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0-APOLLO 15-launch_wide.jpgThe Launch of Apollo 15227 visiteThe "ORIGINAL" Apollo Time-Table (from Apollo 13)
APOLLO 13. March, 1970. Land in Fra Mauro formation of flat highlands, stay about 22 hours. Collect soil and rock from an old area relatively untouched by what many believed were ancient floods or volcanoes.
APOLLO 14. July, 1970. Land in Censorinus Crater area for a stay of about 22 hours. Investigate craters, possibly carved in Moon's surface by meteors.
APOLLO 15. November, 1970. Land in Littrow area of volcano-like projections, remain about 22 hours. Attempt a pinpoint landing on an exact, pre-selected target.
APOLLO 16. March, 1971. Descend to Crater Copernicus, remaining for about 70 hours. Extract from crater and high-rising column within formation rocks believed to be from far below the lunar surface.
APOLLO 17. Late in 1971. Land near rugged highland crater Tycho for stay of about 70 hours. Test first moon "rover" vehicle.
APOLLO 18. Early 1972. Land in Marius Hills, remain about 70 hours. Collect soil and rock samples from volcanic-like domes and valleys between.
APOLLO 19. Middle or late 1972. Land deep in Schroeter's Valley, with about 70 hours on the surface. Attempt a descent into a deep crater to determine cause of mysterious "red flashes" seen there by astronomers.
APOLLO 20. Late 1972 or early 1973. Land near the Hyginus Rill, a long, major canyon, for stay of about 70 hours. Investigate canyon for possible lunar core material.
This timeline had been altered slightly even before the Apollo 13 mission, when in January, 1970, Apollo 20 was cancelled in order to reserve the last production Saturn V for use in launching the planned Skylab orbiting laboratory a few years later. This change shifted the planned Apollo 18 and 19 lunar missions to 1974 to follow Skylab, but further budget-cutting in late 1970 also resulted in the cancellation of Apollo 18 and 19.
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000-0-Mars.jpgMeteor strike on Mars112 visiteMars may have lost much of its atmosphere during asteroid impacts early in its history.
The Beagle 2 lander will look for signatures of life on Mars, whether long-dead or still-living, by measuring the ratio of two different types of carbon in the rocks. Biological processes on Earth favour the lighter isotope of carbon, carbon-12, over the heavier carbon-13. Hence, a high carbon-12 to carbon-13 ratio is taken as evidence of life and has been found in rocks up to 4 billion years old, even where geological processing has occurred. The hope is that the same occurred on Mars.
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051-The Moon from Clem-Aristarchus.jpg043 - Aristarchus Plateau (natural colors)55 visiteA mosaic of more than 250 images showing the complex and diverse Aristarchus Region of the Moon in approximately natural colors (blue = 415 nanometers, green = 750 nanometers, red = 950 nanometers). The plateau is an uplifted block of complex, highland terrain, partly flooded by later mare basalt lavas. Dark, pyroclastic glasses partly cover the uplifted terrain. The crater Aristarchus (47 Km in diameter) has formed in the South-East corner of the plateau, excavating both highlands and mare rocks.
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085-Marshorizon_opportunity_big.jpgOk, it's official: NASA is "copying" our Work...109 visiteCari Amici, scusateci "l'arroganza" ma, guardate Voi stessi, a noi pare che questa visione di Marte - inclusiva dei commenti - non abbia nulla di diverso da alcune delle nostre più recenti elaborazioni sui “real colors of Mars” proposte in questa Sezione.
La NASA ci legge e ci copia, dunque?
Leggerci, diremmo proprio di si (la NASA, direttamente od indirettamente, legge tutto quello che il Web propone in materia di Spazio e quindi legge ANCHE Lun-Ex-It); copiarci, probabilmente no.
Diciamo che la NASA (e coloro che operano attorno ad essa) "si ispira", spesso, al Lavoro fatto dai Liberi e Privati Ricercatori di tutto il Mondo e poi, agendo da buon "ente ciclope", spaccia per farina del proprio sacco anche la farina "rubacchiata" (sorry: volevamo dire "presa a prestito - ma un prestito deciso unilateralmente, definitivo e non restituibile...) altrove.
