| Piú votate - Mars Reconnaissance Orbiter (MRO) |
ESP_026394_2160-PCF-LXTT-00.jpgHuge Dust Devil in Amazonis Planitia (CTX Frame - Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team) 91 visiteMars Local Time: 15:02 (early afternoon)
Coord. (centered): 35,5° North Lat. and 201,5° East Long.
Spacecraft altitude: 295,8 Km (such as about 184,9 miles)
Original image scale range: 31,9 cm/pixel (with 2 x 2 binning) so objects ~ 1 mt and 18 cm across are resolved (with 4 x 4 binning)
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,3°
Sun - Mars - MRO (or "Phase") Angle: 40,4°
Solar Incidence Angle: 40° (meaning that the Sun is about 50° above the Local Horizon)
Solar Longitude: 83,0° (Northern Spring)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
(7 voti)
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ESP_026394_2160-PCF-LXTT-01.jpgHuge Dust Devil in Amazonis Planitia (EDM - Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team) 90 visiteMars Local Time: 15:02 (early afternoon)
Coord. (centered): 35,5° North Lat. and 201,5° East Long.
Spacecraft altitude: 295,8 Km (such as about 184,9 miles)
Original image scale range: 31,9 cm/pixel (with 2 x 2 binning) so objects ~ 1 mt and 18 cm across are resolved (with 4 x 4 binning)
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,3°
Sun - Mars - MRO (or "Phase") Angle: 40,4°
Solar Incidence Angle: 40° (meaning that the Sun is about 50° above the Local Horizon)
Solar Longitude: 83,0° (Northern Spring)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
(7 voti)
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ESP_023464_0945_RED_abrowse-PCF-LXTT-01.jpgSouth Polar Summer (EDM - Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)407 visiteMars Local Time: 16:28 (Middle Afternoon)
Coord. (centered): 85,3° South Lat. and 319,7° East Long.
Spacecraft altitude: 245,2 Km (such as about 153,2 miles)
Original image scale range: 49,1 cm/pixel (with 2 x 2 binning) so objects ~ 1 mt and 47 cm across are resolved
Map projected scale: 50 cm/pixel
Map projection: POLAR STEREOGRAPHIC
Emission Angle: 0,4°
Sun-Mars-Spacecraft (or "Phase") Angle: 78,2°
Solar Incidence Angle: 78° (meaning that the Sun is about 12° above the Local Horizon)
Solar Longitude: 336,2° (Northern Winter)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Dr Paolo C. Fienga - Lunar Explorer ItaliaMareKromium
(7 voti)
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Craters-Proctor_Crater-PIA13076.jpgProctor's Dunes (Possible Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)88 visiteThis observation shows the edge of a dark Dunefield on the Floor of Proctor Crater, an about 150 Km (approx. 93 miles) diameter crater in the Southern Highlands of Mars.
This subimage is a close-up view of the dark dunes. These dunes are most likely composed of basaltic sand that has collected on the bottom of the crater. Superimposed on their surface are smaller secondary dunes which are commonly seen on terrestrial dunes of this size. Near the crests of the dark dunes are bright patches of frost. Dark spots within the frost patches are areas where defrosting is occurring.
Many smaller and brighter bed forms, most likely small dunes or granule ripples, cover the substrate between the larger dark dunes as well as most of the Floor of Proctor Crater. In many locations, large boulders are seen on the same surfaces as the bright bed forms.
The dark dunes stratigraphically overlie the small bright bed forms indicating that the darker dunes formed more recently.
However in several areas, the dark dunes appear to influence the orientation of the small bright dunes, possibly by wind flowing around the larger dunes, suggesting that both dark and bright bed forms are coeval.MareKromium
(7 voti)
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ESP_16978_1730-MF-LXTT1.jpgFalling Down... (an Image-Mosaic by Dr Marco Faccin - Lunexit Team)64 visiteThe lower flanks of Arsia Mons, one of the giant volcanoes on Mars, is riddled with Pits of various sizes. These have been of great interest to a number of researchers because they have the potential to be openings into underground caverns.
Such caverns have some potential for holding ice and offer protection from radiation and small meteorites. These are good things if one is looking for a safe place for current life on Mars or future human life.
However, this image shows some of the pitfalls of such hopes. Most of these pits are largely filled with rubble and dust that hide any potential links to larger underground areas. Furthermore, the entrances are steep and rocky, making them difficult areas to traverse. They would be a very exciting, if not safe, place to visit!MareKromium
(7 voti)
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PSP_001370_2505_RED_abrowse.jpgIce Patch or Frozen Lake? (Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)54 visitenessun commentoMareKromium
(7 voti)
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ESP_014423_1040_RED_abrowse.jpgSouth Polar Region (Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)54 visiteSomewhere in this patterned landscape, less than 1000 Km (about 600 miles) from the South Pole of Mars, a treasure may be hiding.
In January 1999, NASA launched a rocket containing the Mars Polar Lander (MPL), an exploration vehicle with a weather station and a subsurface probe designed to search for water ice, towards the Layered Terrain near the Martian South Pole. The layers are thought to be a sequence of alternating dust-rich and dust-poor ice deposited by the seasonal advance and retreat of the South Polar Ice Cap and could be an important record of climate on the Red Planet.
On 3 December 1999, just before the Lander entered the Martian Atmosphere, MPL went silent. Investigations propose the most likely cause of the mission failure is that the Spacecraft’s computers misinterpreted the release of the Lander’s legs in preparation for descent as touch-down on the Martian Surface, causing descent engines to shut off when the lander was still 40 meters (130 feet) above ground.
However, no one knows for sure.
An immediate search began for the remains of the MPL using images from Mars Global Surveyor. HiRISE is continuing the search with high resolution images of the area in which MPL could, most likely, have crash-landed. MareKromium
(7 voti)
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ESP_014417_1975_RED_abrowse-00.jpgChrise Planitia (Natural Colors; credits: Lunexit)54 visitenessun commentoMareKromium
(7 voti)
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ESP_014326_1715_RED_abrowse.jpgLight-toned Layering along Jus Chasma's Wallrock and Plains (Natural Colors; credits: Lunexit)54 visitenessun commentoMareKromium
(7 voti)
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ESP_014404_1275-GB-LXT-03.jpgExtremely Unusual Surface Feature in Argyre Planitia (Natural Colors - SuperEDM n.2 - credits: Dr G. Barca & Lunexit)54 visitenessun commentoMareKromium
(7 voti)
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ESP_014392_0955_RED_abrowse.jpgSouth Polar Residual Cap Monitoring - Downwasting Processes (Natural Colors; credits: Lunexit)55 visitenessun commentoMareKromium
(7 voti)
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ESP_014418_0930_RED_abrowse.jpgSouth Polar Residual Cap Monitoring (Natural Colors; credits: Lunexit)54 visitenessun commentoMareKromium
(7 voti)
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