| Piú viste - Mars, Deimos and Phobos: Maps |
005-Surface_Ages.jpgMars Global Map: Age of Main Surface Features99 visitenessun commento
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012-Thermal_Inertia.jpgMars Global Map: Thermal Inertia99 visitenessun commento
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009-Mars_North_East.jpgThe North-Eastern Region of Mars99 visitenessun commento
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023-Mars_Water-3.jpgMap of Water on Mars96 visiteI raggi cosmici, dopo aver aver raggiunto il Pianeta, interagiscono rapidamente con gli elementi presenti negli strati superficiali del suolo Marziano. Da questo impatto e dalle conseguenti reazioni, scaturisce una (+ o - elevata) dispersione di neutroni. Sapendo che, per quanto maggiore è il quantitativo di H presente in detti strati, tanto minore è la dispersione di neutroni, misurando il loro > o < assorbimento, misuriamo anche il > o < quantitativo di H presente in essi.Sapendo che la forma più probabile in cui si può trovare H in prossimità della superficie di Marte è quella che lo vede aggregato all’O2, deduciamo che, laddove viene rilevata una maggiore presenza di H è altrettanto probabile che vi sia anche una maggiore presenza di H2O.
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034-Methane_of_Mars.jpgMap of the "Martian Methane"74 visiteCaption NASA:"Why is there Methane on Mars? No one is sure.
An important confirmation that Methane exists in the Atmosphere of Mars occurred last week, bolstering previous controversial claims made as early as 2003. The confirmation was made spectroscopically using large ground-based telescopes by finding precise colors absorbed on Mars that match those absorbed by Methane on Earth.
Given that Methane is destroyed in the open martian air in a matter of years, the present existence of the fragile gas indicates that it is currently being released, somehow, from the Surface of Mars.
One prospect is that microbes living underground are creating it, or created in the past. If true, this opens the exciting possibility that life might be present under the Surface of Mars even today. Given the present data, however, it is also possible that a purely geologic process, potentially involving volcanism or rust and not involving any life forms, is the Methane creator.
Pictured above is an image of Mars superposed with a map of the recent Methane detection".
Nota Lunexit: se la Mappa NASA è realmente accurata ed il quantitativo di Metano presente in Atmosfera è quello "suggerito" dalla Mappa stessa, allora - sempre seguendo la "Logica NASA" - ci troveremmo davanti a due possibili scenari:
1) Scenario Geologico (Metano come prodotto di processi geologici): Marte è ancora soggetto attivo di fenomeni vulcanici tutt'altro che minori e residuali, visti i quantitativi e la distribuzione del Metano nell'Atmosfera del Pianeta Rosso, oppure
2) Scenario Biologico (Metano come sottoprodotto di attività biologiche attuali): Marte è, letteralmente, "brulicante di Vita" - altro che batteri e micro-organismi - visti, come sopra, i quantitativi e la distribuzione del Metano nell'Atmosfera del Pianeta Rosso.
SOTTOLINEIAMO che queste nostre congetture DERIVANO LOGICAMENTE DALL'ANALISI DEI DATI NASA e NON da nostre speculazioni!
Vi suggeriamo, inoltre, di notare la posizione dei maggiori quantitativi di Metano nell'Atmosfera Marziana...MareKromium
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028-Mars_Colors-MF-LXTT2.jpgFull Map of Mars (Approximate Natural Colors; credits: Dr Marco Faccin - Lunexit Team)71 visite...E anche questa è ARTE...MareKromium
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030-Mars-17-PIA09225_fig1.jpgThe "Lower Boundary" of the Icy Layers Covering Mars' South Polar Region (Map 2)62 visiteThis map shows the topography of the South Polar Region of Mars, including topography buried by thick deposits of icy material. The map is a combination of surface elevation data acquired by the Mars Orbiter Laser Altimeter aboard NASA's Mars Global Surveyor orbiter, and subsurface elevation data acquired by the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) aboard the European Space Agency's Mars Express orbiter.
The black line shows the boundary of the South Polar Layered Deposits, an ice-rich geologic unit that was probed by MARSIS. Elevation values within the black outline, as measured by MARSIS, show the topography at the boundary between the layered deposits and the underlying material, an interface known as the "bed" of the deposits. The elevation of the terrain is shown by colors, with purple and blue representing the lowest areas, and orange and red the highest. The total range of elevation shown is about 5 Km.
The radar data reveal previously undetected features of topography of the bed, including depressions as deep as 1 Km (0,6 miles) shown in purple in the near-polar region.
The boundary of the layered deposits was mapped by scientists from the U.S. Geological Survey. The dark circle in the upper center is the area poleward of 87° South Latitude, where MARSIS data cannot be collected.
The map covers an area of 1670 by 1800 Km (about 1035 by 1115 miles).
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016-Mars_Altitudes.jpgMars "Ups and Downs"...57 visiteTo complement the MOLA Laser Altimeter Mercator maps of Mars' elevations and topography, the MOLA Team also produced views of selected hemispheres.
These views emphasize specific interesting areas or angles. These maps show altitude data coded into colors - blue is low and red/white are high.
These two hemispheres are centered on the Tharsis Plateau (including the Valles Marineris and the large volcanos) and on the Isidis Impact Basin (with the Hellas Basin to the South).MareKromium
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026-Mars_Advanced_Map.jpgAdvanced Mars Global Map57 visitePublisher: Aeronautical Chart and Information Center
Scale: 1:35.000.000
Projection: Mercator MareKromium
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024-Iani_Chaos_and_Ares_Valles.jpgMargaritifer Terra56 visiteCaption ESA originale:"This map shows that the Iani Chaos depression – 180 Km long and 200 Km wide – is connected to the beginning of Ares Vallis by a 100-Km wide Transition Zone, centred around 342,5º East and 3º North".
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025-Mars_Global_with_Nomenclature.jpgMars Map for Beginners56 visiteUna Mappa semplice ed immediata non guasta mai...MareKromium
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Phobos_Map.jpgPhobos (credits: NASA - USGS)56 visitenessun commentoMareKromium
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