di masa mendatang. Secara umum, hasil kajian ini sampai pada penyimpulan spirit Gusjigang sebagai

  19. Volatile composition and sensory characters of commercial Galician orujo spirits.

    Science.gov (United States)

    Diéguez, Sandra C; de la Peña, M Luisa G; Gómez, Esperanza F

    2005-08-24

    Nineteen samples of commercial Galician orujo spirits were analyzed by gas chromatography and distinguished from one another on the basis of the concentrations of major volatile compounds (methanol, higher alcohols, esters, acetates, and aldehydes). The spirits were also sensorily analyzed to emphasize this differentiation and to establish a sensory profile as a function of the attributes defined by the tasters. The results show that the Galician orujo spirits present notably significant differences in the concentrations of 2-butanol, methanol, acetaldehyde, and ethyl lactate, whereas their ethylic esters contents are similar. Sensorily, the orujo spirits can be differentiated by taste but have similar characteristics of bouquet, the best of which are from the Godello variety. The descriptions employed to define the orujo spirits were herbaceous, floral, fruity, vegetal, alcohol, toasted, and "others". Floral and fruity were predominant in the Albariño orujo spirits; herbaceous was predominant in the plurivarietal orujo spirits, vegetal in the Godello spirits, and dried fruit or toasted in the Mencia spirits. The orujo spirits from Treixadura have the most diverse profile, with the participation of most of the attributes.

  20. Emphasizing humanities in medical education: Promoting the integration of medical scientific spirit and medical humanistic spirit.

    Science.gov (United States)

    Song, Peipei; Tang, Wei

    2017-05-23

    In the era of the biological-psychological-social medicine model, an ideal of modern medicine is to enhance the humanities in medical education, to foster medical talents with humanistic spirit, and to promote the integration of scientific spirit and humanistic spirit in medicine. Throughout the United States (US), United Kingdom (UK), other Western countries, and some Asian countries like Japan, many medical universities have already integrated the learning of medical humanities in their curricula and recognized their value. While in China, although medical education reform over the past decade has emphasized the topic of medical humanities to increase the professionalism of future physicians, the integration of medical humanity courses in medical universities has lagged behind the pace in Western countries. In addition, current courses in medical humanities were arbitrarily established due to a lack of organizational independence. For various reasons like a shortage of instructors, medical universities have failed to pay sufficient attention to medical humanities education given the urgent needs of society. The medical problems in contemporary Chinese society are not solely the purview of biomedical technology; what matters more is enhancing the humanities in medical education and fostering medical talents with humanistic spirit. Emphasizing the humanities in medical education and promoting the integration of medical scientific spirit and medical humanistic spirit have become one of the most pressing issues China must address. Greater attention should be paid to reasonable integration of humanities into the medical curriculum, creation of medical courses related to humanities and optimization of the curriculum, and actively allocating abundant teaching resources and exploring better methods of instruction.

  1. Compositions of Diverse Noachian Lithologies at Marathon Valley, Endeavour Crater Rim, Mars

    Science.gov (United States)

    Mittlefehldt, David W.; Gellert, Ralf; Yen, Albert S.; Ming, Douglas W.; Van Bommel, Scott; Farrand, William H.; Arvidson, Raymond E.; Rice, James W., Jr.

    2015-01-01

    Mars Exploration Rover Opportunity has been exploring Meridiani Planum for 11+ years, and is presently investigating the geology of rim segments of 22 km diameter, Noachian-aged Endeavour crater. The Alpha Particle X-ray Spectrometer has determined the compositions of a pre-impact lithology and impact breccias representing ejecta from the crater. Opportunity is now investigating the head (higher elevation, western end) of Marathon Valley. This valley cuts eastward through the central portion of the Cape Tribulation rim segment and provides a window into the lower stratigraphic record of the rim. At the head of Marathon Valley is a shallow (few 10s of cm), ovoid depression approximately 27×36 m in size, named Spirit of Saint Louis, that is surrounded by approximately 20-30 cm wide zone of more reddish rocks (red zone). Opportunity has just entered a region of Marathon Valley that shows evidence for Fe-Mg smectite in Compact Reconnaissance Imaging Spectrometer for Mars spectra indicating areally extensive and distinct lithologic units and/or styles of aqueous alteration. Rocks at the head of Marathon Valley and within Spirit of Saint Louis are breccias (valley-head rocks). In some areas, layering inside Spirit of Saint Louis appears continuous with the rocks outside. The valley-head rocks are of similar, generally basaltic composition. The continuity in composition, texture and layering suggest the valley-head rocks are coeval breccias, likely from the Endeavour impact. These local breccias are similar in non-volatile-element composition to breccias investigated elsewhere on the rim. Rocks within the red zone are like those on either side in texture, but have higher Al, Si and Ge, and lower S, Mn, Fe, Ni and Zn as compared to rocks on either side. The valley-head rocks have higher S than most Endeavour rim breccias, while red zone rocks are like those latter breccias in S. Patches within the rocks outside Spirit of Saint Louis have higher Al, Si and Ge indicating

  2. Laboratory approach to natural craters, can we?

    International Nuclear Information System (INIS)

    Tara Desai; Dimitri Batani; Marco Bussoli; Annamaria Villa; Biljana Gakovic

    2006-01-01

    Complete test of publication follows. In the present work we report an experimental study on the crater development using Nd:YAG laser system of 40 ps at 1.06 and 0.532 μm laser wavelength with optical energy ∼ 100 and 50 mJ respectively. A flat aluminium (20 x 10 x 2 mm) of density 2.7 g/cc was used as a target. Experiments were performed in a plasma chamber under vacuum exceeding 10 -4 torr. We have measured the diameter and depth of the craters with different techniques. Crater diameter was measured using optical microscope and images were recorded using CCD camera. Optical Confocal Microscope and profilometry were used to measure crater diameter, depth and crater lips. Our preliminary results show that the initial diameter (Φ i ) of the laser spot on the target plays an important role in estimating the final diameter as Φ F = Φ i + E β where E is the incident energy and β ∼ 0.30. under our experimental conditions using 0.532 μm laser. A similar scaling for the meteor-craters yield β = 0.20. - 0.25 for simple craters according to meteor study. Although energy variation is several orders of magnitudes (with few joules laser energy in the lab to megatons of meteor energy), physics of crater formation in both cases draws close resemblance. Aim of our work is to understand the physics of laser produced laboratory craters to recognize some aspects of the natural craters. Recently, Petawatt lasers have been proposed to study meteorite impact physics (Rubenchik LLNL report, 1999). Several megatons meteors approaching the earth with velocity ∼ 20-100 Km/sec is a rare event, approximately, once in million years but accompanying effects persist in time. Remnants of the craters (including simple or complex craters) provide information with substantial margin error about the cratering processes on the terrestrial surfaces (including earth, moon, Jupiter etc.) and, mass and velocity during impact of the dead meteor. Several efforts are being made to scale such

  3. Dark Valley in Newton Crater

    Science.gov (United States)

    2003-01-01

    MGS MOC Release No. MOC2-418, 11 July 2003This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) high resolution image shows part of a dark-floored valley system in northern Newton Crater. The valley might have been originally formed by liquid water; the dark material is probably sand that has blown into the valley in more recent times. The picture was acquired earlier this week on July 6, 2003, and is located near 39.2oS, 157.9oW. The picture covers an area 2.3 km (1.4 mi) across; sunlight illuminates the scene from the upper left.

  4. Impact craters in South America

    CERN Document Server

    Acevedo, Rogelio Daniel; Ponce, Juan Federico; Stinco, Sergio G

    2015-01-01

    A complete and updated catalogue of impact craters and structures in South America from 2014 is presented here. Approximately eighty proven, suspected and disproven structures have been identified by several sources in this continent. All the impact sites of this large continent have been exhaustively reviewed: the proved ones, the possible ones and some very doubtful. Many sites remain without a clear geological ""in situ"" confirmation and some of them could be even rejected. Argentina and Brazil are leading the list containing almost everything detected. In Bolivia, Chile, Colombia, Guyana,

  5. Consciousness, Mind, and Spirit: Three Levels of Human Cognition

    Directory of Open Access Journals (Sweden)

    Andrej Ule

    2015-10-01

    Full Text Available The article elucidates three important concepts and realities that refer to cognitive phenomena and are often (mistakenly used as synonyms: consciousness (slo. zavest, mind (slo. um, and spirit (slo. duh. They present three levels of human cognition: individual-experiential, individual-mental, and trans-individual-mental. Simply put: the concept of consciousness pertains to the waking mental life of a human being, while the concept of mind pertains to the ability and activity to consciously comprehend and understand contents and objects of human activity. I delineate three “types” of spirit: personal spirit, objective spirit, and the objectification of spirit in productions of human culture; I have doubts, however, about the existence of cosmic or super-cosmic dimensions of spirit, although some interpretations of quantum physics and modern cosmology suggest that such dimensions are possible.

  6. Application of high explosion cratering data to planetary problems

    Science.gov (United States)

    Oberbeck, V. R.

    1977-01-01

    The present paper deals with the conditions of explosion or nuclear cratering required to simulate impact crater formation. Some planetary problems associated with three different aspects of crater formation are discussed, and solutions based on high-explosion data are proposed. Structures of impact craters and some selected explosion craters formed in layered media are examined and are related to the structure of lunar basins. The mode of ejection of material from impact craters is identified using explosion analogs. The ejection mode is shown to have important implications for the origin of material in crater and basin deposits. Equally important are the populations of secondary craters on lunar and planetary surfaces.

  7. Research on how to build team spirit of enterprise

    OpenAIRE

    Gao, Bingshun

    2015-01-01

    The purpose of this thesis was to introduce the importance of team spirit in enterprisees. This article focuses on the team's meaning and the importance of modern enterprise organization, exploring the Chinese team construction of the enterprise and the problems that exist in team. Team spirit is the key point for team members to achieve the mutual goal. Team spirit is the spiritual pillar of the enterprise, without the spiritual pillar of enterprise, there will be no more energy and comp...

  8. Hydrothermal Alteration at Lonar Crater, India and Elemental Variations in Impact Crater Clays

    Science.gov (United States)

    Newsom, H. E.; Nelson, M. J.; Shearer, C. K.; Misra, S.; Narasimham, V.

    2005-01-01

    The role of hydrothermal alteration and chemical transport involving impact craters could have occurred on Mars, the poles of Mercury and the Moon, and other small bodies. We are studying terrestrial craters of various sizes in different environments to better understand aqueous alteration and chemical transport processes. The Lonar crater in India (1.8 km diameter) is particularly interesting being the only impact crater in basalt. In January of 2004, during fieldwork in the ejecta blanket around the rim of the Lonar crater we discovered alteration zones not previously described at this crater. The alteration of the ejecta blanket could represent evidence of localized hydrothermal activity. Such activity is consistent with the presence of large amounts of impact melt in the ejecta blanket. Map of one area on the north rim of the crater containing highly altered zones at least 3 m deep is shown.

  9. Processes Modifying Cratered Terrains on Pluto

    Science.gov (United States)

    Moore, J. M.

    2015-01-01

    The July encounter with Pluto by the New Horizons spacecraft permitted imaging of its cratered terrains with scales as high as approximately 100 m/pixel, and in stereo. In the initial download of images, acquired at 2.2 km/pixel, widely distributed impact craters up to 260 km diameter are seen in the near-encounter hemisphere. Many of the craters appear to be significantly degraded or infilled. Some craters appear partially destroyed, perhaps by erosion such as associated with the retreat of scarps. Bright ice-rich deposits highlight some crater rims and/or floors. While the cratered terrains identified in the initial downloaded images are generally seen on high-to-intermediate albedo surfaces, the dark equatorial terrain informally known as Cthulhu Regio is also densely cratered. We will explore the range of possible processes that might have operated (or still be operating) to modify the landscape from that of an ancient pristinely cratered state to the present terrains revealed in New Horizons images. The sequence, intensity, and type of processes that have modified ancient landscapes are, among other things, the record of climate and volatile evolution throughout much of the Pluto's existence. The deciphering of this record will be discussed. This work was supported by NASA's New Horizons project.

  10. AHP 21: Review: Spirits of the Place

    Directory of Open Access Journals (Sweden)

    William B. Noseworthy

    2012-12-01

    Full Text Available John Holt draws deeply upon more than twenty years of scholarship on the Theravadin world in Spirits of the Place, a work that analyzes the historical role of Buddhism in Laos. This work will appeal to scholars in such diverse fields as history, anthropology, sociology, religious studies, US foreign policy, and area studies. In this study Holt turns his focus to the Lao ethnic majority of Laos and the Lao ethnic minority of Isan Province, Thailand,1 in five chapters that compellingly combine historiographic and anthropological analysis, including what (MacDaniel 2010:120 has referred to as "the best Literature review of scholarship on Lao religion to date…" ...

  11. Spirit, Mind and Body in Chumash Healing

    Directory of Open Access Journals (Sweden)

    James D. Adams

    2005-01-01

    Full Text Available This article discusses the importance of the spirit and mind in health and well-being among Chumash people. Prayer was the first step in healing since prayer invites the participation of God. Initiation practices are discussed that encouraged young people to develop the maturity and spiritual strength to become productive members of society. Pictographs were used in healing usually not only as a relaxation therapy, but also as a mode of education. A supportive environment was an important factor in Chumash health care, since the support of friends helps, comforts and relieves anxiety that is detrimental to healing.

  12. Monod and the spirit of molecular biology.

    Science.gov (United States)

    Morange, Michel

    2015-06-01

    The founders of molecular biology shared views on the place of biology within science, as well as on the relations of molecular biology to Darwinism. Jacques Monod was no exception, but the study of his writings is particularly interesting because he expressed his point of view very clearly and pushed the implications of some of his choices further than most of his contemporaries. The spirit of molecular biology is no longer the same as in the 1960s but, interestingly, Monod anticipated some recent evolutions of this discipline. Copyright © 2015 Académie des sciences. Published by Elsevier SAS. All rights reserved.

  13. Technical problems and future cratering experiments

    International Nuclear Information System (INIS)

    Knox, J.B.

    1969-01-01

    This paper reviews some of the key technical problems that remain to be solved in nuclear cratering technology. These include: (1) developing a broader understanding of the effects that material properties and water content of the earth materials around the shot have on cratering behavior, (2) extending the experimental investigation of retarc formation to include intermediate yields and various materials, and (3) improving our ability to predict the escape of radioactive material to the atmosphere to form the cloud source responsible for fallout. The formation processes of ejecta craters, retarcs, and subsidence craters are described in the light of our present understanding, and the major gaps in our understanding are indicated. Methods of calculating crater and retarc formation are discussed, with particular reference to the input information needed. Methods for calculating fallout are presented, and their shortcomings are discussed. A preliminary analysis of the safety factors associated with the presently proposed nuclear excavation concepts is presented. (author)

  14. Finding the Spirit Within: A Critical Analysis of Film Techniques in "Spirited Away"

    Science.gov (United States)

    Cooper, Damon

    2010-01-01

    In 2008 the New South Wales Board of Studies included Hayao Miyazaki's film "Spirited Away" as the prescribed text for the Higher School Certificate Japanese Extension course. A study of the film in this context requires students to engage with the text in three distinct ways: through language, cultural symbolism and relevance, and…

  15. 'Do not quench the Spirit!' The discourse of the Holy Spirit in earliest ...

    African Journals Online (AJOL)

    The Trinitarian discourse of the 4th and 5th centuries grew out of earlier developments, whilst at the same time reflecting a renewal over against the language of the earliest Christian sources. This article reflects on the way in which early Christianity thought about the Holy Spirit and developed a new discourse on the basis ...

  16. International Assistance in Naming Craters on Mercury

    Science.gov (United States)

    Weir, H. M.; Edmonds, J.; Hallau, K.; Hirshon, B.; Goldstein, J.; Hamel, J.; Hamel, S.; Solomon, S. C.

    2015-12-01

    NASA's robotic MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft made history in March 2011 by becoming the first to orbit Mercury. During the mission, MESSENGER acquired more than 250,000 images and made many other kinds of measurements. Names are often given to surface features that are of special scientific interest, such as craters. To draw international attention to the achievements of the spacecraft and engineers and scientists who made the MESSENGER mission a success, the MESSENGER Education and Public Outreach (EPO) Team initiated a Name a Crater on Mercury Competition.Five craters of particular geological interest were chosen by the science team. In accordance with International Astronomical Union (IAU) rules for Mercury, impact craters are named in honor of those who have made outstanding or fundamental contributions to the arts and humanities. He or she must have been recognized as a historically significant figure in the arts for at least 50 years and deceased for the last three years. We were particularly interested in entries honoring people from nations and cultural groups underrepresented in the current list of crater names. From more than 3600 entries received from around the world, the EPO team was able to reduce the number of entries to about 1200 names of 583 different artists who met the contest eligibility criteria. Next, the proposed individuals were divided into five artistic field groups and distributed to experts in that respective field. Each expert reviewed approximately100 artists with their biographical information. They narrowed down their list to a top ten, then to a top five by applying a rubric. The final selection was based on the reviewer lists and scores, with at least three finalist names selected from each artistic field. Of the 17 finalists provided to the IAU, the following names were selected: Carolan crater, Enheduanna crater, Karsh crater, Kulthum crater, and Rivera crater. For more

  17. Conference report. Can spirit of Cairo survive?

    Science.gov (United States)

    Chhabra, R

    1994-01-01

    Country representatives from around the globe came together at the 1994 International Conference on Population and Development (ICPD) to draft a document in the spirit of compromise and unified intent. Marked controversy and conflict plagued the conference, both before and during the official meetings. Accord was nonetheless reached. The author wonders how long and to what extent the euphoria and compromise of the ICPD will last now that official talks are over. It is clear that paranoia and discord subsumed during the conference will persist, foment, and potentially resurface in confrontation over time. The South, for example, was upset about the failure of the conference to focus more upon development and environmental issues, while the Southern women's groups invested their energies into political ideologies and their development as a counterforce to international multinational scientific and corporate lobbies on pharmaceutical and contraceptive technologies. The women's caucus instead adopted a Western world view of sexuality which effectively permeated their lobbying and the conference. While dissent may resurface over time, the ICPD nonetheless set into motion positive processes for nongovernmental organization participation in a spirit of partnership within the UN systems and in the formulation of national policies and programs of their respective countries. In closing, the author expresses her regret that China and India maintained a low profile at the official meeting, and that Pakistan, rooted in Islam, spoke for the Indian subcontinent.

  18. A NOESY-HSQC simulation program, SPIRIT

    International Nuclear Information System (INIS)

    Zhu Leiming; Dyson, H. Jane; Wright, Peter E.

    1998-01-01

    A program SPIRIT (Simulation Program considering Incomplete Recovery of z magnetization and INEPT Transfer efficiency) has been developed to simulate three-dimensional NOESY-HSQC spectra. This program takes into account (1) different transfer efficiency during INEPT and reverse INEPT durations due to differential relaxation rates and 1 J coupling constants; (2) the different effect of the sensitivity-enhancement scheme on CH, CH 2 and CH 3 systems; and (3) incomplete recovery of longitudinal magnetization between scans. The simulation program incorporates anisotropic tumbling mode for symmetric tops, and allows for differential external relaxation rates for protons. Some well-defined internal motions, such as the fast rotation of methyl groups, are taken into account. The simulation program also allows for input of multiple conformations and their relative populations to calculate the average relaxation matrix to account for slow internal motions. With the SPIRIT program, the sensitivity-enhanced NOESY-HSQC experiment can be used directly in the evaluation of the accuracy of structures, which can potentially be improved by direct refinement against the primary data. Abbreviations: NOESY, nuclear Overhauser enhancement spectroscopy; HSQC, heteronuclear single quantum correlation; INEPT, insensitive nuclei enhanced by polarization transfer

  19. Investigations of Ceres's Craters with Straightened Rim

    Science.gov (United States)

    Frigeri, A.; De Sanctis, M. C.; Ammannito, E.; Raponi, A.; Formisano, M.; Ciarniello, M.; Magni, G.; Combe, J. P.; Marchi, S.; Raymond, C. A.; Schwartz, S. J.

    2017-12-01

    Dwarf planet Ceres hosts some geological features that are unique in the solar system because its composition, rich in aqueously-altered silicates, is usually found on full-size planets, whereas its mean radius is smaller than most natural satellites in the solar system. For example, the local high-albedo, carbonate-rich areas or faculaeare specific to Ceres; also, the absence of big impact crater structures is key to understand the overall mechanical behaviour of the Cerean crust. After the first findings of water ice occurring in the shadowed areas of craters on Ceres by the NASA/Dawn mission (1, 2), we analyzed the morphology of craters looking for features similar to the ones where the water ice composition has been detected analyzing the data from the VIR spectrometer (3). These craters fall outside of the family of polygonal craters which are mainly related to regional or global scale tectonics (4). We analyzed the morphology on the base of the global mosaic, the digital terrain model derived by using the stereo photogrammetry method and the single data frames of the Framing Camera. Our investigation started from crater Juling, which is characterized by a portion of the rim which forms a straight segment instead of a portion of a circle. This linear crater wall is also steep enough that it forms a cliff that is in the shadowed area in all images acquired by Dawn. Very smooth and bright deposits lay at the foot of this crater-wall cliff. Then, we identified several other craters, relatively fresh, with radius of 2 to 10 kilometers, showing one or two sectors of the crater-rim being truncated by a mass-wasting process, probably a rockfall. Our first analysis show that in the selected craters, the truncated sectors are always in the north-eastern sector of the rim for the craters in the southern hemisphere. Conversely, the craters on the northern hemisphere exhibit a truncated rim in their south-eastern sector. Although a more detailed analysis is mandatory

  20. The effect of target properties on transient crater scaling for simple craters

    Science.gov (United States)

    Prieur, N. C.; Rolf, T.; Luther, R.; Wünnemann, K.; Xiao, Z.; Werner, S. C.

    2017-08-01

    The effects of the coefficient of friction and porosity on impact cratering are not sufficiently considered in scaling laws that predict the crater size from a known impactor size, velocity, and mass. We carried out a systematic numerical study employing more than 1000 two-dimensional models of simple crater formation under lunar conditions in targets with varying properties. A simple numerical setup is used where targets are approximated as granular or brecciated materials, and any compression of porous materials results in permanent compaction. The results are found to be consistent with impact laboratory experiments for water, low-strength and low-porosity materials (e.g., wet sand), and sands. Using this assumption, we found that both the friction coefficient and porosity are important for estimating transient crater diameters as is the strength term in crater scaling laws, i.e., the effective strength. The effects of porosity and friction coefficient on impact cratering were parameterized and incorporated into π group scaling laws, and predict transient crater diameters within an accuracy of ±5% for targets with friction coefficients f ≥ 0.4 and porosities Φ = 0-30%. Moreover, 90 crater scaling relationships are made available and can be used to estimate transient crater diameters on various terrains and geological units with different coefficient of friction, porosity, and cohesion. The derived relationships are most robust for targets with Φ > 10-15%, applicable for a lunar environment, and could therefore yield significant insights into the influence of target properties on cratering statistics.

  1. Evidence for rapid topographic evolution and crater degradation on Mercury from simple crater morphometry

    Science.gov (United States)

    Fassett, Caleb I.; Crowley, Malinda C.; Leight, Clarissa; Dyar, M. Darby; Minton, David A.; Hirabayashi, Masatoshi; Thomson, Bradley J.; Watters, Wesley A.

    2017-06-01

    Examining the topography of impact craters and their evolution with time is useful for assessing how fast planetary surfaces evolve. Here, new measurements of depth/diameter (d/D) ratios for 204 craters of 2.5 to 5 km in diameter superposed on Mercury's smooth plains are reported. The median d/D is 0.13, much lower than expected for newly formed simple craters ( 0.21). In comparison, lunar craters that postdate the maria are much less modified, and the median crater in the same size range has a d/D ratio that is nearly indistinguishable from the fresh value. This difference in crater degradation is remarkable given that Mercury's smooth plains and the lunar maria likely have ages that are comparable, if not identical. Applying a topographic diffusion model, these results imply that crater degradation is faster by a factor of approximately two on Mercury than on the Moon, suggesting more rapid landform evolution on Mercury at all scales.Plain Language SummaryMercury and the Moon are both airless bodies that have experienced numerous impact events over billions of years. These impacts form craters in a geologic instant. The question examined in this manuscript is how fast these craters erode after their formation. To simplify the problem, we examined craters of a particular size (2.5 to 5 km in diameter) on a particular geologic terrain type (volcanic smooth plains) on both the Moon and Mercury. We then measured the topography of hundreds of craters on both bodies that met these criteria. Our results suggest that craters on Mercury become shallower much more quickly than craters on the Moon. We estimate that Mercury's topography erodes at a rate at least a factor of two faster than the Moon's.

  2. Small Craters and Their Diagnostic Potential

    Science.gov (United States)

    Bugiolacchi, R.

    2017-07-01

    I analysed and compared the size-frequency distributions of craters in the Apollo 17 landing region, comprising of six mare terrains with varying morphologies and cratering characteristics, along with three other regions allegedly affected by the same secondary event (Tycho secondary surge). I propose that for the smaller crater sizes (in this work 9-30 m), a] an exponential curve of power -0.18D can approximate Nkm-2 crater densities in a regime of equilibrium, while b] a power function D-3 closely describes the factorised representation of craters by size (1 m). The saturation level within the Central Area suggests that c] either the modelled rates of crater erosion on the Moon should be revised, or that the Tycho event occurred much earlier in time than the current estimate. We propose that d] the size-frequency distribution of small secondary craters may bear the signature (in terms of size-frequency distribution of debris/surge) of the source impact and that this observation should be tested further.

  3. Processing Images of Craters for Spacecraft Navigation

    Science.gov (United States)

    Cheng, Yang; Johnson, Andrew E.; Matthies, Larry H.

    2009-01-01

    A crater-detection algorithm has been conceived to enable automation of what, heretofore, have been manual processes for utilizing images of craters on a celestial body as landmarks for navigating a spacecraft flying near or landing on that body. The images are acquired by an electronic camera aboard the spacecraft, then digitized, then processed by the algorithm, which consists mainly of the following steps: 1. Edges in an image detected and placed in a database. 2. Crater rim edges are selected from the edge database. 3. Edges that belong to the same crater are grouped together. 4. An ellipse is fitted to each group of crater edges. 5. Ellipses are refined directly in the image domain to reduce errors introduced in the detection of edges and fitting of ellipses. 6. The quality of each detected crater is evaluated. It is planned to utilize this algorithm as the basis of a computer program for automated, real-time, onboard processing of crater-image data. Experimental studies have led to the conclusion that this algorithm is capable of a detection rate >93 percent, a false-alarm rate <5 percent, a geometric error <0.5 pixel, and a position error <0.3 pixel.

  4. Buried Mid-Latitude Craters

    Science.gov (United States)

    2004-01-01

    MGS MOC Release No. MOC2-577, 17 December 2003This September 2003 Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) picture shows six circular features, three of which exhibit concentric, or 'bullseye,' patterns within them. Each circular feature is the remains of a partly-buried, partly-eroded, and partly-filled meteor impact crater. These occur in northeastern Arabia Terra. Areas such as this, located near the middle latitudes of Mars, commonly have a 'scabby' or roughened appearance. The cause of this 'terrain roughening' texture is unknown, although some scientists have speculated that it might result from the erosion and removal (by way of sublimation) of ground ice. This idea remains highly speculative. These features are located near 28.4oN, 317.5oW. The image covers an area 3 km (1.9 mi) wide; sunlight illuminates the scene from the lower left.

  5. Locating the LCROSS Impact Craters

    Science.gov (United States)

    Marshall, William; Shirley, Mark; Moratto, Zachary; Colaprete, Anthony; Neumann, Gregory A.; Smith, David E.; Hensley, Scott; Wilson, Barbara; Slade, Martin; Kennedy, Brian; hide

    2012-01-01

    The Lunar CRater Observations and Sensing Satellite (LCROSS) mission impacted a spent Centaur rocket stage into a permanently shadowed region near the lunar south pole. The Sheperding Spacecraft (SSC) separated approx. 9 hours before impact and performed a small braking maneuver in order to observe the Centaur impact plume, looking for evidence of water and other volatiles, before impacting itself. This paper describes the registration of imagery of the LCROSS impact region from the mid- and near-infrared cameras onboard the SSC, as well as from the Goldstone radar. We compare the Centaur impact features, positively identified in the first two, and with a consistent feature in the third, which are interpreted as a 20 m diameter crater surrounded by a 160 m diameter ejecta region. The images are registered to Lunar Reconnaisance Orbiter (LRO) topographical data which allows determination of the impact location. This location is compared with the impact location derived from ground-based tracking and propagation of the spacecraft's trajectory and with locations derived from two hybrid imagery/trajectory methods. The four methods give a weighted average Centaur impact location of -84.6796 deg, -48.7093 deg, with a 1s uncertainty of 115 m along latitude, and 44 m along longitude, just 146 m from the target impact site. Meanwhile, the trajectory-derived SSC impact location is -84.719 deg, -49.61 deg, with a 1 alpha uncertainty of 3 m along the Earth vector and 75 m orthogonal to that, 766 m from the target location and 2.803 km south-west of the Centaur impact. We also detail the Centaur impact angle and SSC instrument pointing errors. Six high-level LCROSS mission requirements are shown to be met by wide margins. We hope that these results facilitate further analyses of the LCROSS experiment data and follow-up observations of the impact region

  6. Cratering Rates in the Jovian System

    Science.gov (United States)

    Zahnle, K.; Dons, L.; Levison, H.

    2004-01-01

    We use several independent constraints on the number of ecliptic comets to estimate impact cratering rates on the Jupiter moons. The impact rate on Jupiter by 1.5-km diameter ecliptic comets is currently NY(d > 1.5km) = 0.005(+0.006)(-0.003) per annum. Asteroids and long period comets are currently unimportant. The size-number distribution of ecliptic comets smaller than 20 km is inferred from size-number distributions of impact craters on Europa, Ganymede, and Triton. For comets bigger than 50 km we use the size-number distribution of Kuiper Belt Objects. The overview of the impact rate at Jupiter in general and at Europa in particular are given. These impact rates imply cratering rates on Europa of 0.5 per Ma per 10(exp 6) sq km for impact craters bigger than 1 km, and of 0.015 per Ma per 10(exp 6) sq km for impact craters bigger than 20 km. The latter corresponds to an average recurrence time of 2.2 Ma for 20 km craters. The best current estimates for the number of 20 km craters on Europa appear to range between about twelve to thirty. This implies that the average age of Europa's surface is between 30 and 70 Ma. The average density of craters with diameter greater than 1 km on well-mapped swaths on Europa is 30 per 10(exp 6) sq km. The corresponding nominal surface age would be 60 Ma. These two estimates are not truly independent because we have used size-number distribution of the Europan craters to help generate the size-number distribution of comets. The uncertainty of the best estimate - call it 42 Ma for specificity - is at least a factor of 3.

  7. Craters of the Pluto-Charon System

    Science.gov (United States)

    Robbins, Stuart J.; Singer, Kelsi N.; Bray, Veronica J.; Schenk, Paul; Lauer, Todd R.; Weaver, Harold A.; Runyon, Kirby; Mckinnon, William B.; Beyer, Ross A.; Porter, Simon; hide

    2016-01-01

    NASA's New Horizons flyby mission of the Pluto-Charon binary system and its four moons provided humanity with its first spacecraft-based look at a large Kuiper Belt Object beyond Triton. Excluding this system, multiple Kuiper Belt Objects (KBOs) have been observed for only 20 years from Earth, and the KBO size distribution is unconstrained except among the largest objects. Because small KBOs will remain beyond the capabilities of ground-based observatories for the foreseeable future, one of the best ways to constrain the small KBO population is to examine the craters they have made on the Pluto-Charon system. The first step to understanding the crater population is to map it. In this work, we describe the steps undertaken to produce a robust crater database of impact features on Pluto, Charon, and their two largest moons, Nix and Hydra. These include an examination of different types of images and image processing, and we present an analysis of variability among the crater mapping team, where crater diameters were found to average +/-10% uncertainty across all sizes measured (approx.0.5-300 km). We also present a few basic analyses of the crater databases, finding that Pluto's craters' differential size-frequency distribution across the encounter hemisphere has a power-law slope of approximately -3.1 +/- 0.1 over diameters D approx. = 15-200 km, and Charon's has a slope of -3.0 +/- 0.2 over diameters D approx. = 10-120 km; it is significantly shallower on both bodies at smaller diameters. We also better quantify evidence of resurfacing evidenced by Pluto's craters in contrast with Charon's. With this work, we are also releasing our database of potential and probable impact craters: 5287 on Pluto, 2287 on Charon, 35 on Nix, and 6 on Hydra.

  8. Impact mechanics at Meteor Crater, Arizona

    Science.gov (United States)

    Shoemaker, Eugene Merle

    1959-01-01

    Meteor Crator is a bowl-shaped depression encompassed by a rim composed chiefly of debris stacked in layers of different composition. Original bedrock stratigraphy is preserved, inverted, in the debris. The debris rests on older disturbed strata, which are turned up at moderate to steep angles in the wall of the crater and are locally overturned near the contact with the debris. These features of Meteor Crater correspond closely to those of a crater produced by nuclear explosion where depth of burial of the device was about 1/5 the diameter of the resultant crater. Studies of craters formed by detonation of nuclear devices show that structures of the crater rims are sensitive to the depth of explosion scaled to the yield of the device. The structure of Meteor Crater is such as would be produced by a very strong shock originating about at the level of the present crater floor, 400 feet below the original surface. At supersonic to hypersonic velocity an impacting meteorite penetrates the ground by a complex mechanism that includes compression of the target rocks and the meteorite by shock as well as hydrodynamic flow of the compressed material under high pressure and temperature. The depth of penetration of the meteorite, before it loses its integrity as a single body, is a function primarily of the velocity and shape of the meteorite and the densities and equations of state of the meteorite and target. The intensely compressed material then becomes dispersed in a large volume of breccia formed in the expanding shock wave. An impact velocity of about 15 km/sec is consonant with the geology of Meteor Crater in light of the experimental equation of state of iron and inferred compressibility of the target rocks. The kinetic energy of the meteorite is estimated by scaling to have been from 1.4 to 1.7 megatons TNT equivalent.

  9. The discourse of the Holy Spirit in earliest Christianity

    African Journals Online (AJOL)

    2015-09-30

    Sep 30, 2015 ... In his Apology, chapter 10, Athenagoras explicitly describes the Holy Spirit as part of God. He refutes the allegation that. Christians are atheists and describes God as the triune ruler of the spiritual world: The prophetic Spirit also agrees with our statements. 'The Lord,' it says, 'made me, the beginning of His ...

  10. 27 CFR 17.184 - Distilled spirits container marks.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Distilled spirits container marks. 17.184 Section 17.184 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND... MANUFACTURING NONBEVERAGE PRODUCTS Miscellaneous Provisions § 17.184 Distilled spirits container marks. All...

  11. 27 CFR 19.996 - Withdrawal of spirits.

    Science.gov (United States)

    2010-04-01

    ... alcohol fuel plant, they must be rendered unfit for beverage use as provided in this subpart. Spirits rendered unfit for beverage use (fuel alcohol) may be withdrawn free of tax from plant premises exclusively... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Withdrawal of spirits. 19...

  12. 27 CFR 26.211 - Warehouse receipts covering distilled spirits.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Warehouse receipts... and Recordkeeping § 26.211 Warehouse receipts covering distilled spirits. The sale of warehouse..., warehouse receipts for distilled spirits stored in warehouses, or elsewhere, must register and keep records...

  13. 27 CFR 26.45 - Warehouse receipts covering distilled spirits.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Warehouse receipts... Recordkeeping § 26.45 Warehouse receipts covering distilled spirits. The sale of warehouse receipts for... distilled spirits into the United States from Puerto Rico who sells, or offers for sale, warehouse receipts...

  14. Ceres and the terrestrial planets impact cratering record

    Science.gov (United States)

    Strom, R. G.; Marchi, S.; Malhotra, R.

    2018-03-01

    Dwarf planet Ceres, the largest object in the Main Asteroid Belt, has a surface that exhibits a range of crater densities for a crater diameter range of 5-300 km. In all areas the shape of the craters' size-frequency distribution is very similar to those of the most ancient heavily cratered surfaces on the terrestrial planets. The most heavily cratered terrain on Ceres covers ∼15% of its surface and has a crater density similar to the highest crater density on population whose size-frequency distribution resembles that of the Main Belt Asteroids.

  15. Solidarity and Community Spirit during Evil Times

    Directory of Open Access Journals (Sweden)

    SIMONA-GRAZIA DIMA,

    2010-04-01

    Full Text Available The article aims both at identifying the various facets under which human solidarity manifested itself during the War of ethnic cleansing in Bosnia-Herzegovina (1992-1995 and at highlighting the growing awareness of the community spirit in the same period of time, resulting in a part of the population being saved and in many spiritual and material values being preserved. The analysis is based on genuine interviews given by subjects involved in the events, all of which being collected in the volume Good People in an Evil Time by Dr. Svetlana Broz, a journalist, social activist and cardiologist (now president of the Bosnia-Herzegovina branch of GARIWO International. This book has been a best seller, and has been translated in many languages and presented over many tours in about 50 universities in the USA.

  16. Field Reconnaissance Geologic Mapping of the Columbia Hills, Mars: Results from MER Spirit and MRO HiRISE Observations

    Science.gov (United States)

    Crumpler, L.S.; Arvidson, R. E.; Squyres, S. W.; McCoy, T.; Yingst, A.; Ruff, S.; Farrand, W.; McSween, Y.; Powell, M.; Ming, D. W.; Morris, R.V.; Bell, J.F.; Grant, J.; Greeley, R.; DesMarais, D.; Schmidt, M.; Cabrol, N.A.; Haldemann, A.; Lewis, Kevin W.; Wang, A.E.; Schroder, C.; Blaney, D.; Cohen, B.; Yen, A.; Farmer, J.; Gellert, Ralf; Guinness, E.A.; Herkenhoff, K. E.; Johnson, J. R.; Klingelhofer, G.; McEwen, A.; Rice, J. W.; Rice, M.; deSouza, P.; Hurowitz, J.

    2011-01-01

    Chemical, mineralogic, and lithologic ground truth was acquired for the first time on Mars in terrain units mapped using orbital Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (MRO HiRISE) image data. Examination of several dozen outcrops shows that Mars is geologically complex at meter length scales, the record of its geologic history is well exposed, stratigraphic units may be identified and correlated across significant areas on the ground, and outcrops and geologic relationships between materials may be analyzed with techniques commonly employed in terrestrial field geology. Despite their burial during the course of Martian geologic time by widespread epiclastic materials, mobile fines, and fall deposits, the selective exhumation of deep and well-preserved geologic units has exposed undisturbed outcrops, stratigraphic sections, and structural information much as they are preserved and exposed on Earth. A rich geologic record awaits skilled future field investigators on Mars. The correlation of ground observations and orbital images enables construction of a corresponding geologic reconnaissance map. Most of the outcrops visited are interpreted to be pyroclastic, impactite, and epiclastic deposits overlying an unexposed substrate, probably related to a modified Gusev crater central peak. Fluids have altered chemistry and mineralogy of these protoliths in degrees that vary substantially within the same map unit. Examination of the rocks exposed above and below the major unconformity between the plains lavas and the Columbia Hills directly confirms the general conclusion from remote sensing in previous studies over past years that the early history of Mars was a time of more intense deposition and modification of the surface. Although the availability of fluids and the chemical and mineral activity declined from this early period, significant later volcanism and fluid convection enabled additional, if localized, chemical activity.

  17. On the Clustering of Europa's Small Craters

    Science.gov (United States)

    Bierhaus, E. B.; Chapman, C. R.; Merline, W. J.

    2001-01-01

    We analyze the spatial distribution of Europa's small craters and find that many are too tightly clustered to result from random, primary impacts. Additional information is contained in the original extended abstract.

  18. Latitude Variation for Pluto's Crater Distribution

    Science.gov (United States)

    Dwivedi, A. K.; Binzel, R. P.; Earle, A. M.; Singer, K. N.; Stern, A.; Olkin, C.; Weaver, H. A., Jr.; Ennico Smith, K.; Young, L. A.

    2017-12-01

    The crater population distribution on Pluto and Charon have been studied to infer the size distribution of objects in the Kuiper belt (Singer et al. 2017; submitted). In this talk, we will look at the variation in crater distribution with latitude. To circumvent possible bias effects in the analysis, we focus our analysis on a region having the most consistent imaging resolution afforded by the flyby geometry. The longitudinal extent of our study region is 90E to 150E, and the latitudinal extent is 0°N to 90°N. Our preliminary analysis shows crater population peaks in the latitude range 30°N to 60°N and drops off sharply toward the north pole. Here we describe how we quantify the crater distribution in this region and explore a range of processes for volatile transport over both orbital timescales and perihelion precession timescales, including million year Milankovitch cycles for obliquity oscillations.

  19. Topography of the Martian Impact Crater Tooting

    Science.gov (United States)

    Mouginis-Mark, P. J.; Garbeil, H.; Boyce, J. M.

    2009-01-01

    Tooting crater is approx.29 km in diameter, is located at 23.4degN, 207.5degE, and is classified as a multi-layered ejecta crater [1]. Our mapping last year identified several challenges that can now be addressed with HiRISE and CTX images, but specifically the third dimension of units. To address the distribution of ponded sediments, lobate flows, and volatile-bearing units within the crater cavity, we have focused this year on creating digital elevation models (DEMs) for the crater and ejecta blanket from stereo CTX and HiRISE images. These DEMs have a spatial resolution of approx.50 m for CTX data, and 2 m for HiRISE data. Each DEM is referenced to all of the available individual MOLA data points within an image, which number approx.5,000 and 800 respectively for the two data types

  20. Key Recent Scientific Results from the Opportunity Rover's Exploration of Endeavour Crater, Mars

    Science.gov (United States)

    Arvidson, R. E.; Squyres, S. W.; Gellert, R.; Herkenhoff, K.; Mittlefehldt, D.; Crumpler, L.; McLennan, S.; Farrand, W. H.; Joliff, B. L.; Morris, R. V.

