 
2/5/79 28.4 million km (17.6 million mi) Jupiter is the largest planet in our solar system, with a diameter 11 times that of Earth. Jupiter rotates very quickly, making one full rotation in just under ten hours. Composed primarily of hydrogen and helium, Jupiter’s colorfully banded atmosphere displays complex patterns highlighted by the Great Red Spot, a large, circulating atmospheric disturbance. Three of Jupiter’s 13 known satellites are also visible in this Voyager 1 photograph. The innermost large satellite, Io, can be seen in front of Jupiter and is distinguished by its bright, orange surface. To the right of Jupiter is Europa, also very bright but with fainter surface markings. Callisto is barely visible beneath Jupiter. These satellites orbit Jupiter in the equatorial plane and appear in their present position because Voyager is above the plane. Jupiter’s atmosphere is undergoing constant change, presenting an ever-shifting face to observers. The Great Red Spot has undergone three major periods of activity in the last 15 years. These images of Jupiter, taken by Voyager 1 (top) and Voyager 2 (bottom) almost four months apart, show that cloud movement in the Jovian atmosphere is not uniform because wind speeds vary at different latitudes. For example, the white ovals which appear below the Great Red Spot dramatically shifted between January and May, the time interval between these two pictures. The bright “tongue” extending upward from the Great Red Spot interacted with a thin, bright cloud above it that had traveled twice around Jupiter in four months. Eddy patterns to the left of the Great Red Spot, which have been observed since 1975, appear to be breaking up. 1/24/79 40 million km (25 million mi) 5/9/79 46.3 million km (28.7 million mi) 2/25/79 9.2 million km (5.7 million mi) The Great Red Spot on Jupiter is a tremendous atmospheric storm, twice the size of Earth, that has been observed for centuries. The Great Red Spot rotates counterclockwise with one revolution every six days. Wind currents on the top flow east to west, and currents on the bottom flow west to east. This Voyager 1 picture shows the complex flow and turbulent patterns that result from the Great Red Spot’s interactions with these flows. The large white oval is a similar, but smaller, storm center that has existed for about 40 years. 7/3/79 6 million km (3.72 million mi) A comparison of the Voyager 2 photograph above with the preceding Voyager 1 photograph shows several distinct changes in the Jovian atmosphere around the Great Red Spot. The white oval beneath the Great Red Spot in the first picture has moved farther around Jupiter, and a different white oval has appeared under the Great Red Spot in the Voyager 2 picture taken four months later. The disturbed cloud regions around the Great Red Spot have noticeably changed, and the white zone west of the Great Red Spot has narrowed. 3/2/79 4 million km (2.5 million mi) High-speed wind currents in the mid-latitudes of Jupiter are shown in this high-resolution Voyager 1 photograph. The pale orange line running diagonally to the upper right is the high-speed north temperate current with a wind speed of about 120 meters per second (260 miles per hour), over twice as fast as severe hurricane winds on Earth. Toward the top of the picture, a weaker jet of approximately 30 meters per second (65 miles per hour) is characterized by wave patterns and cloud features that rotate in a clockwise manner. 3/2/79 4 million km (2.5 million mi) The large brown-colored oval appearing in this Voyager 1 picture was selected as one of the targets to be photographed near closest approach to Jupiter because it is probably an opening in the upper cloud deck that exposes deeper, warmer cloud levels. Brown ovals (which can also be seen in the preceding and following photographs) are common features in Jupiter’s northern latitudes and have an average lifetime of one to two years. 6/28/79 10.3 million km (6.4 million mi) Jupiter’s Equatorial Zone is the broad, orange band that traverses the center of this Voyager 2 picture. This zone is characterized by the wispy clouds along its northern edge. The brown oval was observed by Voyager 1 four months earlier, illustrating the stability of this type of feature in the Jovian atmosphere. In contrast, the turbulent region in the lower right of the picture, which lies just to the left of the Great Red Spot, shows features that are relatively short lived. With the exception of the cooler Great Red Spot, as colors range from white to orange to brown, we are generally looking at deeper and warmer layers in the Jovian atmosphere. This infrared image of Jupiter was taken from Earth and shows heat radiating from deep holes in Jupiter’s clouds. Bright areas in the image are higher temperature regions than the dark areas and correspond to parts of the atmosphere that are relatively free of obscuring clouds. The Great Red Spot appears on the left limb, or edge of the planet, as a dark area encircled by a bright ring, indicating that the Spot is cooler than the surrounding region. The infrared image was recorded by the 200-inch Hale telescope on Mount Palomar in California. 