Mars Reconnaissance Orbiter (MRO)
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Psp_009502_1980_red.jpgDark Spot Near Olmpus Mons Volcano (natural colors; credits: Lunexit)52 visiteThis image covers a relatively dark-toned patch of ground West of the Olympus Mons volcano. This spot is one of several "Dark Areas" in this Region of Mars.
These Dark Spots are distinctive because much of the surrounding area appears to be covered by light-toned dust.
In pre-HiRISE images, the origin of this Dark Spot was ambiguous. This HiRISE image reveals that the dark color is likely the result of accumulations of Basaltic Sand (smooth, brown-colored material in this natural color view) on top of otherwise relatively dust-free bedrock.
Evidence of layering is also visible within the dark area. There are alternating bands of lighter- and darker-toned material, consistent with alternating layers of bedrock. These alternating bands are not apparent outside of the Dark Area. This may mean that alternating layers of bedrock only occur within the dark area, or that these bedrock layers occur throughout the region but are covered and obscured by light-toned dust outside of the Dark Area.MareKromium
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Psp_009501_1755_red.jpgTube-Fed Lava Flow Field (natural colors; credits: Lunexit)52 visiteThis Lava Flow Field is part of a Small Shield Volcano within the Lava Plains South of Pavonis Mons. It illustrates the importance of Lava Tubes in the formation of large lava flow fields.
Shield Volcanoes are often covered by a combination of open Lava Channels and partly enclosed Lava Tubes, through which lava once flowed when the volcano was active. Tubes are often located axial to topographic ridges, and after a Lava Flow ends, a tube can drain leaving an empty space into which the roof can collapse.
However, if a tube is filled to capacity or under pressure when the lava is flowing, narrow ridge-like features and/or small Lava Flow breakouts can form.
This scenario is one possible explanation for the Ridged Lava Flow in the center of this image.
Here, a narrow wall-like feature is axial to a larger topographic ridge that appears to be the source for a series of smaller Lava Flows.MareKromium
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Psp_009497_2210_red.jpgEroded Mesa in Western Cydonia Region (possible True Colors; credits: Lunar Explorer Italia)53 visiteMars Local Time: 15:25 (early afternoon)
Coord. (centered): 40,7 North Lat. and 351,0 East Long.
Spacecraft altitude: 307,8 Km (such as about 192,4 miles)
Original image scale range: 30,8 cm/pixel (with 1 x 1 binning) so objects ~92 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 14,8
Phase Angle: 31,0
Solar Incidence Angle: 46 (meaning that the Sun is about 44 above the Local Horizon)
Solar Longitude: 108,5 (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009492_3080_red.jpgNorthern Surface (possible True Colors; credits: Lunar Explorer Italia)52 visiteMars Local Time: 15:41 (middle afternoon)
Coord. (centered): 51,8 North Lat. and 304,8 East Long.
Spacecraft altitude: 304,5 Km (such as about 190,3 miles)
Original image scale range: 121,8 cm/pixel (with 1 x 1 binning) so objects ~3,66 mt across are resolved
Map projected scale: 1 mt/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,3
Phase Angle: 90,0
Solar Incidence Angle: 90 (meaning that the Sun is about 0 above the Local Horizon)
Solar Longitude: 108,3 (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009488_2485_red.jpgPhoenix Landing Site (possible True Colors; credits: Lunar Explorer Italia)53 visiteMars Local Time: 15:23 (early afternoon)
Coord. (centered): 68,2 North Lat. and 234,3 East Long.
Spacecraft altitude: 338,8 Km (such as about 211,8 miles)
Original image scale range: 67,8 cm/pixel (with 1 x 1 binning) so objects ~2,03 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 24,2
Phase Angle: 33,2
Solar Incidence Angle: 54 (meaning that the Sun is about 36 above the Local Horizon)
Solar Longitude: 108,2 (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009480_2265_red.jpgLayers and Scallops (True Colors; credits: Lunar Explorer Italia)63 visiteMars Local Time: 15:10 (early afternoon)
Coord. (centered): 45,9 North Lat. and 91,1 East Long.
Spacecraft altitude: 306,6 Km (such as about 191,6 miles)
Original image scale range: 30,7 cm/pixel (with 1 x 1 binning) so objects ~92 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 11,8
Phase Angle: 55,8
Solar Incidence Angle: 44 (meaning that the Sun is about 46 above the Local Horizon)
Solar Longitude: 107,9 (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009478_1770_red.jpgCratered Cones in Zephyria Planum (False Colors; credits: Lunar Explorer Italia)52 visiteMars Local Time: 15:21 (early afternoon)
Coord. (centered): 3,1 South Lat. and 152,3 East Long.
