| Piú votate - Mars Reconnaissance Orbiter (MRO) |
PSP_002884_1395_RED_abrowse-01.jpgUnnamed Southern Crater with deep Gullies (EDM - Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)83 visitenessun commentoMareKromium
(2 voti)
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ESP_019669_2450_RED_abrowse.jpgMega-Polygons in Vastitas Borealis (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)78 visitenessun commentoMareKromium
(2 voti)
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ESP_019589_2340_RED_abrowse-GB-PCF-LXTT-0.jpgNorhern Plains (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team:)121 visitenessun commentoMareKromium
(2 voti)
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ESP_019565_2355_RED_abrowse-PCF-LXTT.jpgNorthern Plains (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team:)107 visitenessun commentoMareKromium
(2 voti)
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ESP_019533_2310_RED_abrowse.jpgNorhern Plains (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team:)87 visitenessun commentoMareKromium
(2 voti)
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ESP_019521_1750_RED_abrowse-PCF-LXTT.jpgCandor Chasma (Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)81 visitenessun commentoMareKromium
(2 voti)
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ESP_019526_2220_RED_abrowse.jpgNorhern Plains, S/W of Galaxias Colles (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team:)71 visitenessun commentoMareKromium
(2 voti)
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PSP_003162_1445_RED_abrowse-00-PCF-LXTT.jpgUnnamed Southern Crater with deep Gullies and Fill (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)85 visitenessun commentoMareKromium
(2 voti)
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PSP_004423_1755_RED_abrowse-PCF-LXTT.jpgInverted Channels and Layers near Juventae Chasma (an Image-Mosaic in Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team:)98 visitePSP_004423_1755 shows Plains North of the South-Western Juventae Chasma, a Canyon belonging to the gigantic Valles Marineris Canyon System.
There are 3 distinct type of Terrains in this image:
1) Plains with possible Inverted Channels,
2) Plains with exposed Layers and
3) Layers on a wall of Juventae Chasma.
The right half of the image contains Plains with Craters and Sinuous Ridge Features that are possibly Inverted Stream Channels.
Inverted relief occurs when a formerly low-lying area becomes high-standing. There are several possible reasons why Channels might stand out in inverted relief. The streambed material may become cemented by precipating minerals, contain larger rocks, or become filled with lava, all which are more resistant to erosion.
Finer-grained, more erodable material surrounding the channel is blown away by the wind or carried away by water, leaving the resistant channel bed high and dry around its environs.
Another example of erosion can be seen in the next Terrain which covers about 2/3 of the left half of the image. Erosion has exposed a beautiful series of light and dark tone Layers (approximately 1 Km across). In the inset, the smallest of the rings is the deepest exposed Layer.
Layers are common in the Martian Canyons, but it is unknown what process formed them. It is likely, though, that the Layers in the Plains here are made of the same material as the Layers in the Canyons. MareKromium
(2 voti)
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PSP_004006_1900_RED_abrowse-PCF-LXTT.jpgFissure in Cerberus Fossae (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)90 visitenessun commentoMareKromium
(2 voti)
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PSP_002824_1355_RED_abrowse-01.jpgDunefield inside Rabe Crater (EDM - Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)77 visiteMareKromium
(2 voti)
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ESP_019482_2135_RED_abrowse-03.jpgEverything fades... (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga - Lunexit Team)94 visiteThis young impact site was discovered by the MRO CTX Science Team. A new "Dark Spot" appeared in a CTX image from July 2008 that was not seen when the region was previously imaged by the Mars Odyssey THEMIS VIS instrument in November 2004. High resolution imaging by HiRISE in November 2008 (left panel of the inset) confirmed that the Dark Spot was Ejecta from a Cluster of Craters.
Three large craters ranging from about 3 to 5 meters diameter and at least 5 smaller craters make up the Cluster. A smaller outlier (approximately 2 meters in diameter, not pictured in the inset) landed 300 meters away to the North/West. These craters were likely produced by a single Impactor that broke into pieces as it fell through the Martian Atmosphere.
The Impactor probably approached from the North/West, judging from the shape of the Ejecta Pattern and the location of the small outlier.
The impacts sprayed the site with Dark Ejecta excavated from beneath the bright Surface. The conspicuous, newly formed feature, will now provide an ideal location to monitor the effects of Winds on the (relatively) modern Martian Surface.
HiRISE imaged the site again in September 2010, after the passage of a full Martian year, when the illumination was similar to the previous HiRISE image. By luck, the SIA (Solar Incidence Angle, such as the Zenith Angle of the Sun) of the later image was only 0,2° different from that of the earlier image.
However, the Phase Angle (such as the angle between the Sun, the Target, and the Spacecraft Camera) was smaller by about 14° as the Spacecraft rolled in the opposite direction.
The new picture shows the Ejecta Pattern apparently faded in comparison to the previous image. The contrast of other features in the scene (such as the Hills and Boulders) is similar, but the Ejecta from the Crater Cluster are noticeably brighter in the HiRISE image from 2010. One possibility is that the Dark Ejecta reflects Sunlight differently than the bright surrounding Terrain - becoming darker more rapidly as Phase Angle increases.
Another possibility is that the Ejecta Pattern was mantled by a thin Layer of bright Dust that settled out of the Atmosphere during the 20 month interval between the two images.
Further monitoring of this site by HiRISE will help choose between these hypotheses.
This target illustrates how the various instruments on MRO work together. The spatial coverage of HiRISE is too limited to search for new impact craters across the Martian globe. Yet the spatial resolution of HiRISE can be used to verify and study details in sites identified as suspicious by CTX.
The complimentary capabilities of the MRO instruments provide a fuller understanding of Mars together than their insights taken separately.MareKromium
(2 voti)
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