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Images of 'Saturn's Moon' found, 170

Saturn above the clouds of Titan - Illustration - Saturn from atop Titan's hydrocarbon haze - Artist's view of the planet Saturn view 80 km above the surface of his satellite Titan. In the plane of the rings of the planet appear from left to right the satellites Enceladus, Dione, Tethys and Rhea. Saturn and its rings would be a majestic sight lording over Titan's hydrocarbon haze. The viewpoint is from 50 miles above Titan's surface and three - quarters of a million miles away from Saturn itself. Four of Saturn's smaller satellites can also be seen along the ring plane: left to right are Enceladus, Dione, Tethys and Rhea. Technically, the orange clouds mark the beginning of Titan's condensate haze, which consists of ethane, methane, nitrogen, and a variety of hydrocarbons known collectively as tholin. These gases and hydrocarbons extend upward another 250 miles, resulting in a bluish, earthlike sky, albeit darker due to Titan's great distance from the Sun. Tholin is created by the interaction of the nitrogen - rich gases with ultraviolet light from the Sun and ultimately precipitates all the way down to Titan's surface. Notwithstanding its flame - like colors, this haze is chilled to minus 330o F
Dunes sur Titan - Artist view
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Enceladus, Saturn's satellite, seen by the Cassini probe - Saturn's moon Enceladus seen by Cassini spacecraft - Mosaic of false-coloured images obtained by the Cassini probe during the flight over this satellite on 5 October 2008. The image shows a fractured region in the southern hemisphere of the satellite. On Oct. 5, 2008, just after coming within 25 kilometers (15.6 miles) of the surface of Enceladus, Nasa's Cassini captured this stunning mosaic as the spacecraft sped away from this geologically active moon of Saturn. Craters and cratered terrains are rare in this view of the southern region of the moon's Saturn - facing hemisphere. Instead, the surface is replete with fractures, folds, and ridges - - all hallmarks of remarkable tectonic activity for a relatively small world. In this enhanced - color view, regions that appear blue - green are thought to be coated with larger grains than those that appear white or gray. Portions of the tiger stripe fractures, or sulci, are visible along the terminator at lower right, surrounded by a circumpolar belt of mountains. The icy moon's famed jets emanate from at least eight distinct source regions, which lie on or near the tiger stripes. However, in this view, the most prominent feature is Labtayt Sulci, the approximately one - kilometer (0.6 miles) deep northward - trending chasm located just above the center of the mosaic. Near the top, the conspicuous ridges are Ebony and Cufa Dorsae. This false - color mosaic was created from 28 images obtained at seven footprints, or pointing positions, by Cassini's narrow - angle camera. At each footprint, four images using filters sensitive to ultraviolet, visible and infrared light (spanning wavelengths from 338 to 930 nanometers) were combined to create the individual frames. The mosaic is an orthographic projection centered at 64.49 degrees south latitude, 283.87 west longitude, and it has an image scale of 196 kilometers (122.5 miles) per pixel. The original images ranged in resolution
The formation of Saturn's rings - Artist's view - Saturn moon break up - A satellite of Saturn breaks giving birth to the rings of Saturn and has small satellites
Astronauts and Geyser on Enceladus - Artist view - Astronauts and Water geyser on Enceladus - Artist view: Two astronauts explore the surface of the Enceladus satellite
Astronauts and Geyser on Enceladus - Artist view - Astronauts and Water geyser on Enceladus - Artist view: Two astronauts explore the surface of the Enceladus satellite
Exploration of Titan - Illustration - Looking for life on Titan - An automatic probe explores a hydrocarbon marsh in search of traces of life. A robotic probe explores a frigid ethane lake on Titan. Like the European Space Agency's Huygens probe, this probe carries its own light source as the surface of Titan is only 0.1 percent as bright as the Earth's. Titan is host to a plethora of organic (carbon - based) compounds, hence this is one of the few places in the Solar System where life outside of the Earth may have evolved. In many ways, Titan resemble a frozen primordial Earth, though the greatest obstacle to Titan harboring life - - as we know it - - is the extreme cold. Even though all the chemical ingredients are present, Titan simply may not be warm enough to initiate the chemical reactions required for life. Perhaps sometime in the next decades such a mission to Titan will be a reality
The Cassini spacecraft looks toward Rhea, Saturn's second-largest moon
