Range : 1.2 million km. ( 740,000 miles ) P-23954C Voyager 2 obtained this color image of Saturn's F-ring and its small inner sheparding satellite (1990S27) against the full disk of the planet. TheA-ring and the Encke Gap appear in the lower left corner. This view shows that the shepard is more refective than Sturn's clouds, suggesting that it is an icy, bright surfaced object like the larger satellites and the ring particles themselves.

Range : 147,000 km. ( 91,000 mi. ) Resolution : 2.7 km. ( 1.7 mi. ) P-29524C this Voyager 2 color image of the Uranian satellite, Miranda is a composite of three shots taken through green, violet, and ultraviolet filters from the narrow angle camera. It is the best color image of Miranda returned to date. Miranda, just 480 km. (300 mi.) across, is the smallest of Uranus' five major satellites. Miranda's regional geologic provinces show very well in this view of the southern hemisphere. The dark and bright banded region, with its curvilinear traces, covers about half of the image. Higher resolution pictures taken later show many fault lines valleys and ridges parallel to these bands. Near the terminator (at right), another system of ridges and valleys abuts the banded terrain, while many impact craters pockmark the surface in this region. The largest of these are about 30 km. (20 mi.) in diameter. Many more lie in the range of 5 to 10 km. (3 to 6 mi.) in diameter

P-34690 Field of View : 1,000 km. or 600 miles This photograph of Neptune's moon Triton was acquired by Voyager 2. Triton's limb cuts obliquely accross the middle of the image. Three irregular dark areas, surrounded by brighter material, dominate the image. Low-lying material with intermediate albedo occupies the central area, anf fresh craters occur along the right margin. sub-parallel alignment of linear patches of dark material shown in the lower and left part of the image suggests that the patches are structurally controlled.

Range : 900,000 miles A brilliant halo around Jupiter, the thin ring of particles discovered by Voyager 1 four months ago, is seen here unusually bright due to forward scattering of the particles within it. Similiarly, the planet is outlined by sunlight scattered toward the spacecraft from a haze layer high in jupiter's atmosphere. The arms of the ring are cut off on each sideby the planet's shadow as they approach the brightly outlined disk. The night side of the planet appears completly dark in this reproduction, but later will be specially reprocessed to search for evidence of lightning sorms and auroras. This 4 image mosaic was obtained with Voyager 2's wide angle camera.

P-21749 C Range: 6 million kilometers (4 million miles) This photograph of Ganymede, the largest satellite of Jupiter, is shown at approximately the same distance as that photographed at close range by Voyager 1 in March. This picture, taken by Voyager 2, illustrates well the light, bluish regions near the north and south poles. It is known that there is exposed water ice on the surface of Ganymede, and pehaps these polar caps are composed of a light covering of water ice or frost. Voyager 2 will pass within 63,000 kilometers (39,000 miles) of Ganymede.

210' Dish Antenna at Goldstone Ca - used in tracking Pioneer spacecraft

P-29514 BW Miranda reveals a complex geologic history in this view acquired by Voyager 2 around its closest approach to the Uranian moon. At least three terrain types of different age and geologic style are evident at this resolution of about 700 meters (2,300 feet). Visible in this clear-filter, narrow-angle image are from left: 1) an apparently ancient, cratered terrain consisting of rolling, subdued hills and degraded medium-sized craters; 2) a grooved terrain with linear valleys and ridges developed at the expense of, or replacing, the first terrain type; and 3) a complex terrain seen along the terminator, in which intersecting curvillinear ridges and troughs are abrubtly truncated by the linear, grooved terrain. Voyager scientists believe this third terrain type is intermediate in age between the first two.

Range : 6 Million km. ( 3.72 million miles ) This photograph of Jupiter, shot from Voyager 2, shows the equator to the southern polar latitudes, near the Great Red Spot. The white oval that appears here is different from the one seen in a similiar position when voyager 1 passed years before. The region of white clouds now extends from east of The Red Spot and around it's northern boundary, preventing small cloud vortices from circling the feature. The disturbed region west of The Red Spot has also changed since Voyager1. It shows more small scale structure and cloud vortices being formed out of the wave structures.

After traveling more than 1.5 billion km (948 million mi.), the Magellan spacecraft was inserted into orbit around Venus on Aug. 10, 1990. This mosaic consists of adjacent pieces of two magellan image strips obtained in the first radar test. The radar test was part of a planned In-Orbit Checkout sequence designed to prepare the magellan spacecraft and radar to begin mapping after Aug. 31. The strip on the left was returned to the Goldstone Deep Space Network station in California; the strip to the right was received at the DSN in Canberra, Australia. A third station that will be receiving Magellan data is locaterd near Madrid, Spain. Each image strip is 20 km (12 mi.) wide and 16,000 km (10,000 mi.) long. This mosaic is a small portion 80 km (50 mi.) long. This image is centered at 21 degrees north latitude and 286.8 degrees east longitude, southeast of a volcanic highland region called Beta Regio. The resolution of the image is about 120 meters (400 feet), 10 times better than revious images of the same area of Venus, revealing many new geologic features. The bright line trending northwest-southeast across the center of the image is a fracture or fault zone cutting the volcanic plains. In the upper lest corner of the image, a multiple-ring circular feature of probable volcanic origin can be seen, approx. 4.27 km (2.65 mi.) across. The bright and dark variations seen in the plains surrounding these features correspond to volcanic lava flows of varying ages. The volcanic lava flows in the southern half of the image have been cut by north-south trending faults. This area is similar geologically to volcanic deposits seen on Earth at Hawaii and the Snake River Plains in Idaho.

P-21752 BW Range: 1.2 million kilometers This image of Europa shows detail about 20 kilometers across and is somewhat higher resolution than the best Voyager 1 image. The part of Europa shown is the hemisphere that will be viewed at even higher resolution during another Voyager 2 encounter with Europa. Color reconstruction in this image was slightly enhanced to bring out detail in the complicated mottled region on the west limb, containing some of the linear fracture-like features discovered by Voyager 1. The regions in the north and south polar areas which appear bluish in this version are in fact white.

Deep Space Antenna 210' at Goldstone, CA (JPL ref: P-116594AC)

Range : 85,000 kilometers (53,000 miles) This photo of Jupiter's satellite Ganymede shows ancient cratered terrain. A variety of impact craters of different ages are shown. The brightest craters are the youngest. The ejecta blankets fade with age. The center shows a bright patch that represents the rebounding of the floor of the crater. The dirty ice has lost all topography except for faint circular patterns. Also shown are the 'Callisto type' curved troughs and ridges that mark an ancient enormous impact basin. The basin itself has been destroyed by later geologic processes. Only the ring features are preserved on the ancient surface. Near the bottom of the picture, these curved features are trumcated by the younger grooved terrain.

P-21745 BW Range: 1.1 million miles (675,000 miles) This image of Callisto taken by Voyager 2 was enhanced to reveal detail in the scene. Voyager 1's high resolution coverage was of the hemisphere just over the right-hand (eastern) horizon, and the large ring structure discovered by Voyager 1 is just over the eastern limb. This image shows yet another ring structure in the upper part of the picture. Callisto exhibits some of the most ancient terrain seen on any of the satellites. Scientists think Callisto's surface is a mixture of ice and rock dating back to the final stages of planetary accretion (over 4 billion years ago) when the surface was pockmarked by a torrential bombardment of meteorites. Younger craters show as bright spots, probably because they expose fresh ice and frost.

