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SOL1230-1.jpgDeep inside "The Mark" - Sol 1230 (Superdefinition + MULTISPECTRUM; credits: Dr G. Barca & Lunexit)60 visitenessun commentoMareKromium
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as14-66-09323.jpgAS 14-66-9323 - A little look, out of the Window60 visiteCaption NASA:"Photo out Ed's (Mitchell) window, showing the TV Camera and the S-Band Antenna". MareKromium
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as10-27-3924.jpgAS 10-27-3924 - Mare Crisium (Special Processing by Lunexit)60 visitenessun commentoMareKromium
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as10-27-3945.jpgAS 10-27-3945 - Mare Australe and Mare Nectaris (Special Processing by Lunexit)60 visitenessun commentoMareKromium
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Atlas-PIA09818.jpgIn the Night...60 visiteCaption NASA:"Two of Saturn's ring moons draw close momentarily, before the inner of the pair moves off alone.
Atlas passes Prometheus (about 86 Km, or approx. 53 miles across, at center left) about once a month, then slowly and steadily pulls ahead of its slower moving sibling.
This view looks toward the unilluminated side of the Rings from about 23° above the Ring-Plane. The image was taken in visible light with the Cassini spacecraft narrow-angle camera on April 6, 2008. The view was acquired at a distance of approx. 1,6 MKN (such as about 975.000 miles) from Atlas.
Image scale is roughly 9 Km (about 6 miles) per pixel".MareKromium
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Weather-PIA10672.gifClear Skies over the Northern Regions (GIF-Movie; credits: NASA)60 visiteScientists are anticipating clear skies when NASA's Phoenix Mars Lander arrives on the north polar plains of the Red Planet Sunday, May 25, 2008.
This orbital view of the north polar region of Mars, where NASA's Phoenix Mars Lander will land, shows clear skies as of May 22, 2008. Mission planners are always on the lookout for dust storms in daily weather updates like this one, provided by the Mars Color Imager on NASA's Mars Reconnaissance Orbiter. Based on current conditions, they are predicting good weather when Phoenix arrives May 25, 2008.
Temperature profiles, used to calculate atmospheric density, are also updated on a regular basis, provided by the Mars Climate Sounder, another instrument on the Mars Reconnaissance Orbiter. Atmospheric density was well within expectations as of May 22, 2008. Mission planners will continue to receive updates on weather and atmospheric conditions prior to landing.
The animated orbital view shows recent weather conditions from May 16 to May 22, 2008, as tracked by the Mars Color Imager on NASA's Mars Reconnaissance Orbiter. A cloud of dust kicked up by Martian winds traveled from west to east between May 19 and May 22, 2008, passing over Phoenix's landing site. The dust cloud was about 500 kilometers (300 miles) from head to tail and made the skies somewhat hazy. Since then, the dust has been replaced by clear skies, indicating that Phoenix will not land in any dust clouds, which are a common occurrence in the northern latitudes of Mars.
MareKromium
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SunFlare-prom1743_eit_big.jpgA Twisted Solar Eruptive Prominence60 visiteCaption NASA:"Ten Earths could easily fit in the "claw" of this seemingly solar monster. The monster, though, visible on the lower left, is a huge Eruptive Prominence seen moving out from our Sun. The above dramatic image taken early in the year 2000 by the Sun-orbiting SOHO satellite. This large prominence, though, is significant not only for its size, but its shape. The twisted figure eight shape indicates that a complex magnetic field threads through the emerging solar particles. Differential rotation inside the Sun might help account for the surface explosion.
Although large prominences and energetic Coronal Mass Ejections (CMEs) are relatively rare, they are occurred more frequently near Solar Maximum, the time of peak sunspot and solar activity in the eleven-year Solar Cycle".MareKromium
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ZZ-Mercury-Terminator-PIA10609.jpgMercurian Rupes (MULTISPECTRUM; credits: Lunexit)60 visiteWhen MESSENGER flew by Mercury on January 14, 2008, the Mercury Dual Imaging System (MDIS) snapped images of a large portion of Mercury's surface that had not been previously seen by spacecraft. On these images, new examples of long cliffs were identified and viewed for the first time. This image, taken by the Narrow Angle Camera (NAC), shows one of those cliffs in the bottom right corner. The cliff can be followed from the bottom edge of the image, cutting through and deforming an impact crater, and curving out of the image frame on the middle right edge.