Tethys and Titan, Saturn satellites - Tethys and Titan - The Tethys satellite passes behind the Titan satellite. These images were taken 18 minutes apart (the first image taken is on the right) by the Cassini probe on 26 November 2009 at a distance of 1 million km from Titan and 2.2 million km from Tethys. Saturn's moon Tethys with its prominent Odysseus Crater silently slips behind Saturn's largest moon Titan and then emerges on the other side. Tethys is not actually enshrouded in Titan's atmosphere. Tethys (1,062 kilometers, or 660 miles across) is more than twice as far from Cassini than Titan (5,150 kilometers, or 3,200 miles across) in this sequence. Tethys is 2.2 million kilometers (1.4 million miles) from Cassini. Titan is about 1 million kilometers (621,000 miles) away. These two color views were captured about 18 minutes apart, with the view on the right taking place first. These images are part of a mutual event sequence in which one moon passes close to or in front of another as seen from the spacecraft. Such observations help scientists refine their understanding of the orbits of Saturn's moons. Images taken using red, green and blue spectral filters were combined to create this natural color view. The images were obtained with the Cassini spacecraft narrow - angle camera on Nov. 26, 2009. Image scale is 6 kilometers (4 miles) per pixel on Titan and 13 kilometers (8 miles) per pixel on Tethys
Saturn seen from a satellite Irregulier - Illustration: Irregular satellite of Saturn
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Saturn seen from the Atmosphere of Titan - Saturn from Titan - Illustration
Saturn view of its satellite Hyperion - Artist view - Saturn from its moon Hyperion - Artist view
Saturn and Titan - Illustration - Saturn from Titan orbit - The planet Saturn seen from the orbit of its Titan satellite. This is how Saturn and Titan might look from a position in orbit around Titan. While in reality Saturn is vastly larger than Titan, it appears smaller here because Titan's orbit puts Saturn at a distance of about 700 thousand miles. Sunlight filtering through Titan's upper atmospheric haze - - extending over 300 miles above the surface - - gives a bluish cast to its limb
Titan, Saturn satellite seen by Cassini - Titan near Saturn seen by Cassini spacecraft - Natural color image of Titan near Saturn blade taken by the Cassini probe on 29 January 2008 at a distance of about 2.3 million km from the satellite. Swathed in its thick blanket of atmosphere, frigid Titan approaches the brilliant limb of Saturn. Images taken using red, green and blue spectral filters were combined to create this natural color view. The images were acquired with the Cassini spacecraft narrow - angle camera on Jan. 29, 2008 at a distance of approximately 2.3 million kilometers (1.4 million miles) from Titan. Image scale is 14 kilometers (8 miles) per pixel
The formation of Saturn's rings - Artist's view - The origin of Saturn's rings
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Saturn seen from its satellite Japet - Saturn from Iapetus - The planet Saturn accompanied by three satellites (from left to right Tethys, Rhea and Dione) seen from the icy surface of Japet. In this image Saturn dominates Iapetus' velvet black sky framed by three inner moons. Left to right are Tethys, Rhea and Dione. Less than half the size of the Earth's moon, ice - covered Iapetus is one of the few places in the Solar System that offers a good view of Saturn's rings. This is because Iapetus' orbit is inclined almost 15 degrees to Saturn's equator. With the exception of Phoebe, none of Saturn's other satellites offer such a vantage point. Unlike haze - shrouded Titan, Iapetus has no atmosphere to speak of and is believed to be composed almost entirely of water ice
Enceladus, Saturn's satellite, seen by Cassini - Saturn's moon Enceladus from Cassini - Mosaic of false-coloured images obtained by the Cassini probe during the flight over this satellite on 11 August 2008. The image shows a fractured region in the southern hemisphere of the satellite. This mosaic of Saturn's moon Enceladus provides broad regional context for the ultra - sharp, close - up views Nasa's Cassini spacecraft acquired minutes earlier, during its flyby on Aug. 11, 2008. This false - color mosaic combines Imaging Science Subsystem (ISS) narrow - angle camera images obtained through ultraviolet, green, and near - infrared camera filters. Areas that are greenish in appearance are believed to represent deposits of coarser grained ice and solid boulders that are too small to be seen at this scale, but which are visible in the higher resolution views, while whitish deposits represent finer grained ice. The mosaic shows that coarse - grained and solid ice are concentrated along valley floors and walls, as well as along the upraised flanks of the “” tiger stripe”” fractures, which may be covered with plume fallout that landed not far from the sources. Elsewhere on Enceladus, this coarse water ice is concentrated within outcrops along cliff faces and at the top of ridges. The sinuous boundary of scarps and ridges that encircles the south polar terrain at about 55 degrees south latitude is conspicuous. Much of the coarse - grained or solid ice along this boundary may be blocky rubble that has crumbled off of cliff faces as a result of ongoing seismic activity. The lighting conditions over the polar region highlight features, such as fractures and ridges, that are barely visible in the July 2005 views, and vice versa. The four most prominent sulci (from top to bottom: Damascus, Baghdad, Alexandria and Cairo) appear as generally horizontal fractures near lower right, and they extend into the moon's night side. The mosaic is an orthographic projection centered at 63.0 degrees south
Saturn from his satellite Dione - Illustration
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A satellite of Saturn breaks into the rings of Saturn and has small satellites.
