Daphnis is one of Saturns small moons that is embedded in the Keeler gap in the ring system. This image from Cassini shows it kicking up waves as it orbits.
Daphnis is only about 8 km across, but its gravity is powerful enough to disrupt the particles near the edge of the A ring at the Keeler gap’s edge. Wave-like features form as the moon moves along.
Image Credit: NASA
Video Credit: NASA
Saturn’s moon Tethys seems to float in front of Saturn’s rings in this picture taken by the Cassini spacecraft. The rings appear almost edge-on as dark bands above Tethys, and their curving shadows fall on the planet at the bottom of the image.
Image Credit: NASA
Here’s a picture of a moon shining by the light of its planet. Most of Enceladus in this image is illuminated by sunlight reflected from Saturn. The normally snow-white moon appears in the gold color of Saturn’s cloud tops. Because the light comes from the image left, a labyrinth of ridges throws notable shadows just to the right of the image center; the kilometer-deep canyon Labtayt Sulci is visible just below. The bright crescent on the is the part of Enceladus directly lit by the Sun. This image was taken by the Cassini spacecraft during a close pass by by the moon in 2011. If you look closely at the lower leftt of this digitally sharpened image, you can see plumes of ice crystals thought to originate in a subsurface sea.
Image Credit: NASA
Saturn’s two largest moons, Titan and Rhea, seem to be stacked together in this true-color picture taken by the Cassini spacecraft. This view looks toward the Saturn-facing side of Rhea. North on Rhea is up and rotated 35 degrees to the right.
Separate images taken with red, green and blue filters using Cassini‘s narrow-angle camera were combined to create this natural-color view. The spacecraft was approximately 1.8 million km away from Rhea and 2.5 million km from Titan.
Image Credit: NASA
When this picture was taken in December, 2013, winter was approaching in the southern hemisphere of Saturn, and with that even colder season came a blue hue to some of the planet’s clouds. The color is likely caused by a reduction of ultraviolet sunlight and the haze it produces. With less haze the atmosphere is clearer, increasing Rayleigh scattering (scattering by molecules and smaller particles) and methane absorption. Both processes make the atmosphere appear blue. A similar process cause the blue color of the clouds on Uranus and Neptune.
BTW, it’s now spring in the southern hemisphere of Saturn.
Image Credit: NASA
The Cassini spacecraft took this wide-angle view of Saturn on 28 October, 2016, when it was about 1.4 million km from the planet. This point of view is from the far side of the planet showing shadows that can’t be seen from Earth. The spacecraft has spent 13 years exploring Saturn and its moons before being de-orbited into the planet’s atmosphere..
Image Credit: NASA
Some parts of the surface of Saturn’s moon Dione are covered by linear features, called chasmata, in dramatic contrast to the round impact craters that cover most moons. The bright network of fractures on Dione was seen in poor resolution Voyager images and was called “wispy terrain.” The actual nature of this terrain was unclear until Cassini photos showed we weren’t seeing something like surface deposits of frost but a pattern of bright icy cliffs among myriad fractures. This stress pattern may be related to Dione’s orbital evolution and the effect of tidal stresses over time.
Image Credit: NASA
Two bodies in the Solar System have freely flowing liquids on their surface. The Earth has water. Saturn’s largest moon Titan is too cold for liquid water, but it does have liquid methane.
This image shows a flash of sunlight reflected off a lake on Titan. Its northern hemisphere is shrouded in darkness for nearly 15 years, but the sun begins to illuminate the area again as it approaches its spring equinox. The Cassini spacecraft was able to detect the glint at the beginning of Titan’s spring in 2009. The moon’s hazy atmosphere scatters and absorbs many wavelengths of light, including most of the visible spectrum. But an onboard instrument was able to detect the glint in infrared wavelengths that can penetrate through Titan’s atmosphere. This image was created using wavelengths of light in the 5 µm range.
Image Credit: NASA
Because of the angle that the Sun’s light is falling on them, Mimas (right) and Dione (left) appear to be staring up at Saturn looming in the background of this image captured by the Cassini spacecraft.
