Mars Reconnaissance Orbiter (MRO)
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Psp_008779_1905_red.jpgThe Head of Athabasca Valles (natural colors; credits: Lunexit)54 visiteThis observation is located at the head of the Athabasca Valles Channel System, which lies just North of Mars’ Equator, in a low-elevation Region known as Elysium Planitia.
Athabasca Valles has an interesting geologic history. It was probably carved by one or more catastrophic floods of water, but more recently, a flood of lava coursed through the channel system. Both the water and the lava erupted from a few discrete points (or “vents”) along the Cerberus Fossae, a 1600-Km(1000-mile) long network of extensional (or “normal”) faults. The two prominent troughs that cut across the Southern end of this HiRISE image are part of the Cerberus Fossae. They are distinct fault segments that overlap at their tips, as one tapers in and the other pinches out.
They were not always as wide as they are today. Erosional processes have widened the troughs over time. Major eruptions occurred along both of the fault segments seen in this image, though they occurred to either side of the imaged area itself. Lava that erupted from the western vent covers the northern half of the image. The lava has raised, lobate margins and is slightly darker in tone than the older cratered plains it embays. The lava also has a banded appearance of subtly contrasting lighter and darker tones, that correspond to variations in surface roughness.
The bands are concentric to a vent located immediately west of the imaged area. Unfortunately, vents along the Cerberus Fossae are not well preserved.MareKromium
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Psp_008891_2050_red.jpgCharacterize Surface Hazards and Science of Possible MSL Rover Landing - Mawrth Vallis (natural colors; credits: Lunexit)54 visitenessun commentoMareKromium
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Psp_008982_1965_red.jpgLayered Deposits in Arabia Terra Region (natural colors; credits: Lunexit)56 visiteThis image shows the floor of an Unnamed Impact Crater in Arabia Terra that has Layered Deposits. There are many craters in this Region, where layering is observed.
These layers are often exposed along the sides of large isolated mounds, small knobs and mesas, and other positive relief features. In some cases, the layering is expressed as narrow sinuous ridge-like structures along crater floors.
The presence of Layered Deposits is of particular interest because these materials are not likely to be related to the impact event, but rather post-impact infill of the Crater. Modification of the Deposits has now revealed layers of material.
HiRISE and other instruments onboard the Mars Reconnaissance Orbiter may provide more clues to the origin of the these deposits.MareKromium
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Psp_009011_1705_red.jpg"Apparent Valley", West of Ganges Chasma (natural colors; credits: Lunexit)60 visiteThis image shows an "Apparent Valley" North of a 37-Km long pit called Ophir Cavus. This valley is just West of another 155-Km long valley system called Allegheny Vallis, that also emanates from the pit.
The association of valleys with the pit suggests that water was released when the pit formed, perhaps when volcanic eruptions melted ice in the surface or subsurface.
The HiRISE image reveals light-toned units along portions of the plains and these could be minerals deposited by the flowing water or alteration of the plains by the water that once flowed here.MareKromium
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Psp_009029_1430_red.jpgDeposits in Electris Region (natural colors; credits: Lunexit)63 visiteThis observation reveals a portion of a long outcrop of a deposit in the Electris Region of Mars.
The Electris' Deposits occur over a range of landforms and relief and the process(es) responsible for their emplacement remain speculative.
Close examination of the outcrops reveal layering that in some places appear to include meter-scale blocks. Comparison with other HiRISE images of the deposit will enable more detailed mapping of its extent and nature and should provide new insight into the origin of these enigmatic materials.MareKromium
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Psp_009207_1765_red.jpgCharacterize Surface Hazards and Science of MSL Rover Landing Site - Equatorial Regions/Meridiani Planum (natural colors; credits: Lunexit)69 visitenessun commentoMareKromium
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Psp_009317_1980_red~0.jpgPortion of the Southern Wall of Olympus Mons Caldera (Absolute Natural Colors; credits for the additional process. and color: Dr Paolo C. Fienga - Lunexit Team)133 visiteMars Local Time: 15:21 (early afternoon)
Coord. (centered): 17,8° North Lat. and 226,6° East Long.
Spacecraft altitude: 259,3 Km (such as about 162,1 miles)
Original image scale range: 51,9 cm/pixel (with 1 x 1 binning) so objects ~1,56 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 3,3°
Phase Angle: 50,1°
Solar Incidence Angle: 47° (meaning that the Sun is about 43° above the Local Horizon)
Solar Longitude: 102,1° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Dr Paolo C. Fienga - Lunar Explorer Italia MareKromium
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Psp_009319_1650_red.jpgDust Devil Tracks in Gusev Crater (Extremely Enhanced Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)58 visiteGusev Crater is decorated by tracks made by Dust Devils that have been observed by the Mars Exploration Rover Spirit, Mars Orbiter Camera (MOC), and HiRISE images.
Dust Devils are of interest because they may clean the Solar Panels that provide power to Spirit, and are partially responsible for dust transportation on the surface of Mars.
Dust Devils are actually giant convective vortices that form as a result of atmospheric vertical instability. Solar radiation warms the surface, forcing air to rise to an atmospheric convective boundary, where it then cools. The denser, cold air parcel descends and generates a circulation that creates a suction effect.
As the Dust Devil picks up material from the bright dust-mantled surface, it exposes the darker basaltic substrate. These scribble marks will follow the prevailing winds and tend to cluster together as the lower albedo surface heats up more quickly.
Scientists are trying to understand the relationship between Dust Devils and craters and other topographic features that generate multiple wind directions.MareKromium
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Psp_009342_2650_red.jpgNorthern Dunes (possible True Colors; credits: Lunar Explorer Italia)55 visiteMars Local Time: 13:43 (early afternoon)
Coord. (centered): 84,9° North Lat. and 234,4° East Long.
Spacecraft altitude: 319,4 Km (such as about 199,6 miles)
Original image scale range: 32,0 cm/pixel (with 1 x 1 binning) so objects ~96 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 6,5°
Phase Angle: 55,9°
Solar Incidence Angle: 61° (meaning that the Sun is about 29° above the Local Horizon)
Solar Longitude: 103,0° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009346_1985_red.jpgThila Crater (extremely enhanced natural colors; credits: Lunar Explorer Italia)54 visiteMars Local Time: 15:24 (early afternoon)
Coord. (centered): 18,1° North Lat. and 155,5° East Long.
Spacecraft altitude: 284,2 Km (such as about 177,6 miles)
Original image scale range: 28,4 cm/pixel (with 1 x 1 binning) so objects ~85 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 6,0°
Phase Angle: 42,3°
Solar Incidence Angle: 48° (meaning that the Sun is about 42° above the Local Horizon)
Solar Longitude: 103,1° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009352_1770_red.jpgLight Toned Materials and Plains in Southern Meridiani Planum (Extremely Enhanced Natural Colors; credits: Lunexit)54 visitenessun commentoMareKromium
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Psp_009353_1550_red~0.jpgLadon Valles (possible True Colors; credits: Lunar Explorer Italia)54 visiteMars Local Time: 15:30 (middle afternoon)
Coord. (centered): 24,6° South Lat. and 329,1° East Long.
Spacecraft altitude: 261,2 Km (such as about 163,3 miles)
Original image scale range: 52,3 cm/pixel (with 1 x 1 binning) so objects ~1,57 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 2,5°
Phase Angle: 72,6°
Solar Incidence Angle: 71° (meaning that the Sun is about 19° above the Local Horizon)
Solar Longitude: 103,4° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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