Mars Reconnaissance Orbiter (MRO)
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PSP_003176_1745_RED_browse-01~0.jpgLayered Region in Gale Crater (EDM - Natural Colors; credits: Lunexit)54 visiteThis EDM shows several Light-Toned Layers.
The origin of the sediments composing the Layers is unknown and could have included deposition in an ancient flood or lake or the deposition of windblown particles such as Dust or Volcanic Ash.
The relatively uniform character of the Layers and the manner of erosion suggests that the sediments are fine-grained. MareKromium
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PSP_003180_0945_RED_abrowse-00.jpgSouth Polar Dust Fans (CTX Frame - Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)55 visiteDuring the long and dark night of Martian Winter at the South Pole, CO2 in its solid form ("dry ice") accumulates and forms the so-called "Seasonal South Polar Cap". Afterwards, as the Sun comes up in the Spring, the ice evaporates in a complex way.
This observation shows Dark Dust being blown across the Seasonal South Polar Cap. The dust comes from the Surface beneath the ice: it either starts at spots bare of ice, or it's possible that it's lofted from below the ice in geyser-like plumes.
Local winds blow the dust from its source, forming a long Fan. When the wind changes direction, a new Fan is formed pointing in the new direction In this image we can see that the wind has blown in a number of directions.
These data will be used to study - among other things - the Weather Patterns near the South Pole.MareKromium
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PSP_003180_0945_RED_abrowse-01.jpgSouth Polar Dust Fans (EDM n.1 - Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)58 visitenessun commentoMareKromium
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PSP_003180_0945_RED_abrowse-02.jpgSouth Polar Dust Fans (EDM n.2 - Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)54 visitenessun commentoMareKromium
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PSP_003180_0945_RED_abrowse-03.jpgSouth Polar Dust Fans (Enhanced Natural Colors; Credits for the add. process. and color.: Dr Paolo C. Fienga)127 visitenessun commentoMareKromium
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PSP_003193_0850_RED_abrowse-00.jpgThe South Polar Spring of AD 2007 (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)76 visitenessun commentoMareKromium
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PSP_003193_0850_RED_browse_00.jpgMartian Spring: the "V" Fans (context image)53 visiteSouthern Spring sunshine is causing the seasonal Carbon Dioxide (CO2) Cap at the South Pole to evaporate.
This process happens fitfully, as small and large spots expose bare ground, which warms up, causing small spots to grow.
The defrosting areas are controlled by small scale differences in topography, which cause some areas of frost to be sheltered longer than others.
Once dust has accessed the surface it is blown in directions controlled by the local winds, making a distinctive fan. When the wind changes direction the fans broaden or may show multiple orientations.
It has also been proposed that dust is carried to the top of translucent seasonal carbon dioxide ice by release of gas held under pressure by the ice cap. When the pressure is released, like pulling the cork out of a champagne bottle, the gas escapes, carrying dust with it.MareKromium
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PSP_003193_0850_RED_browse_01.jpgMartian Spring: the "V" Fans (extra-detail mgnf)69 visitenessun commentoMareKromium
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PSP_003222_1565_RED_browse.jpgProposed MSL Site in Eberswalde Crater55 visitenessun commentoMareKromium
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PSP_003223_1755_RED_browse.jpgInverted Channels Near Juventae Chasma53 visiteThis image shows several long, sinuous features on the plains near Juventae Chasma. These features have been explained as former stream channels now preserved in inverted relief.
Inverted relief occurs when a formerly low-lying area becomes high-standing. For instance, depressions may become filled with lava that is more resistant to erosion. In the case of stream channels, there are several possible reasons why the channel might stand out in inverted relief. The streambed may contain larger rocks, which remain while fine material is blown away by the wind, or it could be cemented by some chemical precipitating from flowing water.
These features are old, since several impact craters cut the ridges. They provide important information about past processes on Mars. Understanding how streams could have formed is an important issue in understanding the history of water on Mars.MareKromium
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PSP_003231_2095_RED_abrowse-00.jpgRocky Mesas in Nilosyrtis Mensae (CTX Frame - Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)120 visiteMareKromium
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PSP_003231_2095_RED_abrowse-01.jpgRocky Mesas in Nilosyrtis Mensae (EDM - Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)105 visiteMareKromium
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