| Piú viste - The Clementine Files |
Moon_Full-STB.jpg026 - Earthshine55 visitenessun commento
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Froelich&LovelaceCrater-NIR.gif080 - Froelich Crater55 visitenessun commento
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ZZ-Southside-Clem.jpg011 - The Southern Side of the Moon55 visitenessun commento
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Tycho-1.jpg201 - Tycho Crater55 visitenessun commento
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Tycho-2.jpg202 - Tycho Crater55 visitenessun commento
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Ukert-2.jpg141 - Ukert Crater55 visitenessun commento
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NorthPoleoftheMoon.JPG114 - North Polar Region (in natural colors)55 visitenessun commento
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034-The Moon from Clem-PolarAreas.jpg110 - Polar Areas: the Peaks of Eternal Light54 visiteAs Clementine flew over the Pole - every 5 hours - it began its photographic mapping pass by imaging the Pole. These images are composites, showing the addition of alternate orbit polar images over the course of 1 Lunar Day (such as 1 Earth month). In these composite maps, areas in permanent darkness are black, while areas of permanent illumination are white; areas of mixed lighting condition are represented in various shades of gray. Note that the South Polar Area has the largest area of permanent darkness, measuring more than 15,000 square kilometers. The north pole shows only about 500 square kilometers of darkness. Several areas are evident that have near-constant Sun illumination. Such zones would have great value as sites for a permanent lunar outpost.
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Rydberg Crater.JPG191 - Rydberg Crater54 visiteRydberg crater mosaic imaged by the UV/VIS camera from an altitude of about 485 Km. Rydberg is located at 47° North Lat. and 97° West Long.
Strip width is about 50 Km.
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Plato Crater.JPG091 - Plato Crater54 visitePlato crater imaged by the UV/VIS camera at 1 micron, from an altitude of about 485 Km.
Plato is situated at 51° North Lat. and 9° West Long.; North is up. The strip width of this mosaic is about 90 Km.
The smallest craters visible are roughly 600 meters across.
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Moon-Clem.JPG015 - The Moon (visible and near-infrared)54 visiteOne of the major scientific goals of the Clementine mission is to map the Moon in 11 different wavelengths in the visible and near-infrared parts of the spectrum. The filter colors of the Clementine cameras were carefully chosen to differentiate types of lunar surface material. In our first look at the global color, each Clementine image made by the UV/VIS camera has been reduced to its average value, producing a picture of the Moon at low resolution (about 50 kilometers per pixel). These pictures show the albedo (brightness) and color of the Moon from three aspects: the Earth-centered view (near side) with a 0 degree central longitude, and two far side views with 120 degrees East and 120 degrees West central longitudes. These images have been made by assigning colors to the relative reflectance values obtained through various filters, resulting in a map showing the compositional variation of the Moon.
Major compositional provinces in the highlands are evident. The large dark red-gray region on the far side is the South Pole-Aitken basin, an ancient impact feature that apparently contains rocks of distinct composition. A newly discovered compositional anomaly on the east limb of the Moon (pink area near center of 120 degrees East image) may be related to ancient flows of lava. The color picture shows that very high titanium lavas (deep blue and cyan colors) appear to be largely confined to the Oceanus Procellarum, Mare Imbrium, and Mare Tranquillitatis areas (near side). These views of the Moon in three colors only hint at the scientific richness contained within the Clementine global data, which will be investigated for years to come.
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NorthPoleoftheMoon.JPG114 - North Polar Region54 visiteThis shows a 630-Km long mosaic of the Northern Polar Region along the 180° West Longitude line from 69° to 90° North Latitude.
Imaged by the UV/VIS camera.
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