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| Piú votate - Mars Reconnaissance Orbiter (MRO) |
S-PIA08813_modest.jpgVictoria Crater, from MRO71 visitenessun commento
(4 voti)
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R-PIA08788-2.jpgOlympia Undae (2)59 visiteThis image shows three representations of the 72 colors. The left panel is a nearly true-color composite in which the blue, green, and red planes are 0.44, 0.53, and 0.60 micrometer light -- nearly as the human eye would see. The contrast between the bright ice and dark dunes is so large that the dunes are barely seen. The middle panel is false color constructed from infrared wavelengths just beyond the range of the human eye. The blue, green, and red planes cover 0.80, 0.95, and 1.06 micrometer light. In this rendering of the data the differences between ice- and soil-rich regions are not as apparent because the colors of ice and dust are similar in this wavelength region. The right panel uses 1.15, 1.8, and 2.25 micrometer light in the blue, green and red planes and provides a dramatically different view of the scene. The areas of highest ice content appear in blue, and those with a mix of dust and ice -- most of the scene -- appear yellowish. The dunes are now visible against the ice because of their higher brightness at longer infrared wavelengths, and appear ruddy brown.
(4 voti)
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R-PIA08788-1.jpgOlympia Undae (1)55 visiteThe Compact Reconnaissance Imaging Spectrometer for Mars, a mineral mapping instrument on NASA's Mars Reconnaissance Orbiter (CRISM), began observing Mars after its lens cover was opened on Sept. 27, 2006.
This image shows one of the first regions of Mars measured after CRISM's cover was opened.
CRISM takes images in two basic formats. The first format is a "targeted image" about 10 by 10 Km (about 6 by 6 miles), at about 18 mt (60 feet) per pixel, in 544 colors covering wavelengths of 0,36 to 3,92 micrometers. The second format is a lower-resolution strip 10 Km (about 6 miles) wide and thousands of kilometers long, at 200 mt (660 feet) per pixel, in 72 colors. Many thousands of these "multispectral survey" strips are used to build a global map.
The image is part of the second multispectral survey strip, taken at 22:36 UTC (6:36 p.m. EDT) on Sept. 27, 2006. Only minimal processing of the data has been done at this early point in the MRO's Mission.
The strip crosses part of the north polar region named Olympia Undae, and stretches between 76.7 north latitude, 141.9 east longitude and 85.5 north, 115.8 east. From the top, the northern end of the image crosses layers of dusty and clean ice in the north polar cap. Moving south the image covers dusty sedimentary deposits, dark sand dunes, and outlying polar ice deposits.
(4 voti)
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Q-V-Argyre Basin-PIA08067.jpgArgyre Basin59 visiteThis picture (MARCI2-2b) shows a color composite made from the MARCI red, green, and blue bands.
It differs from the MOC wide angle color composite because, to create a color image with MOC data, we synthesize (fake) a green channel by adding the red and blue channels together and dividing by two. The slightly greenish tint of the MARCI image shows that the approximation used for MOC images underestimates the amount of green. Further calibration will be needed before a "true" color image — as it would appear to a human eye looking down from orbit — can be reconstructed from the MARCI data.
(4 voti)
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Q-U-Bosporus Planum (IR-VIS)-02.jpgBosporus Planum - detail mgnf (2)58 visiteCaption originale NASA, riferita al full-frame:"Large-scale streaks in the northern half are due to the action of wind on surface materials. The blankets of material ejected from the many small fresh craters are generally brighter and redder than the surrounding surface, but a few are darker and less red. Two greenish spots in the middle right of the scene may have an unusual composition, and are good future targets for the Compact Reconnaissance Imaging Spectrometer for Mars, a mineral-identifying instrument on MRO (http://crism.jhuapl.edu/). In the bottom half of the image we see a redder color in the rough areas, where wind and sublimation of water or carbon dioxide ice have partially eroded patches of smooth-textured deposits".