Quest'opera, presentata nella rubrica "NASA - Picture of the Day" del 17 Ottobre 2006, non è altro che una versione (leggerissimamente) migliorata del nostro processo di colorizzazione delle immagini.
Ed il “dramma” lo sapete qual è? E’ che non sappiamo se essere fieri di noi stessi e del nostro lavoro oppure se renderci conto che è giunto il momento di “chiudere la baracca” e continuare a lavorare a “luci (completamente) spente”. La “fama”, a quel punto, non arriverà di certo, ma almeno i “ladri” non ci entreranno in casa con così grande facilità e sfacciataggine…
EccoVi il testo originale:"If you could stand on Mars -- what might you see? Like the robotic Opportunity rover rolling across the red planet, you might well see vast plains of red sand, an orange tinted sky, and wispy light clouds. The Opportunity rover captured just such a vista after arriving at Victoria Crater earlier this month, albeit in a completely different direction from the large crater. Unlike other Martian vistas, few rocks are visible in this exaggerated color image mosaic. The distant red horizon is so flat and featureless that it appears similar to the horizon toward a calm blue ocean on Earth. Clouds on Mars can be composed of either carbon dioxide ice or water ice, and can move quickly, like clouds move on Earth. The red dust in the Martian air can change the sky color above Mars from the blue that occurs above Earth toward the red, with the exact color depending on the density and particle size of the floating dust particles".
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088-SOL932-McMurdo_L257F-A814R1_cbr2-00.jpgMc Murdo Panorama (1)76 visiteCaption NASA originale:"This beautiful scene reveals a tremendous amount of detail in Spirit's surroundings. Many dark, porous-textured volcanic rocks can be seen around the Rover, including many on Low Ridge. Two rocks to the right of center, brighter and smoother-looking in this image and more reflective in infrared observations by Spirit's Miniature Thermal Emission Spectrometer, are thought to be meteorites. On the right, "Husband Hill" on the horizon, the rippled El Dorado sand dune field near the base of that hill and lighter-toned Home Plate below the dunes provide context for Spirit's travels since mid-2005. Left of center, tracks and a trench dug by Spirit's right-front wheel, which no longer rotates, have exposed bright underlying material. This bright material is evidence of sulfur-rich salty minerals in the subsurface, which may provide clues about the watery past of this part of Gusev Crater".
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088-SOL932-McMurdo_L257F-A814R1_cbr2-01.jpgMc Murdo Panorama (2)63 visiteCaption NASA originale:"Spirit has stayed busy at Winter Haven during the past six months even without driving.
In addition to acquiring this spectacular panorama, the Rover Team has also acquired significant new assessments of the elemental chemistry and mineralogy of rocks and soil targets within reach of the rover's arm. The team plans soon to have Spirit drive to a very nearby spot on Low Ridge to access different rock and soil samples while maintaining a good solar panel tilt toward the Sun for the rest of the Martian Winter.
Despite the long span of time needed for acquiring this 360° view - a few images at a time every few Soles over a total of 119 Soles because the available power was so low -- the lighting and color remain remarkably uniform across the mosaic".
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089-Craters-Licinia_Crater-PIA16050-PCF-LXTT-IPF.jpgLicinia Crater (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)67 visiteThis NASA - Dawn Spacecraft Framing Camera (FC) image of 4-Vesta shows Licinia Crater, which is the large Impact Crater positioned in the center of the picture. Licinia Crater has a fresh, sharp Rim that is scalloped in shape; all around the Inner Walls of Licinia Crater there are many Streaks of Dark and Bright Dusty Material cascading towards the Crater's center. There are also many hummocky Slumps of Material around the Crater's Walls and Base. A large Mound of Material (most likely made of small Rocks and Dust) is well visible in the Crater's center, and the Mound itself is surrounded by more smooth and dark unidentified Material. The possibility that such (as of yet, we repeat, unidentified) smooth Material visible on 4-Vesta's Surface might be the so-called "Impact Melt" is currently under investigation. Licinia Crater is one of the freshest Impact Craters that can be seen in this image.