P-29499 Rings of Uranus

P-34679 Range : 2 million km. ( 1.2 million miles ) In this Voyager 2, wide-angle image, the two main rings of Neptune can be clearly seen. In the lower part of the frame, the originally-announced ring arc, consisting of three distinct features, is visible. This feature covers about 35 degrees of longitude and has yet to be radially resolved in Voyager Images. from higher resolution images it is known that this region contains much more material than the diffuse belts seen elsewhere in its orbit, which seem to encircle the planet. This is consistent with the fact that ground-based observations of stellar occultations by the rings show them to be very broken and clumpy. The more sensitive, wide-angle camera is revealing more widely distributed but fainter material. Each of these rings of material lies just outside of the orbit of a newly discovered moon. One of these moons, 1989N2, may be seen in the upper right corner. The moon is streaked by its orbital motion, whereas the stars in the frame are less smeared. the dark area around the bright moon and star are artifacts of the processing required to bring out the faint rings.

Range : 660,000 kilometers (400,000 miles) Time : 5:05 am PST This Voyager 1 picture of Mimas shows a large impact structure at 110 degrees W Long., located on that face of the moon which leads Mimas in its orbit. The feature, about 130 kilometers in diameter (80 miles), is more than 1/4 the diameter of the entire moon. This is a particularly interesting feature in view of its large diameter compared with the size of the satellite, and may have the largest crater diameter/satillite diameter ratio in the solar system. The crater has a raised rim and central peak, typical of large impact structures on terrestrial planets. Additional smaller craters, 15-45 kilometers in diameter, can be seen scattered across the surface, particularly alon the terminator. Mimas is one of the smaller Saturnian satellites with a low density implying its chief component is ice.

Range : 12.9 million km. ( 8.0 million miles ) P-29467B/W Time lapse Voyager 2 images of Uranus show the movement of two small, bright, streaky clouds, the first such features ever seen on the planet. The clouds were detected in this series of orange filtered images, over a 4.6 hour interval ( from top to bottom ). Uranus, which is tipped on its side with respect to the other planets, is rotating in a counter-clockwise direction, with its pole of rotation near the center of the disk, as are the two clouds seen here as bright streaks. The larger of the two clouds is ata lattitude of 33 degrees. The smaller cloud, seen faintly in the three lower images, lies at 26 degrees ( a lower alttitude and hence closer to the limb). Their counterclockwise periods of rotation are 16.2 and 16.9 hours, respectively. This difference implies that the lower lattitude feature is lagging behind the higher latitude feture at a speed of almost 100 meters pers second (220 mph). Latitudinal bands are also visible in these images, the faint bands, more numerous now then in previous Voyager images from longer range, are concentric with the pole rotation. thatis, they circle the planet in lines of contant latitude.

Range : 2.7 million miles (1.7 million miles) P-29497C Tis Voyager 2, false color composite of Uranus demonstrates the usefulness of special filters in the Voyager cameras for revealing the presence of high altitude hazes in Uranus' atmosphere. The picture is a composite of images obtained through the single orange and two methane filters of Voyager's wide angle camera. Orange, short wavelength and long wavelength methane images are displayed, retrospectively, as blue, green, and orange. The pink area centered on the pole is due to the presence of hazes high in the atmosphere that reflect the light before it has traversed a long enough path through the atmosphere to suffer absorbtion by methane gas. The bluest region at mid-latitude represent the most haze free regions on Uranus, thus, deeper cloud levels can be detected in these areas.

P-29509 C Range: 500,000 kilometers (300,000 miles) This high-resolution color composite of Titania was made as Voyager 2 neared its closest approach to Uranus. Voyager's narrow-angle camera acquired this image through the violet and clear filters and shows details about 9 km (6 mi) in size. Titania has a diameter of about 1,600 km (1,000 MI). In addition to many scars due to impacts, Titania displays evidence of other geologic activity at some point in its history. The large trench-like feature near the terminator (day-night boundary) at middle right suggests at least one episode of tectonic activity, Another, basinlike structure near the upper right is evidence of an ancient period of heavy impact activity. The neutral gray color of Titania is characteristic of the Uranian satellites as a whole.

Range : 16 million km (9.9 million miles) P-34616 This series of six Voyager 2 images of Neptune through different filters reveals altitude in Neptune's clouds. The top three images, taken though orange, violet, and ultraviolet filters by the narrow-angle camera, show several bright cloud features, clearly visible in each image. The 'scooter' cloud, at 42 degrees south latitude, although prominent in the orange image, is invisible in ultraviolet, where scattering by atmospheric molecules is strongest. The disappearance can be understood if the 'scooter cloud has more obscurring atmosphere above it ( i.e. the scooter cloud is lower ) than other bright clouds. The observation also suggest that the centrally located Great Dark Spot is also a low lying feature because it also loses visiblity in the ultraviolet image. The lower three wide angle images ( from left to right: orange, weak methane [541nm], and strong methane [619nm] are arranged in increasing absorption by methane in Neptune's atmosphere. In the lower images the 'scooter cloud' becomes less obvious from left to right, implying there is relatively more absorbing methane above the 'scooter cloud'. Thus the set of images also implies that the 'scooter cloud' is deeper in the atmosphere ( and therefore at higher atmospheric pressure ) than the other bright clouds.

Saturn and it's rings, with callouts, as photographed by Voyager 2

Range : 4 million km. ( 2.5 million miles ) P-34654 This Voyager 2 image of Neptune's satteltite Triton was made by combining images taken through the green, clear, and violet filters. The smallest feature seen are about 74 km, or 46 miles accross. The south pole of Triton is currently tipped toward the sun and it is summer in the southern hemisphere. The south pole is located about a quarter of the way up from the bottom if the image. The bright band near the top of the image nearly coincides with the equator of Triton. One prominent and several smaller bright, wispy streaks extend from the band into the darker northern hemisphere. The prominent wispy streak shows bluish-white color, while the darker northern hemisphere is reddish in color. This may indicate that the streak is freshly deposited frost while the red color in the northern hemisphere may result from methane frost that has been darkened by radiation. Individual markings appear to rotate with the satellite and retain their shapes indicating they are indeed surface features and not in the tenuous atmosphere.

Range : 12.9 million miles (8.0 million miles) P-29468C This false color Voyager photograph of Uranus shows a discrete cloud seen as a bright streak near the planets limb. The cloud visible here is the most prominent feature seen in a series of Voyager images designed to track atmospheric motions. The occasional donut shaped features, including one at the bottom, are shadows cast by dust on the camera optics. The picture is a highly processed composite of three images. The processing necessary to bring out the faint features on the planet also brings out these camera blemishes. The three seperate images used where shot through violet, blue, and orange filters. Each color image showd the cloud to a different degree; because they were not exposed at the same time , the images were processed to provide a good spatial match. In a true color image, the cloud would be barely discernable; the false color helps to bring out additional details. The different colors imply variations in vertical structure, but as of yet it is not possible to be specific about such differences. One possiblity is that the uranian atmosphere may contain smog like constituents, in which case some color differences may represent differences in how these molecules are distributed.

Range : 74 million km. ( 46 million miles ) P-29313CThis Voyager photograph of Uranus is a composite of for images taken by the narrow angle camera. At this range, clouds and other features in the atmosphere as small as 1,370 km. could be detected by Voyager 2. Yet, no such features are visible. This view is toward the illuminated south pole of Uranus. The predominant blue color is the result of atmospheric methane, which absorbs the red wavelengths from incoming sunlight. The spot at the upper left edge of the planet's disk reulted from the removal of a reseau mark used in making measurments on the photograph. Three of Uranus' five known satellites are visible; Miranda ( at far right, closest to the planet ), Ariel ( next out , at top), and Umbriel ( lower left ). Titania and Oberon are now outside the narrow angle camera's field of view when it centered on the planet. This color composite was made from images taken through blue, green, orange, and clear filters.

