Mars Reconnaissance Orbiter (MRO)
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ESP_016173_2005_RED_abrowse-3.jpgSmall Shield Volcano with "Summit Caldera" (Saturated and Enhanced Natural Colors; credits: Dr M. Faccin - Lunexit Team)54 visiteAlthough there are a few truly giant Shield Volcanoes on Mars, there are also many smaller ones.
There's a strong interest in imaging the Volcanic Vent Regions of Mars, in order to understand not only the Volcanic Processes themselves, but also to search for any signs of recent activity.
In fact, it has been suggested that active volcanism is one possible explanation for the Methane gas that has been detected in the Atmosphere of Mars.
This HiRISE image shows that the Summit Caldera of a small Shield Volcano is mantled by Dust and covered by tiny Impact Craters. And it is just this last element (such as the existence of Impact Craters all over the Caldera) the one that allows us to believe that there are basically no chances that the imaged Volcano was active recently enough to affect the Atmosphere of Mars through the release of any gas whatsoever.MareKromium
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ESP_016190_2635_RED_abrowse.jpgFrost-covered Northern Dunefield (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team:)60 visitenessun commentoMareKromium
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ESP_016228_2650_RED_abrowse-PCF-LXTT-02.jpgNorth Polar Avalanches (CTX Frame and EDM - Absolute Natural Colors; credits for the additoonal process. and color.: Dr Paolo C. Fienga - Lunexit Team)206 visiteMars Local Time: 12:36 (Early Afternoon)
Coord. (centered): 85,0° North Lat. and 151,5° East Long.
Spacecraft altitude: 320,0 Km (such as about 200,0 miles)
Original image scale range: 32,0 cm/pixel (with 1 x 1 binning) so objects ~ 96 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: POLAR STEREOGRAPHIC
Emission Angle: 1,7°
Phase Angle: 71,6°
Solar Incidence Angle: 70° (meaning that the Sun is about 20° above the Local Horizon)
Solar Longitude: 36,6° (Northern Spring)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Dr Paolo C. Fienga - Lunar Explorer ItaliaMareKromium
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ESP_016276_2575_RED_abrowse.jpgTranslucent Ice-Patches in the Northern Plains (possible Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)54 visitenessun commentoMareKromium
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ESP_016280_2655_RED_abrowse.jpgMartian Tears... (possible Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)62 visitenessun commentoMareKromium
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ESP_016288_2610_RED_abrowse.jpgHigh Northern Latitudes (possible Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)54 visitenessun commentoMareKromium
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ESP_016644_1780_RED_abrowse-00.jpgOn the Edge of Concepcin (CTX Frame - Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)63 visiteThis image was acquired by HiRISE on 13 February 2010, on Sol 2153 of Opportunity’s Mission on Mars.
Note the Rover Tracks in the Ripples to the North and North-West of the Rover. Scientists use these high-resolution images (about 25 cm/pixel) to help navigate the Rover. In addition, Rover exploration of areas covered by such high-resolution images provides “ground truth” for the orbital data.MareKromium
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ESP_016644_1780_RED_abrowse-01.jpgOn the Edge of Concepcin (EDM - Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)54 visiteThis EDM shows the Mars Exploration Rover Opportunity perched on the edge of Concepción Crater in Meridiani Planum, Mars.
Concepción Crater is a fresh, 10 meter-diameter crater with dark rays that clearly overprint the North trending Aeolian Ripples.
The dark rays are produced by shadows cast by blocky ejecta and the presence of the rays and similar relationships with other fresh craters in Meridiani Planum indicate that this is likely the youngest crater visited by either Rover on Mars (estimated to have impacted thousands to tens of thousands of years ago).MareKromium
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ESP_016916_1655_RED_abrowse-00.jpgLinear Dunes and Sand Sheets inside Herschel Crater (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)108 visitenessun commentoMareKromium
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ESP_017348_1910_RED_abrowse-00.jpgPolygonal Ridges in Gordii Dorsum (CTX Frame - Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)84 visiteThis image from the Gordii Dorsum Region of Mars shows a large area covered with Polygonal Ridges in an almost geometric pattern.
The Ridges may have originally been Dunes which hardened (indurated) through the action of an unknown process.
Groundwater might have been involved.MareKromium
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ESP_017348_1910_RED_abrowse-01.jpgPolygonal Ridges in Gordii Dorsum (EDM - Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)121 visitenessun commentoMareKromium
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ESP_017405_2270_RED_abrowse.jpgNorthern Hemisphere Gullies on West-Facing Crater Slope (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)159 visiteThis image shows the Eastern (West-facing) side of an Unnamed Impact Crater in the Mid-Latitudes of the Northern Hemisphere.
Like many Mid-Latitude Craters, this one has Gullies along its Walls that are composed of Alcoves, Channels and Debris Aprons. The origins of these Gullies have been the subject of much debate; they could have formed by flowing water, liquid Carbon Dioxide, or dry granular flows. The orientation of these Gullies is of interest because many Craters only contain Gullies on certain Walls, such as those that are Pole-facing. This could be due to changes in orbital conditions and differences in solar heating along specific Walls.
Many of the other features observed in and around this Crater however are indicative of an ice-rich terrain, which may lend credence to the water formation hypothesis, at least for the Gullies visible here. The most notable of these features is the "Scalloped Terrain" in and around the Crater.
This type of Terrain has been interpreted as a sign of surface caving, perhaps due to sublimation of underlying ice.
Another sign of ice is the presence of parallel lineations and pitted material on the Floor of the Crater, similar to what is referred to as concentric Crater Fill. Parallel linear cracks are also observed along the Crater Wall over the Gullies, which could be due to thermal contraction of ice-rich material.
All of these features taken together are evidence for ice-rich material having been deposited in this Region during different climatic conditions that has subsequently begun to melt and/or sublimate under current conditions. More recently, Aeolian Deposits have accumulated around the Crater as evidenced by the parallel ridges dominating the landscape.
Dust Devil Streaks are also visible crossing the Aeolian Ridges.
Written by: Dan BermanMareKromium
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