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  • 1
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    Mapping the Apollo 17 landing site area based on Lunar Reconnaissance Orbiter Camera images and Apollo surface photography (2012)
    Wiley
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    Publikationsdatum: 2012-05-15
    Beschreibung: Newly acquired high resolution Lunar Reconnaissance Orbiter Camera (LROC) images allow accurate determination of the coordinates of Apollo hardware, sampling stations, and photographic viewpoints. In particular, the positions from where the Apollo 17 astronauts recorded panoramic image series, at the so-called “traverse stations”, were precisely determined for traverse path reconstruction. We analyzed observations made in Apollo surface photography as well as orthorectified orbital images (0.5 m/pixel) and Digital Terrain Models (DTMs) (1.5 m/pixel and 100 m/pixel) derived from LROC Narrow Angle Camera (NAC) and Wide Angle Camera (WAC) images. Key features captured in the Apollo panoramic sequences were identified in LROC NAC orthoimages. Angular directions of these features were measured in the panoramic images and fitted to the NAC orthoimage by applying least squares techniques. As a result, we obtained the surface panoramic camera positions to within 50 cm. At the same time, the camera orientations, North azimuth angles and distances to nearby features of interest were also determined. Here, initial results are shown for traverse station 1 (northwest of Steno Crater) as well as the Apollo Lunar Surface Experiment Package (ALSEP) area.
    Print ISSN: 0148-0227
    Thema: Geologie und Paläontologie , Physik
    Publiziert von Wiley im Namen von American Geophysical Union (AGU).
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  • 2
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    Morphometric analysis of small-scale lobate scarps on the Moon using data from the Lunar Reconnaissance Orbiter (2012)
    Wiley
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    Publikationsdatum: 2012-03-07
    Beschreibung: Prior to Lunar Reconnaissance Orbiter (LRO), the morphology and dimensions of only a limited number of lobate scarps, all located near the equator (within 21°), had been characterized. Topography derived from LRO Camera stereo images and Lunar Orbiter Laser Altimeter (LOLA) ranging is used to measure the relief and analyze the morphology of previously known and newly detected low and high latitude lobate scarps. The asymmetric profiles and maximum slopes on scarp faces (∼5° to 29°) of lunar lobate scarps are similar to those of lobate scarps observed on Mars and Mercury. Scarp lengths range from ∼0.6 to 21.6 km (mean = ∼6.0 km, median = ∼4.4 km, n = 79), and measured relief ranges from ∼5 to 150 m (mean = ∼35 m, median = ∼20 m, n = 26). Assuming a range of 20° to 40° for the fault plane dip, estimated lower limits for the horizontal shortening (S) expressed by the lobate scarp thrust faults range from ∼10 to 410 m. The range in S estimated for the lunar scarps is roughly an order of magnitude lower than estimates of S for lobate scarp thrust faults on Mars and Mercury. The relatively small range of S estimated for the growing number of well-characterized lunar scarps is consistent with a small amount of global contraction.
    Print ISSN: 0148-0227
    Thema: Geologie und Paläontologie , Physik
    Publiziert von Wiley im Namen von American Geophysical Union (AGU).
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  • 3
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    GLD100: The near-global lunar 100 m raster DTM from LROC WAC stereo image data (2012)
    Wiley
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    Publikationsdatum: 2012-03-30
    Beschreibung: We derived near-global lunar topography from stereo image data acquired by the Wide-angle Camera (WAC) of the Lunar Reconnaissance Orbiter Camera (LROC) system. From polar orbit tracks, the LROC WAC provides image data with a mean ground resolution at nadir of 75 m/pixel with substantial cross-track stereo overlap. WAC stereo images from the one-year nominal mission and the first months of the science mission phase are combined to produce a near-global digital terrain model (DTM) with a pixel spacing of 100 m, the Global Lunar DTM 100 m, or “GLD100.” It covers 79°S to 79°N latitudes, 98.2% of the entire lunar surface. We compare the GLD100 with results from previous stereo and altimetry-based products, particularly with the Lunar Orbiter Laser Altimeter (LOLA) altimetry, which is the current topographic reference for the Moon. We describe typical characteristics of the GLD100 and, based upon the comparison to the LOLA data set, assess its vertical and lateral resolution and accuracy. We conclude that the introduced first version of the stereo-based GLD100 is a valuable topographic representation of the lunar surface, complementary to the LOLA altimetry data set. Further improvements can be expected from continuative investigations.
    Print ISSN: 0148-0227
    Thema: Geologie und Paläontologie , Physik
    Publiziert von Wiley im Namen von American Geophysical Union (AGU).
