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Titan-Regions-Dichotomy_Boundary_Region-PIA12586.jpgThe "Dichotomy Boundary" on Titan (N-IR Light - Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)55 visiteCaption NASA:"The Cassini Spacecraft records Titan's Seasonal Hemispheric Dichotomy, with the moon's northern half appearing slightly lighter than the southern half in this image.
This view looks toward the Trailing Hemisphere of Titan. North on Titan is up and rotated 12° to the right.
The image was taken with the Cassini Spacecraft narrow-angle camera on Feb. 16, 2010 using a spectral filter sensitive to wavelengths of Near-InfraRed Light centered at 889 nanometers. The view was obtained at a distance of approx. 1,1 MKM (such as about 684.000 miles) from Titan and at a Sun-Titan-Spacecraft, or Phase, Angle of 28°.
Image scale is roughly 7 Km (about 4,3 miles) per pixel".MareKromium
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Titan-Regions-Fensal_Aztlan_Aaru_and_Senkyo_Regions-PIA12531.jpgTitanian Geography (Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)55 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-Regions-Fensal_Region-PIA07753.jpgThe "New World": Fensal Region and more54 visiteOriginal caption:"Like an ancient mariner charting the coastline of an unexplored wilderness, Cassini's repeated encounters with Titan are turning a mysterious world into a more familiar place.
During a Titan flyby on Sept. 7, 2005, the spacecraft's narrow-angle camera acquired multiple images that were combined to create the mosaic presented here. Provisional names applied to Titan's features are shown.
The image shows more than half of Titan's Saturn-facing hemisphere at moderate resolution, including the Fensal-Aztlan region, formerly known as "the H." This view is centered at 6,5° North Lat. and 20,6° West Long. and has a pixel scale of approx. 2 Km (about 1 mile) per pixel.
It is an orthographic projection, rotated so that North on Titan is up.
This view is composed of 20 images obtained on Sept. 7, 2005, each processed to enhance surface detail".
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Titan-Regions-Fensal_and_Aztlan_Region-PIA07634.jpgFensal-Aztlan Region54 visiteOriginal caption:"The H-shaped region Fensal-Aztlan is faintly visible on Saturn's murky moon Titan in this enhanced clear-filter view from Cassini.
While most of the light passing through the clear filters is visible light, a small portion of the light is in the treasured infrared windows that allow views down to the moon's frigid surface (nota: la NASA persiste nel definire Titano come un mondo "gelido". Forse è vero - a logica diremmo di si - ma i dati che possediamo non autorizzano ancora tale conclusione la quale, ovviamente, è ad oggi solo speculativa).
At the upper left, dark wavelike features in the atmosphere encircle the moon's North Pole.
The view shows principally the Saturn-facing Hemisphere on Titan; North is up and rotated 35° to the left.
The image was taken with the Cassini spacecraft narrow-angle camera on Oct. 7, 2005, at a distance of approximately 2,4 MKM (about 1,5 MMs) from Titan and at a phase angle of 33°. The image scale is 14 Km (about 9 miles) per pixel".
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Titan-Regions-Fensal_and_Aztlan_Region-PIA07732.jpgFensal and Aztlan Region on Titan56 visiteDuring its Sept. 7, 2005, flyby of Titan, Cassini acquired images of territory on the moon's Saturn-facing hemisphere that were assembled to create this mosaic. Once known only as "The H" because the Region looks something like the letter on its side, features in this Region now possess provisional names. The Northern Branch of the H is now called Fensal, while the Southern Branch is known as Aztlan.
Fensal is littered with small "islands" ranging in size from 5 to 40 Km across. These landforms currently are thought to be water ice upland areas, surrounded by shallower terrain that is filled-in with dark particulate material from the atmosphere. A few larger islands are also seen, like Bazaruto Facula (near right, containing a dark crater) and several islands in Western Fensal. When viewed in images of Shangri-La (on the other side of Titan), island-like landforms of this size tend to occur in clusters with apparent preferred orientations. The small islands in Fensal appear much more scattered (and most appear roughly circular), although a few islands do have an east-west orientation to their long axis.
Aztlan, on the other hand, appears comparatively devoid of small islands, with three large islands in its western reaches, plus only a few smaller islands. The largest of these islands is called "Sotra Facula" (just right of center in the bottom left mosaic frame), and measures 240 by 120 kilometers (149 to 75 miles) across.
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Titan-Regions-Fensal_and_Aztlan_Region-PIA08352.jpgFensal and Aztlan Region54 visiteAs Cassini continues its reconnoitering flybys of Titan, the imaging science team continues to improve its ability to tease out surface details hidden in the unprocessed images. This mosaic provides the best view yet obtained by Cassini's cameras, showing terrain on the moon's sub-Saturn Hemisphere -- the side of the moon that always faces toward Saturn. This mosaic has better resolution, both in pixel scale and from improved signal-to-noise, compared to previous views of the area.