    2015-01-01

    The Opportunity Rover is currently in its 11th year of operations, exploring the rim of the approximately 22 km wide Noachian-age Endeavour Crater. Opportunity spent its 5th winter season in Cook Haven, a gentle swale along Murray Ridge. Two small rocks serendipitously overturned by rover wheel motions show evidence for aqueous precipitation of sulfates, and interaction with a strong oxidant (e.g., O2) to form a thin, high valence state Mn oxide coating. After the winter, Opportunity headed south to Cape Tribulation and explored Shoemaker formation impact breccias, finding numerous Ca-sulfate veins cutting across outcrops. A key target for Opportunity's measurements has been the Spirit of Saint Louis crater (SoSL), which is approximately 25 m wide, oval in plan view, shallow, flat-floored, and has a slightly raised rim. SoSL crater is surrounded by an apron of bright, polygonally-shaped outcrops and is superimposed on a gentle swale in Cape Tribulation. Rocks in a thin reddish zone on the rim are enriched in hematite, Si, and Ge, and depleted in Fe, relative to surrounding rocks. Apron rocks include an outcrop also enriched in Si and Ge, and slightly depleted in Fe. In general rocks in the crater and apron have elevated S relative to Shoemaker formation breccias, tracking values observed in the Cook Haven and the Hueytown (fracture running perpendicular to Cape Tribulation) outcrops. SoSL crater lies just to the west of Marathon Valley, a key target for exploration by Opportunity because five separate CRISM observations indicate the presence of Fe/Mg smectites on the upper valley floor. Opportunity data show that low relief, relatively bright polygonal outcrops dominate the valley floor where not covered by scree and soil shed from surrounding walls. Initial reconnaissance shows that the outcrops are breccias with compositions similar to the typical SoSL crater apron and floor rocks, although only the very upper portion of the valley has been explored as of August

  1. Crater Mound Formation by Wind Erosion on Mars

    Science.gov (United States)

    Steele, L. J.; Kite, E. S.; Michaels, T. I.

    2018-01-01

    Most of Mars' ancient sedimentary rocks by volume are in wind-eroded sedimentary mounds within impact craters and canyons, but the connections between mound form and wind erosion are unclear. We perform mesoscale simulations of different crater and mound morphologies to understand the formation of sedimentary mounds. As crater depth increases, slope winds produce increased erosion near the base of the crater wall, forming mounds. Peak erosion rates occur when the crater depth is ˜2 km. Mound evolution depends on the size of the host crater. In smaller craters mounds preferentially erode at the top, becoming more squat, while in larger craters mounds become steeper sided. This agrees with observations where smaller craters tend to have proportionally shorter mounds and larger craters have mounds encircled by moats. If a large-scale sedimentary layer blankets a crater, then as the layer recedes across the crater it will erode more toward the edges of the crater, resulting in a crescent-shaped moat. When a 160 km diameter mound-hosting crater is subject to a prevailing wind, the surface wind stress is stronger on the leeward side than on the windward side. This results in the center of the mound appearing to "march upwind" over time and forming a "bat-wing" shape, as is observed for Mount Sharp in Gale crater.

  2. Nuclear cratering on a digital computer

    International Nuclear Information System (INIS)

    Terhune, R.W.; Stubbs, T.F.; Cherry, J.T.

    1970-01-01

    Computer programs based on the artificial viscosity method are applied to developing an understanding of the physics of cratering, with emphasis on cratering by nuclear explosives. Two established codes, SOC (spherical symmetry) and TENSOR (cylindrical symmetry), are used to illustrate the effects of variations in the material properties of various media on the cratering processes, namely shock, spall, and gas acceleration. Water content is found to be the most important material property, followed by strength, porosity, and compressibility. Crater profile calculations are presented for Pre-Gondola Charley (20-ton nitromethane detonation in shale) and Sedan (100-kt nuclear detonation in alluvium). Calculations also are presented for three 1-Mt yields in saturated Divide basalt and 1-Mt yield in dry Buckboard basalt, to show crater geometry as a function of the burial depth for large explosive yields. The calculations show, for megaton-level yields, that gas acceleration is the dominate mechanism in determining crater size and depends in turn on the water content in the medium. (author)

  3. Gamma radiation use on the aging of sugar cane spirit

    International Nuclear Information System (INIS)

    Walder, Julio M. M.; Spoto, Marta H. F.; Novaes, Fernando V.; Alcarde, Andre R.

    2002-01-01

    The objective of this work was to verify the influence of gamma radiation on the aging of sugarcane spirit. Samples of sugarcane spirit (cachaca ) were irradiated in a Gammabeam Cobalt-60 source with doses between 0 (control) and 300 Gy, with 50 Gy increasing. The irradiated samples were offered to 5 expert judges for sensorial tests using the comparison: irradiated versus control. The chemical volatile components of the irradiated spirit were determined using a gas chromatograph. Sensorial tests elected the dose of 150 Gy as the best for sugarcane spirit irradiation based on its flavour and bouquet. These sensorial characteristics were due to the chemical changes observed in esters, aldehydes and higher alcohol's concentrations. The samples irradiated with 250 and 300 Gy developed a bitter taste and an 'oxidized' flavour. A second experiment was carried out using single and twice-distilled sugarcane spirit, normal aged in oak barrels or not, or added with oak extract. Samples were irradiated with the dose of 150 Gy and scored by the same sensorial analysis methodology. All irradiated samples had their flavour improved. The irradiation of the non-maturated twice-distilled sugarcane spirit produced a flavour compared to spirits maturated during one year of normal aging. (author)

  4. WATER ON MARS: EVIDENCE FROM MER MISSION RESULTS

    Science.gov (United States)

    Landis, Geoffrey A.

    2006-01-01

    The Mars Exploration Rover (MER) mission landed two rovers on Mars, equipped with a highly-capable suite of science instruments. The Spirit rover landed on the inside Gusev Crater on January 5, 2004, and the Opportunity rover three weeks later on Meridiani Planum. This paper summarizes some of the findings from the MER rovers related to the NASA science strategy of investigating past and present water on Mars.

  5. Sand Dunes in Kaiser Crater

    Science.gov (United States)

    2002-01-01

    Full size (780 KBytes) This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) high resolution image shows a field of dark sand dunes on the floor of Kaiser Crater in southeastern Noachis Terra. The steepest slopes on each dune, the slip faces, point toward the east, indicating that the strongest winds that blow across the floor of Kaiser move sand in this direction. Wind features of three different scales are visible in this image: the largest (the dunes) are moving across a hard surface (light tone) that is itself partially covered by large ripples. These large ripples appear not to be moving--the dunes are burying some and revealing others. Another type of ripple pattern is seen on the margins of the dunes and where dunes coalesce. They are smaller (both in their height and in their separation) than the large ripples. These are probably coarse sediments that are moving with the dunes. This picture covers an area approximately 3 km (1.9 mi) across and is illuminated from the upper left.

  6. Spirit's Surroundings on 'West Spur,' Sol 305 (Vertical)

    Science.gov (United States)

    2005-01-01

    This 360-degree panorama shows the terrain surrounding NASA's Mars Exploration Rover Spirit as of the rover's 305th martian day, or sol, (Nov. 11, 2004). At that point, Spirit was climbing the 'West Spur' of the 'Columbia Hills.' The rover had just finished inspecting a rock called 'Lutefisk' and was heading uphill toward an area called 'Machu Picchu.' Spirit used its navigational camera to take the images combined into this mosaic. The rover's location when the images were taken is catalogued as the mission's site 89, position 205. The view is presented here as a vetical projection with geometric seam correction.

  7. Spirit's Surroundings on 'West Spur,' Sol 305 (Polar)

    Science.gov (United States)

    2005-01-01

    This 360-degree panorama shows the terrain surrounding NASA's Mars Exploration Rover Spirit as of the rover's 305th martian day, or sol, (Nov. 11, 2004). At that point, Spirit was climbing the 'West Spur' of the 'Columbia Hills.' The rover had just finished inspecting a rock called 'Lutefisk' and was heading uphill toward an area called 'Machu Picchu.' Spirit used its navigational camera to take the images combined into this mosaic. The rover's location when the images were taken is catalogued as the mission's site 89, position 205. The view is presented here as a polar projection with geometric seam correction.

  8. Health improvement of domestic hot tap water supply Gusev, Kaliningrad Region, Russia. Make-up water tank project. Final report

    Energy Technology Data Exchange (ETDEWEB)

    Aagaard, Joergen

    1998-07-01

    This report describes the project `Health Improvement of Domestic Hot Tap Water Supply, Gusev, Kaliningrad, Russia`, which was carried out in the autumn of 1996 and financed by the Danish Environmental Protection Agency, the Danish Energy Agency and Gusev Municipality. The project proposal and application outlined the following objectives: Erection of system so that hot tap water, which is tapped directly from the district heating system, obtains an acceptable quality in health terms; Complete training and education, so that the plant can be operated and maintained by the power station`s staff and rehabilitation projects within supply of domestic water and district heating can be promoted to the greatest possible extent; Systems for heat treatment of make-up water were implemented in less than three months; The project was carried out in close Danish-Russian co-operation from the beginning of engineering to the commissioning and resulted in transfer and demonstration of know-how and technology; Information was recorded on the existing domestic water and heat supply systems as well as on the treatment of sewage, and recommendations for rehabilitation projects were made. Previously, when the temperature in the district heating system was relatively high, a heat treatment apparently took place in the district heating system. However, due to the current poor economic situation there are no means with which to buy the fuel quantities necessary to maintain the previously normal district heating temperature. In the new concept the cold make-up water is heated to >80 deg. C as required by the health authorities before it is led to the district heating return system and subsequently heated to the actual supply temperature of 50-60 deg. C. The energy consumption in the two concepts is approximately the same. A 1,000 m{sup 3} tank with heating coils was erected between the make-up water system and the district heating system. The tank should equalise the daily capacity

  9. Pancam Peek into 'Victoria Crater' (Stereo)

    Science.gov (United States)

    2006-01-01

    [figure removed for brevity, see original site] Left-eye view of a stereo pair for PIA08776 [figure removed for brevity, see original site] Right-eye view of a stereo pair for PIA08776 A drive of about 60 meters (about 200 feet) on the 943rd Martian day, or sol, of Opportunity's exploration of Mars' Meridiani Planum region (Sept. 18, 2006) brought the NASA rover to within about 50 meters (about 160 feet) of the rim of 'Victoria Crater.' This crater has been the mission's long-term destination for the past 21 Earth months. Opportunity reached a location from which the cameras on top of the rover's mast could begin to see into the interior of Victoria. This stereo anaglyph was made from frames taken on sol 943 by the panoramic camera (Pancam) to offer a three-dimensional view when seen through red-blue glasses. It shows the upper portion of interior crater walls facing toward Opportunity from up to about 850 meters (half a mile) away. The amount of vertical relief visible at the top of the interior walls from this angle is about 15 meters (about 50 feet). The exposures were taken through a Pancam filter selecting wavelengths centered on 750 nanometers. Victoria Crater is about five times wider than 'Endurance Crater,' which Opportunity spent six months examining in 2004, and about 40 times wider than 'Eagle Crater,' where Opportunity first landed. The great lure of Victoria is the expectation that a thick stack of geological layers will be exposed in the crater walls, potentially several times the thickness that was previously studied at Endurance and therefore, potentially preserving several times the historical record.

  10. 27 CFR 19.372 - Receipt of spirits, wines and alcoholic flavoring materials for processing.

    Science.gov (United States)

    2010-04-01

    ... which received until used. Spirits and wines received by pipeline shall be deposited in tanks, gauged by... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Receipt of spirits, wines... Spirits, Wines and Alcoholic Flavoring Materials § 19.372 Receipt of spirits, wines and alcoholic...

  11. 27 CFR 19.342 - Receipt and storage of bulk spirits and wines.

    Science.gov (United States)

    2010-04-01

    ... Receipt and storage of bulk spirits and wines. (a) Deposit. All spirits entered for deposit in the storage... spirits or wines are being deposited in a partially filled tank in storage on bonded premises... bulk spirits and wines. 19.342 Section 19.342 Alcohol, Tobacco Products and Firearms ALCOHOL AND...

  12. 27 CFR 30.51 - Procedures for measurement of bulk spirits.

    Science.gov (United States)

    2010-04-01

    ... the standard temperature by means of table 7. In the case of denatured spirits, the temperature..., should be that given in table 7 for 100 proof spirits. When the quantity of spirits, in wine gallons, has... the wine gallons by the proof of the spirits as determined under § 30.31. Example. Gauge glass reading...

  13. 27 CFR 27.75 - Samples of distilled spirits, wine, and beer for quality control purposes.

    Science.gov (United States)

    2010-04-01

    ... DISTILLED SPIRITS, WINES, AND BEER General Requirements Exemptions § 27.75 Samples of distilled spirits, wine, and beer for quality control purposes. Samples of distilled spirits, wine, and beer in containers... spirits, wine, and beer for quality control purposes. 27.75 Section 27.75 Alcohol, Tobacco Products and...

  14. 27 CFR 28.26 - Entry of distilled spirits into customs bonded warehouses.

    Science.gov (United States)

    2010-04-01

    ... eligible for export with benefit of drawback. Bottled distilled spirits eligible for export with benefit of... bonded warehouse from which distilled spirits may be exported. These withdrawals shall be treated as... spirits were for exportation. (c) Time deemed exported. For the purpose of this part, distilled spirits...

  15. SPIRIT 2013 Statement: defining standard protocol items for clinical trials

    Directory of Open Access Journals (Sweden)

    An-Wen Chan

    Full Text Available The protocol of a clinical trial serves as the foundation for study planning, conduct, reporting, and appraisal. However, trial protocols and existing protocol guidelines vary greatly in content and quality. This article describes the systematic development and scope of SPIRIT (Standard Protocol Items: Recommendations for Interventional Trials 2013, a guideline for the minimum content of a clinical trial protocol. The 33-item SPIRIT checklist applies to protocols for all clinical trials and focuses on content rather than format. The checklist recommends a full description of what is planned; it does not prescribe how to design or conduct a trial. By providing guidance for key content, the SPIRIT recommendations aim to facilitate the drafting of high-quality protocols. Adherence to SPIRIT would also enhance the transparency and completeness of trial protocols for the benefit of investigators, trial participants, patients, sponsors, funders, research ethics committees or institutional review boards, peer reviewers, journals, trial registries, policymakers, regulators, and other key stakeholders.

  16. African Gifts of the Spirit: Pentecostalism & the Rise of a ...

    African Journals Online (AJOL)

    African Gifts of the Spirit: Pentecostalism & the Rise of a Zimbabwean Transnational Religious Movement by David Maxwell (Ohio: Ohio University Press, 2006) – XI + 250 pp., ISBN 13:978-0-8124-1738-6, Paperback.

  17. SPIRITS: Uncovering Unusual Infrared Transients with Spitzer

    Energy Technology Data Exchange (ETDEWEB)

    Kasliwal, Mansi M.; Jencson, Jacob E.; Tinyanont, Samaporn; Cao, Yi; Cook, David [Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125 (United States); Bally, John [Center for Astrophysics and Space Astronomy, University of Colorado, 389 UCB, Boulder, CO 80309 (United States); Masci, Frank; Armus, Lee [Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125 (United States); Cody, Ann Marie [NASA Ames Research Center, Moffett Field, CA 94035 (United States); Bond, Howard E. [Dept. of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States); Contreras, Carlos [Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena (Chile); Dykhoff, Devin A.; Amodeo, Samuel; Carlon, Robert L.; Cass, Alexander C.; Corgan, David T.; Faella, Joseph [Minnesota Institute for Astrophysics, School of Physics and Astronomy, 116 Church Street, S. E., University of Minnesota, Minneapolis, MN 55455 (United States); Boyer, Martha [NASA Goddard Space Flight Center, MC 665, 8800 Greenbelt Road, Greenbelt, MD 20771 (United States); Cantiello, Matteo [Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010 (United States); Fox, Ori D. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); and others

    2017-04-20

    We present an ongoing, five-year systematic search for extragalactic infrared transients, dubbed SPIRITS—SPitzer InfraRed Intensive Transients Survey. In the first year, using Spitzer /IRAC, we searched 190 nearby galaxies with cadence baselines of one month and six months. We discovered over 1958 variables and 43 transients. Here, we describe the survey design and highlight 14 unusual infrared transients with no optical counterparts to deep limits, which we refer to as SPRITEs (eSPecially Red Intermediate-luminosity Transient Events). SPRITEs are in the infrared luminosity gap between novae and supernovae, with [4.5] absolute magnitudes between −11 and −14 (Vega-mag) and [3.6]–[4.5] colors between 0.3 mag and 1.6 mag. The photometric evolution of SPRITEs is diverse, ranging from <0.1 mag yr{sup −1} to >7 mag yr{sup −1}. SPRITEs occur in star-forming galaxies. We present an in-depth study of one of them, SPIRITS 14ajc in Messier 83, which shows shock-excited molecular hydrogen emission. This shock may have been triggered by the dynamic decay of a non-hierarchical system of massive stars that led to either the formation of a binary or a protostellar merger.

  18. Design and construction of the spirit TPC

    Science.gov (United States)

    Tangwancharoen, Suwat

    The nuclear symmetry energy, the density dependent term of the nuclear equation of state (EOS), governs important properties of neutron stars and dense nuclear matter. At present, it is largely unconstrained in the supra-saturation density region. This dissertation concerns the design and construction of the SpiRIT Time Projection Chamber (SpiRIT-TPC) at Michigan State University as part of an international collaborations to constrain the symmetry energy at supra-saturation density. The SpiRIT-TPC has been constructed during the dissertation and transported to Radioactive Isotope Beam Factory (RIBF) at RIKEN, Japan where it will be used in conjunction with the SAMURAI Spectrometer. The detector will measure yield ratios for pions and other light charged particles produced in central collisions of neutron-rich heavy ions such as 132Sn + 124Sn. The dissertation describes the design and solutions to the problem presented by the measurement. This also compares some of the initial fast measurement of the TPC to calculation of the performance characteristics.

  19. Cratering Equations for Zinc Orthotitanate Coated Aluminum

    Science.gov (United States)

    Hyde, James; Christiansen, Eric; Liou, Jer-Chyi; Ryan, Shannon

    2009-01-01

    The final STS-125 servicing mission (SM4) to the Hubble Space Telescope (HST) in May of 2009 saw the return of the 2nd Wide Field Planetary Camera (WFPC2) aboard the shuttle Discovery. This hardware had been in service on HST since it was installed during the SM1 mission in December of 1993 yielding one of the longest low Earth orbit exposure times (15.4 years) of any returned space hardware. The WFPC2 is equipped with a 0.8 x 2.2 m radiator for thermal control of the camera electronics (Figure 1). The space facing surface of the 4.1 mm thick aluminum radiator is coated with Z93 zinc orthotitanate thermal control paint with a nominal thickness of 0.1 0.2 mm. Post flight inspections of the radiator panel revealed hundreds of micrometeoroid/orbital debris (MMOD) impact craters ranging in size from less than 300 to nearly 1000 microns in diameter. The Z93 paint exhibited large spall areas around the larger impact sites (Figure 2) and the craters observed in the 6061-T651 aluminum had a different shape than those observed in uncoated aluminum. Typical hypervelocity impact craters in aluminum have raised lips around the impact site. The craters in the HST radiator panel had suppressed crater lips, and in some cases multiple craters were present instead of a single individual crater. Humes and Kinard observed similar behavior after the WFPC1 post flight inspection and assumed the Z93 coating was acting like a bumper in a Whipple shield. Similar paint behavior (spall) was also observed by Bland2 during post flight inspection of the International Space Station (ISS) S-Band Antenna Structural Assembly (SASA) in 2008. The SASA, with similar Z93 coated aluminum, was inspected after nearly 4 years of exposure on the ISS. The multi-crater phenomena could be a function of the density, composition, or impact obliquity angle of the impacting particle. For instance, a micrometeoroid particle consisting of loosely bound grains of material could be responsible for creating the

  20. The Crater Ejecta Distribution on Ceres

    Science.gov (United States)

    Schmedemann, Nico; Neesemann, Adrian; Schulzeck, Franziska; Krohn, Katrin; Gathen, Isabel; Otto, Katharina; Jaumann, Ralf; Michael, Gregory; Raymond, Carol; Russell, Christopher

    2017-04-01

    Since March 6 2015 the Dawn spacecraft [1] has been in orbit around the dwarf planet Ceres. At small crater diameters Ceres appears to be peppered with secondary craters that often align in chains or form clusters. Some of such possible crater chains follow curved geometries and are not in a radial orientation with respect to possible source craters [2]. Ceres is a fast rotating body ( 9 h per revolution) with comparatively low surface gravity ( 0.27 m/s2). A substantial fraction of impact ejecta may be launched with velocities similar to Ceres' escape velocity (510 m/s), which implies that many ejected particles follow high and long trajectories. Thus, due to Ceres' fast rotation the distribution pattern of the reimpacting ejected material is heavily affected by Coriolis forces that results in a highly asymmetrical and curved pattern of secondary crater chains. In order to simulate flight trajectories and distribution of impact ejected material for individual craters on Ceres we used the scaling laws by [3] adjusted to the Cerean impact conditions [4] and the impact ejecta model by [5]. These models provide the starting conditions for tracer particles in the simulation. The trajectories of the particles are computed as n-body simulation. The simulation calculates the positions and impact velocities of each impacting tracer particle with respect to the rotating surface of Ceres, which is approximated by a two-axis ellipsoid. Initial results show a number of interesting features in the simulated deposition geometries of specific crater ejecta. These features are roughly in agreement with features that can be observed in Dawn imaging data of the Cerean surface. For example: ray systems of fresh impact craters, non-radial crater chains and global scale border lines of higher and lower color ratio areas. Acknowledgment: This work has been supported by the German Space Agency (DLR) on behalf of the Federal Ministry for Economic Affairs and Energy, Germany, grants 50 OW

  1. TESLA'S INVENTIONS IN PHYSICS AND HIS ENGINEERING SPIRIT

    OpenAIRE

    Petković, T.

    2006-01-01

    The article describes Tesla’s inventions in physics. Tesla’s engineering spirit is compared to M. Faraday’s and A. A. Michelson’s spirit of discovery in electromagnetism. Tesla’s unfinished investigative journey, from great experiments in electrical technology and radio technology to the physical theories he derived from them, are examined historically and scientifically. Several discoveries and individual experiments are described that were significant in the subsequent development of accele...

  2. Spirit-guided care: Christian nursing for the whole person.

    Science.gov (United States)

    Murphy, Lyn S; Walker, Mark S

    2013-01-01

    Healthcare today is challenged to provide care that goes beyond the medical model of meeting physical needs. Despite a strong historical foundation in spiritual whole person care, nurses struggle with holistic caring. We propose that for the Christian nurse, holistic nursing can be described as Spirit-guided care--removing oneself as the moiatiating force and allowing Christ, in the furm of the Holy Spirit, to flow through and guide the nurse in care of patients and families.

  3. Two-dimensional computer simulation of hypervelocity impact cratering: some preliminary results for Meteor Crater, Arizona

    Energy Technology Data Exchange (ETDEWEB)

    Bryan, J.B.; Burton, D.E.; Cunningham, M.E.; Lettis, L.A. Jr.

    1978-04-01

    A computational approach used for subsurface explosion cratering has been extended to hypervelocity impact cratering. Meteor (Barringer) Crater, Arizona, was selected for our first computer simulation because it was the most thoroughly studied. It is also an excellent example of a simple, bowl-shaped crater and is one of the youngest terrestrial impact craters. Shoemaker estimates that the impact occurred about 20,000 to 30,000 years ago (Roddy (1977)). Initial conditions for this calculation included a meteorite impact velocity of 15 km/s. meteorite mass of 1.57E + 08 kg, with a corresponding kinetic energy of 1.88E + 16 J (4.5 megatons). A two-dimensional Eulerian finite difference code called SOIL was used for this simulation of a cylindrical iron projectile impacting at normal incidence into a limestone target. For this initial calculation a Tillotson equation-of-state description for iron and limestone was used with no shear strength. A color movie based on this calculation was produced using computer-generated graphics. Results obtained for this preliminary calculation of the formation of Meteor Crater, Arizona, are in good agreement with Meteor Crater Measurements.

  4. Two-dimensional computer simulation of hypervelocity impact cratering: some preliminary results for Meteor Crater, Arizona

    International Nuclear Information System (INIS)

    Bryan, J.B.; Burton, D.E.; Cunningham, M.E.; Lettis, L.A. Jr.

    1978-04-01

    A computational approach used for subsurface explosion cratering has been extended to hypervelocity impact cratering. Meteor (Barringer) Crater, Arizona, was selected for our first computer simulation because it was the most thoroughly studied. It is also an excellent example of a simple, bowl-shaped crater and is one of the youngest terrestrial impact craters. Shoemaker estimates that the impact occurred about 20,000 to 30,000 years ago [Roddy (1977)]. Initial conditions for this calculation included a meteorite impact velocity of 15 km/s. meteorite mass of 1.57E + 08 kg, with a corresponding kinetic energy of 1.88E + 16 J (4.5 megatons). A two-dimensional Eulerian finite difference code called SOIL was used for this simulation of a cylindrical iron projectile impacting at normal incidence into a limestone target. For this initial calculation a Tillotson equation-of-state description for iron and limestone was used with no shear strength. A color movie based on this calculation was produced using computer-generated graphics. Results obtained for this preliminary calculation of the formation of Meteor Crater, Arizona, are in good agreement with Meteor Crater Measurements

  5. Two-dimensional computer simulation of hypervelocity impact cratering: some preliminary results for Meteor Crater, Arizona

    Energy Technology Data Exchange (ETDEWEB)

    Bryan, J.B.; Burton, D.E.; Cunningham, M.E.; Lettis, L.A. Jr.

    1978-06-01

    A computational approach used for subsurface explosion cratering was extended to hypervelocity impact cratering. Meteor (Barringer) Crater, Arizona, was selected for the first computer simulation because it is one of the most thoroughly studied craters. It is also an excellent example of a simple, bowl-shaped crater and is one of the youngest terrestrial impact craters. Initial conditions for this calculation included a meteorite impact velocity of 15 km/s, meteorite mass of 1.67 x 10/sup 8/ kg, with a corresponding kinetic energy of 1.88 x 10/sup 16/ J (4.5 megatons). A two-dimensional Eulerian finite difference code called SOIL was used for this simulation of a cylindrical iron projectile impacting at normal incidence into a limestone target. For this initial calculation, a Tillotson equation-of-state description for iron and limestone was used with no shear strength. Results obtained for this preliminary calculation of the formation of Meteor Crater are in good agreement with field measurements. A color movie based on this calculation was produced using computer-generated graphics. 19 figures, 5 tables, 63 references.

  6. Two-dimensional computer simulation of hypervelocity impact cratering: some preliminary results for Meteor Crater, Arizona

    International Nuclear Information System (INIS)

    Bryan, J.B.; Burton, D.E.; Cunningham, M.E.; Lettis, L.A. Jr.

    1978-06-01

    A computational approach used for subsurface explosion cratering was extended to hypervelocity impact cratering. Meteor (Barringer) Crater, Arizona, was selected for the first computer simulation because it is one of the most thoroughly studied craters. It is also an excellent example of a simple, bowl-shaped crater and is one of the youngest terrestrial impact craters. Initial conditions for this calculation included a meteorite impact velocity of 15 km/s, meteorite mass of 1.67 x 10 8 kg, with a corresponding kinetic energy of 1.88 x 10 16 J (4.5 megatons). A two-dimensional Eulerian finite difference code called SOIL was used for this simulation of a cylindrical iron projectile impacting at normal incidence into a limestone target. For this initial calculation, a Tillotson equation-of-state description for iron and limestone was used with no shear strength. Results obtained for this preliminary calculation of the formation of Meteor Crater are in good agreement with field measurements. A color movie based on this calculation was produced using computer-generated graphics. 19 figures, 5 tables, 63 references

  7. Experimental investigation of crater growth dynamics

    Science.gov (United States)

    Schmidt, R. M.; Housen, K. R.; Bjorkman, M. D.; Holsapple, K. A.

    1985-01-01

    This work is a continuation of an ongoing program whose objective is to perform experiments and to develop scaling relationships for large-body impacts onto planetary surfaces. The centrifuge technique is used to provide experimental data for actual target materials of interest. With both power and gas guns mounted on the rotor arm, it is possible to match various dimensionless similarity parameters, which have been shown to govern the behavior of large-scale impacts. The development of the centrifuge technique has been poineered by the present investigators and is documented by numerous publications, the most recent of which are listed below. Understanding the dependence of crater size upon gravity has been shown to be key to the complete determination of the dynamic and kinematic behavior of crater formation as well as ejecta phenomena. Three unique time regimes in the formation of an impact crater have been identified.

  8. Crater monitoring through social media observations

    Science.gov (United States)

    Gialampoukidis, I.; Vrochidis, S.; Kompatsiaris, I.

    2017-09-01

    We have collected more than one lunar image per two days from social media observations. Each one of the collected images has been clustered into two main groups of lunar images and an additional cluster is provided (noise) with pictures that have not been assigned to any cluster. The proposed lunar image clustering process provides two classes of lunar pictures, at different zoom levels; the first showing a clear view of craters grouped into one cluster and the second demonstrating a complete view of the Moon at various phases that are correlated with the crawling date. The clustering stage is unsupervised, so new topics can be detected on-the-fly. We have provided additional sources of planetary images using crowdsourcing information, which is associated with metadata such as time, text, location, links to other users and other related posts. This content has crater information that can be fused with other planetary data to enhance crater monitoring.

  9. Physics of soft impact and cratering

    CERN Document Server

    Katsuragi, Hiroaki

    2016-01-01

    This book focuses on the impact dynamics and cratering of soft matter to describe its importance, difficulty, and wide applicability to planetary-related problems. A comprehensive introduction to the dimensional analysis and constitutive laws that are necessary to discuss impact mechanics and cratering is first provided. Then, particular coverage is given to the impact of granular matter, which is one of the most crucial constituents for geophysics. While granular matter shows both solid-like and fluid-like behaviors, neither solid nor fluid dynamics is sufficient to fully understand the physics of granular matter. In order to reveal its fundamental properties, extensive impact tests have been carried out recently. The author reveals the findings of these recent studies as well as what remains unsolved in terms of impact dynamics. Impact crater morphology with various soft matter impacts also is discussed intensively. Various experimental and observational results up to the recent Itokawa asteroid’s terrain...

  10. Titan's Impact Cratering Record: Erosion of Ganymedean (and other) Craters on a Wet Icy Landscape

    Science.gov (United States)

    Schenk, P.; Moore, J.; Howard, A.

    2012-04-01

    We examine the cratering record of Titan from the perspective of icy satellites undergoing persistent landscape erosion. First we evaluate whether Ganymede (and Callisto) or the smaller low-gravity neighboring icy satellites of Saturn are the proper reference standard for evaluating Titan’s impact crater morphologies, using topographic and morphometric measurements (Schenk, 2002; Schenk et al. (2004) and unpublished data). The special case of Titan’s largest crater, Minrva, is addressed through analysis of large impact basins such as Gilgamesh, Lofn, Odysseus and Turgis. Second, we employ a sophisticated landscape evolution and modification model developed for study of martian and other planetary landforms (e.g., Howard, 2007). This technique applies mass redistribution principles due to erosion by impact, fluvial and hydrological processes to a planetary landscape. The primary advantage of our technique is the possession of a limited but crucial body of areal digital elevation models (DEMs) of Ganymede (and Callisto) impact craters as well as global DEM mapping of Saturn’s midsize icy satellites, in combination with the ability to simulate rainfall and redeposition of granular material to determine whether Ganymede craters can be eroded to resemble Titan craters and the degree of erosion required. References: Howard, A. D., “Simulating the development of martian highland landscapes through the interaction of impact cratering, fluvial erosion, and variable hydrologic forcing”, Geomorphology, 91, 332-363, 2007. Schenk, P. "Thickness constraints on the icy shells of the galilean satellites from impact crater shapes". Nature, 417, 419-421, 2002. Schenk, P.M., et al. "Ages and interiors: the cratering record of the Galilean satellites". In: Jupiter: The Planet, Satellites, and Magnetosphere, Cambridge University Press, Cambridge, UK, pp. 427-456, 2004.

  11. Comparison of Patterns of Use of Unrecorded and Recorded Spirits: Survey of Adult Drinkers in Rural Central China

    OpenAIRE

    Shiqing Wei; Ping Yin; Ian M. Newman; Ling Qian; Duane F. Shell; Lok-wa Yuen

    2017-01-01

    About 70% of the beverage alcohol consumed in China annually is spirits. Recorded spirits make up most spirit consumption, but about 25% of total alcohol consumption (1.7 L pure alcohol per capita annually) is unrecorded spirits (bai jiu), either homemade or made in unregulated distilleries. In some parts of China, the consumption of unrecorded spirits is higher than average. This paper compares the patterns of use of unrecorded distilled spirits and recorded distilled spirits among rural res...

  12. Embodiment of the Spirit: A Case Study

    Directory of Open Access Journals (Sweden)

    Jan Grimell

    2017-02-01

    Full Text Available Adopting a longitudinal approach to exploring the psychology of the transition from military to civilian life, one case study is presented that adds a spiritual perspective to the transition process. This case study serves as an example representative from a group of participants who have been followed through a research project on identity reconstruction during the transition to civilian life. This individual, not unlike many others within the group, undergoes an unexpected progression of the military I-position of the self throughout the process of becoming a civilian. This study utilizes a dialogical approach to the identity work to further the understanding of longitudinal adjustments to the self. An analysis of the narrative developments and interactions among pre-existing and new I-positions of the self over time has been made based upon three annually conducted interviews spanning from 2014 to 2016. The results lead to the suggestion that if a military I-position of the self grows more salient and voiced throughout the process of transitioning into civilian life, then this vocalization may be related to the spirit of a person embodied in a specific I-position of the self. Such growth of a military I-position after leaving active service may gravitate around a deep sense of “who I am” with a profound sense of meaning attached to this position. Instead of perceiving as an unwanted development the growth of a military sense of “who I am,” one should acknowledge it as a deeper dimension of self and life. It is important to find an outlet for such a progression of the self so as to sustain balance and dialogue. Future research is encouraged to further examine these qualitative findings.

  13. 'Sharks Teeth' -- Sand Dunes in Proctor Crater

    Science.gov (United States)

    2001-01-01

    Sometimes, pictures received from Mars Global Surveyor's Mars Orbiter Camera (MOC) are 'just plain pretty.' This image, taken in early September 2000, shows a group of sand dunes at the edge of a much larger field of dark-toned dunes in Proctor Crater. Located at 47.9oS, 330.4oW, in the 170 km (106 mile) diameter crater named for 19th Century British astronomer Richard A. Proctor (1837-1888), the dunes shown here are created by winds blowing largely from the east/northeast. A plethora of smaller, brighter ripples covers the substrate between the dunes. Sunlight illuminates them from the upper left.

  14. North Rim of Endeavour Crater on Horizon

    Science.gov (United States)

    2009-01-01

    [figure removed for brevity, see original site] A northern portion of the rim of Endeavour Crater is visible on the horizon of this image taken by the panoramic camera (Pancam) on NASA's Mars Exploration Rover Opportunity on March 7, 2009, during the 1,820st Martian day, or sol, of the rover's mission on Mars. That portion of Endeavour's rim is about 20 kilometers (12 miles) away from Opportunity's position west of the crater when the image was taken. The width of the image covers approximately one degree of the horizon.

  15. East Rim of Endeavour Crater on Horizon

    Science.gov (United States)

    2009-01-01

    [figure removed for brevity, see original site] A high point on the distant eastern rim of Endeavour Crater is visible on the horizon in this image taken by the panoramic camera (Pancam) on NASA's Mars Exploration Rover Opportunity on March 8, 2009, during the 1,821st Martian day, or sol, of the rover's mission on Mars. That portion of Endeavour's rim is about 34 kilometers (21 miles) away from Opportunity's position west of the crater when the image was taken. The width of the image covers approximately one degree of the horizon.

  16. View of the crater on lunar farside from Apollo 13

    Science.gov (United States)

    1970-01-01

    This bright-rayed crater on the lunar farside was photographed from the Apollo 13 spacecraft during its pass around the Moon. This area is northeast of Mare Marginus. The bright-rayed crater is located at about 105 degrees east longitude and 45 degrees north latitude. The crater Joliot-Curie is located between Mare Marginus and the rayed crater. This view is looking generally toward the northeast.

  17. Crater ejecta scaling laws: fundamental forms based on dimensional analysis

    International Nuclear Information System (INIS)

    Housen, K.R.; Schmidt, R.M.; Holsapple, K.A.

    1983-01-01

    A model of crater ejecta is constructed using dimensional analysis and a recently developed theory of energy and momentum coupling in cratering events. General relations are derived that provide a rationale for scaling laboratory measurements of ejecta to larger events. Specific expressions are presented for ejection velocities and ejecta blanket profiles in two limiting regimes of crater formation: the so-called gravity and strength regimes. In the gravity regime, ejectra velocities at geometrically similar launch points within craters vary as the square root of the product of crater radius and gravity. This relation implies geometric similarity of ejecta blankets. That is, the thickness of an ejecta blanket as a function of distance from the crater center is the same for all sizes of craters if the thickness and range are expressed in terms of crater radii. In the strength regime, ejecta velocities are independent of crater size. Consequently, ejecta blankets are not geometrically similar in this regime. For points away from the crater rim the expressions for ejecta velocities and thickness take the form of power laws. The exponents in these power laws are functions of an exponent, α, that appears in crater radius scaling relations. Thus experimental studies of the dependence of crater radius on impact conditions determine scaling relations for ejecta. Predicted ejection velocities and ejecta-blanket profiles, based on measured values of α, are compared to existing measurements of velocities and debris profiles

  18. Impact and cratering rates onto Pluto

    Science.gov (United States)

    Greenstreet, Sarah; Gladman, Brett; McKinnon, William B.

    2015-09-01

    The New Horizons spacecraft fly-through of the Pluto system in July 2015 will provide humanity's first data for the crater populations on Pluto and its binary companion, Charon. In principle, these surfaces could be dated in an absolute sense, using the observed surface crater density (# craters/km2 larger than some threshold crater diameter D). Success, however, requires an understanding of both the cratering physics and absolute impactor flux. The Canada-France Ecliptic Plane Survey (CFEPS) L7 synthetic model of classical and resonant Kuiper belt populations (Petit, J.M. et al. [2011]. Astron. J. 142, 131-155; Gladman, B. et al. [2012]. Astron. J. 144, 23-47) and the scattering object model of Kaib et al. (Kaib, N., Roškar, R., Quinn, T. [2011]. Icarus 215, 491-507) calibrated by Shankman et al. (Shankman, C. et al. [2013]. Astrophys. J. 764, L2-L5) provide such impact fluxes and thus current primary cratering rates for each dynamical sub-population. We find that four sub-populations (the q impact flux, each providing ≈ 15- 25 % of the total rate. Due to the uncertainty in how the well-characterized size distribution for Kuiper belt objects (with impactor diameter d > 100km) connects to smaller projectiles, we compute cratering rates using five model impactor size distributions: a single power-law, a power-law with a knee, a power-law with a divot, as well as the "wavy" size distributions described in Minton et al. (Minton, D.A. et al. [2012]. Asteroids Comets Meteors Conf. 1667, 6348) and Schlichting et al. (Schlichting, H.E., Fuentes, C.I., Trilling, D.E. [2013]. Astron. J. 146, 36-42). We find that there is only a small chance that Pluto has been hit in the past 4 Gyr by even one impactor with a diameter larger than the known break in the projectile size distribution (d ≈ 100km) which would create a basin on Pluto (D ⩾ 400km in diameter). We show that due to present uncertainties in the impactor size distribution between d = 1- 100km , computing

  19. Cratering on Small Bodies: Lessons from Eros

    Science.gov (United States)

    Chapman, C. R.

    2003-01-01

    Cratering and regolith processes on small bodies happen continuously as interplanetary debris rains down on asteroids, comets, and planetary satellites. Butthey are very poorly observed and not well understood. On the one hand, we have laboratory experimentation at small scales and we have examination of large impact craters (e.g. Meteor Crater on Earth and imaging of abundant craters on terrestrial planets and outer planet moons). Understanding cratering on bodies of intermediate scales, tens of meters to hundreds of km in size, involves either extrapolation from our understanding of cratering phenomena at very different scales or reliance on very preliminary, incomplete examination of the observational data we now have for a few small bodies. I review the latter information here. It has been generally understood that the role of gravity is greatly diminished for smaller bodies, so a lot of cratering phenomena studied for larger bodies is less applicable. But it would be a mistake to imagine that laboratory experiments on gravitationless rocks (usually at 1 g) are directly applicable, except perhaps to those monolithic Near Earth Asteroids (NEAs) some tens of meters in size that spin very rapidly and can be assumed to be "large bare rocks" with "negative gravity". Whereas it had once been assumed that asteroids smaller than some tens of km diameter would retain little regolith, it is increasingly apparent that regolith and megoregolith processes extend down to bodies only hundreds of meters in size, perhaps smaller. Yet these processes are very different from those that pertain to the Moon, which is our chief prototype of regolith processes. The NEAR Shoemaker spacecraft's studies of Eros provide the best evidence to date about small-body cratering processes, as well as a warning that our theoretical understanding requires anchoring by direct observations. Eros: "Ponds", Paucity of Small Craters, and Other Mysteries. Although Eros is currently largely detached

  20. Using THEMIS thermal infrared observations of rays from Corinto crater to study secondary crater formation on Mars

    Science.gov (United States)

    Williams, J. P.

    2017-12-01

    Corinto crater (16.95°N, 141.72°E), a 13.8 km diameter crater in Elysium Planitia, displays dramatic rays in Mars Odyssey's Thermal Emission Imaging System (THEMIS) nighttime infrared imagery where high concentrations of secondary craters have altered the thermophysical properties of the martian surface. The THEMIS observations provide a record of secondary crater formation in the region and ray segments are identified up to 2000 km ( 145 crater radii) distance [1][2]. Secondary craters are likely to have the largest influence on model surfaces ages between 0.1 to a few Myr as there is the potential for one or two sizeable craters to project secondary craters onto those surfaces and thus alter the crater size-frequency distribution (CSFD) with an instantaneous spike in crater production [3]. Corinto crater is estimated to be less than a few Ma [4] placing the formation of its secondaries within this formative time period. Secondary craters superposed on relatively young impact craters that predate Corinto provide observations of the secondary crater populations. Crater counts at 520 and 660 km distance from Corinto (38 and 48 crater radii respectively), were conducted. Higher crater densities were observed within ray segments, however secondary craters still influenced the CSFD where ray segments were not apparent, resulting in steepening in the CSFD. Randomness analysis confirms an increase in clustering as diameters decrease suggesting an increasing fraction of secondary craters at smaller diameters, both within the ray and outside. The counts demonstrate that even at nearly 50 crater radii, Corinto secondaries still influence the observed CSFD, even outside of any obvious rays. Crater populations used to derive model ages on many geologically young regions on Mars, such as glacial and periglacial landforms related to obliquity excursions that occur on 106 - 107 yr cycles, should be used cautiously and analyzed for any evidence, either morphologic or

  1. Implications of a global survey of venusian impact craters

    Science.gov (United States)

    Herrick, Robert R.; Phillips, Roger J.

