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| Risultati della ricerca nelle immagini - "Craters'" |
00-VictoriafromMRO.jpgVictoria Crater, from MRO (natural colors)192 visiteQuesto (spettacolare) frame lo potete trovare, in "Approximate True Colors", anche sui Siti NASA dedicati alle Missioni Mars Reconnaissance Orbiter, Opportunity e sul NASA Planetary Photojournal.
Noi, dopo aver valutato le immagini a colori della Regione di Meridiani (sia ottenute dal suolo, sia orbitali), abbiamo concluso che questo frame è stato elaborato non solo in falsi colori, ma "a tavolino", usando un Programma tipo "Paint" o "Photoshop".
Ciò premesso, abbiamo prima decolorizzato il frame NASA Originale e quindi lo abbiamo raffinato e ricolorizzato usando un nostro modestissimo software.
Risultato (che potrete verificare Voi stessi avendo solo un pizzico di pazienza e quindi ponendo a confronto il frame "NASA Originale" con questo): la densità cromatica del frame elaborato da noi è finalmente omogenea (con colori credibili e congrui rispetto ai colori visibili "dal suolo") ed il frame, qualora sottoposto a stretching, non si sgrana (come invece accade al frame NASA Originale).
Attenzione: noi non stiamo dicendo che "siamo più bravi" della NASA! Stiamo solo dicendo che la NASA, per motivi che preferiamo non commentare, "pasticcia" il suo stesso lavoro.
Pensateci sopra...MareKromium
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003.jpgSpace Heat-Shields - The Area151 visite3 - IL LUOGO
In questa immagine 3D vediamo il Cratere Bonneville, così come ripreso dalla Sonda "Mars Global Surveyor".
Il numero 1 indica la posizione fornita dalla NASA per l’Heat-Shield; il 2 contrassegna una massiccia perforazione a forma di “8†a cavallo dell’orlo del Cratere ed interessata da visibili protuberanze; il 3 identifica il fondo del Cratere, contrassegnato da stratificazioni visibilmente rilevate.
Le lettere A, B e C evidenziano, invece, lungo il pendio, tre bande di materiale roccioso più chiare rispetto al colore del fondo del Cratere Bonneville stesso (presumibilmente si tratta di rocce aventi una composizione analoga a quelle della piana circostante).
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03-PythagorasCrater-1.jpgPythagoras Crater153 visiteCaption ESA originale:"This mosaic view of Pythagoras is composed of images taken by the AMIE camera during two successive orbits on 29 and 30 December 2004 from an altitude of ~ 4000 Km.
Pythagoras is a 120 km diameter complex large Lunar Crater characterized by a relatively flat crater floor, a central peak and terraced walls.
The terraced walls height reaches 5000 mt."
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08-AMIEmosaic-291204.jpgGioja, Mouchez, Poncelet, Carpenter and Pythagoras106 visiteUn bellissimo foto-mosaico (purtroppo una delle pochissime immagini ad oggi disponibili della Luna 'vista' dalla Sonda Europea SMART-1) che ci mostra una serie di interessanti e relativamente famosi crateri - su tutti il Cratere Pitagora - ripresi da una distanza di circa 4000 Km.
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13-Billy Crater.jpgBilly Crater (HR)75 visiteCrater Billy, located at 50,1° West and 13,8° South on the Lunar Surface at the southern edge of Oceanus Procellarum, has a diameter of 46 Km and is up to 1,3 Km deep.
Billy is filled with dark mare material and is one of the darkest spots on the Lunar Surface. The crater is deemed to be of age class 5 - indicating an ancient crater [in this case at least 3,2 BY old] and filled, or partially filled with lava.
The image represents a composite made from two raw images (i.e. no flat field or other corrections have been applied) of the region taken one orbit apart.
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14-De Gasparis Crater.jpgDe Gasparis Crater70 visiteDe Gasparis is a small to medium sized crater 30 Km in diamater located on the western flank of Mare Humorum. The rim of the crater is worn and eroded. The interior has, at some point, been flooded by lava and sits around 0,8 Km below the surrounding surface. The crater is intersected by a number of rimae including, running from top-left to lower-right of the crater, a part of the 93 Km long Rimae De Gasparis.
Due to the consistent depth of the rimae it evidently formed after the crater and is possibly associated with the tectonic activity which saw the infilling of the crater.
The crater is named after the Italian Astronomer Annibale de Gasparis (1819-1892, director of the observatory in Naples, Italy and discoverer of 9 asteroids). Along with the crater and rimae, asteroid 4279 is also named in his honour.
The image represents raw data and no flat field or other corrections have been applied.
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14-Peirce Crater-LO4.jpgPeirce Crater121 visiteCrateri (piccoli e geologicamente giovani) all'interno di un cratere (grande ed antico): questo, in pochissime e semplici parole, è quanto ci mostra ad una prima e superficiale occhiata il Cratere Peirce - immortalato nella sua curiosa forma e grande bellezza in questo frame d'epoca (Lunar Orbiter 4 - 1967). Da notare anche i "gradoni" che sembrano caratterizzare il suo versante Nord (come ricollegarli ad una meccanica formativa da impatto?) ed i modesti dossi - knobs e collinette, si direbbe - che intravediamo in area centrale e verso Sud, Sud-Est.
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15-Bond&Mayer Craters.jpgBond-Mayer Crater90 visiteAn image of craters Bond - after an American Astronomer - (large feature marked by two smaller crater on left of image) and Mayer - after a Czech Astronomer (large isloated crater on lower right) located in Northern Central Region of the Moon, near Mare Frigoris. The image is a composite of 5 AMIE images acquired on 5/6 February 2006, from altitudes ranging between 2685 (bottom of the composite) and 2709 Km (top). Each individual snapshot, taken with the AMIE clear filter, is a square of side about 135 Km. The whole composite covers approximately 270 Km. The outer rim of the original Bond Crater has been eroded and reshaped, and now it basically consists of an outline of hills and mounts.