(4 voti)
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Q-S-BosporusRupes-PIA08047_modest.jpgBosporos Rupes59 visiteThis image was taken in the mid-latitudes of Mars' Southern Hemisphere near the giant Argyre Impact Basin. It is located just to the West of a prominent scarp known as Bosporos Rupes. The left side of the image shows cratered plains. Some of the craters are heavily mantled and indistinct, whereas others exhibit sharp rims and dramatic topography. The largest crater in this half of the image is about 2,5 Km wide. Mounds and ridges, which may be remnants of an ice-rich deposit, are visible on its floor. Three sinuous valleys occupy the center of the image. Valleys such as these were first observed in data returned by the NASA Mariner 9 spacecraft, which reached Mars in 1971. The right side of the image shows part of an impact crater that is approx. 20 Km in diameter. The furrowed appearance of the crater's inner wall suggests that it has been extensively modified, perhaps by landslides and flowing water. Like other craters in the area, the floor of this crater has a rough and dissected texture that is often attributed to the loss of ice-rich material.
This image was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard NASA's Mars Reconnaissance Orbiter spacecraft on March 24, 2006. The image is centered at 40,64° South Latitude, 303,49° East Longitude. The image is oriented such that North is 7° to the left of up. The range to the target was 2.044 Km (about 1.270 miles). At this distance the image scale is 2,04 mt (6,69 feet) per pixel, so objects as small as 6,1 mt (20 feet) are resolved. In total this image is 40,90 Km (about 25,41 miles) or 20.081 pixels wide and 11,22 Km (such as 6,97 miles) or 5.523 pixels high. The image was taken at a Local Mars Time of 07:30 and the scene is illuminated from the upper right with a solar incidence angle of 81,4° (this meaning that the Sun was about 8,6° above the horizon).
(4 voti)
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PIA08014_modest.jpgThe "First Frame" from MRO (detail mgnf)85 visiteThe scene covers an area 49,8 Km (about 30,9 mi) wide and 23,6 Km (about 11,7 mi) high, of landscape typical of Mars' mid-latitude Southern Highlands. The location is 34° South Latitude, 305° East Longitude. An old, muted crater lies at the middle of the scene, with sets of channels to the left and right. Superimposed on parts of this terrain is a much younger, layered mantle of debris. The debris mantle is smooth in places but rough in other areas where it may have partially sublimated. This suggests that the debris mantle is (or was) rich in volatiles such as ices of water, CO2 or both. Also superimposed on the landscape are many small sharp-rimmed impact craters and wind-blown dunes. This image illustrates processes that may have involved water both on ancient Mars (channels and eroded craters) and much more recently in Mars' history (volatile-rich debris mantle). The radiometric and geometric processing of this image is very preliminary. In particular there are mismatches visible at full resolution along the seams between the 10 side-by-side images from separate CCDs (charge-coupled devices, which are electronic optical sensors).
(4 voti)
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Remnants-ESP_038184_1815_40-1.jpgUnusually-looking Surface Features on Mars (EDM from ESP 038184-1815-40)181 visitenessun commentoMareKromium
(3 voti)
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Dust_Storm-MGS-41668_PIA22519_original_marci-dgm-v04-for-home-page-5.gifThe Global Dust Storm that wiped Oppy away118 visiteCaption NASA:"This set of images from NASA’s Mars Reconnaissance Orbiter (MRO) shows a fierce, giant Dust Storm is kicking up on Mars, with Rovers on the Surface indicated as icons. The spread of the Storm can be seen in the salmon-colored overlay. These images from MRO's Mars Color Imager start from May 31, when the Dust Event was first detected, and go through June 11, 2018.
