<text>Because the Ulysses mission to the Sun acquired data about Jupiter during its gravitational boost and the Galileo spacecraft is currently speeding toward Jupiter, no future missions are planned at this time.</text>
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<text>To be launched in October, 1997 on a Titan IV-Centaur rocket from Cape Canaveral, Florida, Cassini will execute two gravity-assist flybys of Venus, then one each of Earth and Jupiter to send it on to arrive at Saturn in June, 2004.Equipment for a total of twelve science experiments will be carried onboard the Cassini orbiter. Some of these instruments which could be used during the Jupiter flyby include an imaging system for pictures in near-ultraviolet, visible, and near-infrared light; mass spectrometers to examine neutral and charged particles near the planet, and a magnetometer to study the magnetosphere.The Cassini mission is a joint project of NASA and the European Space Agency.</text>
<text>Ulysses: Launched October 6, 1990. Ulysses reached Jupiter in February 1992, and used the giant planet's gravity to speed it on its way toward the south pole of the Sun. As it swung around Jupiter, Ulysses studied the planet's magnetic field and radiation belts, and passed through a ring of ionized gas produced by volcanism on the moon Io.</text>
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<text>Artist's conception of the Galileo Probe entering the Jovian atmosphere.</text>
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<text>In order to reach Jupiter, Galileo must pick up the necessary speed by flying past Venus and twice by the Earth, using the well-tried gravity-assist technique, used previously by Voyager and other planetary missions.In December 1995 the Galileo atmospheric probe will conduct a direct examination of Jupiter's atmosphere, while the larger part of the craft, the orbiter, begins a 23-month, 10-orbit tour of the major satellites and the magnetosphere, including long- term observations of Jupiter throughout this phase.</text>
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<text>Galileo is a NASA spacecraft mission to Jupiter, launched October 18, 1989 by the space shuttle Atlantis, and designed to study the planet's atmosphere, satellites and surrounding magnetosphere for 2 years starting in late 1995. It was named for the Italian Renaissance scientist who discovered Jupiter's major moons in 1610 with the first astronomical telescope.This mission will be the first to make direct measurements from an instrumented probe within Jupiter's atmosphere, and the first to conduct long-term observations of the planet and its magnetosphere and satellites from orbit around Jupiter. It will be the first orbiter and atmospheric probe of an outer planet.</text>
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<text>Galileo during final assembly.</text>
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<text>Galileo in Atlantis cargo bay.</text>
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<text>Galileo being released from Atlantis cargo bay.</text>
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<text>The first Voyager was launched on August 20th, and the second on September 1st, 1977. They arrived at Jupiter in 1979, Saturn in 1980, and Uranus in 1986. Voyager 2 reached Neptune in 1989. The two spacecraft will be considered to have left the solar system when they cross the orbit of Pluto in 1989.</text>
<text>The Voyager mission was designed to take advantage of a rare geometric arrangement of the outer planets in the late 1970s and the 1980s. This layout of Jupiter, Saturn, Uranus and Neptune, which occurs about every 175 years, allows a spacecraft on a particular flight path to swing from one planet to the next without the need for large onboard propulsion systems. The flyby of each planet bends the spacecraft's flight path and increases its velocity enough to deliver it to the next destination. Using this "gravity assist" technique, the flight time to Neptune can be reduced from 30 years to 12.While the four-planet mission was known to be possible, it was deemed to be too expensive to build a spacecraft that could go the distance, carry the instruments needed and last long enough to accomplish such a long mission. Thus, the Voyagers were funded to conduct intensive flyby studies of Jupiter and Saturn only. More than 10,000 trajectories were studied before choosing the two that would allow close flybys of Jupiter and its large moon Io, and Saturn and its large moon Titan; the chosen flight path for Voyager 2 also preserved the option to continue on to Uranus and Neptune.Voyager 1 made its closest approach to Jupiter on March 5, 1979, and Voyager 2 followed with its closest approach occurring on July 9, 1979. The first spacecraft flew within 206,700 kilometers (128,400 miles) of the planet's cloud tops, and Voyager 2 came within 570,000 kilometers (350,000 miles).</text>