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Titan, Saturn satellite seen by Cassini - Saturn's moon Titan as seen by Cassini spacecraft: Titan images obtained by the Cassini probe on 21 March 2017. On the left, Titan seen in real colors. On the right, infrared image showing surface details as well as clouds in the northern hemisphere. These views were obtained with the Cassini spacecraft narrow-angle camera on March 21, 2017. Images taken using red, green and blue spectral filters were combined to create the natural-color view at left. The false-color view at right was made by substituting an infrared image (centered at 938 nanometers) for the red color channel. A large, bright and feathery band of summer clouds can be seen arcing across high northern latitudes in the view at right. The views were acquired at a distance of approximately 613,000 miles (986,000 kilometers) from Titan. Image scale is about 4 miles (6 kilometers) per pixel
Clouds on the south pole of Titan - Illustration - Clouds over Titan's south pole - Artist's view of methane clouds observed over the south pole of Titan by the Cassini probe in October 2004. In October 2004 the Cassini orbiter revealed for the first time what may be highly reflective (in the infrared at least) methane clouds over Titan's south pole. This image suggests how those clouds may appear from within the cloud deck itself. The Sun is visible immediately above, though from this great distance the Sun appears to be only 1/10th its diameter from Earth
Saturn and satellites seen by the Cassini probe on 30/01/2008 - Saturn and satellites seen by Cassini spacecraft Jan. 30 2008 - Saturn seen by the Cassini probe on 30 January 2008 at a distance of 1.3 million km from the planet. The Tethys satellite is visible under Saturn's rings and the Titan satellite appears at the top of the picture. Titan emerges from behind Saturn, while Tethys streaks into view, in this colorful scene. Saturn's shadow darkens the far arm of the rings near the planet's limb. Titan is 5,150 kilometers (3,200 miles) wide; Tethys is 1,071 kilometers (665 miles) wide. This view looks toward the unilluminated side of the rings from about 3 degrees above the ringplane. Images taken using red, green and blue spectral filters were combined to create this natural color view. The images were acquired with the Cassini spacecraft wide - angle camera on Jan. 30, 2008 at a distance of approximately 1.3 million kilometers (800,000 miles) from Saturn. Image scale is 77 kilometers (48 miles) per pixel on Saturn
Size comparison: Enceladus, Earth and Moon satellite - Enceladus, Earth, and Earth's Moon Compared - Saturn Enceladus satellite (500 km in diameter) compares with Earth and Moon. Enceladus is considered one of Saturn's major satellites, however it is quite diminutive when compared with the Earth and Earth's Moon. With a radius of only 160 miles, Enceladus could rest in the Gulf of Mexico with plenty of room to spare. Enceladus is one of the brightest objects in the Solar System. Where Earth's Moon has a surface reflectively about the same as charcoal, Enceladus is covered in water ice that reflects sunlight like freshly fallen snow
Saturn seen from his satellite Japet - Saturn as seen from Iapetus
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Saturn and Mimas seen by the Cassini probe on 04/09/2007 - Saturn and Mimas seen by Cassini spacecraft Sept. 4 2007 - Saturn seen by the Cassini probe on 4/09/2007 at a distance of 2.7 million km from the planet. The Mimas ice satellite is visible under Saturn's rings. The Cassini spacecraft looks beyond Saturn's limb towards the icy face of Mimas, the innermost of the planet's major moons. This view looks toward the sunlit side of the rings from about 3 degrees below the ringplane. Mimas is 396 kilometers (246 miles) across. Images taken using red, green and blue spectral filters were combined to create this natural color view. The images were acquired with the Cassini spacecraft narrow - angle camera on Sept. 4, 2007 at a distance of approximately 2.7 million kilometers (1.7 million miles) from Saturn and 2.8 million kilometers (1.8 million miles) from Mimas. Image scale is 16 kilometers (10 miles) per pixel on Saturn and 17 kilometers (11 miles) per pixel on Mimas
Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft: The Tethys satellite photographed by the Cassini probe on 11 April 2015 has a distance of 53,000 km from the satellite. Tethys is about 1070 km in diameter. - This enhancement-color mosaic of Saturn's icy moon Tethys shows a range of features on the moon's trailing hemisphere. Tethys is tidally locked to Saturn, so the trailing hemisphere is the side of the moon that always faces opposite its direction of motion as it orbits the planet - Images taken using clear, green, infrared and ultraviolet spectral filters were combined to create the view, which highlights subtle color differences across Tethys' surface at wavelengths not visible to human eyes. The moon's surface is fairly uniform in natural color - The color of the surface changes conspicuously across the disk, from yellowish hues to nearly white. These broad color changes are affected by a number of external processes. First, Saturn's diffuse E-ring preferentially bombards Tethys' leading hemisphere, towards the right side of this image, with ice bright ice grains. At the same time, charged particles from Saturn's radiation belt bombard the surface on the trailing side, causing color changes due to chemical alteration of the materials there. The albedo - a measure of the surface's reflectivity - drops by 10 to 15 percent from the moon's leading side to the trailing side. Similar global color patterns exist on other Saturnian moons - Mountains on the floor of the 280 mile- (450 km-) wide Odysseus impact basin are visible at upper right, around the two o'clock position - This mosaic is an orthographic projection constructed from 52 Cassini images obtained on April 11, 2015 with the Cassini spacecraft narrow-angle camera. Resolution is about 1,000 feet (300 meters) per pixel. The images were obtained at a distance of approximately 33,000 miles (53,000 kilometers) from Tethys
Rhea, satellite of Saturn, seen by Cassini - Saturn's moon Rhea seen by Cassini - Mosaic of images obtained by the Cassini probe in March 2015. Rhea is the second largest satellite in Saturn (1528 km in diameter). After a couple of years in high - inclination orbits that limited its ability to encounter Saturn's moons, Nasa's Cassini spacecraft returned to Saturn's equatorial plane in March 2015.Image taken using clear, green, infrared and ultraviolet spectral filters were combined to create these enhanced color views, which offer an expanded range of the colors visible to human eyes in order to highlight subtle color differences across Rhea's surface. The moon's surface is fairly uniform in natural color.This view at right is centered at 9 degrees north latitude, 254 degrees west longitude. Resolution in this mosaic is 300 meters (984 feet) per pixel. The image was acquired at a distance that ranged from about 36,000 to 32.100 miles (57,900 to 51,700 kilometers) from Rhea
Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft: The Tethys satellite photographed by the Cassini probe on 11 April 2015 has a distance of 53,000 km from the satellite. Tethys is about 1070 km in diameter. - This enhancement-color mosaic of Saturn's icy moon Tethys shows a range of features on the moon's trailing hemisphere. Tethys is tidally locked to Saturn, so the trailing hemisphere is the side of the moon that always faces opposite its direction of motion as it orbits the planet - Images taken using clear, green, infrared and ultraviolet spectral filters were combined to create the view, which highlights subtle color differences across Tethys' surface at wavelengths not visible to human eyes. The moon's surface is fairly uniform in natural color - The color of the surface changes conspicuously across the disk, from yellowish hues to nearly white. These broad color changes are affected by a number of external processes. First, Saturn's diffuse E-ring preferentially bombards Tethys' leading hemisphere, towards the right side of this image, with ice bright ice grains. At the same time, charged particles from Saturn's radiation belt bombard the surface on the trailing side, causing color changes due to chemical alteration of the materials there. The albedo - a measure of the surface's reflectivity - drops by 10 to 15 percent from the moon's leading side to the trailing side. Similar global color patterns exist on other Saturnian moons - This mosaic is an orthographic projection constructed from 52 Cassini images obtained on April 11, 2015 with the Cassini spacecraft narrow-angle camera. Resolution is about 1,000 feet (300 meters) per pixel. The images were obtained at a distance of approximately 33,000 miles (53,000 kilometers) from Tethys
Titan, Saturn satellite seen by Cassini - Saturn's moon Titan as seen by Cassini spacecraft: Visible and infrared composite image of Titan taken by the Cassini probe on November 13, 2015. View of the hemisphere oriente towards Saturn - This composite image shows an infrared view of Saturn's moon Titan from Nasa's Cassini spacecraft, acquired during the mission's “” T-114”” flyby on Nov. 13, 2015. The spacecraft's visual and infrared mapping spectrometer (VIMS) instrument made these observations, in which blue represents wavelengths centered at 1.3 microns, green represents 2.0 microns, and red represents 5.0 microns. A view at visible wavelengths (centered around 0.5 microns) would show only Titan's hazy atmosphere (as in PIA14909). The near-infrared wavelengths in this image allow Cassini's vision to penetrate the haze and reveal the moon's surface - During this Titan flyby, the spacecraft's close-approach altitude was 6,200 miles (10,000 kilometers), which is considerably higher than those of typical flybys, which are around 750 miles (1,200 kilometers). The high flyby allowed VIMS to gather moderate-resolution views over wide areas (typically at a few kilometers per pixel) - The view looks toward terrain that is mostly on the Saturn-facing hemisphere of Titan. The scene features the parallel, dark, dune-filled regions named Fensal (to the north) and Aztlan (to the south), which form the shape of a sideways letter “” H.””” - Several places on the image show the surface at higher resolution than elsewhere. These areas, called subframes, show more detail because they were acquired near closest approach. They have finer resolution, but cover smaller areas than data obtained when Cassini was farther away from Titan - Near the limb at left, above center, is the best VIMS view so far of Titan's largest confirmed impact crater, Menrva. Similarly detailed subframes show eastern Xanadu, the basin Hotei Regio, and channels within bright terrains east of Xanadu. - Due to the
Saturn seen from Enceladus - Illustration - Saturn from the surface of Enceladus: The planet Saturn seen from the icy surface of its satellite Enceladus
Titan, Saturn satellite seen by Cassini: Visible and infrared composite image of Titan taken by the Cassini probe on September 12, 2013. View of methane and ethane lakes. - This false-color mosaic, made from infrared data collected by Nasa's Cassini spacecraft, reveals the differences in the composition of surface materials around hydrocarbon lakes at Titan, Saturn's largest moon. Titan is the only other place in the solar system that we know has stable liquid on its surface, though its lakes are made of liquid ethane and methane rather than liquid water. While there is one large lake and a few smaller ones near Titan's south pole, almost all of Titan's lakes appear near the moon's north pole - Scientists mapped near-infrared colors onto the visible color spectrum. Red in this image was assigned a wavelength of 5 microns (10 times longer than visible light), green 2.0 microns (four times longer than visible light), and blue 1.3 microns (2.6 times longer than visible light) - The orange areas are thought to be evaporite - the Titan equivalent of salt flats on Earth. The evaporated material is thought to be organic chemicals originally from Titan's haze particles that once dissolved in liquid methane. They appear orange in this image against the greenish backdrop of Titan's typical bedrock of water ice - In this mosaic, Kraken Mare, which is Titan's largest sea and covers about the same area as Earth's Caspian Sea and Lake Superior combined, can be seen spreading out with many tendrils on the upper right,. The big dark zone up and left of Kraken is Ligeia Mare, the second largest sea. Below Ligeia, shaped similar to a sports fan's foam finger that points just up from left, is Punga Mare, the third largest Titan Sea. Numerous other smaller lakes dot the area. Titan's north pole is located in the geographic location just above the end of the “” finger”” of Punga Mare. The data shown here were obtained by Cassini's visual and infrared mapping spectrometer during
Oil Lake on Titan - Titan's ethane ocean - Artist's view of a hydrocarbon lake (methane - ethane) on the surface of Titan. Compared to the Earth, Titan is very far from the Sun's warming rays - - about ten times further - - and this leaves Titan a very cold world. Titan has an average surface temperature of minus 290o F. If there is any water on Titan it is frozen hard as steel, yet Titan may be the only body in the Solar System besides the Earth that harbors a liquid ocean. Titan's ocean would not be one of water, rather it would probably be composed of (very cold) liquid ethane. (On the Earth we know ethane as a colorless, odorless, nontoxic, flammable gas, a constituent of natural gas and petroleum.) If this werenn't exotic enough, immediately beneath this ocean may lie hundreds of feet of frozen acetylene (a common component of welder's torches)
