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OPP-SOL500-3.jpgRover Tracks - Sol 500 (possible True Colors; credits: Dr G. Barca)60 visitenessun commentoMareKromium
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vo1-PIA00300-PCF-LXTT.jpgOlympus Mons (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)60 visitenessun commentoMareKromium
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SOU-SOL016-PCF-LXTT.jpgUs, beyond the Martian Clouds... - Sol 16 (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunar Explorer Italia)60 visitenessun commentoMareKromium
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PSP_004078_2015_RED_browse-01.jpgLayered Rocks within Becquerel Crater (enhanced natural colors; credits: Lunar Explorer Italia)60 visiteRhythmic bedding in sedimentary bedrock within Becquerel Crater on Mars is suggested by the patterns in this image from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter.
Three dimensional analysis based on stereo pairs of images confirmed the regularity of repetition in the thickness of the beds. In the left half of this image, some of the rhythm is apparent as a series of bundles of about 10 individual layers per bundle. By corresponding to a known 10-to-one pattern in changes in the tilt of Mars' Rotation Axis, this pattern suggests the periodicity in the rock layers results from cyclical changes in the Planet's tilt.
This view covers an area about 1150 meters (0,7 miles) wide. Individual layers in the scence average 3,6 meters (12 feet) thick. The view is presented in enhanced natural colors emphasizing the differing compositions of surface material. Sand trapped in relative low points in the terrain appears grey-blueish. Sedimentary rocks appear brown.
Faulting apparent in the image suggests that the deposits are hardened rock, not softer material. Tilting of the layers in different ways and the surface topography made the three-dimensional analysis necessary for determining the thickness of layers.
This image is a portion of the HiRISE image catalogued as PSP_004078_2015, taken on June 10, 2007.
The location of the imaged area is at 22° North Latitude, 352° East Longitude, within the Arabia Terra Region.MareKromium
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SOL1377-4.jpgRocky Landscape - Sol 1377 (possible True Colors; credits: Dr G. Barca & Lunexit)60 visitenessun commentoMareKromium
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Titan-N00124864.jpgTitan in possible True Colors (credits by Lunar Explorer Italia)60 visiteCaption NASA:"N00124864.jpg was taken on December 05, 2008 and received on Earth December 06, 2008. The camera was pointing toward TITAN that, at the time, was approximately 171.534 Km away.
The image was taken using the CL1 and CB3 filters".MareKromium
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Titan-W00051746.jpgCrescent Titan (possible True Colors; credits: Lunar Explorer Italia)60 visiteCaption NASA:"W00051746.jpg was taken on December 06, 2008 and received on Earth December 06, 2008. The camera was pointing toward TITAN that, at the time, was approx. 313.546 Km away.
The image was taken using the CL1 and CL2 filters".MareKromium
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SNR-Tycho-SR-PIA11435.jpgTycho: the most colourful Supernova Remnant60 visiteThis composite image of the Tycho Supernova Remnant combines InfraRed and X-Ray observations obtained with NASA's Spitzer and Chandra space observatories, respectively, and the Calar Alto observatory, Spain.
It shows the scene more than four centuries after the brilliant star explosion witnessed by Tycho Brahe and other astronomers of that era.
The explosion has left a blazing hot cloud of expanding debris (green and yellow). The location of the blast's outer shock wave can be seen as a blue sphere of ultra-energetic electrons. Newly synthesized dust in the ejected material and heated pre-existing dust from the area around the supernova radiate at infrared wavelengths of 24 microns (red).
Foreground and background stars in the image are white.MareKromium
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PSP_004085_1420_PSP_004019_1420_RED_browse.jpgMultiple Levels of Gullies (3D and possible True Colors; credits: NASA and Lunar Explorer Italia)60 visiteThis image shows groups of gullies at different elevations on the same crater wall. Although gullies are common in the mid-latitudes of Mars, they are rarely found to exist at such distinct elevations as visible here.
