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Erathostenes.jpg221 - Wallace and Erathostenes "A" and "B"60 visitenessun commento
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040-The Moon from Clem-Apollo 16 LandingSite.jpg216-0 - The Apollo 16 "Landing Site" (in natural colors)59 visiteThis is the Apollo 16 Landing Site as seen from Clementine. This is a natural color rendition of the site. Clementine images were deliberately taken at very low phase angles (which means high Sun angles) to emphasize color differences, so surface textures are much less apparent here than in the orbital Apollo view.
Note the very bright appearance of South Ray and North Ray Craters (center right).
Promemoria: l'angolo "di fase" è l'angolo formato da Sole, corpo/rilievo ripreso e Sonda.
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003-The Moon and Venus from Clem.JPG021 - The Moon, Solar Corona and Venus59 visiteThis color-enhanced image of Venus, the solar corona, and the Moon was acquired by the Startracker.
The Terminator between the dark side of the Moon and the Earth-lit side can also be seen.
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FarSideAlbedo.jpg006 - Farside Albedo59 visiteGlobal map of the albedo from the 750-nanometer filter of the Clementine UV-VIS camera and this is the FarSide of the Moon, shown in Lambert equal-area projection.
Note the lack of maria on the FarSide, as compared to the NearSide.
The relatively dark area at center-bottom outlines the extent of the South Pole-Aitken Basin. This view has been subsampled to a resolution of about 1 Km per pixel, about 5 times lower than the full-resolution data.
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017-The Moon from Clem-NearSide-PIA00302.jpg003 - The Near-Side of the Moon58 visiteAbout 50.000 Clem images were processed to produce the 4 orthographic views of the Moon. Images PIA00302, PIA00303, PIA00304 and PIA00305 show albedo variations (normalized brightness or reflectivity) of the surface at a wavelength of 750 nm (just longward of visible red). The Lunar Near-Side is a contrast between dark and light albedo surfaces that has been fancied as the "Man in the Moon". Lunar terrain types are still designated by their 17th century name and that is:
1. Maria (dark albedo features also known as basins) and
2. Terra (brighter albedo features also known as uplands or highlands).
The Maria constitutes about 16% while the Terra 84% of the Lunar Surface. The nearside is composed of about 30 percent maria. Extensive bright ray systems surround craters Copernicus (upper left center) and Tycho (near bottom).
Studies have shown that two major processes, impact and basaltic volcanism have shaped the major physical features of the Lunar Surface.
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051-The Moon from Clem-Aristarchus.jpg043 - Aristarchus Plateau (natural colors)58 visiteA mosaic of more than 250 images showing the complex and diverse Aristarchus Region of the Moon in approximately natural colors (blue = 415 nanometers, green = 750 nanometers, red = 950 nanometers). The plateau is an uplifted block of complex, highland terrain, partly flooded by later mare basalt lavas. Dark, pyroclastic glasses partly cover the uplifted terrain. The crater Aristarchus (47 Km in diameter) has formed in the South-East corner of the plateau, excavating both highlands and mare rocks.
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052-The Moon from Clem-Dionysus.jpg061 - Dionysius Crater (natural colors)58 visiteThe Crater Dionysius (3° North Lat. and, 17° East Long.; western edge of Mare Tranquillitatis; 18 Km in diameter) shows striking contrasts in albedo. The outside of the Crater is a very bright halo in its near-rim field, while farther out, darker material is exposed, including rare dark rays. Crater deposits on the left side of this mosaic are on light Cayley plains of highland composition, while deposits on the right side are on the basalts of Mare Tranquillitatis.
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009-The Moon from Clem-Corona.JPG022 - Solar Corona58 visiteThe Earth-lit Moon, The Sun's corona, and - to the far right - Venus, are visible in this color-enhanced Startracker image. The Mare Humorum is the dark circular mare at the center of the lunar disk.