Although certainly large enough to be noticeable, moons like Mimas (396 km across) and Dione (1123 km across) are tiny compared to Saturn (120,700 km across). Even the enormous moon Titan (5,150 kilometers across, larger than the planet Mercury) would be dwarfed by the giant planet in such a picture.
Image Credit: NASA
The Cassini spacecraft took this picture of Saturn’s Moon Titan looking at the side that always faces away from the planet because the moon’s orbit is tidal locked (like Earth’s Moon’s) Titan is the only moon in the Solar System with a dense atmosphere (visible in this picture), liquid on its surface, and a cycle of evaporation and liquid rain.
Image Credit: NASA
The Cassini spacecraft relayed to Earth thist close-up, visible-light views of a monster hurricane swirling around Saturn’s north pole. It’s 2,000 km wide, 20 times larger than the average hurricane eye on Earth. The clouds at the outer edge of the hurricane are moving at 150 meters per second as the storm swirls inside a large, six-sided weather pattern known as the hexagon. This false-color image highlights the storm at Saturn’s north pole.
A natural color image is at left.
Hurricanes on Earth feed off warm ocean water, but there is no body of water on Saturn. Learning how these Saturnian storms use water vapor might tell scientists more about how terrestrial hurricanes are generated and sustained. Both terrestrial hurricanes and Saturn’s north polar vortex have a central eye with no clouds or very low clouds. Both have high clouds forming an eye wall, other high clouds spiraling around the eye, and a counter-clockwise spin in the northern hemisphere. But the one on Saturn is much bigger than its counterparts on Earth and spins surprisingly fast. On Saturn, the wind in the eye wall blows more than four times faster than hurricane-force winds on Earth. Terrestrial hurricanes move around, but Saturn’s hurricane is parked over the planet’s north pole. On Earth, hurricanes tend to drift northward because of the forces acting on the winds as the planet rotates. Saturn’s does not drift; it’s already as far north as it can be.
Scientists believe the massive storm has been churning for years. When Cassini arrived in the Saturn system in 2004, Saturn’s north pole was in winter darkness. Cassini‘s composite infrared spectrometer and visual and infrared mapping spectrometer detected the great vortex, but a visible-light image had to wait for the equinox in 2009 when sunlight begin falling on the higher latitudes of Saturn’s northern hemisphere.
Image Credits: NASA
In this picture the Sun’s light is glinting off of a hydrocarbon sea on Saturn’s moon Titan. The infrared image was taken in 2014, and the reflect sunlight was so bright is saturated the camera on the Cassini spacecraft.
Image Credit: NASA / JPL / U. Arizona / U. Idaho
This is Saturn, as seen by the Very Large Array (VLA) radio telescope. The bright disk of the planet gradually fades toward the edge, an effect called limb darkening. It’s caused by the gradual cooling moving outward in Saturn’s atmosphere. The rings are seen as emitters of energy outside the planet’s disk, but in front of the planet they absorb the radiation from the bright disk behind and appear as a dark band. That’s in contrast to their appearance in visible light where they reflect the incident sunlight. At radio wavelengths sunlight is much fainter, and we see the actual radio emissions from Saturn.
Image Credit: NRAO
Iapetus is the third-largest satellite of Saturn and the eleventh-largest in the Solar System. Iapetus has a bright hemisphere and a dark hemisphere. Because it is tidally locked, it always keeps the same face towards Saturn. The bright hemisphere is visible from Earth when Iapetus is on the western side of Saturn, and the dark hemisphere is visible when Iapetus is on the eastern side.
This image was pieced together from data taken by the Cassini spacecraft.
Image Cedit: NASA
Saturns rings are divided into distinct bands. The Saturnian moons Prometheus and Pan are both caught “shepherding” their respective rings in this image (click the image to embiggen it). Through their gravitational effect on nearby ring particles, one moon maintains a gap in the outer A ring, and the other helps keep another ring narrowly confined.
