| Piú viste - Mars through Mars Express (ESA - Original Raw Frames & Orbital Panoramas) |
Craters-Lauth_Crater_in_Vastitas_Borealis_Region-Frozen_Lake-W-212-010705-1343-6-3d-01-01.jpgThe misterious "Frozen Lake" of Vastitas Borealis (2 - False Colors; credits for the additional process. and color.: Lunar Explorer Italia)57 visiteNoi non sappiamo se i riflessi color verde ed azzurro che cogliamo nelle immagini telescopiche di Marte (sia ottenute da Terra, sia dallo Spazio - via HST ad esempio) sìano il prodotto di mere aberrazioni cromatiche o se essi possano effettivamente costituire l'evidenza tangibile, rispettivamente, di forme di vegetazione indigena e/o di acque correnti superficiali.
Quello che sappiamo è che non possiamo - semplicemente - ignorare questi dati in sede di interpretazione "cromatica" delle immagini possedute, qualunque ne sia la fonte.
Questa "visione" (di fantasia, ma sino ad un certo punto...) del Lago Ghiacciato di Vastitas si riferisce alla tarda Primavera Polare Marziana.MareKromium
|
|
B-h0032_0000_ir3-00.jpgFrame Mars Express RAW n. h0032_0000_ir357 visite
|
|
Volcanoes-Olympus_Mons-PCF-LXTT.jpgOlympus Mons and Surroundings (Absolute Natural Colors; credits for the additional process. and color: Dr Paolo C. Fienga - Lunexit Team)57 visiteUna nostra elaborazione Multispettrale del maestoso Vulcano Olympus, ottenuta da un frame HR proveniente dalla Sonda ESA "Mars Express".
Caption ESA:"This is a mosaic of Olympus Mons, the highest volcano on Mars, which towers 26 Km above the surrounding plains. The image covers an area of approx. 600.000 sq/km.
The High Resolution Stereo Camera (HRSC) on board ESA’s Mars Express Orbiter imaged the Region over 18 orbits.
This image is an ortho-image mosaic, where the projecting rays are perpendicular to the plane of projection.
This corrects any deformations introduced by an imaging camera and therefore such an image can be fitted directly on to a map.
From the observations, 16 HRSC orbit strips, with around 35 Gigabytes of data were used to generate a Digital Terrain Model (DTM) mosaic and an ortho-image mosaic. The DTM mosaic has a resolution of 150 mt/pixel. The resolution of individual nadir images (taken by pointing the camera vertically down to the surface) is in the range of 12 to 40 mt/pixel. Individual terrain models with a resolution of up to 50 mt were derived for every HRSC image strip.
The HR DTMs and ortho-images are derived through a complex process. Matching surface features were used to 'stitch' the images strips together, and complex geometrical calculations were used to produce the 3D coordinates of all measured points in the area".MareKromium
|
|
Craters-Unnamed_Double_Crater_in_Terra_Tyrrhena.jpgDouble Impact Crater in Terra Tyrrhena (Natural Colors + MULTISPECTRUM; credits: ESA & Lunexit)57 visiteThe High Resolution Stereo Camera (HRSC), ESA’s Mars Express obtained images of the Tyrrhena Terra Impact Region on Mars.
On 10 May 2007, the spacecraft was in orbit number 4294 when it snapped pictures of the Region located at 18° South Lat. and 99° East Long. with a ground resolution of approximately 15 metres per pixel.
The Western part of the scene is dominated by a 35 Km-wide and approx. 1000 mt-deep impact crater with an extremely cliffy and chiseled edge. Another, 18 Km-long and approx. 750 mt-deep impact crater, in all likelihood a ‘double impact crater’, is located South of the large crater.
These 'double impact craters' develop when two objects, part of a binary, hit the surface almost simultaneously.MareKromium
|
|
Craters-Terby_Crater.jpgTerby Crater (Natural Colors + MULTISPECTRUM; credits: ESA & Lunexit)57 visiteThe High Resolution Stereo Camera (HRSC) on board ESA’s Mars Express Orbiter imaged the Terby Crater on Mars on 13 April 2007 during orbit 4199.
The Region is of great scientific interest as sediments there hold information on the role of water in the history of the Planet. Eye-catching finger-shaped plateaux extend in the North-South direction. They rise up to 2000 mt above the surrounding terrain. The relatively old crater was filled with sediments in the past, which formed plateaux on erosion.
The flanks of the plateaux clearly exhibit layering of different-coloured material. Differences in colour usually indicate changes in the composition of the material and such layering is called ‘bedding’. Bedding structures are typical of sedimentary rock, which has been deposited either by wind or water. Different rock layers erode differently, forming terraces.
The valleys exhibit gullies, or channels cut in the ground by running liquid, mainly in the Northern part of the image.
These gullies and the rock-bedding structure indicate that the region has been affected by water.
MareKromium
|
|
Volcanoes-Arsia_Mons-Eruption-03.gifArsia Mons is erupting? (a GIF-Movie by: Dr Marco Faccin - Lunexit Team)57 visitenessun commentoMareKromium
|
|
Craters-Lauth_Crater_in_Vastitas_Borealis_Region-Frozen_Lake-W-212-010705-1343-6-3d-01-03.jpgThe misterious "Frozen Lake" of Vastitas Borealis (4 - Extremely Enhanced Natural Colors; credits for the additional process. and color.: Lunar Explorer Italia)56 visitePiena Estate Polare Marziana: polveri rosse ricoprono il cratere senza nome di Vastitas Borealis e colorano, in parte, il suo "laghetto" centrale.