P-29515 BW Range: 42,000 kilometers (26,000 miles) This image of Miranda, obtained by Voyager 2 on approach, shows an unusual 'chevron' figure and regions of distinctly differing terrain on the Uranian moon. Grooved areas baring light and dark bands, distinct from other areas of mottled terrain, are visible at this resolution of about 600 meters (2,000 feet). The bright V-shaped feature in the grooved areas is the 'cheron' observed in earlier, lower-resolution images. Cutting across the bands are sinuous scarps, probably faults. Superimposed on both types of terrain are many bowl-shaped impact craters less than 5 km (3 mi) wide. The entire picture spans an area about 220 km (140 mi) across.

This Magellan image mosaic shows the impact crater Golubkina, first identified in Soviet Venera 15/16 data. The crater is names after Anna Golubkina (1864-1927), a Soviet sculptor. The crater is about 34 km (20.4 mi.) across, similar to the size of the West Clearwater impact structure in Canada. The crater Golubkina is located at about 60.5 degrees north latitude, 286.7 degrees est longitude. Magellan data reveal that Golubkina has many characteristics typical of craters formed by a mereorite impact including terraced inner walls, a central peak, and radar-bright rough ejecta surrounding the crater. The extreme darkness of the crater floor indicates a smooth surface, perhaps formed by the ponding of lava flows in the crater floor as seen in may lunar impact craters. The radar-bright ejecta surrounding the crater indicates a relatively fresh or young crater. Craters with centeral peaks in the Soviet data range in size from about 10-60 km (6-36 mi.) across. The largest crater identifed in the Soviet Venera data is 140 km (84 mi) in diameter. This Magellan image strip in approx. 100 km (62 mi.) long. The image is a mosaic of two orbits obtained in the first Magellan radar test and played back to Earth to the Deep Space Network stations near Goldstone, CA and Canberra, Australia, respectively. The resolution of this image is approximately 120 meters (400 feet). The see-saw margins result from the offset of individual radar frames obtained along the orbit. The spacecraft moved from the north (top) to the south, looking to the left.

P-34689 Range : 130,000 km. ( 80,000 miles ) Smallest Resolvable Feature : 2.5 km or 1.5 miles This image of Neptune's moon Triton, shot by Voyager 2, is seen here. The long linear feature exteding vertically across the image is probably a graben -- a norrow down-dropped fault block about 35 km. or 20 miles across. The ridge in the center of the graben. The surrounding terrain is a relatively young icy surface with few impact craters.

P-21736 BW This Voyager 2 pictures shows the Great Red Spot and the south equatorial belt extending into the equatorial region. At right is an interchange of material between the south equatorial belt and the equatorial zone. The clouds in this zone are more diffuse and do not display the structures seen in other locations. Considerable structure is evident within the Great Red Spot.

P-21761 C Range: 313,000 kilometers (194,000 miles) This color reconstruction of part of the northern hemisphere of Ganymede shows a scene approximately 1,300 kilometers (806 miles) across. It shows part of dark, densely cratered block which is bound on the south by lighter, and less cratered grooved terrain. The dark blocks are believed to be the oldest parts of Ganymede's surface. Numerous craters are visible, many with central peaks. The large bright circular features have little relief and are probably the remnants of old, large craters that have been annealed by flow of the icy near-surface material. The closely-spaced arcuate, linear features are probably analogous to similiar features on Ganymede which surround a large impact basin. The linear features here may indicate the former presence of a large impact basin to the southwest.

P-34715 Range: 900,000 kilometers (560,000 miles) This post-encounter view of the south pole of Neptune was obtained after Voyager 2 passed the planet and sped away on a southward-trending trajectory. Voyager's wide-angle camera saw features as small as 120 km (75 mi) in diameter. The angle between the Sun, the center of the planet, and the spacecraft is 137 °, so the entire south polar region is illuminated. Near the bright limb, clouds located at 71 and 42 degrees south latitude rotate eastward onto Neptune's night side. A bright cloud (bottom center) lies within 1.5 ° of Neptune's south pole, which has been determined from the orbits of the planet's rings and satellites. The feature is believed to be created by an organized circulation around the pole that forms a clear 'eye' at the center of the system.

This photo of Callisto, outermost of Jupiter's four Galilean satellites, was taken a few minutes after midnight (PST) Feb. 25 by Voyager 1. The distance to Callisto was 8,023,000 kilometers (4.98 million miles). The hemisphere in this picture shows a fairly uniform surface dotted with brighter spots that are up to several hundred kilometers across. Scientists believe the spots may be impact craters but higher-resolution photos will be necessary before the features can be interpreted. Callisto is about the same size as the planet Mercury--about 5,000 kilometers (3,000 miles) in diameter. Callisto is less massive than Mercury, however, giving it a density less than twice that of water. Scientists believe Callisto, therefore, is composed of a mixture of rock and ice (up to about 50 percent by weight). Its surface is darker than those of the other Galilean satellites, but is still about twice as bright as Earth's Moon. This black-and-white photo was taken through a violet filter. Jet Propulsion Laboratory manages and controls the Voyager project for NASA's Office of Space Science. (JPL ref. No. P-21149)

(P-37375) Moon craters as seen by Galileo spacecraft

P-34687 Range : 530,000 km. ( 330,000 miles ) Smallest Resolvable Feature : 10 km or 6 miles This Voyager 2 image of Neptune's satellite Triton shows the first photo of Triton to reveal surface topography. The south pole, continuously illuminated by sunlight at this season, ia at bottom left. the boundary between bright southern hemisphere and the darker and the darker, northern hemisphere is clearly visible. Both the darker regions to the north and the very bright sub-equatorial band show a complex pattern of irregular topography that somewhat resembles 'fretted terrain' on parts of Venus and Mars. The pattern of dark and light regions over most of the southern hemisphere will require higher resolution images for interpretation. Also evident are long, straight lines that appear to be surface expressions of internal, tectonic processes. No large impact ctaters are visible, suggesting that the crust of Triton has been renewed relatively recently, that is, within the last bllion years or less.

P-34713 This Voyager image of Triton reveals two kinds of mid-latitude terrain. Near the center and the lower half of the frame is a gently rolling terrain pock-marked with a modest number of impact craters. The density of impact craters is somewhat similiar to that found on the mare surface of Earth's moon. Crossing this rolling surface are narrow rifts, one of which grades into a chain of craters that probably are of collapse origin. In the upper right part of the frame is a smooth terrain with very sparse impact craters. This terrain evidently has been formed by flooding of the surface by low-viscosity fluids rather late in geologic time. One of the vents from which these fluids erupted probably is represented by a deep, elongate crater near the middle of the right side of the image. Two slightly dark regions underlain by late eruptive material also occur in the left half of the image. Apparent vents for these eruptions are marked by shallow depressiions, which may have been formed by drain back of material at the end of the eruptive episode.

Range : 106,250,000 km. ( 66 million miles) P-22830C This, Voyager 1 image shows Saturn and three of its satellites. A series of dark and light cloud bands appears through high altitude haze in the northern hemisphere. Cosiderable structure can be seen in the rings. The Cassini division, between the A-ring and B-ring, is readily visible. The shadow of rings on the planet's disk can also be seeen. The three satellites visible are, left to right, Enceladus (off the left edge of rings), Dione (just below the planet), and Tethys (at right edge of frame). The spacecraft will make its closest approach, 124,200 km. (77,174 miles) abovr the cloud tops, at 3:45 pm PST on Nov. 12, 1980. Nine months later, in August 1981, Voyager 2 will encounter Saturn and then continue on to Uranus.

Jupiter as seen by Voyager 1, mosaic of planet. (JPL ref. No. P-21147)

P-29512 BW Range: 36,000 kilometers (22,000 miles) Miranda, innermost of Uranus' large satellites, is seen at close range as part of a Voyager 2 high-resolution mosaicking sequence. This clear-filter, narrow-angle image shows an area about 250 km (150 mi) across, at a resolution of about 800 meters (2,600 feet). Two distinct terrain types are visible; a rugged, higher-elevation terrain (right) and a lower, striated terrain. Numerous craters on the rugged, higher terain indicate that it is older than the lower terrain. Several scarps, probably faults, cut the different terrains. The impact crater in the lower part of this image is about 25 km (15 mi) across.

