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009-1-Ceres-PIA19884-PCF-LXTT-IPF-1.jpgWhite Unnamed Crater on 1-Ceres (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)59 visiteToday's APOD is an Extra Detail Magnification (or "EDM", for short) of yesterday's Contextual (or "CTX", for short) Frame, taken by the NASA - Dawn Spacecraft that shows us a small White Crater (---> also informally known as "White Spot") that is located in the Northern Hemisphere of the Dwarf Planet named 1-Ceres.
Now, we ask you one (extremely complicated, in fact) question that you, however, should try to answer: why, on 1-Ceres, the huge and deep Impact Craters do not show "White Material" inside them, while, on the other hand, the small and shallow ones (Impact Craters) do? Probably because, but we, as IPF, cannot be sure of this (just like everyone else), the White Material, in the end, does not belong to/comes from the Sub-Surface of 1-Ceres (as we thought, at the beginning), but it belongs to/comes from the Impactors. And you, what do you think?...If you want to share your opinion, please, write us at alphacentauri@intercom.it
The picture was taken from an altitude of approx. 915 miles (such as about 1472,5461 Km) from the Surface, with a resolution of roughly 450 feet (such as about 137,16 meters) per pixel, was taken on August 21, 2015.
This image (which is a crop taken from an Original NASA - Dawn Spacecraft's b/w and NON Map-Projected frame published on the NASA - Planetary Photojournal with the ID n. PIA 19884 - Dawn HAMO Image 8) has been additionally processed, extra-magnified to aid the visibility of the details, contrast enhanced and sharpened, Gamma corrected and then colorized (according to an educated guess carried out by Dr Paolo C. Fienga-LXTT-IPF) in Absolute Natural Colors (such as the colors that a normal human eye would actually perceive if someone were onboard the NASA - Dawn Spacecraft and then looked ahead, towards the Surface of 1-Ceres), by using an original technique created - and, in time, dramatically improved - by the Lunar Explorer Italia Team.MareKromium
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081-The Moon from Clem-SouthPole.jpg112 - Polar Areas: View of the South Pole54 visiteMosaic of about 650 Clementine images of the South Pole of the Moon, from 80° South Lat. to the Pole (center). The Near-Side of the Moon is the top half of the image; the bottom half is the Far-Side. The dark region near the Pole indicates an old depression, inside the rim crest of the South Pole-Aitken Basin. Large parts of this area (about 15.000 Km2) are permanently shadowed and bistatic radar results from Clementine indicate that they could contain deposits of water ice.
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090-Craters-Cornelia_Crater-PIA16489-PCF-LXTT-IPF.jpgCornelia Crater (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)106 visiteThis frame shows us a consistent number of examples of long, narrow and sinuous Gullies that scientists on NASA's Dawn Mission have found on the Giant Asteroid 4-Vesta. The Impact Crater shown here is called Cornelia and the Gullies inside it - called "Type-B" Gullies - are different substantially from the straighter, wider, shorter Gullies that Planetary Scientists have found on different Celestial Bodies (like the ones located on the Rims of many Martian Impact Craters, for instance) and which are designated as "Type-A" Gullies (and the reason of such a distinction is found in the circumstance that these two Gully-types have different formation mechanisms). This picture was obtained by the NASA - Dawn Spacecraft Framing Camera on January 11, 2012; North is up.
This frame (which is an Original NASA - Dawn Spacecraft b/w image published on the NASA - Planetary Photojournal with the ID n. PIA 16489) has been additionally processed and then colorized, according to an informed speculation carried out by Dr Paolo C. Fienga (LXTT-IPF), in Absolute Natural Colors (such as the colors that a human eye would actually perceive if someone were onboard the NASA - Dawn Spacecraft and then looked outside, towards the Surface of the Giant Asteroid 4-Vesta), by using an original technique created - and, in time, dramatically improved - by the Lunar Explorer Italia Team. Different colors, as well as different shades of the same color, mean, among others, the existence of different Elements present on the Surface of 4-Vesta, each having a different Albedo (---> Reflectivity) and Chemical Composition.MareKromium
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1-AA-Surveyor 5.jpgSurveyor 5 - September 1967239 visiteDal "NASA - Picture of the Day" di Sabato 23 Ottobre 2004:
"Safe!" In September 1967, during regular season play, the Surveyor 5 lander actually slid several feet while making a successful soft landing on the Moon's Mare Tranquillitatis. Equipped with television cameras and soil sampling experiments, the US Surveyor spacecraft were intended to determine if the lunar surface at chosen locations was safe for the planned Apollo landings. Surveyor 5 touched down on the inside edge of a small crater inclined at about 20°. Its footpad slipped and dug the trench visible in the picture. Covered with dusty lunar soil, the footpad is about half a meter in diameter".