Astronauts on Titan - Illustration - Walking a dry gully on Titan - Astronauts explore Titan's surface. Earthlings explore a dry gully on Saturn's moon Titan. In early 2005 the European Space Agency's Huygens probe revealed a surface carved by numerous drainage channels similar to river deltas on Earth. While the exact nature of these channels is not yet known, one theory proposes that Titan's surface of hydrocarbon sediments has been washed from the highlands by methane rain
The clouds of Titan - Artist view - Titan's clouds
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Saturn from its moon Epimethee - Illustration - Saturn from its moon Epimetheus
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Astronauts on Titan - Illustration - First steps on Titan - Astronauts explore Titan's surface. Perhaps some day in the far future humans will set foot on Saturn's mysterious moon Titan, one of the most interesting worlds in the Solar System. Larger than the planet Mercury, Earth's moon, and the dwarf planet Pluto, and second only in size to Jupiter's satellite Ganymede, Titan is the only known extraterrestrial world with a dense atmosphere that realistically could be visited by humans. A visit to Titan would require a space journey of a year or more and traverse over 700 million miles. Beneath Titan's 350 miles of atmosphere, intrepid explorers would likely find a dark, forbidding landscape of rock, ice, and possibly tarry layers of hydrocarbons and lakes of liquid ethane and/or methane (AKA natural gas). The Surface temperature would be around minus 300* F, cold enough to freeze exposed human tissue within seconds. There would be no oxygen to breathe, and any water to be found would be as hard and dense as granite. Despite these harsh conditions, Titan could yet yield secrets regarding the origin of life itself as it is believed that, with the exception of the extreme cold, Titan resemble the primordial Earth at the time living organisms first appeared. In this image, Titan's first human visitors are protected by thick suits and helmets to shield them from the extreme cold - - and possibly toxic compounds such as hydrogen cyanide. They carry their own oxygen as Titan's atmosphere is primarily nitrogen with lesser amounts of argon, methane and other gases. Each explorer also carries “” head”” lights attached to their helmets to help them navigate a terrain that receives only 1/1000th the Sun's illumination on the Earth; while this means that noon on Titan would appear relatively dim, it would yet be over 300 times brighter than the Earth under a full moon
Saturn and Mimas seen by the Cassini probe 18/01/2005 - Saturn and Mimas seen by Cassini spacecraft Jan. 18 2005 - The Mimas satellite photographed in front of Saturn by the Cassini probe on 18 January 2005 at a distance of 1.4 million km from the planet. The shadow of Saturn's rings is projected on the planet. Mimas drifts along in its orbit against the azure backdrop of Saturn's northern latitudes in this true color view. The long, dark lines on the atmosphere are shadows cast by the planet's rings. Saturn's northern hemisphere is presently relatively cloud - free, and rays of sunlight take a long path through the atmosphere. This results in sunlight being scattered at shorter (bluer) wavelengths, thus giving the northernmost latitudes their bluish appearance at visible wavelengths. At the bottom, craters on icy Mimas (398 kilometers, or 247 miles across) give the moon a dimpled appearance. Images taken using infrared (930 nanometers), green (568 nanometers) and ultraviolet (338 nanometers) spectral filters were combined. The colors have been adjusted to match closely what the scene would look like in natural color. The images were obtained using the Cassini spacecraft narrow angle camera on Jan. 18, 2005, at a distance of approximately 1.4 million kilometers (870,000 miles) from Saturn. Resolution in the image is 8.5 kilometers (5.3 miles) per pixel on Saturn and 7.5 kilometers (4.7 miles) per pixel on Mimas. The image has been contrast - enhanced to aid visibility
Saturn view of the surroundings of Dione - Illustration - Saturn from the vicinity of Dione - The planet Saturn seen from the surroundings of its satellite Dione. Dione, visible in the foreground, has a diameter of about 1100 km and is mainly composed of ice. In the background, another Saturn ice satellite is visible, Tethys. This is how Saturn might appear from near Dione, one of Saturn's inner icy satellites. Dione is about 700 miles in diameter and is believed to be composed primarily of water ice along with lesser amounts of silicate rocks. In this image, Dione is in the foreground orbiting about 197 thousand miles above Saturn's cloud tops. Further towards Saturn at a distance of 50 thousand miles from Dione is Tethys, another icy moon, slightly smaller than Dione. Tethys is silhouetted against the “” ring shine”” on Saturn's night side - - reflected sunlight on the cloud tops from Saturn's rings
Saturn view of its satellite Dione - Illustration - Ice walls of Dione
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Geyser sur Enceladus - Artist view - Water geyser on Enceladus - Artist view - Artist view of an ice geyser on the surface of the Enceladus satellite. In the sky, the planet Saturn. A look at the water geysers of Saturn's moon Enceladus, which have been revealed to us so brilliantly by the Cassini Saturn orbiter. This digital illustration shows the water jets shooting out from vents in the bottom of one of the icy moon's multitude of folded, fractured valleys
Saturn view of Enceladus - Illustration - Saturn from the surface of Enceladus - The planet Saturn seen from the ice surface of Enceladus. This is how Saturn may appear from the icy surface of Enceladus, one of Saturn's eight major satellites. At a distance of 148 thousand miles, Saturn would subtend an angle of 29o in Enceladus' sky, about the same width as 58 Earth moon's lined up side - by - side. While the surface of Enceladus is as reflective as new fallen snow, it would probably appear leaden about an hour before sunrise with a crescent Saturn as the only source of illumination. Like all of Saturn's major satellites, Enceladus always keeps the same side facing its host planet. From the perspective of a stationary observer on Enceladus, Saturn would always appear in the same position in the sky, cycling through its phases in about one - and - half Earth days. This image also illustrates a phenomenon only recently discovered by Nasa's Cassini probe: sunlight reflecting off of Saturn's rings casts a faint glow onto the cloud tops of Saturn's night side. The illumination is about the same as three of Earth's full moon combined