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<text>Revealing more detail than the very best groundbased telescopic photographs, this Voyager 1 image of Jupiter taken December 10 from 52 million miles shows the Great Red Spot (lower right) surrounded by a turbulent atmosphere. The entire visible surface of Jupiter is made up of multiple layers of clouds, composed primarily of ammonia ice crystals colored by small amounts of materials of unknown composition. Near the center is a bright convective cloud and an associated plume which has been swept westward (to the left) by local currents in the planet's equatorial wind system. This same atmospheric feature was seen prominently, in the Pioneer 10 and 11 spacecraft pictures of Jupiter taken four and five years ago this month. Below and to .the left of the Great Red Spot is a white oval cloud, one of three which formed nearly 40 years ago in the south temperate region. Largest of all of the planets, Jupiter's volume could contain more than 1200 Earths. Voyager 1 will fly past Jupiter on March 5, 1979, studying the planet and five of its 13 moons, and continue on to Saturn. An identical spacecraft, Voyager 2, arrives at Jupiter on July 9,1979, and will proceed to Saturn, and possibly Uranus. Both were launched in 1977. Among 11 science instruments, each spacecraft is equipped with two slow-scan TV cameras. This picture was taken with a camera equipped with a 1500 millimeter focal-length telescope.</text>
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<text>This recent photo of Jupiter taken by the television cameras aboard NASA's Voyager 1 is dominated by the Great Red Spot. Although the spacecraft is still 34 million miles (54 million kilometers) from a March 5 closest approach, Voyager's cameras already reveal details within the spot that aren't visible from earth. An atmospheric system larger than earth and more than 300 years old, the Great Red Spot remains a mystery and a challenge to Voyager's instruments. Swirling, storm-like features possibly associated with wind shear can be seen both to the left and above the Red Spot. Analysis of motions of the features will lead to a better understanding of weather in Jupiter's atmosphere. This photo was taken Jan. 9, 1979, through a blue filter and reassembled at Jet Propulsion Laboratory's Image Processing Laboratory. The streak is a dropped line of data.</text>
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<text>Voyager 1 took this photo of the planet Jupiter on Jan. 24, while still more than 25 million miles (40 million kilometers) away. As the spacecraft draws closer to the planet (about 1 million kilometers a day) are emerging more details in the turbulent clouds. The Great Red Spot shows prominently below center, surrounded by what scientists call a remarkable complex region of the giant planet's atmosphere. An elongated yellow cloud within the Great Red Spot is swirling around the spot's interior boundary in a counterclockwise direction with a period of a little less than six days, confirming the whirlpool-like circulation that astronomers have suspected from ground-based photographs. Ganymede, Jupiter's largest satellite, can be seen to the lower left of the planet. Ganymede is a planet-sized body larger than Mercury. This black and white image was taken through a blue filter.</text>
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<text>Voyager 1's cameras captured two of Jupiter's moons, Ganymede (right center) and Europa (top right) in this picture taken the morning of Jan. 17, 1979, from a distance of 47 million kilometers (29 million miles). Despite the small images of the moons, this photo and others are beginning to show details on the satellites not seen before in photos from Earth. Europa, an unusually bright satellite a little smaller than the Moon, is revealed to have a dark equatorial band. Although scientists believe Europa is a rocky satellite, its surface appears to be covered with a layer of ice or frost of undetermined thickness. Ganymede is larger than the planet Mercury. This photo shows only the darker side of the big satellite. The hidden half seen in other photos of Ganymede is marked by a large bright region. Ganymede is believed to be composed of a mixture of rock and water ice with a surface of ice or frost with a scattering of darker soil. Scientists at Jet Propulsion Laboratory have been observing rapid changes in Jupiter's atmosphere -- some occurring within 20 hours (two Jovian days). An example is changes in the long series of wave-like patterns trailing Jupiter's Great Red Spot. The bright zone stretching across the northern hemisphere may be clouds of frozen ammonia similar to cirrus clouds of water ice in Earth's atmosphere. Voyager 1 will fly by Jupiter on March 5 and continue on to a 1980 encounter with Saturn. This black and white photo was taken through a blue filter. </text>
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<text>Each of the two Voyager probes carry the 'Sounds of Earth' record. The 12 inch copper disk contains greetings from Earth people in sixty languages, samples of music from different cultures and eras, and natural sounds of surf, wind and thunder, birds, whales, and other animals. The record also contains electronic information that can be converted into diagrams, pictures, and printed words.The messages on the record were designed to enable possible extraterrestrial civilizations who might intercept the spacecraft millions of years hence to put together some picture of 20th century Earth and its inhabitants.</text>