1/10/79 535,000 km (332 million mi) This Voyager 1 picture was also taken the same day, about one hour after the infrared image. 3/5/79 515,000 km (320,000 mi) The largest aurora ever observed, nearly 29,000 kilometers (18,000 miles) long, appears in this Voyager 1 photograph, taken on the dark side of Jupiter six hours after closest encounter. The auroral lights are brighter than any northern lights seen on Earth. Jupiter’s north pole is approximately midway along the auroral arc. This timed exposure of the aurora also shows what appear to be lightning storms several thousand kilometers below the aurora. The strength of the lightning bolts is comparable to that of superbolts seen near cloud tops above Earth. Lightning had been suspected to exist on Jupiter, but at lower levels in the atmosphere. 3/4/79 1.2 million km (750,000 mi) The first evidence of a ring around Jupiter is seen in this photograph taken by Voyager 1. This photograph was part of a sequence planned to search for such rings around Jupiter. The multiple image of the extremely thin, faint ring appears as a broad light band crossing the center of the picture. This multiple image and the elongated, wavy motion of the background stars are due to the 11-minute, 12-second exposure and the very slow natural oscillation of the spacecraft. The ring, which is in Jupiter’s equatorial plane, is invisible from Earth because of its thinness and transparency and because of Jupiter’s brightness. The black dots in the picture are calibration points in the camera. Because of Voyager 1’s discovery of a ring around Jupiter, Voyager 2 was programmed to take additional pictures of the ring. These three Voyager 2 images show Jupiter’s ring in progressively higher resolution. The pictures were taken when Jupiter was eclipsed by the Sun, and the ring appears unusually bright because of the forward scattering of sunlight by small ring particles. 7/10/79 1.45 million km (900,000 mi) In this four-picture mosaic, the arms of the ring curving toward the spacecraft (on the near side of the planet) are cut off by the planet’s shadow. Scientists estimate that the distance from the Jovian cloud tops to the outer edge of the ring is 55,000 kilometers (35,000 miles). 7/10/79 1.55 million km (961,000 mi) In this picture, which is composed of six images, there is evidence of structure within the ring, but the spacecraft motion during these long exposures obscured the highest resolution detail. However, there is speculation that the ring width, estimated at 6000 kilometers (4000 miles), contains more than one ring. 7/10/79 1.45 million km (900,000 mi) This photograph is an enlargement of the isolated left frame in the first picture and reveals a density gradient of very small particles extending inward from the ring. The thickness of the ring has been estimated at less than one kilometer (0.6 mile) although the ring appears about 30 kilometers (19 miles) thick in the image, due to camera motion and finite resolution. Composition of the low-albedo (dark) particles is not known, but particle size probably ranges from microscopic to at most a few meters in diameter. If collected together to form a single body, the total mass of the Jovian rings would form an object with a diameter less than twice that of tiny Amalthea. 2/13/79 20 million km (12.4 million mi) Jupiter and two of its planet-sized satellites, Io at left and Europa at right, are visible in this Voyager 1 picture. Jupiter’s four largest satellites—Io, Europa, Ganymede and Callisto—were discovered in 1610 by Galileo Galilei. The two outer Galilean satellites are Ganymede and Callisto, not shown in this picture. All four satellites probably formed about four billion years ago but their surfaces vary in age tremendously. Io and Europa have younger, more active surfaces than Ganymede and Callisto. Like our Moon, the satellites keep the same face toward Jupiter. In this picture, the sides of the satellites that always face away from the planet are visible. Amalthea, Jupiter’s innermost satellite, was discovered in 1892. It is so small and close to Jupiter that it is extremely difficult to observe from Earth. Amalthea’s surface is dark and red, quite unlike any of the Galilean satellites. The three Voyager 1 pictures and the one Voyager 2 picture following (seen against the disk of Jupiter) reveal a small, elongated object, about 265 kilometers (165 miles) long and 150 kilometers (90 miles) in diameter. Amalthea keeps its long axis pointed toward Jupiter as it orbits around the planet every 12 hours. 