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Copernicus Crater.JPG053 - Copernicus Crater (mosaic)58 visiteMosaic of the lunar crater Copernicus produced using images obtained by the Clementine UV/VIS camera. This 95-km crater, believed to be approximately 800 million years old, is located near the center of the lunar nearside and exhibits prominent rays extending in all directions. The right section of the image is a color composite mosaic of the eastern half of Copernicus. This color mosaic was prepared using images obtained through filters of three different colors chosen to allow small lunar color differences to be mapped in a geologic context. In this image, the color assignments are: red (750/415 nm), green ( 750/950 nm), and blue (415/750 nm). The left section of the image is a mosaic of the same area prepared using frames obtained through a single filter (750 nm). This mosaic is displayed as a mirror image to the color composite to allow easy comparison of geologic features and their color.
Extensive large- and small-scale heterogeneity of materials excavated by this large crater is readily evident from the color composite mosaic. Bright blue tones typically suggest fresh material similar to Apollo 16 rocks and breccias, mottled red-orange tones indicate material similar to Apollo 16 soils, vivid red is associated with deposits of impact melt (seen most prominently in the northwestern part of the crater floor), and green-yellow tones along the southern wall imply a higher abundance of iron-bearing materials.
Impact craters can be used as windows into the interior and this multispectral image of Copernicus provides dramatic new information about how materials are excavated, melted, mixed, and deposited in a major impact event. The extensive heterogeneity around the wall of the crater indicates materials are not intimately mixed in spite of the huge energy involved during crater formation. Similarly, impact melt (target rock melted during the impact event) is not distributed uniformly, but can be seen to be concentrated in large sections of the floor and in small areas along ledges of the walls.
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015-The Moon from Clem-FarSide-PIA00304.jpg002 - The Far-Side of the Moon57 visiteClementine Project Information
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Clementine was a joint project between the Strategic Defense Initiative Organization and NASA. The objective of the mission was to test sensors and spacecraft components under extended exposure to the space environment and to make scientific observations of the Moon and the near-Earth asteroid 1620 Geographos. The observations included imaging at various wavelengths including ultraviolet and infrared, laser ranging altimetry, and charged particle measurements. These observations were originally for the purposes of assessing the surface mineralogy of the Moon and Geographos, obtaining lunar altimetry from 60N to 60S latitude, and determining the size, shape, rotational characteristics, surface properties, and cratering statistics of Geographos.
Clementine was launched on 25 January 1994 at 16:34 UTC (12:34 PM EDT) from Vandenberg AFB aboard a Titan IIG rocket. After two Earth flybys, lunar insertion was achieved on February 21. Lunar mapping took place over approximately two months, in two parts. The first part consisted of a 5 hour elliptical polar orbit with a perilune of about 400 km at 28 degrees S latitude. After one month of mapping the orbit was rotated to a perilune of 29 degrees N latitude, where it remained for one more month. This allowed global imaging as well as altimetry coverage from 60 degrees S to 60 degrees N.
After leaving lunar orbit, a malfunction in one of the on-board computers on May 7 at 14:39 UTC (9:39 AM EST) caused a thruster to fire until it had used up all of its fuel, leaving the spacecraft spinning at about 80 RPM with no spin control. This made the planned continuation of the mission, a flyby of the near-Earth asteroid Geographos, impossible. The spacecraft remained in geocentric orbit and continued testing the spacecraft components until the end of mission.
More information on the Clementine mission, instruments, and early results can also be found in the Clementine special issue of Science magazine, Vol. 266, No. 5192, December 1994.
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020-The Moon from Clem-Solar Corona.jpg023 - Solar Corona57 visiteImage of the Moon taken by the Star Tracker camera onboard Clementine. The bright glow over the horizon is the Solar Corona (outer atmosphere) showing from behind the Moon. Craters at left are illuminated by Earthshine, the light reflected off the Earth and onto the Moon. The dark part of the Moon is on the Lunar Far-Side. Do not equate "Dark-Side" with "Far-Side": the Far-Side experiences the same day-night cycle (28 days) as the Near-Side.
It just happens to be night on the Far-Side in this image.
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023-The Moon from Clem-SchroendingerBasin.jpg045 - Schroedinger Basin (detail mgnf)57 visiteDetail from the UV-VIS Clementine Camera of the floor of the basin Schrodinger, showing the coverage (inset strip) of the HR camera for comparison. The Dark Halo Crater (center at 76° South Lat. and 139° East Long.; 5 Km across) is a volcanic vent that erupted ash during the period of mare volcanism on the Moon, more than 3,5 BY ago.
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