This area visible here is located in the "Floronia Quadrangle" of 4-Vesta, in the Northern Hemisphere of the Giant Asteroid. The NASA - Dawn Spacecraft obtained this image with its Framing Camera (FC) on October 11, 2011. The image was taken through the Camera's Clear Filter and the distance of the Spacecraft from the Surface of 4-Vesta was, at the time that the picture was taken, of approx. 700 Km (such as a little less than 435 miles); the image has a resolution of about 63 meters (207 feet) per pixel. This picture of Licinia Crater was acquired during the HAMO (---> High-Altitude Mapping Orbit) phase of the mission.
This frame (which is an Original NASA - Dawn Spacecraft b/w image published on the NASA - Planetary Photojournal with the ID n. PIA 16050) 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 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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101955-Bennu-Z-Landing-GIF_Movie.gifThe Landing on 101955 Bennu129 visiteCaption NASA:" On October 20, 2020, after a careful approach to the boulder-strewn Surface, the OSIRIS-REx Spacecraft's arm reached out and touched Asteroid Bennu.
Dubbed a Touch-And-Go (TAG) sampling event, the 30 cm wide sampling head (TAGSAM) appears to crush some of the rocks in this snapshot. The close-up scene was recorded by the spacecraft's SamCam some 321 million kilometers from planet Earth, just after surface contact.
One second later, the Spacecraft fired Nitrogen gas from a bottle intended to blow a substantial amount of Bennu's regolith into the sampling head, collecting the loose surface material. Data show the Spacecraft spent approximately 5 more seconds in contact with Bennu's Nightingale sample site and then performed its back-away burn. Timelapse frames from SamCam reveal the aftermath". MareKromium
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16-Lunar Alps_H_SEMG9R7X9DE.jpgThe Lunar Alps103 visiteOriginal caption:"The European Alps were formed over millions of years by slow-moving sections of Earth’s crust pushed together, squeezing the land to form a giant arc of upthrust mountains, but the Lunar Alps were formed in an instant. It is thought that the Moon collided with a huge object, such as an asteroid, 3850 million years ago. The collision formed a huge crater, about 1000 Km in diameter. This crater was later filled with basaltic lava, forming the dark circular basin known as Mare Imbrium (Sea of Rains). After the explosive collision, fragments, rocks and dust fell back to the surface. While there is considerable debate as to the actual mechanism which formed the concentric rings, it is agreed they are not 'fallback' material. Some scientists argue that the the impact caused the lower layers to act as a liquid and that the rings then 'froze' in place. A flood of lava covered the lower inner one, but the outer one remains as a series of arc-shaped mountain ranges.
In places these mountains rise over 3000 metres. Their inner walls are steep and well defined, but their outer slopes become more broken as elevation decreases away from the impact site. Early European astronomers named them after familiar mountain ranges, such as the Juras, the Apennines and the Alps.
Seen in this image, Vallis Alpes (Alpine Valley) is a spectacular feature that bisects the Montes Alpes range. This valley was discovered in 1727 by Francesco Bianchini. It extends 166 kilometres from Mare Imbrium, trending north-east to the edge of the Mare Frigoris (Sea of Cold). The valley is narrow at both ends and widens to about 10 kilometres across.
The valley floor is a flat, lava-flooded surface that has narrow sinous ‘rille’ running down the middle. It is generally considered to be a 'graben', an area between two parallel faults which has dropped below the surrounding area. This is believed to have formed after the formation of the basin, but before the full maria lava flows. The rille corresponds to a ‘lava tube’ formed in a later geological episode by high-speed and low viscosity magma.
"SMART-1 is studying the signature of violent processes that took place during the formation of these giant impact basins, as well as the sequence of late volcanic history over the lunar surface until 3000 million years ago,” said ESA’s SMART-1 Project Scientist Bernard Foing.
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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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APOLLO 12 AS 12-46-6719 HR.jpgAS 12-46-6719 - Boot-Prints, "breccia" and little rocks (HR)501 visiteOriginal caption:"Cross-Sun to the south of the area where Pete Conrad collected the contingency sample starting at 115:23:55 (MT). One of the shallow trenches he made with the sampler is above center.
Scan courtesy NASA Johnson SC".
Cerchiatura Rossa: un curiosissimo (ed intrigante) rilievo a forma conica (o, comunque, "a punta") che, a quanto ne sappiamo, è passato del tutto inosservato.
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