Mars Reconnaissance Orbiter (MRO)
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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_009492_3080_red.jpgNorthern Surface (possible True Colors; credits: Lunar Explorer Italia)53 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_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_009501_1755_red.jpgTube-Fed Lava Flow Field (natural colors; credits: Lunexit)53 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_009502_1980_red.jpgDark Spot Near Olmpus Mons Volcano (natural colors; credits: Lunexit)53 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_009505_1755_red.jpgThe Floor of Gale Crater (natural colors; credits: Lunexit)53 visitenessun commentoMareKromium
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Psp_009510_1825_red.jpgUnnamed Crater with Deposits in Meridiani Planum (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunar Explorer Italia)53 visiteMars Local Time: 15:28 (early afternoon)
Coord. (centered): 2,4° North Lat. and 359,9° West Long.
Spacecraft altitude: 272,1 Km (such as about 170,1 miles)
Original image scale range: 27,2 cm/pixel (with 1 x 1 binning) so objects ~82 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 4,1°
Phase Angle: 51,3°
Solar Incidence Angle: 55° (meaning that the Sun is about 35° above the Local Horizon)
Solar Longitude: 108,9° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009513_1810_red.jpgEchus Chasma (Enxtrelmely Enhanced Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunar Explorer Italia)54 visiteMars Local Time: 15:28 (early afternoon)
Coord. (centered): 1,1° North Lat. and 278,0° East Long.
Spacecraft altitude: 266,2 Km (such as about 166,4 miles)
Original image scale range: 53,3 cm/pixel (with 1 x 1 binning) so objects ~1,60 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 2,8°
Phase Angle: 53,0°
Solar Incidence Angle: 55° (meaning that the Sun is about 35° above the Local Horizon)
Solar Longitude: 109,0° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009520_1520_red.jpgVery recent small Impact Crater near Hadriaca Patera (Enhanced and Saturated Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunar Explorer Italia)55 visiteMars Local Time: 15:35 (middle afternoon)
Coord. (centered): 27,9° South Lat. and 90,7° East Long.
Spacecraft altitude: 256,9 Km (such as about 160,5 miles)
Original image scale range: 51,4 cm/pixel (with 1 x 1 binning) so objects ~1,54 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 4,1°
Phase Angle: 70,5°
Solar Incidence Angle: 73° (meaning that the Sun is about 17° above the Local Horizon)
Solar Longitude: 109,3° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009529_2260_red.jpgSmall Mound in Arcadia Planitia (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunar Explorer Italia)54 visiteMars Local Time: 15:17 (early afternoon)
Coord. (centered): 45,8° North Lat. and 194,9° East Long.
Spacecraft altitude: 303,0 Km (such as about 189,4 miles)
Original image scale range: 60,6 cm/pixel (with 1 x 1 binning) so objects ~1,82 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,5°
Phase Angle: 44,9°
Solar Incidence Angle: 45° (meaning that the Sun is about 45° above the Local Horizon)
Solar Longitude: 109,6° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009531_2155_red.jpgPits near Galaxias Region (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunar Explorer Italia)54 visiteMars Local Time: 15:21 (early afternoon)
Coord. (centered): 35,2° North Lat. and 142,2° East Long.
Spacecraft altitude: 296,1 Km (such as about 185,1 miles)
Original image scale range: 59,3 cm/pixel (with 1 x 1 binning) so objects ~1,78 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 2,3°
Phase Angle: 42,6°
Solar Incidence Angle: 45° (meaning that the Sun is about 45° above the Local Horizon)
Solar Longitude: 109,7° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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Psp_009535_2240_red.jpgMerging Lobate Debris Aprons of Deuteronilus Mensae (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunar Explorer Italia)118 visiteThis image lies within the Deuteronilus Mensae Region, located on the Northern Edge of Arabia Terra and borders the high-standing, heavily cratered Southern Hemisphere and the low, relatively uncratered, plains of the Northern Hemisphere of Mars.
Deuteronilus Mensae is characterized by hills and mesas surrounded by broad debris aprons and this HiRISE image shows examples where lobate-shaped debris aprons appear to overlap.
There is zone of ridges that formed in an area where lobate debris aprons merged from different directions. A current hypothesis is that these ridges are expressions of compressional deformation between two lobes acting like a viscous fluid. One possibility, given the high latitude of the occurrence, is that the lobes of debris are ice-rich and flow somewhat like glaciers.
Recent results from the SHAllow RADar (SHARAD) instrument, also onboard the Mars Reconnaissance Orbiter, indicate that lobate debris aprons in Deuteronilus Mensae are composed of material dominated by ice [Plaut et al., 2008].
This supports the interpretation that these might be potential debris-covered glaciers or rock glaciers.
Some of the detailed textures on the surface of the debris aprons are commonly believed to be the result of ice loss due to sublimation (ice changing into water vapor). On Earth, debris-covered glaciers/rock glaciers typically develop wrinkles and fractures due to stresses in the ice as it flows. Where flows merge, they can buckle and push up ridges producing features similar to those visible here.MareKromium
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