Da notare che, in accordo alle nostre assunzioni di partenza (ed in accordo a regole elementari di logica e di buon senso), un cielo ricco di polveri color arancio, gialle e rossastre (e dunque, di conseguenza, un cielo color rosso/arancio e giallo - di base) si dovrebbe adeguatamente riflettere con questi medesimi colori nelle acque - a questo punto ghiacciate o meno diventa indifferente - del lago di Vastitas.
Ebbene, la regola elementare per cui le acque e/o i ghiacci superficiali, "usualmente", riflettono il colore del cielo, nel frame ESA Originale (fateci caso!) diremmo che NON trova applicazione.
Come mai? Forse abbiamo sbagliato noi...O forse l'immagine ESA è un'mmagine bella ma fasulla? O forse i suoi colori sono stati taroccati (male)?
O magari essa è frutto di incompetenza?
Oppure - chissà... - l'immagine ESA di partenza è un mix di tutte e tre le possibili (e summenzionate) variabili... Decidetelo Voi.MareKromium
|
|
Craters-Lauth_Crater_in_Vastitas_Borealis_Region-Frozen_Lake-W-212-010705-1343-6-3d-01-00.jpgThe misterious "Frozen Lake" of Vastitas Borealis (1 - Natural Colors; credits ESA)56 visiteCaption ESA:"The HRSC on ESA's Mars Express obtained this perspective view on 2 February 2005 during orbit 1343 with a ground resolution of approximately 15 mt per pixel. It shows an unnamed impact crater located on Vastitas Borealis, a broad plain that covers much of Mars's far Northern Latitudes, at approx. 70,5° North Lat. and 103° East Long.
The crater is about 35 Km wide and has a maximum depth of approx. 2 Km beneath the crater rim. The circular patch of bright material located at the centre of the crater is residual water ice.
The colours are very close to natural, but the vertical relief is exaggerated three times. The view is looking East".
Nota: noi crediamo che questo cratere sia molto più enigmatico di quanto non appaia poichè, pur avendo esaminato tutti i frames NASA-MGS relativi alla Regione di Vastitas Borealis (in particolare quelli rapprsentativi dell'area suggerita dalle coordinate ESA), non ci è riuscito di individuare il "laghetto ghiacciato".
Il cratere senza nome che lo dovrebbe contenere, poi, appare solo una volta - e solo in una veduta PARZIALE! - in un frame NASA-Mars Odyssey che Vi proporremo qui di seguito.
Infine, i "colori naturali" di Vastitas Borealis, in accordo ai dati NASA disponibili (i quali sono anche comprensivi di informazioni ottenute sia attraverso vedute telescopiche HST, sia attraverso osservazioni effettuate da Terra), dovrebbero essere molto diversi da quelli suggeriti dall'ESA (noi Vi proporremo tre elaborazioni al riguardo).
|
|
NP-S-h0241_0009_nd3-00.jpgFrame Mars Express RAW n. h0241_0009_nd356 visiteMareKromium
|
|
Hebes_Chasma.jpgHebes Chasma (Natural Colors + MULTISPECTRUM; credits: ESA and Lunexit)56 visiteThe Region is an "Enclosed Trough" situated in Valles Marineris, the Grand Canyon of Mars, where water is believed to have flowed. The High Resolution Stereo Camera (HRSC) on ESA’s Mars Express studied the area providing new pictorial clues to its history.
Hebes Chasma is located at approx. 1° South Lat. and 282° East Long. Image data was obtained on 16 September 2005 with a ground resolution of approx. 15 mt/pixel.
The Region is an enclosed, almost 8 Km-deep trough in the most northern part of Valles Marineris, the 3000-Km long “Grand Canyon of Mars”.
The steep flanks of the trough show branched incisions and small veins of rock. Below the flanks, run-off and material from larger landslides is also visible.
A flat-topped mountain is located in the centre of Hebes Chasma.
It reaches 8000 mt above the graben floor and rises to almost the same height as the plains surrounding the trough. MareKromium
|
|
Chasmas-Candor_Chasma.jpgCandor Chasma (Natural Colors; credits: Lunexit)56 visitenessun commentoMareKromium
|
|
Phobos-400-455-20091201.jpgBig Brother and Little Brother56 visitePhobos and Deimos RAW (left panel) and processed images (right panel).
In a first, ESA’s Mars Express Orbiter imaged the Martian Moons Phobos and Deimos together on November, 5th, 2009.
Apart from their ‘wow’ factor, these unique images will help the HRSC team validate and refine existing orbit models of the two moons.
The images were acquired with the Super Resolution Channel (SRC) of the High Resolution Stereo Camera (HRSC). The camera took 130 images of the moons on November 5th at 09:14 CET in a span of 1,5 minutes at intervals of 1", speeding up to 0,5" intervals toward the end. The image resolution is 110 m/pixel for Phobos and 240 m/pixel for Deimos — Deimos was more than twice as far from the camera.
The Super Resolution Channel of the HRSC uses an additional lens, which has a very narrow field of view of just 0,5°, providing four times the magnification than otherwise providing four times the resolution of the HRSC colour stereo channel.
Phobos, the larger of the two moons, orbits closer to the Red Planet, circling it every 7 hours and 39 minutes. It travels faster relative to Mars than the Moon relative to Earth.
Phobos was about 11.800 Km from Mars Express when the images were taken. Deimos, instead, was about 26.200 Km away.MareKromium
|
|
| 106 immagini su 9 pagina(e) |
 |
|
|
|
|
7 | |
|