3/4/79 1.25 million km (780,000 mi) 3/4/79 695,000 km (430,000 mi) 3/5/79 425,000 km (264,000 mi) 7/9/79 560,000 km (350,000 mi) Amalthea was observed end-on in the Voyager 2 picture, which has been computer-processed to enhance the image. 3/4/79 377,000 km (234,000 mi) Io, Jupiter’s innermost Galilean satellite, displays great diversity in color and brightness. This Voyager 1 four-picture mosaic shows Io’s complex coloration of red-orange, black, and white regions, and the two major topographic features: volcanic regions, the most prominent of which is the “hoofprint” (volcanic deposition feature) in the center-right, and the intervolcanic plains that are relatively featureless. Io’s vivid coloring is probably due to its composition of sulfur-rich materials that have been brought to the surface by volcanic activity. 3/5/79 129,600 km (80,500 mi) The bright area at the upper right in this Voyager 1 picture of Io appears to be a caldera (collapsed volcano) that is venting clouds of gases. The clouds may condense to form extremely fine particles that scatter light and appear blue. Because the infrared spectrometer discovered sulfur dioxide on Io, scientists believe this gas may be the main component of the clouds. Sulfur dioxide clouds would rapidly freeze and snow back to the surface. It is also possible that dark areas in the floors of the calderas are pools of encrusted liquid sulfur. 3/5/79 66,000 km (41,000 mi) Evidence of erosion in Io’s southern polar region is visible in this Voyager 1 high-resolution image. The picture has been computer-enhanced to bring out surface detail while suppressing bright markings. A depressed segment of the crust, bounded by faults, is seen near the terminator in the upper right portion of the image. At the lower center are complicated scarps (slopes) and portions of isolated elevated terrain that geologists interpret as “islands” left behind as the scarps eroded. Scientists speculate that sulfur dioxide (as a subsurface liquid) may be a determinant in the creation of these features. 3/4/79 862,000 km (540,000 mi) Io’s surface, less than ten million years old, is quite young compared to the other Galilean satellites and to other terrestrial bodies, such as Mercury and the Moon. The surface is composed of large amounts of sulfur and sulfur dioxide frost, both of which account for most of the surface color. This picture was taken by Voyager 1. Material deposited by the volcano (see following pictures) can be seen as a white ring near the center of Io. The first active volcanic eruptions other than on Earth were discovered on Io. These volcanoes are extremely explosive with ejection velocities of more than one kilometer per second (2200 miles per hour), which is more violent than Etna, Vesuvius, or Krakatoa on Earth. Both pictures below were taken by Voyager 1. 3/4/79 450,000 km (280,000 mi) In this picture, the plume visible on the right edge extends more than 100 kilometers (60 miles) above the surface. 3/4/79 499,000 km (310,000 mi) The same volcano is shown in this picture, photographed one hour and 52 minutes earlier. 3/4/79 490,000 km (304,000 mi) Special color reconstruction by means of ultraviolet, blue, green, and orange filters allowed scientists to study the amount of gas and dust and the size of the dust particles that erupted from the volcano on Io shown in this Voyager 1 image. The region that is brighter in the ultraviolet (blue area) is about 210 kilometers (130 miles) high, over twice the height of the denser, bright yellow core. The vent area is visible on page 18 as a dark ring in the upper left region of Io. 7/10/79 1.2 million km (750,000 mi) Of the eight active volcanoes discovered on Io by Voyager 1, six of the seven volcanoes sighted by Voyager 2 were still active. The giant volcano observed by Voyager 1 over the “hoofprint” region (see page 18) had become inactive. Scientists, therefore, believe that the satellite is undergoing continuous volcanic activity, making Io’s surface the most active in the solar system. This Voyager 2 photograph, which shows three active volcanoes, was one of the last of an extensive sequence of “volcano watch” pictures planned as a result of Voyager 1’s volcano discovery. The black dots are calibration points on the camera. 