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  • 4
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    How old are young lunar craters? (2012)
    Wiley
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    Publikationsdatum: 2012-02-21
    Beschreibung: The accurate definition of the lunar cratering chronology is important for deriving absolute model ages across the lunar surface and throughout the Solar System. Images from the Lunar Reconnaissance Orbiter Narrow Angle Cameras and Wide-Angle Camera and the SELENE/Kaguya Terrain Camera provide new opportunities to investigate crater size-frequency distributions (CSFDs) on individual geological units at lunar impact craters. We report new CSFD measurements for the Copernican-aged craters North Ray, Tycho, and Copernicus, which are crucial anchor points for the lunar cratering chronology. We also discuss possible reasons for an age discrepancy observed between the impact melt and ejecta units. Our CSFDs for North Ray and Tycho crater ejecta deposits are consistent with earlier measurements. However, for Copernicus crater and one of its rays, we find significantly lower cumulative crater frequencies than previous studies. Our new results for Copernicus crater fit the existing lunar absolute chronologies significantly better than the previous counts. Our derived model ages of the ejecta blankets of North Ray, Tycho, and Copernicus agree well with radiometric and exposure ages of the Apollo 16, 17, and 12 landing sites, respectively, and are generally consistent with a constant impact rate over the last 3 Ga. However, small variations of the impact rate cannot be resolved in our data and require further investigations.
    Print ISSN: 0148-0227
    Thema: Geologie und Paläontologie , Physik
    Publiziert von Wiley im Namen von American Geophysical Union (AGU).
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  • 5
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    Evidence for basaltic volcanism on the Moon within the past 100 million years (2014)
    Springer Nature
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    Publikationsdatum: 2014-10-31
    Beschreibung: Nature Geoscience 7, 787 (2014). doi:10.1038/ngeo2252 Authors: S. E. Braden, J. D. Stopar, M. S. Robinson, S. J. Lawrence, C. H. van der Bogert & H. Hiesinger The bulk of basaltic magmatism on the Moon occurred from 3.9 to 3.1 billion years ago on the ancient lunar mare plains. There is evidence for basaltic volcanism as recently as 2.9 billion years ago from crystallization ages and a billion years ago from stratigraphy. An enigmatic surface formation named Ina (18.65° N, 5.30° E) may represent much younger mare volcanism, but age estimates are poorly constrained. Here we investigate 70 small topographic anomalies, termed irregular mare patches (100–5,000 m maximum dimension), on the lunar nearside with irregular morphologies and textures similar to Ina, using Lunar Reconnaissance Orbiter narrow angle camera images, digital terrain models and wide angle camera colour ratios. The irregular mare patches exhibit sharp, metre-scale morphology with relatively few superposed impact craters larger than ten metres in diameter. Crater distributions from the three largest irregular mare patches imply ages younger than 100 million years, based on chronology models of the lunar surface. The morphology of the features is also consistent with small basaltic eruptions that occurred significantly after the established cessation of lunar mare basaltic volcanism. Such late-stage eruptions suggest a long decline of lunar volcanism and constrain models of the Moon’s thermal evolution.
    Print ISSN: 1752-0894
    Digitale ISSN: 1752-0908
    Thema: Geologie und Paläontologie
    Publiziert von Springer Nature
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  • 6
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    Resolved Hapke Parameter Maps of the Moon (2014)
    Wiley
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    Publikationsdatum: 2014-07-03
    Beschreibung: We derived spatially resolved near-global Hapke photometric parameter maps of the Moon from 21 months of Lunar Reconnaissance Orbiter Camera (LROC) Wide Angle Camera (WAC) multispectral observations using a novel " tile-by-tile" method (1° latitude by 1°longitude bins). The derived six parameters ( w , b , c , B S 0 , h S , ) for each tile were used to normalize the observed reflectance (standard angles i  =  g  = 60°, e  = 0° instead of the traditional angles i  =  g  = 30°, e = 0°) within each tile, resulting in accurate normalization optimized for the local photometric response. Each pixel in the seven-color near-global mosaic (70°S to 70°N and 0°E to 360°E) was computed by the median of normalized reflectance from large numbers of repeated observations (UV: ~50, visible: ~126 on average). The derived mosaic exhibits no significant artifacts with latitude or along the tile boundaries demonstrating the quality of the normalization procedure. The derived Hapke parameter maps reveal regional photometric response variations across the lunar surface. The b , c (Henyey-Greenstein double-lobed phase function parameters) maps demonstrate decreased backscattering in the maria relative to the highlands (except 321 nm band), probably due to the higher content of both SMFe (sub-micron iron) and ilmenite in the interiors of back scattering agglutinates in the maria. The h S (angular width of shadow hiding opposition effect) map exhibits relatively lower values in the maria than the highlands, and slightly higher values for immature highland crater ejecta, possibly related to the variation in a grain size distribution of regolith.
    Print ISSN: 0148-0227
    Thema: Geologie und Paläontologie , Physik
    Publiziert von Wiley im Namen von American Geophysical Union (AGU).