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<text>This picture of a crescent-shaped Earth and Moon -- the first of its kind ever taken by a spacecraft -- was recorded Sept. 18, 1977, by NASA's Voyager 1 when it was 7.25 million miles (11.66 million kilometers) from Earth. The Moon is at the top of the picture and beyond the Earth as viewed by Voyager. In the picture are eastern Asia. the western Pacific Ocean and part of the Arctic. Voyager 1 was directly above Mt. Everest (on the right side of the planet at 25 degrees north latitude) when the picture was taken. The photo was made from three images taken through color filters, then processed by the Image Processing Lab at Jet Propulsion Laboratory. Because the Earth is many times brighter than the Moon, the Moon was artificially brightened by a factor of three relative to the Earth by computer enhancement so that both bodies would show clearly, in the prints. Two Voyager spacecraft are en route to Jupiter, Saturn and beyond. Voyager 2 was launched Aug. 20, 1977; Voyager 1 was launched Sept. 5.They will arrive at Jupiter in 1979 and at Saturn in 1980 and 1981.</text>
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<text>Pioneers 10 and 11, launched March 3, 1972, and April 5, 1973, were sister ships designed to be the first spacecraft to leave the inner solar system. Pioneer 10 traveled toward Jupiter at a speed of 51,800 km per hour, faster than any previous probe, and reached the massive planet on December 4, 1973. Before and after the closest approach of 130,300 km, many instruments continuously gathered data. These included devices to measure ultraviolet and infrared light, a magnetometer, a plasma analyzer, high energy particle detectors, and an asteroid telescope. Though it was damaged by Jupiter's intense radiation, Pioneer 10 transmitted all of its data back to Earth. The probe is still in communication with the Earth; it passed Neptune's orbit in June, 1983. It is now considered to have left the solar system even though it has not yet passed the heliopause.Pioneer 11 approached Jupiter three times closer to Jupiter than did Pioneer 10. Pioneer 11 carried the same instruments as Pioneer 10 with the addition of a second magnetometer in order to better measure Jupiter's incredibly strong magnetic field. Data from Pioneer 11 confirmed that Jupiter is composed mainly of hydrogen in liquid form. After observing Jupiter, Pioneer 11 became the first spacecraft to approach Saturn.</text>
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<text>In 1972, NASA sent the first of four spacecraft slated to conduct initial surveys of Jupiter. Pioneer 10 lifted off in March 1972 and returned the first close-up images of Jupiter in December 1973, flying within 132,252 km (82,178 miles) of the cloud tops. Pioneer 11 followed 1 year later. Voyagers 1 and 2 were launched in the summer of 1977 and did flybys in 1979.A new mission to Jupiter, known as the Galileo project, is under way. On December 7, 1995, the orbiter will spend two years circling the planet and flying close to the large moons. It will also drop an atmospheric probe into the cloud layers to relay information back to Earth.</text>
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<text>These four pictures of Jupiter's Great Red Spot were taken Feb. 2 and 3, 1979, when Voyager 1 was about 31 million kilometers (19.4 million miles) from Jupiter. The pictures were taken one Jupiter rotation apart, so that together they depict four days in the life of the centuries-old Red Spot. The pictures clearly demonstrate changes in circulation around the Red Spot during the 40-hour period. The photos were taken through a blue filter. Jet Propulsion Laboratory manages the Voyager project for NASA's Office of Space Science.</text>
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<text>This picture shows a region of the southern hemisphere extending from the Great Red Spot to the south pole. The white oval is seen beneath the Great Red Spot, and several small scale spots are visible farther to the south. Some of these organized cloud spots have similar morphologies, such as anticyclonic rotations and cyclonic regions to their west. The presence of the white oval causes the streamlines of the flow to bunch up between it and the Great Red Spot.</text>
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<text>This view of the region just to the Southeast of the Great Red Spot was taken by Voyager 1 on March 4, 1979 at a distance of 1,100,000 miles (1,800,000 kin). Differences in cloud color may indicate relative heights of the cloud layers but the exact relationship between color and height has not yet been established. The smallest clouds seen in this picture are approximately 20 miles (30 km) across.</text>
