Risultati della ricerca nelle immagini - "de" |
000-OPP-SOL1095-MF-LXT.jpgVictoria's Capes - Sol 1095 (Hi-Def3-D - credits and Copyright: Dr M. Faccin and Lunar Explorer Italia)100 visiteUna "Nuova Visione" di Marte, Made by Lunexit: si tratta di frames processati tridimensionalmente, ma adottando una tecnica ed un processing totalmente innovativi.
Confrontate queste "Visioni di Marte" con i 3D "Standard" NASA e...Vedrete la differenza, e CHE differenza!
Questa tecnica di elaborazione delle immagini (sviluppata da Marco Faccin e Gianluigi Barca, sotto Copyright Lunar Explorer Italia) è il primo passo verso la creazione di frames tridimensionali a colori (non più il "solito" blu/verde e rosso) e ad altissima definizione. Frames che permetteranno a chiunque li guardi (ed anche a persone che hanno problemi di vista) di mettere - letteralmente - gli occhi ed il naso "all'interno del paesaggio ripreso".
Ed ora (e per il momento), indossate gli "occhialini" e...in un istante Vi ritroverete DENTRO e AD UN PASSO dal margine e dai Promontori di Victoria Crater!
MareKromium
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000-The Moon from Clem.JPG014 - Light-up the Moon!58 visiteMosaic of the near side of the Moon lit by Earthshine, as imaged by a Startracker camera on March 15, 1994.
The Southern Hemisphere is up.
The bright crater toward the top of the image is Tycho.
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015-The Moon from Clem-FarSide-PIA00304.jpg002 - The Far-Side of the Moon55 visiteClementine Project Information
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Clementine was a joint project between the Strategic Defense Initiative Organization and NASA. The objective of the mission was to test sensors and spacecraft components under extended exposure to the space environment and to make scientific observations of the Moon and the near-Earth asteroid 1620 Geographos. The observations included imaging at various wavelengths including ultraviolet and infrared, laser ranging altimetry, and charged particle measurements. These observations were originally for the purposes of assessing the surface mineralogy of the Moon and Geographos, obtaining lunar altimetry from 60N to 60S latitude, and determining the size, shape, rotational characteristics, surface properties, and cratering statistics of Geographos.
Clementine was launched on 25 January 1994 at 16:34 UTC (12:34 PM EDT) from Vandenberg AFB aboard a Titan IIG rocket. After two Earth flybys, lunar insertion was achieved on February 21. Lunar mapping took place over approximately two months, in two parts. The first part consisted of a 5 hour elliptical polar orbit with a perilune of about 400 km at 28 degrees S latitude. After one month of mapping the orbit was rotated to a perilune of 29 degrees N latitude, where it remained for one more month. This allowed global imaging as well as altimetry coverage from 60 degrees S to 60 degrees N.
After leaving lunar orbit, a malfunction in one of the on-board computers on May 7 at 14:39 UTC (9:39 AM EST) caused a thruster to fire until it had used up all of its fuel, leaving the spacecraft spinning at about 80 RPM with no spin control. This made the planned continuation of the mission, a flyby of the near-Earth asteroid Geographos, impossible. The spacecraft remained in geocentric orbit and continued testing the spacecraft components until the end of mission.
More information on the Clementine mission, instruments, and early results can also be found in the Clementine special issue of Science magazine, Vol. 266, No. 5192, December 1994.
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017-The Moon from Clem-NearSide-PIA00302.jpg003 - The Near-Side of the Moon56 visiteAbout 50.000 Clem images were processed to produce the 4 orthographic views of the Moon. Images PIA00302, PIA00303, PIA00304 and PIA00305 show albedo variations (normalized brightness or reflectivity) of the surface at a wavelength of 750 nm (just longward of visible red). The Lunar Near-Side is a contrast between dark and light albedo surfaces that has been fancied as the "Man in the Moon". Lunar terrain types are still designated by their 17th century name and that is:
1. Maria (dark albedo features also known as basins) and
2. Terra (brighter albedo features also known as uplands or highlands).
The Maria constitutes about 16% while the Terra 84% of the Lunar Surface. The nearside is composed of about 30 percent maria. Extensive bright ray systems surround craters Copernicus (upper left center) and Tycho (near bottom).
Studies have shown that two major processes, impact and basaltic volcanism have shaped the major physical features of the Lunar Surface.
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032-Mars_Interior.jpgWhat's inside Mars?173 visiteMars interior is simply modeled as a core and mantle with a thin crust, similar to Earth. Mars' size and total mass are known. Given four parameters, the core size and mass and mantle size and mass can be determined.
