| Risultati della ricerca nelle immagini - "Volcano" |
Arsia_Chasmata-PIA13499.jpgArsia Mons Chasmata (Absolute Natural Colors; additional process.: Dr Paolo C. Fienga - Lunexit Team)102 visitenessun commentoMareKromium
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ESP_011664_2015_RED_abrowse-00.jpgAt the base of Olympus Mons... (ctx frame - Natural Colors; credits: Lunar Explorer Italia)59 visiteThis image is located at the foot of the largest volcano of the Solar System: Olympus Mons.
The entire scene is covered with a multitude of Lava Flows. Most of the Flows consisted of relatively sticky lava that froze after flowing for only a short distance (often less than 1 Km, or about 1/2 a mile). However, a few of the Flows were more fluid and actually drained out of their Channels, leaving Troughs with distinct levees. These “Channelized” Flows extend out of the HiRISE image so they must be at least several kilometers (a few miles) long.
In all likelihood, both the short and long Lava Flows have very similar chemical compositions.
Based on experience with Lava Flows on Earth, the Channelized Flows were probably fed by more vigorous eruptions. That is, the Lava Flow was fed so quickly that the lava traveled a long distance before it solidified. With the shorter flows, a slow dribble of lava froze before going more than the equivalent of a few city blocks.MareKromium
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ESP_011664_2015_RED_abrowse-01.jpgAt the base of Olympus Mons... (edm - Natural Colors; credits: Lunar Explorer Italia)56 visiteThe Ridge with 2 Knobs in the center of this edm is of special interest. The Lava Flows radiate away from these Knobs, indicating that the Flows were fed from these points. However, based on experience with the current eruption of Kilauea Volcano in Hawaii, it seems that these Vents were fed by a Lava Tube.
Thus the magma first reached the Surface some distance away, then was transported through a Tube to this location. A blockage in the Tube would force the lava to burst out and erupt onto the Surface.MareKromium
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ESP_012692_1810_RED_abrowse.jpgThe "Dusty" Summit of Pavonis Mons (Natural Colors; credits: Lunar Explorer Italia)54 visitePavonis Mons is one of the 3 giant Tharsis Montes Shield Volcanoes. Its Summit rises so far above the Surface that the Atmosphere is extremely thin, even for Mars.
Dust that reaches these heights (for example, during major Dust Storms) is hard to remove, so the upper parts of these Volcanoes are covered by vast deposits of dust. The dust is moved a little by the thin winds, producing ripples and other textures near the limit of HiRISE’s resolution. The fluffy, ripply surface looks “smudged” or out of focus, but by looking at some of the small impact craters you can see that the HiRISE camera is, indeed, properly focused. It’s the surface of Mars that is blurry!
Nota Lunexit: NO. A nostro parere NON è la Superficie di Marte che è "sfuocata" (blurry) e non è neppure la fotocamera dell'Orbiter che è "out of focus". Si tratta, come abbiamo già visto in passato (nelle immagini dei fly-by ravvicinati di alcune Lune Saturniane - Encelado su tutte) di un caso classico di "Sfuocatura da Movimento" (in altre parole: è un mero problema di lunghezza dell'esposizione - ivi: eccessiva -, data la vicinanza del target ripreso in rapporto alla velocità dell'Orbiter rispetto al medesimo). Curioso che i Ragazzi di Pasadena non ci abbiano pensato...
The impact craters also show that the dust is not a thin veneer. Instead, it is a thick coat, at least several meters deep. This mantling of dust hides the details of the Lava Flows and Vents, frustrating volcanologists but delighting those who study dust.
Mars Local Time: 15:23 (early afternoon)
Coord. (centered): 0,9° North Lat. and 246,8° East Long.
Spacecraft altitude: 254,1 Km (such as about 158,8 miles)
Original image scale range: 50,8 cm/pixel (with 1 x 1 binning) so objects ~1,53 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 2,5°
Phase Angle: 52,4°
Solar Incidence Angle: 55° (meaning that the Sun is about 35° above the Local Horizon)
Solar Longitude: 244,7° (Northern Autumn)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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ESP_016173_2005_RED_abrowse-PCF-LXTT.jpgSmall Shield-Volcano (Absolute Natural Colors; credits for the additonal process. and color.: Dr Paolo C. Fienga - Lunar Explorer Italia)200 visiteMars Local Time: 14:44 (Early Afternoon)
Coord. (centered): 20,1° North Lat. and 250,3° East Long.