Voyager 1 catches volcanic eruption on Jupiter's moon Io JPL ref No. P-21334

Range : 280,000 km. ( 170,000 miles ) P-34726 BW Two 10 minute exposures of Neptune's rings clearly show the two main rings , as well as the inner faint ring and the faint band that extends planetward from roughly halfway between the two bright rings. Both bright rings have material throughout their entire orbit, and are therefore continuous. The inner ring and the broad band are much fainter than the two narrow main rings. These images were taken 1 hour and 27 minutes aprt, using the clear filter on Voyager 2's wide angle camera. These long exposures images were taken while the rings were backlit by the sun. This viewing geometry enhances the visibility of dust and allows optically thinner parts of the rings to be seen. The bright glare in the center is due to overexposure of the crescent of Neptune . The two gaps in the upper part of the outer ring in the image on the left are due to the removal of blemishes during computer processing of the images. Numerous bright stars are evident in the background.

Range : 12 million km (7.5 million miles) Resolution 110 km (68 miles) per pixel. These 2 images of Neptune were taken by Voyager 2's narrow-angle camera. During the 17.6 hours between the left and right images, the Great Dark Spot, at 22 degrees south latitude (left of center), has completed a little less than one rotation of Neptune. The smaller dark spot, at 54 south, completed a little more than one rotation, as can be seen by comparing its relative positions in the two pictures. The Great Dark Spot and the smaller spot have a relative velocity of 100 meters per second (220 miles an hour). The light and dark bands circling Neptune indicate predominantly zonal (east-west) motion. The diffuse white feature north of the Great Dark Spot is near Neptune's equator, and rotates with about the same period as the Great Dark Spot. Streak of bright clouds at the south edge, and just east of the Great Dark Spot, are its constatnt companions, and change the details of their appearance, often within a few hours. Changing brightness of the cloud streaks could be a result of vertical mortions.

Range : 1,450,000 km. ( 900,000 miles ) Jupiter's faint ring system is shown here as two orange lines protrude from the left toward Jupiter's limb. This colorful composite was taken in Jupiter's shadow through orange and violet filters. The colorful images of Jupiter's limb are evidence of the spacecraft motion dering this long exposure. Voyager 2 was about 2 degrees below the plane of the ring when this was shot, leaving the lower ring image cut short by Jupiter's shadow on the ring. (JPL ref No. P-21779)

P-21760 BW This color image of the Jovian moon Europa, which is the size of our moon, is thought to have a crust of ice perhaps 100 kilometers thick which overlies the silicate crust. The complex array of streaks indicate that the crust has been fractured and filled by materials from the interior. The lack of relief, any visible mountains or craters, on its bright limb is consistent with a thick ice crust. In contrast to its icy neighbors, Ganymede and Callisto, Europa has very few impact craters. One possible candidate is the small feature near the center of this image with radiating rays and a bright circular interior. The relative absence of features and low topography suggests the crust is young and warm a few kilometers below the surface. The tidal heating process suggested for Io also may be heating Europa's interior at a lower rate.

P-29502C Range: 1.04 million kilometers (650,000 miles) This color photo of Umbriel, the darkest of Uranus' five large moons was synthesized from frames exposed with the Voyager narrow-angle camera's violet and clear filters and has a resolution of 19 km (12 mi.). Umbriel is characterized by the darkest surface and smallest brightness variations of any of the large satellites of Uranus. As seen here, the surface is also generally gray and colorless. Nevertheless, at this resolution, considerable topographic detail is revealed, showing that Umbriel's surface is covered by impact craters. The brightest spot (shown at top near the equator at approxiamately 270 ° longitude) appears as a bright ring. Its geological significance is not yet understood. Umbriel has a diameter of about 1,200 km (750 miles) and orbits 267,000 km (166,000 mi) from Uranus' center. The satellite's name, from Alexander Pope's 'Rape of the Lock,' means 'dark angel'.

Europa , the smallest of the Galilean satellites, or Moons , of Jupiter , is seen here as taken by Voyager 1. Range : 2 million km (1.2 million miles) is centered at about the 300 degree Meridian. The bright areas are probably ice deposits, while the dark may be rocky surface or areas of more patchy ice distribution. Most unusual features are systems of linear structures crossing the surface in various directions. Of these, some of which are over 1000 km. long , & 2 or 3 hundred km. wide, may be faults which have disrupted the surface.

Resolution : 1 km. ( .6 miles ) Region Shown : 100 km. ( 60 miles ) P-24068C This computer generated photograph was created from a cross-section of Saturn's rings as measured by Voyager 2 photopolarimeter's occulation of the star Delta Scorpii. The region shown is near the inner edge of the Encke Division in the outer part of A-ring. The waves seen at left become successively closer together nearer to the Encke Division. At right are four strands of the ringlet that lies within the Encke Division. Voyager 2's imaging system saw this structure as a single ringlet.

P-34705 This false-color photograph of Neptune was made from Voyager 2 images taken through three filters: blue, green, and a filter that passes light at a wavelength that is absorbed by methane gas. Thus, regions that appear white or bright red are those that reflect sunlight before it passes through a large quantity of methane. The image reveals the presence of a ubiquitous haze that covers Neptune in a semitransparent layer. Near the center of the disk, sunlight passes through the haze and deeper into the atmosphere, where some wavelenghths are absorbed by methane gas, causing the center to appear less red. Near the edge of the planet, the haze scatters sunlight at a higher altitude, above most of the methane, causing the bright red edge around the planet. By measuring haze brightness at several wavelengths, scientists are able to estimate the thickness of the haze and its ability to scatter sunlight. The image is among the last of the full-disk photos that Voyager 2 took before beginning its endless journey into interstellar space.

P-21763 C Range: 1,400,000 kilometers (870,000 miles) Jupiter's thin ring of particles was photographed by Voyager 2's telescope-equipped TV camera through three color filters to provide this color representation. During the three long exposures the spacecraft drifted, smearing out the ring image. The linear feature just above the ring is a star trail. True color of the ring cannot be deduced from this photo.

P-21738 BW Raange: 4.76 million kilometers (2.9 million miles) This Voyager 2 picture of Io was taken in ultraviolet light and shows one of the volcanic eruption plumes first photographed by Voyager 1. (the bright spot on the right limb) The plume is more than 200 kilometers (124 miles) high. The volcano apparently has been erupting since it was observed by Voyager 1 in March, 1979. This suggests that the volcanoes on Io probably are in continuous eruption.

P-29516 BW Range: 125, 000 kilometers (78,000 miles) Voyager 2's wide-angle camera captured this view of the outer part of the Uranian ring system just 11 minutes before passing though the ring plane. The resolution in this clear-filter view is slightly better than 9 km (6 mi). The brightest, outermost ring is known as epsilon. Interior to epsilon lie (from top) the newly discovered 10th ring of Uranus--designated 1986UR1 and barely visible here--and then the delta, gamma and eta rings.

P-34764 Voyager 2 obtained this high resolution color image of Neptune's large satellite Triton during its close flyby. Approximately a dozen individual images were combined to produce this comprehensive view of the Neptune-facing hemisphere of Triton. Fine detail is provided by high resolution, clear-filter images, with color information added from lower resolution frames. The large south polar cap at the bottom of the image is highly refective and slightly pink in color , and may consist of a slowly evaporating layer of nitrogen ice deposited during the previous winter. From the ragged edge of the polar cap northward the satellite's face is generously darker and redder in color. This coloring may be produced by the action of ultraviolet light and magnetospheric radiation upon methane in the atmosphere and surface. Running across this darker region , approximately parallel to the edge of the polar cap, is a band of brighter white material that is almost bluish in color. The underlying topography in this bright band is similiar, however to that in the darker, redder regions surrounding it.