    1994-01-01

    We present a global survey of the areal distribution, size-frequency distribution, and morphometric properties of the venusian impact cratering record. We explore the resurfacing history of Venus, crater degradation, ejecta emplacement, and cratering mechanics. The number of volcanically embayed and tectonically deformed craters from 0.5 to 1.0 km above mean planetary radius is disproportionately high for an otherwise crater-deficient elevation range. More resurfacing occurred in this range, an elevation range dominated by volcanic rises, rifts, and coronae, than elsewhere on Venus. Although the majority of craters appear to be relatively undisturbed and have intact ejecta blankets, some craters appear particularly `fresh' because thay have radar-bright floors, a radar-dark halo surrounding the ejecta blanket, and a west facing parabola of low radar return; 20, 35, and 8%, respectively, of craters with diameters greater than 22.6 km have these features. Characteristics of ejecta deposits for venusian craters change substantially with size, particularly at 20 km crater diameter, which marks the transition at which the boundaries of ejecta blankets go from ragged to lobate and the slope of the ejecta distance vs diameter curve steepens. Secondary craters are a ubiquitous part of the ejecta blanket for craters over 50 km but occur infrequently as isolated rays about smaller craters. Comparison of complex craters found on Venus with those of other planets gave results that were consistent with the idea that interplanetary differences in complex crater shape are controlled by interplanetary differences in gravity and crustal strength. The interplanetary comparison indicates that Venus, the Moon, and Mercury appear to have stronger crusts than do Mars and Ganymede/Callisto.

  2. Some Studies of Terrestrial Impact Cratering Rate

    Directory of Open Access Journals (Sweden)

    Jetsu L.

    2011-06-01

    Full Text Available In 1984, a 28.4 Myr periodicity was detected in the ages of terrestrial impact craters and a 26 Myr periodicity in the epochs of mass extinctions of species. Periodic comet showers from the Oort cloud seemed to cause catastrophic events linked to mass extinctions of species. Our first study revealed that the only significant detected periodicity is the “human signal” caused by the rounding of these data into integer numbers. The second study confirmed that the original 28.4 Myr periodicity detection was not significant. The third study revealed that the quality and the quantity of the currently available data would allow detection of real periodicity only if all impacts have been periodic, which cannot be the case. The detection of a periodic signal, if present, requires that more craters should be discovered and the accuracy of age estimates improved. If we sometimes will be able to find the difference between the craters caused by asteroid and comet impacts, the aperiodic component could be removed. The lunar impact craters may eventually provide the required supplementary data.

  3. Signs of Landscape Modifications at Martian Crater

    Science.gov (United States)

    2009-01-01

    [figure removed for brevity, see original site] Click on the image for larger version The lower portion of this image from the Thermal Emission Imaging System camera (THEMIS) on NASA's Mars Odyssey orbiter shows a crater about 16 kilometers (10 miles) in diameter with features studied as evidence of deposition or erosion. The crater is centered at 40.32 degrees south latitude and 132.5 degrees east longitude, in the eastern portion of the Hellas basin on Mars. It has gullies and arcuate ridges on its north, pole-facing interior wall. This crater is in the center of a larger (60-kilometer or 37-mile diameter) crater with lobate flows on its north, interior wall. The image, number V07798008 in the THEMIS catalog, covers a swath of ground 17.4 kilometers (10.8 miles) wide. NASA's Jet Propulsion Laboratory manages the Mars Odyssey mission for NASA's Office of Space Science. THEMIS was developed by Arizona State University in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

  4. Cepstrum Analysis of Terrestrial Impact Crater Records

    Directory of Open Access Journals (Sweden)

    Heon-Young Chang

    2008-06-01

    Full Text Available Study of terrestrial impact craters is important not only in the field of the solar system formation and evolution but also of the Galactic astronomy. The terrestrial impact cratering record recently has been examined, providing short- and intermediate-term periodicities, such as, Myrs, Myrs. The existence of such a periodicity has an implication in the Galactic dynamics, since the terrestrial impact cratering is usually interpreted as a result of the environmental variation during solar orbiting in the Galactic plane. The aim of this paper is to search for a long-term periodicity with a novel method since no attempt has been made so far in searching a long-term periodicity in this research field in spite of its great importance. We apply the cepstrum analysis method to the terrestrial impact cratering record for the first time. As a result of the analysis we have found noticeable peaks in the Fourier power spectrum appear ing at periods of Myrs and Myrs, which seem in a simple resonance with the revolution period of the Sun around the Galactic center. Finally we briefly discuss its implications and suggest theoretical study be pursued to explain such a long-term periodicity.

  5. The Carancas meteorite impact crater, Peru: Geologic surveying and modeling of crater formation and atmospheric passage

    Science.gov (United States)

    Kenkmann, T.; Artemieva, N. A.; Wünnemann, K.; Poelchau, M. H.; Elbeshausen, D.; Núñez Del Prado, H.

    2009-08-01

    The recent Carancas meteorite impact event caused a worldwide sensation. An H4-5 chondrite struck the Earth south of Lake Titicaca in Peru on September 15, 2007, and formed a crater 14.2 m across. It is the smallest, youngest, and one of two eye-witnessed impact crater events on Earth. The impact violated the hitherto existing view that stony meteorites below a size of 100 m undergo major disruption and deceleration during their passage through the atmosphere and are not capable of producing craters. Fragmentation occurs if the strength of the meteoroid is less than the aerodynamic stresses that occur in flight. The small fragments that result from a breakup rain down at terminal velocity and are not capable of producing impact craters. The Carancas cratering event, however, demonstrates that meter-sized stony meteoroids indeed can survive the atmospheric passage under specific circumstances. We present results of a detailed geologic survey of the crater and its ejecta. To constrain the possible range of impact parameters we carried out numerical models of crater formation with the iSALE hydrocode in two and three dimensions. Depending on the strength properties of the target, the impact energies range between approximately 100-1000 MJ (0.024- 0.24 t TNT). By modeling the atmospheric traverse we demonstrate that low cosmic velocities (12- 14 kms-1) and shallow entry angles (<20°) are prerequisites to keep aerodynamic stresses low (<10 MPa) and thus to prevent fragmentation of stony meteoroids with standard strength properties. This scenario results in a strong meteoroid deceleration, a deflection of the trajectory to a steeper impact angle (40-60°), and an impact velocity of 350-600 ms-1, which is insufficient to produce a shock wave and significant shock effects in target minerals. Aerodynamic and crater modeling are consistent with field data and our microscopic inspection. However, these data are in conflict with trajectories inferred from the analysis of

  6. The Mystery Soil

    Science.gov (United States)

    2004-01-01

    [figure removed for brevity, see original site] Click for larger view This high-resolution image from the panoramic camera on the Mars Exploration Rover Spirit shows the region containing the patch of soil scientists examined at Gusev Crater just after Spirit rolled off the Columbia Memorial Station. Scientists examined this patch on the 13th and 15th martian days, or sols, of Spirit's journey. Using nearly all the science instruments located on the rover's instrument deployment device or 'arm,' scientists yielded some puzzling results including the detection of a mineral called olivine and the appearance that the soil is stronger and more cohesive than they expected. Like detectives searching for clues, the science team will continue to peruse the landscape for explanations of their findings.Data taken from the camera's red, green and blue filters were combined to create this approximate true color picture, acquired on the 12th martian day, or sol, of Spirit's journey.The yellow box (see inset above) in this high-resolution image from the panoramic camera on the Mars Exploration Rover Spirit outlines the patch of soil scientists examined at Gusev Crater just after Spirit rolled off the Columbia Memorial Station.

  7. Bright Soil Churned by Spirit's Sol 1861 Drive

    Science.gov (United States)

    2009-01-01

    NASA's Mars Exploration Rover Spirit drove 22.7 meters (74 feet) toward the southwest on the 1,861st Martian day, or sol, of Spirit's mission on Mars (March 28, 2009). After the drive, the rover took this image with its front hazard-avoidance camera, looking back at the tracks from the drive. As usual since losing the use of its right-front wheel in 2006, Spirit drove backwards. The immobile right-front wheel churned up a long stripe of bright soil during this drive. Where Spirit has found such bright soil in the past, subsequent analysis of the composition found concentrations of sulfur or silica that testified to past action of water at the site. When members of the rover team saw the large quantity of bright soil exposed by the Sol 1861 drive, they quickly laid plans to investigate the composition with Spirit's alpha particle X-ray spectrometer. The Sol 1861 drive took the rover past the northwest corner of the low plateau called 'Home Plate,' making progress on a route around the western side of Home Plate. The edge of Home Plate forms the horizon on the right side of this image. Husband Hill is on the horizon on the left side. For scale, the parallel rover wheel tracks are about 1 meter (40 inches) apart. The rover's hazard-avoidance cameras take 'fisheye' wide-angle images.

  8. New Record Five-Wheel Drive, Spirit's Sol 1856

    Science.gov (United States)

    2009-01-01

    NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this stereo, 180-degree view of the rover's surroundings during the 1,856th Martian day, or sol, of Spirit's surface mission (March 23, 2009). The center of the view is toward the west-southwest. The rover had driven 25.82 meters (84.7 feet) west-northwestward earlier on Sol 1856. This is the longest drive on Mars so far by a rover using only five wheels. Spirit lost the use of its right-front wheel in March 2006. Before Sol 1856, the farthest Spirit had covered in a single sol's five-wheel drive was 24.83 meters (81.5 feet), on Sol 1363 (Nov. 3, 2007). The Sol 1856 drive made progress on a route planned for taking Spirit around the western side of the low plateau called 'Home Plate.' A portion of the northwestern edge of Home Plate is prominent in the left quarter of this image, toward the south. This view is presented as a cylindrical projection with geometric seam correction.

  9. 'Lyell' Panorama inside Victoria Crater (False Color)

    Science.gov (United States)

    2008-01-01

    Photojournal note: This very large image (487.9 MB TIFF and 17.71 MB JPEG) may be too large for some web browsers to handle. Users may right-click on the TIFF or JPEG link in the legend above to download the file to their desktop. The image can then be viewed in an image manipulation application such as Adobe Photoshop. During four months prior to the fourth anniversary of its landing on Mars, NASA's Mars Exploration Rover Opportunity examined rocks inside an alcove called 'Duck Bay' in the western portion of Victoria Crater. The main body of the crater appears in the upper right of this stereo panorama, with the far side of the crater lying about 800 meters (half a mile) away. Bracketing that part of the view are two promontories on the crater's rim at either side of Duck Bay. They are 'Cape Verde,' about 6 meters (20 feet) tall, on the left, and 'Cabo Frio,' about 15 meters (50 feet) tall, on the right. The rest of the image, other than sky and portions of the rover, is ground within Duck Bay. Opportunity's targets of study during the last quarter of 2007 were rock layers within a band exposed around the interior of the crater, about 6 meters (20 feet) from the rim. Bright rocks within the band are visible in the foreground of the panorama. The rover science team assigned informal names to three subdivisions of the band: 'Steno,' 'Smith,' and 'Lyell.' This view combines many images taken by Opportunity's panoramic camera (Pancam) from the 1,332nd through 1,379th Martian days, or sols, of the mission (Oct. 23 to Dec. 11, 2007). Images taken through Pancam filters centered on wavelengths of 753 nanometers, 535 nanometers and 432 nanometers were mixed to produce this view, which is presented in a false-color stretch to bring out subtle color differences in the scene. Some visible patterns in dark and light tones are the result of combining frames that were affected by dust on the front sapphire window of the rover's camera. Opportunity landed on Jan. 25, 2004

  10. Ganymede and Callisto - Complex crater formation and planetary crusts

    Science.gov (United States)

    Schenk, Paul M.

    1991-01-01

    Results are presented on measurements of crater depths and other morphological parameters (such as central peak and terrace frequency) of fresh craters on Ganymede and Callisto, two geophysically very similar but geologically divergent large icy satellites of Jupiter. These data were used to investigate the crater mechanics on icy satellites and the intersatellite crater scaling and crustal properties. The morphological transition diameters of and complex crater depths on Ganymede and Callisto were found to be similar, indicating that the crusts of both satellites are dominated by water ice with only a minor rocky component.

  11. Automated detection and classification for craters based on geometric matching

    Science.gov (United States)

    Chen, Jian-qing; Cui, Ping-yuan; Cui, Hui-tao

    2011-08-01

    Crater detection and classification are critical elements for planetary mission preparations and landing site selection. This paper presents a methodology for the automated detection and matching of craters on images of planetary surface such as Moon, Mars and asteroids. For craters usually are bowl shaped depression, craters can be figured as circles or circular arc during landing phase. Based on the hypothesis that detected crater edges is related to craters in a template by translation, rotation and scaling, the proposed matching method use circles to fitting craters edge, and align circular arc edges from the image of the target body with circular features contained in a model. The approach includes edge detection, edge grouping, reference point detection and geometric circle model matching. Finally we simulate planetary surface to test the reasonableness and effectiveness of the proposed method.

  12. Dust Devil in Spirit's View Ahead on Sol 1854

    Science.gov (United States)

    2009-01-01

    NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this stereo, 180-degree view of the rover's surroundings during the 1,854th Martian day, or sol, of Spirit's surface mission (March 21, 2009). The rover had driven 13.79 meters (45 feet) westward earlier on Sol 1854. West is at the center, where a dust devil is visible in the distance. North on the right, where Husband Hill dominates the horizon; Spirit was on top of Husband Hill in September and October 2005. South is on the left, where lighter-toned rock lines the edge of the low plateau called 'Home Plate.' This view is presented as a cylindrical projection with geometric seam correction.

  13. Spirit's Surroundings on 'West Spur,' Sol 305 (3-D)

    Science.gov (United States)

    2005-01-01

    [figure removed for brevity, see original site] Figure 1 [figure removed for brevity, see original site] Figure 2 This 360-degree stereo panorama shows the terrain surrounding NASA's Mars Exploration Rover Spirit as of the rover's 305th martian day, or sol, (Nov. 11, 2004). At that point, Spirit was climbing the 'West Spur' of the 'Columbia Hills.' The rover had just finished inspecting a rock called 'Lutefisk' and was heading uphill toward an area called 'Machu Picchu.' Spirit used its navigational camera to take the images combined into this mosaic. The rover's location when the images were taken is catalogued as the mission's site 89, position 205. The stereo-anaglyph view presented here is a cylindrical projection with geometric seam correction. Figure 1 is the left-eye view of a stereo pair and Figure 2 is the right-eye view of a stereo pair.

  14. The spirit of hypnosis: doing hypnosis versus being hypnotic.

    Science.gov (United States)

    Yapko, Michael D

    2014-01-01

    The spirit of hypnosis is reflected in the belief that people are more resourceful than they realize and through hypnosis can create meaningful possibilities. Thus, it is puzzling why hypnosis isn't better regarded. Do we present as too internally conflicted to inspire others' confidence? Do we overstate the dangers of hypnosis and scare people away? Do we define hypnosis as such a unique approach that others don't see its relevance for their work? Self-exploration is important if we want to ensure we are not unwittingly adding to our image problems as a field. Beyond these considerations, the novel and spirited application of hypnosis in the context of captive elephant breeding is discussed, as is a personal acknowledgment of some of the pioneers who manifested the spirit of hypnosis.

  15. Spiritual Treatment for Depression in Brazil: An Experience From Spiritism.

    Science.gov (United States)

    Lucchetti, Alessandra L Granero; Peres, Mario F Prieto; Vallada, Homero P; Lucchetti, Giancarlo

    2015-01-01

    Spiritism has been strongly connected with mental health in Brazil. However, there is a lack of descriptions of spiritual treatment provided by thousands of Brazilian Spiritist centers. The present study aims to describe the spiritual care for depression provided by one large Spiritist center in São Paulo, Brazil. This is a descriptive study carried out in 2012 at "São Paulo Spiritist Federation." Authors visited the "spiritual intervention sections," observed the therapies provided, listened to the "spirits' communication," and interviewed two patients. The assistance consists on a 90-min "Spiritual healing" session which includes educational lectures, "disobsession" (spirit release therapy), "passe" (laying on of hands) and person advice. Both patients had remitted depression when they were interviewed. Further studies would be necessary to report other religious/spiritual treatments in order to improve our understanding of the available practices used by patients and optimize the integration of conventional care with spiritual treatments. Copyright © 2015 Elsevier Inc. All rights reserved.

  16. ‘Do not quench the Spirit!’ The discourse of the Holy Spirit in earliest Christianity

    Directory of Open Access Journals (Sweden)

    Bert Jan Lietaert Peerbolte

    2015-09-01

    Full Text Available The Trinitarian discourse of the 4th and 5th centuries grew out of earlier developments, whilst at the same time reflecting a renewal over against the language of the earliest Christian sources. This article reflects on the way in which early Christianity thought about the Holy Spirit and developed a new discourse on the basis of earlier, Jewish traditions. It situates the development of the idea of the Holy Spirit as God’s presence in past and present within the social history of the developing Christian movement, and shows how this idea was connected to the concept of apostolic succession. Thus, emerging Christianity legitimised itself and its social structures by the theology of the Holy Spirit. Its message was presented as old instead of new, as the Holy Spirit had foretold the Christ event. Its organisation was seen as divinely inspired, because its leaders were thought to be endowed with the Spirit. In this development, the narrative of Luke-Acts has thoroughly influenced the way in which Christianity developed a new discourse to present itself as old.

  17. Analytical color analysis of irradiated sugar cane spirit with grapes

    Energy Technology Data Exchange (ETDEWEB)

    Pires, Juliana A.; Delabio, Aline S., E-mail: jujuba_angelo@yahoo.com.br, E-mail: aline_sd_timao@hotmail.com [Faculdade de Tecnologia em Piracicaba (FATEP), Piracicaba, SP (Brazil); Harder, Marcia N.C.; Moraes, Liz M.B.; Silva, Lucia C.A.; Arthur, Paula B.; Arthur, Valter, E-mail: mnharder@terra.com.br, E-mail: lizmarybueno@gmail.com, E-mail: lcasilva@cena.usp.br, E-mail: paula.arthur@hotmail.com, E-mail: arthur@cena.usp.br [Centro de Energia Nuclear na Agricultura (CENA/USP), Piracicaba, SP (Brazil)

    2013-07-01

    The aim of this work was to irradiate a Sugar Cane Spirit with grapes by gamma radiation (Co60) aiming the color alteration like an aging parameter. The Sugar Cane Spirit is a distilled beverage and in order that bouquet and flavor are enhanced, usually the Sugar Cane Spirit goes through a process of maturation in wooden barrels or in bottles with the presence of wood chips, which alters their appearance. However, is possible to get this same result with the use of gamma radiation from Co60 and there is a possibility of indicative the premature aging by the Sugar Cane Spirit color change, through the extraction of grape phenolic compounds. The Sugar Cane Spirit samples were prepared with grapes type Crimson in polypropylene bottles. The samples was irradiated at doses of 0 (control); 0.3KGy; 2kGy and 6kGy, subsequently were performed the colorimetric analyzes in periods of 5; 10; 20 and 50 days after the irradiation treatment. There was no significant statistical difference for the parameters L; a; b; Chrome and Hue-Angle, at 5; 10 and 20 days. On the 50th day only the parameter a shows significant statistical difference at the dose of 0.3kGy, that was higher than 2kGy and 6kGy doses, but not differ the between the control sample. So by the showed results was concluded that the irradiation at doses of 0.3Gy, 2kGy and 6kGy, do not change the color of the Sugar Cane Spirit. (author)

  18. Analytical color analysis of irradiated sugar cane spirit with grapes

    International Nuclear Information System (INIS)

    Pires, Juliana A.; Delabio, Aline S.; Harder, Marcia N.C.; Moraes, Liz M.B.; Silva, Lucia C.A.; Arthur, Paula B.; Arthur, Valter

    2013-01-01

    The aim of this work was to irradiate a Sugar Cane Spirit with grapes by gamma radiation (Co60) aiming the color alteration like an aging parameter. The Sugar Cane Spirit is a distilled beverage and in order that bouquet and flavor are enhanced, usually the Sugar Cane Spirit goes through a process of maturation in wooden barrels or in bottles with the presence of wood chips, which alters their appearance. However, is possible to get this same result with the use of gamma radiation from Co60 and there is a possibility of indicative the premature aging by the Sugar Cane Spirit color change, through the extraction of grape phenolic compounds. The Sugar Cane Spirit samples were prepared with grapes type Crimson in polypropylene bottles. The samples was irradiated at doses of 0 (control); 0.3KGy; 2kGy and 6kGy, subsequently were performed the colorimetric analyzes in periods of 5; 10; 20 and 50 days after the irradiation treatment. There was no significant statistical difference for the parameters L; a; b; Chrome and Hue-Angle, at 5; 10 and 20 days. On the 50th day only the parameter a shows significant statistical difference at the dose of 0.3kGy, that was higher than 2kGy and 6kGy doses, but not differ the between the control sample. So by the showed results was concluded that the irradiation at doses of 0.3Gy, 2kGy and 6kGy, do not change the color of the Sugar Cane Spirit. (author)

  19. Hailar crater - A possible impact structure in Inner Mongolia, China

    Science.gov (United States)

    Xiao, Zhiyong; Chen, Zhaoxu; Pu, Jiang; Xiao, Xiao; Wang, Yichen; Huang, Jun

    2018-04-01

    Hailar crater, a probable impact structure, is a circular depression about 300 m diameter in Inner Mongolia, northeast China. With broad elevated rims, the present rim-to-floor depth is 8-20 m. Regional geological background and geomorphological comparison suggest that this feature is likely not formed by surface processes such as salt diapir, karst, aeolian, glacial, or volcanic activity. Its unique occurrence in this region and well-preserved morphology are most consistent with it being a Cenozoic impact crater. Two field expeditions in 2016 and 2017 investigated the origin of this structure, recognizing that (1) no additional craters were identified around Hailar crater in the centimeter-scale digital topography models that were constructed using a drone imaging system and stereo photogrammetry; (2) no bedrock exposures are visible within or adjacent to the crater because of thick regolith coverage, and only small pieces of angular unconsolidated rocks are present on the crater wall and the gently-sloped crater rim, suggesting recent energetic formation of the crater; (3) most samples collected from the crater have identical lithology and petrographic characteristics with the background terrain, but some crater samples contain more abundant clasts and silicate hydrothermal veins, indicating that rocks from depths have been exposed by the crater; (4) no shock metamorphic features were found in the samples after thin section examinations; and (5) a systematic sample survey and iron detector scan within and outside of the crater found no iron-rich meteorites larger than 2 cm in size in a depth of 30 cm. Although no conclusive evidence for an impact origin is found yet, Hailar crater was most likely formed by an impact based on its unique occurrence and comparative geomorphologic study. We suggest that drilling in the crater center is required to verify the impact origin, where hypothesized melt-bearing impactites may be encountered.

  20. Wrinkle Ridges and Young Fresh Crater

    Science.gov (United States)

    2002-01-01

    (Released 10 May 2002) The Science Wrinkle ridges are a very common landform on Mars, Mercury, Venus, and the Moon. These ridges are linear to arcuate asymmetric topographic highs commonly found on smooth plains. The origin of wrinkle ridges is not certain and two leading hypotheses have been put forth by scientists over the past 40 years. The volcanic model calls for the extrusion of high viscosity lavas along linear conduits. This thick lava accumulated over these conduits and formed the ridges. The other model is tectonic and advocates that the ridges are formed by compressional faulting and folding. Today's THEMIS image is of the ridged plains of Lunae Planum located between Kasei Valles and Valles Marineris in the northern hemisphere of the planet. Wrinkle ridges are found mostly along the eastern side of the image. The broadest wrinkle ridges in this image are up to 2 km wide. A 3 km diameter young fresh crater is located near the bottom of the image. The crater's ejecta blanket is also clearly seen surrounding the sharp well-defined crater rim. These features are indicative of a very young crater that has not been subjected to erosional processes. The Story The great thing about the solar system is that planets are both alike and different. They're all foreign enough to be mysterious and intriguing, and yet familiar enough to be seen as planetary 'cousins.' By comparing them, we can learn a lot about how planets form and then evolve geologically over time. Crinkled over smooth plains, the long, wavy raised landforms seen here are called 'wrinkle ridges,' and they've been found on Mars, Mercury, Venus, and the Moon - that is, on rocky bodies that are a part of our inner solar system. We know from this observation that planets (and large-enough moons) follow similar processes. What we don't know for sure is HOW these processes work. Scientists have been trying to understand how wrinkle ridges form for 40 years, and they still haven't reached a conclusion. That

  1. BIOLOGICALLY ACTIVE SUBSTANCES OF SPIRIT PRODUCTION WASTE

    Directory of Open Access Journals (Sweden)

    A. S. Kayshev

    2014-01-01

    Full Text Available A content of biologically active compounds (BAC with signified pharmacological activity in distillers grains was proved. It is prospective for applications of these grains as a raw material resource of pharmaceuticals. A composition of BAC distillers grains received from wheat, corn, barley, millet at different spirit enterprises which use hydro fermentative grain processing. Considering polydispersity of distillers grains they were separated on solid and liquid phases preliminary. Physical and chemical characteristics of distillers grains' liquid base were identified. Elementary composition of distillers grains is signified by active accumulation of biogenic elements (phosphorus, potassium, magnesium, calcium, sodium, iron and low content of heavy metals. The solid phase of distillers grains accumulates carbon, hydrogen and nitrogen in high concentration. The liquid phase of distillers grains contains: proteins and amino acids (20-46%, reducing sugars (5,6%-17,5%, galacturonides (0,8-1,4%, ascorbic acid (6,2-11,4 mg%. The solid base of distillers grains contains: galacturonides (3,4-5,3%, fatty oil (8,4-11,1% with predomination of essential fatty acids, proteins and amino acids (2,1-2,5%, flavonoids (0,4-0,9%, tocopherols (3,4-7,7 mg%. A method of complex processing of distillers grains based on application of membrane filtering of liquid phase and liquid extraction by inorganic and organic solvents of solid phase, which allows almost full extraction of the sum of biologically active compounds (BAC from liquid phase (Biobardin BM and solid phase (Biobardin UL. Biobardin BM comprises the following elements: proteins and amino acids (41-69%, reducing sugars (3,5-15,6%, fatty oil (0,2-0,3%, flavonoids (0,2-0,7%, ascorbic acid (17-37 mg%. Biobardin UL includes: oligouronids (16,4-19,5%, proteins and amino acids (11-21%, fatty oil (3,2-4,9% which includes essential acids; flavonoids (0,6-1,5%, tocopherols (6,6-10,2 mg%, carotinoids (0,13-0,21 mg

  2. Democracy, Corruption and the Politics of Spirits in Contemporary Indonesia

    DEFF Research Database (Denmark)

    Bubandt, Nils Ole

    contentious area of democracy in Indonesia – elections, corruption, decentralization, and regional representation. The chapters explore the intimate ways in which the political world and the spirit world are entangled. The core argument of the book is that Indonesia’s seemingly peculiar problems...... with democracy and spirits in fact reflect a set of contradictions within democracy itself. The book will be of interest to academics in the fields of Asian Studies, anthropology and political science and relevant for the study of Indonesian politics and democracy in Asia and beyond....

  3. Heavy Cratering near Callisto's South Pole

    Science.gov (United States)

    1997-01-01

    Images from NASA's Galileo spacecraft provide new insights into this region near Callisto's south pole. This two frame mosaic shows a heavily cratered surface with smooth plains in the areas between craters. North is to the top of the image. The smoothness of the plains appears to increase toward the south pole, approximately 480 kilometers (293 miles) south of the bottom of the image. This smoothness of Callisto's surface was not evident in images taken during the 1979 flyby of NASA's Voyager spacecraft because the resolution was insufficient to show the effect. This smooth surface, and the process(es) that cause it, are among the most intriguing aspects of Callisto. Although not fully understood, the process(es) responsible for this smoothing could include erosion by tiny meteorites and energetic ions. Some craters, such as Keelut, the 47 kilometer (29 mile) crater in the lower right corner, have sharp, well defined rims. Keelut contains an inner ring surrounding a central depression about 17 kilometers (11 miles) in diameter. Keelut, and the more irregularly shaped, degraded Reginleif, the 32 kilometer (19.5 mile) crater in the top center of the image, are very shallow and have flat floors. Crater forms can be seen down to less than 2 kilometers (1.2 miles) in diameter in the image. Each picture element (pixel) in this image is approximately 0.68 kilometers (0.41 miles) across.This image which was taken by the Galileo spacecraft's solid state imaging (CCD) system during its eighth orbit around Jupiter, on May 6th, 1997. The center of the image is located at 71.3 degrees south latitude, 97.6 degrees west longitude, and was taken when the spacecraft was approximately 35,470 kilometers (21,637 miles) from Callisto.The Jet Propulsion Laboratory, Pasadena, CA manages the mission for NASA's Office of Space Science, Washington, DC.This image and other images and data received from Galileo are posted on the World Wide Web, on the Galileo mission home page at URL http

  4. 27 CFR 28.192 - Packages of distilled spirits to be gauged.

    Science.gov (United States)

    2010-04-01

    ... packages which are to be removed for export with benefit of drawback, shall be gauged by the distilled... Spirits With Benefit of Drawback Filing of Notice and Removal § 28.192 Packages of distilled spirits to be...

  5. Geological Mapping of Lunar Crater Lalande: Topographic Configuration, Morphology and Cratering Process

    Science.gov (United States)

    Li, B.; Ling, Z. C.; Zhang, J.; Chen, J.; Liu, C. Q.; Bi, X. Y.

    2017-07-01

    Highland crater Lalande (4.45° S, 8.63° W; D = 23.4 km) is located on the PKT area of the lunar near side, southeast of Mare Insularum. It is a complex crater in Copernican era and has three distinguishing features: high silicic anomaly, highest Th abundance and special landforms on its floor. There are some low-relief bulges on the left of crater floor with regular circle or ellipse shapes. They are  250 to 680 m wide and  30 to 91 m high with maximum flank slopes > 20°. There are two possible scenarios for the formation of these low-relief bulges which are impact melt products or young silicic volcanic eruptions. According to the absolute model ages of ejecta, melt ponds and hummocky floor, the ratio of diameter and depth, similar bugle features within other Copernican-aged craters and lack of volcanic source vents, we hypothesized that these low-relief bulges were most consistent with an origin of impact melts during the crater formation instead of small and young volcanic activities occurring on the crater floor. Based on Kaguya TC ortho-mosaic and DTM data produced by TC imagery in stereo, geological units and some linear features on the floor and wall of Lalande have been mapped. Eight geological units are organized by crater floor units: hummocky floor, central peak and low-relief bulges; and crater wall units: terraced walls, channeled and veneered walls, interior walls, mass wasting areas, blocky areas, and melt ponds. These geological units and linear features at Lalande provided us a chance to understand some details of the cratering process and elevation differences on the floor. We evaluated several possibilities to understand the potential causes for the observed elevation differences on the Lalande's floor. We proposed that late-stage wall collapse and subsidence due to melt cooling could be the possible causes of observed elevation differences on the floor.

  6. Aqueous alteration detection in Tikhonravov crater, Mars

    Science.gov (United States)

    Mancarella, F.; Fonti, S.; Alemanno, G.; Orofino, V.; Blanco, A.

    2018-03-01

    The existence of a wet period lasting long enough to allow the development of elementary forms of life on Mars has always been a very interesting issue. Given this perspective, the research for geological markers of such occurrences has been continually pursued. Once a favorable site is detected, effort should be spent to get as much information as possible aimed at a precise assessment of the genesis and evolution of the areas showing the selected markers. In this work, we discuss the recent finding of possible deposits pointing to the past existence of liquid water in Tikhonravov crater located in Arabia Terra. Comparison of CRISM spectra and those of laboratory minerals formed by aqueous alteration has led us to the conclusion that the studied areas within the impact crater host phyllosilicates deposits. In addition, analysis of the CRISM spectra has resulted in the tentative identification of carbonates mixed with phyllosilicates.

  7. Spectral Clustering of Hermean craters hollows

    Science.gov (United States)

    Lucchetti, Alice; Pajola, Maurizio; Cremonese, Gabriele; Carli, Cristian; Marzo, Giuseppe; Roush, Ted

    2017-04-01

    The Mercury Dual Imaging System (MDIS, Hawkins et al., 2007) onboard NASA MESSENGER (MErcury Surface, Space ENvironment, GEochemistry, and Ranging) spacecraft, provided high-resolution images of "hollows", i.e. shallow, irregular, rimless, flat-floored depressions with bright interiors and halos, often found on crater walls, rims, floors and central peaks (Blewett et al., 2011, 2013). The formation mechanism of these features was suggested to be related to the depletion of subsurface volatiles (Blewett et al., 2011, Vaughan et al., 2012). To understand the hollows' mineralogical composition, which can provide new insights on Mercury's surface characterization, we applied a spectral clustering method to different craters where hollows are present. We chose, as first test case, the 20 km wide Dominici crater due to previous multiple spectral detection (Vilas et al., 2016). We used the MDIS WAC dataset covering Dominici crater with a scale of 935 m/pixel through eight filters, ranging from 0.433 to 0.996 μm. First, the images have been photometrically corrected using the Hapke parameters (Hapke et al., 2002) derived in Domingue et al. (2015). We then applied a statistical clustering over the entire dataset based on a K-means partitioning algorithm (Marzo et al., 2006). This approach was developed and evaluated by Marzo et al. (2006, 2008, 2009) and makes use of the Calinski and Harabasz criterion (Calinski, T., Harabasz, J., 1974) to identify the intrinsically natural number of clusters, making the process unsupervised. The natural number of ten clusters was identified and spectrally separates the Dominici surrounding terrains from its interior, as well as the two hollows from their edges. The units located on the brightest part of the south wall/rim of Dominici crater clearly present a wide absorption band between 0.558 and 0.828 μm. Hollows surrounding terrains typically present a red slope in the VNIR with a possible weak absorption band centered at 0.748

  8. Asymmetric Space Weathering on Lunar Crater Walls

    Science.gov (United States)

    Sim, Chae Kyung; Kim, Sungsoo S.; Lucey, Paul G.; Garrick-Bethell, Ian; Choi, Young-Jun

    2017-11-01

    Using new topography-corrected spectral data from the SELENE spacecraft, here we report a new lunar crater property produced by space weathering. We find that the optical properties of north, south, east, and west walls vary systematically across the Moon; pole-facing walls are brighter and less red (i.e., less mature) than their equator-facing counterparts as latitude increases, which we explain by reduced solar wind flux in pole-facing slopes. On the nearside, we find that east-west differences in crater wall brightness and redness vary with longitude, which we explain by solar wind shielding as the Moon passes through the Earth's magnetosphere. Because micrometeoroids are largely unaffected by magnetosphere passage, the longitudinal effect is used to discriminate between micrometeoroid and solar wind effects. Thus, for the first time we quantify how surface optical properties vary with solar wind flux.

  9. Rochechouart meteorite crater - Identification of projectile

    Science.gov (United States)

    Janssens, M.-J.; Hertogen, J.; Takahashi, H.; Anders, E.; Lambert, P.

    1977-01-01

    Ten samples from the 20-km Rochechouart crater in France have been analyzed for the siderophile elements Ir, Os, Re, Au, Pd, Ni, and Ge by radiochemical neutron activation analysis. The up to 1000-fold enrichment of siderophiles correlates with shock effects, increasing in the following order from least to greatest: basement rocks, glass-free breccias, glassy breccias, impact melts. The abundance pattern of the meteorite was determined from interelement correlations. Several samples fell off the correlation lines, presumably due to recrystallization and weathering of impact glasses during the approximately 165-m.y. age of the crater. The most reliable diagnostic elements were Os, Ir, Ni, and Pd; their abundance ratios suggest that the Rochechouart meteorite was a IIA iron.

  10. Low-velocity impact cratering experiments in granular slopes

    Science.gov (United States)

    Hayashi, Kosuke; Sumita, Ikuro

    2017-07-01

    Low-velocity impact cratering experiments are conducted in sloped granular targets to study the effect of the slope angle θ on the crater shape and its scales. We use two types of granular matter, sand and glass beads, former of which has a larger friction coefficient μs = tanθr , where θr is the angle of repose. Experiments show that as θ increases, the crater becomes shallower and elongated in the direction of the slope. Furthermore the crater floor steepens in the upslope side and a thick rim forms in the downslope side, thus forming an asymmetric profile. High-speed images show that these features are results of ejecta being dispersed farther towards the downslope side and the subsequent avalanche which buries much of the crater floor. Such asymmetric ejecta dispersal can be explained by combining the Z-model and a ballistic model. Using the topographic maps of the craters, we classify crater shape regimes I-III, which transition with increasing θ : a full-rim crater (I), a broken-rim crater (II), and a depression (III). The critical θ for the regime transitions are larger for sand compared to glass beads, but collapse to close values when we use a normalized slope θ^ = tanθ / tanθr . Similarly we derive θ^-dependences of the scaled crater depth, length, width and their ratios which collapse the results for different targets and impact energies. We compare the crater profiles formed in our experiments with deep craters on asteroid Vesta and find that some of the scaled profiles nearly overlap and many have similar depth / length ratios. This suggests that these Vestan craters may also have formed in the gravity regime and that the formation process can be approximated by a granular flow with a similar effective friction coefficient.

  11. Structural and Geological Interpretation of Posidonius Crater on the Moon

    Science.gov (United States)

    Ishihara, Y.; Chiba, T.; Haruyama, J.; Otake, H.; Ohtake, M.

    2015-12-01

    Posidonius crater locates on northeastern rim parts of the Serenitatis basin and is a typical floor-fractured crater. Because of Posidonius is located lunar central nearside and easily observed by ground-base telescope, the complex texture of crater floor attracted planetary scientist attention from before lunar exportation era. However, origin or formation histories of floor fractures are not fully resolved yet. In this study, we try to estimate geologic histories of Posidonius crater based on topographic data and multiband image data obtained by Terrain Camera (TC) and Multiband Imager (MI) onboard Kaguya. A part of crater floor of Posidonius is flooded by mare basalt. Previous studies interpreted that the source of mare basalt is located somewhere at Mare Serenitatis and flooded into Posidonius crater, then sinuous rill (Rimae Posidonius) is the resulting structure of flooded basalt flow. However, based on TC topographic data, sinuous rill feature indicate opposite flow direction to previous interpretations. Based on TC topographic data, we could interpret topographic features as follows; Rimare Posidonius flow from volcanic vent located at northern edge of Posidonius crater floor and flow out to Mare Serenitatis at western rim, the central part of crater floor slightly leaned to west and broken in several regions. From band depth of MI data, eastern part of crater floor is mostly consisted by highland materials and complex rills are basically not showing the basaltic feature. Combined both analysis results, we interpret the cause of complex structure of Posidonius crater is as follows; after crater formation, large sill intruded below crater floor and uppermost layer of crater floor is delaminated from the basement then floats on basaltic intrusion as "otoshibuta" (Japanese style lid for stew). Complex fracture was probably formed delamination and flotation stage by mechanical stress.

  12. 27 CFR 19.701 - Spirits withdrawn from bonded premises.

    Science.gov (United States)

    2010-04-01

    ... withdrawn shall be limited to an amount necessary for conduct of the testing, research or development. If... other market analysis) to determine the quality or character of the finished product. The quantity of spirits so withdrawn shall not exceed the amount necessary for conduct of the proprietor's operations. (b...

  13. Engaging in Educational Leadership: The Generosity of Spirit

    Science.gov (United States)

    Benham, Maenette; Murakami-Ramalho, Elizabeth

    2010-01-01

    This study presents key principles and a model of engaged leadership in indigenous communities. Engaged leadership champions children and youth, delivers learning and teaching within the context of place and spirit, and occurs in partnerships with diverse communities. Stories of educational leaders grounded in the concepts of "ha," place,…

  14. Spirit's View Beside 'Home Plate' on Sol 1823

    Science.gov (United States)

    2009-01-01

    NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this 180-degree view of the rover's surroundings during the 1,823rd Martian day, or sol, of Spirit's surface mission (Feb. 17, 2009). The center of the view is toward the south-southwest. The rover had driven 7 meters (23 feet) eastward earlier on Sol 1823, part of maneuvering to get Spirit into a favorable position for climbing onto the low plateau called 'Home Plate.' However, after two driving attempts with negligible progress during the following three sols, the rover team changed its strategy for getting to destinations south of Home Plate. The team decided to drive Spirit at least partway around Home Plate, instead of ascending the northern edge and taking a shorter route across the top of the plateau. Layered rocks forming part of the northern edge of Home Plate can be seen near the center of the image. Rover wheel tracks are visible at the lower edge. This view is presented as a cylindrical projection with geometric seam correction.

  15. 27 CFR 28.280 - Distilled spirits and wines.

    Science.gov (United States)

    2010-04-01

    ... departure of the aircraft, and the brand, kind, and quantity of distilled spirits or wines. Where the... who certifies to the lading for attachment to the outgoing manifest. The other two copies shall be... shall be delivered to the customs officer for attachment to the incoming manifest. The remaining copy...

  16. Chinchirisi: The Phenomenon of "Spirit Children" Among the ...

    African Journals Online (AJOL)

    ... what others say or do, 'it is in our blood', they say. This raises concerns. In what ways and to what extent is this religio-cultural phenomenon a challenge to euthanasia, human rights and rural development in the contemporary society? This paper examines the phenomenon of 'spirit children' from an insider perspective.

  17. The Spirit of Creativity and Innovation in Mathematics

    Indian Academy of Sciences (India)

    Home; Journals; Resonance – Journal of Science Education; Volume 12; Issue 1. The Spirit of Creativity and Innovation in Mathematics. S Ramanan. Reflections Volume 12 Issue 1 January 2007 pp 82-90. Fulltext. Click here to view fulltext PDF. Permanent link: http://www.ias.ac.in/article/fulltext/reso/012/01/0082-0090 ...

  18. Themes in Spirit Possession in Ugandan Christianity | James ...

    African Journals Online (AJOL)

    . This paper discerns a number of common themes that run through many of these experiences. In particular, sex as a motif for deviance and evil is noted as a common feature of many of the possession stories and all contact with spirits is seen ...

  19. The Spirit of Adventure and the Art of Creation

    Indian Academy of Sciences (India)

    Home; Journals; Resonance – Journal of Science Education; Volume 19; Issue 7. The Spirit of Adventure and the Art of Creation: Camphor to Vitamin B12. Setty Mallikarjuna Babu Subramania Ranganathan. General Article Volume 19 Issue 7 July 2014 pp 593-623 ...

