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APOLLO_14_AS_14-77-10367_HR-a.JPGAS 14-77-10367 (a) - Thermal Degradation Sample62 visiteThermal Degradation Sample; taken in the vicinity of Station "A".MareKromium
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APOLLO_14_AS_14-77-10369a.JPGAS 14-77-10369 (a) - Lunar Bootprint62 visiteAstronaut bootprint; taken in the vicinity of Station "A".MareKromium
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APOLLO_14_AS_14-77-10373a.JPGAS 14-77-10373 (a) - Soil-covered Rock (slightly sunstruck)62 visiteSoil-covered rock surface. Taken at the LM.MareKromium
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APOLLO_11_AS_11-45-6699a.JPGAS 11-45-6699 (a) - Disturbed or NOT disturbed?62 visiteSoil not distubed or only somewhat disturbed by LM Descent Engine.
Nota Lunexit: la "criptica" Caption NASA vuol solo dire che il "Suolo Lunare" ivi ripreso NON è stato "naturalmente" disturbato (ergo: o NON è disturbato in toto o, se lo è stato, allora il "disturbo" è il frutto di un'azione meccanica - e cioè, probabilmente, il "getto" di materiale proveniente dal Propulsore di Discesa del Modulo Lunare - LM Descent Engine).MareKromium
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SOU-SOL019-81991_full.jpgDeflated Airbags and Rocky Landscape - Sol 19 (MULTISPECTRUM; credits: Lunexit)62 visitenessun commentoMareKromium
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Craters-Terby_Crater.jpgTerby Crater (Natural Colors + MULTISPECTRUM; credits: ESA & Lunexit)62 visiteThe High Resolution Stereo Camera (HRSC) on board ESA’s Mars Express Orbiter imaged the Terby Crater on Mars on 13 April 2007 during orbit 4199.
The Region is of great scientific interest as sediments there hold information on the role of water in the history of the Planet. Eye-catching finger-shaped plateaux extend in the North-South direction. They rise up to 2000 mt above the surrounding terrain. The relatively old crater was filled with sediments in the past, which formed plateaux on erosion.
The flanks of the plateaux clearly exhibit layering of different-coloured material. Differences in colour usually indicate changes in the composition of the material and such layering is called ‘bedding’. Bedding structures are typical of sedimentary rock, which has been deposited either by wind or water. Different rock layers erode differently, forming terraces.
The valleys exhibit gullies, or channels cut in the ground by running liquid, mainly in the Northern part of the image.
These gullies and the rock-bedding structure indicate that the region has been affected by water.
MareKromium
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PSP_006999_1965_RED_abrowse.jpgFissure-Vent along Cerberus Fossae (MULTISPECTRUM; credits: Lunexit)62 visitenessun commentoMareKromium
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OPP-SOL1452-3.jpgMagnetic Drawing - Sol 1452 (Superdefinition; credits: Dr M. Faccin)62 visitenessun commentoMareKromium
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PSP_001691_1320_COLOR-01.jpgGullied Trough in Noachis Terra (extra-detail mgnf n. 1; Superdefinition + MULTISPECTRUM; credits: Dr M. Faccin & Lunexit)62 visiteCoord.: 47,5° South Lat. and 4,4° East Long.
Spacecraft altitude: about 258 Km
M.L.T.: 15:39 (middle afternoon)
Solar Incidence Angle: 78° (meaning that the Sun was 12° above the Local Horizon)MareKromium
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Petals.jpgPetals on Mars (by Bruce Moyant)62 visitenessun commentoMareKromium
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Sunset~1.jpgUntitled (by Brian Cameron)62 visitenessun commentoMareKromium
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Polygons-PIA10658.jpgMartian and Earthly Polygons (comparison)62 visiteSome High-Latitude Areas on Mars (left) and Earth (right) exhibit similarly patterned ground where shallow fracturing has drawn Polygons on the surface. This patterning may result from cycles of freezing and thawing (---> disgelo).
The left image shows ground within the targeted landing area NASA's Phoenix Mars Lander before the Winter frost had entirely disappeared from the Surface. The bright ice in shallow crevices accentuates the area's polygonal fracturing pattern. The polygons are a few meters (several feet) across.
The image is a small portion of an exposure taken in March 2008 by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter.
The image on the right is an aerial view of similarly patterned ground in Antarctica.MareKromium
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