The combination of Pathfinder Doppler data with earlier data from the Viking Landers has determined a very important parameter, the "Moment of Inertia", through measurement of Mars' precession rate. A fourth measurement is needed to complete the interior model. This may be achieved through future Doppler tracking of Pathfinder, since the presence of a fluid core may be detectable through its effect on Mars' nutation. The determination of the moment of inertia is a significant constraint on possible models for Mars' interior. If the core is as dense as possible (i.e. completely iron) and the mantle is similar to Earth's (or similar to the SNC meteorites thought to originate on Mars) then the minimum core radius is about 1300 Km. If the core is made of less-dense material (i.e. a mixture of iron and sulfur) than the core radius is probably no more than 2000 Km.
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033-Mars_Rotation.jpgMars' Rotation and Orbit Dynamics129 visiteMars rotation around its pole causes a signature in the data with a daily minimum, when the Lander is closest to the Earth. Changes in such a daily signature may reveal information about the interior of Mars, through its effect on Mars' precession and nutation.
The signature is also sensitive to variations in Mars' Rotation Rate, as the mass of the atmosphere increases and decreases along with the Polar Caps increase and decrease (obviously the Polar Caps increase during the Martian Fall and Winter and then, due to the higher heating of the Planet - and subsequent evaporation phoenomena - they decrease in Spring and Summer).
Long term signatures in the range to the Lander are caused by asteroids perturbing Mars' orbit; an analysis of these perturbations may allow us to also determinate the masses of these asteroids.
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0800-ExplodedPipe.jpgExploded "Pipe" - and other "Things" (by Dr M. Faccin)116 visiteUn titolo autoesplicativo; un'elaborazione perfetta e dei contenuti...straordinariamente esotici ed affascinanti!MareKromium
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14-vg1_1610104.jpgJupiter, Io, Ganymede and...54 visiteL'oggetto indicato dalla freccia e contraddistinto da un "?" non è un photoartifact (nella maniera più categorica) e non è neppure una delle altre Lune Maggiori (o Galileiane) di Giove - e quindi non si tratta nè di Europa, nè di Callisto.
Abbiamo pensato potesse trattarsi di Amalthea, ma l'oggetto è troppo piccolo e non riusciamo a risolverlo per osservarne i dettagli superficiali e, soprattutto, le fattezze esteriori.
Se qualcuno di Voi avesse delle idee, ci scriva!
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500-PIA02233.jpgGanymede (HR)54 visiteCaption NASA originale:"This picture of Ganymede was taken from a range of about 272.000 Km. The center of the picture lies at 13° Latitude and 359° Longitude. Many bright impact craters are shown that have radial ejecta patterns. These rays lie across and therefore are younger than the bright and dark background material. Many older impact craters are shown that have lost their rays probably by impact erosion. The bright background areas contain grooves and ridges that may be caused by faulting of the surface materials".
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501-vg1_1641854.jpgGanymede (HR)54 visitenessun commento
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502-PIA01515.jpgGanymede (natural colors and HR)62 visiteCaption NASA originale:"This color picture was acquired by Voyager 1 during its approach to Ganymede. At ranges between about 230 to 250.000 Km. The images show detail on the surface with a resolution of 4,5 Km/px. This picture is relevant to a region in the Northern Hemisphere, near the terminator. It shows a variety of impact structures, including both razed and unrazed craters, and the odd, groove-like structures discovered by Voyager in the lighter regions. The most striking features are the bright ray craters which have a distinctly 'bluer' color appearing white against the redder background. Ganymede's surface is known to contain large amounts of surface ice and it appears that these relatively young craters have spread bright fresh ice materials over the surface. Likewise, the lighter color and reflectivity of the grooved areas suggests that here, too, there is cleaner ice".
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504-PIA01516.jpgGanymede (natural colors and HR)54 visiteCaption NASA originale:"This color picture as acquired by Voyager 1 during its approach to Ganymede, at ranges between about 230 to 250.000 Km. The image shows detail on the surface with a resolution of 4,5 Km/px.
This picture shows the two distinctive types of terrain found by Voyager: the darker ungrooved regions and the lighter areas which show the grooves or fractures in abundance. The most striking features are the bright ray craters which have a distinctly "bluer" color appearing white against the redder background. Ganymede's surface is known to contain large amounts of surface ice and it appears that these relatively young craters have spread bright fresh ice materials over the surface. Likewise, the lighter color and reflectivity of the grooved areas suggests that here too, there is cleaner ice. We see ray craters with all sizes of ray patterns, ranging from extensive systems of the crater in the northern part of this picture, which has rays at least 300-500 kilometers long, down to craters which have only faint remnants of bright ejecta patterns".
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