The interior floor is relatively flat in comparison with the rim region, although there are sections of rough terrain near the northern rim. In the centre of the walled plain is a rille that runs toward East.
To the southeast of this formation is Bond-B, a circular, simple bowl-shaped crater.
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15-V-Parry.jpgFrà Mauro, Parry and Bonpland Crater, from Lunar Orbiter 5 (3D)78 visiteOriginal caption:"Stereoscopic view of 3 adjoining craters; Frà Mauro to the North (left), Parry (upper right) and Bonpland (lower right). The area where the 3 rims meet is about 1200 meters higher than the crater floors. The two linear rilles form a "V" whose apex is at the left edge of the photograph. They dissect the crater floors and rims alike. The more westerly rille is bordered on the West (near the center of the anaglyph) by a chain of domes. The adjacent areas of the rille is nearly filled with dark, smooth material that appears to have come from the domes".
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16-Lichtenberg Crater.jpgLichtenberg Crater (HR)70 visiteAn image of the prominent crater Lichtenberg with a diameter of 20 Km. The crater shows a 1300 mt height difference between crater floor and surrounding lava plain. The actual target of this observation was the 'ghost' crater on the lower left of Lichtenberg. It is almost hidden by overflown lava from Oceanus Procellarum in which it is located. This area is of high geological interest and it was selected for the study of the most recent lunar volcanism. It is thought to contain the youngest basalts on the Lunar Surface, with an age of about 1000 MY. Recent data show that lunar volcanism was active for at least 2000 MY from 4000 MY ago, ceasing at about 2000 MY. In Oceanus Procellarum, it is thought that these basalts are the youngest basalts on the lunar surface with an age of less than 1000 MY. This should be compared with the age of the Moon at about 4500 MY. This crater is named after the German physicist Georg Christoph Lichtenberg (1742-1799) who was professor at the newly formed Goettingen University.
Nota: a nostro parere, questa caption ESA è - sostanzialmente - del tutto incomprensibile ed anche errata. Nel momento in cui si sostiene, infatti, che il vulcanismo lunare è cessato da svariate centinaia di milioni di anni (o anche di più), implicitamente si dice che alcuni grandissimi Astronomi della nostra Storia, da Galileo a Flammarion (i quali hanno assistito a possibili eventi vulcanici lunari classificati come TLP nel famoso NASA Technical Report R-277), erano e sono, in realtà , dei "visionari".
Triste, come sempre; molto triste.
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25-Crater Hopmann.jpgA postcard from the Far-Side: Hopmann Crater71 visiteThis image, taken by the advanced Moon Imaging Experiment (AMIE) on board ESA’s SMART-1 spacecraft, shows one quarter of crater Hopmann - an impact structure about 88 Km in diameter.
AMIE obtained this image on January, 25th, 2006 from a distance of about 840 Km from the surface, with a ground resolution of 76 mt per pixel.
The imaged area, not visible from Earth because it is located on the Far-Side of the Moon, is positioned at Latitude of 51,7º South and Longitude 159,2º East. It covers a square of about 39 Km per side.
Nota: osservate con attenzione il bordo del cratere Hopmann e poi cercate di spiegare e di spiegarVi come un margine "infossato" come quello che vediamo in questa discreta (anche se leggermente sfuocata) immagine possa essere il semplice risultato di una, tutto sommato semplice, "meccanica di impatto".
Confrontate questo cratere, p.e., con Tsiolkowsky, Arago-C, Copernicus e Clavius e poi, se volete, provate a redigere una serie di elenchi di crateri lunari associati sulla base della loro apparenza esteriore (e cioè in base alla loro somiglianza): noterete che, delle due l'una:1) o le tipologie di impatti sono migliaia di migliaia di milioni (il che è vero solo in teoria) o 2) è ragionevole supporre che alcuni crateri potrebbero non essere il mero prodotto di un impatto.
E nel ragionarci sopra, tenete a mente il Rasoio di Okkam...
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27-Zucchius Crater.jpgZucchius Crater82 visiteThis image of the central peaks of crater Zucchius was obtained by AMIE on 14 January 2006 from a distance of about 753 kilometres from the surface, with a ground resolution of 68 metres per pixel.
The imaged area is centred at a latitude of 61.3° South and longitude 50.8° West. Zucchius is a prominent lunar impact crater located near the southwest limb. It is 66 kilometres in diameter, but due to SMART-1's proximity to the surface, the AMIE field of view covers only the central 35 kilometres of the crater in this image.
Because of its location, the crater appears oblong-shaped due to foreshortening. It lies just to the south-southwest of the Segner crater, and northeast of the much larger Bailly walled-plain. To the southeast is the Bettinus crater, a formation only slightly larger than Zucchius.
Zucchius formed in the Copernican era, a period in the lunar planetary history that goes from 1200 million years ago to present times. Another example of craters from this period are Copernicus (about 800 milion years old) and Tycho (100 million years old). Craters from the Copernican era show characteristic ejecta ray patterns - as craters age, ejecta rays darken due to weathering by the flowing solar wind.
The hills near the centre of the image are the central peaks of the crater, features that form in large craters on the Moon. This type of feature is formed by the impact of a small asteroid onto the lunar surface. The surface is molten and, similarly to when a drop of water falls into a full cup of coffee, the hit surface bounces back and solidifies into the central peak.
The Zucchius crater is named after the Italian Mathematician and astronomer Niccolo Zucchi (1586-1670).
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