| Risultati della ricerca nelle immagini - "Tectonic" |
Claritas_Fossae-1-029-290304-0068-6-co-02.jpgClaritas Fossae (1 - ESA/ DLR/ FU Berlin - G. Neukum)67 visiteCaption ESA originale:"These Mars Express images show Claritas Fossae, an ancient tectonic region on Mars, west of Solis Planum, a tectonic and volcanic area south-east of the Tharsis volcano group.
The images were taken by the High-Resolution Stereo Camera (HRSC) on Mars in orbit 68 from an altitude of 271 Km. The images are centred at 255,7° East and 30,9° North. North is on the left".
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Claritas_Fossae-2-029-290304-0068-6-co-02.jpgClaritas Fossae (2 - ESA/ DLR/ FU Berlin - G. Neukum)57 visitevedi il commento al frame che precede
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Claritas_Fossae-3-096-140904-0508-6-co-01-ClaritasFossae_hires.jpgClaritas Fossae (3 - ESA/ DLR/ FU Berlin - G. Neukum)60 visiteCaption ESA originale:"The displayed region is the eastern part of Claritas Fossae and the western part of Solis Planum at longitude 260° East and latitude of about 28° South.
The diffuse blue-white streaks in the northern parts of the scene (Sx di chi guarda) are clouds or aerosols. The Claritas Fossae (‘fossa’ is Latin for trough----->canale) region is characterised by systems of ‘grabens’ running mainly north-west to south-east. These can be traced several hundred kilometres up to the northern Tharsis shield volcanoes.
A "graben" forms when a block of the planet’s crust drops down between 2 faults, due to extension, or pulling, of the crust. A ‘horst and graben’ system can occur where there are several parallel faults.
Geographically, the grabens separate the eastern volcanic plains of the Solis Planum region from the western Daedalia Planum lava plains.
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Claritas_Fossae-4-096-140904-0508-6-co-01-ClaritasFossae_hires.jpgClaritas Fossae (4 - ESA/ DLR/ FU Berlin - G. Neukum)55 visiteCaption ESA originale:"The lava blankets of the Solis Planum area cover the eastern parts of the older Claritas Fossae ridge and surround some of the higher ground. The geological history of this region can be reconstructed by analysing the layers of tectonic grabens, impact craters, volcanic features and even small valley networks. The complexity of Claritas Fossae Region suggests that some of the events took place at the same time. Furthermore, the detailed view of the large southern impact crater shows patches of dark material which are located near the central and marginal parts of the impact crater floor. This material may be of volcanic origin".
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Claritas_Fossae-5-098-140904-0508-6-3d-01-ClaritasFossae_hires.jpgClaritas Fossae (5 - ESA/ DLR/ FU Berlin - G. Neukum)71 visitenessun commento
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Hestia_Rupes-PIA00469.jpgComplex Network of Narrow Fractures near Hestia Rupes Region (possible Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)55 visiteThis is a Magellan radar image covering an about 105- Km (approx. 63-mile) by 45-Km (approx. 27-mile) Region near Hestia Rupes on the North-Western corner of Aphrodite Terra.
The complex network of narrow (such as <1 Km) Fractures in the center of the image extends for approx. 50 Km (about 31 miles). This network exhibits tributary-like branches similar to those observed in river systems on Earth. However, the angular intersections of the tributaries suggest tectonic control.
These features appear to be due to drainage of lava along preexisting fractures and subsequent collapse of the Surface. The underlying tectonic fabric can be observed in the North-East trending Ridges which predate the Plains.MareKromium
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Psp_010689_2025_red~0.jpgTectonic Fissure (Absolute Natural Colors; credits for the additional process. and color: Dr Paolo C. Fienga - Lunexit Team)134 visiteThis image of a region East of Tooting Crater is centered on a Tectonic Fissure West of the Olympus Mons Aureole. Three other Channel Systems formed along it.
The feature of note is a broad shallow Channel System exhibiting a braided pattern that abruptly changes to a steep walled channel system near the Fissure.
These steep walled channel systems are thought to be formed when ground water flowing out along a cliff undermines the slope resulting in collapse of overlying materials. Erosion then typically moves in a headward direction along the pre-existing shallow Channel System. This process is known as "Groundwater Sapping".
There are other places on Mars (such as Cerberus Fossae), where these fissures appear to have flood channels associated with them.
Within this channel there is a more resistant, cliff-forming layer near the surface with some defined horizontal Strata (such as Layers). Multiple Dark Streaks known as slope streaks originate from the base of this hard layer. Slope Streaks are generally dark when first formed and then gradually fade over time. The origin of these Slope Streaks is still under debate, but they are thought to be dry Dust Avalanches.
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Mars Local Time: 15:38 (middle afternoon)
Coord. (centered): 22,1° North Lat. and 208,7° East Long.
Spacecraft altitude: 286,2 Km (such as about 178,9 miles)
Original image scale range: 57,3 cm/pixel (with 1 x 1 binning) so objects ~1,72 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,8°
Phase Angle: 53,9°
Solar Incidence Angle: 53° (meaning that the Sun is about 37° above the Local Horizon)
Solar Longitude: 153,3° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Dr Paolo C. Fienga - Lunar Explorer Italia MareKromium
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Sirenum_Fossae-20090624a.jpgFissure in the Eastern End of Sirenum Fossae (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunar Explorer Italia)54 visitenessun commentoMareKromium
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