Range : 241,000km (150,600 mi.). This black and white image of Europa, smallest of Jupiter's four Galilean satellites, was acquired by Voyager 2. Europa, the brightest of the Galiliean satellites, has a density slightly less than Io, suggesting it has a substantial quantity of water. Scientists previously speculated that the water must have cooled from the interior and formed a mantle of ice perhaps 100 km thick. The complex patterns on its surface suggest that the icy surface was fractured, and that the cracks filled with dark material from below. Very few impact craters are visible on the surface, suggesting that active processes on the surface are still modifying Europa. The tectonic pattern seen on its surface differs drastically from the fault systems seen on Ganymede where pieces of the crust have moved relative to each other. On Europa, the crust evidently fractures but the pieces remain in roughly their original position.

Range : top- 86,000 miles bottom- 192,000 mi. These two close-ups of Ganymede, the largest of Jupiter's 13 moons, show different views of the largest block of dark, heavily cratered terrain. The bottom image shows objects 3 or 4 miles across, with resolution of about 1.5 miles. The light, linear stripes recurring across the dark region resemble the outer rings of the large ring structure around Callisto. If these features are related to an ancient ring structure formed by a large impact, their small curvature suggests that the original structure was even larger than one seen on Callisto. There is no apparent trace now of the center of this suggested structure, which must have been destroyed by the resurfacing evident over most of Ganymede in the grooved terrain. Another interpretation is that these features are not impact-related rings, but rather internally produced fractures crossing the dark terrain, similiar to the grooved bands.

P-34692 Range : 500 km. ( 300 miles ) Smallest Resolvable Feature : 900 m. or 2,700 ft. Part of Triton's complex geological history canbe seen in this image, shot by Voyager 2. Part of a sequence, this photograph encompasses two depressions, possibly old impact basins, that have been extensively modified by floodind, melting, faulting, and collapse. Several episodes of filling and partial removal of material appear to have occurred. The rough area in the middle of the bottom depression probably marks the most recent eruption of material. Only a few impact craters dot the area, which shows the dominance of internally driven geologic processes on Triton.

P29501C Moon from Voyager 2 Uranus flyby

ref # P-37330 Range : 1.3 million miles This color image of the Earth was obtained by the Galileo spacecraft at about 6:10 am PST. The color composite used images taken through the red, green and violet filters. South America is near the center of the picture, and the white, sunlit continent of Antarctica is below. Picturesque weather fronts are visible in the South Atlantic, lower right. This is the first frame of the Galileo Earth spin movie, a 500-frame time-lapse motion picture showing a 25-hour period of Earth's rotation and atmosphertic dynamics.

P-21751 C Range: 1.2 million kilometers This Voyager 2 color photo of Ganymede, the largest Galilean satellite, shows a large dark circular feature about 3200 kilometers in diameter with narrow closely-spaced light bands traversing its surface. The bright spots dotting the surface are relatively recent impact craters, while the lighter circular areas may be older impact areas. The light branching bands are ridged and grooved terrain first seen on Voyager 1 and are younger than the more heavily cratered dark regions. The nature of the brightish region covering the northern part of the dark circular fature is uncertain, but it may be some type of condensate. Most of the features seen on the surface of Ganymede are probably both internal and external responses of the very thick icy layer which comprises the crust of this satellite.

The bright cirrus-like clouds of Neptune change rapidly, often forming and dissipation over periods of several to tens of hours. In this sequence spanning two rotations of Neptune (about 36 hours) Voyager 2 observed cloud evolution in the region around the Great Dark Spot (GDS) at an effective resolution of about 100 km (62 miles) per pixel. The surprisingly rapid changes which occur over the 18 hours separating each panel shows that in this region Neptune's weather is perhaps as dynamic and variable as that of the Earth. However, the scale is immense by our standards--the Earth and the GDS are of similar size -- and in Neptune's frigid atmosphere, where temperatures are as low as 55 degree Kelvin (-360F), the cirrus clouds are composed of frozen methane rather than Earth's crystalse of water ice.

Range : 1.7 million miles This colorized picture of Venus was taken about 6 days after Galileo's closest approach to the planet. It has been colorized to a bluish hue to emphasize subtle contrasts in the cloud markings and to indicate that it was taken through a violet filter. Features in the sulfuric acid clouds near the top of the planet's atmosphere are most prominent in violet and ultraviolet light. This image shows the east-to-west-trending cloud banding and the brighter polar hoods familiar from past studies of Venus. The features are embedded in winds that flow from east to west at about 230 mph. The smallest features visible are about 45 miles across. An intriguing filamentary dark pattern is seen immediately left of the bright region at the subsolar point (equatorial 'noon'). North is at the top and the evening terminator is to the left.

Range : 40,000 km (24,8000 mi.) This picture of Triton is a mosaic of the highest resolution images taken by Voyager 2. The mosaic is superimposed on the lower-resolution mapping images taken about 2 hours earlier in order to fill in gaps between high-resolution images. The smallest features that can be seen on the images are about 0.8 km (0.5 mi.) across. The terminator (line separation day and night) is at the top of the picture and is centered at about 30 degrees north latitude and 330 degrees longitude. These highest-resolution images were targeted for the terminator region to show details of the topography by the shadows it casts. Near the center of the picture is a depression filled with smooth plains that are probably ices which were once erupted in a fluid state. The depth of the depression is about 300 meters (900 feet) and the prominent fresh impact crater on its floor is about 20 km (12 mi.) in diameter and about 1 km (0.6 mi.) deep. On the right is a elongate crater with adjacent dark deposits about it. This feature may be an explosive eruption vent formed by gaps within the ice. The linear structure on the lest is probably a fracture along which fresh ice has been extruded.

P-21747 C Range: 2,200,000 miles This image shows a region of the Jovian atmosphere from approximately 25° N to the equatorial region. The north temperate jet, at approximately 23° N, where the wind speed is about 150 meters per second, is seen as a dark brown line from the left-hand edge to the right-hand corner of the picture. The wispy clouds of the north equatorial belt appear as shades of brown. The lower right-hand corner of the image shows the brighter (white) clouds of the equatorial region. A small blue area is apparent near the lower edge, which corresponds to a region free of the upper clouds, where it is possible to penetrate to cloud layers approximately 60 kilometers below the visible surface.

JUPITER'S FAINT RING SYSTEM IS SHOWN HERE AS TWO ORANGE LINES PROTRUDE FROM THE LEFT TOWARD JUPITER'S LIMB. THIS COLORFUL COMPOSITE WAS TAKEN IN JUPITER'S SHADOW THROUGH ORANGE AND VIOLET FILTERS. THE COLORFUL IMAGES OF JUPITER'S LIMB ARE EVIDENCE OF THE SPACECRAFT MOTION DERING THIS LONG EXPOSURE. VOYAGER 2

Range : 60,000 miles This image is a false-color version of a near- infrared map of lower-level clouds on the night side of Venus, obtained by the Near Infrared Mapping Spectrometer aboard Galileo. Taken at an infrared wavelength of 2.3 microns (about three times the longest wavelength visible to the human eye) the map shows the turbulent, cloudy middle atmosphere some 30-33 miles above the surface, 6-10 miles below the visible cloudtops. The image shows the radiant heat from the lower atmosphere (about 400 degrees F) shining through the sulfuric acid clouds, which appear as much as 10 times darker than the bright gaps between clouds. The colors indicate relative cloud transparency; white and red show thin cloud regions, while black and blue represent relatively this clouds. This cloud layer is at about 170 degrees F., at a pressure about 1/2 Earth's atmospheric pressure. About 2/3 of the dark hemisphere is visible, centered on longitude 350 West, with bright slivers of daylit high clouds visible at top and bottom left. Near the equator, the clouds appear fluffy and blocky; farther north, they are stretched out into East-West filaments by winds estimated at more than 150 mph, while the poles are capped by thick clouds at this altitude. The Near Infrared Mapping Spectrometer (NIMS) on the Galileo is a combined mapping (imaging) and spectral instrument. It can sense 408 contiguous wavelengths from 0.7 microns (deep red) to 5.2 microns, and can construct a map or image by mechanical scanning. It can spectroscopic-ally analyze atmospheres and surfaces and construct thermal and chemical maps. Designed and operated by scientists and engineers at the JPL, NIMS involves 15 scientists in the US, England and France.

