| Piú viste - Mars Reconnaissance Orbiter (MRO) |
PSP_010025_1410_RED.jpgDark Area in Hartwig Crater (possible True Colors; credits: Lunar Explorer Italia)57 visiteMars Local Time: 15:39 (middle afternoon)
Coord. (centered): 38,2° South Lat. and 344,1° East Long.
Spacecraft altitude: 256,7 Km (such as about 160,4 miles)
Original image scale range: 51,4 cm/pixel (with 1 x 1 binning) so objects ~1,54 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 6,6°
Phase Angle: 82,8°
Solar Incidence Angle: 78° (meaning that the Sun is about 12° above the Local Horizon)
Solar Longitude: 127,6° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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PSP_010017_1460_RED.jpgRelatively Flat Crater Floor bounded By sharp change in Slope (possible True Colors; credits: Lunar Explorer Italia)57 visiteMars Local Time: 15:42 (middle afternoon)
Coord. (centered): 33,7° South Lat. and 202,9° East Long.
Spacecraft altitude: 253,3 Km (such as about 158,3 miles)
Original image scale range: 50,7 cm/pixel (with 1 x 1 binning) so objects ~1,52 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 5,2°
Phase Angle: 71,8°
Solar Incidence Angle: 75° (meaning that the Sun is about 15° above the Local Horizon)
Solar Longitude: 127,3° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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PSP_010063_2135_RED.jpgIsmenius Lacus (possible True Colors; credits: Lunar Explorer Italia)57 visiteMars Local Time: 14:16 (early afternoon)
Coord. (centered): 33,2° North Lat. and 17,4° East Long.
Spacecraft altitude: 296,7 Km (such as about 185,5 miles)
Original image scale range: 29,7 cm/pixel (with 1 x 1 binning) so objects ~59,4 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 6,9°
Phase Angle: 54,4°
Solar Incidence Angle: 47° (meaning that the Sun is about 43° above the Local Horizon)
Solar Longitude: 129,0° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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PSP_010054_1765_RED.jpgPlain North-West of Tithonium Chasma (possible True Colors; credits: Lunar Explorer Italia)57 visiteMars Local Time: 15:34 (middle afternoon)
Coord. (centered): 3,6° South Lat. and 268,4° East Long.
Spacecraft altitude: 260,2 Km (such as about 162,6 miles)
Original image scale range: 52,1 cm/pixel (with 1 x 1 binning) so objects ~1,56 mt across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,3°
Phase Angle: 57,8°
Solar Incidence Angle: 58° (meaning that the Sun is about 32° above the Local Horizon)
Solar Longitude: 128,7° (Northern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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PSP_010047_1745_RED-01.jpgStar-like shaped Hill in Terra Tyrrhena (edm - possible True Colors; credits: Lunar Explorer Italia)57 visite...Pubblichiamo questo extra-detail magnification (edm) girando a Voi la domanda postaci dal nostro Caro Amico "Cano00": questa striscia di puntini (si direbbero dei mini-segmenti scuri) allineati, che cos'è? E' un intrigantissimo rilievo superficiale, oppure è un image-artifact?
Ed in ogni caso: COMPLIMENTI a Cano00 per l'occhio (straordinario) che ha avuto!...MareKromium
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PSP_005392_0995_RED_abrowse-01~0.jpgImpact Crater on the South Polar Layered Deposits (EDM n.1; MULTISPECTRUM - credits: Lunexit)57 visiteA problem with using craters to determine age on the icy SPLD is that erosion of the icy substrate and relaxation of crater topography (i. e., relief becoming more gentle) is probably more rapid on ice than on harder rocky surfaces.
A detailed study of craters in ice will help better to understand this process of how craters in ice degrade, or deteriorate, with time.
Perhaps then we will know how to use the number and distribution of craters over the icy polar layered deposits in constraining the geologic and climate history of the Mars Polar Regions.MareKromium
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PSP_005343_2170_RED_abrowse-00~0.jpgScarp with Landslides and Boulder Tracks (context frame; natural colors - elab. Lunexit)57 visiteThis observation shows an equatorial scarp (cliff) with possible landslides and boulder tracks.
The cliff has several distinct layers visible near its top. There is a smoother, possibly fine-grained layer on top, underlain by a relatively bright and a dark layer. It is possible that the entire cliff face consists of layers but that erosion has not exposed others yet.
There are two main landslide scars, locations where a landslide has carved into the slope. Both of the scars have boulder tracks, several of which have boulders at their ends as they progress down the slope or reach the end of the slope.MareKromium
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PSP_006252_2220_RED_abrowse.jpgLineated Valley Fill (MULTISPECTRUM; credits: Lunexit)57 visiteFlow patterns dominate this Region of Mars in Deuteronilus Mensae. Many of the valley floors in the area exhibit complex alignments of small ridges, hills, and pits – often called “lineated valley fill”. The cause of the small-scale texture is not known, but it may result from patterns in ice rich soils or the loss of ice.
The linear alignment we see is probably caused by downhill movement of ice-rich soil, or glacial flow in dirty ice or ice-rich soil.
The result is flow patterns, called “stream lines”, that follow the valleys and around obstacles. Many of the large knobs and mesas in this region are also surrounded by aprons of debris that appear to have flowed away from the knobs and may be ice-rich themselves. Around one large knob in this image the debris flow appears to lie on top of the lineated valley fill and is therefore probably a younger deposit.MareKromium
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PSP_004071_1425_RED_browse-01.jpgMesas in Gorgonum Chaos (edm - possible True Colors; credits: Lunar Explorer Italia)57 visitePSP_004071_1425 shows mesas that are part of Gorgonum Chaos, a region of chaotic terrain, which is a jumble of mounds and mesas grouped together.
Chaotic terrain is most commonly found in Mars near the sources of the gigantic outflow channels. Gorgonum Chaos is one of the few exceptions.
Some of the troughs between the mesas appear to have V-shaped bottoms; there is no obvious flat floor in between. Others have dunes running down their centers probably indicating flat floors. It is possible that the mesas were once connected and that something caused fractures in the original mesa's surface that were then preferentially eroded.MareKromium
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Psp_001443_1695_red~0.jpgFeatures of Melas Chasma (possible True Colors; credits: Lunar Explorer Italia)57 visitenessun commentoMareKromium
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Psp_001477_2470_red.jpgDust Devils' Tracks on the Northern Plains (possible True Colors; credits: Lunar Explorer Italia)57 visitenessun commentoMareKromium
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PSP_001521_2025_RED_abrowse-00.jpgThe Viking Lander 1 Landing Site - Thomas Mutch Memorial Station (ctx frame - Natural Colors; credits: Lunar Explorer Italia)57 visiteViking Lander 1 (VL1) touched down in Western Chryse Planitia on July 20, 1976.
The Lander, which has a diameter of about 3 meters, has been precisely located in the HiRISE orbital image, and likely locations have been found for the Heat-Shield, Backshell and Parachute attached to the Backshell.
The Lander location has been confirmed by overlaying the lander-derived topographic contours on the HiRISE image, which provides an excellent match. VL1 was one element of an ambitious mission to study Mars, with a 4-spacecraft flotilla consisting of 2 Orbiters and 2 Landers.MareKromium
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