Sembra essere passato un secolo (o anche di più) da quel Settembre del '67. Erano i giorni gloriosi della "Moon Race" fra USA ed URSS: il Mondo aveva tantissimi problemi (più o meno come oggi...), sparsi tra il Biafra, il VietNam e la Cold War, ma quando si guardava alla Luna l'Umanità, in fondo, era unita.
O così, almeno, mi sembra di ricordare...
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20000217a-PCF-LXTT-IPF.jpgOrbiting 433-Eros (Absolute Natural Colors; credits for the additional process. and color: Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)146 visiteCaption NASA:"This picture of 433-Eros, the first of an Asteroid taken from an orbiting spacecraft, is a mosaic of 4 images obtained by NEAR on February 14, 2000, immediately after the Spacecraft's insertion into orbit. We are looking down over the North Pole of Eros at one of the largest craters on the surface, which measures 4 miles (about 6 Km) across. Inside the crater walls are subtle variations in brightness that hint at some layering of the rock in which the crater formed. Narrow grooves that run parallel to the long axis of Eros cut through the South-Eastern part of the crater rim. A house-sized boulder is present near the floor of the crater; it appears to have rolled down the bowl-shaped crater wall. A large number of boulders is also present on other parts of the Asteroid's surface. The surface of the Asteroid is heavily cratered, indicating that 433-Eros is relatively old.
(Mosaic of images 0125956839, 0125957025, 0125957087, 0125957273)MareKromium
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20000217c.jpg433-Eros From orbit: the Giant Gouge (natural colors; credits: Lunexit)53 visiteThis picture was taken from NEAR on February 15, 2000, while the Spacecraft was passing directly over the large gouge that creates Eros's characteristic peanut shape.
It is a mosaic of individual images showing features as small as 120 feet (35 meters) across. Although most of the asteroid is in shadow, we are able to see inside the gouge. Many narrow parallel troughs closely follow the shape of the gouge. Although they appear curvilinear from this view, they are most likely oriented parallel to the length of the asteroid.
The strong lighting contrast along the terminator (the line separating day from night on Eros) makes it easy to see that most of the surface is saturated with impact craters. Inside the gouge, however, only smaller craters are present, indicating that the area within the gouge is younger than the surface along the terminator.
This implies that the event that caused the gouge must have happened more recently than the formation of the rest of the surface of Eros.
(Mosaic of images 0126023473, 0126023535, 0126023721, 0126023783, 0126023845, 0126023907, 0126024093, 0126024155)MareKromium
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20000309.jpgOblique view of the "Large Crater" (natural colors; credits: Lunexit)53 visiteThis image, showing an oblique view of Eros' "Large (central) Crater", was taken at a resolution of about 20 meters (65 feet) per pixel. The brightness or albedo patterns on the walls of this crater are clearly visible, with the brighter materials near the tops of the walls and darker materials on the lower walls. Boulders are seen inside this crater and the smaller nearby craters. The higher density of craters to the left of the large crater implies that this region is older than the smoother area seen associated with the Saddle Region on the opposite side of the asteroid.
(Image 0127591846)MareKromium
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31-Gassendi.jpgGassendi Crater61 visiteCaption ESA originale:"This mosaic of 2 images, taken by the advanced Moon Imaging Experiment (AMIE) on board ESA's SMART-1 spacecraft, shows the inside of crater Gassendi. AMIE obtained these images on 13 January 2006, 1' apart from each other, from a distance of about 1220 Km(top frame) and 1196 Km (bottom frame) from the surface, with a ground resolution of 110 and 108 mt per pixel, respectively.
The area shown in the top image is centred at a Latitude of 16,2º South and Longitude 40,2º West, while the bottom images is centred at a Latitude of 17,9º South and Longitude 40,2º West.
Gassendi is an impact feature located on the Near Side of the Moon, at the Northern Edge of Mare Humorum. The crater is actually much larger than the field of view visible in this image. The hills on the lower right of the mosaic are the central peak of the crater, with a height of roughly 1,2 Km. The crater almost fully visible on the top is called Gassendi A".
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35-Lomonosov Crater-AMI_EAE3_001856_00042_00038.jpgLomonosov Crater73 visiteCaption ESA originale:"This image, taken by the Advanced Moon Imaging Experiment (AMIE) on board ESA’s SMART-1 spacecraft, shows crater Lomonosov, on the Moon’s Far (or "Dark") Side.
AMIE obtained the image on 30 January 2006 from a distance of about 2100 Km from the surface, with a ground resolution of 190 mt per pixel. The imaged area is centred at a Latitude of 27,8º North and a Longitude of 98,6º East.
