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| Risultati della ricerca nelle immagini - "Area," |
01-SMART-1%20northpole29Dec4.jpgThe "North Pole" of the Moon132 visiteCaption ESA originale:"This image was taken by the AMIE camera on board SMART-1 on 29 December 2004 from a distance of 5.500 Km.
It shows an area, 275 Km across, of heavily cratered highland terrain close to the Lunar North Pole (upper left corner).
The image is used to monitor illumination of the polar areas, and long shadows cast by large crater rims".
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029-Mars-16-PIA09224_fig1.jpgThe "Thickness" of Mars' South Polar Layered Deposits (Map 1)52 visiteThis map shows the thickness of the South Polar Layered Deposits of Mars, an ice-rich geologic unit that was probed by the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS). The MARSIS radar is an instrument on the European Space Agency's Mars Express orbiter. The thickness of the layered deposits was determined by measuring the time delay between radar echoes from the surface and those from the lower boundary, or "bed", of the deposits.
The radar data indicate that the deposit, larger than Texas in area, is more than 3,7 Km (about 2,3 miles) thick in places, and that the material consists of nearly pure water ice with only a small component of dust.
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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 ESAs 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 51,7 South and Longitude 159,2 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 cio 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 vero solo in teoria) o 2) 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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APOLLO 15 AS 15 87-11852 HR.jpgAS 15-87-11852 (HR) - Panorama with LM and LR315 visiteIstantanea ottenuta durante la seconda escursione (EVA-2) degli Astronauti Scott ed Irwin. Le grigie e (relativamente) dolci colline della Luna dominano il panorama che si stende dietro al Lunar Module ed al Lunar Rover i quali appaiono entrambi in tutta la loro piccolezza e fragilit.
Interessanti le tracce lasciate dalle ruote del Lunar Rover sulla superficie della Luna ma, soprattutto, ci colpiscono le impronte degli stivali indossati dagli astronauti (in primissimo piano).
Sono impronte che, salvo l'occorrere di eventi decisamente rari, imprevisti ed imprevedibili (un impatto meteorico proprio su quell'area, p.e.), resteranno immutate per l'eternit (o quasi).
La luminosit che proviene da Sole, piuttosto alto sull'orizzonte, conferisce all'immagine un quid di serena familiarit: la Luna, quando immersa nella luce, non sembra poi cos spettrale!...
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Almahata-Sitta15_2048.jpgAlmahata Sitta 1576 visiteDa "NASA - Picture of the Day", del giorno 28 Marzo 2009:"Small Asteroid 2008 TC3 fell to Earth at dawn on October 7, 2008, tracking through the skies over the Nubian Desert in Northern Sudan. That event was remarkable because it was the first time an asteroid was detected in space before crashing into planet Earth's Atmosphere.
It was generally assumed the asteroid itself had completely disintegrated to dust. But, based on satellite and ground observations of the atmospheric impact event, Dr. Mauwia Shaddad of the University of Khartoum, aided by Dr. Peter Jenniskens of the SETI Institute and NASA Ames Research Center, led an expedition of students and staff to the area, combing the desert for surviving fragments.
On December 6, 2008, 2 hours after their search began, the first meteorite was found. The team ultimately collected some 280 small meteorites, now called Almahata Sitta, with a total mass of about 5 kilograms -- the first material recovered from a known asteroid. In stark contrast to the lighter-colored stones, the black fragment in the picture is Almahata Sitta meteorite number 15. About 4 centimeters in diameter, it is seen as it came to rest on the desert floor".
Nota Lunexit: la fotografia, sebbene suggestiva, presenta - a nostro parere - delle notevoli incongruenze di texture e colore. In altre parole, sembra pi un image-composite che un vero e proprio single still.
Abbiamo quindi leggermente modificato la colorizzazione del frame, adattando il suolo al colore tipico della superficie del Deserto Sudanese (la "fotografia" originale sembra essere parecchio sovrasaturata) ed il colore blu del cielo stato leggermente abbassato di tonalit ed intensificato (cos ricreando - in visione - le condizioni atmosferiche tipiche dei cieli che sovrastano regioni desertiche in cui l'Atmosfera estremamente secca e l'Opacit - Atmosferica - bassissima o nulla).MareKromium
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Channels-Auqakuh_Vallis-MGS-PCF-LXTT.jpgAuqakuh Vallis: "Old Riverbed" or "Windblown Ripples"? (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunar Explorer Italia)54 visiteCaption NASA originale:"This MGS-MOC image shows windblown ripples on the floor of Auqakuh Vallis.
The light-toned area, running diagonally across the scene from South-West to North-East, may be dust that has accumulated in the bottom of the valley and on top of the ripples".
Location near: 31,3 North; 299,3 West
Image width: ~3 Km (~1,9 mi)
Illumination from: lower left
Season: Northern SpringMareKromium
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Channels-Auqakuh_Vallis-MGS.JPGAuqakuh Vallis: "Old Riverbed" or "Windblown Ripples"? (Original NASA/MGS/MSSS b/w Frame)54 visiteCaption NASA originale:"This MGS-MOC image shows windblown ripples on the floor of Auqakuh Vallis.
The light-toned area, running diagonally across the scene from South-West to North-East, may be dust that has accumulated in the bottom of the valley and on top of the ripples".
