2 edition of A spectral survey of the Crisium basin region of the Moon found in the catalog.
A spectral survey of the Crisium basin region of the Moon
by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va
Written in English
|Statement||D.T. Blewett ... [et al.].|
|Series||[NASA contractor report] -- NASA-CR-204593., NASA contractor report -- NASA CR-204593.|
|Contributions||Blewett, D. T., United States. National Aeronautics and Space Administration.|
|The Physical Object|
Multispectral images obtained during the Galileo probe's second encounter with the moon reveal the compositional nature of the north polar regions and the northeastern limb. Mare deposits in these regions are found to be primarily low to medium titanium lavas and, as on the western limb, show only slight spectral heterogeneity. properties was examined in each basin and among the basins. DATA The lunar Digital Image Model (DIM) produced from Clementine UV/VIS data by the U. S. Geological Survey (Eliason et al. ; Isbell et al. ) was used in this study. This DIM consists of 5 spectral bands (– nm) and is.
Sinus Iridum, the Copernicus Crater, and the pyroclastic deposit in the volcanic vents in the southeast of Orientale Basin were selected as the study areas. Olivine distribution was surveyed, and the relative Fo# calculation of olivine was implemented based on Moon Mineralogy Mapper (M 3) data. Results demonstrated that olivine in the crater. Spudis P.D. () Inventory of multi-ring basins on the Moon after the Clementine mission Meteorit Bussey D.B.J. and Spudis P.D. () A compositional study of lunar sinuous rilles. Lunar Planet. Sci. XXVII,
The Apollo orbital geochemistry, photogeologic, and other remote sensing data sets were used to identify and characterize geochemical anomalies on the eastern limb and farside of the Moon and to investigate the processes responsible for their formation. The anomalies are located in the following regions: (1) Balmer basin, (2) terrain northeast of Mare Smythii, (3) near Langemak crater, (4. In addition to band analysis, spectral mixing models based on the results of principal components analysis of a group of Crisium spectra were conducted. The results of the spectral work invited further study at higher spatial resolution. Such data sets for the Moon have been provided by CCD cameras operating in the extended visible range (
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A spectral survey of the Crisium basin region of the Moon D. Blewett, B. Hawke, and P. Lucey PlanetaryGeosciences. Hawaii Instituteof Geophysics &Planetology,SOEST,Universityof Hawaii, Honolulu P. Spudis Lunar & PlanetaryInstitute.
Houston, Texas Abstract. The Crisium basin region harbors a number of in. A Spectral Survey of the Crisium Basin Region of the Moon GEOPHYSICAL RESEARCH LETTERS, NO. 22, PAGESNOVEM. A spectral survey of the Crisium basin region of the Moon D.
B lewett, B. Hawke, and P. Lucey. Get this from a library. A spectral survey of the Crisium basin region of the Moon. [D T Blewett; United States. National Aeronautics and Space Administration.;]. So, while the results of this survey offer some insight, until we pay Crisium and the moon’s other basins a visit, the solar system’s earliest days.
The Crisium basin region harbors a number of interesting features, including geochemical and radar anomalies, light plains units and possible hidden mare deposits (cryptomaria). This report presents preliminary results of a telescopic near-infrared spectral study concerning a variety of surface units in the Crisium region.
A spectral survey of the Crisium Basin Region of the Moon - NASA/ADS The Crisium basin region harbors a number of interesting features, including geochemical and radar anomalies, light plains units and possible hidden mare deposits (cryptomaria).
The geology of the Crisium basin has been studied previously [e.g., Wilhelms and El‐Baz, ; Wilhelms, ; Spudis, ], but new high‐resolution images from the Lunar Reconnaissance Orbiter and compositional data from the Clementine and Lunar Prospector missions permit a more detailed study of this region.
Crisium is a multiring. Laboratory studies of this sample provide information that is used to understand the source region on the moon using remote sensing data. spectral survey of the Crisium Basin Region of the Moon, Geophysical Research Letters, /95GL, 22, 22, (), (). Wiley Online Library.