The mounds on the floor, one of which contains gullies, probably formed during a late stage of crater formation. Both levels of gullies appear to originate at layers. These layers might be ice-rich, or they might be capable of conducting water to the surface. The anaglyph image, providing a three-dimensional perspective, reveals the relative depth of the gullies in the crater walls and amount of alluvial material deposited at the bottom of the gullies.
The gullies visible here are good candidates for formation by subsurface water, as opposed to melting ice or snow originating on the surface. The rounded, theater-shaped alcove and tributary heads are typical of features formed by groundwater sapping on Earth. Surface runoff does not form this morphology.
This image contains possible evidence of subsurface piping, when soil pores connect to form a "pipe" that transports water. When piping occurs, water carries soil with it, leaving empty space beneath the surface. As this process continues, the overlying surface can no longer support itself, and it collapses to form a depression. Several depressions that could have formed this way are seen in this image. The depressions are also directly upslope of more developed alcoves. They also originate at upslope layers, and might be examples of developing alcoves.
Mars Local Time: 15:21 (early afternoon)
Coord. (centered): 37,9° South Lat. and 169,6° East Long.
Spacecraft altitude: 268,5 Km (such as about 167,8 miles)
Original image scale range: 26,9 cm/pixel (with 1 x 1 binning) so objects ~81 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 20,6°
Phase Angle: 24,7°
Solar Incidence Angle: 45° (meaning that the Sun is about 45° above the Local Horizon)
Solar Longitude: 255,0° (Northern Autumn)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009442_2030_red.jpgAntoniadi Crater (possible True Colors; credits: Lunar Explorer Italia)60 visiteMars Local Time: 15:22 (early afternoon)
Coord. (centered): 22,9° North Lat. and 53,5° East Long.
Spacecraft altitude: 282,0 Km (such as about 176,2 miles)
Original image scale range: 56,4 cm/pixel (with 1 x 1 binning) so objects ~1,69 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,3°
Phase Angle: 46,1°
Solar Incidence Angle: 46° (meaning that the Sun is about 44° above the Local Horizon)
Solar Longitude: 106,5° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Moonrise.JPGMoonrise over Lick Observatory60 visitenessun commentoMareKromium
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Enceladus-PIA11133.jpgCrescent Enceladus (possible True Colors; credits: Lunar Explorer Italia)60 visiteCaption NASA:"On Oct. 5, 2008, just after coming within 25 kilometers (15.6 miles) of the surface of Enceladus, NASA's Cassini captured this stunning mosaic as the Spacecraft sped away from this geologically active moon of Saturn.
Craters and cratered terrains are rare in this view of the Southern Region of the moon's Saturn-facing Hemisphere. Instead, the surface is replete with fractures, folds, and ridges — all hallmarks of remarkable tectonic activity for a relatively small world. In this True Colors view, regions that appear blueish are thought to be coated with larger grains than those that appear white or gray.
Portions of the Tiger Stripe Fractures, or Sulci, are visible along the Terminator at lower right, surrounded by a circumpolar belt of mountains. The icy moon's famed jets emanate from at least 8 distinct Source Regions, which lie on or near the Tiger Stripes. However, in this view, the most prominent feature is Labtayt Sulci, the approximately one-kilometer (such as 0,6 miles) deep Northward-trending chasm located just above the center of the mosaic.
Near the top, the conspicuous ridges are Ebony and Cufa Dorsae. This mosaic was created from 28 images obtained at seven footprints, or pointing positions, by Cassini's narrow-angle camera. At each footprint, 4 images using filters sensitive to UltraViolet (UV), Visible (V) and InfraRed light (IR) - spanning wavelengths from 338 to 930 nanometers) were combined to create the individual frames. The mosaic is an orthographic projection centered at 64,49° South Lat. and 283,87° West Long., and it has an image scale of 196 Km (about 122,5 miles) per pixel. The original images ranged in resolution from 180 meters (594 feet) to 288 meters (950 feet) per pixel and were acquired at distances ranging from 30.000 to 48.000 Km (such as from about 18.750 to 30.000 miles) as the Spacecraft receded from Enceladus.
The view was acquired at a Sun-Enceladus-spacecraft, or phase, angle of 73°".MareKromium
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