  20. Body-Mind-Spirit Practice for Healthy Aging

    Science.gov (United States)

    Lee, Eun-Kyoung Othelia; Yoon, Hyunsook; Lee, Jungui; Yoon, Jiyoung; Chang, Eunjin

    2012-01-01

    This community-based, health promotion intervention for seniors provided a comprehensive review of the effect of body-mind-spirit (BMS) interventions on health behaviors. The 12-week curriculum offered sessions on exercise, nutrition, sexuality, leisure, stress management, cognitive behavioral therapy, forgiveness, and happiness. Gerontological…

  1. St Paul on Soul, Spirit and the Inner Man

    NARCIS (Netherlands)

    van Kooten, G.H.; Elkaisy-Friemuth, M.; Dillon, J.M.

    2009-01-01

    George H. van Kooten, “St Paul on Soul, Spirit and the Inner Man,” in The Afterlife of the Platonic Soul: Reflections on Platonic Psychology in the Monotheistic Religions (ed. Maha Elkaisy-Friemuth and John M. Dillon; Ancient Mediterranean and Medieval Texts and Contexts: Studies in Platonism,

  2. Phenolic constituents, furans, and total antioxidant status of distilled spirits.

    Science.gov (United States)

    Goldberg, D M; Hoffman, B; Yang, J; Soleas, G J

    1999-10-01

    The concentrations of 11 phenols and 5 furans were measured in 12 categories of distilled spirits by HPLC methodology, together with the total antioxidant status (TAS) of the same beverages. Ellagic acid was the phenol present in highest concentration in all beverages. Moderate amounts of syringaldehyde, syringic acid, and gallic acid, as well as lesser amounts of vanillin and vanillic acid, were measurable in most samples of whiskey, brandy, and rum but were largely undetectable in gin, vodka, liqueurs, and miscellaneous spirits. 5-(Hydroxymethyl)furfural was the predominant furan in the former three beverages, notably cognac, with 2-furaldehyde the next highest, but these were undetectable in most of the latter beverages. Highest TAS values were given by armagnac, cognac, and bourbon whiskey, all three of which tended toward the highest concentrations of phenols. Negative TAS values were exhibited by rum, vodka, gin, and miscellaneous spirits in line with the low or undetectable phenol concentrations in these beverages. Wood aging is the most likely source of phenols and furans in distilled spirits. Those beverages exposed to this treatment contain significant antioxidant activity, which is between the ranges for white and red wines, with the potential to augment the antiatherosclerotic functions attributable to the ethanol that they contain.

  3. The Spirit of Adventure and the Art of Creation

    Indian Academy of Sciences (India)

    IAS Admin

    The Spirit of Adventure and the Art of Creation. Camphor to Vitamin B. 12. Setty Mallikarjuna Babu and Subramania Ranganathan. What is described in the pages that follow, is the recounting of an exciting epoch in creative chemistry, namely, the synthesis of the complex molecule cyanocobalamin or vitamin B. 12 . It is the ...

  4. Biodegradation of premium motor spirit (PMS) by lipase from ...

    African Journals Online (AJOL)

    Biodegradation of premium motor spirit (PMS) by lipase from Bacillus thuringiensis and Lysinibacillus sphaericus. ... The PDF file you selected should load here if your Web browser has a PDF reader plug-in installed (for example, a recent version of Adobe Acrobat Reader). If you would like more information about how to ...

  5. Book Reviews: The Spirit Level | Turok | New Agenda: South African ...

    African Journals Online (AJOL)

    The spirit level - Why more equal societies almost always do better. Richard Wilkinson, Kate Pickett. Allen Lane: London. 2009. 340 pp. Full Text: EMAIL FULL TEXT EMAIL FULL TEXT · DOWNLOAD FULL TEXT DOWNLOAD FULL TEXT · AJOL African Journals Online. HOW TO USE AJOL... for Researchers · for Librarians ...

  6. Performing the Holy Spirit: Ritualised Manifestation of Faith in an ...

    African Journals Online (AJOL)

    This research examines the aesthetic manifestations of religious belief, particularly in the Holy Spirit, through consideration of the performative dimensions and ritualised behaviours in the church services of an African Independent Church, namely, the New Gospel Church in Zion of Africa (NGCZA). The significance of ...

  7. Divine empowerment: The Holy Spirit and church revitalisation

    Directory of Open Access Journals (Sweden)

    Brian A. DeVries

    2015-07-01

    Full Text Available How do principles of church revitalisation correlate with the divine work of the Holy Spirit? This article argues that the Spirit is the primary agent of church revitalisation, and churchleaders should cooperate with the Spirit as he works for revitalisation. Thus the Spirit empowers church leaders who are used by him to revive, renew, and revitalise a church community. After briefly defining the Spirit’s empowerment with biblical examples, this article examines the underlying principles of empowerment for church leaders, followed by briefly considering methodology for church revitalisation. The author concludes by suggesting several signs of biblical empowerment in a local church community. Goddelike bemagtiging: Die Heilige Gees en kerkherstel. Watter plek beklee die goddelike werking van die Heilige Gees in die beginsels van kerkherstel? Hierdie artikel poneer dat die Heilige Gees die primêre agent is om nuwe lewe in die kerk te bring en kerkleiers behoort onder leiding van die Heilige Gees hulle hiervoor te beywer. Die Heilige Gees bemagtig dus die kerkleiers wat Hy gebruik om ’n kerklike gemeenskap te laat herleef, te vernuwe en hulle te besiel met lewenskragtigheid. Die Gees se bemagtiging word kortliks aan die hand van bybelse voorbeelde gedefineer, waarna die grondliggende beginsels vir die bemagtiging van die kerkleiers ondersoek word. Daarna word die metodologie om nuwe lewenskrag in die kerk te bring kortliks oorweeg. Die outeur sluit af deur verskeie tekens uit te lig wat op skriftuurlike bemagtiging van die Heilige Gees in die plaaslike kerkgemeenskap dui.

  8. Discursive investigation into John's internalised spirit identity and its ...

    African Journals Online (AJOL)

    What does it mean to live in a society where everything good is located within one ethnicity, and geography? In reading the gospel of John, one gets the impression that faithful disciples, the Holy Spirit and morality are exclusively located within the Johannine community and can only permeate to the outside through the ...

  9. The Holy Spirit as Dove and as Tongues of Fire

    DEFF Research Database (Denmark)

    Nielsen, Kirsten

    2011-01-01

    and the dove as metaphor in the Old Testament and in Mark 1:9-11 (the baptism of Jesus). Theories on metaphors, intertextuality and Conceptual Blending are applied to show how Gustava Brandt gives an interpretation of the holy spirit as a messenger of love where love is both burning and purifying. Finally...

  10. Window to 'Clovis's' Altered Past

    Science.gov (United States)

    2004-01-01

    This image taken by the Mars Exploration Rover Spirit shows a rock outcrop dubbed 'Clovis.' The rock was discovered to be softer than other rocks studied so far at Gusev Crater after the rover easily ground a hole (center) into it with its rock abrasion tool. An analysis of the interior of the hole with the rover's alpha particle X-ray spectrometer found higher concentrations of sulfur, bromine and chlorine compared to basaltic, or volcanic, rocks at Gusev. This might indicate that Clovis was chemically altered, and that fluids once flowed through the rock depositing these elements. Spirit's solar panels can be seen in the foreground. This image was taken by the rover's navigation camera on sol 205 (July 31, 2004).

  11. Field reconnaissance geologic mapping of the Columbia Hills, Mars, based on Mars Exploration Rover Spirit and MRO HiRISE observations

    Science.gov (United States)

    Crumpler, L.S.; Arvidson, R. E.; Squyres, S. W.; McCoy, T.; Yingst, A.; Ruff, S.; Farrand, W.; McSween, Y.; Powell, M.; Ming, D. W.; Morris, R.V.; Bell, J.F.; Grant, J.; Greeley, R.; DesMarais, D.; Schmidt, M.; Cabrol, N.A.; Haldemann, A.; Lewis, K.W.; Wang, A.E.; Schroder, C.; Blaney, D.; Cohen, B.; Yen, A.; Farmer, J.; Gellert, Ralf; Guinness, E.A.; Herkenhoff, K. E.; Johnson, J. R.; Klingelhfer, G.; McEwen, A.; Rice, J.W.; Rice, M.; deSouza, P.; Hurowitz, J.

    2011-01-01

    Chemical, mineralogic, and lithologic ground truth was acquired for the first time on Mars in terrain units mapped using orbital Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (MRO HiRISE) image data. Examination of several dozen outcrops shows that Mars is geologically complex at meter length scales, the record of its geologic history is well exposed, stratigraphic units may be identified and correlated across significant areas on the ground, and outcrops and geologic relationships between materials may be analyzed with techniques commonly employed in terrestrial field geology. Despite their burial during the course of Martian geologic time by widespread epiclastic materials, mobile fines, and fall deposits, the selective exhumation of deep and well-preserved geologic units has exposed undisturbed outcrops, stratigraphic sections, and structural information much as they are preserved and exposed on Earth. A rich geologic record awaits skilled future field investigators on Mars. The correlation of ground observations and orbital images enables construction of a corresponding geologic reconnaissance map. Most of the outcrops visited are interpreted to be pyroclastic, impactite, and epiclastic deposits overlying an unexposed substrate, probably related to a modified Gusev crater central peak. Fluids have altered chemistry and mineralogy of these protoliths in degrees that vary substantially within the same map unit. Examination of the rocks exposed above and below the major unconformity between the plains lavas and the Columbia Hills directly confirms the general conclusion from remote sensing in previous studies over past years that the early history of Mars was a time of more intense deposition and modification of the surface. Although the availability of fluids and the chemical and mineral activity declined from this early period, significant later volcanism and fluid convection enabled additional, if localized, chemical activity

  12. The central uplift of Ritchey crater, Mars

    Science.gov (United States)

    Ding, Ning; Bray, Veronica J.; McEwen, Alfred S.; Mattson, Sarah S.; Okubo, Chris H.; Chojnacki, Matthew; Tornabene, Livio L.

    2015-01-01

    Ritchey crater is a ∼79 km diameter complex crater near the boundary between Hesperian ridged plains and Noachian highland terrain on Mars (28.8°S, 309.0°E) that formed after the Noachian. High Resolution Imaging Science Experiment (HiRISE) images of the central peak reveal fractured massive bedrock and megabreccia with large clasts. Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) spectral analysis reveals low calcium pyroxene (LCP), olivine (OL), hydrated silicates (phyllosilicates) and a possible identification of plagioclase bedrock. We mapped the Ritchey crater central uplift into ten units, with 4 main groups from oldest and originally deepest to youngest: (1) megabreccia with large clasts rich in LCP and OL, and with alteration to phyllosilicates; (2) massive bedrock with bright and dark regions rich in LCP or OL, respectively; (3) LCP and OL-rich impactites draped over the central uplift; and (4) aeolian deposits. We interpret the primitive martian crust as igneous rocks rich in LCP, OL, and probably plagioclase, as previously observed in eastern Valles Marineris. We do not observe high-calcium pyroxene (HCP) rich bedrock as seen in Argyre or western Valles Marineris. The association of phyllosilicates with deep megabreccia could be from impact-induced alteration, either as a result of the Richey impact, or alteration of pre-existing impactites from Argyre basin and other large impacts that preceded the Ritchey impact, or both.

  13. The isostatic state of Mead crater

    Science.gov (United States)

    Banerdt, W. B.; Konopliv, A. S.; Rappaport, N. J.; Sjogren, W. L.; Grimm, R. E.; Ford, P. G.

    1994-01-01

    We have analyzed high-resolution Magellan Doppler tracking data over Mead crater, using both line-of-sight and spherical harmonic methods, and have found a negative gravity anomaly of about 4-5 mgal (at spacecraft altitude, 182 km). This is consistent with no isostatic compensation of the present topography; the uncertainty in the analysis allows perhaps as much as 30% compensation at shallow dpeths (approximately 25 km). This is similar to observations of large craters on Earth, which are not generally compensated, but contrasts with at least some lunar basins which are inferred to have large Moho uplifts and corresponding positive Bouguer anomalies. An uncompensated load of this size requires a lithosphere with an effective elastic lithosphere thickness greater than 30 km. In order for the crust-mantle boundary not to have participated in the deformation associated with the collapse of the transient cavity during the creation of the crater, the yield strength near the top of the mantle must have been significantly higher on Earth and Venus than on the Moon at the time of basin formation. This might be due to increased strength against frictional sliding at the higher confining pressures within the larger planets. Alternatively, the thinner crusts of Earth and Venus compared to that of the Moon may result in higher creep strength of the upper mantle at shallower depths.

  14. Dynamics of the spirit possession phenomenon in Eastern Tanzania

    Directory of Open Access Journals (Sweden)

    Marja-Liisa Swantz

    1976-01-01

    Full Text Available The discussion on the spirit possession phenomenon is related in this study to the more general question of the role of religious institutions as part in the development process of a people living in a limited geographical area of a wider national society. It is assumed that religion, like culture in general, has its specific institutional forms as result of the historical development of a society, but at the same time religion is a force shaping that history. People's cultural resources influence their social and economic development and form a potential creative element in it'. Some of the questions to be asked are: "How are specific religious practices related to the dynamics of change in the societies in question? What is the social and religious context in which the spirit possession phenomenon occurs in them? What social and economic relations get their expression in them? To what extent is spirit possession in this case a means of exerting values and creatively overcoming a crisis or conflict which the changing social and economic relations impose on the people? The established spirit possession cults are here seen as the institutional forms of religious experience. At the same time it becomes evident that there is institutionalization in process as well as deinstitutionalization of spirit possession where it occurs outside established institutional forms. Institution is taken as a socially shared form of behaviour the significance of which is commonly recognized by those who share it. By the term spirit possession cult is meant a ritual form of spirit possession of a group which is loosely organized and without strict membership. The context of the study is four ethnic groups in Eastern Tanzania, near the coast of the Indian Ocean. The general theme of the project is The Role of Culture in the Restructuring of Tanzanian Rural Areas. The restructuring refers to a villagisation programme carried out in the whole country. People are being

  15. 27 CFR 19.241 - Operations bond-distilled spirits plant and adjacent bonded wine cellar.

    Science.gov (United States)

    2010-04-01

    ... spirits plant and adjacent bonded wine cellar. 19.241 Section 19.241 Alcohol, Tobacco Products and... wine cellar. (a) General. A wine cellar under the provisions of 27 CFR part 24 shall be treated as... subpart G for the production of distilled spirits; and (2) Such wine cellar and distilled spirits plant...

  16. 27 CFR 19.532 - Withdrawals of spirits for use in wine production.

    Science.gov (United States)

    2010-04-01

    ... use in wine production. 19.532 Section 19.532 Alcohol, Tobacco Products and Firearms ALCOHOL AND... Withdrawals Withdrawal of Spirits Without Payment of Tax § 19.532 Withdrawals of spirits for use in wine production. Wine spirits may be withdrawn to a bonded wine cellar without payment of tax for use in wine...

  17. 27 CFR 19.203 - Alternation of distilled spirits plant and bonded wine cellar premises.

    Science.gov (United States)

    2010-04-01

    ... spirits plant and bonded wine cellar premises. 19.203 Section 19.203 Alcohol, Tobacco Products and... spirits plant and bonded wine cellar premises. (a) General. A proprietor of a distilled spirits plant operating a contiguous bonded wine cellar desiring to alternate the use of each premises by extension and...

  18. 27 CFR 24.91 - Conveyance of untaxpaid wine or spirits.

    Science.gov (United States)

    2010-04-01

    ... wine or spirits. 24.91 Section 24.91 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU, DEPARTMENT OF THE TREASURY LIQUORS WINE Administrative and Miscellaneous Provisions Conveyance of Wine Or Spirits on Wine Premises § 24.91 Conveyance of untaxpaid wine or spirits. Untaxpaid...

  19. The role of the Holy spirit in Calvin's doctrine of the sacraments ...

    African Journals Online (AJOL)

    Calvin has frequently been labeled "the theologian of the Holy Spirit". Although there have been a number of studies of various aspects of the Holy Spirit in Calvin's theology since the significant works of Simon van der Linde (1943) and Werner Krusche (1957), none has dealt with the role the Spirit plays in Calvin's doctrine ...

  20. 27 CFR 28.301 - Loss of distilled spirits in transit.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Loss of distilled spirits in transit. 28.301 Section 28.301 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND....301 Loss of distilled spirits in transit. The tax on distilled spirits withdrawn without payment of...

  1. 27 CFR 28.310 - Loss of specially denatured spirits in transit.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Loss of specially denatured spirits in transit. 28.310 Section 28.310 Alcohol, Tobacco Products and Firearms ALCOHOL AND... Denatured Spirits § 28.310 Loss of specially denatured spirits in transit. Losses of specially denatured...

  2. 27 CFR 26.230 - Containers of distilled spirits to bear closures.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Containers of distilled spirits to bear closures. 26.230 Section 26.230 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO... distilled spirits to bear closures. Containers of 1 gallon (3.785 liters) or less of distilled spirits, upon...

  3. 27 CFR 19.204 - Alternation of distilled spirits plant and taxpaid wine bottling house premises.

    Science.gov (United States)

    2010-04-01

    ... spirits plant and taxpaid wine bottling house premises. 19.204 Section 19.204 Alcohol, Tobacco Products... distilled spirits plant and taxpaid wine bottling house premises. (a) General. A proprietor of a distilled spirits plant operating a contiguous taxpaid wine bottling house desiring to alternate the use of each...

  4. 27 CFR 19.396 - Spirits removed for shipment to Puerto Rico.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Spirits removed for shipment to Puerto Rico. 19.396 Section 19.396 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO... § 19.396 Spirits removed for shipment to Puerto Rico. Spirits removed for shipment to Puerto Rico with...

  5. “Bond of love”: The action of the spirit | Williams | Acta Theologica

    African Journals Online (AJOL)

    The ancient idea, seen especially in Augustine, is that the main activity of the Spirit is that of providing relationship, as the “bond of love”; this provides a key concept which undergirds the work of the Spirit in creation, redemption, sanctification and empowering. It is hoped that increased understanding of the work of the Spirit ...

  6. Numerical simulation of turbulent flows over crater-like obstacles: application to Gale crater, landing site of the Curiosity rover

    Science.gov (United States)

    Anderson, W.; Day, M. D.

    2017-12-01

    Mars is a dry planet with a thin atmosphere. Aeolian processes - wind-driven mobilization of sediment and dust - are the dominant mode of landscape variability on the dessicated landscapes of Mars. Craters are common topographic features on the surface of Mars, and many craters on Mars contain a prominent central mound (NASA's Curiosity rover was landed in Gale crater, with the rover journeying across an inner plan and towards Gale's central mound, Aeolus Mons). These mounds are composed of sedimentary fill, and, therefore, they contain rich information on the evolution of climatic conditions on Mars embodied in the stratigraphic "layering" of sediments. Many other craters no longer house a mound, but contain sediment and dust from which dune fields and other features form. Using density-normalized large-eddy simulations, we have modeled turbulent flows over crater-like topographies that feature a central mound. Resultant datasets suggest a deflationary mechanism wherein vortices shed from the upwind crater rim are realigned to conform to the crater profile via stretching and tilting. This insight was gained using three-dimensional datasets (momentum, vorticity, and turbulent stresses) retrieved from LES, and assessment of the relative influence of constituent terms responsible for the sustenance of mean vorticity. The helical, counter-rotating vortices occupy the inner region of the crater, and, therefore, are argued to be of great importance for aeolian morphodynamics in the crater (radial katabatic flows are also important to aeolian processes within the crater).

  7. New Record Five-Wheel Drive, Spirit's Sol 1856 (Stereo)

    Science.gov (United States)

    2009-01-01

    [figure removed for brevity, see original site] Left-eye view of a color stereo pair for PIA11962 [figure removed for brevity, see original site] Right-eye view of a color stereo pair for PIA11962 NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this stereo, 180-degree view of the rover's surroundings during the 1,856th Martian day, or sol, of Spirit's surface mission (March 23, 2009). The center of the view is toward the west-southwest. This view combines images from the left-eye and right-eye sides of the navigation camera. It appears three-dimensional when viewed through red-blue glasses with the red lens on the left. The rover had driven 25.82 meters (84.7 feet) west-northwestward earlier on Sol 1856. This is the longest drive on Mars so far by a rover using only five wheels. Spirit lost the use of its right-front wheel in March 2006. Before Sol 1856, the farthest Spirit had covered in a single sol's five-wheel drive was 24.83 meters (81.5 feet), on Sol 1363 (Nov. 3, 2007). The Sol 1856 drive made progress on a route planned for taking Spirit around the western side of the low plateau called 'Home Plate.' A portion of the northwestern edge of Home Plate is prominent in the left quarter of this image, toward the south. This view is presented as a cylindrical-perspective projection with geometric seam correction.

  8. Morphological Indicators of a Mascon Beneath Ceres's Largest Crater, Kerwan

    Science.gov (United States)

    Bland, M. T.; Ermakov, A. I.; Raymond, C. A.; Williams, D. A.; Bowling, T. J.; Preusker, F.; Park, R. S.; Marchi, S.; Castillo-Rogez, J. C.; Fu, R. R.; Russell, C. T.

    2018-02-01

    Gravity data of Ceres returned by the National Aeronautics and Space Administration's Dawn spacecraft is consistent with a lower density crust of variable thickness overlying a higher density mantle. Crustal thickness variations can affect the long-term, postimpact modification of impact craters on Ceres. Here we show that the unusual morphology of the 280 km diameter crater Kerwan may result from viscous relaxation in an outer layer that thins substantially beneath the crater floor. We propose that such a structure is consistent with either impact-induced uplift of the high-density mantle beneath the crater or from volatile loss during the impact event. In either case, the subsurface structure inferred from the crater morphology is superisostatic, and the mass excess would result in a positive Bouguer anomaly beneath the crater, consistent with the highest-degree gravity data from Dawn. Ceres joins the Moon, Mars, and Mercury in having basin-associated gravity anomalies, although their origin may differ substantially.

  9. A schematic model of crater modification by gravity

    Science.gov (United States)

    Melosh, H. J.

    1982-01-01

    The morphology of craters found on planets and moons of the solar system is examined and a development model which can account for the observed crater characteristics is discussed. The prompt collapse of craters to form flat floors, terraced walls, and central peak structures is considered to be the result of an approximate Bingham plastic rheology of the material surrounding the crater. This rheology is induced dynamically by the strong incoherent acoustic 'noise' accompanying excavation of the crater. Central pits, peak rings, and other multiple symmetric-profile rings originate by oscillation of this fluid. Large craters with transient depths comparable to the lithosphere thickness are subject to collapse by fragmentation of the lithosphere as well as fluidization. The considered concepts are developed mathematically. A model emerges which appears capable of explaining most of the qualitative features of large impact structures.

  10. Structural uplift and ejecta thickness of lunar mare craters: New insights into the formation of complex crater rims

    Science.gov (United States)

    Krüger, Tim; Kenkmann, Thomas

    2015-04-01

    Most complex impact craters on solid planetary surfaces throughout the Solar System exhibit elevated crater rims similar to the elevated crater rims of simple craters. In principal the final elevation of the crater rim is due to the deposition of ejecta on the structurally uplifted bedrock of the pre-impact surface. For simple craters the elevated crater rim is due to two well understood factors: (i) Emplacement of the coherent proximal ejecta material at the transient cavity rim (overturned flap) [1]. (ii) Structural uplift of the pre-impact surface in the proximity of the transient cavity [1, 2]. The amount of structural uplift at the rim of simple craters is due to plastic thickening of the target rock, the emplacement of interthrust wedges and/or the injection of dike material in the underlying target [1, 2, 3, 4]. Both factors, (i) and (ii), are believed to equally contribute to the structural uplift of simple craters. Larger craters have complex morphologies and the crater's extent may considerably exceed that of the transient cavity due to gravity-driven adjustment movements. For instance, the Ries crater's final diameter is twice of its transient cavity size. It is expected that both ejecta thickness and structural uplift decrease with increasing distance from the rim of the transient crater. For lunar craters the continuous ejecta extends up to 2 crater radii from the crater center. The ejecta blanket thickness ET at the rim crest of the transient crater (which is inside the final crater) is a function of the distance r from the crater center, with RT as the radius of the transient crater [2, 6, 7] and is expressed by the following function: (1) ET = 0.033 RT (r/RT)^-3.0 for r ≥ RT [5, 6] The structural uplift is largest at the transient cavity rim and gets rapidly smaller with increasing distance to the crater center and disappears after 1.3 - 1.7 crater radii [1]. These circumstances raise the question, how elevated rims of complex craters form? Based

  11. Roter Kamm Impact Crater in Namibia

    Science.gov (United States)

    1995-01-01

    This space radar image shows the Roter Kamm impact crater in southwest Namibia. The crater rim is seen in the lower center of the image as a radar-bright, circular feature. Geologists believe the crater was formed by a meteorite that collided with Earth approximately 5 million years ago. The data were acquired by the Spaceborne Imaging Radar-C/X-Band Synthetic Aperture Radar (SIR-C/X-SAR) instrument onboard space shuttle Endeavour on April 14, 1994. The area is located at 27.8 degrees south latitude and 16.2 degrees east longitude in southern Africa. The colors in this image were obtained using the following radar channels: red represents the L-band (horizontally transmitted and received); green represents the L-band (horizontally transmitted and vertically received); and blue represents the C-band (horizontally transmitted and vertically received). The area shown is approximately 25.5 kilometers (15.8 miles) by 36.4 kilometers (22.5 miles), with north toward the lower right. The bright white irregular feature in the lower left corner is a small hill of exposed rock outcrop. Roter Kamm is a moderate sized impact crater, 2.5 kilometers (1.5 miles) in diameter rim to rim, and is 130 meters (400 feet) deep. However, its original floor is covered by sand deposits at least 100 meters (300 feet) thick. In a conventional aerial photograph, the brightly colored surfaces immediately surrounding the crater cannot be seen because they are covered by sand. The faint blue surfaces adjacent to the rim may indicate the presence of a layer of rocks ejected from the crater during the impact. The darkest areas are thick windblown sand deposits which form dunes and sand sheets. The sand surface is smooth relative to the surrounding granite and limestone rock outcrops and appears dark in radar image. The green tones are related primarily to larger vegetation growing on sand soil, and the reddish tones are associated with thinly mantled limestone outcrops. Studies of impact craters on

  12. Geological mapping of lunar highland crater Lalande: Topographic configuration, morphology and cratering process

    Science.gov (United States)

    Li, Bo; Ling, Zongcheng; Zhang, Jiang; Chen, Jian; Liu, ChangQing; Bi, Xiangyu

    2018-02-01

    Highland crater Lalande (4.45°S, 8.63°W; D = 23.4 km) is located on the PKT area of the lunar near side, southeast of the Mare Insularum. It is a complex crater in Copernican era and has three distinguishing features: high silicic anomaly, the highest Th abundance and special landforms on its floor. There are some low-relief bulges on the left of Lalande's floor with regular circle or ellipse shapes. They are ∼250-680 m wide and ∼30-91 m high with maximum flank slopes >20°. There are two possible scenarios for the formation of these low-relief bulges which are impact melt products or young silicic volcanic eruptions. We estimated the absolute model ages of the ejecta deposits, several melt ponds and the hummocky floor and determined the ratio of diameter and depth of the crater Lalande. In addition, we found some similar bugle features within other Copernican-aged craters and there were no volcanic source vents on Lalande's floor. Thus, we hypothesized that these low-relief bulges were most consistent with an origin of impact melts during the crater formation instead of small and young volcanic activities occurring on the floor. Based on Kaguya Terrain Camera (TC) ortho-mosaic and Digital Terrain Model (DTM) data produced by TC imagery in stereo, geological units and some linear features on the floor and wall of Lalande have been mapped. Eight geological units are organized by crater floor units: hummocky floor, central peak and low-relief bulges; and crater wall units: terraced walls, channeled and veneered walls, interior walls, mass wasting areas, blocky areas, and melt ponds. These geological units and linear features provided us a chance to understand some details of the cratering process and elevation differences on the floor. We proposed that subsidence due to melt cooling, late-stage wall collapse and rocks uplifted from beneath the surface could be the possible causes of the observed elevation differences on Lalande's floor.

  13. Constructing Stratigraphic Relationships Using Secondary Craters: A Lunar Test Case

    Science.gov (United States)

    Wells, Kassandra; Campbell, D. B.; Campbell, B. A.; Carter, L. M.

    2008-09-01

    Secondary cratering is a possible contaminant of small crater distributions used to date young terrains in the Solar System. As such, much attention has been paid to identifying the effect of the secondary population on the cratering record of various bodies. Our technique utilizes 100m resolution circular polarization ratio (CPR) maps generated from 2.38 GHz Arecibo radar data of the lunar South Pole to distinguish secondary craters from small primaries at large distances from the primary impact. High levels of CPR are indicative of blocky ejecta tails and can be used not only to identify secondaries in this "far field” regime, but can also indicate the associated primary crater by the tail direction. We apply this method to a region on the floor of Newton-A crater ( 60 km diameter), where our refined counts identify 56 secondary craters with diameters above 400m (43.8% of the total population) associated with the primary crater Tycho (85 km diameter)—some 1000 km to the north. In addition to providing information on the relative importance of secondary and primary craters at small diameters, this method of secondary crater identification provides valuable information about the terrains on which they are emplaced. Secondary craters associated with a single primary event form simultaneously, therefore serving as a convenient layer around which stratigraphic relationships can be constructed—particularly if the age of the primary is well constrained. For extensive secondary networks, the semi-global reach of this layer provides a way to compare in a standardized way terrain units separated by thousands of kilometers. As a demonstration of this technique, we employ a combination of crater morphology and CPR tail analysis to determine the ages of features on the floor of Newton-A relative to the layer of Tycho secondaries present there. Funding by NASA's Planetary Astronomy program is acknowledged.

  14. Geologic map of Tooting crater, Amazonis Planitia region of Mars

    Science.gov (United States)

    Mouginis-Mark, Peter J.

    2015-01-01

    Tooting crater has a diameter of 27.2 km, and formed on virtually flat lava flows within Amazonis Planitia ~1,300 km west of the summit of Olympus Mons volcano, where there appear to have been no other major topographic features prior to the impact. The crater formed in an area ~185 x 135 km that is at an elevation between −3,870 m and −3,874 m relative to the Mars Orbiter Laser Altimeter (MOLA) Mars datum. This fortuitous situation (for example, a bland, horizontal target) allows the geometry of the crater and the thickness of the ejecta blanket to be accurately determined by subtracting the appropriate elevation of the surrounding landscape (−3,872 m) from the individual MOLA measurements across the crater. Thus, for the first time, it is possible to determine the radial decrease of ejecta thickness as a function of distance away from the rim crest. On the basis of the four discrete ejecta layers surrounding the crater cavity, Tooting crater is classified as a Multiple-Layered Ejecta (MLE) crater. By virtue of the asymmetric distribution of secondary craters and the greater thickness of ejecta to the northeast, Morris and others (2010) proposed that Tooting crater formed by an oblique impact from the southwest. The maximum range of blocks that produced identifiable secondary craters is ~500 km (~36.0 crater radii) from the northeast rim crest. In contrast, secondary craters are only identifiable ~215 km (15.8 radii) to the southeast and 225 km (16.5 radii) to the west.

  15. Impact spacecraft imagery and comparative morphology of craters

    International Nuclear Information System (INIS)

    Moutsoulas, M.; Piteri, S.

    1979-01-01

    The use of hard-landing 'simple' missions for wide-scale planetary exploration is considered. As an example of their imagery potentialities, Ranger VII data are used for the study of the morphological characteristics of 16 Mare Cognitum craters. The morphological patterns of lunar craters, expressed in terms of the Depth/Diameter ratios appear to be in most cases independent of the crater location or size. (Auth.)

  16. The role of strength defects in shaping impact crater planforms

    Science.gov (United States)

    Watters, W. A.; Geiger, L. M.; Fendrock, M.; Gibson, R.; Hundal, C. B.

    2017-04-01

    High-resolution imagery and digital elevation models (DEMs) were used to measure the planimetric shapes of well-preserved impact craters. These measurements were used to characterize the size-dependent scaling of the departure from circular symmetry, which provides useful insights into the processes of crater growth and modification. For example, we characterized the dependence of the standard deviation of radius (σR) on crater diameter (D) as σR ∼ Dm. For complex craters on the Moon and Mars, m ranges from 0.9 to 1.2 among strong and weak target materials. For the martian simple craters in our data set, m varies from 0.5 to 0.8. The value of m tends toward larger values in weak materials and modified craters, and toward smaller values in relatively unmodified craters as well as craters in high-strength targets, such as young lava plains. We hypothesize that m ≈ 1 for planforms shaped by modification processes (slumping and collapse), whereas m tends toward ∼ 1/2 for planforms shaped by an excavation flow that was influenced by strength anisotropies. Additional morphometric parameters were computed to characterize the following planform properties: the planform aspect ratio or ellipticity, the deviation from a fitted ellipse, and the deviation from a convex shape. We also measured the distribution of crater shapes using Fourier decomposition of the planform, finding a similar distribution for simple and complex craters. By comparing the strength of small and large circular harmonics, we confirmed that lunar and martian complex craters are more polygonal at small sizes. Finally, we have used physical and geometrical principles to motivate scaling arguments and simple Monte Carlo models for generating synthetic planforms, which depend on a characteristic length scale of target strength defects. One of these models can be used to generate populations of synthetic planforms which are very similar to the measured population of well-preserved simple craters on

  17. Floor-Fractured Craters through Machine Learning Methods

    Science.gov (United States)

    Thorey, C.

    2015-12-01

    Floor-fractured craters are impact craters that have undergone post impact deformations. They are characterized by shallow floors with a plate-like or convex appearance, wide floor moats, and radial, concentric, and polygonal floor-fractures. While the origin of these deformations has long been debated, it is now generally accepted that they are the result of the emplacement of shallow magmatic intrusions below their floor. These craters thus constitute an efficient tool to probe the importance of intrusive magmatism from the lunar surface. The most recent catalog of lunar-floor fractured craters references about 200 of them, mainly located around the lunar maria Herein, we will discuss the possibility of using machine learning algorithms to try to detect new floor-fractured craters on the Moon among the 60000 craters referenced in the most recent catalogs. In particular, we will use the gravity field provided by the Gravity Recovery and Interior Laboratory (GRAIL) mission, and the topographic dataset obtained from the Lunar Orbiter Laser Altimeter (LOLA) instrument to design a set of representative features for each crater. We will then discuss the possibility to design a binary supervised classifier, based on these features, to discriminate between the presence or absence of crater-centered intrusion below a specific crater. First predictions from different classifier in terms of their accuracy and uncertainty will be presented.

  18. The large crater on the small Asteroid (2867) Steins

    Science.gov (United States)

    Burchell, M. J.; Leliwa-Kopystynski, J.

    2010-12-01

    The maximum size of impact craters on finite bodies marks the largest impact that can occur short of impact induced disruption of the body. Recently attention has started to focus on large craters on small bodies such as asteroids and rocky and icy satellites. Here the large crater on the recently imaged Asteroid (2867) Steins (with crater diameter to mean asteroid radius ratio of 0.79) is shown to follow a limit set by other similar sized bodies with moderate macroporosity (i.e. fractured asteroids). Thus whilst large, the crater size is not novel, nor does it require Steins to possess an extremely large porosity. In one of the components of the binary Asteroid (90) Antiope there is the recently reported presence of an extremely large depression, possibly a crater, with depression diameter to mean asteroid radius ratio of ˜(1.4-1.62). This is consistent with the maximum size of a crater expected from previous observations of very porous rocky bodies (i.e. rubble-pile asteroids). Finally, a relationship between crater diameter (normalised to body radius) is proposed as a function of body porosity which suggests that the doubling of porosity between fractured asteroids and rubble-pile asteroids, nearly doubles the size ( D/ R value) of the largest crater sustainable on a rocky body.

  19. Determining long-term regional erosion rates using impact craters

    Science.gov (United States)

    Hergarten, Stefan; Kenkmann, Thomas

    2015-04-01

    More than 300,000 impact craters have been found on Mars, while the surface of Moon's highlands is even saturated with craters. In contrast, only 184 impact craters have been confirmed on Earth so far with only 125 of them exposed at the surface. The spatial distribution of these impact craters is highly inhomogeneous. Beside the large variation in the age of the crust, consumption of craters by erosion and burial by sediments are the main actors being responsible for the quite small and inhomogeneous crater record. In this study we present a novel approach to infer long-term average erosion rates at regional scales from the terrestrial crater inventory. The basic idea behind this approach is a dynamic equilibrium between the production of new craters and their consumption by erosion. It is assumed that each crater remains detectable until the total erosion after the impact exceeds a characteristic depth depending on the crater's diameter. Combining this model with the terrestrial crater production rate, i.e., the number of craters per unit area and time as a function of their diameter, allows for a prediction of the expected number of craters in a given region as a function of the erosion rate. Using the real crater inventory, this relationship can be inverted to determine the regional long-term erosion rate and its statistical uncertainty. A limitation by the finite age of the crust can also be taken into account. Applying the method to the Colorado Plateau and the Deccan Traps, both being regions with a distinct geological history, yields erosion rates in excellent agreement with those obtained by other, more laborious methods. However, these rates are formally exposed to large statistical uncertainties due to the small number of impact craters. As higher crater densities are related to lower erosion rates, smaller statistical errors can be expected when large regions in old parts of the crust are considered. Very low long-term erosion rates of less than 4

  20. Secondary Crater-Initiated Debris Flow on the Moon

    Science.gov (United States)

    Martin-Wells, K. S.; Campbell, D. B.; Campbell, B. A.; Carter, L. M.; Fox, Q.

    2016-01-01

    In recent work, radar circular polarization echo properties have been used to identify "secondary" craters without distinctive secondary morphologies. Because of the potential for this method to improve our knowledge of secondary crater population-in particular the effect of secondary populations on crater- derived ages based on small craters-it is important to understand the origin of radar polarization signatures associated with secondary impacts. In this paper, we utilize Lunar Reconnaissance Orbiter Camera photographs to examine the geomorphology of secondary craters with radar circular polarization ratio enhancements. Our investigation reveals evidence of dry debris flow with an impact melt component at such secondary craters. We hypothesize that these debris flows were initiated by the secondary impacts themselves, and that they have entrained blocky material ejected from the secondaries. By transporting this blocky material downrange, we propose that these debris flows (rather than solely ballistic emplacement) are responsible for the tail-like geometries of enhanced radar circular polarization ratio associated with the secondary craters investigated in this work. Evidence of debris flow was observed at both clustered and isolated secondary craters, suggesting that such flow may be a widespread occurrence, with important implications for the mixing of primary and local material in crater rays.

  1. Evidence for self-secondary cratering of Copernican-age continuous ejecta deposits on the Moon

    Science.gov (United States)

    Zanetti, M.; Stadermann, A.; Jolliff, B.; Hiesinger, H.; van der Bogert, C. H.; Plescia, J.

    2017-12-01

    Crater size-frequency distributions on the ejecta blankets of Aristarchus and Tycho Craters are highly variable, resulting in apparent absolute model age differences despite ejecta being emplaced in a geologic instant. Crater populations on impact melt ponds are a factor of 4 less than on the ejecta, and crater density increases with distance from the parent crater rim. Although target material properties may affect crater diameters and in turn crater size-frequency distribution (CSFD) results, they cannot completely reconcile crater density and population differences observed within the ejecta blanket. We infer from the data that self-secondary cratering, the formation of impact craters immediately following the emplacement of the continuous ejecta blanket by ejecta from the parent crater, contributed to the population of small craters (impact melt ponds most accurately reflecting the primary crater flux (N(1) = 3.4 × 10-5). Using the cratering flux recorded on Tycho impact melt deposits calibrated to accepted exposure age (109 ± 1.5 Ma) as ground truth, and using similar crater distribution analyses on impact melt at Aristarchus Crater, we infer the age of Aristarchus Crater to be ∼280 Ma. The broader implications of this work suggest that the measured cratering rate on ejecta blankets throughout the Solar System may be overestimated, and caution should be exercised when using small crater diameters (i.e. < 300 m on the Moon) for absolute model age determination.

  2. Empty Nest

    Science.gov (United States)

    2004-01-01

    This image mosaic taken by the panoramic camera onboard the Mars Exploration Rover Spirit shows the rover's landing site, the Columbia Memorial Station, at Gusev Crater, Mars. This spectacular view may encapsulate Spirit's entire journey, from lander to its possible final destination toward the east hills. On its way, the rover will travel 250 meters (820 feet) northeast to a large crater approximately 200 meters (660 feet) across, the ridge of which can be seen to the left of this image. To the right are the east hills, about 3 kilometers (2 miles) away from the lander. The picture was taken on the 16th martian day, or sol, of the mission (Jan. 18/19, 2004). A portion of Spirit's solar panels appear in the foreground. Data from the panoramic camera's green, blue and infrared filters were combined to create this approximate true color image.

  3. A model for the dynamics of crater-centered intrusion: Application to lunar floor-fractured craters

    Science.gov (United States)

    Thorey, Clément; Michaut, Chloé

    2014-01-01

    Lunar floor-fractured craters are a class of craters modified by post-impact mechanisms. They are defined by distinctive shallow floors that are convex or plate-like, sometimes with a wide floor moat bordering the wall region. Radial, concentric, and polygonal floor fractures suggest an endogenous process of modification. Two mechanisms have been proposed to account for such deformations: viscous relaxation and spreading of a magma intrusion at depth below the crater. To test the second assumption and bring more constraints on the intrusion process, we develop a model for the dynamics of magma spreading below an elastic overlying layer with a crater-like topography. As predicted in earlier more qualitative studies, the increase in lithostatic pressure at the crater wall zone prevents the intrusion from spreading laterally, leading to the thickening of the intrusion. Additionally, our model shows that the final crater floor appearance after the uplift, which can be convex or flat, with or without a circular moat bordering the wall zone, depends on the elastic thickness of the layer overlying the intrusion and on the crater size. Our model provides a simple formula to derive the elastic thickness of the overlying layer hence a minimum estimate for the intrusion depth. Finally, our model suggests that crust redistribution by cratering must have controlled magma ascent below most of these craters.

