| Piú viste - Titan: The "Foggy" Moon |
Titan-Surface-34-PIA06440.jpgOn the Surface... (Natural Colors; credits: Lunar Explorer Italia)58 visitenessun commentoMareKromium
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Titan-W00002390.jpgFrom the Dark Side... (Natural - but enhanced - Colors; credits: Lunar Explorer Italia)58 visitenessun commentoMareKromium
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Titan-PIA11522.jpgSenkyo (Natural Colors; credits: Lunar Explorer Italia)58 visiteCaption NASA:"The Cassini Spacecraft examines the dark region of Senkyo on Saturn's largest moon, Titan. Senkyo is in the center of the image, and it lies just south of the moon's equator. For an earlier view of this Region, see PIA08231.
Lit terrain seen here is on the Saturn-facing side of Titan. North on Titan is up and rotated 6° to the left.
The image was taken with the Cassini Spacecraft narrow-angle camera on March 21, 2009 using a spectral filter sensitive to wavelengths of near-InfraRed Light centered at 938 nanometers.
The view was obtained at a distance of approx. 994.000 Km (about 618.000 miles) from Titan and at a Sun-Titan-Spacecraft, or Phase, Angle of 63°.
Image scale is roughly 6 Km (a little less than 4 miles) per pixel".MareKromium
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Titan-Volcanic_Features-PIA12111.jpgSouth Polar Basin58 visiteCaption NASA:"An enigmatic large Basin appears in the South Polar Region of Saturn's moon Titan at the center of this Titan Radar Mapper image from NASA's Cassini Spacecraft acquired on June 22, 2009.
The Basin has several possible origins.
It may be a Volcanic Caldera, produced by collapse after cryovolcanic eruptions.
It might be a Modified Impact Basin, partially infilled with sedimentary material.
Alternately, the basin may have formed by some other collapse process related to the presence of Subsurface Methane.
Evidence for lakes elsewhere on Titan suggests that it might have been later partially filled with liquid Methane and Ethane".
MareKromium
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Titan-Lakes-South_Polar_Unnamed_Lake-PIA12162.jpgLake-like Feature near the South Pole of Titan58 visiteCaption NASA:"This mosaic of image swaths from Cassini's Titan Radar Mapper, taken with the Synthetic-Aperture Radar (SAR), features a large Dark Region several hundred kilometers across that differs in several significant ways from potential lakes observed on Titan.
It is not as dark to the radar as many lakes (including lakes seen here), and the nature of the margin is unusual. It has many characteristics in common with lakes, including its channels and interior, yet its differences distinguish it from other similar features. Some similarities are seen with the dark feature in Titan pass T7 (see PIA03563).
At top (North), the feature has characteristics of a shoreline, with round bay-like margins and channels that drain into it; at left (West) and right (East) it is rimmed by bright, feathery, branching channel-like structures, some of which extend for tens of kilometers. Within the Dark Feature some details can be seen, some of which seem to be extensions of the channels draining into the Dark Feature.
The mosaic is near the South Pole, centered near 82° South and 205° West. It includes data from Titan passes T39, T55, T57, T58, and T59, collected between December 2007 and July 2009. The individual swaths vary in resolution and illumination angle, so the edges are visible and surface features look somewhat different across swath boundaries, but the regional view can still be understood. As more SAR image swaths of Titan are collected by Cassini, mosaics of those images reveal features that cannot be appreciated within the individual observations".MareKromium
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Titan-PIA11594.jpgNorthern Layers (UV + Natural Colors; credits: Lunexit)58 visiteCaption NASA:"This UltraViolet view of Titan shows the moon's North Polar "Hood" (---> cappuccio) and its detached, high-altitude haze layer. See also PIA08137 to learn more.
This view looks toward the Saturn-facing side of Titan.
North on Titan is up and rotated 2° to the left.
The image was taken with the Cassini Spacecraft narrow-angle camera on Aug. 13, 2009 using a spectral filter sensitive to wavelengths of UltraViolet Light centered at 338 nanometers. The view was acquired at a distance of approx. 2,2 MKM (about 1,4 MMs) from Titan and at a Sun-Titan-Spacecraft, or Phase, Angle of 61°.
Image scale is roughly 26 Km (about 16 miles) per pixel".MareKromium
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Titan-PIA11603.jpgSeasonal Changes on Titan (Natural Colors; credits: NASA/JPL/Space Science Institute)58 visiteSeasonal changes in the Atmosphere of Saturn's largest moon are captured in this Natural Color image, which shows Titan with a slightly darker top half and a slightly lighter bottom half.