Japet, satellite of Saturn, seen by Cassini - Saturn's moon Iapetus seen by Cassini spacecraft - Comparison of the two hemispheres of Japet, a satellite of Saturn of 1471 kilometres in diameter. Its main feature is the color difference between the two hemispheres. On the left, the dark region called Cassini Regio with to the east the largest crater of Japet, named Turgis (580 km in diameter). On the right, the bright side of the satellite with Roncevaux Terra (north) and Saragossa Terra (south) housing the large impact crater Engelier (504 km in diameter). Both images were obtained by the Cassini probe on 10 September 2007 (right) and 27 December 2004 (left). These two global images of Iapetus show the extreme brightness dichotomy on the surface of this peculiar Saturnian moon. The left - hand panel shows the moon's leading hemisphere and the right - hand panel shows the moon's trailing side. While low and mid latitudes of the leading side exhibit a surface almost as dark as charcoal, broad tracts of the trailing side are almost as bright as snow. The dark terrain covers about 40 percent of the surface and is named Cassini Regio. The names of the bright terrain are Roncesvaux Terra (north) and Saragossa Terra (south). On both hemispheres, the dominant landforms are impact craters. The largest known well - preserved basin on Iapetus, called Turgis, has a diameter of about 580 kilometers (360 miles). It lies at 17 degrees north latitude, 28 degrees west longitude at the eastern edge of the dark Cassini Regio and is visible on the right side of the left - hand panel. The prominent basin on the southern trailing side (at the lower left of the right - hand panel) is Engelier. Engelier is located at 41 degrees south latitude, 265 degrees west longitude, and has a diameter of about 504 kilometers (313 miles). Its formation destroyed about half of Gerin, another large basin on Iapetus. Gerin is located at 46 degrees south latitude, 233 degrees
Mimas, satellite of Saturn, seen by the Cassini probe on 13/02/2010 - Saturn's moon Mimas seen by Cassini spacecraft - February 13 2010 - The Mimas satellite photographed by the Cassini probe on 13 February 2010 has a distance of 30,000 km from the satellite. Mimas is about 400 km in diameter. In the centre, the large impact crater Herschel, 130 km wide. This mosaic, created from images taken by Nasa's Cassini spacecraft during its closest flyby of Saturn's moon Mimas, looks straight at the moon's huge Herschel Crater and reveals new insights about the moon's surface. Bright - walled craters, with floors and surroundings about 20 percent darker than the steep crater walls, are notable in this view. Mimas 'original surface, like the surfaces of most of the other major Saturnian moons without atmospheres, is not pure ice but contains some dark impurities. Herschel Crater (130 kilometers, 80 miles wide) and some of the smaller craters seen in this mosaic show relatively dark markings along the lower portion of their crater walls (marked in green in the annotated version of the image). Cassini scientists interpret this darkening as evidence for the gradual concentration of impurities from evaporating icy materials in areas where the dark impurities slide slowly down the crater wall. There, bright ice is baked away by the sun and the vacuum of space. At Herschel, the edge where the darker regions contact the crater floor is interrupted by an extensive hummocky area. Scientists believe the hummocky texture came from the flow of melted ice that occurred during the impact that created the crater. That melt filled the bottom of the crater around the central peak. Dark streaks are seen making their way down the sides of some craters, often originating from pockets of dark contaminants embedded just below the rim of the crater wall. The pockets themselves likely represent small, pre - existing, dark - floored craters that were buried by the blanket of material that
Mimas, satellite of Saturn, seen by the Cassini probe on 13/02/2010 - Saturn's moon Mimas seen by Cassini spacecraft - February 13 2010 - The Mimas satellite seen in false colours by the Cassini probe on 13 February 2010 has a distance of 16,000 km from the satellite. Color differences reveal differences in terrain nature. Mimas is about 400 km in diameter. At the right centre is the large impact crater Herschel, 130 km wide. Subtle color differences on Saturn's moon Mimas are apparent in this false - color view of Herschel Crater captured by Nasa's Cassini spacecraft during its closest - ever flyby of that moon. The image shows terrain - dependent color variations, particularly the contrast between the bluish materials in and around Herschel Crater (130 kilometers, or 80 miles, wide) and the greenish cast on older, more heavily cratered terrain elsewhere. The origin of the color differences is not yet understood, but may be caused by subtle differences in the surface composition between the two terrains. Herschel Crater covers most of the bottom of this image. To create this false - color view, ultraviolet, green and infrared images were combined into a single picture that exaggerates the color differences of terrain on the moon. These data were combined with a high - resolution image taken in visible light to provide the high - resolution information from the clear - filter image and the color information from the ultraviolet, green and infrared filter images. The natural color of Mimas visible to the human eye may be a uniform gray or yellow color, but this mosaic has been contrast - enhanced and shows differences at other wavelengths of light. During its closest - ever flyby on Feb. 13, 2010, Cassini came within about 9,500 kilometers (5,900 miles) of Mimas. This view looks toward the northern part of the hemisphere of Mimas that leads in the moon's orbit around Saturn. Mimas is 396 kilometers (246 miles) across. North on Mimas is up