  4. Effect of Topography Degradation on Crater Size-Frequency Distributions: Implications for Populations of Small Craters and Age Dating

    Science.gov (United States)

    Xie, Minggang; Zhu, Meng-Hua; Xiao, Zhiyong; Wu, Yunzhao; Xu, Aoao

    2017-10-01

    Whether or not background secondary craters dominate populations of small impact craters on terrestrial bodies is a half-century controversy. It has been suggested that small craters on some planetary bodies are dominated by background secondary craters based partly on the steepened slope of crater size-frequency distribution (CSFD) toward small diameters, such as the less than 1 km diameter crater population on the lunar mare. Here we show that topography degradation enlarges craters and increases CSFD slopes with time. When topography degradation is taken into account, for various-aged crater populations, the observed steep CSFD at small diameters is uniformly consistent with an originally shallower CSFD, whose slope is undifferentiated from the CSFD slope estimated from near-Earth objects and terrestrial bolides. The results show that the effect of topography degradation on CSFD is important in dating planetary surfaces, and the steepening of CSFD slopes is not necessarily caused by secondary cratering, but rather a natural consequence of topography degradation.

  5. Cratering record in the inner solar system: Implications for earth

    International Nuclear Information System (INIS)

    Barlow, N.G.

    1988-01-01

    Internal and external processes have reworked the Earth's surface throughout its history. In particular, the effect of meteorite impacts on the early history of the earth is lost due to fluvial, aeolian, volcanic and plate tectonic action. The cratering record on other inner solar system bodies often provides the only clue to the relative cratering rates and intensities that the earth has experienced throughout its history. Of the five major bodies within the inner solar system, Mercury, Mars, and the Moon retain scars of an early episode of high impact rates. The heavily cratered regions on Mercury, Mars, and the Moon show crater size-frequency distribution curves similar in shape and crater density, whereas the lightly cratered plains on the Moon and Mars show distribution curves which, although similar to each other, are statistically different in shape and density from the more heavily cratered units. The similarities among crater size-frequency distribution curves for the Moon, Mercury, and Mars suggest that the entire inner solar system was subjected to the two populations of impacting objects but Earth and Venus have lost their record of heavy bombardment impactors. Thus, based on the cratering record on the Moon, Mercury, and Mars, it can be inferred that the Earth experienced a period of high crater rates and basin formation prior to about 3.8 BY ago. Recent studies have linked mass extinctions to large terrestrial impacts, so life forms were unable to establish themselves until impact rates decreased substantially and terrestrial conditions became more benign. The possible periodicity of mass extinctions has led to the theory of fluctuating impact rates due to comet showers in the post heavy bombardment period. The active erosional environment on the Earth complicates attempts to verify these showers by erasing geological evidence of older impact craters

  6. Detection of lunar floor-fractured craters using machine learning methods

    Science.gov (United States)

    Thorey, C.

    2015-10-01

    About 200 Floor Fractured Craters (FFCs) have been identified by Schultz (1976) on the Moon, mainly around the lunar maria. These craters are a class of impact craters that are distinguished by having radi-ally and concentric floor-fractured networks and ab-normally shallow floors. In some cases, the uplift of the crater floor can be as large as 50% of the initial crater depth. These impact craters are interpreted to have undergone endogenous deformations after their formation.

  7. Spirit of place of Merdeka corridor in Selatpanjang City

    Science.gov (United States)

    Aldy, Pedia; Dharma, S. Mira

    2018-03-01

    Historical city area was developing by an accumulation of developmental stages which influenced by various factors. The factors are political, economic, social, cultural, and modernization. The research will discuss the spirit of place of Merdeka corridor in Selatpanjang city, Meranti Islands. The purpose is to identify the spirit of place of Merdeka corridor and to find out the tourism concept by characters that support urban tourism in Selatpanjang city. The research method used is qualitative research method with the rationalistic paradigm. Based on cultural history, physical building, and spatial pattern, Merdeka corridor has unique characteristic, and it persists if compared by another in Selatpanjang city. However, damage of corridor, physical changes, and functions can slowly happen due to modernization and cannot avoid.

  8. The SPIRIT Telescope Initiative: Six Years On (Abstract)

    Science.gov (United States)

    Luckas, P.

    2017-12-01

    (Abstract only) Now in its sixth year of operation, the SPIRIT initiative remains unique in Australia, as a robust web-enabled robotic telescope initiative funded for education and outreach. With multiple modes of operation catering for a variety of usage scenarios and a fully supported education program, SPIRIT provides free access to contemporary astronomical tools for students and educators in Western Australia and beyond. The technical solution itself provides an excellent model for low cost robotic telescope installations, and the education program has evolved over time to include a broad range of student experiences - from engagement activities to authentic science. This paper details the robotic telescope solution, student interface, and educational philosophy, summarizes achievements and lessons learned, and examines the possibilities for future enhancement including spectroscopy.

  9. Time for a Change; Spirit's View on Sol 1843

    Science.gov (United States)

    2009-01-01

    NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this full-circle view of the rover's surroundings during the 1,843rd Martian day, or sol, of Spirit's surface mission (March 10, 2009). South is in the middle. North is at both ends. The rover had driven 36 centimeters downhill earlier on Sol 1854, but had not been able to get free of ruts in soft material that had become an obstacle to getting around the northeastern corner of the low plateau called 'Home Plate.' The Sol 1854 drive, following two others in the preceding four sols that also achieved little progress in the soft ground, prompted the rover team to switch to a plan of getting around Home Plate counterclockwise, instead of clockwise. The drive direction in subsequent sols was westward past the northern edge of Home Plate. This view is presented as a cylindrical projection with geometric seam correction.

  10. Forma dat esse: a Christian ontology of human spirit

    Directory of Open Access Journals (Sweden)

    Joan Martínez Porcell

    2015-09-01

    Full Text Available Forma dat esse was initially high fertility existential anthropology. Christian philosophy inherited although explanations hylemorphic with explaining human nature knew register the being and doing of the person inside the ontology of created spirits. The presence of human corporeality was a spirit that existed in the boundary and the horizon of eternity. The plasticity of human tendencies was a sign of his intelligence and it should be defined by their spirituality. The word was being-communication and love was the most important act of his life fertility. No wonder that we offer existential self as memory itself and the presence of the soul from the patenting of his spiritual being.

  11. Evidence of a Christmas spirit network in the brain

    DEFF Research Database (Denmark)

    Hougaard, Anders; Lindberg, Ulrich; Arngrim, Nanna

    2015-01-01

    OBJECTIVE: To detect and localise the Christmas spirit in the human brain. DESIGN: Single blinded, cross cultural group study with functional magnetic resonance imaging (fMRI). SETTING: Functional imaging unit and department of clinical physiology, nuclear medicine and PET in Denmark. PARTICIPANTS...... theme. METHODS: Functional brain scans optimised for detection of the blood oxygen level dependent (BOLD) response were performed while participants viewed a series of images with Christmas themes interleaved with neutral images having similar characteristics but containing nothing that symbolises...... spirit network" in the human brain comprising several cortical areas. This network had a significantly higher activation in a people who celebrate Christmas with positive associations as opposed to a people who have no Christmas traditions and neutral associations. Further research is necessary...

  12. Medical Eschatologies: The Christian Spirit of Hospital Protocol.

    Science.gov (United States)

    Langford, Jean M

    2016-01-01

    If much has been written of the forms of bodiliness reinforced by hospitals, less attention has been paid to the medicalization of the soul. The medical management of death institutionalizes divisions between body and soul, and matter and spirit, infusing end-of-life care with latent Christian theological presumptions. The invisibility of these presumptions is partly sustained by projecting religiosity on those who endorse other cosmologies, while retaining for medicine a mask of secular science. Stories of conflict with non-Christian patients force these presumptions into visibility, suggesting alternative ethics of care and mourning rooted in other understandings. In this article, I explore one such story. Considering the story as an allegory for how matter and spirit figure in contemporary postmortem disciplines, I suggest that it exposes both the operation of a taboo against mixing material and spiritual agendas, and an assumption that appropriate mourning is oriented toward symbolic homage, rather than concern for the material welfare of the dead.

  13. 27 CFR 19.742 - Tank record of wine or spirits of less than 190 degrees of proof.

    Science.gov (United States)

    2010-04-01

    ... wine or spirits of less than 190 degrees of proof to show deposits into, withdrawals from, and the... spirits by pipeline; (6) Wine gallons of wine, or proof gallons of spirits deposited; (7) If subject to... its serial number for deposits or withdrawals; (10) Wine gallons of wine, or proof gallons of spirits...

  14. 27 CFR 27.56 - Distilled spirits containers of a capacity of not more than 1 gallon.

    Science.gov (United States)

    2010-04-01

    ... containers of a capacity of not more than 1 gallon. 27.56 Section 27.56 Alcohol, Tobacco Products and... DISTILLED SPIRITS, WINES, AND BEER General Requirements Packaging and Marking of Distilled Spirits § 27.56 Distilled spirits containers of a capacity of not more than 1 gallon. Bottled distilled spirits imported...

  15. Iron-Rich Carbonates as the Potential Source of Evolved CO2 Detected by the Sample Analysis at Mars (SAM) Instrument in Gale Crater

    Science.gov (United States)

    Sutter, B.; Heil, E.; Rampe, E. B.; Morris, R. V.; Ming, D. W.; Archer, P. D.; Eigenbrode, J. L.; Franz, H. B.; Glavin, D. P.; McAdam, A. C.; hide

    2015-01-01

    The Sample Analysis at Mars (SAM) instrument detected at least 4 distinct CO2 release during the pyrolysis of a sample scooped from the Rocknest (RN) eolian deposit. The highest peak CO2 release temperature (478-502 C) has been attributed to either a Fe-rich carbonate or nano-phase Mg-carbonate. The objective of this experimental study was to evaluate the thermal evolved gas analysis (T/EGA) characteristics of a series of terrestrial Fe-rich carbonates under analog SAM operating conditions to compare with the RN CO2 releases. Natural Fe-rich carbonates (<53 microns) with varying Fe amounts (Fe(0.66)X(0.34)- to Fe(0.99)X(0.01)-CO3, where X refers to Mg and/or Mn) were selected for T/EGA. The carbonates were heated from 25 to 715 C (35 C/min) and evolved CO2 was measured as a function of temperature. The highest Fe containing carbonates (e.g., Fe(0.99)X(0.01)-CO3) yielded CO2 peak temperatures between 466-487 C, which is consistent with the high temperature RN CO2 release. The lower Fe-bearing carbonates (e.g., Fe(0.66)X(0.34)CO3) did not have peak CO2 release temperatures that matched the RN peak CO2 temperatures; however, their entire CO2 releases did occur within RN temperature range of the high temperature CO2 release. Results from this laboratory analog analysis demonstrate that the high temperature RN CO2 release is consistent with Fe-rich carbonate (approx.0.7 to 1 wt.% FeCO3). The similar RN geochemistry with other materials in Gale Crater and elsewhere on Mars (e.g., Gusev Crater, Meridiani) suggests that up to 1 wt. % Fe-rich carbonate may occur throughout the Gale Crater region and could be widespread on Mars. The Rocknest Fe-carbonate may have formed from the interaction of reduced Fe phases (e.g., Fe2+ bearing olivine) with atmospheric CO2 and transient water. Alternatively, the Rocknest Fe-carbonate could be derived by eolian processes that have eroded distally exposed deep crustal material that possesses Fe-carbonate that may have formed through

  16. Technical Preparation of the Airplane "Spirit of St. Louis."

    Science.gov (United States)

    Hall, Donald A

    1927-01-01

    Given here is a brief history of the design and construction of the "Spirit of St. Lewis", the airplane that Charles Lindbergh flew solo across the Atlantic. Although the plan was to modify a standard model Ryan M-2, it was quickly determined that modification was less practical than redesign. Colonel Lindbergh's active participation in the design of the aircraft is noted. Given here are the general dimensions, specifications, weight characteristics, and man hours required to build the aircraft.

  17. Spirit's View Beside 'Home Plate' on Sol 1823 (Stereo)

    Science.gov (United States)

    2009-01-01

    [figure removed for brevity, see original site] Left-eye view of a color stereo pair for PIA11971 [figure removed for brevity, see original site] Right-eye view of a color stereo pair for PIA11971 NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this stereo, 180-degree view of the rover's surroundings during the 1,823rd Martian day, or sol, of Spirit's surface mission (Feb. 17, 2009). This view combines images from the left-eye and right-eye sides of the navigation camera. It appears three-dimensional when viewed through red-blue glasses with the red lens on the left. The center of the view is toward the south-southwest. The rover had driven 7 meters (23 feet) eastward earlier on Sol 1823, part of maneuvering to get Spirit into a favorable position for climbing onto the low plateau called 'Home Plate.' However, after two driving attempts with negligible progress during the following three sols, the rover team changed its strategy for getting to destinations south of Home Plate. The team decided to drive Spirit at least partway around Home Plate, instead of ascending the northern edge and taking a shorter route across the top of the plateau. Layered rocks forming part of the northern edge of Home Plate can be seen near the center of the image. Rover wheel tracks are visible at the lower edge. This view is presented as a cylindrical-perspective projection with geometric seam correction.

  18. Consciousness, Mind, and Spirit: Three Levels of Human Cognition

    OpenAIRE

    Andrej Ule

    2015-01-01

    The article elucidates three important concepts and realities that refer to cognitive phenomena and are often (mistakenly) used as synonyms: consciousness (slo. zavest), mind (slo. um), and spirit (slo. duh). They present three levels of human cognition: individual-experiential, individual-mental, and trans-individual-mental. Simply put: the concept of consciousness pertains to the waking mental life of a human being, while the concept of mind pertains to the ability and activity to conscious...

  19. Puumeelsuse ülistus - Spirit of Nature / Agneta Land

    Index Scriptorium Estoniae

    Land, Agneta

    2008-01-01

    Rahvusvaheline puitarhitektuuri näitus 11.09.- 31.10.2008 Lahtis (Soome) Pro Puu galeriis. Eksponeeritakse Renzo Piano (Itaalia), Kengo Kuma (Jaapan), Richard Leplastrier'i (Austraalia), Peter Zumthor'i (Šveits) ja Jose Cruz Ovalle (Tšiili) loomingut. 2008. aastal pälvis Spirit of Nature auhinna tšiili arhitekt Jose Cruz Ovalle (sünd. 1948). Tema eluloolisi andmeid, looming, portreefoto

  20. Community Adaptation to the Hebei-Spirit Oil Spill

    OpenAIRE

    So-Min Cheong

    2012-01-01

    The focus of the research is the significance of dependence for communities to survive and adapt in times of environmental disasters. It shifts the emphasis on self-reliant communities for survival and examines the types and effects of dependence and external linkages by analyzing the range of community responses that include initial responses, early social impact, compensation, and conflicts after the Hebei-Spirit oil spill in December 2007 in Korea. The findings reveal that dependence is ...

  1. Mothers and Spirits: Religious Identity, Alcohol, and Death

    OpenAIRE

    Candi K. Cann

    2016-01-01

    Mothers and Spirits examines the intersection of women, alcohol, and death through a comparative analysis. Offering a brief history of the study of drinking, followed by a short analysis of drinking in European and Chinese cultures, Cann examines two religious texts central to the roles of women and alcohol in Chinese religious thought and Christianity. Finally, Cann utilizes the historical and textual background to contextualize her ethnographic study of women, alcohol, and death in Mexican ...

  2. View Ahead After Spirit's Sol 1861 Drive (Stereo)

    Science.gov (United States)

    2009-01-01

    [figure removed for brevity, see original site] Left-eye view of a color stereo pair for PIA11977 [figure removed for brevity, see original site] Right-eye view of a color stereo pair for PIA11977 NASA's Mars Exploration Rover Spirit used its navigation camera to take the images combined into this stereo, 210-degree view of the rover's surroundings during the 1,861st to 1,863rd Martian days, or sols, of Spirit's surface mission (March 28 to 30, 2009). This view combines images from the left-eye and right-eye sides of the navigation camera. It appears three-dimensional when viewed through red-blue glasses with the red lens on the left. The center of the scene is toward the south-southwest. East is on the left. West-northwest is on the right. The rover had driven 22.7 meters (74 feet) southwestward on Sol 1861 before beginning to take the frames in this view. The drive brought Spirit past the northwestern corner of Home Plate. In this view, the western edge of Home Plate is on the portion of the horizon farthest to the left. A mound in middle distance near the center of the view is called 'Tsiolkovsky' and is about 40 meters (about 130 feet) from the rover's position. This view is presented as a cylindrical-perspective projection with geometric seam correction.

  3. Dust Devil in Spirit's View Ahead on Sol 1854 (Stereo)

    Science.gov (United States)

    2009-01-01

    [figure removed for brevity, see original site] Left-eye view of a color stereo pair for PIA11960 [figure removed for brevity, see original site] Right-eye view of a color stereo pair for PIA11960 NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this stereo, 180-degree view of the rover's surroundings during the 1,854th Martian day, or sol, of Spirit's surface mission (March 21, 2009). This view combines images from the left-eye and right-eye sides of the navigation camera. It appears three-dimensional when viewed through red-blue glasses with the red lens on the left. The rover had driven 13.79 meters (45 feet) westward earlier on Sol 1854. West is at the center, where a dust devil is visible in the distance. North on the right, where Husband Hill dominates the horizon; Spirit was on top of Husband Hill in September and October 2005. South is on the left, where lighter-toned rock lines the edge of the low plateau called 'Home Plate.' This view is presented as a cylindrical-perspective projection with geometric seam correction.

  4. Brazilian organic sugarcane spirits: Physicochemical and chromatographic profile

    Directory of Open Access Journals (Sweden)

    Felipe Cimino Duarte

    Full Text Available ABSTRACT There has been a growing demand for products from organic agriculture for the food market. Brazil leads the production of sugarcane spirits and produces about 1.6 billion liters/year. New technologies have been sought throughout the supply chain to improve production, and organic raw material has been used in the production of sugar cane for the production of beverages. This study aimed to define the physicochemical and chromatographic profiles of eleven organic sugarcane spirits samples from various Brazilian states. The secondary components and contaminants were identified and quantified through physicochemical analyses, HPLC and gas chromatography (GC. A significant percentage of the organic sugarcane spirits samples contained concentrations of components that were above the limits required by the Ministry of Agriculture, Livestock and Provisioning (MAPA, specifically the esters (18.20%, copper and dry extract (9.10%. This contamination is caused by bad conditions employed during the production process, which are not in compliance with the good manufacturing practices determined and legislated by Brazilian law.

  5. Evolution of Volatile Compounds during the Distillation of Cognac Spirit.

    Science.gov (United States)

    Awad, Pierre; Athès, Violaine; Decloux, Martine Esteban; Ferrari, Gérald; Snakkers, Guillaume; Raguenaud, Patrick; Giampaoli, Pierre

    2017-09-06

    Cognac wine spirit has a complex composition in volatile compounds which contributes to its organoleptic profile. This work focused on the batch distillation process and, in particular, on volatile compounds specifically produced by chemical reactions during the distillation of Cognac wine spirit, traditionally conducted in two steps with charentais pot stills. The aim of this study was to characterize these volatile compounds formed during distillation. Sampling has been performed on the distillates and inside the boiler during a typical Cognac distillation. The analysis of these samples allowed us to perform a mass balance and to point out several types of volatile compounds whose quantities strongly increased during the distillation process. These compounds were distinguished by their chemical family. It has been found that the first distillation step was decisive for the formation of volatile compounds. Moreover, 2 esters, 3 aldehydes, 12 norisoprenoids, and 3 terpenes were shown to be generated during the process. These results suggest that some volatile compounds found in Cognac spirit are formed during distillation due to chemical reactions induced by high temperature. These findings give important indications to professional distillers in order to enhance the product's quality.

  6. 36 CFR 7.2 - Crater Lake National Park.

    Science.gov (United States)

    2010-07-01

    ... 36 Parks, Forests, and Public Property 1 2010-07-01 2010-07-01 false Crater Lake National Park. 7.2 Section 7.2 Parks, Forests, and Public Property NATIONAL PARK SERVICE, DEPARTMENT OF THE INTERIOR SPECIAL REGULATIONS, AREAS OF THE NATIONAL PARK SYSTEM § 7.2 Crater Lake National Park. (a) Fishing...

  7. Layers and Boulders in Crater Wall, Nepenthes Mensae Region

    Science.gov (United States)

    1999-01-01

    Peering down into craters offers Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) scientists an opportunity to examine one of the few landforms that Mars shares in common with the other planets and moons of our Solar System.The picture on the left (above) is a MOC context frame taken at the same time as the MOC high resolution image on the right. The white box on the left shows the location of the high resolution view. The high resolution image was targeted on a 3 kilometers (1.9 miles) wide impact crater on the floor of a larger crater in the Nepenthes Mensae region (near 3oS, 239oW). The context image is about 115 km (71 mi) across, the high-resolution image is 3 km (1.9 mi) across, and both are illuminated from the left/lower left.The 3 km diameter crater in the MOC image on the right is three times wider than the famous Meteor Crater in northern Arizona, USA. The high resolution image shows many small windblown drifts or dunes in the low areas both within the crater and outside on the surrounding terrain. Some portions of the crater's walls exhibit outcrops of bare, layered rock. Large boulders have been dislodged from the walls and have tumbled down the slopes to the crater floor. Many of these boulders are bigger than school buses and automobiles.

  8. Determination of lunar surface ages from crater frequency–size ...

    Indian Academy of Sciences (India)

    Crater size–frequency distribution is one of the powerful techniques to estimate the ages of planetary surfaces, especially from remote sensing studies. This has been applied to images of the Moon obtained from Clementine mission in 1994. Simple techniques of measurement of the diameter of the craters (in pixels) are ...

  9. Evolution of Occator Crater on (1) Ceres

    Energy Technology Data Exchange (ETDEWEB)

    Nathues, A.; Platz, T.; Thangjam, G.; Hoffmann, M.; Corre, L. Le; Reddy, V.; Kallisch, J. [Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Goettingen (Germany); Mengel, K. [IELF, TU Clausthal, Adolph-Roemer-Straße 2A, 38678 Clausthal-Zellerfeld (Germany); Cloutis, E. A. [University of Winnipeg, Winnipeg, MB R3B 2E (Canada); Crown, D. A., E-mail: nathues@mps.mpg.de, E-mail: platz@mps.mpg.de, E-mail: thangjam@mps.mpg.de, E-mail: hoffmann@mps.mpg.de, E-mail: kallisch@mps.mpg.de, E-mail: gkmengel@t-online.de, E-mail: e.cloutis@uwinnipeg.ca, E-mail: lecorre@psi.edu, E-mail: reddy@psi.edu, E-mail: crown@psi.edu [Planetary Science Institute, 1700 East Fort Lowell Rd, Suite 106, Tucson, AZ 85719-2395 (United States)

    2017-03-01

    The dwarf planet Ceres (diameter 939 km) is the largest object in the main asteroid belt. Recent investigations suggest that Ceres is a thermally evolved, volatile-rich body with potential geological activity, a body which was never completely molten but possibly differentiated into a rocky core, an ice-rich mantle, and which may contain remnant internal liquid water. Thermal alteration and exogenic material infall contribute to producing a (dark) carbonaceous chondritic-like surface containing ammoniated phyllosilicates. Here we report imaging and spectroscopic analyses of Occator crater derived from the Framing Camera and the Visible and Infrared Spectrometer onboard Dawn. We found that the central bright spot (Cerealia Facula) of Occator is ∼30 Myr younger than the crater itself. The central spot is located in a central pit which contains a dome that is spectrally homogenous, exhibiting absorption features that are consistent with carbonates. Multiple radial fractures across the dome indicate an extrusive formation process. Our results lead us to conclude that the floor region was subject to past endogenic activity. Dome and bright material in its vicinity formed likely due to a long-lasting, periodic, or episodic ascent of bright material from a subsurface reservoir rich in carbonates. Originally triggered by an impact event, gases, possibly dissolved from a subsurface water/brine layer, enabled material rich in carbonates to ascend through fractures and be deposited onto the surface.

  10. Mass Movement on Vesta at Steep Scarps and Crater Rims

    Science.gov (United States)

    Krohn, K.; Jaumann, R.; Otto, K.; Hoogenboom, T.; Wagner, R.; Buczkowski, D. L.; Garry, B.; Williams, D. A.; Yingst, R. A.; Scully, J.; hide

    2014-01-01

    The Quadrangles Av-11 and Av-12 on Vesta are located at the northern rim of the giant Rheasilvia south polar impact basin. The primary geologic units in Av-11 and Av-12 include material from the Rheasilvia impact basin formation, smooth material and different types of impact crater structures (such as bimodal craters, dark and bright crater ray material and dark ejecta material). Av-11 and Av-12 exhibit almost the full range of mass wasting features observed on Vesta, such as slump blocks, spur-and-gully morphologies and landslides within craters. Processes of collapse, slope instability and seismically triggered events force material to slump down crater walls or scarps and produce landslides or rotational slump blocks. The spur-and-gully morphology that is known to form on Mars is also observed on Vesta; however, on Vesta this morphology formed under dry conditions.

  11. Acoustic fluidization and the scale dependence of impact crater morphology

    Science.gov (United States)

    Melosh, H. J.; Gaffney, E. S.

    1983-01-01

    A phenomenological Bingham plastic model has previously been shown to provide an adequate description of the collapse of impact craters. This paper demonstrates that the Bingham parameters may be derived from a model in which acoustic energy generated during excavation fluidizes the rock debris surrounding the crater. Experimental support for the theoretical flow law is presented. Although the Bingham yield stress cannot be computed without detailed knowledge of the initial acoustic field, the Bingham viscosity is derived from a simple argument which shows that it increases as the 3/2 power of crater diameter, consistent with observation. Crater collapse may occur in material with internal dissipation Q as low as 100, comparable to laboratory observations of dissipation in granular materials. Crater collapse thus does not require that the acoustic field be regenerated during flow.

  12. Crater ejecta scaling laws - Fundamental forms based on dimensional analysis

    Science.gov (United States)

    Housen, K. R.; Schmidt, R. M.; Holsapple, K. A.

    1983-01-01

    Self-consistent scaling laws are developed for meteoroid impact crater ejecta. Attention is given to the ejection velocity of material as a function of the impact point, the volume of ejecta with a threshold velocity, and the thickness of ejecta deposit in terms of the distance from the impact. Use is made of recently developed equations for energy and momentum coupling in cratering events. Consideration is given to scaling of laboratory trials up to real-world events and formulations are developed for calculating the ejection velocities and ejecta blanket profiles in the gravity and strength regimes of crater formation. It is concluded that, in the gravity regime, the thickness of an ejecta blanket is the same in all directions if the thickness and range are expressed in terms of the crater radius. In the strength regime, however, the ejecta velocities are independent of crater size, thereby allowing for asymmetric ejecta blankets. Controlled experiments are recommended for the gravity/strength transition.

  13. SPIRITS 15c and SPIRITS 14buu: Two Obscured Supernovae in the Nearby Star-forming Galaxy IC 2163

    Energy Technology Data Exchange (ETDEWEB)

    Jencson, Jacob E.; Kasliwal, Mansi M.; Cao, Yi [Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125 (United States); Johansson, Joel [Benoziyo Center for Astrophysics, Weizmann Institute of Science, 76100 Rehovot (Israel); Contreras, Carlos; Castellón, Sergio; Morrell, Nidia; Phillips, Mark [Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena (Chile); Bond, Howard E.; Monson, Andrew J. [Dept. of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States); Masci, Frank J.; Helou, George [Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125 (United States); Cody, Ann Marie [NASA Ames Research Center, Moffett Field, CA 94035 (United States); Andrews, Jennifer E. [Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 (United States); Bally, John; Green, Wayne [Center for Astrophysics and Space Astronomy, University of Colorado, 389 UCB, Boulder, CO 80309 (United States); Fox, Ori D. [Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218 (United States); Gburek, Timothy; Gehrz, Robert D. [Minnesota Institute for Astrophysics, School of Physics and Astronomy, 116 Church Street, S. E., University of Minnesota, Minneapolis, MN 55455 (United States); Hsiao, Eric, E-mail: jj@astro.caltech.edu [Department of Physics, Florida State University, 77 Chieftain Way, Tallahassee, FL, 32306 (United States); and others

    2017-03-10

    SPitzer InfraRed Intensive Transients Survey—SPIRITS—is an ongoing survey of nearby galaxies searching for infrared (IR) transients with Spitzer /IRAC. We present the discovery and follow-up observations of one of our most luminous ( M {sub [4.5]} = −17.1 ± 0.4 mag, Vega) and reddest ([3.6] − [4.5] = 3.0 ± 0.2 mag) transients, SPIRITS 15c. The transient was detected in a dusty spiral arm of IC 2163 ( D ≈ 35.5 Mpc). Pre-discovery ground-based imaging revealed an associated, shorter-duration transient in the optical and near-IR (NIR). NIR spectroscopy showed a broad (≈8400 km s{sup −1}), double-peaked emission line of He i at 1.083 μ m, indicating an explosive origin. The NIR spectrum of SPIRITS 15c is similar to that of the Type IIb SN 2011dh at a phase of ≈200 days. Assuming an A {sub V} = 2.2 mag of extinction in SPIRITS 15c provides a good match between their optical light curves. The NIR light curves, however, show some minor discrepancies when compared with SN 2011dh, and the extreme [3.6]–[4.5] color has not been previously observed for any SN IIb. Another luminous ( M {sub 4.5} = −16.1 ± 0.4 mag) event, SPIRITS 14buu, was serendipitously discovered in the same galaxy. The source displays an optical plateau lasting ≳80 days, and we suggest a scenario similar to the low-luminosity Type IIP SN 2005cs obscured by A{sub V} ≈ 1.5 mag. Other classes of IR-luminous transients can likely be ruled out in both cases. If both events are indeed SNe, this may suggest that ≳18% of nearby core-collapse SNe are missed by currently operating optical surveys.

  14. High Ethanol Contents of Spirit Drinks in Kibera Slums, Kenya: Implications for Public Health

    Directory of Open Access Journals (Sweden)

    Alex O. Okaru

    2017-10-01

    Full Text Available Cheap licit and artisanal illicit spirit drinks have been associated with numerous outbreaks of alcohol poisoning especially with methanol. This study aimed to evaluate the quality of cheap spirit drinks in Kibera slums in Nairobi County, Kenya. The samples consisted of cheap licit spirits (n = 11 and the artisanal spirit drink, ‘chang’aa’, (n = 28. The parameters of alcoholic strength and volatile composition were used as indicators of quality and were determined using gas chromatography with flame ionization detection (GC-FID and gas chromatography-mass spectrometry (GC-MS respectively. The ranges for alcoholic strength were 42.8–85.8% vol and 28.3–56.7% vol for chang’aa and licit spirit drinks respectively, while the pH ranges were 3.3–4.2 and 4.4–4.8 for chang’aa and licit spirit drinks respectively. The majority of volatiles were found in artisanal spirits and they included higher alcohols, ethyl esters and carbonyl compounds. The alcoholic strength of all the artisanal spirits (100% and 91% of the licit spirits was above the 40% vol of standard spirits such as vodka. The high ethanol content of the alcohol products was the only element of public health significance in this study.

  15. High Ethanol Contents of Spirit Drinks in Kibera Slums, Kenya: Implications for Public Health.

    Science.gov (United States)

    Okaru, Alex O; Abuga, Kennedy O; Kibwage, Isaac O; Lachenmeier, Dirk W

    2017-10-17

    Cheap licit and artisanal illicit spirit drinks have been associated with numerous outbreaks of alcohol poisoning especially with methanol. This study aimed to evaluate the quality of cheap spirit drinks in Kibera slums in Nairobi County, Kenya. The samples consisted of cheap licit spirits ( n = 11) and the artisanal spirit drink, ' chang'aa' , ( n = 28). The parameters of alcoholic strength and volatile composition were used as indicators of quality and were determined using gas chromatography with flame ionization detection (GC-FID) and gas chromatography-mass spectrometry (GC-MS) respectively. The ranges for alcoholic strength were 42.8-85.8% vol and 28.3-56.7% vol for chang'aa and licit spirit drinks respectively, while the pH ranges were 3.3-4.2 and 4.4-4.8 for chang'aa and licit spirit drinks respectively. The majority of volatiles were found in artisanal spirits and they included higher alcohols, ethyl esters and carbonyl compounds. The alcoholic strength of all the artisanal spirits (100%) and 91% of the licit spirits was above the 40% vol of standard spirits such as vodka. The high ethanol content of the alcohol products was the only element of public health significance in this study.

  16. Simple Impact Crater Shapes From Shadows - The Sequel

    Science.gov (United States)

    Chappelow, J. E.

    2008-12-01

    At the last LPSC meeting I presented the outline of a method for determining simple impact crater shapes from shadows. In theory the shadow cast within a simple crater provides enough information to derive its cross-sectional shape from shadow measurements, at least to the maximum depth to which the shadow extends. Under certain simple assumptions, this can be done analytically. If the crater is conic-section - shaped, then it can be shown that the down-sun bound of any shadow cast within it is elliptical, with one axis along the direction of illumination and the other (perpendicular to it) of semi-length D/2 (where D is diameter). The properties of this shadow-ellipse can be related to the parameters of the crater shape conic-section, thus measurements of the shadow-ellipse yield not only crater depth and diameter but also the approximate crater shape, in terms of conic sections. The method also does not depend upon the shadow crossing near the crater center, which avoids a pitfall of older shadow measurement methods. The technique is also amenable to computer implementation, which has already been largely completed. Once computerized, crater measurements can be made rapidly and repeatably. The program reads in an image, its resolution, and the solar elevation and azimuth. The user then defines the crater rim by 'clicking' on three points, and the shadow ellipse by clicking on two more. The program calculates and outputs the diameter, the depth, and parameters describing the crater's approximating conic-section. It is highly applicable to situations where only single-image photography is available, for example MESSENGER flybys of Mercury. At the meeting I will present the finished math for this method and give some examples of its use.

  17. LU60645GT and MA132843GT Catalogues of Lunar and Martian Impact Craters Developed Using a Crater Shape-based Interpolation Crater Detection Algorithm for Topography Data

    Science.gov (United States)

    Salamuniccar, Goran; Loncaric, Sven; Mazarico, Erwan Matias

    2012-01-01

    For Mars, 57,633 craters from the manually assembled catalogues and 72,668 additional craters identified using several crater detection algorithms (CDAs) have been merged into the MA130301GT catalogue. By contrast, for the Moon the most complete previous catalogue contains only 14,923 craters. Two recent missions provided higher-quality digital elevation maps (DEMs): SELENE (in 1/16° resolution) and Lunar Reconnaissance Orbiter (we used up to 1/512°). This was the main motivation for work on the new Crater Shape-based interpolation module, which improves previous CDA as follows: (1) it decreases the number of false-detections for the required number of true detections; (2) it improves detection capabilities for very small craters; and (3) it provides more accurate automated measurements of craters' properties. The results are: (1) LU60645GT, which is currently the most complete (up to D>=8 km) catalogue of Lunar craters; and (2) MA132843GT catalogue of Martian craters complete up to D>=2 km, which is the extension of the previous MA130301GT catalogue. As previously achieved for Mars, LU60645GT provides all properties that were provided by the previous Lunar catalogues, plus: (1) correlation between morphological descriptors from used catalogues; (2) correlation between manually assigned attributes and automated measurements; (3) average errors and their standard deviations for manually and automatically assigned attributes such as position coordinates, diameter, depth/diameter ratio, etc; and (4) a review of positional accuracy of used datasets. Additionally, surface dating could potentially be improved with the exhaustiveness of this new catalogue. The accompanying results are: (1) the possibility of comparing a large number of Lunar and Martian craters, of e.g. depth/diameter ratio and 2D profiles; (2) utilisation of a method for re-projection of datasets and catalogues, which is very useful for craters that are very close to poles; and (3) the extension of the

  18. Creation of High Resolution Terrain Models of Barringer Meteorite Crater (Meteor Crater) Using Photogrammetry and Terrestrial Laser Scanning Methods

    Science.gov (United States)

    Brown, Richard B.; Navard, Andrew R.; Holland, Donald E.; McKellip, Rodney D.; Brannon, David P.

    2010-01-01

    Barringer Meteorite Crater or Meteor Crater, AZ, has been a site of high interest for lunar and Mars analog crater and terrain studies since the early days of the Apollo-Saturn program. It continues to be a site of exceptional interest to lunar, Mars, and other planetary crater and impact analog studies because of its relatively young age (est. 50 thousand years) and well-preserved structure. High resolution (2 meter to 1 decimeter) digital terrain models of Meteor Crater in whole or in part were created at NASA Stennis Space Center to support several lunar surface analog modeling activities using photogrammetric and ground based laser scanning techniques. The dataset created by this activity provides new and highly accurate 3D models of the inside slope of the crater as well as the downslope rock distribution of the western ejecta field. The data are presented to the science community for possible use in furthering studies of Meteor Crater and impact craters in general as well as its current near term lunar exploration use in providing a beneficial test model for lunar surface analog modeling and surface operation studies.

  19. Fourier analysis of planimetric lunar crater shape - Possible guide to impact history and lunar geology

    Science.gov (United States)

    Eppler, D. T.; Nummedal, D.; Ehrlich, R.

    1977-01-01

    If the lithology of lunar crust influences impact crater morphology, a method of analysis that is sensitive to small-scale changes in crater shape is required. In the present paper, it is shown that Fourier analysis in closed form can provide detailed information regarding planimetric crater shape. Preliminary analysis of the rim crest outline of 247 nearside lunar craters (larger than 18 km in diam) led to the following information: Imbrian and pre-Imbrian craters are more elongate than younger craters, possibly as a result of widespread crustal deformation early in the moon's history. Crater size does not affect the planimetric shape of craters. Highland craters are less circular than mare craters, probably due to the greater structural and lithologic complexity of the highland crust. Craters comprising each shape family of the eleventh harmonic typically are located in the same general geographic region of the moon.

  20. Spirits Trade After Reform in 1863: To the Issue of Efficiency of State Regulation of Spirits Turnover in Terms of Free Trade

    Directory of Open Access Journals (Sweden)

    Natalia Ye. Goryushkina

    2015-12-01

    Full Text Available On the grounds of published and non-published archive materials the article estimates efficiency of state regulation of spirits turnover in terms of excise taxation period. It also states types of spirits trade, types of public houses, groups of people that have obtained the right for wholesale, retail and that of small amount tradeoff spirits. License gaining procedures are widely described as well. The author pays significant attention to the areas in cities and countryside, where the public houses should not have been opened as well as the individuals who were admitted to spirits trade; also he states events which influenced the sale of spirits. The requirements to interior of public houses, working hours, quality and volumes of trade are also specified. It is pointed out that the officials of excise tax board were to control the regulations of spirit trade, their authority extended to public houses control in 1885. The author comes to the conclusion that regulatory means of excise tax was efficient and by increasing and decreasing of license cost, complication and simplification of new public houses opening all together allowed to regulate the turnover of spirits in terms of free trade thus influencing the number, types, density, range and quality of spirits. However, there was distinct ambiguity in Ministry of Finance policy during the stated excise taxation period. On the one hand it limited free sale of spirits, eradicating public houses which were considered detrimental. On the other hand, the Ministry was set not to notice abuse in trade which gave the opportunity to gain greater benefits at public cost from spirits sales.

  1. Riddles in the Dark: Imaging Inside Mercury's Permanently Shadowed Craters

    Science.gov (United States)

    Ernst, C. M.; Chabot, N. L.; Denevi, B. W.; Nair, H.; Deutsch, A. N.; Murchie, S. L.; Robinson, M. S.; Blewett, D. T.; Head, J. W.; Harmon, J. K.; Neumann, G. A.; Solomon, S. C.

    2013-12-01

    Numerous lines of evidence independently point to the presence of water ice in Mercury's polar regions: Earth-based radar shows radar-bright regions; Mariner 10 and MESSENGER Mercury Dual Imaging System (MDIS) images reveal that these regions are permanently (south polar region) or persistently (north polar region) shadowed; neutron spectrometry indicates hydrogen-rich material; thermal models support the presence of water ice; and Mercury Laser Altimeter (MLA) reflectance measurements at 1064 nm show high and low reflectance deposits consistent in location to where models predict surface and buried water ice, respectively. Throughout 2013, MESSENGER executed a campaign dedicated to imaging the permanently shadowed crater floors of Mercury's north polar region using sunlight scattered from nearby terrain. The campaign makes use of the broadband clear filter (central wavelength 700 nm, bandwidth 600 nm) of the MDIS wide-angle camera (WAC) to target and image radar-bright areas within all host craters > 10 km in diameter under multiple lighting conditions. To date, MESSENGER has imaged the interiors of nearly 20 craters that host radar-bright deposits, including the largest such deposits near the north pole that are likely to host surface water ice. The images reveal a variety of surface morphologies, ranging from the smooth crater floor of the fresh Kandinsky crater, to the moderately cratered floor of Tolkien crater, and to the battered floor of Prokofiev crater, in which the permanently shadowed region does not differ morphologically from the rest of the crater floor. Thus, no distinct morphology is identified in association with polar deposits, and craters hosting such material span the typical range of degradation states relative to their illuminated counterparts. MDIS images also reveal albedo differences in craters with floors not fully in permanent shadow. Prokofiev provides a special environment for viewing a radar- and MLA-bright region suspected to host

  2. Neurological effects of white spirit: Contribution of animal studies during a 30-year period

    DEFF Research Database (Denmark)

    Nielsen, Gunnar Damgård; Lund, Søren Peter; Ladefoged, Ole

    2006-01-01

    Numerous studies have suggested that long-term occupational exposure to white spirit may cause chronic toxic encephalopathy (WHO 1996). This review summarizes the chronic nervous system effects of white spirit in animal studies during a 30-year period. First, routine histopathology was consistently...... unable to reveal adverse peripheral or central nervous system effects after inhalation of white spirit. Second, neurobehavioural studies in animals showed no adverse effect after inhalation of white spirit with a high content of aromatics in contrast to what was found with products with a low content....... Third, white spirit with a high content of aromatics induced adverse neurochemical changes at inhalation of 400 ppm and possibly already at 100 ppm. In the studied parameters, white spirit with a low content of aromatics showed no clear adverse neurochemical effects at inhalation of 400 ppm...

  3. Secondary Craters and the Size-Velocity Distribution of Ejected Fragments around Lunar Craters Measured Using LROC Images

    Science.gov (United States)

    Singer, K. N.; Jolliff, B. L.; McKinnon, W. B.

