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Dione-PIA07638.jpgDione: Carthage Linea61 visiteDione's icy surface is scarred by craters and sliced up by multiple generations of geologically-young bright fractures. Numerous fine, roughly-parallel linear grooves run across the terrain in the upper left corner. Most of the craters seen here have bright walls and dark deposits of material on their floors. As on other Saturnian moons, rockslides on Dione may reveal cleaner ice, while the darker materials accumulate in areas of lower topography and lower slope (e.g. crater floors and the bases of scarps).
The terrain seen here is centered at 15,4° North Latitude, 330,3° West Longitude, in a Region called Carthage Linea. North on Dione is up and rotated 50° to the left.
The image was taken in visible green light with the Cassini narrow-angle camera on Oct. 11, 2005, at a distance of approx. 19.600 Km (roughly 12.200 miles) from Dione. The image scale is about 230 mt (760 feet) per pixel".
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Dione-PIA07748.jpgThe surface of Dione from about 4486 Km65 visiteThe terrain in this image is located within a 60-Km-wide impact crater along the feature called Padua Linea. The western rim of the encompassing crater runs from the middle left to the upper right. The crater's central peak can be seen at the lower right. Multiple generations of fractures are visible here. Numerous fine, roughly parallel linear grooves run across the terrain from top to bottom and are interrupted by the larger, irregular bright fractures. In several places, fractures postdate some deposits in the bottoms of craters that are not badly degraded by time. Such a fracture, for example, runs from the center toward the upper right. Most of the craters seen here have bright walls and dark deposits of material on their floors. As on other Saturnian moons, rockslides on Dione may reveal cleaner ice, while the darker materials accumulate in areas of lower topography and lower slope (e.g. crater floors and the bases of scarps). This view is centered on terrain near 11° South lat. and 238° West long.
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ESP_017581_1765_RED_abrowse.jpgExposed Light Material in Upland Region in Aureum Chaos (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)127 visiteThe Plateau visible in this image is located within Aureum Chaos. Chaotic Terrains on Mars are blocky, fractured regions of flat-topped hills, plateaus, plains and depressions thought to have formed by the collapse of the heavily cratered uplands.
Large Outflow Channels appear to emerge from Aureum Chaos and other Chaotic Terrains leading researchers to posit that these large collapse regions were formed by the catastrophic release of ground water. Aureum Chaos is located just to the North-East of Valles Marineris adjacent to Margaritifer Terra, and it has a diameter of approximately 368 kilometers.
The steep-sided Plateau in this image has a sharp, undulating surface possibly etched out and eroded by persistent winds. These same winds may well have transported the resulting sediment to the surrounding plains helping to form the Dunes below. The Plateau slopes are steep and consist of a series of parallel bright, more resistant cliff forming layers and darker, less resistant slope material. A good way to see the differences in color between the plateau's bright layered deposits and the surrounding area is to look at some of the blocks that have fallen off the cliff onto the the dark sands below.
By studying areas of Mars such as this one, researchers hope to understand how the chaos regions formed and how their formation related to the release of ground water to form the outflow channels, if indeed the two are connected in this way.
Written by: Shawn Hart and Ginny GulickMareKromium
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ESP_022195_1335_RED_abrowse-Slope_Linea-PCF-LXTT-2.jpgTransient "Slope Linea Formation" in a well-preserved Unnameed Southern Crater (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)215 visiteAcquisition date: 21 April 2011
Mars Local Time (M.L.T.): 14:48 (Early Afternoon)
Latitude (centered): 45,9° North
Longitude (East): 9,5°
Range to Target Site (Spacecraft Altitude): 250,9 Km (156,8 miles)
Original Image Scale Range: 25,1 cm/pixel (with 1 x 1 binning) so objects ~75 cm across are resolved
Map Projected Scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 2,0°
Sun-Crater-Spacecraft Angle (Phase Angle): 37,9°
Solar Incidence Angle (S.AI.A.): 40° (with the Sun about 50° above the Local Horizon)
Solar Longitude: 278,5° (Northern Winter)
MareKromium
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Linear_Ridges-PCF-LXTT-1.jpgLinear Ridges (Enhanced Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)56 visitenessun commentoMareKromium
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MartianTerminator-TRA_000841_1300_RED.jpgHalf in the light and half in the darkness... (possible True Colors; credis: Lunar Explorer Italia)53 visiteCaption NASA originale:"Image TRA_000841_1300 was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard the Mars Reconnaissance Orbiter spacecraft on October 1, 2006. The complete image is centered at 49,7° South Lat. and 154,2° East Long. The range to the target site was 248,4 Km (such as about 155,3 miles).
