| Piú votate - Mars Reconnaissance Orbiter (MRO) |
PSP_006978_1190_RED_abrowse.jpgSouthern DD Tracks (Absolute Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)64 visitenessun commentoMareKromium
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PSP_006982_1745_RED_abrowse-PCF-LXTT.jpgPortion of the "Interior" of Tithonium Chasma (Absolute Natural Colors; credits for the additional process. and color.: Drr Gianluigi Barca and Paolo C. Fienga - Lunexit Team)62 visitenessun commentoMareKromium
(5 voti)
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ESP_020395_1260_RED_abrowse.jpgFeatures of Liu Hsin Crater (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)125 visitenessun commentoMareKromium
(5 voti)
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Volcanoes-Arsia_Mons-PIA13540-1.jpgLayers in the lower West Flank of Arsia Mons (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)116 visiteMareKromium
(5 voti)
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Volcanoes-Arsia_Mons-PIA13540-2.jpgLayers in the lower West Flank of Arsia Mons (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)118 visiteCaption NASA:"This image - dated July, 18th, 2007) covers a Pit in the lower West Flank of Arsia Mons, one of the four Giant Volcanoes of the Tharsis Volcanic District.
Many Layers are exposed in the Pit, probably marking individual Lava Flows, and they can provide useful information about the nature of some of the many Martian Volcanic Eruptions.
This image was acquired in the middle of a large Regional Dust Storm, but the Atmosphere over this image is only moderately dusty because the altitude is 6,5 Km higher than the Planetary Mean, so the air is quite thin and cannot hold as much Dust. Although the Atmosphere was not too dusty, the Surface is buried by a Dust Layer which is probably several meters thick.
These high-altitude locations on Mars have thick Dust Deposits because the thin air cannot blow away the Dust, or at least not as fast as it accumulates. On Earth the oceans serve as "Dust Traps", but on Mars, it is a job for the highest Volcanoes".MareKromium
(5 voti)
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ESP_019197_2290_RED_abrowse-01.jpgExtremely unusually-looking Unnamed Northern Crater (EDM n.1 - Absolute Natural Colors; credits for the additional process. and color.: Drr Gianluigi Barca and Paolo C. Fienga - Lunexit Team)107 visitenessun commentoMareKromium
(5 voti)
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PSP_003907_1780_RED_browse-1.jpgProposed MSL Site in Iani Chaos (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)58 visitenessun commentoMareKromium
(5 voti)
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PSP_003618_1725_RED_abrowse-PCF-LXTT.jpgGanges Chasma (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)56 visitenessun commentoMareKromium
(5 voti)
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PSP_003695_1250_RED_abrowse-01.jpgUnnamed Southern Crater with Large Dunefield and DD Streaks (EDM - Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)62 visiteThis EDM, approx. 750 mt across, shows Dust Devil Tracks near the South-West edge of the Dunefield. The bright protruding rocks on the lower side of the image are either being exposed or being buried, as the Dunes migrate. MareKromium
(5 voti)
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PSP_002922_1725_RED_abrowse-02.jpgPossible Volcanic "Mouth", on Arsia Mons' Flank (EDM - RAW Natural Colors - credits for the additional process.: Dr Marco Faccin)59 visitenessun commentoMareKromium
(5 voti)
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ESP_014287_1685_RED_abrowse-00.jpgNoctis Labyrinthus (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)54 visiteThis image spans the floor and two walls of a pit in Noctis Labyrinthus, a System of deep, steep-walled Valleys on the Western Edge of Valles Marineris.
The Valleys themselves are tectonic features known as "Graben" (---> trench-like features that form in response to extension (or stretching) of the Crust). In the case of Noctis Labyrinthus, volcanic activity in the Tharsis Region may have formed a bulge, which then stretched and fractured the Crust above it.MareKromium
(5 voti)
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PSP_002922_1725_RED_abrowse-00.jpgGlacier-like Flow on Arsia Mons (CTX frame - Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)54 visiteThis observation shows a "Glacier-like Flow" in a Depression located on the flanks of Arsia Mons.
Arsia Mons is one of the large Martian Volcanoes that sits near the Equator on the Tharsis Rise. Downslope is towards the upper right of CTX frame, and the Flow is in this direction. It is interesting to note that the Depression is not directly radial from the Volcano's Peak, but rather oriented approximately 45° away, along the Flanks of the Volcano.
The pitted texture of the material suggests that sublimation is occurring or has occurred. The Surface Temperature and Pressure on Mars are such that water in ice-rich material can easily sublimate leaving behind a depression where the volatiles were removed.MareKromium
(5 voti)
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