    2013-12-01

    Title: Secondary Craters and the Size-Velocity Distribution of Ejected Fragments around Lunar Craters Measured Using LROC Images Authors: Kelsi N. Singer1, Bradley L. Jolliff1, and William B. McKinnon1 Affiliations: 1. Earth and Planetary Sciences, Washington University in St Louis, St. Louis, MO, United States. We report results from analyzing the size-velocity distribution (SVD) of secondary crater forming fragments from the 93 km diameter Copernicus impact. We measured the diameters of secondary craters and their distances from Copernicus using LROC Wide Angle Camera (WAC) and Narrow Angle Camera (NAC) image data. We then estimated the velocity and size of the ejecta fragment that formed each secondary crater from the range equation for a ballistic trajectory on a sphere and Schmidt-Holsapple scaling relations. Size scaling was carried out in the gravity regime for both non-porous and porous target material properties. We focus on the largest ejecta fragments (dfmax) at a given ejection velocity (υej) and fit the upper envelope of the SVD using quantile regression to an equation of the form dfmax = A*υej ^- β. The velocity exponent, β, describes how quickly fragment sizes fall off with increasing ejection velocity during crater excavation. For Copernicus, we measured 5800 secondary craters, at distances of up to 700 km (15 crater radii), corresponding to an ejecta fragment velocity of approximately 950 m/s. This mapping only includes secondary craters that are part of a radial chain or cluster. The two largest craters in chains near Copernicus that are likely to be secondaries are 6.4 and 5.2 km in diameter. We obtained a velocity exponent, β, of 2.2 × 0.1 for a non-porous surface. This result is similar to Vickery's [1987, GRL 14] determination of β = 1.9 × 0.2 for Copernicus using Lunar Orbiter IV data. The availability of WAC 100 m/pix global mosaics with illumination geometry optimized for morphology allows us to update and extend the work of Vickery

  4. Noachian and more recent phyllosilicates in impact craters on Mars.

    Science.gov (United States)

    Fairén, Alberto G; Chevrier, Vincent; Abramov, Oleg; Marzo, Giuseppe A; Gavin, Patricia; Davila, Alfonso F; Tornabene, Livio L; Bishop, Janice L; Roush, Ted L; Gross, Christoph; Kneissl, Thomas; Uceda, Esther R; Dohm, James M; Schulze-Makuch, Dirk; Rodríguez, J Alexis P; Amils, Ricardo; McKay, Christopher P

    2010-07-06

    Hundreds of impact craters on Mars contain diverse phyllosilicates, interpreted as excavation products of preexisting subsurface deposits following impact and crater formation. This has been used to argue that the conditions conducive to phyllosilicate synthesis, which require the presence of abundant and long-lasting liquid water, were only met early in the history of the planet, during the Noachian period (> 3.6 Gy ago), and that aqueous environments were widespread then. Here we test this hypothesis by examining the excavation process of hydrated minerals by impact events on Mars and analyzing the stability of phyllosilicates against the impact-induced thermal shock. To do so, we first compare the infrared spectra of thermally altered phyllosilicates with those of hydrated minerals known to occur in craters on Mars and then analyze the postshock temperatures reached during impact crater excavation. Our results show that phyllosilicates can resist the postshock temperatures almost everywhere in the crater, except under particular conditions in a central area in and near the point of impact. We conclude that most phyllosilicates detected inside impact craters on Mars are consistent with excavated preexisting sediments, supporting the hypothesis of a primeval and long-lasting global aqueous environment. When our analyses are applied to specific impact craters on Mars, we are able to identify both pre- and postimpact phyllosilicates, therefore extending the time of local phyllosilicate synthesis to post-Noachian times.

  5. Crater Topography on Titan: Implications for Landscape Evolution

    Science.gov (United States)

    Neish, Catherine D.; Kirk, R.L.; Lorenz, R. D.; Bray, V. J.; Schenk, P.; Stiles, B. W.; Turtle, E.; Mitchell, K.; Hayes, A.

    2013-01-01

    We present a comprehensive review of available crater topography measurements for Saturn's moon Titan. In general, the depths of Titan's craters are within the range of depths observed for similarly sized fresh craters on Ganymede, but several hundreds of meters shallower than Ganymede's average depth vs. diameter trend. Depth-to-diameter ratios are between 0.0012 +/- 0.0003 (for the largest crater studied, Menrva, D approximately 425 km) and 0.017 +/- 0.004 (for the smallest crater studied, Ksa, D approximately 39 km). When we evaluate the Anderson-Darling goodness-of-fit parameter, we find that there is less than a 10% probability that Titan's craters have a current depth distribution that is consistent with the depth distribution of fresh craters on Ganymede. There is, however, a much higher probability that the relative depths are uniformly distributed between 0 (fresh) and 1 (completely infilled). This distribution is consistent with an infilling process that is relatively constant with time, such as aeolian deposition. Assuming that Ganymede represents a close 'airless' analogue to Titan, the difference in depths represents the first quantitative measure of the amount of modification that has shaped Titan's surface, the only body in the outer Solar System with extensive surface-atmosphere exchange.

  6. Crater topography on Titan: implications for landscape evolution

    Science.gov (United States)

    Neish, Catherine D.; Kirk, R.L.; Lorenz, R.D.; Bray, V.J.; Schenk, P.; Stiles, B.W.; Turtle, E.; Mitchell, Ken; Hayes, A.

    2013-01-01

    We present a comprehensive review of available crater topography measurements for Saturn’s moon Titan. In general, the depths of Titan’s craters are within the range of depths observed for similarly sized fresh craters on Ganymede, but several hundreds of meters shallower than Ganymede’s average depth vs. diameter trend. Depth-to-diameter ratios are between 0.0012 ± 0.0003 (for the largest crater studied, Menrva, D ~ 425 km) and 0.017 ± 0.004 (for the smallest crater studied, Ksa, D ~ 39 km). When we evaluate the Anderson–Darling goodness-of-fit parameter, we find that there is less than a 10% probability that Titan’s craters have a current depth distribution that is consistent with the depth distribution of fresh craters on Ganymede. There is, however, a much higher probability that the relative depths are uniformly distributed between 0 (fresh) and 1 (completely infilled). This distribution is consistent with an infilling process that is relatively constant with time, such as aeolian deposition. Assuming that Ganymede represents a close ‘airless’ analogue to Titan, the difference in depths represents the first quantitative measure of the amount of modification that has shaped Titan’s surface, the only body in the outer Solar System with extensive surface–atmosphere exchange.

  7. The Morphology of Craters on Mercury: Results from MESSENGER Flybys

    Science.gov (United States)

    Barnouin, Oliver S.; Zuber, Maria T.; Smith, David E.; Neumann, Gregory A.; Herrick, Robert R.; Chappelow, John E.; Murchie, Scott L.; Prockter, Louise M.

    2012-01-01

    Topographic data measured from the Mercury Laser Altimeter (MLA) and the Mercury Dual Imaging System (MDIS) aboard the MESSENGER spacecraft were used for investigations of the relationship between depth and diameter for impact craters on Mercury. Results using data from the MESSENGER flybys of the innermost planet indicate that most of the craters measured with MLA are shallower than those previously measured by using Mariner 10 images. MDIS images of these same MLA-measured craters show that they have been modified. The use of shadow measurement techniques, which were found to be accurate relative to the MLA results, indicate that both small bowl-shaped and large complex craters that are fresh possess depth-to-diameter ratios that are in good agreement with those measured from Mariner 10 images. The preliminary data also show that the depths of modified craters are shallower relative to fresh ones, and might provide quantitative estimates of crater in-filling by subsequent volcanic or impact processes. The diameter that defines the transition from simple to complex craters on Mercury based on MESSENGER data is consistent with that reported from Mariner 10 data.

  8. Slope activity in Gale crater, Mars

    Science.gov (United States)

    Dundas, Colin M.; McEwen, Alfred S.

    2015-01-01

    High-resolution repeat imaging of Aeolis Mons, the central mound in Gale crater, reveals active slope processes within tens of kilometers of the Curiosity rover. At one location near the base of northeastern Aeolis Mons, dozens of transient narrow lineae were observed, resembling features (Recurring Slope Lineae) that are potentially due to liquid water. However, the lineae faded and have not recurred in subsequent Mars years. Other small-scale slope activity is common, but has different spatial and temporal characteristics. We have not identified confirmed RSL, which Rummel et al. (Rummel, J.D. et al. [2014]. Astrobiology 14, 887–968) recommended be treated as potential special regions for planetary protection. Repeat images acquired as Curiosity approaches the base of Aeolis Mons could detect changes due to active slope processes, which could enable the rover to examine recently exposed material.

  9. Martian Fluvial Conglomerates at Gale Crater

    Science.gov (United States)

    Williams, R. M. E.; Grotzinger, J. P.; Dietrich, W. E.; Gupta, S.; Sumner, D. Y.; Wiens, R. C.; Mangold, N.; Malin, M. C.; Edgett, K. S.; Maurice, S.; Forni, O.; Gasnault, O.; Ollila, A.; Newsom, H. E.; Dromart, G.; Palucis, M. C.; Yingst, R. A.; Anderson, R. B.; Herkenhoff, K. E.; Le Mouélic, S.; Goetz, W.; Madsen, M. B.; Koefoed, A.; Jensen, J. K.; Bridges, J. C.; Schwenzer, S. P.; Lewis, K. W.; Stack, K. M.; Rubin, D.; Kah, L. C.; Bell, J. F.; Farmer, J. D.; Sullivan, R.; Van Beek, T.; Blaney, D. L.; Pariser, O.; Deen, R. G.; Kemppinen, Osku; Bridges, Nathan; Johnson, Jeffrey R.; Minitti, Michelle; Cremers, David; Edgar, Lauren; Godber, Austin; Wadhwa, Meenakshi; Wellington, Danika; McEwan, Ian; Newman, Claire; Richardson, Mark; Charpentier, Antoine; Peret, Laurent; King, Penelope; Blank, Jennifer; Weigle, Gerald; Schmidt, Mariek; Li, Shuai; Milliken, Ralph; Robertson, Kevin; Sun, Vivian; Baker, Michael; Edwards, Christopher; Ehlmann, Bethany; Farley, Kenneth; Griffes, Jennifer; Miller, Hayden; Newcombe, Megan; Pilorget, Cedric; Rice, Melissa; Siebach, Kirsten; Stolper, Edward; Brunet, Claude; Hipkin, Victoria; Léveillé, Richard; Marchand, Geneviève; Sobrón Sánchez, Pablo; Favot, Laurent; Cody, George; Steele, Andrew; Flückiger, Lorenzo; Lees, David; Nefian, Ara; Martin, Mildred; Gailhanou, Marc; Westall, Frances; Israël, Guy; Agard, Christophe; Baroukh, Julien; Donny, Christophe; Gaboriaud, Alain; Guillemot, Philippe; Lafaille, Vivian; Lorigny, Eric; Paillet, Alexis; Pérez, René; Saccoccio, Muriel; Yana, Charles; Aparicio, Carlos Armiens; Caride Rodríguez, Javier; Carrasco Blázquez, Isaías; Gómez Gómez, Felipe; Elvira, Javier Gómez; Hettrich, Sebastian; Lepinette Malvitte, Alain; Marín Jiménez, Mercedes; Frías, Jesús Martínez; Soler, Javier Martín; Torres, F. Javier Martín; Molina Jurado, Antonio; Sotomayor, Luis Mora; Muñoz Caro, Guillermo; Navarro López, Sara; González, Verónica Peinado; García, Jorge Pla; Rodriguez Manfredi, José Antonio; Planelló, Julio José Romeral; Alejandra Sans Fuentes, Sara; Sebastian Martinez, Eduardo; Torres Redondo, Josefina; O'Callaghan, Roser Urqui; Zorzano Mier, María-Paz; Chipera, Steve; Lacour, Jean-Luc; Mauchien, Patrick; Sirven, Jean-Baptiste; Manning, Heidi; Fairén, Alberto; Hayes, Alexander; Joseph, Jonathan; Squyres, Steven; Thomas, Peter; Dupont, Audrey; Lundberg, Angela; Melikechi, Noureddine; Mezzacappa, Alissa; DeMarines, Julia; Grinspoon, David; Reitz, Günther; Prats, Benito; Atlaskin, Evgeny; Genzer, Maria; Harri, Ari-Matti; Haukka, Harri; Kahanpää, Henrik; Kauhanen, Janne; Paton, Mark; Polkko, Jouni; Schmidt, Walter; Siili, Tero; Fabre, Cécile; Wray, James; Wilhelm, Mary Beth; Poitrasson, Franck; Patel, Kiran; Gorevan, Stephen; Indyk, Stephen; Paulsen, Gale; Bish, David; Schieber, Juergen; Gondet, Brigitte; Langevin, Yves; Geffroy, Claude; Baratoux, David; Berger, Gilles; Cros, Alain; Uston, Claude d.; Lasue, Jérémie; Lee, Qiu-Mei; Meslin, Pierre-Yves; Pallier, Etienne; Parot, Yann; Pinet, Patrick; Schröder, Susanne; Toplis, Mike; Lewin, Éric; Brunner, Will; Heydari, Ezat; Achilles, Cherie; Oehler, Dorothy; Sutter, Brad; Cabane, Michel; Coscia, David; Szopa, Cyril; Robert, François; Sautter, Violaine; Nachon, Marion; Buch, Arnaud; Stalport, Fabien; Coll, Patrice; François, Pascaline; Raulin, François; Teinturier, Samuel; Cameron, James; Clegg, Sam; Cousin, Agnès; DeLapp, Dorothea; Dingler, Robert; Jackson, Ryan Steele; Johnstone, Stephen; Lanza, Nina; Little, Cynthia; Nelson, Tony; Williams, Richard B.; Jones, Andrea; Kirkland, Laurel; Treiman, Allan; Baker, Burt; Cantor, Bruce; Caplinger, Michael; Davis, Scott; Duston, Brian; Fay, Donald; Hardgrove, Craig; Harker, David; Herrera, Paul; Jensen, Elsa; Kennedy, Megan R.; Krezoski, Gillian; Krysak, Daniel; Lipkaman, Leslie; McCartney, Elaina; McNair, Sean; Nixon, Brian; Posiolova, Liliya; Ravine, Michael; Salamon, Andrew; Saper, Lee; Stoiber, Kevin; Supulver, Kimberley; Van Beek, Jason; Zimdar, Robert; French, Katherine Louise; Iagnemma, Karl; Miller, Kristen; Summons, Roger; Goesmann, Fred; Hviid, Stubbe; Johnson, Micah; Lefavor, Matthew; Lyness, Eric; Breves, Elly; Dyar, M. Darby; Fassett, Caleb; Blake, David F.; Bristow, Thomas; DesMarais, David; Edwards, Laurence; Haberle, Robert; Hoehler, Tori; Hollingsworth, Jeff; Kahre, Melinda; Keely, Leslie; McKay, Christopher; Bleacher, Lora; Brinckerhoff, William; Choi, David; Conrad, Pamela; Dworkin, Jason P.; Eigenbrode, Jennifer; Floyd, Melissa; Freissinet, Caroline; Garvin, James; Glavin, Daniel; Harpold, Daniel; Mahaffy, Paul; Martin, David K.; McAdam, Amy; Pavlov, Alexander; Raaen, Eric; Smith, Michael D.; Stern, Jennifer; Tan, Florence; Trainer, Melissa; Meyer, Michael; Posner, Arik; Voytek, Mary; Anderson, Robert C.; Aubrey, Andrew; Beegle, Luther W.; Behar, Alberto; Brinza, David; Calef, Fred; Christensen, Lance; Crisp, Joy A.; DeFlores, Lauren; Feldman, Jason; Feldman, Sabrina; Flesch, Gregory; Hurowitz, Joel; Jun, Insoo; Keymeulen, Didier; Maki, Justin; Mischna, Michael; Morookian, John Michael; Parker, Timothy; Pavri, Betina; Schoppers, Marcel; Sengstacken, Aaron; Simmonds, John J.; Spanovich, Nicole; de la Torre Juarez, Manuel; Vasavada, Ashwin R.; Webster, Christopher R.; Yen, Albert; Archer, Paul Douglas; Cucinotta, Francis; Jones, John H.; Ming, Douglas; Morris, Richard V.; Niles, Paul; Rampe, Elizabeth; Nolan, Thomas; Fisk, Martin; Radziemski, Leon; Barraclough, Bruce; Bender, Steve; Berman, Daniel; Dobrea, Eldar Noe; Tokar, Robert; Vaniman, David; Leshin, Laurie; Cleghorn, Timothy; Huntress, Wesley; Manhès, Gérard; Hudgins, Judy; Olson, Timothy; Stewart, Noel; Sarrazin, Philippe; Grant, John; Vicenzi, Edward; Wilson, Sharon A.; Bullock, Mark; Ehresmann, Bent; Hamilton, Victoria; Hassler, Donald; Peterson, Joseph; Rafkin, Scot; Zeitlin, Cary; Fedosov, Fedor; Golovin, Dmitry; Karpushkina, Natalya; Kozyrev, Alexander; Litvak, Maxim; Malakhov, Alexey; Mitrofanov, Igor; Mokrousov, Maxim; Nikiforov, Sergey; Prokhorov, Vasily; Sanin, Anton; Tretyakov, Vladislav; Varenikov, Alexey; Vostrukhin, Andrey; Kuzmin, Ruslan; Clark, Benton; Wolff, Michael; McLennan, Scott; Botta, Oliver; Drake, Darrell; Bean, Keri; Lemmon, Mark; Lee, Ella Mae; Sucharski, Robert; Hernández, Miguel Ángel de Pablo; Blanco Ávalos, Juan José; Ramos, Miguel; Kim, Myung-Hee; Malespin, Charles; Plante, Ianik; Muller, Jan-Peter; González, Rafael Navarro; Ewing, Ryan; Boynton, William; Downs, Robert; Fitzgibbon, Mike; Harshman, Karl; Morrison, Shaunna; Kortmann, Onno; Williams, Amy; Lugmair, Günter; Wilson, Michael A.; Jakosky, Bruce; Zunic, Tonci Balic; Frydenvang, Jens; Kinch, Kjartan; Stipp, Susan Louise Svane; Boyd, Nick; Campbell, John L.; Gellert, Ralf; Perrett, Glynis; Pradler, Irina; VanBommel, Scott; Jacob, Samantha; Owen, Tobias; Rowland, Scott; Savijärvi, Hannu; Boehm, Eckart; Böttcher, Stephan; Burmeister, Sönke; Guo, Jingnan; Köhler, Jan; García, César Martín; Mellin, Reinhold Mueller; Schweingruber, Robert Wimmer; McConnochie, Timothy; Benna, Mehdi; Franz, Heather; Bower, Hannah; Brunner, Anna; Blau, Hannah; Boucher, Thomas; Carmosino, Marco; Atreya, Sushil; Elliott, Harvey; Halleaux, Douglas; Rennó, Nilton; Wong, Michael; Pepin, Robert; Elliott, Beverley; Spray, John; Thompson, Lucy; Gordon, Suzanne; Williams, Joshua; Vasconcelos, Paulo; Bentz, Jennifer; Nealson, Kenneth; Popa, Radu; Moersch, Jeffrey; Tate, Christopher; Day, Mackenzie; Kocurek, Gary; Hallet, Bernard; Sletten, Ronald; Francis, Raymond; McCullough, Emily; Cloutis, Ed; ten Kate, Inge Loes; Arvidson, Raymond; Fraeman, Abigail; Scholes, Daniel; Slavney, Susan; Stein, Thomas; Ward, Jennifer; Berger, Jeffrey; Moores, John E.

    2013-05-01

    Observations by the Mars Science Laboratory Mast Camera (Mastcam) in Gale crater reveal isolated outcrops of cemented pebbles (2 to 40 millimeters in diameter) and sand grains with textures typical of fluvial sedimentary conglomerates. Rounded pebbles in the conglomerates indicate substantial fluvial abrasion. ChemCam emission spectra at one outcrop show a predominantly feldspathic composition, consistent with minimal aqueous alteration of sediments. Sediment was mobilized in ancient water flows that likely exceeded the threshold conditions (depth 0.03 to 0.9 meter, average velocity 0.20 to 0.75 meter per second) required to transport the pebbles. Climate conditions at the time sediment was transported must have differed substantially from the cold, hyper-arid modern environment to permit aqueous flows across several kilometers.

  10. Self-sacrificial behavior and its explanation in terms of Max Scheler's concept of spirit.

    Science.gov (United States)

    Alyushin, Alexey

    2014-12-01

    One of the key concepts of the German philosopher Max Scheler (1874-1928) is his concept of spirit. He understands spirit as one of several naturally functioning human mental agencies, such as consciousness, will, memory, etc. That is, he treats the mental agency of spirit in a scientific way and avoids any esoteric or religious connotations that this peculiar term may involve. The nature of human spirit, according to Scheler, is the ability to withstand and deliberately redirect biological imperatives and instinctive drives, up to the point of purposefully throwing away one's own life. The presence of spirit constitutes the essence of the human being that differentiates him qualitatively from all animals. In this article, I argue that it is human spirit that plays the determinative role in causing heroic and self-sacrificial behavior. I also argue that the individual human spirit experiences its inherent development, thus having several rather dissimilar stages and manifestations. I discuss the meaning that the term 'spirit' has in the English and the American philosophical and psychological traditions and the meaning of the corresponding term 'der Geist' in the German traditions. The specific English-language understanding of the term 'spirit', compared to its German counterpart 'der Geist', namely, less scientific and more religious and esoteric and metaphorical for the former, makes it alien and almost unusable in the English and American traditions. The linguistic difference leads to the misunderstanding of some very important ideas brought by the concept of spirit as introduced by Scheler. My purpose is to overcome this discrepancy and omission and to introduce the notion and the concept of spirit, in their scientific understanding, into the arsenal of modern English-language cognitive science, psychology, and philosophy in order to provide for the full explanatory force of the hitherto neglected concept of spirit.

  11. Rock spatial densities on the rims of the Tycho secondary craters in Mare Nectaris

    Science.gov (United States)

    Basilevsky, A. T.; Michael, G. G.; Kozlova, N. A.

    2018-04-01

    The aim of this work is to check whether the technique of estimation of age of small lunar craters based on spatial density of rock boulders on their rims described in Basilevsky et al. (2013, 2015b) and Li et al. (2017) for the craters work presents the rock counts on the rims of four craters having diameters 1000, 1100, 1240 and 1400 m located in Mare Nectaris. These craters are secondaries of the primary crater Tycho, whose age was found to be 109 ± 4 Ma (Stoffler and Ryder, 2001) so this may be taken as the age of the four craters, too. Using the dependence of the rock spatial densities at the crater rims on the crater age for the case of mare craters (Li et al., 2017) our measured rock densities correspond to ages from ∼100 to 130 Ma. These estimates are reasonably close to the given age of the primary crater Tycho. This, in turn, suggests that this technique of crater age estimation is applicable to craters up to ∼1.5 km in diameter. For the four considered craters we also measured their depth/diameter ratios and the maximum angles of the crater inner slopes. For the considered craters it was found that with increasing crater diameter, the depth/diameter ratios and maximum angles of internal slopes increase, but the values of these parameters for specific craters may deviate significantly from the general trends. The deviations probably result from some dissimilarities in the primary crater geometries, that may be due to crater to crater differences in characteristics of impactors (e.g., in their bulk densities) and/or differences in the mechanical properties of the target. It may be possible to find secondaries of crater Tycho in the South pole area and, if so, they may be studied to check the specifics and rates of the rock boulder degradation in the lunar polar environment.

  12. Framing the policy debate over spirits excise tax in Poland.

    Science.gov (United States)

    Zatoński, Mateusz; Hawkins, Benjamin; McKee, Martin

    2016-12-23

    Industry lobbying remains an obstacle to effective health-oriented alcohol policy. In 2013, an increase in excise tax on spirits was announced by the Polish government. This article presents a qualitative analysis of the public debate that ensued on the potential economic, health and social effects of the policy. It focuses on how competing groups, including industry actors, framed their position and sought to dominate the debate. Online archives of five Polish national newspapers, two spirits trade associations, and parliamentary and ministerial archives were searched. A thematic content analysis of the identified sources was conducted. The overall findings were compared with existing research on the framing of the Minimum Unit Pricing (MUP) debate in the UK. A total of 155 sources were analysed. Two main frames were identified: health, and economic The spirits industry successfully promoted the economic frame in their own publications and in the media. The debate was dominated by arguments about potential growth of the grey market and losses in tax revenue that might result from the excise tax increase. The framing of the debate in Poland differed from the framing of the MUP debate in the United Kingdom. The Polish public health community was unsuccessful in making health considerations a significant element of the alcohol policy debate. The strategies pursued by UK health advocates offer lessons for how to make a more substantial impact on media coverage and promote health-oriented legislation. © The Author 2016. Published by Oxford University Press. All rights reserved. For Permissions, please email: journals.permissions@oup.com.

  13. Using panel data to determine the effect of advertising on brand-level distilled spirits sales.

    Science.gov (United States)

    Gius, M P

    1996-01-01

    The purpose of the present study is to determine the effect that brand-level advertising has on brand-level spirits demand. Using a panel data set consisting of 16 brands and 14 years of data, a fixed effects model of brand-level spirits demand was estimated. It was found that own-brand advertising, income, rival-brand price, a time trend and brand loyalty all have a significant effect on brand-level spirits demand. These results indicate that brand-level spirits advertising results only in brand switching and does not increase the overall size of the market.

  14. Gathering and Dispersing: The Absolute Spirit in Hegel’s Philosophy

    Directory of Open Access Journals (Sweden)

    George Vassilacopoulos

    2007-12-01

    Full Text Available This paper explores the meaning and being of the absolute spirit in Hegelrsquo;s thought by reflecting through the idea that spirit is the activity and being of gathering through dispersal. In Hegelrsquo;s thought gathering and dispersing are the primary movements through which spirit engages in the processes of its absolute self-cognition, the processes, that is, that underpin the eternal becoming of communal being. Gathering and dispersing thus define the pulsating movement of the absolute spirit in all its facets

  15. Curiosity's field site in Gale Crater, Mars, in context

    Science.gov (United States)

    Edgett, K. S.; Malin, M. C.

    2011-12-01

    NASA's Mars rover, Curiosity, is anticipated to land in Gale Crater in August 2012. Gale is a 155 km-diameter impact crater adjacent to the ancient crustal "north-south dichotomy boundary." It contains a mound of layered rock (of yet-unknown proportions of clastic sediment, tephra, and chemical precipitates) ˜5 km-high that was eroded by fluvial, eolian, and mass-movement processes. The stratigraphy includes erosional unconformities representing periods when new impact craters formed and streams cut canyons into layered rock. The majority of known impact sites on Earth are craters that were filled and buried in sediment; examples occur under the Chesapeake Bay and beneath the Chicago O'Hare Airport. The upper crust of Mars, with its relative lack of tectonism, is almost entirely a layered, cratered volume of filled, buried, and complexly-interbedded craters and fluvial systems. Some of these have been exhumed or partly exhumed; some, like Gale, were once filled with extensive rock layers that were eroded to form mounds or mesas. Landforms all across Arabia Terra show that similar materials were also deposited between craters. Gale is of the family of Mars craters that were filled and buried (or nearly so). The highest elevation on the Gale mound exceeds the crater's north rim by ˜2 km and is within 500 m of the highest point on the south rim. Many similar craters occur in Arabia Terra; these are instructive as some contain mounds, others have mesas or buttes or other erosional expressions. Craters within 10s to a few 100s of km of each other typically contain very different materials, as exhibited by varied erosional expression, bedding style, and layer thickness. This suggests that the depositional environments, sources, and physical properties of the deposited material differed from place to place and time to time, even in neighboring settings. The Curiosity site in Gale has the potential to illuminate processes that acted locally and globally on early Mars. In

  16. Green waste from spirit; Gruener Abfall zu Sprit

    Energy Technology Data Exchange (ETDEWEB)

    Heida, Lydia

    2013-05-15

    Bio MCN (Almere, The Netherlands) has built the largest factory of the world for the production of bio-methanol. This factory produces 250 million liter methanol annually from natural gas, green gas (from the fermentation of sugar beet residues) and crude glycerol. Crude glycerol arises from the biodiesel production. As part of the Wood Spirit Project, Bio MCN constructs an additional plant that converts 750,000 tons of wood waste to 250 million liters of methanol. The waste wood is chipped and converted to biochar by means of torrefaction. Biochar is pulverized and converted to synthesis gas. This synthesis gas is converted to methanol by means of a chemical catalyst.

  17. [Study of alcohol-soluble lignin in cognac spirits].

    Science.gov (United States)

    Pisarnitskiĭ, A F; Askenderov, K A

    2008-01-01

    We studied the structure of alcohol-soluble lignin in cognac spirits from Spain (7-year aging) and Azerbaijan (15-year aging). Alcohol-soluble lignin was precipitated and refractionated by means of preparative high-performance liquid chromatography. Lignin was studied by the method of high-performance liquid chromatography and mass spectrometry. Lignin hydrolysis products were assayed by the method of gas-liquid chromatography and mass spectrometry. The structure of lignans was reconstructed from these fragments. Lignans from Spanish and Azeri alcohol were arbitrarily designated as sinapoconiferal triglycoside and glucoferulate flavone diglycoside, respectively.

  18. Project-Based Organizations and the New Spirit of Capitalism

    DEFF Research Database (Denmark)

    Jagd, Søren

    Luc Boltanski and Eve Chiapello’s analysis of recent changes in capitalism – Le nouvel esprit du capitalisme - is an important contribution to the sociological analysis of capitalism. The aim of this paper is to present their main argument. It is argued that a particular important aspect...... of their analysis is the ideal-typical model of the new spirit of capitalism, the ideological underpinning of project-based organizations in ‘The Project World’. It is argued that the ideal-typical model of the Project World is the most elaborated description of the ‘cultural code’ of the emergent form...

  19. Body, spirit and gender in Maria Komornicka’s poetry

    Directory of Open Access Journals (Sweden)

    Katarzyna Lisowska

    2011-06-01

    Full Text Available This paper concerns three significant concepts in Maria Komornicka’s writings: body, spirit and gender. The first two are closely related to each other, thus initial paragraphs are devoted to them both. On the basis of these reflections, I draw some conclusion about the image of gender created by the poet. The notion of gender is analysed in terms of Young Poland discourse of gender and from the perspective of modern methodologies: feminist criticism as well as gender and queer studies. This paper aims at encouraging the reader to reinterpret M. Komornicka’s output with contemporary awareness.

  20. Mothers and Spirits: Religious Identity, Alcohol, and Death

    Directory of Open Access Journals (Sweden)

    Candi K. Cann

    2016-07-01

    Full Text Available Mothers and Spirits examines the intersection of women, alcohol, and death through a comparative analysis. Offering a brief history of the study of drinking, followed by a short analysis of drinking in European and Chinese cultures, Cann examines two religious texts central to the roles of women and alcohol in Chinese religious thought and Christianity. Finally, Cann utilizes the historical and textual background to contextualize her ethnographic study of women, alcohol, and death in Mexican Catholicism, Chinese religions, and American Southern Baptist Christianity. Cann argues that both alcohol and temperance are used as a way to forge, cement, and create gender identity, constructing alternate discourses of power and inclusivity.

  1. Managerial Spirit from de Social Representations: Venezuelan case

    Directory of Open Access Journals (Sweden)

    Leslie Borjas de Xena

    2010-11-01

    Full Text Available This research seeks to characterize the central and peripheral structures of the Social Representations (SR on Entrepreneurial Spirit (ES. The SR are ways of social thinking that include information, beliefs, attitudes, practices and experiences. This type of research is complementary. The methodology called for the analysis of content found in secondary literature and in depth interviews. The corpus includes 65 articles in the 2006-2009 period. The results showed that the anchorage of the SR in the Venezuelan context could be characterized as “highly” entrepreneur

  2. Morphometry and Morphology of Fresh Craters on Titan

    Science.gov (United States)

    Kirk, R. L.; Wood, C. A.; Neish, C.; Lucas, A.; Hayes, A. G.; Cassini Radar Team

    2011-12-01

    Cassini RADAR imagery obtained on Titan flyby T77 revealed a 40-km diameter fresh impact crater at 11.6° N 44.6° W. This is only the 8th crater identified with high confidence (Wood et al., 2010, Icarus 206, 334), and the 3rd (after Sinlap D=79 km and Ksa D=30 km) for which the depth can be estimated by comparing the foreshortening of the near and far walls. This "autostereo" technique yields an estimated depth of 680 m. The T77 image forms a stereo pair with the T17 discovery image of Ksa from which we estimate the depth of Ksa at 750-800 m, in close agreement with SARTopo data. The depth of Sinlap is 760 m based on SARTopo. Depth-diameter ratios for these craters thus range from 0.01 to 0.025 and the depths are comparable to but 200-400 m shallower than fresh craters of the same size on Ganymede (Bray et al., 2008, Met. Planet Sci. 43, 1979). The depth differences could be explained by initial crater morphometry, by relaxation in a different thermal environment, or (perhaps most plausibly given the bland floors of even the freshest Titan craters) to sedimentary infill. In contrast, the 18x36 km elliptical depression at Sotra Facula is much deeper than Ganymede craters of similar size (d=1500 m from stereo), supporting the conclusion that it is not an impact crater. All three craters exhibit a relatively radar-bright annulus around the outer edge of the floor, possibly as the result of mass wasting of blocky materials from the crater walls. The central part of each crater is darker. The central darker floor of the new crater is symmetrical and featureless, whereas Ksa has a bright central ring 7 km in diameter. Stereo spot heights indicate the ring is 350±100 m above the outer floor. This height is in close agreement with the scaling for Ganymede crater central peaks from Bray et al. (2008). The darker floor area of Sinlap is substantially asymmetrical with a small bright central spot whose elevation is unknown. The new crater has continuous, radar

  3. Compound maar crater and co-eruptive scoria cone in the Lunar Crater Volcanic Field (Nevada, USA)

    Science.gov (United States)

    Amin, Jamal; Valentine, Greg A.

    2017-06-01

    Bea's Crater (Lunar Crater Volcanic Field, Nevada, USA) consists of two coalesced maar craters with diameters of 440 m and 1050 m, combined with a co-eruptive scoria cone that straddles the northeast rim of the larger crater. The two craters and the cone form an alignment that parallels many local and regional structures such as normal faults, and is interpreted to represent the orientation of the feeder dyke near the surface. The maar formed among a dense cluster of scoria cones; the cone-cluster topography resulted in crater rim that has a variable elevation. These older cones are composed of variably welded agglomerate and scoria with differing competence that subsequently affected the shape of Bea's Crater. Tephra ring deposits associated with phreatomagmatic maar-forming eruptions are rich in basaltic lithics derived from clasts, consistent with ejection from relatively shallow explosions although a diatreme might extend to deeper levels beneath the maar. Interbedding of deposits on the northeastern cone and in the tephra ring record variations in the magmatic volatile driven and phreatomagmatic eruption styles in both space and time along a feeder dike.

  4. Craters and basins on Ganymede and Callisto - Morphological indicators of crustal evolution

    Science.gov (United States)

    Passey, Q. R.; Shoemaker, E. M.

    The morphologic characteristics of craters and palimpsests on Ganymede and Callisto are surveyed, and the crustal properties of these satellites and the evolution of the properties are studied. The morphology of bowl-shaped craters, smooth-floored craters, craters without central peaks, craters with central pits, chain craters on Callisto, the Gilgamesh and Western Equatorial Basins on Ganymede, crater palimpsests and penepalimpsests, multiring structures on Callisto, and the Galileo Regio rimmed furrow system on Ganymede are described individually. The crustal evolution is addressed by examining the development of the Galileo Regio system, the distribution of crater retention ages, the record of ray clusters, the thermal history of the lithosphere of Ganymede, and the origin of the central pits. It is suggested that as the lithosphere of each satellite cooled and thickened, crater retentivity spread as a wave from the polar regions and the antapex toward the apex; at any given location, progressively larger craters were retained with the passage of time.

  5. Craters and basins on Ganymede and Callisto - Morphological indicators of crustal evolution

    Science.gov (United States)

    Passey, Q. R.; Shoemaker, E. M.

    1982-01-01

    The morphologic characteristics of craters and palimpsests on Ganymede and Callisto are surveyed, and the crustal properties of these satellites and the evolution of the properties are studied. The morphology of bowl-shaped craters, smooth-floored craters, craters without central peaks, craters with central pits, chain craters on Callisto, the Gilgamesh and Western Equatorial Basins on Ganymede, crater palimpsests and penepalimpsests, multiring structures on Callisto, and the Galileo Regio rimmed furrow system on Ganymede are described individually. The crustal evolution is addressed by examining the development of the Galileo Regio system, the distribution of crater retention ages, the record of ray clusters, the thermal history of the lithosphere of Ganymede, and the origin of the central pits. It is suggested that as the lithosphere of each satellite cooled and thickened, crater retentivity spread as a wave from the polar regions and the antapex toward the apex; at any given location, progressively larger craters were retained with the passage of time.

  6. Time for a Change; Spirit's View on Sol 1843 (Stereo)

    Science.gov (United States)

    2009-01-01

    [figure removed for brevity, see original site] Left-eye view of a color stereo pair for PIA11973 [figure removed for brevity, see original site] Right-eye view of a color stereo pair for PIA11973 NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this stereo, full-circle view of the rover's surroundings during the 1,843rd Martian day, or sol, of Spirit's surface mission (March 10, 2009). South is in the middle. North is at both ends. This view combines images from the left-eye and right-eye sides of the navigation camera. It appears three-dimensional when viewed through red-blue glasses with the red lens on the left. The rover had driven 36 centimeters downhill earlier on Sol 1854, but had not been able to get free of ruts in soft material that had become an obstacle to getting around the northeastern corner of the low plateau called 'Home Plate.' The Sol 1854 drive, following two others in the preceding four sols that also achieved little progress in the soft ground, prompted the rover team to switch to a plan of getting around Home Plate counterclockwise, instead of clockwise. The drive direction in subsequent sols was westward past the northern edge of Home Plate. This view is presented as a cylindrical-perspective projection with geometric seam correction.

  7. Time for a Change; Spirit's View on Sol 1843 (Vertical)

    Science.gov (United States)

    2009-01-01

    NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this full-circle view of the rover's surroundings during the 1,843rd Martian day, or sol, of Spirit's surface mission (March 10, 2009). South is in the middle. North is at both ends. This view is presented as a vertical projection with geometric seam correction. North is at the top. The rover had driven 36 centimeters downhill earlier on Sol 1854, but had not been able to get free of ruts in soft material that had become an obstacle to getting around the northeastern corner of the low plateau called 'Home Plate.' The Sol 1854 drive, following two others in the preceding four sols that also achieved little progress in the soft ground, prompted the rover team to switch to a plan of getting around Home Plate counterclockwise, instead of clockwise. The drive direction in subsequent sols was westward past the northern edge of Home Plate.

  8. Time for a Change; Spirit's View on Sol 1843 (Polar)

    Science.gov (United States)

    2009-01-01

    NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this full-circle view of the rover's surroundings during the 1,843rd Martian day, or sol, of Spirit's surface mission (March 10, 2009). South is in the middle. North is at both ends. This view is presented as a polar projection with geometric seam correction. North is at the top. The rover had driven 36 centimeters downhill earlier on Sol 1854, but had not been able to get free of ruts in soft material that had become an obstacle to getting around the northeastern corner of the low plateau called 'Home Plate.' The Sol 1854 drive, following two others in the preceding four sols that also achieved little progress in the soft ground, prompted the rover team to switch to a plan of getting around Home Plate counterclockwise, instead of clockwise. The drive direction in subsequent sols was westward past the northern edge of Home Plate.

  9. Sunset Crater Volcano National Monument : Acoustical Monitoring 2010

    Science.gov (United States)

    2013-05-01

    During the summer of 2010 (July - August), the Volpe Center collected baseline acoustical data at Sunset Crater Volcano National Monument (SUCR) at a site deployed for approximately 30 days. The baseline data collected during this period will help pa...

  10. Vegetation damage and recovery after Chiginagak Volcano Crater drainage event

    Data.gov (United States)

    Department of the Interior — From August 20 — 23, 2006, I revisited Chiginigak volcano to document vegetation recovery after the crater drainage event that severely damaged vegetation in May of...

  11. LRO MOON CRATER EDR RAWDATA VERSION 1.0

    Data.gov (United States)

    National Aeronautics and Space Administration — This data set comprises the raw binary data from from the LRO Cosmic Ray Telescope for the Effects of Radiation (CRaTER) instrument. The data consists of the...

  12. Are the Complex Algerian Meteoritic Craters Potential Hydrocarbon Traps?

    Science.gov (United States)

    Belhai, D.; Merle, O.; Vincent, P.; Afalfiz, A.; Devouard, B.

    2005-03-01

    The geological analysis of the meteoritic craters of Tin Bider and Ouarkziz (Sahara, Algeria) reveals identical characters to those of Ava and Viewfield. Their detailed study will make it possible to slice as for the presence or not ofhydrocarbons.

  13. Fractal Dimension of Geologically Constrained Crater Populations of Mercury

    Science.gov (United States)

    Mancinelli, Paolo; Pauselli, Cristina; Perugini, Diego; Lupattelli, Andrea; Federico, Costanzo

    2015-07-01

    Data gathered during the Mariner10 and MESSENGER missions are collated in this paper to classify craters into four geo-chronological units constrained to the geological map produced after MESSENGER's flybys. From the global catalogue, we classify craters, constraining them to the geological information derived from the map. We produce a size frequency distribution (SFD) finding that all crater classes show fractal behaviour: with the number of craters inversely proportional to their diameter, the exponent of the SFD (i.e., the fractal dimension of each class) shows a variation among classes. We discuss this observation as possibly being caused by endogenic and/or exogenic phenomena. Finally, we produce an interpretative scenario where, assuming a constant flux of impactors, the slope variation could be representative of rheological changes in the target materials.

  14. Mars Climate History: Insights From Impact Crater Wall Slope Statistics

    Science.gov (United States)

    Kreslavsky, Mikhail A.; Head, James W.

    2018-02-01

    We use the global distribution of the steepest slopes on crater walls derived from Mars Orbiter Laser Altimeter profile data to assess the magnitudes of degradational processes with latitude, altitude, and time. We independently confirm that Amazonian polar/high-latitude crater slope modification is substantial, but that craters in the low latitudes have essentially escaped significant slope modification since the Early Hesperian. We find that the total amount of crater wall degradation in the Late Noachian is very small in comparison to the circumpolar regions in the Late Amazonian, an observation that we interpret to mean that the Late Noachian climate was not characterized by persistent and continuous warm and wet conditions. A confirmed elevational zonality in degradation in the Early Hesperian is interpreted to mean that the atmosphere was denser than today.

  15. Planetary science: Meteor Crater formed by low-velocity impact.

    Science.gov (United States)

    Melosh, H J; Collins, G S

    2005-03-10

    Meteor Crater in Arizona was the first terrestrial structure to be widely recognized as a meteorite impact scar and has probably been more intensively studied than any other impact crater on Earth. We have discovered something surprising about its mode of formation--namely that the surface-impact velocity of the iron meteorite that created Meteor Crater was only about 12 km s(-1). This is close to the 9.4 km s(-1) minimum originally proposed but far short of the 15-20 km s(-1) that has been widely assumed--a realization that clears up a long-standing puzzle about why the crater does not contain large volumes of rock melted by the impact.