7/8/79 1.2 million km (750,000 mi) Europa, approximately the same size and density as our Moon, is the brightest Galilean satellite. The surface displays a complex array of streaks, indicating that the crust has been fractured. In contrast to its icy neighbors Ganymede and Callisto, Europa has very few impact craters. The relative absence of features and low topography indicate that the crust is young and probably warm a few kilometers below the surface. The warmth is probably due to a combination of radioactive and tidal heating. The tidal heating within Europa is estimated to be ten percent that of the stronger tidal heating effect within Io. The regions that appear blue in this Voyager 2 image are actually white. 7/9/79 240,000 km (150,000 mi) Europa’s surface is probably a thin ice crust overlying water or softer ice (slush) about 100 kilometers (60 miles) thick that covers a silicate interior. The tectonic processes on Europa’s surface create patterns that are drastically different from the fault systems seen on Ganymede’s surface, where pieces of the crust have moved relative to each other. On Europa, the crust evidently fractures, but the pieces remain roughly in their original position. This Voyager 2 picture is composed of three images. 7/9/79 240,000 km (150,000 mi) Long linear fractures or faults which crisscross Europa’s surface in various directions are over 1000 kilometers (600 miles) long in some places. Large fractures are 200 to 300 kilometers (125 to 185 miles) wide, wider than the crust is thick. Also visible are somewhat darker mottled regions that appear to have a slightly pitted appearance. No large craters (more than five kilometers in diameter) are identifiable in this Voyager 2 picture, indicating that this satellite has a very young surface relative to Ganymede and Callisto, although perhaps not as young as Io’s surface. Scientists believe that the surface is a thin ice crust overlying water or softer ice and that the fracture systems are breaks in the crust. Resurfacing processes, such as the production of fresh ice or snow along the cracks and cold glacier-like flows, have probably removed evidence of impact events (cratering). Europa, therefore, appears to have many properties similar to Ganymede and Io. 7/9/79 240,000 km (150,000 mi) Complex narrow ridges, seen as curved bright streaks 5 to 10 kilometers (3 to 6 miles) wide and typically 100 kilometers (60 miles) long, characterize the surface topography of this view of Europa. The dark bands also visible in this Voyager 2 photo are 20 to 40 kilometers (12 to 25 miles) wide and up to thousands of kilometers long. The fractures on the icy surface are filled with material from beneath, probably as a result of internal tidal flexing which continually heats the thin outer ice crust. A few features are suggestive of degraded impact craters. 3/4/79 2.6 million km (1.6 million mi) Ganymede, Jupiter’s largest satellite, is about one and one-half times the size of our Moon but only about half as dense and is composed of about 50 percent water or ice and the rest rock. The bright surface of Ganymede is a complex montage of ancient, relatively dark and cratered terrain, grooved terrain that resulted from a dramatic history of tectonic movement in the icy crust, and bright young ray craters that expose fresh ice. This photograph was taken by Voyager 1. 7/7/79 1.2 million km (750,000 mi) The dark, cratered, circular feature in this Voyager 2 photograph is about 3200 kilometers (2000 miles) in diameter and is on the side of Ganymede opposite to that shown in the previous picture. This region is apparently the largest piece of ancient, heavily cratered crust left on Ganymede. The light branching bands are ridged and grooved terrain which are younger than the more heavily cratered dark regions. Despite the dramatic surface appearance, Ganymede is relatively devoid of topographic relief due to the consequences of glacier-like “creep” in the icy crust. 7/8/79 312,000 km (194,000 mi) Several different types of terrain common to Ganymede’s surface are visible in this Voyager 2 picture. The boundary of the largest region of dark ancient terrain (also shown in the previous photo) can be seen to the right, revealing the light linear features that may be the remains of shock rings from an ancient impact. The broad light regions are the typical grooved structures contained within the light regions on Ganymede. On the lower left is another example of what might be evidence of large-scale lateral faulting in the crust; the band appears to be offset by a linear feature perpendicular to it. These are the first clear examples of lateral faulting seen on any planet other than Earth. 7/8/79 313,000 km (194,500 mi) This color reconstruction of part of Ganymede’s northern hemisphere, taken by Voyager 2, encompasses an area about 1300 kilometers (800 miles) across. It shows part of a dark, densely cratered region that contains numerous craters, 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 the flow of icy material near the surface. The gradually curving lines that press through the dark region suggest the presence of a large impact basin to the southwest, which has been obliterated by the subsequent formation of younger grooved terrain. 