"Signal-to-noise" is a term scientists use to refer to the amount of meaningful or useful information (signal) in their data versus the amount of background noise. A higher signal-to-noise ratio yields sharper, clearer views of Titan's surface.
The view is centered on terrain in the Fensal-Aztlan region on Titan, at 0,03° South Lat. and 22,18° West Long. The mosaic covers an area 3.500 Km (2.180 miles) North to South and 3.600 Km (2.240 miles) West to East. North is up.
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Titan-Regions-Fensal_and_Senkyo_Regions-PIA12655-PCF-LXTT.jpgAztlan, Fensal and Senkyo Region (Absolute Natural Colors; credits: Dr Paolo C. Fienga - Lunexit Team)55 visiteCaption NASA:"The Cassini Spacecraft looks toward the dark Senkyo Region on Saturn's moon Titan.
Senkyo is the Dark Region towards the right. Two other Dark Regions, Aztlan (to the left, slanting down below the Equator) and Fensal (left, North of Aztlan), are also shown here.
The bright area below Aztlan is called Tsegihi. This view looks toward the Saturn-facing Side of Titan. North on Titan is up and rotated 9° to the left.
The image was taken with the Cassini Spacecraft narrow-angle camera on April 8, 2010 using a spectral filter sensitive to wavelengths of Near-InfraRed Light centered at 938 nanometers. The view was obtained at a distance of approx. 2,1 MKM (about 1,3 MMs) from Titan and at a Sun-Titan-Spacecraft, or Phase, Angle of 33°.
Image scale is roughly 12 Km (a little more than 7 miles) per pixel".MareKromium
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Titan-Regions-Ganesa_Macula_Region-PIA09176.jpgGanesa Macula65 visiteCaption NASA:"This radar image of Titan shows Ganesa Macula, interpreted as a cryovolcano (ice volcano), and its surroundings. Cryovolcanism is thought to have been an important process on Titan and may still be happening today.
This mosaic was made from images obtained by the Cassini radar mapper on two flybys. The lower part of the image was from the flyby on Oct. 26, 2005, while the upper part was from the Jan. 13, 2007, flyby.
Ganesa macula is the dark circular feature seen on the lower left of the mosaic.
Bright rounded features, interpreted as cryovolcanic flows, are seen towards the top and the right of the mosaic.
This image mosaic was taken in synthetic aperture mode. The resolution of the images is approx. 350 mt (1150 feet). North is toward the top. The image mosaic is about 570 Km (about 354 miles) wide and 390 Km (about 240 miles) high".
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Titan-Regions-Hotei_Arcus_Region-PIA11839-1.jpgHotei Arcus in InfraRed (RAW-b&w frame)56 visiteCaption NASA:"This InfraRed image taken by the Visual and InfraRed Mapping Spectrometer (VIMS) on NASA's Cassini Spacecraft shows Hotei Arcus, a Region on Saturn's moon Titan where changes in brightness have been measured several times during the last four years.
The brightness variations, combined with flow-like morphology seen in higher resolution Cassini radar images, suggest that Hotei Arcus may be the site of current activity, possibly an Ice Volcano. If so, it would be the first active Cryovolcano to be observed on Titan.
The red markings in the false color image (next frame) indicate a Region that is chemically distinct from its surroundings, which may correspond to the most recent location of activity.
Visual and InfraRed Mapping Spectrometer Scientists also report the brightness changes are consistent with transient deposits of Ammonia frost on Titan's Surface, although other materials cannot be ruled out.
Ammonia is generally believed to be an important component in the interior of Titan. The association of Ammonia with brightening in this Region would further suggest that Hotei Arcus is presently a center of activity.
This image was taken at a distance of about 29.000 Km (approx. 18.000 miles) on Nov. 19, 2008".
MareKromium
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Titan-Regions-Hotei_Arcus_Region-PIA11839-2.jpgHotei Arcus in InfraRed (False Colors; credits: NASA/JPL/Space Science Institute)59 visitenessun commentoMareKromium
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Titan-Regions-Hotei_Arcus_Region-PIA11839-3.jpgHotei Arcus in InfraRed (possible Natural Colors; credits: Lunar Explorer Italia)58 visitenessun commentoMareKromium
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Titan-Regions-Omacati_Macula_Region-01-LS28_PSS_LASoderblom_VIMSRADAR20070323.jpgDunes in the "Omacati Macula" Region55 visiteThe first two images of Titan (from the top) were obtained by Cassini’s SAR radar and the VIMS imager, respectively. They cover an area about 300 by 1000 Km wide and centred at 20° North and 45° West in the Omacatl Macula Region.
Dunes are generally rare in this area, even if some of them can still be seen in the enlargement provided by the bottom right radar image (blue arrow). These dunes are correlated to the brown spot visible in the VIMS image.
The green arrows linking the lower left radar image with the VIMS image illustrate that in this region the dark blue units are correlated to with sinuous channels and flow features.MareKromium
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