Paul D. Spudis, B. Ray Hawke, Paul Lucey. Mare Crisium basin is a multi-ring basin lies in the northeastern portion of the lunar near side in between latitude of 10° and 30° N and longitude of 50° and 70° E.
Mare Crisium basin has km in diameter with the aerial coverage of 1,76, square kilometers ().The Main ring diameter is about km and it is one of the deepest basin ( km) on the lunar surface which is filled with. Sometime after the solar system formed billion years ago, a projectile slammed into Earth’s youthful moon and formed the mile-wide indentation known as the Crisium basin.
No one knows exactly when this impact happened, but for decades scientists have been trying to solve the puzzle as part of a larger debate over whether the moon and, by proxy, Earth endured a period of frenzied.
Crisium. At Crisium basin we identified 60 spectra with signatures that represent olivine-bearing mixtures, with an average olivine content of 14 wt.% for all olivine-bearing spectra. These spectra are located on the rims of small craters, on massifs at the rim of Crisium, and on mare both inside and outside of Crisium basin (Fig.
8a). The Crisium basin is a Nectarian-age multi-ring impact structure on the eastern nearside of the Moon. Its interior is covered by mare basalt from a protracted period of volcanism over Ga SPECTRAL SURVEY OF CRTSIUM REGION: Blewett D.T.
et al. morphological considerations, led to the suggestion that the light plains NE of Taruntius were formed by the extrusion of post-Crisium Basin mare units followed by contamination of these deposits by highlands material [lo, Spectra for two spots on the plains have band minima.
A spectral. survey of th e Crisium basin region of the Moo n. Geop hys. Res. Lett., 22 New geological mapping of the Crisium basin on the Moon has revealed exposures of the basin. Mare Anguis / ˈ æ ŋ ɡ w ɪ s / (Latin anguis, the "serpent sea") is a lunar mare located on the near side of the Moon, about kilometers in diameter.
Located within the Crisium basin, Mare Anguis is a part of the Nectarian System, meaning that it was formed during the Nectarian time period. Like most mare, the surface of Mare Anguis is dark, indicating that it has been filled with.
Abstract— Clementine UV/VIS multi-spectral data were used to map mare deposits in the eastern lunar nearside region (Mare Tranquillitatis, Mare Fecunditatis, Mare Serenitatis, Mare Crisium, Mare. Extensive regions with densities lower than average are found surrounding the impact basins Orientale and Moscoviense, which are the two largest young impact basins on the Moon's farside hemisphere.
The bulk density determinations are robust to changes in size of the analysis region by a factor of two and are robust to changes in the spectral. David T. Blewett joined the Planetary Exploration Group at the Johns Hopkins University Applied Physics Laboratory in Prior to that he was a Principal Scientist at NovaSol, a small employee-owned high-tech company in Honolulu, Hawaii of which he was a co-founder.
The Crisium basin is a Nectarian-age multi-ring impact structure on the eastern nearside of the Moon. Its interior is covered by mare basalt from a protracted period of volcanism over Ga The abundance in its inner mare basalt ranges from ppm to.
The previously published version of the USGS spectral library (Clark et al., ) is the leading database used by the global scientific community to identify materials by their "spectral fingerprints." The library is fundamental for Mineral Resources Program projects to characterize mineral resources with imaging spectrometer data.
A large spectral survey of small lunar craters: Implications for the composition of the lunar mantle† Basin depth-diameter ratios used in the models required to match the measured composition are consistent with prior estimates for the largest basins. The composition found in the SPA and Imbrium regions are consistent with mafic impact.
The nearside and farside of the Moon are compositionally distinct. The detection of low-calcium pyroxene around large impact basins suggests that the huge Procellarum basin .Spudis, P.
D., Hawke, B. R. & Lucey, P. G. Proc. of 18th Lunar and PlanetarySubsequently, we have conducted an areal survey around the Spectral Profiler Science Conference – (Cambridge Univ.
Press, ).detection points by using Multiband Imager multispectral images with the same