3/5/79 165,000 km (103,000 mi) A broad, north-south strip of grooved terrain on Ganymede, offset by a traversing fault in the upper part of the picture, is shown in this Voyager 1 photograph. There are several other perpendicular fault lines farther down on the fault. Within the major light stripes, the more closely spaced, shallow grooves run parallel to the boundaries of the stripes. The larger striped features divide the cratered terrain into isolated polygons several hundred to about 1000 kilometers (600 miles) across. 3/5/79 145,000 km (90,000 mi) The grooved terrain at higher resolution emphasizes numerous interwoven linear features in this Voyager 1 picture, near the terminator on Ganymede. This suggests an early period in Ganymede’s history when the crust was active and mobile, resembling Earth’s plate tectonics in some ways. The causes of the extreme differences in crustal evolution between Callisto and Ganymede are under investigation. Combinations of radioactive heating and a greater degree of tidal heating for Ganymede are possibilities. 7/9/79 100,000 km (62,000 ml) This mosaic of Ganymede, composed of photographs taken by Voyager 2, shows numerous impact craters, many with bright ray systems. The rough terrain at the lower right is the outer portion of a large, fresh impact basin that postdates most of the other terrain. The dark patches of heavily cratered terrain (right center) are probably ancient mixtures of ice and rock formed prior to the grooved terrain. The large rayed crater at the upper center is about 150 kilometers (95 miles) in diameter. 7/8/79 85,000 km (53,000 mi) Curved troughs and ridges in this high-resolution Voyager 2 photograph of Ganymede are the distinctive characteristics of an enormous, ancient impact basin. The basin itself has been eroded by later geologic processes; only the shock ring features are preserved on the ancient surface. Near the bottom of the picture these curved markings are perforated with the younger, grooved terrain. 7/7/79 2.3 million km (1.4 million mi) Callisto, only slightly smaller than Ganymede, has the lowest density of all the Galilean satellites, implying that it has large amounts of water in its bulk composition. Its surface is darker than the other Galilean satellites, although it is still twice as bright as our Moon. This Voyager 2 image shows Callisto to have the most heavily cratered and, therefore, the oldest surface of the Galilean satellites, probably dating back to the period of heavy meteoritic bombardment ending about four billion years ago. 3/6/79 350,000 km (217,000 mi) The prominent concentric ring structure shown in this Voyager 1 four-picture mosaic of Callisto is believed to be a large impact basin, similar to Mare Orientale on the Moon and Caloris Basin on Mercury. The bright circular spot is about 600 kilometers (360 miles) across, and the outer ring is about 2600 kilometers (1560 miles) across. This is the first recognized basin in the Jovian system and supports the assumption that Callisto’s surface is old. The lack of high ridges, ring mountains, or a large central depression suggests that the impacting body caused melting, some flow, and shock waves, and that the refreezing occurred in time to preserve the concentric shock rings. 7/7/79 390,000 km (245,000 mi) Callisto is the most heavily cratered planetary body in our solar system. In this Voyager 2 nine-frame mosaic, a special computer filter was used to provide high contrast in the surface topography. The impact structure visible at the upper right edge of the satellite is smaller than the largest one found by Voyager 1 but more detail is obvious; it is estimated that 15 concentric rings surround the bright center. Many hundreds of moderate-sized craters are also visible, a few with bright ray patterns. The limb is smooth, which is consistent with Callisto’s icy composition. 3/6/79 200,000 km (125,000 mi) This high-resolution image of Callisto, photographed by Voyager 1, shows details of the large ring structure surrounding the remains of the ancient impact basin visible on page 35. The surface area shown in this image is at the right edge and slightly above the center of the picture on page 35. The relatively undisturbed region on the right shows the shoulder-to-shoulder large impact craters typical of most of Callisto’s surface. A decrease in crater density toward the center of the structure (to the left) is evident, and is caused by the destruction of very old craters by the large impact that formed the ring |
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