Prometheus (86 km across) and its partner Pandora (not seen here), maintains the narrow F ring seen at the bottom left in this image. Pan (28 km across) clears the Encke gap in as it moves along the gap’s center. You may not be able to see Pan unless you embiggen the image. The other bright dot near the inner edge of the Encke gap is a star in the background.
Image Credit: NASA
Titan is the only moon in the solar system with a thick atmosphere, and the only world besides Earth known to have lakes and seas on its surface. However, with a frigid surface temperature of around -290° F (94 K), the rain falling on Titan isn’t water. It’s liquid methane and ethane, compounds that are gases at room temperature on Earth.
Most of Saturn’s moons display their ancient faces pockmarked by thousands of craters. Titan, Saturn’s largest moon, looks younger than it really is because its craters are being eroded. Radar observations by the Cassini spacecraft show that dunes of hydrocarbon sand are filling in the craters.
This image taken with the Cassini radar shows two craters on Titan. On the left is crater Sinlap which is a relatively ‘fresh’ crater, with a depth-to-diameter ratio similar to is found on other large moons in the solar system such as Ganymede. One the right is Soi, an extremely eroded crater with a very small depth compared to similar craters on Ganymede. These craters are both about 80 km (almost 50 miles) in diameter.
Image Credit: NASA
This snapshot was taken by the Cassini spacecraft. The small moon that seems to be hovering over Saturn’s rings is Janus. It’s only about 180 km across. The larger moon is Rhea, which is around 1500 km across. Saturn’s thin outer F ring is visible in front of Rhea, and the top of the moon is visible between the larger A and B rings.
Image Credit: NASA
This is Saturn’s north pole. This image from the Cassini spacecraft shows the planet in natural color.
Image Credit: NASA
Well, you are if you’re over 15 years old. Back in 2006, the Cassini spacecraft orbiting Saturn drifted in giant planet’s shadow and looked back toward the eclipsed Sun. Saturn’s rings lit up so much that new rings were discovered, although they are hard to see in this image. Saturn’s E ring, the ring created by the newly discovered ice-fountains of the moon Enceladus and the outermost ring visible above, does show up in vivid detail. Far in the distance, at about 10 o’clock on the left, just above the bright main rings, is the almost ignorable pale blue dot of Earth. You may have to click on the image to embiggen it in order to see the Earth.
Image Credit: NASA
Images from the Hubble Space Telescope were used to create these animations of the rotation of the outer planets as seen from Earth.
Video Credit: STScI
The Cassini spacecraft snapped this picture of the moon Dione orbiting Saturn. At 1122 km in diameter, Dione is the 15th largest moon in the Solar System. Its interior is probably a combination of equal masses of silicate rock and water ice.
Shape and gravity observations collected by Cassini suggest the moon has a core of around 400 km of rock surrounded by a roughly 160 km envelope of water, probably in the form of ice. However, some models suggest the lowermost part of this layer could be in the form of an internal liquid salt water ocean.
Image Cedit: NASA
Video Credit: NASA
These two natural color images taken by the Cassini spacecraft show how Saturn’s north polar region has changed between 2012 and 2016. The color change is thought to be an effect of Saturn’s seasons. It’s believed that the change from a bluish color to a more golden hue is caused by the increased production of smog in the atmosphere as the north pole approached the summer solstice due in May, 2017.
The hexagon, Saturn’s six-sided jetstream, seems to act as a barrier preventing haze particles produced outside it from entering. If that’s the case, the polar atmosphere becomes clear of aerosols produced by photochemical reactions, reactions caused by sunlight, during the winter darkness. After Saturn’s northern spring equinox, the north pole polar is in continuous sunshine, and smog aerosols can be produced inside the hexagon, making the polar atmosphere appear hazy.
Image Credit: NASA
This picture is a mosaic of nine images taken by the Cassini spacecraft four years ago, just days before in was do-orbited into Saturn’s atmosphere. We won’t be able to view Saturn’s night side again until we again get another spacecraft to the planet’s far side.
Image Credit: NASA