Mars Reconnaissance Orbiter (MRO)
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ESP_011610_0935_RED_abrowse.jpgSawtooth Pattern in Carbon Dioxide Ice (Natural Colors; credits: Lunar Explorer Italia)54 visitenessun commentoMareKromium
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ESP_011618_1885_RED_abrowse-00.jpgRecent Double-Impact (ctx frame - possible Natural Colors; credits: Lunar Explorer Italia)61 visiteMars Local Time: 15:46 (middle afternoon)
Coord. (centered): 8,6° North Lat. and 46,8° East Long.
Spacecraft altitude: 273,6 Km (such as about 171,0 miles)
Original image scale range: 27,4 cm/pixel (with 1 x 1 binning) so objects ~82 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 5,9°
Phase Angle: 64,1°
Solar Incidence Angle: 58° (meaning that the Sun is about 32° above the Local Horizon)
Solar Longitude: 193,2° (Northern Autumn)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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ESP_011618_1885_RED_abrowse-01.jpgRecent Double-Impact (edm - possible Natural Colors; credits: Lunar Explorer Italia)65 visiteThe MRO Context Imager (CTX) team has been discovering many new impact events on Mars, and then they request HiRISE follow-up imaging to confirm an impact origin and to identify and measure the craters.
Crater clusters are common as these small (typically less than 1 meter diameter) objects break up in the thin Martian air and separate a little bit to make crater clusters up to a few hundred meters wide. The example shown here is the result of an impact that occurred between May 2003 and September 2007.
It was first discovered as a dark spot in a CTX image acquired in March 2008, but later found to be partly visible at the very edge of a CTX image acquired in September 2007.
A dark spot is not present in the previous image of this location with sufficient resolution to have detected it, acquired by the visible THEMIS camera on Mars Odyssey in May 2003. Thus the impact might have formed anytime between May 2003 and September 2007. The dark markings are created by removing or disturbing the surficial dust cover, and so far new impact sites have been discovered only in dust-covered regions of Mars.
Although small Martian crater clusters are common, this example is unusual because there is a dark line between the two largest craters. We hypothesize that atmospheric breakup coincidentally made two nearly equal-size objects that impacted close together in space and time so the air blasts interacted with each other to disturb the dust along this line.
Hundreds of these small objects (mostly asteroid fragments) impact Mars per year. A comparable number of small objects impact Earth each year, but explode in the upper reaches of our atmosphere and have no effect on the surface, fortunately for those of us who live here.MareKromium
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ESP_011630_0930_RED_abrowse.jpgFans and Polygons (Natural Colors; credits: Lunar Explorer Italia)54 visitenessun commentoMareKromium
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ESP_011631_1515_RED_abrowse.jpgInside Hellas Basin (Natural Colors; credits: Lunar Explorer Italia)85 visiteThis image shows part of the floor of an impact crater on the Northern Rim of the giant Hellas Basin.
Hellas includes the lowest elevations on Mars, and may have once held lakes or seas; layered rock outcrops occur around much of the edge of the basin. At this site, a large impact crater (about 90 kM across) was partly filled by layered rocks. These rocks on the crater floor are now eroding and forming strange pits.
Here, the layers are mostly exposed on a steep slope which cuts across much of the image. On this slope, they crop out as rocky stripes, some continuous and others not. The material between the stripes is mostly covered by debris, but some areas of exposed rock are visible. The slope is capped by a thick, continuous layer that armors it against erosion; once this cap is gone, the lower material is removed rapidly, forming the steep slope. At the base of this slope, rocks on the floor of the pit appear bright and heavily fragmented by cracks known as joints. The variation in rock types suggests that the rocks here were deposited by multiple processes or in different environments. Sites like this may preserve a record of conditions on early Mars.
Mars Local Time: 15:55 (middle afternoon)
Coord. (centered): 28,4° South Lat. and 57,1° East Long.
Spacecraft altitude: 256,9 Km (such as about 160,6 miles)
Original image scale range: 25,7 cm/pixel (with 1 x 1 binning) so objects ~51,4 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,3°
Phase Angle: 60,1°
Solar Incidence Angle: 60° (meaning that the Sun is about 30° above the Local Horizon)
Solar Longitude: 193,8° (Northern Autumn)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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ESP_011633_1195_RED_abrowse.jpgDunes (Natural Colors; credits: Lunar Explorer Italia)57 visitenessun commentoMareKromium
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ESP_011635_1510.jpgRitchey Crater (perspective view - Natural Colors; credits: Dr M. Faccin & Lunexit)76 visitenessun commentoMareKromium
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ESP_011635_1510_RED_abrowse.jpgRitchey Crater's Central Uplift (Natural Colors; credits: Lunar Explorer Italia)72 visiteThe Natural Color image of this observation includes some interesting features in and near the central uplift of Ritchey Crater.