Crater Lomonosov is a nice example for a large crater (92 Km of diameter) which was filled by lava after the impact, thus exhibiting a flat floor. The terraced walls indicate 'slumping', that is sliding of the rocks downwards due to gravity after the end of the impact. The small craters inside Lomonosov are the result of impacts into this lava floor which happened after the formation of Lomonosov".
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36-Shackleton_Crater-AMI_EAE3_001775_00002_00020.jpgSchakleton Crater in natural colors56 visiteThe Advanced Moon Imaging Experiment Camera (AMIE) obtained this image on 13 January 2006 - close to the time of Lunar Southern Summer - from a distance of about 646 Km over the surface and with a ground resolution of 60 mt per pixel.
Shackleton crater lies at the Lunar South Pole (89,54° S. Lat. and 0° East Lng.) and has a diameter of approx. 19 Km.
SMART-1 monitored this area almost every orbit. This will allow to produce very high resolution maps of the area as well as illumination maps. The long shadows that surround the crater make it very hard to observe. The analysis of the data obtained allowed a very detailed map of its rim, surrounding ejectas and craters.
SMART-1 also made long repeated exposures to see inside the shadowed areas. The purpose was detecting the very weak reflected light from the crater rims, and therefore study the surface reflection properties (albedo) and its spectral variations (mineralogical composition). These properties could reveal patchy ice surface layers inside the crater.
On the 2-kilometre wide inner edge of the crater ridge, at times barely visible from Earth, astronomers using ground radio-telescopes have recently reported they were not able to detect a distinctive signature of thick deposits of ice in the area. Earlier measurements by NASA's Lunar Prospector reported of hydrogen enhancement over large shadowed areas.
"We still do not know if this hydrogen is due to enhanced trapping of solar wind, or to the water ice brought on the Moon by the bombardment of comets and asteroids," says Bernard Foing, ESA's SMART-1 Project Scientist. "These bodies may have deposited on the Moon patchy layers of ice filling about 1.5 percent of the areas in permanent shadow, down to one metre below the surface."
"We need to analyse all remote sensing data sets consistently. Future lander and rover missions to the Moon will help in the search and characterisation of lunar polar ice, both on the surface and below the subsurface," Foing continues. "In any case, one day we may even be able to simply combine the implanted hydrogen and the oxygen extracted from lunar rocks to produce clean water, like we do in laboratory experiments on Earth.”
The crater is named after Ernest Shackleton (1874-1922), an explorer famous for his Antartic expeditions.
MareKromium
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41-Mezentzev Crater.jpgCraters Mezentsev, Niepce and Merril56 visiteThis image was taken by the Advanced Moon Imaging Experiment (AMIE) on 16 May 2006. The imaged area is centred at a Latitude of 73° North and a Longitude of 124° West, on the Far-Side of the Moon.
Normally, the AMIE camera is pointed straight down at the Lunar Surface, in the Nadir pointing mode. In this image, AMIE was pointed towards the horizon, showing the Lunar Surface in an oblique view.
The largest craters in this image are Mezentsev, Niepce and Merrill. Mezentsev is an eroded crater 89 Km in diameter and centred at 72,1° N, and 128,7° W.
A smaller cup-shaped crater resides inside Mezentsev. Niepce and Merrill both have a diameter of 57 Km and are located at 72,7° N-119,1° W and 75,2° N and 116,3° W, respectively.
Mezentsev Crater is named after Yourij Mezentsev, a Soviet engineer (1929 - 1965) who was one of the first people to design rocket launchers, while Joseph Niepce was the French inventor of photography (1765 - 1833); Paul Merrill was an American astronomer (1887 - 1961).
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A - Pluto and Charon - HST.jpgPluto and Charon from the Hubble Space Telescope128 visiteAggiornamento del 19 Agosto 2006: il Sistema "Plutone-Caronte", sino a ieri considerato un sistema equiparabile a quello Terra-Luna (in cui Plutone, al pari della Terra, è il Corpo Maggiore e Caronte, invece ed al pari della Luna, quello minore e dunque SOLO Satellite del primo), in accordo ad una decisione dell'International Astronomical Union (IAO) è stato ora rubricato come "Doppio Pianeta".
Caption IAU originale:"Both Pluto and Charon each are large enough (massive enough) to be spherical. Both bodies independently satisfy the definition of “planet”. The reason they are called a “double planet” is that their common centre of gravity is a point that is located in free space outside the surface of Pluto. Because both conditions are met: each body is “planet-like” and each body orbits around a point in free space that is not inside one of them, the system qualifies to be called a “Double Planet”.
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