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  • 7
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    Reflectance and color variations on Mercury: regolith processes and compositional heterogeneity (2008)
    American Association for the Advancement of Science (AAAS)
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    Publikationsdatum: 2008-07-05
    Beschreibung: Multispectral images of Mercury obtained by the MESSENGER spacecraft reveal that its surface has an overall relatively low reflectance with three large-scale units identified on the basis of reflectance and slope (0.4 to 1.0 micrometer). A higher-reflectance, relatively red material occurs as a distinct class of smooth plains that were likely emplaced volcanically; a lower-reflectance material with a lesser spectral slope may represent a distinct crustal component enriched in opaque minerals, possibly more common at depth. A spectrally intermediate terrain probably forms most of the upper crust. Three other spectrally distinct but spatially restricted units include fresh crater ejecta less affected by space weathering than other surface materials; high-reflectance deposits seen in some crater floors; and moderately high-reflectance, relatively reddish material associated with rimless depressions.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Robinson, Mark S -- Murchie, Scott L -- Blewett, David T -- Domingue, Deborah L -- Hawkins, S Edward 3rd -- Head, James W -- Holsclaw, Gregory M -- McClintock, William E -- McCoy, Timothy J -- McNutt, Ralph L Jr -- Prockter, Louise M -- Solomon, Sean C -- Watters, Thomas R -- New York, N.Y. -- Science. 2008 Jul 4;321(5885):66-9. doi: 10.1126/science.1160080.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA. robinson@ser.asu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18599770" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Digitale ISSN: 1095-9203
    Thema: Biologie , Chemie und Pharmazie , Informatik , Medizin , Allgemeine Naturwissenschaft , Physik
    Publiziert von American Association for the Advancement of Science (AAAS)
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  • 8
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    Recalibrated Mariner 10 Color Mosaics: Implications for Mercurian Volcanism (1997)
    American Association for the Advancement of Science (AAAS)
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    Publikationsdatum: 1997-01-10
    Beschreibung: Recalibration of Mariner 10 color image data allows the identification of distinct color units on the mercurian surface. We analyze these data in terms of opaque mineral abundance, iron content, and soil maturity and find color units consistent with the presence of volcanic deposits on Mercury's surface. Additionally, materials associated with some impact craters have been excavated from a layer interpreted to be deficient in opaque minerals within the crust, possibly analogous to the lunar anorthosite crust. These observations suggest that Mercury has undergone complex differentiation like the other terrestrial planets and the Earth's moon.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Robinson -- Lucey -- New York, N.Y. -- Science. 1997 Jan 10;275(5297):197-200.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉M. S. Robinson, United States Geological Survey, 2255 North Gemini Drive, Flagstaff, Arizona, 86001, USA. P. G. Lucey, Hawaii Institute of Geophysics and Planetology, University of Hawaii, Honolulu, HI 96822, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/8985010" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Digitale ISSN: 1095-9203
    Thema: Biologie , Chemie und Pharmazie , Informatik , Medizin , Allgemeine Naturwissenschaft , Physik
    Publiziert von American Association for the Advancement of Science (AAAS)
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  • 9
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    The South pole region of the moon as seen by clementine (1994)
    American Association for the Advancement of Science (AAAS)
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    Publikationsdatum: 1994-12-16
    Beschreibung: The Clementine mission has provided the first comprehensive set of high-resolution images of the south pole region of the moon. Within 5 degrees of latitude of the pole, an area of an estimated 30,000 square kilometers remained in shadow during a full lunar rotation and is a promising target for future exploration for ice deposits. The Schrodinger Basin (320 kilometers in diameter), centered at 75 degrees S, is one of the two youngest, least modified, great multiring impact basins on the moon. A large maar-type volcano localized along a graben within the Schrodinger Basin probably erupted between 1 and 2 billion years ago.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Shoemaker, E M -- Robinson, M S -- Eliason, E M -- New York, N.Y. -- Science. 1994 Dec 16;266(5192):1851-4.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17737080" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Digitale ISSN: 1095-9203
    Thema: Biologie , Chemie und Pharmazie , Informatik , Medizin , Allgemeine Naturwissenschaft , Physik
    Publiziert von American Association for the Advancement of Science (AAAS)
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  • 10
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    Clementine observations of the aristarchus region of the moon (1994)
    American Association for the Advancement of Science (AAAS)
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    Publikationsdatum: 1994-12-16
    Beschreibung: Multispectral and topographic data acquired by the Clementine spacecraft provide information on the composition and geologic history of the Aristarchus region of the moon. Altimetry profiles show the Aristarchus plateau dipping about 1 degrees to the north-northwest and rising about 2 kilometers above the surrounding lavas of Oceanus Procellarum to the south. Dark, reddish pyroclastic glass covers the plateau to average depths of 10 to 30 meters, as determined from the estimated excavation depths of 100- to 1000-meter-diameter craters that have exposed materials below the pyroclastics. These craters and the walls of sinuous rilles also show that mare basalts underlie the pyroclastics across much of the plateau. Near-infrared images of Aristarchus crater reveal olivine-rich materials and two kilometer-sized outcrops of anorthosite in the central peaks. The anorthosite could be either a derivative of local magnesium-suite magmatism or a remnant of the ferroan anorthosite crust that formed over the primordial magma ocean.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉McEwen, A S -- Robinson, M S -- Eliason, E M -- Lucey, P G -- Duxbury, T C -- Spudis, P D -- New York, N.Y. -- Science. 1994 Dec 16;266(5192):1858-62.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17737082" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Digitale ISSN: 1095-9203
    Thema: Biologie , Chemie und Pharmazie , Informatik , Medizin , Allgemeine Naturwissenschaft , Physik
    Publiziert von American Association for the Advancement of Science (AAAS)
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