Spacecraft altitude: 286,5 Km (such as about 179,0 miles)
Original image scale range: 28,7 cm/pixel (with 1 x 1 binning) so objects ~86 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 20,4
Phase Angle: 72,7
Solar Incidence Angle: 56 (meaning that the Sun is about 34 above the Local Horizon)
Solar Longitude: 107,8 (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009474_1705_red.jpgWater Bearing Minerals in Noctis Labyrinthus (natural colors; credits: Lunexit)52 visiteNoctis Labyrinthus consists of a series of Pits on the western end of the large Valles Marineris Canyon System.
The HiRISE camera and the CRISM Spectrometer have revealed that the floors of some of these Pits exhibit layered rocks, or strata, that contain minerals with water. These Pits were formed several billion years ago, therefore the rocks and sediments on their floors record evidence of water during this period of Mars history.
The walls of the Pits are commonly covered with dust and other loose sediments that form dunes and dune-like forms, and in many cases the floors of the pits are also covered with these materials. This image shows an example of light-toned layers exposed beneath these sediments and dunes, and CRISM data show that these layers have hydrated minerals.
The dark-brown/orange tones in this natural color image correspond to areas with more Pyroxene, a mineral found in volcanic rocks and Martian Dust. Some Pits, such as this one, appear to have deposits associated with large landslides that are younger than the hydrated minerals and partially bury them.MareKromium
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Psp_009468_2385_red.jpgCentral Peak of an Unnamed Crater in the Northern Plains (possible True Colors; credits: Lunar Explorer Italia)59 visiteMars Local Time: 15:13 (early afternoon)
Coord. (centered): 57,9 North Lat. and 58,7 East Long.
Spacecraft altitude: 310,8 Km (such as about 194,2 miles)
Original image scale range: 31,1 cm/pixel (with 1 x 1 binning) so objects ~93 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 6,1
Phase Angle: 42,5
Solar Incidence Angle: 48 (meaning that the Sun is about 42 above the Local Horizon)
Solar Longitude: 107,4 (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009461_2470_red.jpgMonitoring the Northern Plains (possible True Colors; credits: Lunar Explorer Italia)58 visiteMars Local Time: 15:01 (early afternoon)
Coord. (centered): 66,9 North Lat. and 246,0 East Long.
Spacecraft altitude: 312,6 Km (such as about 195,4 miles)
Original image scale range: 31,3 cm/pixel (with 1 x 1 binning) so objects ~62,6 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,3
Phase Angle: 51,4
Solar Incidence Angle: 51 (meaning that the Sun is about 39 above the Local Horizon)
Solar Longitude: 107,2 (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009460_2665_red.jpgSmall Crater on the North Polar Permanent Cap (possible True Colors; credits: Lunar Explorer Italia)52 visiteMars Local Time: 12:06 (early afternoon)
Coord. (centered): 86,5 North Lat. and 227,9 East Long.
Spacecraft altitude: 317,5 Km (such as about 198,4 miles)
Original image scale range: 31,8 cm/pixel (with 1 x 1 binning) so objects ~95 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,2
Phase Angle: 62,6
Solar Incidence Angle: 62 (meaning that the Sun is about 28 above the Local Horizon)
Solar Longitude: 107,2 (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009460_1745_red.jpgCeti Mensa (edm - natural colors; credits: Lunexit)53 visiteThis image gives us another clue to the formation of Ceti Mensa. Close-up examination shows fine banding in the layers of Ceti Mensa that is exposed by the ongoing erosion. The banding is produced by alternating bright and dark material. The thickness of the individual bands ranges from a few meters down to the resolution limit of the image, a few tens of centimeters. The bands are parallel, although they appear wavy on the irregular, eroded surface.
The banding visible in this image most closely resembles terrestrial lake deposits and similar rocks formed in aqueous, low energy depositional environments. Structures such as cross-bedding that are hallmarks of wind-deposited sediments are absent, as are cobbles and clasts that are typical of glacial sediments. If this interpretation is correct, the thickness of Ceti Mensa suggests formation in standing bodies of water that were several kilometers deep.MareKromium
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