This cliff is the northern continuation of the cliff visible in the images previously released on January 16 (PIA10174) and January 27 (PIA10194). This image shows an area of Mercury's surface about 200 Km (about 125 miles) across, and by tracing this cliff through the three images, it can be seen that it extends for hundreds of kilometers.
Cliffs that mark geologic escarpments on Mercury are called "rupes", which is simply the Latin word for cliff. On Mercury, rupes are named after the ships of famous explorers, and names include Discovery Rupes, for a ship of Captain Cook, Santa Maria Rupes, for a ship of Christopher Columbus, and Victoria Rupes, for a ship of Ferdinand Magellan. (The word rupes is both singular and plural).
The MESSENGER Team proposed to the International Astronomical Union, which has the final say on all names of landforms on planets and satellites, that this cliff be named the Beagle Rupes, after the ship on which naturalist Charles Darwin sailed around the world.
Today the MESSENGER Team received word that the proposed name has received formal approval.
Image Mission Elapsed Time (MET): 108827037
MareKromium
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Enceladus-PIA10403.jpgIcy Oasis (MULTISPECTRUM-2; credits: Lunexit)60 visiteCaption NASA:"With its excess warmth, water ice jets and huge vapor plume laced with simple organic materials, Enceladus is an important part of the quest to understand environments compatible with the chemistry of life as we know it. The Sulci, or "Tiger Stripe" fractures, in the South Polar Region are visible at bottom -- the view here is parallel to the direction of the Sulci.
The view looks toward the anti-Saturn Hemisphere on the moon's Trailing Side. North on Enceladus is towards the top of the image.
This view is a composite of individual frames obtained using filters sensitive to ultraviolet (centered at 338 nanometers), green (centered at 568 nanometers) and infrared light (centered at 1002 nanometers).
The broad range of wavelengths exaggerates subtle color variations across the moon's surface.
The images were acquired with the Cassini spacecraft narrow-angle camera on May 11, 2008.
The view was obtained at a distance of approx. 739.000 Km (such as about 459.000 miles) from Enceladus and at Phase Angle of 36°.
Image scale is roughly 4 Km (about 2,5 miles) per pixel".MareKromium
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OPP-SOL1530-Panorama-1.jpgVictoria's Paving - Sol 1530 (Photomosaic + MULTISPECTRUM; credits: Dr G. Barca & Lunexit)60 visitenessun commentoMareKromium
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Janus-PIA10407.jpgJanus60 visiteCaption NASA:"Craters cover the rugged surface of Saturn's moon Janus. The view is from 42° above the moon's Equator. North on Janus (179 Km, or 111 miles across) is towards the top of the image.
The image was taken with the Cassini Spacecraft narrow-angle camera on May 17, 2008 using a combination of spectral filters sensitive to wavelengths of polarized green light centered at 617 and 568 nanometers. The view was acquired at a distance of approx. 350.000 Km (such as about 217.000 miles) from Janus and at a Sun-Janus-Spacecraft, or phase, angle of 101°.
Image scale is roughly 2 Km (a little more than 1 mile) per pixel".MareKromium
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PSP_008426_2595_RED_abrowse-01.jpgPolygons, Crater Layers, and Defrosting Dunes (edm n. 1 - MULTISPECTRUM-2; credits: Lunexit)60 visiteThe dune morphology in this image is complex. Because of the presence of the ice, it is difficult to determine all of the dune types. These jumbled dunes may result from erosion of the layers within the crater walls that act as a dune source. However, two common types of dunes can be classified: the outer ring of the dune field is composed of chains of Barchan Dunes whereas the central area of the field contains transverse dunes.
Barchans are characterized by their crescent-shape with steep horns in the downwind direction. The transverse dunes have asymmetric, nearly parallel ridges and are oriented perpendicular to the wind direction.MareKromium
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