MRO creates Global Maps of Mars but roll maneuvers for targeted observations produce gaps in the coverage, which appear as black gores in the aforementioned Maps. On some days there are data drops where partial or full orbits of coverage are missing. Green and purple observed in the South Polar Region indicate saturated pixels. Latitude is indicated along the Vertical Axis. Longitude is indicated along the Horizontal Axis".MareKromium
(3 voti)
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Chasma-Ophir_Chasma-PSP_007535_1755-PCF-LXTT-IPF.jpgFeatures of Ophir Chasma (CTX Frame - Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)65 visiteThe really huge Landslides existing along the Walls of Ophir Chasma (which is nothing else but a deep Canyon located in the Coprates Quadrangle of Mars, at about 4° South Latitude and 72,5° West Longitude. It is approx. 317 km long and it was so named after a "Classical Albedo Feature") host a variety of Geologic Surfaces and Mineralogies.
Some of them possess a variety of Hydrated Sulfate Minerals that formed, eons ago, in the presence of Partially Acidic Liquid Water. This NASA - Mars Reconnaissance Orbiter's Contextual (or "CTX", for short) Image, which is representing an ancient (possibly and approximately 3 Billion Years-old) Landslide, shows us the presence, within it, of 2 (two) very distinct Surface Albedoes, which, in fact, mark a Transition Zone from one Sulfate Mineralogy to another (a circumstance that proves beyod doubts the occurrence, in a far and distant past, of some remarkable variations in the evolution of the visible Surface).
The Upper Slopes (such as the ones located towards the North) are light-toned, and this fact is due to the concurrent abundance of Hydrated Sulfate Minerals and Bright Surface Dust. On the other hand, the Surfaces that make up the Southern Portion of the Landslide, are darker in tone, and this is due to the greater abundance of Dark Sediment that, in time, formed "Strings of Sand Drifts". In addition to the above, the underlying Units of Bedrock consist of Darker Minerals that received a lesser hydration then the Northern ones, and this further circumstance implies the occurrence of a strong (and, perhaps, sudden) change in the Ancient Aqueous Environments that formed them.
Mars Local Time: 14:52 (Early Afternoon)
Coord. (centered): 4,328° South Lat. and 288,657° East Long.
Spacecraft altitude: 271,0 Km (such as about 168,291 miles)
Original image scale range: 27,1 cm/pixel (with 1 x 1 binning) so objects ~ 81 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 6,3°
Phase Angle: 52,7°
Solar Incidence Angle: 47° (meaning that the Sun was about 43° above the Local Horizon at the time the picture was taken)
Solar Longitude: 27,0° (Northern Spring - Southern Fall)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer Italia
This picture (which is a NASA - Original Mars Reconnaissance Orbiter b/w and NON-Map Projected frame identified by the serial n. PSP_007535_1755) has been additionally processed, magnified, contrast enhanced, Gamma corrected, and then colorized in Absolute Natural Colors (such as the colors that a human eye would actually perceive if someone were onboard the NASA - Mars Reconnaissance Orbiter and then looked down, towards the Surface of Mars), by using an original technique created - and, in time, dramatically improved - by the Lunar Explorer Italia Team.MareKromium
(3 voti)
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Chasma-Echus_Chasma-Fractures-ESP_033591_1805-PCF-LXTT-IPF.jpgFeatures of Echus Chasma (CTX Frame - Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)72 visiteIn this image, we can see a so-called "Intersection Area" created by a number of Fractures (or, perhaps, Fissures and/or Water or Lava-carved narrow Channels) which are all located on the Floor of Echus Chasma (an Equatorial Chasma found in the Lunae Planum High Plateau Region of Mars, slightly to the North of the gigantic Valles Marineris Canyon System, and approx. 100 Km long and 10 Km wide).
Echus Chasma contains several Valleys which range - as far as their depth is concerned - from about 1 to 4 Km, and it is now considered, by Planetary Scientists, to be the Water Source Region that allowed the formation and then the (relevant) water-supply of the Kasei Valles Outflow Channel: a large Valley that extends for thousands of kilometers towards the North of the Red Planet.
Mars Local Time: 14:36 (Early Afternoon)
Coord. (centered): 0,377° North Lat. and 279,483° East Long.
