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T-TRA_000862_1710_RED_CandorChasma_01.jpgCandor Chasma58 visiteThis HiRISE sub-image shows the steep slopes along wallrock in the eastern edge of West Candor Chasma. In general, the rocks in the upper part of the canyons are interpreted to be lava flows that cover the plains surrounding Valles Marineris, whereas the deeper material along the walls could be either more lava flows or megaregolith that resulted from numerous impact craters that disrupted the Martian surface during the first billion years after formation of the planet. Resistant material is visible in portions of the sub-image and HiRISE is able to resolve 1-2 meter size boulders shedding out of these resistant wallrock units. The bright and dark lineations seen in the right of the sub-image follow the slope of the wallrock (downslope is towards the top of the sub-image) and likely represent bright dust and dark sand that are sliding downslope. The large number of small impact craters visible along the slopes indicates that there isn't a large amount of material moving downslope recently because these craters would have been destroyed or buried.
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Craters-Holden_Crater-TRA_000861_1530_RED_Holden_Delta_00.jpgThe beautiful Holden Crater58 visiteThis HiRISE image covers a portion of the floor of Holden Crater situated in southwest Margaritifer Terra. Holden crater has likely experienced extensive modification by running water, which is supported by observations of drainage and deposition into the crater from a large channel breaching Holden's rim and the alluvial fans that built out along the floor of the crater. The HiRISE sub-image shows relatively bright finely layered deposits that are capped by relatively darker materials. Unlike previous images, the HiRISE image shows that the thickness of some of the individual layers are on the order of a meter or even less in thickness and are laterally uniform and continuous over the extent of the imaged outcrop. Some of the layers in the outcrop display an orthogonal pattern or what may be fractures or joints. The "layer-cake" appearance of these layers suggests that they may have been deposited into a lake that once occupied the crater floor and have seen little in the way of deformation since that time. By contrast, the darker materials overlying the layers are younger and may have been sediments deposited off the nearby alluvial fans. Alternatively, they may represent wind-blown deposits lain down during a later much drier period similar to the conditions that currently exist at the surface today. In some locations, the darker materials have been stripped and expose the lighter finely layered sediments underneath, thereby implying the finely layered materials extend much farther than what is visible along the large outcrop.
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M-016-99.jpgM 16 - The "Eagle Nebula"58 visite"...Omnia Mors poscit. Lex est, non poena, perire..."
(Seneca)
"...La Morte chiama a sè ogni cosa, ed il morire non è una pena, ma una Legge..."
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M-042-93.jpgM 42 - The "Great Orion Nebula"58 visite"...Bibamus et gaudeamus dum juvenes sumus; nam cito tarda senectus venit: post eam, Mors et post Mortem, nihil...
(detto dei Goliardi - Medio Evo)
"...Beviamo e divertiamoci, sinchè siamo giovani, poichè rapida sopraggiunge la vecchiaia e, dopo di essa, la Morte. E dopo la Morte, il nulla..."
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Titan-Lakes-Unnamed_North_Polar_Lakes-02-PIA01942.jpgTitanian Northern Lakes (3)58 visiteCaption NASA originale:"Using its radar system, the Cassini spacecraft has imaged new lakes on Titan.
The large dark patch seen on this image, at high latitudes surrounding Titan's North Pole, is most likely a hydrocarbon lake. Several dark channels can be seen; the longest one at the left meanders over almost 100 Km (about 62 miles), and appears to drain into the lake. Some dark channels are remarkably straight, suggesting possible faulting in the subsurface. The bright landforms jutting into the lake indicate that old, eroded landforms may have flooded.
This radar image was acquired by the Cassini radar instrument in synthetic aperture mode on Oct. 9, 2006. The image is centered near 73° North Latitude and 343° West Longitude; it measures about 300 by 140 Km (such as about 190 by 90 miles). Smallest details in this image are about 500 mt (approx. 1.640 feet) across".
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Craters-Becquerel_Crater_mound_6m-02.jpgBeautiful Becquerel Crater (3)58 visitenessun commento
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Craters-Becquerel_Crater_mound_6m-04.jpgBeautiful Becquerel Crater (5)58 visitenessun commento
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TRA_000828_2495_IRB-2.jpgPolygonal Terrain (2)58 visiteImage TRA_000828_2495 was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard the Mars Reconnaissance Orbiter spacecraft on September 30, 2006. The complete image is centered at 69,3° North Latitude and 130,2° East Longitude. The range to the target site was 315 Km (199 miles). At this distance the image scale is 32 cm/pixel (with 1 x 1 binning) so objects ~96 cm across are resolved. The images shown here has been map-projected to 75 cm/pixel and North is up. The image was taken at a local Mars time of 3:01 PM and the scene is illuminated from the West with a solar incidence angle of 53,4°, thus the Sun was about 35,1° above the horizon. At a Solar Longitude of 113,7°, the season on Mars is Northern Summer / Southern Winter.
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TRA_000840_2750_IRB-008.jpgChasma Boreale (7)58 visitenessun commento
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Earth&Sun-001-magfieldG_b.jpgMagnetic Fields... (2)58 visitenessun commento
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TRA_000828_1805_IRB-04.jpgYardangs in Medusae Fossae (4)58 visitenessun commento
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Orion Region.jpgOrion Region and the Orionids Meteor-Shower58 visite"...Il miglior risultato che si può ottenere usando la ragionevolezza durante il confronto con un pazzo, è quello di passare per stupidi..."
(P.C. Floegers - "Conversations")
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