P-29513 BW Range: 31,000 kilometers (19,000 miles) This Voyager 2 image of Miranda was taken shortly before the spacecraft's closet approach to the Uranian moon.The high resolution of 600 meters (2,000 feet) reveals a bewildering variety of fractures, grooves and craters, as well as features of different albedos (reflectances). This clear-filter, narrow-angle view encompasses areas of older, heavily cratered terrain with a wide variety of forms. The grooves and troughs reach depths of a few kilometers and expose materials of different albedos. The great variety of directions of fracture and troughs, and the different densities of impact craters on them, signify a long, complex geologic evolution of this satellite.

Range : 2.52 million miles (1.56 million miles) Resolution : 47km. ( 29 mi.) Closest Approach: 127,000 km. (79,000 mi.) P-29479B/W This Voyager 2 image of the brightest Uranian satellite of the five largest, Ariel, was shot through a clear filter with the narrow angle camera. Ariel is about 1,300 km. ( 800 mi. )in diameter. This image shows several distinct bright areas that reflect nearly 45 % of the incident sunlight. On average, the satellite displays reflectivity of about 25-30 %. The bright areas are probably fresh water ice, perhaps excavated by impacts. the south pole of Ariel is slightly off center of the disk in this view.

This photograph is a Voyager 2 image of one of the moons of Saturn.

Range : 225,000 kilometers (140,625 miles) This image of the Jovian moon Europa was taken by Voyager 2 along the evening terminator, which best shows the surface topography of complex narrow ridges, seen as curved bright streaks, 5 to 10 kilometers wide, and typically 100 kilometers in length. The area shown is about 600 by 800 kilometers, and the smallest features visible are about 4 kilometers in size. Also visable are dark bands, more diffused in character, 20 to 40 kilometers wide and hundreds to thousands of kilometers in length. A few features are suggestive of impact craters but are rare, indication that the surface thought to be dominantly ice is still active, perhaps warmed by tidal heating like Io. The larger icy satellites, Callisto and Ganymede, are evidently colder with much more rigid crusts and ancient impact craters. The complex intersection of dark markings and bright ridges suggest that the surface has been fractured and material from beneath has welled up to fill the cracks.

August 17 to 19, 1989 Range : 11.5 million km (7.1 million mi.) to 7.9 million km (4.9 million mi.) Four black and white images of Neptune's largest satellite, Triton, show it's rotation between the first (upper left) image and the last (lower right). Resolution improves from about 200 km (124 miles) to 150 km (93 miles) per line pair. Triton's south pole lies in the dark area near the bottom of the disk. Dark spots, roughly 1,000 km (620 miles) across, occur near the equator, and show Triton rotation between images. The rotation appears to be synchronous with Triton's 5.88-day orbital period (i.e., Triton rotates on its axis in the same time it revolves around Neptune.) The spots' constant rotation rate and their visibility near the edge of the disk suggest the spots are surface features. Whatever atmosphere is present on Triton appears transparent enough that Voyager 2's cameras can see through it.

Range : 34 million km. ( 21.1 million miles) P-22993C This Voyager 1 photograph of Saturn was taken on the last day it could be captured within a single narrow angle camera frame as the spacecraft neared the planet for it's closest approach on Nov. 12, 1980. Dione, one of Saturn's innermost satellites, appears as three color spots just below the planet's south pole. An abundance of previously unseen detail is apparent in the rings. For example, a gap in the dark, innermst ring, C-ring or Crepe Ring, is clearly shown. Also, material is seen inside the relatively wide Cassini Division, seperating the middle, B-ring from the outermost ring, the A-ring. The Encke division is shown near the outer edge of A-ring. The detail in the ring's shadows cast on the planet is of particular interest. The broad dark band near the equator is the shadow of B-ring. The thinner, brighter line just to the south is the shadow of the less dense A-ring.

(P-19180) Galileo Probe descending into Jupiters atmosphere (artwork)

P-29520 BW Range: 130,000 kilometers (80,000 miles) This mosaic, taken through the clear-filter, narrow-angle camera, of the four highest-resolution images of Ariel represents the most detailed Voyager 2 picture of this satellite of Uranus. Ariel is about 1,200 km (750 mi) in diameter; the resolution here is 2.4 km (1.5 mi). Much of Ariel's surface is densely pitted with craters 5 to 10 km (3 to 6 mi) across. These craters are close to the threshold of detection in this picture. Numerous valleys and fault scarps crisscross the highly pitted terrain. voyager scientists believe the valleys have formed over down-dropped fault blocks (graben); apparently, extensive faulting has occured as a result of expansion and stretching of Ariel's crust. The largest fault valleys, near the terminator at right, as well as a smooth region near the center of this image, have been partly filled with deposits that are younger and less heavily cratered than the pitted terrain. Narrow, somewhat sinuous scarps and valleys have been formed, in turn, in these young deposits. It is not yet clear whether these sinuous features have been formed by faulting or by the flow of fluids.

Range : 1.2 million kilometers (750,000 miles) This picture of Io is one of the last sequence of 'volcano watch' pictures planned as a time lapse study of the nearest of Jupiter's Galilean satellites. The sunlit crescent of Io is seen at the left, and the night side illuminated by light reflected from Jupiter can also be seen. Three volcanic eruption plumes are visible on the limb. All three were previously seen by Voyager 1. On the bright limb Plume 5 (upper) and Plume 6 (lower) are about 100 km high, while Plume 2 on the dark limb is about 185 km high and 325 km wide. The dimensions of Plume 2 are about 1 1/2 times greater than during the Boyager 1 encounter, indicating that the intensity of the eruptions has increased during the four-month time interval between the Boyager encounters. The three volcanic eruptions and at least three others have apparently been active at roughly the same intesity or greater for a period of at least four months.

P-29511 BW Range: 130,000 kilometers (80,000 miles) This clear-filter, narrow-angle picture is part of the high-resolution Voyager 2 imaging sequence of Ariel, a moon of Uranus about 1,300 kilometers (800 miles) in diameter. The complexity of Ariels' surface indicates that a variety of geologic processes have occured. The numerous craters, for example, are indications of an old surface bombarded by meteroids over a long periond. Also conspicuous at this resolution, about 2.4 km (1.5 mi), are linear grooves (evidence of tectonic activity that has broken up the surface) and smooth patches (indicative of deposition of material).