Location near: 31,3 North; 299,3 West
Image width: ~3 Km (~1,9 mi)
Illumination from: lower left
Season: Northern Spring
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Craters-Gale_Crater-PIA14290-PCF-LXTT.jpgGale Crater (Enhanced Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)189 visiteNASA has selected Gale cCrater as the Landing Site for the Mars Science Laboratory Mission. The Rover will be placed on the ground in a Northern portion of the Crater in August 2012. This view of Gale is a mosaic of observations made in the Visible-Light portion of the Spectrum by the Thermal Emission Imaging System camera on NASA's Mars Odyssey orbiter.
Gale crater is roughly 96 miles (about 154 Km) in diameter and holds a layered mountain rising about 3 miles (approx. 5 Km) above the Crater Floor. The ellipse superimposed in this image indicates the intended Landing Area, which is 12,4 miles (about 20 Km) by 15,5 miles (about 25 Km). The portion of the Crater within the Landing Area has an Alluvial Fan likely formed by water-carried sediments. The lower layers of the nearby mountain -- within driving distance for Curiosity -- contain minerals indicating a wet history.
The intended landing site is at 4,5 South Latitude and 137,4 East Longitude.
The Mars Science Laboratory Spacecraft is being prepared for launch during the period Nov. 25 to Dec. 18, 2011. In a prime mission lasting one Martian year -- nearly two Earth years -- after landing, researchers will use the Rover's tools to study whether the landing region has had environmental conditions favorable for supporting microbial life and for preserving clues about whether life existed.MareKromium
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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 costitu 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 svilupp in maniera interessante e costruttiva e ci port 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" certamente riduttivo...
Ogni riferimento alle stupidaggini proferite da noti Eso-Archeografi Italici e non, ASSOLUTAMENTE VOLUTO e NON CASUALE.MareKromium
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ESP_013951_1955_RED_abrowse-00.jpgDark Syrtis Major (CTX Frame - Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)52 visiteOn 13 October 1659, Dutch Astronomer Christiaan Huygens turned one of his telescopes towards a bright orange spot in the sky and produced what Percival Lowell would later call the first drawing of Mars worthy of the name ever made by man.
Huygens included a "dark spot" in his drawing that is thought to represent Syrtis Major, a small sliver of which is visible in this HiRISE image.
Syrtis Major is a Shield Volcano and its dark color comes from the dark Basaltic Rock present in the area, visible because it lacks the Dust that paints the rest of the Planet its distinct, rusty orangish color. By tracking this "dark spot" in repeated observations, Huygens concluded that Mars rotated every 24 hours: a time not too far off from its true rotation period of approx. 24 hours and 39,58 minutes.MareKromium
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Enceladus-PIA10573.jpgCrescent Enceladus (Natural Colors; credits: Lunar Explorer Italia)53 visiteCaption NASA:"Sunrise uncovers both old and new Enceladus in this image from the Cassini Spacecraft. The lit side of the moon faces Saturn in this view of the Trailing Hemisphere. Old craters still pockmark the Northern Hemisphere while more recent geologic activity has swept them away in the South. North is on the right (Dx) in this image.
Mountain Ranges, a.k.a. "Dorsae", undulate across the moon's surface near the Equator.
From this high northern viewing angle, the South Pole's fascinating "Tiger Stripe Area" lies just out of view. Sulci, a.k.a. "furrows", in that area, are the sources of icy plumes being studied by Cassini scientists.
(See also PIA07800 and PIA09761).
Also near the Tiger Stripes are rift segments that resemble the zigzag patterns seen on Earth of sea-floor spreading from upwelling magma. See PIA11138 for a comparison of the phenomena.
Like outstretched fingers, the Samarkand Sulci reach from the West toward the North Pole, clearing their path of craters and slicing some in half.
This Natural Colors mosaic combines narrow-angle camera images obtained through UltraViolet, Green, and near-InfraRed camera filters. The images were acquired on Dec. 2, 2008 at a distance of approx. 124.000 Km (such as about 77.000 miles) from Enceladus and at a Sun-Enceladus-Spacecraft, or Phase, Angle of 116.
Image scale is roughly 742 meters (2430 feet) per pixel".MareKromium
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Europa-PIA01144.jpgCold, cold world...52 visiteThis infrared image of Europa, showing heat radiation from its surface at a wavelength of 27 microns (millionths of a meter), provides the best view yet of Europa's daytime temperatures. Temperatures, derived from the brightness of the infrared radiation, can be determined from the colors by reference to the scale at the bottom of the image. The image, taken by Galileo spacecraft, shows the full disk of Europa, highly distorted by the relative motion of Europa and the spacecraft, centered on longitude 190, with North at the top. The data show that midday temperatures at Europa's Equator reach about 130 Kelvin (-225 F). The surface is even colder toward the Poles and before or after midday.
Small patches of different colors on Europa's disk show regions that are warmer or cooler than their immediate surroundings: the warm patches are generally relatively dark and thus absorb more sunlight, than neighboring Regions, while the cool patches are relatively bright. In the lower left corner, heat radiation from Jupiter itself, appearing orange-red in this representation, can be seen peeking out from behind Europa's disk.
The image was taken with Galileo's PPR (Photopolarimeter-Radiometer) instrument on the spacecraft's seventh orbit around Jupiter, from a range of about 65,000 kilometers (40,389 miles). Surface temperatures derived from the strength of infrared radiation, as was done here, are called "brightness temperatures", and may be slightly in error.
The PPR instrument builds up an image by slowly scanning across the target over a period of up to one hour. The motion of Galileo relative to Europa during this time causes distortions in the satellite shape on the image, which therefore does not appear circular. The small overlapping circles that make up the image show the size of the area, about 160 kilometers (99 miles) across, covered by each individual PPR measurement. Blue spots in the dark sky in the right-hand portion of the image are due to noise.
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