At the top is an ancient streambed, above center are very bright rocks and minerals can be seen in the Central Uplift. Large impact craters are unstable when they are formed, because their Walls are so steep.
Gravity causes the Walls to collapse toward the center of the Crater, colliding to form an Uplift or Peak. This process of Central Uplift formation can bring rocks from deep in the Crater Walls up to the surface. The angular bright blocks near the center of this image show that this process breaks the wall rocks into fragments as the Central Uplift is formed.
Mars Local Time: 16:00 (middle afternoon)
Coord. (centered): 28,5° South Lat. and 309,1° East Long.
Spacecraft altitude: 264,8 Km (such as about 165,5 miles)
Original image scale range: 26,5 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: 15,1°
Phase Angle: 46,9°
Solar Incidence Angle: 61° (meaning that the Sun is about 29° above the Local Horizon)
Solar Longitude: 194,0° (Northern Autumn)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer ItaliaMareKromium
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ESP_011648_1730_RED_abrowse-00.jpgOval Mesa on Ganges Mensa (and another "mistery" solved) - Natural Colors; credits: Lunar Explorer Italia94 visiteMars Local Time: 15:56 (middle afternoon)
Coord. (centered): 7,2° South Lat. and 311,5° East Long.
Spacecraft altitude: 277,5 Km (such as about 173,4 miles)
Original image scale range: 27,8 cm/pixel (with 1 x 1 binning) so objects ~83 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 17,7°
Phase Angle: 41,0°
Solar Incidence Angle: 59° (meaning that the Sun is about 31° above the Local Horizon)
Solar Longitude: 194,6° (Northern Autumn)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer Italia
This Oval Mesa is a remnant of a geological unit that once covered this area, similar to the Mesas and Buttes in Monument Valley, in Arizona and Utah. This is a small remnant of a much larger unit of similar material that caps Ganges Mensa to the West.
As can be seen in the sides of this small Mesa, this remnant consists of a layered stack of rock. Prior to the massive erosion that left this a high-standing Mesa, a more gentle phase of erosion created the small hills and whorls on the upper surface of the Mesa. It seems that this gentle erosion continued even after the Mesa was created, as this pattern of small hills and whorls is visible on the terrain surrounding the Mesa.
Although not visible in the area shown in this HiRISE image, this Mesa actually sits on top of the much larger Ganges Mensa, which is itself a large Mesa within Ganges Chasma.
Nota Lunexit: una diversa ripresa di questo medesimo dettaglio costituì oggetto di una lunga discussione sul Forum degli Amici di "UFO-On Line". La querelle riguardava la presenza di un presunto (ed oggi, come viene ben dimostrato da questa nuova immagine, inesistente) "ingresso" (porta) sul versante Nord-Occidentale della Mesa Ovale che campeggia a centro frame. La discussione, forse innescatasi a seguito delle deliranti asserzioni di un noto Eso-Archeografo Italiano (e relative alla presenza di "evidenti accessi a presidi minerari" sul Pianeta Rosso...) si sviluppò in maniera interessante e costruttiva e ci portò anche al calcolo delle possibili dimensioni della "porta".
Oggi, grazie a questa nuova immagine - che pubblichiamo anche in versione RAW Original b/w - tutti potranno constatare che quella che SEMBRAVA essere una "porta" era, in vero, solo un leggero incavo (indentation) naturale presente sulla parete Nord-Occidentale della Mesa.
Morale: prima di parlare e di lanciarsi in interpretazioni che superano la Fantasia e sconfinano nella Bufala al 100% (e qui, che sia chiaro, NON CI RIFERIAMO agli Amici di "UFO-On Line"!), conviene sempre STUDIARE, DOCUMENTARSI, FARE CONFRONTI FRA DIVERSE IMMAGINI e poi, se proprio si vuol dare aria alla bocca e lavoro alla tastiera, SI SUGGERISCE DI RESTARE SEMPRE POSSIBILISTI - onde evitare di fare delle figure che definirle "meschine" è certamente riduttivo...
Ogni riferimento alle stupidaggini proferite da noti Eso-Archeografi Italici e non, è ASSOLUTAMENTE VOLUTO e NON CASUALE.MareKromium
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ESP_011648_1730_RED_abrowse-01.jpgOval Mesa on Ganges Mensa (and another "mistery" solved) - Full image, map projected, RAW b/w53 visitenessun commentoMareKromium
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ESP_011648_1730_RED_abrowse-02.jpgOval Mesa on Ganges Mensa (and another "mistery" solved) - Full image, non-map projected and Natural Colors; credits: Lunar Explorer Italia53 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)54 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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