At this distance the image scale is 99,4 cm/pixel (with 4 x 4 binning) so objects ~298 cm across are resolved. The image shown here has been map-projected to 100 cm/pixel and North is up. The image was taken at a MLT of 15:39 and the scene is illuminated from the West with a solar incidence angle of 87°, thus the Sun was about 3° above the horizon.
At a Solar Longitude of 114,2°, the season on Mars is Northern Summer". MareKromium
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PSP_008598_2155_RED_abrowse~0.jpgLineated Valley Fill in Coloe Fossae (MULTISPECTRUM; credits: Lunexit)65 visiteThis Region consists of several relatively straight and narrow canyons located near the boundary between the high-standing, heavily cratered areas of the Southern Hemisphere and the low, uncratered plains that cover most of the Northern Hemisphere of Mars.
Transitional areas such as this are known as the “Fretted Terrain” and are characterized by a complicated mix of cliffs, mesas, buttes, and canyons.
This image reveals a canyon with relatively steep and smooth walls. The floor of the canyon displays a complex set of ridges and grooves that are generally parallel to the canyon walls.
The material comprising the canyon floor is common observed in Fretted Terrain and is called "Lineated Valley Fill" (LVF).
The cause of the LVF texture is not well understood but may result from patterns of ice rich soils or ice loss. The linear alignment may be caused by the downhill movement of ice-rich soil, or glacial flow in dirty ice or ice-rich soil.MareKromium
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SOL671-MF.jpg"Rocky Line-up"... - Sol 671 (3D - credits: Dr M. Faccin)80 visiteSoltanto pietre?!? Forse. O forse no.
Guardate bene, nel detail mgnf in basso, la seconda da Sx: illusione ottica, o la roccia presenta una crepa frontale da cui è uscito "qualcosa"?...MareKromium
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ZZ-Mercury-Terminator-PIA14357.jpgMercurian Terminator (credits for the additional process. and color.: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington)79 visiteCaption NASA:"The Terminator of Mercury, shown here in color, is the line between light and dark, or day and night. On Mercury, three days are equivalent to two years or, in other words, the Planet spins around its axis three times for every two orbits around the Sun. The first Mercury year of the MESSENGER mission ended on Monday, June 13, 2011".
Date acquired: June 07, 2011
Image Mission Elapsed Time (MET): 215945273, 215943853, 215945277
Image ID: 349804, 349803, 349805
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 9 (1000 nanometers), 7 (750 nanometers), 6 (430 nanometers)
Center Latitude: 79,32° South
Center Longitude: 173,9° East
Resolution: 1715 meters/pixel
Scale: the approximate width of the image is 1840 KmMareKromium
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ZZ-Mercury-Terminator-PIA17229-PCF-LXTT-IPF.jpgSouthern Terminator (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)96 visiteThis image-mosaic was created by combining two frames that were taken only 96 seconds apart from each other. It is obvious that the NASA - MESSENGER Spacecraft has to be farther away from the Planet Mercury (and, precisely, it must be in the Southern portion of its orbit) to acquire views like these. Mercury's heavily Cratered Surface is very well and really dramatically highlighted here - particularly in the Regions near the Terminator (such as the Boundary Line existing between the Sunlit Dayside and the Dark Nightside of the Planet) -, thus reflecting its, in a way, "violent" history; an history which saw this always mysterious and fascinating Celestial Body being impacted by thousands and thousands of objects (i.e.: Meteors, Comets and, probably, even a few small Asteroids), through the ages.
Date acquired: May 7th, 2013
Images Mission Elapsed Time (MET): 10234404, 10234500
Images ID: 4021801, 4021802
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 60,00° South
Center Longitude: 260,00° East
This picture (which is an Original NASA - MESSENGER Spacecraft's b/w Map-Projected frame published on the NASA - Planetary Photojournal with the ID n. PIA 17229) has been additionally processed, contrast enhanced, magnified and then colorized in Absolute Natural Colors (such as the colors that a human eye would actually perceive if someone were onboard the NASA - MESSENGER Spacecraft and then looked down, towards the Surface of Mercury), by using an original technique created - and, in time, dramatically improved - by the Lunar Explorer Italia Team. Different colors, as well as different shades of the same color, mean, among other things, the existence of different Elements (Minerals) present on the Surface of Mercury, each having a different Albedo (---> Reflectivity) and Chemical Composition.MareKromium
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