Spacecraft altitude: 274,9 Km (such as about 171,8 miles)
Original image scale range: 55,0 cm/pixel (with 2 x 2 binning) so objects ~ 1 mt and 65 cm across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,6°
Sun-Mars-Spacecraft (or "Phase") Angle: 39,1°
Solar Incidence Angle: 40° (meaning that the Sun is about 50° above the Local Horizon)
Solar Longitude: 34,7° (Northern Spring)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Drr Gianluigi Barca and Paolo C. Fienga - Lunar Explorer ItaliaMareKromium
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ESP_017950_2205_RED_abrowse.jpgMore "Mud-Volcanoes" (?) in Acidalia Planitia (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)105 visiteMareKromium
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ESP_019612_2250_RED_abrowse.jpgMud-Volcanoes (?) in Acidalia Planitia (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)101 visiteThis proposed future Mars Landing Site in Acidalia Planitia targets densely occurring Mounds thought to be "Mud Volcanoes".
Mud Volcanoes are geological structures formed when a mixture of gas, liquid and fine-grained rock (or mud) is forced to the Surface from several meters to kilometers underground.
Scientists are targeting these Mud Volcanoes because the sediments, brought from depth, could contain organic materials that might provide evidence for possible past and present microbial life on Mars.MareKromium
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ESP_023531_1840-00.jpgSkylight on the Dusty Slopes of Arsia Mons (CTX Frame and EDM - Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)221 visiteMars Local Time: 14:08 (Early Afternoon)
Coord. (centered): 3,7° North Lat. and 248,5° East Long.
Spacecraft altitude: 263 Km (such as about 164,4 miles)
Original image scale range: 26,3 cm/pixel (with 1 x 1 binning) so objects ~ 79 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 4,1°
Sun-Mars-Spacecraft (or "Phase") Angle: 30,4°
Solar Incidence Angle: 34° (meaning that the Sun is about 56° above the Local Horizon)
Solar Longitude: 339,1° (Northern Winter)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Dr Paolo C. Fienga - Lunar Explorer ItaliaMareKromium
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ESP_023811_1880_RED_abrowse.jpgSmall Volcano in Cerberus Fossae (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)186 visiteMars Local Time: 14:07 (Early Afternoon)
Coord. (centered): 8,1° North Lat. and 162,5° East Long.
Spacecraft altitude: 278,3 Km (such as about 173,9 miles)
Original image scale range: 27,8 cm/pixel (with 1 x 1 binning) so objects ~ 55,7 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 8,2°
Sun-Mars-Spacecraft (or "Phase") Angle: 42,1°
Solar Incidence Angle: 34° (meaning that the Sun is about 56° above the Local Horizon)
Solar Longitude: 350,5° (Northern Winter)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Dr Paolo C. Fienga - Lunar Explorer ItaliaMareKromium
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ESP_023817_1110_RED_abrowse-PCF-LXTT.jpgPutative Subglacial Volcano in the South Polar Region (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)204 visiteMars Local Time: 14:36 (Early Afternoon)
Coord. (centered): 68,7° South Lat. and 11,7° East Long.
Spacecraft altitude: 249,7 Km (such as about 156,1 miles)
Original image scale range: 25,0 cm/pixel (with 1 x 1 binning) so objects ~ 75 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: POLAR STEREOGRAPHIC
Emission Angle: 2,4°
Sun-Mars-Spacecraft (or "Phase") Angle: 71,3°
Solar Incidence Angle: 70° (meaning that the Sun is about 20° above the Local Horizon)
Solar Longitude: 350,7° (Northern Winter)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Dr Paolo C. Fienga - Lunar Explorer ItaliaMareKromium
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ESP_024097_2170-PCF-LXTT-00.jpgSmall Volcano near Western Mareotis Tholus (CTX "A" - Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)216 visiteMars Local Time: 14:09 (Early Afternoon)
Coord. (centered): 36,5° North Lat. and 271,5° East Long.
Spacecraft altitude: 289,6 Km (such as about 181,0 miles)
Original image scale range: 29,0 cm/pixel (with 1 x 1 binning) so objects ~ 87 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,8°
Sun-Mars-Spacecraft (or "Phase") Angle: 46,3°
Solar Incidence Angle: 47° (meaning that the Sun is about 43° above the Local Horizon)
Solar Longitude: 1,8° (Northern Spring)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Dr Paolo C. Fienga - Lunar Explorer ItaliaMareKromium
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ESP_024097_2170-PCF-LXTT-01.jpgSmall Volcano near Western Mareotis Tholus (CTX "B" - Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)202 visiteMars Local Time: 14:09 (Early Afternoon)
Coord. (centered): 36,5° North Lat. and 271,5° East Long.
Spacecraft altitude: 289,6 Km (such as about 181,0 miles)
Original image scale range: 29,0 cm/pixel (with 1 x 1 binning) so objects ~ 87 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,8°
Sun-Mars-Spacecraft (or "Phase") Angle: 46,3°
Solar Incidence Angle: 47° (meaning that the Sun is about 43° above the Local Horizon)
Solar Longitude: 1,8° (Northern Spring)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Dr Paolo C. Fienga - Lunar Explorer ItaliaMareKromium
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