| Piú votate - Mars Reconnaissance Orbiter (MRO) |
PSP_007166_1740_RED_abrowse-00~0.jpgExposure of Layers and Minerals in Candor Chasma (MULTISPECTRUM; credits: Lunexit)53 visiteScanning across several kilometers of relief, this image shows a cliff along a light-toned layered deposit in Valles Marineris. This particular cliff was targeted because of the excellent exposure of layering and the identification of the minerals Kieserite (a mineral containing Magnesium) and Hematite (an Iron Oxide).
The Hematite appears in the darker low-lying region of the image and the Kieserite is associated with the light-toned layers.
The fact that these minerals are found here with a layered deposit suggests that water may have been involved in the deposition of these minerals and the layers.
Erosion by wind has carved V-shaped patterns along the edges of many of the layers. The layers appear friable (easy to erode) so this is why wind can carve deep grooves along a steep cliff such as visible here.
The top of the layered deposit (lower part of image) is smooth and relatively dark because it is covered by debris laid down by the wind, dust and other fine materials.
The cliff has stronger winds flowing up and down it, plus the effects of gravity, so airborne debris can be shed downslope to expose the fresh brighter layered deposit.MareKromium
(1 voti)
|
|
ESP_011618_1885_RED_abrowse-00.jpgRecent Double-Impact (ctx frame - possible Natural Colors; credits: Lunar Explorer Italia)61 visiteMars Local Time: 15:46 (middle afternoon)
Coord. (centered): 8,6° North Lat. and 46,8° East Long.
Spacecraft altitude: 273,6 Km (such as about 171,0 miles)
Original image scale range: 27,4 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: 5,9°
Phase Angle: 64,1°
Solar Incidence Angle: 58° (meaning that the Sun is about 32° above the Local Horizon)
Solar Longitude: 193,2° (Northern Autumn)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
(1 voti)
|
|
Psp_009772_1545_red.jpgSchaeberle Crater (possible True Colors; credits: Lunar Explorer Italia)64 visiteMars Local Time: 15:35 (middle afternoon)
Coord. (centered): 25,4° South Lat. and 50,0° East Long.
Spacecraft altitude: 254,6 Km (such as about 159,1 miles)
Original image scale range: 50,9 cm/pixel (with 1 x 1 binning) so objects ~1,53 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,9°
Phase Angle: 71,4°
Solar Incidence Angle: 71° (meaning that the Sun is about 19° above the Local Horizon)
Solar Longitude: 118,3° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
(1 voti)
|
|
PSP_009725_2485_RED.jpgPhoenix Landing Site (possible True Colors; credits: Lunar Explorer Italia)130 visiteMars Local Time: 14:48 (early afternoon)
Coord. (centered): 68,2° North Lat. and 234,3° East Long.
Spacecraft altitude: 324,1 Km (such as about 202,6 miles)
Original image scale range: 32,4 cm/pixel (with 1 x 1 binning) so objects ~97 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 15,6°
Phase Angle: 66,9°
Solar Incidence Angle: 53° (meaning that the Sun is about 37° above the Local Horizon)
Solar Longitude: 116,6° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
(1 voti)
|
|
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
(1 voti)
|
|
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
(1 voti)
|
|
PSP_009304_1495_RED.jpgSmooth Hills (possible True Colors; credits: Lunar Explorer Italia)53 visiteMars Local Time: 15:31 (middle afternoon)
Coord. (centered): 30,2° South Lat. and 227,9° East Long.
Spacecraft altitude: 253,6 Km (such as about 158,5 miles)
Original image scale range: 50,7 cm/pixel (with 1 x 1 binning) so objects ~1,52 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,3°
Phase Angle: 74,9°
Solar Incidence Angle: 75° (meaning that the Sun is about 15° above the Local Horizon)
Solar Longitude: 101,7° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
(1 voti)
|
|
Psp_001840_1660_red.jpgVolcanic Vent in Syria Planum (natural colors; credits: Lunar Explorer Italia)53 visitePrevious images of this area by other space missions indicate that this is a shield volcano with very shallow slopes. What HiRISE reveals is that it is completely covered by a blanket of dust.
While volcanic featues remain obscure, the dust does exhibit some very strange patterns. As you zoom into the middle of the image, the ground appears covered with a fine network of light and dark polygons. But at full resolution, it can be seen that these polygons are actually the edges of small scallops.
The dust is apparently held together by some unknown means, giving it sufficient strength to be carved into this strange pattern.MareKromium
(1 voti)
|
|
PSP_009460_1745_RED_abrowse-00.jpgCeti Mensa (ctx frame - natural colors; credits: Lunexit)53 visiteThis image shows a steep-sided depression in light-toned, layered rocks in the Valles Marineris Canyon System.
This formation, known as Ceti Mensa, is located in Western Candor Chasma in the Northern Valles.
The origin of Ceti Mensa and other Layered Deposits within the canyons is a source of much debate: proposed interpretations include lake deposits, deposits of volcanic ash, deposits of windblown sand and dust and glacial deposits. Recent spectral observations by the Mars Express and Mars Reconnaissance Orbiter Spacecraft have identified crystalline Iron Oxides and Hydrated Magnesium Sulfate minerals on Ceti Mensa.
These minerals are regarded as indicators of the presence of liquid water during their formation.
The Hydrated Sulfate mineral "Kieserite", in particular, most commonly forms on Earth by evaporation of brines.MareKromium
(1 voti)
|
|
PSP_008075_1590_RED_abrowse.jpgLight-toned Rocks (MULTISPECTRUM; credits: Lunexit)70 visiteThis observation shows a portion of an approximately 30 kilometer diameter impact crater located to the south of Valles Marineris.
The image reveals that the central uplift inside the crater is a mixture of dark-toned and light-toned materials. It’s likely that some of the rocks in the center of the crater represent units at depth that we wouldn’t otherwise see along the plains that surround the crater. The light-toned units in particular are not visible in the plains surrounding this crater so they could be material that is buried beneath the plains and only visible inside craters or other vertical exposures, such as those created by faults.
Some of the light-toned material appears angular and blocky, consistent with material that has been disrupted and uplifted by an explosion associated with the crater’s formation. The reason why some material appears light-toned is unknown but could be due to a different composition than the darker-toned unit.
Many light-toned units seen elsewhere on Mars, including within Valles Marineris, are made of sulfates so there may be sulfate-rich rocks buried beneath the plains at this location and the formation of the crater exposed them. In any case, the distinct materials visible within impact craters suggest that the crust on Mars may contain many units of variable composition.MareKromium
(1 voti)
|
|
PSP_003520_1010_RED_abrowse-00.jpgSouth Polar Spiders (ctx frame - MULTISPECTRUM-2; credits: Lunexit)53 visiteThis image is located in the South Polar Region of Mars and we can see “spiders” likely caused by the sublimation of Carbon Dioxide ice.
As this happens, the gas moves through channels until it reaches the surface and vents out. These vents show up as the dark streaks because they carry dust and dirt up to the surface.MareKromium
(1 voti)
|
|
PSP_008095_2500_RED_abrowse.jpgLouth Crater, Southern Rim (MULTISPECTRUM; credits: Lunexit)85 visitenessun commentoMareKromium
(1 voti)
|
|
| 2234 immagini su 187 pagina(e) |
 |
|
|
|
|
|
|
|
185 | |
|