This image is the first full picture showing both asteroid 243 Ida and its newly discovered moon to be transmitted to Earth from NASA's Galileo spacecraft--the first conclusive evidence that natural satellites of asteroids exist. Ida is the large object to the left, about 56 kilometers (35 miles long). Ida's natural satellite is the small object to the right. This portrait was taken by Galileo's charge-coupled device (CCD) camera on August 28, 1993, about 14 minutes before the spacecraft's closest approach to the asteriod, from a range of 10,870 kilometers (6,755 miles). Ida is a heavily cratered, irregularly shaped asteroid in the main asteroid belt between Mars and Jupiter-- the 243rd asteroid to be discovered since the first one was found at the beginning of the 19th century. It is a member of a group of asteroids called the Koronis family. The small satellite, which is about 1.5 kilometers (1 mile) across in this view, has yet to be given a name by astronomers. It has been provisionally designated '1993 (243) 1' by the International Astronomical Union. (The numbers denote the year the picture was taken, the asteroid number and the fact that it is the first moon of Ida to be found.) ALthough the satellite appears to be 'next' to Ida it is actually slightly in the foreground, closer to the spacecraft than Ida. Combining this image with data from Galileo's near-infrared mapping spectrometer, the science team estimates that the object is about 100 kilometers (60 miles) away from the center of Ida. This image is one of a six-frame series taken through different color filters, this one in green. The spatial resolution in this image is about 100 meters (330 feet) per pixel. The Galileo spacecraft flew past Ida en route to its final destination, Jupiter, where it will go into orbit in December 1995. The Jet Propulsion Laboratory manages the galileo Project for NASA's Office of Space Science. (JPL ref. No. P-43731)

P-29518 BW Range: 130,000 kilometers (80,000 miles) This highest-resolution Voyager 2 view of Ariel's terminator shows a complex array of transecting valleys with superimposed impact craters. This clear-filter, narrow-angle view has a resolution of about 2.4 km (1.5 mi). Particularly striking to Voyager scientists is the fact that the faults that bound the linear valleys are not visible where they transect one another across the valleys. Apparently these valleys were filled with deposits sometime after they were formed by tectonic processes, leaving them flat and smooth. Sinuous rilles (trenches) later formed, probably by some flow process. Some type of fluid flow may well have been involved in their evolution.

Range : 530,000 km (330,000 mi.) This color photo of Neptune's large satellite Triton has a resolution of about 10 km (6.2 mi), sufficient to begin to show topographic detail. The image was made from pictures taken through the green, violet and ultraviolet filters. In this technique, regions that are highly reflective in the ultraviolet appear blue in color. In reality, there is no part of Triton that would appear blue to the eye. The bright southern hemisphere of Triton, which fills most of this frame, is generally pink in tone as is the even brighter equatorial band. The darker regions north of the equator also tend to be pink or reddish in color.

Range : 1,094,666 km (677,000 mi.) This false color picture of Callisto was taken by Voyager 2 and is centered on 11 degrees N and 171 degrees W. This rendition uses an ultraviolet image for the blue component. Because the surface displays regional contrast in UV, variations in surface materials are apparent. Notice in particular the dark blue haloes which surround bright craters in the eastern hemisphere. The surface of Callisto is the most heavily cratered of the Galilean satellites and resembles ancient heavily cratered terrains on the moon, Mercury and Mars. The bright areas are ejecta thrown out by relatively young impact craters. A large ringed structure, probably an impact basin, is shown in the upper left part of the picture. The color version of this picture was constructed by compositing black and white images taken through the ultraviolet, clear and orange filters.

Range : 350,000 miles This image of the western hemisphere of the Moon was taken through a green filter by Galileo at 9:35 am PST. In the center is the Orientale Basin, 600 miles in diameter, formed about 3.8 billion years ago by the impact of an streroid-size body. Orientale's dark center is a small mare. To the right is the lunar near side with the great, dark Oceanus Procellarum above and the small, circular, dark Mare Humorum Below. Maria are broad plains formed mostly over 3 billion years ago as vast bassaltic lava flows. To the left is the lunar far side with fewer maria, but, at lower left, the South-Pole-Aitken basin, about 1200 miles in diameter, which resemble Orientale but is much older and more weathered and battered by cratering. The intervening cratered highlands of both sides, as well as the maria, are dotted with bright, young craters. This image was 'reprojected' so as to center visibility of small features.

Voyager 1 catches volcanic eruption on Jupiter's moon Io JPL - no available

P-21742 BW Range: 6 million kilometers (3.72 million miles) This Voyager 2 image shows the region of Jupiter extending from the equator to the southern polar latitudes in the neighborhood of the Great Red Spot. A white oval, different from the one observed in a similiar position at the time of the Voyager 1 encounter, is situated south of the Great Red Spot. The region of white clouds now extends from east of the red spot and around its northern boundary, preventing small cloud vortices from circling the feature. The disturbed region west of the red spot has also changed since the equivalent Voyager 1 image. It shows more small scale structure and cloud vortices being formed out of the wave structures.

Saturn and it's rings, with callouts, as photographed by Voyager 2

This image of the crescent moon was obtained by the Galileo Solid-State Imaging System, taken at 5 am PST as the spacecraft neared Earth. The image was taken through a green filter and shows the western part of the lunar near side. The smallest features visible are 8 km (5 mi) in size. Major features visible include the dark plains of Mare Imbrium in the upper part of the image, the bright crater Copernicus (100 km, 60 miles in diameter) in the centeral part, and the heavily cratered lunar highlands in the bottom of the image. The landing sides of the Apollo 12,14 and 15 missions lie within the central part of the image. Samples returned from these sites will be used to calibrate this and accompanying images taken in different colors, which will extend the knowledge of the spectral and compositional properties of the near side of the moon, seen from Earth, to the lunar far side.

Range : 7 million kilometers (4.3 million miles) Io is Jupiter's innermost of the four Galilean satellites. Photo taken at 2:00 AM through an ultraviolet filter. The photo's background is part of Jupiter's disk. North is at the top and the central longitude of Io is 180 degrees. Io shows a contrasting surface with dark polar areas and many light and dark regions around the equator. This resolution of about 100 miles/160 kilometers, no topographic features, like craters, can be seen. The brighter regions may be areas containing sulfur and various salts, making Io very reflective(six times brighter thanb Earth's Moon). Io is about the same size and density as our Moon, but has followed a different evolutionary path, influenced by its closeness to Jupiter and the intense bombardment it receives from the Jovian radiation belts of energetic charged particles.

Range : 1 illion km. ( 600,000 mi. ) Resolution : 140 km. ( 90 mi. ) P-29539C This Voyager 2 image of Uranus was captured as the spacecraft was leaving Uranus behind on its cruise to Neptune. The image is a color composite of three photographs taken through blue, grren, and orange filters. Thin thin crecent seen here is at an angle of 153 degrees between the the spacecraft, the planet, and the sun. Even at this extreme angle, uranus retains the pale blue-green color seen by the ground based astronomers and recorded by Voyager 2 during its historic encounter, this color results from the presence of methane in Uranus' atmosphere. The gas absorbs red wavelengths of light, leaving the predominant hue seen here. The tendency for the cresent to become white at the extreme edge is cased by the presence of a high-altitude haze. Voyager 2, having encountered Jupiter in 1979, Saturn in 1981, and Uranus in 1986, will proceed on its jouney to Neptune. Closest approach is scheduled for August 24, 1989.

This picture of Neptune was produced from images taken through the ultraviolet, violet and green filters of the Voyager 2 wide-angle camera. This 'false' color image has been made to show clearly details of the cloud structure and to paint clouds located at different altitudes with different colors. Dark, deeplying clouds tend to be masked in the ultraviolet wavelength since overlying air molecules are particularly effective in scattering sunlight there which brightens the sky above them. Such areas appear dark blue in this photo. The Great Dark Spot (GDS) and the high southern latitudes have a deep bluish cast in this image, indication they are regions where visible light (but not ultraviolet light) may penetrate to a deeper layer of dark cloud or haze in Neptune's atmosphere. Conversely, the pinkish clouds may be positioned at high altitudes.

P-29522BW Range: 369,000 kilometers (229,000 miles) This is the highest-resolution picture of Titania returned by Voyager 2. The picture is a composite of two images taken through the clear-filter of Voyager's narrow-angle camera. The resolution of this image is 13 km (8 mi). Titania is the largest satellite of Uranus, with a diameter of little more than 1,600 km (1,000 mi). Abundant impact craters of many sizes pockmark the ancient surface. The most prominant features are fault valleys that stretch across Titania. They are up to 1,500 km (nearly 1,000 mi) long and as much as 75 km (45 mi) wide. In valleys seen at right center, the sunward-facing walls are very bright. While this is due partly to the lighting angle, the brightness also indicates the presence of a lighter material, possibly young frost deposits. An impact crater more than 200 km (125 mi) in diameter distinguishes the very bottom of the disk; the crater is cut by a younger fault valley more than 100 km (60 mi) wide. An even larger impact crater, perhaps 300 km (180 mi) across, is visible at top.