Mimas, satellite of Saturn, seen by the Cassini probe on 13/02/2010 - Saturn's moon Mimas seen by Cassini spacecraft - February 13 2010 - The Mimas satellite photographed by the Cassini probe on 13 February 2010 has a distance of 16,000 km from the satellite. Mimas is about 400 km in diameter. In the centre left, the large impact crater Herschel, 130 km wide. Relatively dark regions below bright crater walls and streaks on some of the walls are seen in this mosaic of Saturn's moon Mimas, created from images taken by Nasa's Cassini spacecraft during its closest flyby of the moon. The crater floors and surroundings are about 20 percent darker than the steep crater walls in this view. Mimas 'original surface, like the surfaces of most of the other major Saturnian moons without atmospheres, is not pure ice but contains some dark impurities. The relatively dark markings appear along the lower portion of the walls of Herschel Crater (130 kilometers, 80 miles wide) and some of the smaller craters and are marked in green in the annotated version of the image. Cassini scientists interpret this darkening as evidence for the gradual concentration of impurities from evaporating icy materials in areas where the dark impurities slide slowly down the crater wall. There, the bright ice is baked away by the sun and the vacuum of space. At Herschel, the edge where the darker regions contact the crater floor is interrupted by an extensive hummocky area. Scientists believe the hummocky texture came from the flow of melted ice that occurred during the impact that created the crater. That melt filled the bottom of the crater around the central peak. Dark streaks are seen making their way down the sides of some craters and often originated from pockets of dark contaminants embedded just below the rim of the crater wall. The pockets themselves likely represent small, pre - existing, dark - floored craters that were buried by the blanket of material thrown out from the newer im
Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft - The Tethys satellite photographed by the Cassini probe on August 30, 2007 at a distance of 97,000 km. Tethys is about 1070 km in diameter. At the top left of the picture is the gigantic impact crater Odysseus, which measures 450 km in diameter. The vast expanse of the crater Odysseus spreads out below Cassini in this mosaic view of Saturn's moon Tethys. The crater (450 kilometers or 280 miles across) is a remarkably well - preserved example of an ancient multi - ringed impact basin: the outer ring is defined by steep, cliff - like walls that descend to generally broad internal terraces. The inner ring is formed by a prominent, crown - shaped, 140 - kilometer (88 - mile) diameter circular band of icy mountains. Multi - ring basins are seen on rocky bodies as well as icy ones. The complex internal structure and multi - ringed nature of these very large basins are believed to arise from the rebound of intense shock waves that penetrated the body at the time of impact. Tethys is 1,071 kilometers (665 miles) across. This mosaic was assembled from four clear filter, narrow - angle camera images. The view is an orthographic projection centered on 3 degrees south latitude, 119 degrees west longitude and has a resolution of 572 meters (0.35 mile) per pixel. An orthographic view is most like the view seen by a distant observer looking through a telescope. North is up. The view was obtained by the Cassini spacecraft on Aug. 30, 2007, from a distance of approximately 97,000 kilometers (60,000 miles) and at a sun - Tethys - spacecraft, or phase, angle of 51 degrees
Cassini - Huygens en route to Titan - The Cassini - Huygens probe above Titan's atmosphere - Artist's view of the Cassini probe before the separation of the European Huygens module on 25 December 2004. Huygens landed on the Titan satellite on 14 January 2005. The Cassini-Huygens probe was launched on 15 October 1997 and has been placed in orbit around Saturn since 1 July 2004. This artist's conception of the Cassini orbiter shows the Huygens probe before separation to enter Titan's atmosphere. After separation, the probe drifts for about three weeks until reaching its destination. Equipped with a variety of scientific sensors, the Huygens probe will spend 2 - 2.5 hours descending through Titan's dense, murky atmosphere of nitrogen and carbon - based molecules, beaming its findings to the distant Cassini orbiter overhead. The probe could continue to relay information for up to 30 minutes after it lands on Titan's frigid surface, after which the orbiter passes beneath the horizon as seen from the probe
Mimas, satellite of Saturn, seen by the Cassini probe on 13/02/2010 - Saturn's moon Mimas seen by Cassini spacecraft - February 13 2010 - The Mimas satellite photographed by the Cassini probe on 13 February 2010 has a distance of 50,000 km from the satellite. Mimas is about 400 km in diameter. At the right centre is the large impact crater Herschel, 130 km wide. In this view captured by Nasa's Cassini spacecraft on its closest - ever flyby of Saturn's moon Mimas, large Herschel Crater dominates Mimas, making the moon look like the Death Star in the movie “” Star Wars.”” Herschel Crater is 130 kilometers, or 80 miles, wide and covers most of the right of this image. Cassini came within about 9,500 kilometers (5,900 miles) of Mimas on Feb. 13, 2010.This mosaic was created from six images taken that day in visible light with Cassini's narrow - angle camera on Feb. 13, 2010. The images were re - projected into an orthographic map projection. This view looks toward the area between the region that leads on Mimas 'orbit around Saturn and the region of the moon facing away from Saturn. Mimas is 396 kilometers (246 miles) across. This view is centered on terrain at 11 degrees south latitude, 158 degrees west longitude. North is up. This view was obtained at a distance of approximately 50,000 kilometers (31,000 miles) from Mimas and at a sun - Mimas - spacecraft, or phase, angle of 17 degrees. Image scale is 240 meters (790 feet) per pixel
Surface of Titan seen by Huygens - Illustration - Titan Emerges - Artist's view of the surface of Titan as it appeared at the European probe Huygens on January 14, 2005 when it descended, about 20 km from the ground. This is how the surface of Titan may have appeared to the European Space Agency's Huygens probe when it emerged from the satellite's ubiquitous hydrocarbon haze about 12 miles above Titan's surface. Huygens made its historic decent on 14 January 2005, making it the first man - made object to reach the surface of the satellite of another planet
Surface de Titan - Illustration - Titan surface - Artist's view of the surface of Titan. In the sky, the planet Saturn. It is not known what lies beneath Titan's obscuring haze.* What is known is that Titan's atmosphere is one - and - a - half times as dense as the Earth's at sea level, and its composition is roughly 90% nitrogen and 10% other complex molecules such as methane (compare this to the Earth's atmosphere which is 78% nitrogen and 20% oxygen). Sadly, Titan's thick haze would make it unlikely that a visitor to Titan's surface could look up into the sky and see Saturn itself, but what the heck.
