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M-067-0.jpgM 67 - Semi-Globular Star Cluster58 visite"...God saw everything that He had made, and indeed, it was very good..."
- Genesis, 1:31MareKromium
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APOLLO_15_AS_15-96-13064.JPGAS 15-96-13064 - EVA Floodlight near Herodotus "H" and Vallis Schroteri (2)58 visiteImage Collection: 70mm Hasselblad
Mission: 15
Magazine: 96
Magazine Letter: Q
Latitude: 26° North
Longitude: 51° West
Description: EVA FLOODLIGHT
Film Type: SO-368
Film Width: 70 mm
Film Color: colorMareKromium
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PSP_004324_1060_RED_browse.jpgPolygons on South Polar Layered Deposits58 visiteThis image shows an exposure of south polar layered deposits, thought to record recent global climate changes on Mars.
The layers were probably laid down over the past few million years over a large area near the south pole, then eroded to show the layering visible in this image.
The layers appear brighter where their slopes are steeper and facing the Sun.
Within the brighter, steeper part of the layered deposits, a network of polygonal fractures is visible. The polygons outlined by the fractures are typically a few hundred meters (approx. 1000 feet) across, and traverse layer boundaries. Such polygonal fractures are seen on Earth in places where ground ice is present, and previous Mars orbiters have found evidence for abundant ground ice in the south polar region of Mars. So it is not surprising to see polygonal fractures here; what is unusual is that they cross layer boundaries, apparently unaffected by the changes in slope across them.
This suggests that the polygonal fractures formed after the scarp exposing the south polar layered deposits was formed by erosion. This indicates, possibly, that the scarp has been stable for some time, allowing the polygonal fractures to form.
MareKromium
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PSP_003252_1425_RED_browse-01.jpgBright Gully Deposit in Terra Sirenum (the "crater" - close-up; false colors)58 visiteAs seen in the context image and here, the appearance of the crater wall differs between the Northern and Southern Sides. On the Northern Pole-Facing Side Walls, prominent gullies with channels and aprons are apparent, with many of these having valley-like alcoves near their tops. The morphology of the gullies is consistent with formation by a fluid, most likely water.
On the pole-facing slopes, ground ice or aquifers may be more stable, being subjected to less heating from sunlight compared to equator-facing slopes.
In contrast, the Southern, Equator-Facing Walls are dominated by rocky debris flows that lack prominent channels.MareKromium
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ZZ-ZZ-RoverTracks-R9.jpgRover Tracks (natural colors - elab. Lunexit)58 visitenessun commentoMareKromium
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ZZ-ZZ-TheDunes-K15.jpgDunes (natural colors - elab. Lunexit)58 visitenessun commentoMareKromium
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as16-116-18648.jpgAS 16-116-18648 - The "MoonCam" and some bags (additional processing by Lunexit)58 visiteCaption NASA:"Similar to 18647, showing detail of Charlie's camera".MareKromium
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as16-107-17573.jpgAS 16-107-17573 - Unusual boulder at Station 9 (additional processing by Lunexit)58 visiteCaption NASA:"148:14:17 MT - Cross-Sun "after" of the tipped boulder at Station 9".
MareKromium
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as16-118-18977.jpgAS 16-118-18977 - Mendeleev Crater (additional processing by Lunexit)58 visiteImage Collection: 70mm Hasselblad
Mission: 16
Magazine: 118
Magazine Letter: NN
Latitude: 7,7° North
Longitude: 140,2° East
Camera Altitude: 122 Km
Film Type: SO-368
Film Width: 70 mm
Film Color: colorMareKromium
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![ZZ-ZZ-Horizon-2P161783721EFFA500P2664L4M1[1].jpg](albums/userpics/10060/small_ZZ-ZZ-Horizon-2P161783721EFFA500P2664L4M1%5B1%5D.jpg "Nome del file=ZZ-ZZ-Horizon-2P161783721EFFA500P2664L4M1[1].jpg
Dimensione del file=155KiB
Dimensioni=1600x1600
Aggiunta il=Ago 26, 2007")
ZZ-ZZ-Horizon-2P161783721EFFA500P2664L4M1[1].jpgMartian Day with high A.O. over Gusev (3) - (natural colors; Keith Laney and additional processing by Lunexit)58 visitenessun commentoMareKromium
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ZZ-ZZ-Horizon-2P1271708-072648color.jpgMartian Day with high A.O. over Gusev (1) - (natural colors; Keith Laney and additional processing by Lunexit)58 visitenessun commentoMareKromium
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NGC-1333-PIA09966.jpgWater Vapor inside NGC 133358 visiteThis diagram illustrates the earliest journeys of water in a young, forming Star System. Stars are born out of icy cocoons of gas and dust. As the cocoon collapses under its own weight in an inside-out fashion, a stellar embryo forms at the center surrounded by a dense, dusty disk.
The stellar embryo "feeds" from the disk for a few million years, while material in the disk begins to clump together to form planets.
NASA's Spitzer Space Telescope was able to probe a crucial phase of this stellar evolution - a time when the cocoon is vigorously falling onto the pre-planetary disk. The infrared telescope detected water vapor as it smacks down on a disk circling a forming star called NGC 1333-IRAS 4B.
This vapor started out as ice in the outer envelope, but vaporized upon its arrival at the disk.
By analyzing the water in the system, astronomers were also able learn about other characteristics of the disk, such as its size, density and temperature.
How did Spitzer see the water vapor deep in the NGC 1333-IRAS 4B system?
This is most likely because the system is oriented in just the right way, such that its thicker disk is seen face-on from our Earthly perspective. In this "face-on" orientation, Spitzer can peer through a window carved by an outflow of material from the embryonic star. This system in this drawing is shown in the opposite "edge-on" configuration.MareKromium
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