P-21746 BW Range: 390,000 kilometers (245,000 miles) This photomosaic of Callisto is composed of nine frames. The impact crater distribution is very uniform across the disk. Notable are the very bright rayed craters that probably are very young. Near the limb is a giant probable impact structure. Several large structures were discovered by Voyager 1. This one is smaller than the largest one found by Voyager 1 but is more clearly shown. About 15 concentric rings surround the bright central spot. Many hundreds of moderate sized impacts are also seen, a few with bright radial ray patterns. The limb is very smooth confirming that no high topography has been seen on the satellite, and observation consistent with its icy composition.

Voyager 1 views of Jupiter's rings

As Voyager 1 approches Jupiter three of its moons can be seen JPL ref. No. C-206

P-34648 This photograph of Neptune was reconstructed from two images taken by Voyager 2's narrow angle camera, through the green and clear filters. the image shows three of the features that Voyager 2 has been photographing during recent weeks. At the north ( top ) is the Great Dark Spot, accompanied by bright, white clouds that undergo rapid changes in appearance. to the south of the Great Dark Spot is the bright feature that Voyager scientists have nicknamed 'Scooter.' Still farther south is the feature called ' Dark Spot 2,' which has a bright core. Each feature moves eastward at a different at a different velocity, so it is only occasionally that they appear close to each other, such as at the time this picture was taken.

Range : 7 million kilometers (5 million miles) Callisto is Jupiter's outermost Galilean satellites and darkest of the four(but almost twice as bright as Earth's Moon). Mottled appearance from bright and dark patches. Bright spots seem like rayed or bright halved craters seen on our Moon. This face is always turned toward Jupiter. Photo taken through violet filter. Ganymede is slightly larger than Mercury but much less dense (twice the density of water). Its surface brightness is 4 times of Earth's Moon. Mare regions (dark features) are like the Moon's but have twice the brightness, and believed to be unlikely of rock or lava as the Moon's are. It's north pole seems covered with brighter material and may be water frost. Scattered brighter spots may be related to impact craters or source of fresh ice.

Range : 5 to 6.1 million km. ( 3.1-.8 million miles ) P-29314B/W This 'family portrait' of Uranus' five largest moons was compiled from images sent back from Voyager 2 The photographs were taken through a clear filter.

P-21744 C Range: 4.2 million kilometers (2.6 million miles) In this image of Europa acquired by Voyager 2, global scale dark streaks are becoming visible. Europa, the size of the earth's moon, is apparently covered by water ice as indicated by ground based spectrometers and its brightness. The central longitude of this view is 235° west. Bright rayed impact craters which are abundant on ancient Ganymede and Callisto would easily be visible at this range. The suggestion is that Europa's surface is young and that the streaks are reflections of currently active internal dynamic processes.

Range : 5.4 million km (3.3 million miles) Features as small as 100 km (62 miles) across can be seen in this color image of Neptune's satellite Triton, photographed by Voyager 2. Triton's overall pinkish color may be due to reddish materials produced by irradiation of methane gas and ice on the satellite. The dark areas near the top of the image seem to be part of a belt of dark markings observed near Trition's equator at different longitudes. Generally, darker areas on Triton appear to be somewhat redder in color than brighter areas. The central longitude in the image is 123 degrees. Here the south pole is at about 6 o'clock, approximately 1/6th of the way up from the bottom. The color image was made from three black-and-white frames, taken through clear, violet and green filters.

Range : 4.2 million km. ( 2.6 million miles ) P-34649 This photograph of Neptune's southern hemisphere taken by Voyager 2's narrow angle camera, through the green and clear filters. The smallest feature that can be seen are 38 km ( 24 miles ) across. the almond shaped structure at the left is a large cloud system that has been seen for several weeks. Internal details in the feature have become increasingly apparent as Voyager 2 has approached. Systems with similiar shapes in Jupiter's atmosphere rotate about their centers, rolling in the local winds that increase toward the south. However, the wispy nature of the white central clouds in this Neptunian feature make confirmation of the syste.m's rotation difficult

P-21752 C Range: 1.2 million kilometers This image of Europa shows detail about 20 kilometers across and is somewhat higher resolution than the best Voyager 1 image. The part of Europa shown is the hemisphere that will be viewed at even higher resolution during another Voyager 2 encounter with Europa. Color reconstruction in this image was slightly enhanced to bring out detail in the complicated mottled region on the west limb, containing some of the linear fracture-like features discovered by Voyager 1. The regions in the north and south polar areas which appear bluish in this version are in fact white.

Range : 6.5 million kilometers (4 million miles) Six violet images of Jupiter makes the mosaic photo, showing the Great Red Spot as a swirling vortex type motion. This motion is also seen in several nearby white clouds. These bright white clouds and the Red Spot are rotating in a counter clockwise direction, except the peculiar filimentary cloud to the right of the Red Spot is going clockwise. The top of the picture shows the turbulence from the equatorial jet and more northerly atmospheric currents. The smallest clouds shown are only 70 miles (120 km) across.

Range : 4.3 million km. ( 2.7 million miles ) This photograph taken from Voyager I shows Jupiter's Great Red Spot and one of the white ovals seen from Earth . These white ovals were seen to have formed in 1939 & 1940, and have remained somewhat consistant since. The Great Red Spot is three times the size of the Earth. This photograph represents the finnest detail seen to date, with the smallest details being 80 km. ( 45 miles ) across.

P-34630 Range: 10.5 million kilometers (6.5 million miles) This cylindrical projection view of Neptune uses five narrow-angle images equally spaced around the planet. They were taken by Voyager 2 over the course of a Neptunian day, an interval of about 18 hours. Latitude lines are horizontal in the image, and range from 80 degrees south to 30 degrees north of the equator. Near the center, the Great Dark Spot leaves a disturbed wave-like pattern that stretches around Neptune. Features further south move eastward at speeds up to 400 mph relative to the Great Dark Spot. The features are storms--moving cloud systems that persist for months or longer. The weather forecast for Neptune is therefore continued high winds and cold with little change in temperature.

Range : 1 million kilometers Voyager 2 completed a dramatic 10 hour time lapse photo sequence to monitor the active volcanos on Jupiter's moon Io following the spacecraft's closest approach to Jupiter. This picture is one of about 200 images that will be used to generate a time lapse motion picture to illustrate Io's volcanic activity. On the bright limb, two of the plumes (P-5 & P-6) discovered in March by Voyager 1 are again visible. The plumes are spewing materials to a height of about 100 kilometers.

P-34707 Range: 720,000 kilometers (446,400 miles) The Voyager spacecraft took this picture after closest approach to Neptune using the clear filter of the wide-angle camera with an exposure time of 255 seconds. The view back towards Neptune at a phase angle of 135° found the two known rings to be five to ten times brighter than seen in backscattering during Voyager approach at a much lower phase angle. This brightness increase implies a large percentage of microscopic particles within the rings. Although the dominant arc-like clump of the outer ring is not seen here, the inner ring appears brighter than the outer ring at the longitudes seen in this image. A faint sheet of material is also revealed that extends from the faint ring at a radius of 53,200 kilometers (33,000 miles). A new and even fainter ring was also discovered in this image at about 41,000 kilometers (25,400 miles), seen running from the lower left corner to about one-third the way across the top of the frame. This ring is quite broad, about 2,500 kilometers (1,550 miles) in radial width. In contrast to the two previously discovered rings, this feature is quite diffuse and has no well defined radial boundaries.