Titan's Atmosphere has a seasonal hemispheric dichotomy, and this image was taken shortly after Saturn's August 2009 Equinox.
Images taken using red, green and blue spectral filters were combined to create this Natural Color view.
Scientists have found that the Winter Hemisphere typically appears to have more high-altitude haze, making it darker at shorter wavelengths (UltraViolet through blue) and brighter at InfraRed wavelengths.
The switch between dark and bright occurred over the course of a year or two around the last Equinox. Scientists are studying the mechanism responsible for this change, and will monitor the dark-light difference as it flip-flops now that the 2009 Equinox has signaled the coming of Spring and then Summer in the Northern Hemisphere.
Although this hemispheric boundary appears to run directly East-West near the Equator, its position is not level with latitude and is actually offset from the Equator by about 10° of Latitude.
This view looks toward the Saturn-facing side of Titan. North on Titan is up.
The images were obtained with the Cassini Spacecraft wide-angle camera on Aug. 25, 2009 at a distance of approx. 174.000 Km (such as about 108.000 miles) from Titan.
Image scale is roughly 10 Km (a little more than 6 miles) per pixel.MareKromium
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Titan-N00149992-N00150001.jpgTitan, in Time... (Natural Colors; credits: Elisabetta Bonora - Lunexit Team)58 visitenessun commentoMareKromium
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Titan-Regions-Fensal_Aztlan_Aaru_and_Senkyo_Regions-PIA12531.jpgTitanian Geography (Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)58 visiteCaption NASA:"The Cassini Spacecraft gazes at several albedo features on Saturn's largest moon, Titan.
Left to right are four Dark Regions: Fensal, Aztlan, Aaru and a part of Senkyo. The bright area Quivira lies near the center of the image, separating Fensal and Aztlan. This view looks toward the Saturn-facing side of Titan. North on Titan is up and rotated 24° to the right.
The image was taken with the Cassini Spacecraft narrow-angle camera on June 25, 2009 using a spectral filter sensitive to wavelengths of Near-InfraRed Light centered at 938 nanometers. The view was obtained at a distance of approx. 1,3 MKM (about 808.000 miles) from Titan and at a Sun-Titan-Spacecraft, or Phase, Angle of 12°.
Image scale is roughly 8 Km (about 5 miles) per pixel".MareKromium
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Titan-Mountains-PIA12496.jpgNew Wrinkles on Titan (Colorization made on Radar Image - credits: Dr Paolo C. Fienga - Lunexit Team)58 visiteIn this Synthetic Aperture Radar (SAR) image obtained by NASA's Cassini Spacecraft, two generally similar features, upper center and lower right, appear to be low Mountains with Grooves running roughly in the up-down direction.
A set of straight lines are also visible at lower left.
But what made the Grooves?
Grooves can result from forces that originate from within a planet - including forces that pull the Crust of a planet apart and cracks produced by melt intruding into the Crust.
They can also come from external forces like wind or rainfall, which produces river channels that can cut down through layers of rock.
All of these produce grooves on Earth's Surface, and may also be at work on Titan.
Another intriguing thing about this image is that in this image the "light" (actually the radar illumination) comes from the top. With this kind of illumination, the upper side of these mountains should be bright because they face the illumination, but the left side of the upper-center feature and the right side of the lower feature are bright. The brightness indicates that there is a different material in these areas, and the Grooves exist in both dark and light materials.
The Titan Radar Mapper acquired this image at 41° North Latitude and 213° West Longitude on December 28, 2009.
The image measures approx. 250 Km (about 160 miles) high and approx. 285 Km (about 180 miles) wide, with resolution of roughly 350 meters (1100 feet) per pixel. North is on the left, and the image is illuminated from the top.
The S.I.A. varies from 11 to 25°.
Two dark horizontal lines that run across the middle of the image show the joints between individual radar beams and are not features on the Titan Surface.MareKromium
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Titan-IR.jpgIR Titan (credits: Dr M. Faccin - Lunexit Team)58 visitenessun commentoMareKromium
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Titan_and_Dione-EB-LXTT-1.jpgFading in the Background... (Natural Colors; credits: Elisabetta Bonora - Lunexit Team)58 visitenessun commentoMareKromium
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