  16. Extreme Access & Lunar Ice Mining in Permanently Shadowed Craters

    Data.gov (United States)

    National Aeronautics and Space Administration — Results from the recent NASA Lunar CRater Observation and Sensing Satellite, or LCROSS, mission in 2010, indicate that water (H2O), ice and other useful volatiles...

  17. Realization of Best-in-Class Workflows Using Open Spirit Technology

    International Nuclear Information System (INIS)

    Hauser, K.

    2002-01-01

    Open Spirit is the realization of a long sought after dream to create an open systems approach to G and G computing. The focus is on developing a plug-and-play, platform independent, vendor neutral application framework to enable workflow optimization for the oil and gas industry. Through Open Spirit, Oil and gas clients can either develop or purchase Open Spirit enabled applications and combine those applications together to optimize a particular workflow. Currently Open Spirit supports GeoQuest's Geo Frame and Landmark's Open Works project data stores. There are three primary benefits to using Open Spirit enabled applications. Users of Open Spirit enabled applications can access data from a variety of data sources without having to move or reformat the data. This reduces the time to get the information into the appropriate application and eliminates the need to have multiple copies of the same data, simplifying data management efforts. Second, Open Spirit bridges the gap between Unix and PC applications. Through Open Spirit, any applications developed for the NT platform can access information residing in a Unix project data store. Third, Open Spirit supports the concept of a virtual project set. A user can combine any number project data stores (GeoFrame, Open Works, Finder, RECALL and PDS/Tigress) and use the combined project sets as if they were a single project. The data is not moved, but instead accessed dynamically through Open Spirit from the appropriate native data store. Open Spirit allows interpreters to develop their own Best-in-Class workflow and to mix and match the applications they determine to be the best of their interpretation teams independent of vendor

  18. Does price matter? The effect of decreased price on spirits consumption in Switzerland.

    Science.gov (United States)

    Kuo, Meichun; Heeb, Jean-Luc; Gmel, Gerhard; Rehm, Jürgen

    2003-04-01

    On July 1st, 1999, the spirits market in Switzerland was reformed based on the World Trade Organization (WTO) agreement. The tax reform, in addition to increased competition, has resulted in a 30-50% decrease in price for foreign spirits (liquor). The purpose of the present study is to examine whether decreased prices due to the tax reform and the liberalized spirits market in Switzerland have had an effect on spirits consumption, and whether the effect differs by demographic and other correlates. The present study uses data from a longitudinal study on changes in alcohol consumption in Switzerland's resident population. The baseline survey was conducted 3 months before the tax reform and the follow-up was conducted 28 months after the tax reform. A randomly selected sample of 4007 residents aged 15 years or older participated in the baseline survey and 73% in the follow-up survey. The data were obtained by computer-assisted telephone interview, including detailed questions on alcohol consumption, drinking habits, problem drinking, purchase of spirits and socio-demographic characteristics. Consumption of spirits increased after the price of spirits decreased. The increase in spirits consumption was consistent across subgroups, with the exception of the group aged 60 or older. Moreover, the increase in spirits consumption persisted even after adjustment for significant correlates of spirits consumption. Apart from age, there was no evidence that the increase in spirits consumption differed between subgroups as defined by sex, region, working status, education, smoking, drinking frequency, or average number of drinks. The findings demonstrate that younger people are more affected by price than older persons. This study demonstrated that price should be considered an effective policy to reduce alcohol misuse and alcohol-related problems, especially among the younger population.

  19. A global catalogue of Ceres impact craters ≥ 1 km and preliminary analysis

    Science.gov (United States)

    Gou, Sheng; Yue, Zongyu; Di, Kaichang; Liu, Zhaoqin

    2018-03-01

    The orbital data products of Ceres, including global LAMO image mosaic and global HAMO DTM with a resolution of 35 m/pixel and 135 m/pixel respectively, are utilized in this research to create a global catalogue of impact craters with diameter ≥ 1 km, and their morphometric parameters are calculated. Statistics shows: (1) There are 29,219 craters in the catalogue, and the craters have a various morphologies, e.g., polygonal crater, floor fractured crater, complex crater with central peak, etc.; (2) The identifiable smallest crater size is extended to 1 km and the crater numbers have been updated when compared with the crater catalogue (D ≥ 20 km) released by the Dawn Science Team; (3) The d/D ratios for fresh simple craters, obviously degraded simple crater and polygonal simple crater are 0.11 ± 0.04, 0.05 ± 0.04 and 0.14 ± 0.02 respectively. (4) The d/D ratios for non-polygonal complex crater and polygonal complex crater are 0.08 ± 0.04 and 0.09 ± 0.03. The global crater catalogue created in this work can be further applied to many other scientific researches, such as comparing d/D with other bodies, inferring subsurface properties, determining surface age, and estimating average erosion rate.

  20. The effects of in vitro exposure to white spirit on [Ca2+] in synaptosomes from rats exposed prenatally to white spirit

    DEFF Research Database (Denmark)

    Edelfors, S.; Hass, Ulla; Ravn-Jonsen, A.

    1999-01-01

    Female rats were exposed to white spirit (400 and 800 ppm for 6 hr/day) at day 7-20 during pregnancy. Thirty-five days after birth all female offspring were sacrificed, the brains removed, and the synaptosomal fractions prepared for in vitro studies. The cytosolic calcium concentration was measured...... using the FURA-2 technique. The results show that cytosolic calcium was increased in synaptosomes from rats exposed to white spirit prenatally compared to synaptosomes from unexposed rats. When synaptosomes were exposed to white spirit in vitro, the cytosolic calcium concentration changes were identical...... in all groups of rats. The membrane leakage measured as FURA-2 leakage from the synaptosomes identical in all three groups of animals. The results suggest that prenatal exposure to white spirit induces long-lasting and possibly irreversible changes in calcium homeostasis in the rat nervous system....

  1. Finite element models of non-Newtonian crater relaxation

    Science.gov (United States)

    Thomas, Paul J.; Schubert, Gerald

    1987-01-01

    The effects of a non-Newtonian rheology on the profiles of relaxing craters (such as those seen on the surfaces of the icy Galilean and Saturnian satellites) were studied. Two-dimensional finite element simulations of non-Newtonian viscous flow were performed, and the results were compared with those associated with Newtonian rheology. Viscous relaxation of craters in a non-Newtonian medium was significantly different from that in a Newtonian medium. Crater rims are observed to relax at a more rapid rate in a non-Newtonian region as a result of the movement of the low viscosity region to underneath the crater rim after the initial relaxation of the bowl. Significant differences are also found when central depth is plotted as a function of time. For a Newtonian medium, crater relaxation is exponential in form. In contrast, non-Newtonian crater relaxation is initially rapid, in response to the large initial stresses and small viscosities; however, as stresses decrease, this relaxation becomes extremely gradual.

  2. Morphological indicators of a mascon beneath Ceres' largest crater, Kerwan

    Science.gov (United States)

    Bland, Michael T.; Ermakov, Anton; Raymond, Carol A.; Williams, David A.; Bowling, Tim J.; Preusker, F.; Park, Ryan S.; Marchi, Simone; Castillo-Rogez, Julie C.; Fu, R.R.; Russell, Christopher T.

    2018-01-01

    Gravity data of Ceres returned by the National Aeronautics and Space Administration's Dawn spacecraft is consistent with a lower density crust of variable thickness overlying a higher density mantle. Crustal thickness variations can affect the long‐term, postimpact modification of impact craters on Ceres. Here we show that the unusual morphology of the 280 km diameter crater Kerwan may result from viscous relaxation in an outer layer that thins substantially beneath the crater floor. We propose that such a structure is consistent with either impact‐induced uplift of the high‐density mantle beneath the crater or from volatile loss during the impact event. In either case, the subsurface structure inferred from the crater morphology is superisostatic, and the mass excess would result in a positive Bouguer anomaly beneath the crater, consistent with the highest‐degree gravity data from Dawn. Ceres joins the Moon, Mars, and Mercury in having basin‐associated gravity anomalies, although their origin may differ substantially.

  3. Fractal dimensions of rampart impact craters on Mars

    Science.gov (United States)

    Ching, Delwyn; Taylor, G. Jeffrey; Mouginis-Mark, Peter; Bruno, Barbara C.

    1993-01-01

    Ejecta blanket morphologies of Martian rampart craters may yield important clues to the atmospheric densities during impact, and the nature of target materials (e.g., hard rock, fine-grained sediments, presence of volatiles). In general, the morphologies of such craters suggest emplacement by a fluidized, ground hugging flow instead of ballistic emplacement by dry ejecta. We have quantitatively characterized the shape of the margins of the ejecta blankets of 15 rampart craters using fractal geometry. Our preliminary results suggest that the craters are fractals and are self-similar over scales of approximately 0.1 km to 30 km. Fractal dimensions (a measure of the extent to which a line fills a plane) range from 1.06 to 1.31. No correlations of fractal dimension with target type, elevation, or crater size were observed, though the data base is small. The range in fractal dimension and lack of correlation may be due to a complex interplay of target properties (grain size, volatile content), atmospheric pressure, and crater size. The mere fact that the ejecta margins are fractals, however, indicates that viscosity and yield strength of the ejecta were at least as low as those of basalts, because silicic lava flows are not generally fractals.

  4. 100 New Impact Crater Sites Found on Mars

    Science.gov (United States)

    Kennedy, M. R.; Malin, M. C.

    2009-12-01

    Recent observations constrain the formation of 100 new impact sites on Mars over the past decade; 19 of these were found using the Mars Global Surveyor Mars Orbiter Camera (MOC), and the other 81 have been identified since 2006 using the Mars Reconnaissance Orbiter Context Camera (CTX). Every 6 meter/pixel CTX image is examined upon receipt and, where they overlap images of 0.3-240 m/pixel scale acquired by the same or other Mars-orbiting spacecraft, we look for features that may have changed. New impact sites are initially identified by the presence of a new dark spot or cluster of dark spots in a CTX image. Such spots may be new impact craters, or result from the effect of impact blasts on the dusty surface. In some (generally rare) cases, the crater is sufficiently large to be resolved in the CTX image. In most cases, however, the crater(s) cannot be seen. These are tentatively designated as “candidate” new impact sites, and the CTX team then creates an opportunity for the MRO spacecraft to point its cameras off-nadir and requests that the High Resolution Imaging Science Experiment (HiRISE) team obtain an image of ~0.3 m/pixel to confirm whether a crater or crater cluster is present. It is clear even from cursory examination that the CTX observations are areographically biased to dusty, higher albedo areas on Mars. All but 3 of the 100 new impact sites occur on surfaces with Lambert albedo values in excess of 23.5%. Our initial study of MOC images greatly benefited from the initial global observations made in one month in 1999, creating a baseline date from which we could start counting new craters. The global coverage by MRO Mars Color Imager is more than a factor of 4 poorer in resolution than the MOC Wide Angle camera and does not offer the opportunity for global analysis. Instead, we must rely on partial global coverage and global coverage that has taken years to accumulate; thus we can only treat impact rates statistically. We subdivide the total data

  5. 27 CFR 27.1 - Imported distilled spirits, wines, and beer.

    Science.gov (United States)

    2010-04-01

    ..., wines, and beer. 27.1 Section 27.1 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU, DEPARTMENT OF THE TREASURY LIQUORS IMPORTATION OF DISTILLED SPIRITS, WINES, AND BEER Scope of Regulations § 27.1 Imported distilled spirits, wines, and beer. This part, “Importation of...

  6. 78 FR 38628 - Reclassification of Specially Denatured Spirits and Completely Denatured Alcohol Formulas and...

    Science.gov (United States)

    2013-06-27

    ... generally determined at the time the distilled spirits are withdrawn from the bonded premises of a distilled... industry, or for fuel, light, or power, except that, under 26 U.S.C. 5273(b), denatured spirits may not be....D.S.'' for purposes of this preamble). C.D.A. jeopardizes the revenue less than S.D.S. does--first...

  7. 27 CFR 27.61 - Containers of distilled spirits to bear closures.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Containers of distilled spirits to bear closures. 27.61 Section 27.61 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO... spirits to bear closures. No person shall transport, buy, possess, or sell, or transfer any imported...

  8. 27 CFR 26.135 - Containers of distilled spirits to bear closures.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Containers of distilled spirits to bear closures. 26.135 Section 26.135 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO... to bear closures. Containers of 1 gallon (3.785 liters) or less of distilled spirits, upon which all...

  9. 27 CFR 27.48 - Imported distilled spirits, wines, and beer.

    Science.gov (United States)

    2010-04-01

    ... perfumes containing distilled spirits, and on wines and beer, are collected, accounted for, and deposited..., wines, and beer. 27.48 Section 27.48 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU, DEPARTMENT OF THE TREASURY LIQUORS IMPORTATION OF DISTILLED SPIRITS, WINES, AND BEER Tax...

  10. 27 CFR 19.502 - Withdrawal of spirits on production or filling gauge.

    Science.gov (United States)

    2010-04-01

    ... production or filling gauge. 19.502 Section 19.502 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO... Withdrawals General § 19.502 Withdrawal of spirits on production or filling gauge. When the production or filling gauge is made under the provisions of § 19.319(b), spirits may be withdrawn from bonded premises...

  11. 27 CFR 19.682 - Receipt and gauge of returned taxpaid spirits.

    Science.gov (United States)

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Receipt and gauge of... Bonded Premises and Voluntary Destruction Returns § 19.682 Receipt and gauge of returned taxpaid spirits... bonded premises shall be immediately dumped. (b) Gauge. Spirits returned under § 19.681 shall be gauged...

  12. 27 CFR 30.52 - Procedure for measurement of cased spirits.

    Science.gov (United States)

    2010-04-01

    ... spirits in cases shall be determined by multiplying the wine gallons by the proof (divided by 100). (Sec... spirits in a case is to be determined by volume, such determination shall be made by ascertaining the contents of one bottle in the case and multiplying that figure by the number of bottles in the case. For...

  13. 27 CFR 19.990 - Redistillation of spirits or fuel alcohol received on the plant premises.

    Science.gov (United States)

    2010-04-01

    ... or fuel alcohol received on the plant premises. 19.990 Section 19.990 Alcohol, Tobacco Products and... PLANTS Distilled Spirits For Fuel Use Redistillation § 19.990 Redistillation of spirits or fuel alcohol received on the plant premises. (a) Receipts for redistillation. Proprietors of alcohol fuel plants may...

  14. 19 CFR 11.6 - Distilled spirits, wines, and malt liquors in bulk.

    Science.gov (United States)

    2010-04-01

    ... 19 Customs Duties 1 2010-04-01 2010-04-01 false Distilled spirits, wines, and malt liquors in bulk..., and malt liquors in bulk. (a) The port director, in his discretion, may require marks, brands, stamps... conveying imported distilled spirits, wines, and malt liquors, in accordance with 19 U.S.C. 467. (b) Marks...

  15. 27 CFR 19.397 - Spirits not originally intended for export.

    Science.gov (United States)

    2010-04-01

    ..., originally intended for domestic use may be exported with benefit of drawback or without payment of tax if... intended for export. 19.397 Section 19.397 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX....397 Spirits not originally intended for export. Spirits manufactured, produced, bottled in bottles...

  16. 27 CFR 28.197 - Return of spirits withdrawn for export with benefit of drawback.

    Science.gov (United States)

    2010-04-01

    ... withdrawn for export with benefit of drawback. 28.197 Section 28.197 Alcohol, Tobacco Products and Firearms... spirits withdrawn for export with benefit of drawback. When notice is filed by an exporter as provided in... export with benefit of drawback as provided in § 28.171, but which spirits have not been laden for export...

  17. Effect of gamma-radiation on sugar cane spirit

    International Nuclear Information System (INIS)

    Souza, Maria Djiliah Camargo Alvarenga de

    2000-01-01

    Irradiation has appeared as an alternative technique in food preservation. Besides cold decontamination irradiation can increase the quality of the food through the improvement of technological properties. For alcoholic beverages ionizing radiation has been applied to wines, whiskeys and beers in countries such as Thailand and China. In those cases, the purpose of the technique was to accelerate aging, to improve the sensory characteristics and as sterilization treatment. The aim of this work was to study the effect of gamma radiation on the quality of sugar cane spirit by gas chromatography analysis of volatile compounds and sensory analysis. The sugar cane spirit newly distilled samples and commercial samples from different states (SP, CE and RJ) were irradiated either in glass or oak cask (Quercus alba sp) in a 60 Co Gammacell 220 at dose rate of 7.7 kGy/h and total doses of 0; 0.1; 2; 5 and 10 kGy. The analytical determination of esters, acetaldehyde and higher alcohols were performed in a gas chromatograph with flame ionization detector employing a Megabore CG-745 column. The alcoholic graduation was measured in a Gay-Lussac alcohometer and the pH was determined using an Analyser 300 pHmeter. The color change was measured by the absorbance at 420 nm in a Shimadzu UV 1601 spectrophotometer. The acceptance tests related to odor, taste, global impression and color were analyzed using Tukey average tests (p ≤0,05), ANOVA and histograms of panelists' scores frequency. A correlation between acetaldeyde, esters, higher alcohols levels and radiation dose was found in the sugar cane spirit newly distilled samples irradiated in oak cask and commercial samples. An increase in methanol concentration was verified, although remaining enough below the permissible limit accepted by the Brazilian Legislation. A decrease in the alcoholic graduation and pH in the irradiated samples was observed. A slight discoloration in the irradiated samples was verified. According to ANOVA

  18. Neurological effects of white spirit: Contribution of animal studies during a 30-year period

    DEFF Research Database (Denmark)

    Nielsen, Gunnar Damgård; Lund, Søren Peter; Ladefoged, Ole

    2006-01-01

    , but the neurophysiological tests showed adverse effects at this level. Fourth, neurophysiological methods may be more sensitive than histopathological, neurobehavioural and neurochemical methods. Overall, white spirit with a high and a low content of aromatics showed no overt difference in long-term effects in animals......Numerous studies have suggested that long-term occupational exposure to white spirit may cause chronic toxic encephalopathy (WHO 1996). This review summarizes the chronic nervous system effects of white spirit in animal studies during a 30-year period. First, routine histopathology was consistently...... unable to reveal adverse peripheral or central nervous system effects after inhalation of white spirit. Second, neurobehavioural studies in animals showed no adverse effect after inhalation of white spirit with a high content of aromatics in contrast to what was found with products with a low content...

  19. Lappajarvi Meteorite Crater, Western Finland: Structure, Stratigraphy and Geochemistry

    Science.gov (United States)

    Pipping, F.

    1992-07-01

    Research drill holes drilled in the 23 km diameter Lappajarvi Late Cretaceous meteorite impact crater give new information as to the structure, stratigraphy, and geochemistry of the impact formation in the crater (Pipping & Lehtinen, 1992). In one drill hole the sheet of glassy melt rock is 145 m thick and is underlain by 30 m of suevitic rock, followed by loose breccias down to 209 m where the hole ends. In a nearby hole 65 m of suevitic breccia was penetrated, underlain by a fine-grained allochthonous breccia to 160 m, followed by an autochthonous coarse breccia cut by suevitic dikes down to 275 m where the hole ends. A third hole was bored close to the crater rim. Topmost is 75 m of Quaternary glacial tills. After an erosional boundary follows 20 m of Mesoproterozoic (ca. 1200 Ma) sandy-silty sediments. These are underlain--with a tectonic boundary--by an autochthonous saprolite crust of about 40 m thickness. The hole ended in fresh mica schist--no signs of shock metamorphism--at 165 m. The structure typical for large impact craters was thus confirmed, i.e. an annular trough inside the rim of the crater, filled with rocks older than the impact. The stratigraphy of the crater fill is: lowermost autochthonous breccias followed by allochthonous breccias and suevitic breccias, with a melt rock cap covering a part of the crater fill. The general stratigraphy is: Palaeoproterozoic mica schists (1900 Ma), Mesoproterozoic saprolite (1400 Ma) in peneplanated schists, Neoproterozoic sediments (1200 Ma), Late Cretaceous crater (77 Ma, Jessberger & Reimold,1980) with a fill of impact rocks, Quaternary glaciation and sedimentation, and last, recent lake sedimentation. Impact rock geochemistry gives conclusive proof of an origin by meteorite impact. Conspicuous is the threefold Ni-content of the melt rock compared with the target rock, and the two-to-tenfold content of the Pt-metals in the melt rocks and suevites, compared with the target schists. Increased levels of K and Se

  20. The Lord of the Rings - Deep Learning Craters on the Moon and Other Bodies

    Science.gov (United States)

    Silburt, Ari; Ali-Dib, Mohamad; Zhu, Chenchong; Jackson, Alan; Valencia, Diana; Kissin, Yevgeni; Tamayo, Daniel; Menou, Kristen

    2018-01-01

    Crater detection has traditionally been done via manual inspection of images, leading to statistically significant disagreements between scientists for the Moon's crater distribution. In addition, there are millions of uncategorized craters on the Moon and other Solar System bodies that will never be classified by humans due to the time required to manually detect craters. I will show that a deep learning model trained on the near-side of the Moon can successfully reproduce the crater distribution on the far-side, as well as detect thousands of small, new craters that were previously uncharacterized. In addition, this Moon-trained model can be transferred to accurately classify craters on Mercury. It is therefore likely that this model can be extended to classify craters on all Solar System bodies with Digital Elevation Maps. This will facilitate, for the first time ever, a systematic, accurate, and reproducible study of the crater records throughout the Solar System.

  1. Planetary boundary layer and circulation dynamics at Gale Crater, Mars

    Science.gov (United States)

    Fonseca, Ricardo M.; Zorzano-Mier, María-Paz; Martín-Torres, Javier

    2018-03-01

    The Mars implementation of the Planet Weather Research and Forecasting (PlanetWRF) model, MarsWRF, is used here to simulate the atmospheric conditions at Gale Crater for different seasons during a period coincident with the Curiosity rover operations. The model is first evaluated with the existing single-point observations from the Rover Environmental Monitoring Station (REMS), and is then used to provide a larger scale interpretation of these unique measurements as well as to give complementary information where there are gaps in the measurements. The variability of the planetary boundary layer depth may be a driver of the changes in the local dust and trace gas content within the crater. Our results show that the average time when the PBL height is deeper than the crater rim increases and decreases with the same rate and pattern as Curiosity's observations of the line-of-sight of dust within the crater and that the season when maximal (minimal) mixing is produced is Ls 225°-315° (Ls 90°-110°). Thus the diurnal and seasonal variability of the PBL depth seems to be the driver of the changes in the local dust content within the crater. A comparison with the available methane measurements suggests that changes in the PBL depth may also be one of the factors that accounts for the observed variability, with the model results pointing towards a local source to the north of the MSL site. The interaction between regional and local flows at Gale Crater is also investigated assuming that the meridional wind, the dynamically important component of the horizontal wind at Gale, anomalies with respect to the daily mean can be approximated by a sinusoidal function as they typically oscillate between positive (south to north) and negative (north to south) values that correspond to upslope/downslope or downslope/upslope regimes along the crater rim and Mount Sharp slopes and the dichotomy boundary. The smallest magnitudes are found in the northern crater floor in a region that

  2. Earth in the balance - ecology and the human spirit

    Energy Technology Data Exchange (ETDEWEB)

    Gore, A.

    1992-01-01

    This book by Senator Albert Gore presents a global prospective on the environmental crisis facing the Earth. The chapters are framed in the twin ideas of the threat posed by human civilization to the global environment and the threat to human civilization posed by changes in the global environment. Gore first looks at evidence of risk in the environment: historical aspects of climate and civilization; ozone layer; water; land use; food supply; waste disposal. In Part II different aspects of our current approaches to the environment are described: politics; economics; technology; social problems; environmentalism of the human spirit. Finally in Part III, Gore presents his approach to the global environmental crisis, first presenting a section about a global sense of responsibility and purpose and then describing his ideas for A Global Marshal Plan. 169 refs., 4 figs.

  3. Book Review: Gift & Giver: The Holy Spirit for Today

    Directory of Open Access Journals (Sweden)

    John Paul Lathrop

    2017-05-01

    Full Text Available Dr. Craig Keener has established himself as a highly respected New Testament scholar. Over the years he has written a number of very significant commentaries including works on the gospels of Matthew and John, and the book of Acts. His highly acclaimed IVP Bible Background Commentary: New Testament is one of his best known works. In addition, he has produced books devoted to specific biblical topics such as miracles, women in marriage and ministry, and divorce and remarriage. He is not one to shy away from controversial subjects. In this present volume Keener writes about the Holy Spirit including the sometimes controversial charismatic aspects of His ministry. Gift & Giver was first published in theUnited States in 2001. More recently it has been translated into Indonesian and published inIndonesia.

  4. Behavioural characteristics of adulterated Premium Motor Spirit (PMS

    Directory of Open Access Journals (Sweden)

    M.C. Onojake

    2012-12-01

    Full Text Available Distillation profiles and chemical characteristics of ten suspected adulterated Premium Motor Spirit samples randomly collected from different dispensing points were analysed to determine the chemical characteristics of these samples when compared to a reference sample that is not adulterated. Results of the analyses show, Research Octane Number values ranged from 60.10 to 93.30, specific gravity ranged from 0.75 to 0.79, Reid Vapour Pressure ranged from 0.28 kgf/cm2 to 0.60 kgf/cm2 while Atmospheric distillation ranged from 189 to 251 °C. The results of this research reveal that most of the products are highly adulterated and may pose problems when sent to the market for intended end users.

  5. Earth in the balance - ecology and the human spirit

    International Nuclear Information System (INIS)

    Gore, A.

    1992-01-01

    This book by Senator Albert Gore presents a global prospective on the environmental crisis facing the Earth. The chapters are framed in the twin ideas of the threat posed by human civilization to the global environment and the threat to human civilization posed by changes in the global environment. Gore first looks at evidence of risk in the environment: historical aspects of climate and civilization; ozone layer; water; land use; food supply; waste disposal. In Part II different aspects of our current approaches to the environment are described: politics; economics; technology; social problems; environmentalism of the human spirit. Finally in Part III, Gore presents his approach to the global environmental crisis, first presenting a section about a global sense of responsibility and purpose and then describing his ideas for A Global Marshal Plan. 169 refs., 4 figs

  6. The Spirit counts - People at and around CERN

    CERN Multimedia

    CERN. Geneva

    2014-01-01

    After a few biographical remarks I shall concentrate on human aspects which are not covered by official documents, but which are as important to the success of CERN as scientific and technical competence. The approval of LEP, general problems of the project management and the approval of the LEP experiments under conditions never encountered before at CERN will be covered. The special spirit created at CERN based on the competence and solidarity of the CERN staff and its users made it possible to find new ways of successful international collaboration combining competition with cooperation. Career Summary Physics diploma and doctorate from Hamburg University, now Prof. emer.; research assistant at Stockholm Technical University (with Lise Meitner); Cavendish Laboratory UK (with O.R.Frisch); Cornell University (with R.R. Wilson); research in optics, nuclear and elementary particle physics. various professorships in Germany and director of university institutes; Director of DESY, Hamburg, 1973-1980...

  7. E and P integration via the OpenSpirit framework

    International Nuclear Information System (INIS)

    Jennis, S.

    1998-01-01

    The concept of inter-operability among a consortium of oil companies and E and P applications vendors was discussed. This paper describes the business problem including cost, cycle-time and efficiency and presents a solution. Benefits for applications developers will be single development environment for cross platform deployment; focus on value-added functionality instead of infrastructure; transparent access to widely-used data-stores; higher productivity and faster turnaround time to market. Application end-users will also benefit through elimination of the need to reformat due to cross platform and multi-vendor data access; utilization of Web browsers; integration with MS Office applications leveraging desk-top tools; lower purchase and integration cost of new applications. Strategic issues for application developers, and for oil companies, and competitive advantages of the E an P industry adopting OpenSpirit as the standard business object framework were also reviewed

  8. Evidence of a Christmas spirit network in the brain

    DEFF Research Database (Denmark)

    Hougaard, Anders; Lindberg, Ulrich; Arngrim, Nanna

    2015-01-01

    OBJECTIVE: To detect and localise the Christmas spirit in the human brain. DESIGN: Single blinded, cross cultural group study with functional magnetic resonance imaging (fMRI). SETTING: Functional imaging unit and department of clinical physiology, nuclear medicine and PET in Denmark. PARTICIPANTS......: 10 healthy people from the Copenhagen area who routinely celebrate Christmas and 10 healthy people living in the same area who have no Christmas traditions. MAIN OUTCOME MEASURES: Brain activation unique to the group with Christmas traditions during visual stimulation with images with a Christmas...... theme. METHODS: Functional brain scans optimised for detection of the blood oxygen level dependent (BOLD) response were performed while participants viewed a series of images with Christmas themes interleaved with neutral images having similar characteristics but containing nothing that symbolises...

  9. Negative Freedom as Politics of Spirit in Hegel

    Directory of Open Access Journals (Sweden)

    Luis Magno Veras Oliveira

    2017-03-01

    Full Text Available This article aims to present negative freedom as a moment of vitality in the formation of absolute freedom, represented by moral conscience, as a necessary process of realization in political representation based on Hegel’s Phenomenology of the Spirit. In the first moment, we will present the understanding of absolute freedom and the unfolding of its concept as universal will. In the second moment, we will discuss the conception of negative freedom as an experience of the French Revolution and its result as terror. The experience of negative freedom is understood as the possible means for the solution of contradiction, destruction, and death. These means originate from the political representation of the French Revolution. The hermeneutics presented leads to the positive exaltation of negative freedom as the way towards a possible solution of the problems inherent to a representation of absolute freedom as rational.

  10. Community Adaptation to the Hebei-Spirit Oil Spill

    Directory of Open Access Journals (Sweden)

    So-Min Cheong

    2012-09-01

    Full Text Available The focus of the research is the significance of dependence for communities to survive and adapt in times of environmental disasters. It shifts the emphasis on self-reliant communities for survival and examines the types and effects of dependence and external linkages by analyzing the range of community responses that include initial responses, early social impact, compensation, and conflicts after the Hebei-Spirit oil spill in December 2007 in Korea. The findings reveal that dependence is necessary, and the effects of dependence can be both positive and negative depending on the relations between external entities and affected communities as well as the community capacity to absorb resources and information.

  11. Emplacement of Fahrenheit crater ejecta at the Luna-24 site

    International Nuclear Information System (INIS)

    Settle, M.; Cintala, M.J.; Head, J.W.

    1979-01-01

    The Luna-24 site is situated in Mare Crisium at a range of 18.4 km from Fahrenheit, an Eratosthenian-aged crater 6.4 km in diameter. Fahrenheit's ejecta deposits have been degraded to such an extent that secondary craters and rays cannot be unambiguously identified in the vicinity of the Luna-24 site. On the basis of an analogy between Fahrenheit and Lichtenberg B (a much younger crater of comparable size located in northern Oceanus Procellarum) Fahrenheit ejecta deposits near the sample site are inferred to have consisted of secondary crater clusters, subradially aligned secondary crater chains, and lineated terrain furrowed by fine-scale radial grooves. At the range of the Luna-24 site more than 80% of the mare surface should have been morphologically disturbed by the ballistic deposition of Fahrenheit ejecta. Blocks and fragment clusters of primary Fehrenheit ejecta ranging up to 5-20 m in diameter are inferred to have impacted the local surface at velocities of 165-230 m s -1 forming secondary craters ranging up to 100m in diameter. The maximum depth of excavation of primary Fahrenheit ejecta deposited near the sample site is estimated to be at least 100m. Primary Fahremheit ejecta is expected to constitute a substantial fraction of the exterior deposits emplaced at the range of the Luna-24 site. Microgabbro and monomineralic fragments discovered in the Luna-24 drill core may have been derived from gabbroic rocks transported to the sample site by the Fahrenheit cratering event. This hypothesis is consistent with the widespread occurrence and characteristics of Fahrenheit ejecta anticipated in the vicinity of the Luna-24 site. (Auth.)

  12. Evolution of Lunar Crater Ejecta Through Time: Influence of Crater Size on the Record of Dynamic Processes

    Science.gov (United States)

    Ghent, R. R.; Tai Udovicic, C.; Mazrouei, S.; Bottke, W. F., Jr.

    2017-12-01

    The bombardment history of the Moon holds the key to understanding important aspects of the evolution of the Solar System at 1AU. It informs our thinking about the rates and chronology of events on other planetary bodies and the evolution of the asteroid belt. In previous work, we established a quantitative relationship between the ages of lunar craters and the rockiness of their ejecta. That result was based on the idea that crater-forming impacts eject rocks from beneath the regolith, instantaneously emplacing a deposit with characteristic initial physical properties, such as rock abundance. The ejecta rocks are then gradually removed and / or covered by a combination of mechanical breakdown via micrometeorite bombardment, emplacement of regolith fines due to nearby impacts, and possibly rupture due to thermal stresses. We found that ejecta rocks, as detected by the Lunar Reconnaissance Orbiter Diviner thermal radiometer disappear on a timescale of 1 Gyr, eventually becoming undetectable by the Diviner instrument against the ambient background rock abundance of the regolith.The "index" craters we used to establish the rock abundance—age relationship are all larger than 15 km (our smallest index crater is Byrgius A, at 18.7 km), and therefore above the transition diameter between simple and complex craters (15-20 km). Here, we extend our analysis to include craters smaller than the transition diameter. It is not obvious a priori that the initial ejecta properties of simple and complex craters should be identical, and therefore, that the same metrics of crater age can be applied to both populations. We explore this issue using LRO Diviner rock abundance and a high-resolution optical maturity dataset derived from Kaguya multiband imager VIS/NIR data to identify young craters to 5 km diameter. We examine the statistical properties of this population relative to that of the NEO population, and interpret the results in the context of our recently documented evidence

  13. 41 CFR 102-41.205 - Do we report all forfeited distilled spirits, wine, and beer to GSA for disposal?

    Science.gov (United States)

    2010-07-01

    ... forfeited distilled spirits, wine, and beer to GSA for disposal? 102-41.205 Section 102-41.205 Public..., and Beer § 102-41.205 Do we report all forfeited distilled spirits, wine, and beer to GSA for disposal? (a) Yes, except do not report distilled spirits, wine, and beer not fit for human consumption or for...

  14. 27 CFR 28.199 - Responsibility for return of spirits withdrawn for export with benefit of drawback.

    Science.gov (United States)

    2010-04-01

    ... of spirits withdrawn for export with benefit of drawback. 28.199 Section 28.199 Alcohol, Tobacco... EXPORTATION OF ALCOHOL Exportation of Distilled Spirits With Benefit of Drawback Filing of Notice and Removal § 28.199 Responsibility for return of spirits withdrawn for export with benefit of drawback. The...

  15. Acid Sulfate Alteration on Mars

    Science.gov (United States)

    Ming, D. W.; Morris, R. V.

    2016-01-01

    A variety of mineralogical and geochemical indicators for aqueous alteration on Mars have been identified by a combination of surface and orbital robotic missions, telescopic observations, characterization of Martian meteorites, and laboratory and terrestrial analog studies. Acid sulfate alteration has been identified at all three landing sites visited by NASA rover missions (Spirit, Opportunity, and Curiosity). Spirit landed in Gusev crater in 2004 and discovered Fe-sulfates and materials that have been extensively leached by acid sulfate solutions. Opportunity landing on the plains of Meridiani Planum also in 2004 where the rover encountered large abundances of jarosite and hematite in sedimentary rocks. Curiosity landed in Gale crater in 2012 and has characterized fluvial, deltaic, and lacustrine sediments. Jarosite and hematite were discovered in some of the lacustrine sediments. The high elemental abundance of sulfur in surface materials is obvious evidence that sulfate has played a major role in aqueous processes at all landing sites on Mars. The sulfate-rich outcrop at Meridiani Planum has an SO3 content of up to 25 wt.%. The interiors of rocks and outcrops on the Columbia Hills within Gusev crater have up to 8 wt.% SO3. Soils at both sites generally have between 5 to 14 wt.% SO3, and several soils in Gusev crater contain around 30 wt.% SO3. After normalization of major element compositions to a SO3-free basis, the bulk compositions of these materials are basaltic, with a few exceptions in Gusev crater and in lacustrine mudstones in Gale crater. These observations suggest that materials encountered by the rovers were derived from basaltic precursors by acid sulfate alteration under nearly isochemical conditions (i.e., minimal leaching). There are several cases, however, where acid sulfate alteration minerals (jarosite and hematite) formed in open hydrologic systems, e.g., in Gale crater lacustrine mudstones. Several hypotheses have been suggested for the

  16. Atmospheric Tides in Gale Crater, Mars

    Science.gov (United States)

    Guzewich, Scott D,; Newman, C. E; de la Torre Juarez, M.; Wilson, R. J.; Lemmon, M.; Smith, M. D.; Kahanpaa, H.; Harri, A.-M.

    2015-01-01

    Atmospheric tides are the primary source of daily air pressure variation at the surface of Mars. These tides are forced by solar heating of the atmosphere and modulated by the presence of atmospheric dust, topography, and surface albedo and thermal inertia. This results in a complex mix of sun-synchronous and nonsun- synchronous tides propagating both eastward and westward around the planet in periods that are integer fractions of a solar day. The Rover Environmental Monitoring Station on board the Mars Science Laboratory has observed air pressure at a regular cadence for over 1 Mars year and here we analyze and diagnose atmospheric tides in this pressure record. The diurnal tide amplitude varies from 26 to 63 Pa with an average phase of 0424 local true solar time, while the semidiurnal tide amplitude varies from 5 to 20 Pa with an average phase of 0929. We find that both the diurnal and semidiurnal tides in Gale Crater are highly correlated to atmospheric opacity variations at a value of 0.9 and to each other at a value of 0.77, with some key exceptions occurring during regional and local dust storms. We supplement our analysis with MarsWRF general circulation modeling to examine how a local dust storm impacts the diurnal tide in its vicinity. We find that both the diurnal tide amplitude enhancement and regional coverage of notable amplitude enhancement linearly scales with the size of the local dust storm. Our results provide the first long-term record of surface pressure tides near the martian equator.

  17. Eruptive history of the Ubehebe Crater cluster, Death Valley, California

    Science.gov (United States)

    Fierstein, Judy; Hildreth, Wes

    2017-04-01

    A sequence of late Holocene eruptions from the Ubehebe Crater cluster in Death Valley was short-lived, emplacing several phreatomagmatic and magmatic deposits. Seven craters form the main group, which erupted along a north-south alignment 1.5 km long. At least five more make a 500-m east-west alignment west of the main crater group. One more is an isolated shallow crater 400 m south of that alignment. All erupted through Miocene fanglomerate and sandstone, which are now distributed as comminuted matrix and lithic clasts in all Ubehebe deposits. Stratigraphic evidence showing that all Ubehebe strata were emplaced within a short time interval includes: (1) deposits from the many Ubehebe vents make a multi-package sequence that conformably drapes paleo-basement topography with no erosive gullying between emplacement units; (2) several crater rims that formed early in the eruptive sequence are draped smoothly by subsequent deposits; and (3) tack-welded to agglutinated spatter and bombs that erupted at various times through the sequence remained hot enough to oxidize the overlying youngest emplacement package. In addition, all deposits sufficiently consolidated to be drilled yield reliable paleomagnetic directions, with site mean directions showing no evidence of geomagnetic secular variation. Chemical analyses of juvenile components representing every eruptive package yield a narrow range in major elements [SiO2 (48.65-50.11); MgO (4.98-6.23); K2O (2.24-2.39)] and trace elements [Rb (28-33); Sr (1513-1588); Zr (373-404)]. Despite lithologic similarities, individual fall units can be traced outward from vent by recording layer thicknesses, maximum scoria and lithic sizes, and juvenile clast textural variations. This permits reconstruction of the eruptive sequence, which produced a variety of eruptive styles. The largest and northernmost of the craters, Ubehebe Crater, is the youngest of the group. Its largely phreatomagmatic deposits drape all of the others, thicken in

  18. Impact cratering on high-porosity planetary bodies

    Science.gov (United States)

    Collins, Gareth

    2017-06-01

    Porous materials abound in the Solar System. Primordial solids accreted gently from dust into high-porosity aggregates; many asteroids appear to be loosely-bound rubble piles; and the crusts of airless planetary surfaces are heavily fractured from prolonged bombardment of asteroids. High porosity attenuates shock propagation and localizes shock heating, which has several important implications for the evolution of planetary surfaces. Most studies of impact cratering have focused on targets composed of common geologic materials, such as soils and rock, thought to be reasonable proxies for the surfaces of the terrestrial planets. However, it has become clear that those materials are not good analogues for the minor bodies of the Solar System. Here we present numerical and experimental results of impact cratering in high porosity materials that elucidate the compaction regime of planetary cratering: where crater growth is dominated by impactor penetration and compaction, while rapid shock attenuation and extensive collapse limit the volume and speed of ejected material. Understanding these effects is a crucial step in using crater populations to estimate impactor flux, date planetary surfaces and infer subsurface properties, as well as deflecting hazardous near-Earth asteroids. In collaboration with: Kevin Housen, The Boeing Co.

  19. Devolatilization or melting of carbonates at Meteor Crater, AZ?

    Science.gov (United States)

    Hörz, F.; Archer, P. D.; Niles, P. B.; Zolensky, M. E.; Evans, M.

    2015-06-01

    We have investigated the carbonates in the impact melts and in a monolithic clast of highly shocked Coconino sandstone of Meteor Crater, AZ to evaluate whether melting or devolatilization is the dominant response of carbonates during high-speed meteorite impact. Both melt- and clast-carbonates are calcites that have identical crystal habits and that contain anomalously high SiO2 and Al2O3. Also, both calcite occurrences lack any meteoritic contamination, such as Fe or Ni, which is otherwise abundantly observed in all other impact melts and their crystallization products at Meteor Crater. The carbon and oxygen isotope systematics for both calcite deposits suggest a low temperature environment (impact melts, yield 100 wt% element totals by EMPA, suggesting complete loss of CO2. The target dolomite decomposed into MgO, CaO, and CO2; the CO2 escaped and the CaO and MgO combined with SiO2 from coexisting quartz and FeO from the impactor to produce the dominant impact melt at Meteor Crater. Although confined to Meteor Crater, these findings are in stark contrast to Osinski et al. (2008) who proposed that melting of carbonates, rather than devolatilization, is the dominant process during hypervelocity impact into carbonate-bearing targets, including Meteor Crater.