Spacecraft altitude: 269,1 Km (such as about 161,111 miles)
Original image scale range: 53,8 cm/pixel (with 2 x 2 binning) so objects ~ 1 mt and 62 cm across are resolved
Map projected scale: 50 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 7,7°
Phase Angle: 47,6°
Solar Incidence Angle: 40° (meaning that the Sun was about 50° above the Local Horizon at the time the picture was taken)
Solar Longitude: 27,0° (Northern Spring - Southern Fall)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer Italia
This picture (which is a NASA - Original Mars Reconnaissance Orbiter b/w and NON-Map Projected frame identified by the serial n. ESP_033591_1805) has been additionally processed, magnified, contrast enhanced, Gamma corrected, and then colorized in Absolute Natural Colors (such as the colors that a human eye would actually perceive if someone were onboard the NASA - Mars Reconnaissance Orbiter and then looked down, towards the Surface of Mars), by using an original technique created - and, in time, dramatically improved - by the Lunar Explorer Italia Team.MareKromium
(3 voti)
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Meridiani_Planum-ESP_032098_1785-PCF-LXTT-IPF.jpgFeatures of Meridiani Planum (Absolute Natural Colors; credits for the additional process. and color.: Dr Paolo C. Fienga/Lunar Explorer Italia/Italian Planetary Foundation)89 visiteIn this frame, taken by the NASA - Mars Reconnaissance Orbiter on the date of June, 1st, 2013, we can see a few interesting (although very common) Surface Features which characterize the Meridiani Planum Region of Mars. In particular, we can see an old and (still) Unnamed Impact Crater - with the "usual" Dunefield on its Floor - that is located on the very upper portion of the frame and just below a (relatively) Sand-free section of Surface known as "Martian Paving". Afterwards, moving down towards the South (such as towards the lower portion of the frame), we can find an area where there are many Sand Ripples and a few small Impact Craters. Finally, on the very lowest portion of the picture, we can also see more Sand Ripples, a number of Sand Dunes, several very small Impact Craters and quite a few Rocky Outcrops.
However, the Martian Surface pictured here, in our opinion (as IPF), and contrary to the common idea of how the Meridiani Planum Region of Mars is - generally - characterized and known (such as an almost totally plain and reliefs-free Region), is really far from being flat at all: as a matter of fact, if you observe the picture carefully, you will be able to notice that the whole area which has been photographed by the NASA - Mars Reconnaissance Orbiter (and, particularly, the area visible in the central and lower portion of the frame - meaning the one located to the South of the main visible Feature, such as the Unnamed Impact Crater) appears to show several points of Subsidence, a few Ridges and some (most likely very short and small) Hillocks.
Mars Local Time: 14:09 (Early Afternoon)
Coord. (centered): 1,584° South Lat. and 3,132° East Long.
Spacecraft altitude: 268,9 Km (such as about 166,986 miles)
Original image scale range: 26,9 cm/pixel (with 1 x 1 binning) so objects ~ 81 cm across are resolved
Map projected scale: 25 cm/pixel
Map projection: EQUIRECTANGULAR
Emission Angle: 0,0°
Phase Angle: 34,0°
Solar Incidence Angle: 34° (meaning that the Sun was about 56° above the Local Horizon at the time the picture was taken)
Solar Longitude: 328,5° (Northern Winter - Southern Summer)
Credits: NASA/JPL/University of Arizona
Additional process. and coloring: Lunar Explorer Italia
This picturee (which is a NASA - Original Mars Reconnaissance Orbiter NON-Map Projected b/w frame identified by the serial n. ESP_032098_1785) has been additionally processed and then colorized in Absolute Natural Colors (such as the colors that a human eye would actually perceive if someone were onboard the NASA - Mars Reconnaissance Orbiter and then looked down, towards the Surface of Mars), by using an original technique created - and, in time, dramatically improved - by the Lunar Explorer Italia Team.MareKromium
(3 voti)
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