Geyser on Titan - Artist view - Cryogeyser on Titan - Artist view - Artist view of geyser on the surface of Titan, Saturn's largest satellite
Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft - The southern pole of the Tethys satellite photographed by the Cassini probe on September 24, 2005. Mosaic of nine images. With this full - disk mosaic, Cassini presents the best view yet of the south pole of Saturn's moon Tethys. The giant rift Ithaca Chasma cuts across the disk. Much of the topography seen here, including that of Ithaca Chasma, has a soft, muted appearance. It is clearly very old and has been heavily bombarded by impacts over time. Many of the fresh - appearing craters (ones with crisp relief) exhibit unusually bright crater floors. The origin of the apparent brightness (or “” albedo”) contrast is not known. It is possible that impacts punched through to a brighter layer underneath, or perhaps it is brighter because of different grain sizes or textures of the crater floor material in comparison to material along the crater walls and surrounding surface. The moon's high southern latitudes, seen here at the bottom, were not imaged by Nasa's Voyager spacecraft during their flybys of Tethys 25 years ago. The mosaic is composed of nine images taken during Cassini's close flyby of Tethys (1,071 kilometers, or 665 miles across) on Sept. 24, 2005, during which the spacecraft passed approximately 1,500 kilometers (930 miles) above the Moon's surface. This view is centered on terrain at approximately 1.2 degrees south latitude and 342 degrees west longitude on Tethys. It has been rotated so that north is up. The clear filter images in this mosaic were taken with the Cassini spacecraft narrow - angle camera at distances ranging from 71,600 kilometers (44,500 miles) to 62,400 kilometers (38,800 miles) from Tethys and at a Sun - Tethys - spacecraft, or phase, angle of 21 degrees. The image scale is 370 meters (1,200 feet) per pixel
Titan, Saturn satellite seen by Cassini - Saturn's moon Titan as seen by Cassini spacecraft: Visible and infrared composite image of Titan taken by the Cassini probe on August 21, 2014. View of methane and ethane lakes lit by the Sun. - This near-infrared, color mosaic from Nasa's Cassini spacecraft shows the sun glinting off of Titan's north polar seas. - The sunglint, also called a specular reflection, is the bright area near the 11 o'clock position at upper left. This mirror-like reflection, known as the specular point, is in the south of Titan's largest sea, Kraken Mare, just north of an island archipelago separating two separate parts of the sea - This particular sunglint was so bright as to saturate the detector of Cassini's Visual and Infrared Mapping Spectrometer (VIMS) instrument, which captures the view. - The southern portion of Kraken Mare (the area surrounding the specular feature toward upper left) displays a “” bathtub ring”” - a bright margin of evaporate deposits - which indicates that the sea was larger at some point in the past and has become smaller due to evaporation. The deposits are material left behind after the methane & ethane liquid evaporates, somewhat akin to the saline crust on a salt flat
Titan Exploration - Illustration - Exploring a hydrocarbon swamp on Titan - Automatic balloons fly over an oil marsh on the surface of Titan. A pair of balloon - borne probes leisurely survey a methane - ethane “” swamp”” on Titan. Each probe carries its own spot light illuminating the terrain below, augmenting the haze - filtered sunlight. Scientists have long speculated that methane and ethane may exist as liquids on Titan's extremely cold surface, but it wasn't until 2005 that the Cassini spacecraft's radar imager detected what indeed may be large hydrocarbon lakes on Titan's northern latitudes. While it is believed that the liquid in these lakes would be primarily methane and ethane, this won't be confirmed until the lakes - - if that's indeed what they are - - are actually sampled. Whatever lies on Titan's surface, there is the possibility that the ancient and exotic environment has given rise to compounds heretofore unknown on Earth. Large quantities of Methane and ethane exist in Earth's relatively warm environment as components of natural gas
Saturn seen by the Cassini probe 02/2007 - Saturn from Cassini spacecraft 02/2007 - Image obtained by the Cassini probe on 3 February 2007 at a distance of 1.1 million km from the planet. At the bottom of the picture, near the planet blade on the left, we can distinguish the Janus satellite. View of Saturn obtained with the Cassini spacecraft on February 03 2007, at a distance of approximately 1.1 million kilometers from the planet. The small moon Janus can be spotted off the planet's western limb near the image bottom