  20. Measuring impact crater depth throughout the solar system

    Science.gov (United States)

    Robbins, Stuart J.; Watters, Wesley A.; Chappelow, John E.; Bray, Veronica J.; Daubar, Ingrid J.; Craddock, Robert A.; Beyer, Ross A.; Landis, Margaret E.; Ostrach, Lillian; Tornabene, Livio L.; Riggs, Jamie D.; Weaver, Brian P.

    2018-01-01

    One important, almost ubiquitous, tool for understanding the surfaces of solid bodies throughout the solar system is the study of impact craters. While measuring a distribution of crater diameters and locations is an important tool for a wide variety of studies, so too is measuring a crater's “depth.” Depth can inform numerous studies including the strength of a surface and modification rates in the local environment. There is, however, no standard data set, definition, or technique to perform this data‐gathering task, and the abundance of different definitions of “depth” and methods for estimating that quantity can lead to misunderstandings in and of the literature. In this review, we describe a wide variety of data sets and methods to analyze those data sets that have been, are currently, or could be used to derive different types of crater depth measurements. We also recommend certain nomenclature in doing so to help standardize practice in the field. We present a review section of all crater depths that have been published on different solar system bodies which shows how the field has evolved through time and how some common assumptions might not be wholly accurate. We conclude with several recommendations for researchers which could help different data sets to be more easily understood and compared.

  1. Fiery Spirits in the context of institutional entrepreneurship in Swedish healthcare.

    Science.gov (United States)

    Eriksson, Nomie; Ujvari, Sandor

    2015-01-01

    Clinical governance and leadership concepts can lead to more or less successful implementations of new clinical practice. The purpose of this paper is to examine how Fiery Spirits, as institutional entrepreneurs can, working in a team, implement sustained change in hospital clinical practice. This paper describes two case studies, conducted at two Swedish hospitals over a period of two years, in which changes in clinical practice were implemented. In both cases, key-actors, termed Fiery Spirits, played critical roles in these changes. The authors use a qualitative approach and take an intra-organizational perspective with semi-structured in-depth interviews and document analysis. The new clinical practices were successfully implemented with a considerable influence of the Fiery Spirits who played a pivotal role in the change efforts. The Fiery Spirits persuasively, based on their structural and normative legitimacy and the adoption of learning processes, advocated, and supported change. Fiery Spirits, given flexibility and opportunity, can be powerful forces for change outside the trajectory of management-inspired and management-directed change. Team members, when inspired and encouraged by Fiery Spirits, are less resistant to change and more willing to test new clinical practices. The paper complements literature on how the Fiery Spirit concept aligns with concepts of clinical governance and leadership and how change can be achieved. Additionally, the findings show the effects of legitimacy and learning processes on change in clinical practice.

  2. Chemical profile of sugarcane spirits produced by double distillation methodologies in rectifying still

    Directory of Open Access Journals (Sweden)

    André Ricardo Alcarde

    2011-06-01

    Full Text Available The objective of this study was to determine the chemical profile of sugarcane spirits produced by different double distillation methodologies in rectifying still. Fermented sugarcane juice was distilled in rectifying still according to three double distillation methodologies: the methodology used for cognac production; the methodology used for whisky production; and the 10-80-10 percentage composition methodology, referring to the volumes of head, heart and tail of the distillate fractions from the second distillation. For comparison purposes, a simple distilled spirit was also produced. The distillates were analyzed for concentrations of ethanol, copper, volatile acidity, furfural and hydroxymethylfurfural, aldehydes, esters, methanol and higher alcohols. The spirits were also evaluated on the sensory attributes of aroma, taste and preference. Compared to simple distillation, double distillation improved the chemical quality of the spirits, since it has reduced the concentrations of acids, aldehydes, esters, methanol, higher alcohols and, consequently, their coefficient of congeners. Regardless of the methodology employed, the double distillation improved the sensory quality of the spirits since they obtained higher sensory acceptance in relation to spirits produced by simple distillation. Among double distilled spirits, the one produced according to whisky methodology obtained the best scores from appraisers on the aroma and flavor parameters and it was also the most preferred.

  3. Problems determining relative and absolute ages using the small crater population

    Science.gov (United States)

    Xiao, Zhiyong; Strom, Robert G.

    2012-07-01

    The small crater populations (diameter smaller than 1 km) are widely used to date planetary surfaces. The reliability of small crater counts is tested by counting small craters at several young and old lunar surfaces, including Mare Nubium and craters Alphonsus, Tycho and Giordano Bruno. Based on high-resolution images from both the Lunar Reconnaissance Orbiter Camera and Kaguya Terrain Camera, small craters in two different diameter ranges are counted for each counting area. Large discrepancies exist in both the cumulative (absolute model ages) and relative plots for the two different size ranges of the same counting areas. The results indicate that dating planetary surfaces using small crater populations is highly unreliable because the contamination of secondaries may invalidate the results of small crater counts. A comparison of the size-frequency distributions of the small crater populations and impact ejected boulders around fresh lunar craters shows the same upturn as typical martian secondaries, which supports the argument that secondaries dominate the small crater populations on the Moon and Mars. Also, the size-frequency distributions of small rayed lunar and martian craters of probable primary origin are similar to that of the Population 2 craters on the inner Solar System bodies post-dating Late Heavy Bombardment. Dating planetary surfaces using the small crater populations requires the separation of primaries from secondaries which is extremely difficult. The results also show that other factors, such as different target properties and the subjective identification of impact craters by different crater counters, may also affect crater counting results. We suggest that dating planetary surfaces using small crater populations should be with highly cautious.

  4. Pathological spirit possession as a cultural interpretation of trauma-related symptoms.

    Science.gov (United States)

    Hecker, Tobias; Barnewitz, Eva; Stenmark, Hakon; Iversen, Valentina

    2016-07-01

    Spirit possession is a phenomenon frequently occurring in war-torn countries. It has been shown to be an idiom of distress entailing dissociative symptoms. However, its association with trauma exposure and trauma-related disorders remains unclear. This study aimed to explore subjective disease models and the relationship between pathological spirit possession and trauma-related disorders in the Eastern Democratic Republic of the Congo. Seventy-three (formerly) possessed persons (74% female, mean age = 34 years), referred by traditional and spiritual healers, were interviewed about their experiences of pathological spirit possession, trauma exposure, posttraumatic stress disorder (PTSD) symptoms, depressive symptoms, shame and guilt, psychotic symptoms, somatic complaints, and the impairment of psychosocial functioning. The most common disease model for pathological spirit possession was another person having sent the spirit, mostly a family member or a neighbor, out of jealousy or conflict over resources. Significant correlations were found between spirit possession over lifetime and PTSD symptom severity, feelings of shame and guilt, depressive symptoms, somatic complaints, and psychotic symptoms. Spirit possession during the preceding 4 weeks was associated with PTSD symptom severity, impairment of psychosocial functioning, and psychotic symptom severity. The results of this study indicate that pathological spirit possession is a broad explanatory framework for various subjectively unexplainable mental and physical health problems, including but not limited to trauma-related disorders. Understanding pathological spirit possession as a subjective disease model for various mental and physical health problems may help researchers and clinicians to develop culturally sensitive treatment approaches for affected individuals. (PsycINFO Database Record (c) 2016 APA, all rights reserved).

  5. Behavioural effects in rats after prenatal exposure to dearomatized white spirit

    DEFF Research Database (Denmark)

    Hass, Ulla; Ladefoged, Ole; Lam, H.R.

    2001-01-01

    The purpose of the study was to investigate the potential developmental neurotoxicity of the widely used organic solvent, white spirit. Rats (Mol:WIST) were exposed to 0 or 800 ppm dearomatized white spirit for 6 hr per day on gestation days 7-20. Developmental and neurobehavioural effects...... months, learning and memory deficits were observed in exposed offspring. The differences were not related to poorer swimming capabilities. because swim speeds were similar to control values. The results show that prenatal exposure to 800 ppm white spirit caused longlasting learning and memory deficits...

  6. Postulated impact craters yield oil and gas, lively debate

    Energy Technology Data Exchange (ETDEWEB)

    Petzet, G.A.

    1995-04-10

    Impact craters, also called astroblemes, are the most common landform in the solar system, and several on earth have produced oil and gas. Significant cross-disciplinary study is being aimed at understanding the origin, structure, and economic potential of surface and buried craters worldwide. The Oklahoma Geological Survey and the US Department of Energy organized a workshop to discuss the Ames structure, a feature in Major Country, Okla., along the sprawling, giant Sooner Trend/Ringwood oil producing complex. This rundown is designed to provide basic information gleaned from speakers and abstracts presented at the workshop. OGS is to publish proceedings later. This paper discusses meteors vs. volcanoes, the Oklahoma crater, questions about Ames, producing astroblemes, and future research.

  7. Hydrological Modeling of the Jezero Crater Outlet-Forming Flood

    Science.gov (United States)

    Fassett, Caleb I.; Goudge, Timothy A.

    2017-01-01

    Jezero crater is a site of prime scientific interest because it was a lake early in Mars history. Preserved clay- and carbonate-bearing sedimentary fans on Jezero's western and northwestern margin (Fig. 2) are accessible to future exploration. Geologic context [1] and stratigraphic analysis of the western fan strongly support the interpretation that these fans were deposited as deltas into the lake. This has helped establish Jezero as one of the final candidate landing sites for Mars 2020. The high level of certainty that Jezero was a lake results from the existence of its outlet valley, which required filling of the crater to form [e.g., 1,4]. Here, we specifically focus on how this outlet valley was carved by the dam breach flood that eroded the eastern crater rim. We have completed preliminary modeling in both 1D and 2D of the outlet's formation.

  8. Geologic map of Mount Mazama, Crater Lake, Oregon

    Science.gov (United States)

    Bacon, Charles

    1990-01-01

    Crater Lake caldera collapsed about 6,850 yr B.P. during the climactic eruption of Mount Mazama, a High Cascade basaltic andesitic to dacitic volcanic center that was constructed during a period of about 400,000 yr. The caldera and the products of the climactic eruption are clear evidence for the presence of a shallow magma body that must have supported a hydrothermal system in the recent past. The geology of Mount Mazama has been mapped at a scale of 1:24,000 based on detailed study of the walls of Crater Lake caldera and mapping of the flanks of the volcano. The map shows lavas and fragmental deposits of Mount Mazama, lavas of nearby monogenetic volcanoes, pre-Mazama silicic volcanic rocks, products of the climactic eruption, and glacial deposits. Related topical studies of the volcanology, geochronology, petrology, and geochemistry of the Crater Lake area depend on field relations established by geologic mapping.

  9. Ganymede - A relationship between thermal history and crater statistics

    Science.gov (United States)

    Phillips, R. J.; Malin, M. C.

    1980-01-01

    An approach for factoring the effects of a planetary thermal history into a predicted set of crater statistics for an icy satellite is developed and forms the basis for subsequent data inversion studies. The key parameter is a thermal evolution-dependent critical time for which craters of a particular size forming earlier do not contribute to present-day statistics. An example is given for the satellite Ganymede and the effect of the thermal history is easily seen in the resulting predicted crater statistics. A preliminary comparison with the data, subject to the uncertainties in ice rheology and impact flux history, suggests a surface age of 3.8 x 10 to the 9th years and a radionuclide abundance of 0.3 times the chondritic value.

  10. The Links Between Target Properties and Layered Ejecta Craters in Acidalia and Utopia Planitiae Mars

    Science.gov (United States)

    Jones, E.; Osinski, G. R.

    2013-08-01

    Layered ejecta craters on Mars may form from excavation into subsurface volatiles. We examine a new catalogue of martian craters to decipher differences between the single- and double-layered ejecta populations in Acidalia and Utopia.

  11. Application of X-ray computed microtomography to soil craters formed by raindrop splash

    Science.gov (United States)

    Beczek, Michał; Ryżak, Magdalena; Lamorski, Krzysztof; Sochan, Agata; Mazur, Rafał; Bieganowski, Andrzej

    2018-02-01

    The creation of craters on the soil surface is part of splash erosion. Due to the small size of these craters, they are difficult to study. The main aim of this paper was to test X-ray computed microtomography to investigate craters formed by raindrop impacts. Measurements were made on soil samples moistened to three different levels corresponding with soil water potentials of 0.1, 3.16 and 16 kPa. Using images obtained by X-ray microtomography, geometric parameters of the craters were recorded and analysed. X-ray computed microtomography proved to be a useful and efficient tool for the investigation of craters formed on the soil surface after the impact of water drops. The parameters of the craters changed with the energy of the water drops and were dependent on the initial moisture content of the soil. Crater depth is more dependent on the increased energy of the water drop than crater diameter.

  12. Hypothetical Source Crater for Australasian Tektites: Moving from Indochina to Northwest China?

    Science.gov (United States)

    Mizera, J.; Řanda, Z.; Kameník, J.; Klokočník, J.; Kostelecký, J.

    2016-08-01

    We argue against the generally accepted hypothetical location of the unknown source crater for Australasian tektites to Indochina, and present a hypothesis of a possible location of the AAT source crater in deserts of NW China.

  13. Quantum Poetics: Science and Spirit in Twentieth Century American Poetry

    Science.gov (United States)

    Monaghan, (Mary) Patricia

    Concepts from quantum physics illuminate ways in which five 20th century American poets struggle with the expression of nonlinear, nontemporal experiences in linear, temporal language. An "experience of spirit"- -an experience of cosmic unity which occurs in a timeless moment and involves a paradoxical sensuality--is expressed by poets Wallace Stevens, Albert Goldbarth, Nancy Willard, Linda Gregg and Marilyn Waniek. Contemporary science similarly seeks ways to express nonlinear realities in linear language. The English language is found to guide users to linear, time-bounded expression through the noun (leading to nominalization), the verb (demanding experience be limited to past, present or future), adverb and adjective (which separate senses from each other and divide attributes from essence). English presents structural difficulties to those who wish to express experiences of spirit--difficulties also articulated by quantum theorists struggling to express unvisualizable concepts. Wallace Stevens devoted the first half of his poetic career to questions of order, which find reflections within the works of quantum physicists who theorize an "implicate order" within the subatomic universe. During his later years, Stevens turned to the question of chaos, an interest paralleled by recent developments in dynamical systems theory. Albert Goldbarth and Nancy Willard alter narrative form in three ways to convey nonlinear possibilities. The "parabolic" narrative uses story to exemplify a moral or philosophical message. The "midrashic" illuminates the meaning of one story by the telling of another. Finally, the "coyotic" begins with one, apparently ordinary, story which is then altered to introduce fantastical realities. These narratives form a "relative time," similar to that which Einstein defined in his special theory of relativity. The works of Marilyn Waniek and Linda Gregg are examined in terms of the language of paradoxical sensuality, which calls into question the

  14. Spirit Piagam Jakarta Dalam Undang-Undang Dasar 1945

    Directory of Open Access Journals (Sweden)

    Mujar Ibnu Syarif

    2016-10-01

    Full Text Available Abstract: In the second trial BPUPKI, both nationalist and Islamic groups consensual that the future of Indonesia's independence will be based on the principle "godhood by running Shari'ah obligation for adherents". The consensus seems to be built on the foundation is not solid. Therefore it is not surprising that one day after the proclamation of independence, the agreement re-questioned. That same day, PPKI held a hearing to review the deal. As a result, the clause contained in the Preamble of the 1945 Constitution was changed to "Based on Belief in God Almighty". After the issuance of a Presidential Decree, began the debate about the existence of the spirit of the Jakarta Charter in 1945 which is applicable in the context of Indonesian politics in this contemporary age.  Abstrak: Spirit Piagam Jakarta dalam Undang-Undang Dasar 1945 Pasca Lahirnya Dekrit Presiden 5 Juli 1959. Pada sidang kedua Badan Penyelidik Usaha-Usaha Persiapan Kemerdekaan Indonesia (BPUPKI / Dokuritsu Zyunbi Tyosakai yang berlangsung sejak tanggal 10 hingga 16 Juli 1945, baik golongan nasionalis maupun golongan Islam berkonsensus bahwa masa depan Indonesia merdeka akan didasarkan pada sila "Ketuhanan dengan kewajiban menjalankan syari'at Islam bagi pemeluk-pemeluknya".  Penting dicatat, konsensus tersebut agaknya dibangun di atas landasan yang tidak kokoh. Karena itu, tidak aneh bila satu hari setelah proklamasi Kemerdekaan RI, tepatnya tanggal 18 Agustus 1945, kesepakatan tersebut kembali dipersoalkan. Pada hari itu juga, Panitia Persiapan Kemerdekaan Indonesia (PPKI yang dibentuk tanggal 7 Agustus 1945 dan diketuai oleh Soekarno, menyelenggarakan sidang untuk meninjau kembali kesepakatan tersebut. Dalam sidang tersebut, anak kalimat  yang terdapat dalam Pembukaan UUD 1945 (Piagam Jakarta, yakni: "Berdasarkan kepada Ketuhanan, dengan kewajiban menjalankan syari'at Islam bagi pemeluk-pemeluknya" diubah menjadi "Berdasar atas Ketuhanan Yang Maha Esa".  Setelah

  15. Ceres' intriguing Occator crater and its faculae: formation and evolution

    Science.gov (United States)

    Buczkowski, D.; Scully, J. E. C.; Bowling, T.; Bu, C.; Castillo, J. C.; Jaumann, R.; Longobardo, A.; Nathues, A.; Neesemann, A.; Palomba, E.; Platz, T.; Quick, L. C.; Raponi, A.; Raymond, C. A.; Ruesch, O.; Russell, C. T.; Schenk, P.; Stein, N.

    2017-12-01

    Since March 2015, the Dawn spacecraft has orbited and explored Ceres, which is a dwarf planet and the largest object in the asteroid belt (radius 470 km). One of the most intriguing features on Ceres' surface is Occator crater, a 92-km-diameter impact crater that contains distinctive bright spots, called faculae, within its floor (Nathues et al., 2015; Russell et al., 2016; Schenk et al., 2017). Occator crater has been dated to 20-30 million years old (Nathues et al., 2017; Neesemann et al., 2017). The single scattering albedo of Occator's faculae is 0.67-0.80, which is greater than Ceres' average single scattering albedo of 0.09-0.11 (Li et al., 2016). The central facula is named Cerealia Facula, and is located in a 9 km wide and 700 m deep pit. There are also multiple additional faculae in the eastern crater floor, which are named the Vinalia Faculae. The faculae are mostly composed of sodium carbonate, are distinct from Ceres' average surface composition and are proposed to be the solid residues of crystallized brines (De Sanctis et al., 2016). The presence of such bright, apparently fresh, material on the surface of a dwarf planet that is billions of years old is intriguing, and indicates that active processes involving brines occurred within the geologically recent past. The Dawn Science Team has investigated whether the processes that formed the crater and the faculae are entirely endogenic, entirely exogenic or a combination of both. For example, the extensive lobate materials within the crater floor have been proposed to be impact melt, mass wasting deposits or cryolava flows (e.g. Buczkowski et al., 2017; Jaumann et al., 2017; Nathues et al., 2017; Schenk et al., 2017). Each possibility has the potential to provide fascinating insights into Ceres' evolution, including the potential for liquids within Ceres' interior today. The team's in-depth investigation of Occator crater will be presented in an upcoming special issue of the journal Icarus. This special

  16. Parameters critical to the morphology of fluidization craters

    Science.gov (United States)

    Siegal, B. S.; Gold, D. P.

    1973-01-01

    In order to study further the role of fluidization on the moon, a laboratory investigation was undertaken on two particulate material size fractions to determine the effect of variables, such as, duration of gas streaming, gas pressure, and 'regolith' thickness on the morphology of fluidization craters. A 3.175-mm cylindrical vent was used to simulate a gas streaming conduit. Details of the fluidization chamber are discussed together with questions of experimental control, aspects of nomenclature, crater measurements, and the effect of variables.

  17. Mini-RF Bistatic Observations of Lunar Crater Ejecta

    Science.gov (United States)

    Stickle, A. M.; Patterson, G. W.; Cahill, J. T.

    2017-12-01

    The Mini-RF radar onboard the Lunar Reconnaissance Orbiter (LRO) is currently operating in a bistatic configuration using the Goldstone DSS-13 and Arecibo Observatory as transmitters in X-band (4.2-cm) and S-band (12.6 cm), respectively. The Circular Polarization Ratio (CPR) is a typical product derived from backscattered microwave radiation that examines the scattering properties of the lunar surface, particularly the roughness of the surface on the order of the radar wavelength. Throughout the LRO extended mission, Mini-RF has targeted young craters on the lunar surface to examine the scattering properties of their ejecta blankets in both S- and X-band. Several observed craters and their ejecta blankets exhibit a clear coherent backscatter opposition effect at low bistatic (phase) angles. This opposition effect is consistent with optical studies of lunar soils done in the laboratory, but these observations are the first time this effect has been measured on the Moon at radar wavelengths. The style of the observed opposition effect differs between craters, which may indicate differences in ejecta fragment formation or emplacement. Differences in the CPR behavior as a function of bistatic angle may also provide opportunities for relative age dating between Copernican craters. Here, we examine the ejecta of nine Copernican and Eratosthenian aged craters in both S-band and X-band and document CPR characteristics as a function bistatic angle in order to test that hypothesis. The youngest craters observed by Mini-RF (e.g., Byrgius A (48 My), Kepler (635-1250 My)) exhibit a clear opposition effect, while older craters such as Hercules have a fairly flat response in CPR as a function of phase angle. Craters with ages between these two ends, e.g., Aristarchus, exhibit a weaker opposition response. Observing the scattering behavior of continuous ejecta blankets in multiple wavelengths may provide further information about the rate of breakdown of rocks of varying size to

  18. Geomorphometric analysis of selected Martian craters using polar coordinate transformation

    Science.gov (United States)

    Magyar, Zoltán; Koma, Zsófia; Székely, Balázs

    2016-04-01

    Centrally symmetric landform elements are very common features on the surface of the planet Mars. The most conspicuous ones of them are the impact craters of various size. However, a closer look on these features reveals that they show often asymmetric patterns as well. These are partially related to the geometry of the trajectory of the impacting body, but sometimes it is a result of surface processes (e.g., freeze/thaw cycles, mass movements). Geomorphometric studies have already been carried out to reveal these pecularities. Our approach, the application of polar coordinate transformation (PCT) very sensitively enhances the non-radial and non-circular shapes. We used digital terrain models (DTMs) derived from the ESA Mars Express HRSC imagery. The original DTM or its derivatives (e.g. slope angle or aspect) are PCT transformed. We analyzed the craters inter alia with scattergrams in polar coordinates. The resulting point cloud can be used directly for the analysis, but in some cases an interpolation should be applied to enhance certain non-circular features (especially in case of smaller craters). Visual inspection of the crater slopes, coloured by the aspect, reveals smaller features. Some of them are processing artefacts, but many of them are related to local undulations in the topography or indications of mass movements. In many cases the undulations of the crater rim are due to erosional processes. The drawbacks of the technology are related to the uneven resolution of the projected image: features in the crater centre should be left out from the analysis because PCT has a low resolution around the projection center. Furthermore, the success of the PCT depends on the correct definition of the projection centre: erroneously centered images are not suitable for analysis. The PCT transformed images are also suitable for radial averaging and calculation of standard deviations, resulting in typical, comparable craters shapes. These studies may lead to a deeper

  19. Role of the granular nature of meteoritic projectiles in impact crater morphogenesis

    OpenAIRE

    Bartali, Roberto; Rodríguez-Liñán, Gustavo M.; Nahmad-Molinari, Yuri; Sarocchi, Damiano; Ruiz-Suárez, J. C.

    2013-01-01

    By means of novel volume-diameter aspect ratio diagrams, we ponder on the current conception of crater morphogenesis analyzing crater data from beam explosions, hypervelocity collisions and drop experiments and comparing them with crater data from three moons (the Moon, Callisto, and Ganymede) and from our own experimental results. The distinctive volume-diameter scaling laws we discovered make us to conclude that simple and complex craters in satellites and planets could have been formed by ...

  20. Standard techniques for presentation and analysis of crater size-frequency data

    Science.gov (United States)

    1978-01-01

    In September 1977, a crater studies workshop was held for the purpose of developing standard data analysis and presentation techniques. This report contains the unanimous recommendations of the participants. This first meeting considered primarily crater size-frequency data. Future meetings will treat other aspects of crater studies such as morphologies.

  1. An in-depth study of Marcia Crater, Vesta

    Science.gov (United States)

    Hiesinger, Harald; Ruesch, Ottaviano; Williams, David A.; Nathues, Andreas; Prettyman, Thomas H.; Tosi, Frederico; De Sanctis, M. Christina; Scully, Jennifer E. C.; Schenk, Paul M.; Aileen Yingst, R.; Denevi, Bret W.; Jaumann, Ralf; Raymond, Carol A.; Russell, Chris T.

    2014-05-01

    After visiting the second most massive asteroid Vesta from July 2011 to September 2012, the Dawn spacecraft is now on its way to asteroid Ceres. Dawn observed Vesta with three instruments: the German Framing Camera (FC), the Italian Visible and InfraRed mapping spectrometer (VIR), and the American Gamma Ray and Neutron Detector (GRaND) [1]. Marcia crater (190°E, 10°N; 68 x 58 km) is the largest of three adjacent impact structures: Marcia (youngest), Calpurnia, and Minucia (oldest). It is the largest well-preserved post-Rheasilvia impact crater, shows a complex geology [2], is young [2], exhibits evidence for gully-like mass wasting [3], contains the largest location of pitted terrain [4], has smooth impact melt ponds [5], shows enhanced spectral pyroxene signatures on its inner walls [2], and has low abundances of OH and H in comparison to the surrounding low-albedo terrain [6, 7]. Geophysically, the broad region of Marcia and Calpurnia craters is characterized by a higher Bouguer gravity, indicating denser material [9]. Williams et al. [2] have produced a detailed geologic map of Marcia crater and the surrounding terrain. They identified several units within Marcia crater, including bright crater material, pitted terrain, and smooth material. Units outside Marcia, include undivided crater ejecta material, bright lobate material, dark lobate material, and dark crater ray material [2]. Because of its extensive ejecta and fresh appearance, the Marcia impact defines a major stratigraphic event, postdating the Rheasilvia impact [2]. However, the exact age of Marcia crater is still under debate. Compositionally, Marcia crater is characterized by higher iron abundances, which were interpreted as more basaltic-eucrite-rich materials suggesting that this region has not been blanketed by diogenitic materials from large impact events [10, 11]. Using FC data, [13] identified "gray material" associated with the ejecta blanket of Marcia crater. This material is characterized

  2. NPDES Draft Permit for Spirit Lake Water Treatment Facility in North Dakota

    Science.gov (United States)

    Under NPDES draft permit ND-0031101, Spirit Lake Water Resource Management is authorized to discharge to an unnamed intermittent tributary to Devils Lake which is tributary to Sheyenne River in North Dakota.

  3. Effects of white spirits on rat brain 5-HT receptor functions and synaptic remodeling

    DEFF Research Database (Denmark)

    Lam, Henrik Rye; Plenge, P.; Jørgensen, O.S.

    2001-01-01

    , and subcellular levels. This study investigates the effects of two types of white spirit on 5-hydroxytryptamine (5-HT) transporters (5-HTT), 5-HT2A and 5-HT4 receptor expression in forebrain, and on neural cell adhesion molecule (NCAM) and 25-kDa synaptosomal associated protein (SNAP-25) concentrations when......Previously, inhalation exposure to different types of white spirit (i.e. complex mixtures of aliphatic, aromatic, alkyl aromatic, and naphthenic hydrocarbons) has been shown to induce neurochemical effects in rat brains. Especially, the serotonergic system was involved at the global, regional...... applied as indices for synaptic remodeling in forebrain, hippocampus, and entorhinal cortex. Male Wistar rats were exposed to 0, 400, or 800 ppm of aromatic (20 vol.% aromatic hydrocarbons) or dearomatized white spirit (catalytically hydrogenated white spirit) in the inhaled air for 6 h/day, 7 days...

  4. Administrator of 9/11 victim compensation fund to administer Hokie Spirit Memorial Fund distributions

    OpenAIRE

    Hincker, Lawrence

    2007-01-01

    Virginia Tech President Charles Steger has asked Kenneth R. Feinberg, who served as "Special Master of the federal September 11th Victim Compensation Fund of 2001," to administer distributions of the university Hokie Spirit Memorial Fund (HSMF).

  5. Effects of white spirits on rat brain 5-HT receptor functions and synaptic remodeling

    DEFF Research Database (Denmark)

    Lam, Henrik Rye; Plenge, P.; Jørgensen, O.S.

    2001-01-01

    Previously, inhalation exposure to different types of white spirit (i.e. complex mixtures of aliphatic, aromatic, alkyl aromatic, and naphthenic hydrocarbons) has been shown to induce neurochemical effects in rat brains. Especially, the serotonergic system was involved at the global, regional......, and subcellular levels. This study investigates the effects of two types of white spirit on 5-hydroxytryptamine (5-HT) transporters (5-HTT), 5-HT2A and 5-HT4 receptor expression in forebrain, and on neural cell adhesion molecule (NCAM) and 25-kDa synaptosomal associated protein (SNAP-25) concentrations when...... applied as indices for synaptic remodeling in forebrain, hippocampus, and entorhinal cortex. Male Wistar rats were exposed to 0, 400, or 800 ppm of aromatic (20 vol.% aromatic hydrocarbons) or dearomatized white spirit (catalytically hydrogenated white spirit) in the inhaled air for 6 h/day, 7 days...

  6. PENN neurodegenerative disease research - in the spirit of Benjamin Franklin.

    Science.gov (United States)

    Trojanowski, John Q

    2008-01-01

    Benjamin Franklin (1706-1790) was entrepreneur, statesman, supporter of the public good as well as inventor, and his most significant invention was the University of Pennsylvania (PENN). Franklin outlined his plans for a college providing practical and classical instruction to prepare youth for real-world pursuits in his 'Proposals Relating to the Education of Youth in Pensilvania' (1749), and Franklin's spirit of learning to serve society guides PENN to the present day. This is evidenced by the series of articles in this special issue of Neurosignals, describing research conducted by seasoned and newly recruited PENN faculty, addressing consequences of the longevity revolution which defines our epoch at the dawn of this millennium. While aging affects all organ systems, the nervous system is most critical to successful aging. Thus, the articles in this special issue of Neurosignals focus on research at PENN that is designed to prevent or ameliorate aging-related neurodegenerative disorders such as Alzheimer's and Parkinson's disease, amyotrophic lateral sclerosis and frontotemporal dementia. This research could enhance our chances of aging successfully in the continuing longevity revolution, and the essay here provides context and background on this research.

  7. Haunted Headwaters: Ecotourism, Animism, and the Blurry Line Between Science and Spirits

    OpenAIRE

    McCann Gregory; Hsu Yi-Chung

    2014-01-01

    The highlanders of Ratanakiri, Cambodia believe that certain mountains cannot be hunted or logged because they are the abode of powerful spirits. They are convinced that mountain spirits will exact revenge on them in the form of serious injury or illness if they do not follow the animist behavioral etiquette regarding these sacred peaks. It may seem easy to dismiss these convictions as ancient superstitions, and many scientists do because biological explanations can explain the illnesses suff...

  8. Modeling Human Exposure Levels to Airborne Volatile Organic Compounds by the Hebei Spirit Oil Spill

    OpenAIRE

    Kim, Jong Ho; Kwak, Byoung Kyu; Ha, Mina; Cheong, Hae-Kwan; Yi, Jongheop

    2012-01-01

    Objectives The goal was to model and quantify the atmospheric concentrations of volatile organic compounds (VOCs) as the result of the Hebei Spirit oil spill, and to predict whether the exposure levels were abnormally high or not. Methods We developed a model for calculating the airborne concentration of VOCs that are produced in an oil spill accident. The model was applied to a practical situation, namely the Hebei Spirit oil spill. The accuracy of the model was verified by comparing the res...

  9. Usability of small impact craters on small surface areas in crater count dating: Analysing examples from the Harmakhis Vallis outflow channel, Mars

    Science.gov (United States)

    Kukkonen, S.; Kostama, V.-P.

    2018-05-01

    The availability of very high-resolution images has made it possible to extend crater size-frequency distribution studies to small, deca/hectometer-scale craters. This has enabled the dating of small and young surface units, as well as recent, short-time and small-scale geologic processes that have occurred on the units. Usually, however, the higher the spatial resolution of space images is, the smaller area is covered by the images. Thus the use of single, very high-resolution images in crater count age determination may be debatable if the images do not cover the studied region entirely. Here we compare the crater count results for the floor of the Harmakhis Vallis outflow channel obtained from the images of the ConTeXt camera (CTX) and High Resolution Imaging Science Experiment (HiRISE) aboard the Mars Reconnaissance Orbiter (MRO). The CTX images enable crater counts for entire units on the Harmakhis Vallis main valley, whereas the coverage of the higher-resolution HiRISE images is limited and thus the images can only be used to date small parts of the units. Our case study shows that the crater count data based on small impact craters and small surface areas mainly correspond with the crater count data based on larger craters and more extensive counting areas on the same unit. If differences between the results were founded, they could usually be explained by the regional geology. Usually, these differences appeared when at least one cratering model age is missing from either of the crater datasets. On the other hand, we found only a few cases in which the cratering model ages were completely different. We conclude that the crater counts using small impact craters on small counting areas provide useful information about the geological processes which have modified the surface. However, it is important to remember that all the crater counts results obtained from a specific counting area always primarily represent the results from the counting area-not the whole

  10. Morphological Features-Based Descriptive Index System for Lunar Impact Craters

    Directory of Open Access Journals (Sweden)

    Min Chen

    2017-12-01

    Full Text Available Lunar impact craters are important for studying lunar surface morphology because they are the most typical morphological units of the Moon. Impact crater descriptive indices can be used to describe morphological features and thus provide direct evidence for both the current state and evolution history of the Moon. Current description methods for lunar impact craters are predominantly qualitative, and mostly focus on their morphological profiles. Less attention is paid to the detailed morphological features inside and outside of the craters. A well-established and descriptive index system is required to describe the real morphological features of lunar impact craters, which are complex in a systematic way, and further improve study, such as heterogeneity analyses of lunar impact craters. This study employs a detailed lunar surface morphological analysis to propose a descriptive index system for lunar impact craters, including indices for the description of individual craters based on their morphological characteristics, spatial structures and basic composition (i.e., crater rim, crater wall, crater floor, central uplift, and ejecta, and indices for crater groups, including spatial distribution and statistical characteristics. Based on the proposed descriptive index system, a description standard for lunar impact craters is designed for categorising and describing these indices in a structured manner. To test their usability and effectiveness, lunar impact craters from different locations are manually detected, and corresponding values for different indices are extracted and organised for a heterogeneity analysis. The results demonstrate that the proposed index system can effectively depict the basic morphological features and spatial characteristics of lunar impact craters.

  11. Determination of lunar surface ages from crater frequency–size ...

    Indian Academy of Sciences (India)

    ... mission in 1994.Simple techniques of measurement of the diameter of the craters (in pixels)are used and converted into linear dimensions.Among the several maria studied,the results of Mare Humorum and the central region of Mare Imbrium are reported.The results are compared with age estimates from other sources.

  12. Malaria among the pastoral communities of the Ngorongoro Crater ...

    African Journals Online (AJOL)

    Malaria among the pastoral communities of the Ngorongoro Crater Area, northern Tanzania. L.E.G Mboera, R.C Malima, P.E Mangesho, K.P Senkoro, V Mwingira. Abstract. No Abstract. Full Text: EMAIL FREE FULL TEXT EMAIL FREE FULL TEXT · DOWNLOAD FULL TEXT DOWNLOAD FULL TEXT.

  13. Impact cratering – fundamental process in geoscience and planetary ...

    Indian Academy of Sciences (India)

    several planetary objects were mapped, and with the Apollo 11 landing on the Moon, Solar System- wide exploration and scientific analysis had begun. Figure 2. Heavily cratered, ancient highland terrane typ- ical for nearly 85 per cent of the Moon's surface. Photo- graph by the Apollo 16 crew on their flight back to Earth.

  14. Cones and craters on Mount Pavagadh, Deccan Traps: Rootless ...

    Indian Academy of Sciences (India)

    R. Narasimhan (Krishtel eMaging) 1461 1996 Oct 15 13:05:22

    The mountain is surrounded by smaller hills, some of which apparently represent individ- ual satellite vents. Rhyolite outcrops, and volcanic breccia deposits with clear quaquaversal dips, are seen in these hills. Here we describe the shal- low cones with craters that are found on the uppermost mafic lava flow of Mount ...

  15. Role of impact cratering for Mars sample return

    International Nuclear Information System (INIS)

    Schultz, P.H.

    1988-01-01

    The preserved cratering record of Mars indicates that impacts play an important role in deciphering Martian geologic history, whether as a mechanism to modify the lithosphere and atmosphere or as a tool to sample the planet. The various roles of impact cratering in adding a broader understanding of Mars through returned samples are examined. Five broad roles include impact craters as: (1) a process in response to a different planetary localizer environment; (2) a probe for excavating crustal/mantle materials; (3) a possible localizer of magmatic and hydrothermal processes; (4) a chronicle of changes in the volcanic, sedimentary, atmospheric, and cosmic flux history; and (5) a chronometer for extending the geologic time scale to unsampled regions. The evidence for Earth-like processes and very nonlunar styles of volcanism and tectonism may shift the emphasis of a sampling strategy away from equally fundamental issues including crustal composition, unit ages, and climate history. Impact cratering not only played an important active role in the early Martian geologic history, it also provides an important tool for addressing such issues

  16. Impact craters as biospheric microenvironments, Lawn Hill Structure, Northern Australia.

    Science.gov (United States)

    Lindsay, John; Brasier, Martin

    2006-04-01

    Impact craters on Mars act as traps for eolian sediment and in the past may have provided suitable microenvironments that could have supported and preserved a stressed biosphere. If this is so, terrestrial impact structures such as the 18-km-diameter Lawn Hill Structure, in northern Australia, may prove useful as martian analogs. We sampled outcrop and drill core from the carbonate fill of the Lawn Hill Structure and recorded its gamma-log signature. Facies data along with whole rock geochemistry and stable isotope signatures show that the crater fill is an outlier of the Georgina Basin and was formed by impact at, or shortly before, approximately 509-506 million years ago. Subsequently, it was rapidly engulfed by the Middle Cambrian marine transgression, which filled it with shallow marine carbonates and evaporites. The crater formed a protected but restricted microenvironment in which sediments four times the thickness of the nearby basinal succession accumulated. Similar structures, common on the martian surface, may well have acted as biospheric refuges as the planet's water resources declined. Low-pH aqueous environments on Earth similar to those on Mars, while extreme, support diverse ecologies. The architecture of the eolian crater fill would have been defined by long-term ground water cycles resulting from intermittent precipitation in an extremely arid climate. Nutrient recycling, critical to a closed lacustrine sub-ice biosphere, could be provided by eolian transport onto the frozen water surface.

  17. Time/Frequency Analysis of Terrestrial Impack Crater Records

    Directory of Open Access Journals (Sweden)

    Heon-Young Chang

    2006-09-01

    Full Text Available The terrestrial impact cratering record recently has been examined in the time domain by Chang & Moon (2005. It was found that the ˜ 26 Myr periodicity in the impact cratering rate exists over the last ˜ 250 Myrs. Such a periodicity can be found regardless of the lower limit of the diameter up to D ˜ 35 km. It immediately called pros and cons. The aim of this paper is two-fold: (1 to test if reported periodicities can be obtained with an independent method, (2 to see, as attempted earlier, if the phase is modulated. To achieve these goals we employ the time/frequency analysis and for the first time apply this method to the terrestrial impact cratering records. We have confirmed that without exceptions noticeable peaks appear around ˜ 25 Myr, corresponding to a frequency of ˜ 0.04 (Myr^{-1}. We also find periodicities in the data base including small impact craters, which are longer. Though the time/frequency analysis allows us to observe directly phase variations, we cannot find any indications of such changes. Instead, modes display slow variations of power in time. The time/frequency analysis shows a nonstationary behavior of the modes. The power can grow from just above the noise level and then decrease back to its initial level in a time of order of 10 Myrs.

  18. Evidence for gravity scaling and implications for explosion craters

    Energy Technology Data Exchange (ETDEWEB)

    Chabai, A.J.

    1979-01-01

    Crater data have been examined from recent hypervelocity impact and chemical explosion experiments conducted in accelerating frames. Data have been identified from experiments for which the conditions of similitude have been very nearly achieved. Examination of these data from similar experiments indicates that fourth-root or gravity scaling is the rule which best relates crater dimensions to the energy release of impacting projectiles or explosives. Implications for chemical and nuclear explosion cratering are that in model experiments where the gravitational field is constant the specific energy and dimensions of the explosive must be scaled as the fourth-root of explosion energy release. Additionally, medium properties must be appropriately scaled in similar experiments. Because of the impracticability of realizing the constraints imposed on model experiments by similitude requirements attention in future experiments should be focused on the sources of similarity violation and their influence on empirical relationships derived from experiments. Experiments in accelerating frames with both explosive sources and hypervelocity impact projectiles offer one means for investigating effects of similitude violation. To further elucidate the question of crater scaling, experiments in accelerating frames may be conducted which most nearly achieve the conditions of similitude required.

  19. Evidence for gravity scaling and implications for explosion craters

    International Nuclear Information System (INIS)

    Chabai, A.J.

    1979-01-01

    Crater data have been examined from recent hypervelocity impact and chemical explosion experiments conducted in accelerating frames. Data have been identified from experiments for which the conditions of similitude have been very nearly achieved. Examination of these data from similar experiments indicates that fourth-root or gravity scaling is the rule which best relates crater dimensions to the energy release of impacting projectiles or explosives. Implications for chemical and nuclear explosion cratering are that in model experiments where the gravitational field is constant the specific energy and dimensions of the explosive must be scaled as the fourth-root of explosion energy release. Additionally, medium properties must be appropriately scaled in similar experiments. Because of the impracticability of realizing the constraints imposed on model experiments by similitude requirements attention in future experiments should be focused on the sources of similarity violation and their influence on empirical relationships derived from experiments. Experiments in accelerating frames with both explosive sources and hypervelocity impact projectiles offer one means for investigating effects of similitude violation. To further elucidate the question of crater scaling, experiments in accelerating frames may be conducted which most nearly achieve the conditions of similitude required

  20. Impact Crater Experiments for Introductory Physics and Astronomy Laboratories

    Science.gov (United States)

    Claycomb, J. R.

    2009-01-01

    Activity-based collisional analysis is developed for introductory physics and astronomy laboratory experiments. Crushable floral foam is used to investigate the physics of projectiles undergoing completely inelastic collisions with a low-density solid forming impact craters. Simple drop experiments enable determination of the average acceleration,…