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<text>This photo of Jupiter was taken by Voyager 1 on March 1, 1979, from a distance of 2.7 million miles (4.3 million kilometers). The region shown is just to the southeast of the Great Red Spot. A small section of the spot can be seen at upper left. One of the 40-year-old white ovals in Jupiter's atmosphere can also be seen at middle left, as well as a wealth of other atmospheric features, including the flow lines in and around the ovals. The smallest details that can be seen in this photo are about 45 miles (80 kilometers) across.</text>
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<text>This photo of Jupiter was taken by Voyager 1 on the evening of March 1, 1979, from a distance of 2.7 million miles (4.3 million kilometers). The photo shows Jupiter's Great Red Spot (top) and one of the white ovals that can be seen in Jupiter's atmosphere from Earth. The white ovals were seen to form in 1939, and 1940, and have remained more or less constant ever since. None of the structure and detail evident in these features have ever been seen from Earth. The Great Red Spot is three times as large as Earth. Also evident in the picture is a great deal of atmospheric detail that will require further study for interpretation. The smallest details that can be seen in this picture are about 45 miles (80 kilometers) across.</text>
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<text>This mosaic of the Great Red Spot shows that the region has changed significantly. Around the northern boundary a white cloud is seen, which extends to east of the region. The presence of this cloud prevents small cloud vertices from circling the spot in the manner seen in the Voyager 1 encounter. Another white oval cloud (different from the one present in this position three months ago) is seen south of the Great Red Spot. The internal structure of these spots is identical. Since they both rotate in an anticyclonic manner these observations indicate that they are meteorologically similar. This image was taken on July 6 from a range of 2,633,003 kilometers.</text>
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<text>This color composite made from Voyager 2 narrow-angle camera frames shows the Great Red Spot during the late Jovian afternoon. North of the Red Spot lies a curious darker section of the South Equatorial Belt (SEB), the belt in which the Red Spot is located. A bright eruption of material passing from the SEB northward into the diffuse equatorial clouds has been observed on all occasions when this feature passes north of the Red Spot. The remnants of one such eruption are apparent in this photograph. To the lower left of the Red Spot lies one of the three long-lived White Ovals. This photograph was taken on June 29, 1979, when Voyager 2 was over 9 million kilometers (nearly 6 million miles) from Jupiter. The smallest features visible are over 170 kilometers ( 106 miles) across.</text>
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<text>This Jupiter image taken by Voyager 2 shows an area from 10┬░ N. Lat. to 34┬░ S. Lat. in a region west of the Great Red Spot. At the top of the picture, equatorial plumes are seen. These features move along the edge of the equatorial zone. The remainder of the equatorial region is characterized by diffuse clouds. The region west of the Great Red Spot is seen as a disturbed wave-like pattern. Similar flows are seen to the west of the white oval at bottom.</text>
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<text>This Jupiter image taken by Voyager 2 shows an area from 10┬░ N. Lat. to 34┬░ S. Lat. in a region west of the Great Red Spot. At the top of the picture, equatorial plumes are seen. These features move along the edge of the equatorial zone. The remainder of the equatorial region is characterized by diffuse clouds. The region west of the Great Red Spot is seen as a disturbed wave-like pattern. Similar flows are seen to the west of the white oval at bottom.</text>
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<text>This Voyager 1 picture of the outermost Galilean satellite, Callisto, was taken Feb. 28, through a violet filter from a distance of about 5 million miles (7 million kilometers). Callisto is the darkest of the four Galilean satellites of Jupiter, but is still nearly twice as bright as Earth's Moon. It shows a mottled appearance consisting of bright and dark patches. The bright spots remind scientists of rayed or bright halved craters, similar to those seen on our Moon. This face of Callisto is always turned toward Jupiter.</text>
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<text>This picture of a multi-ring basin on Callisto was taken the morning of March 6, 1979, from a distance of about 200,000 km. The complicated circular structure seen at left center is similar to the large circular impact basins that dominate the surface of the Earth's moon and also the planet Mercury. The inner parts of these basins are generally surrounded by radially lineated ejecta and several concentric mountainous ring structures that are thought to form during the impact event. This multi-ring basin on Callisto consists of a light floored central basin some 300 km in diameter surrounded by at least eight to ten discontinuous rhythmically spaced ridges. No radially lineated ejecta can be seen. The ring structures on Moon and Mercury have been likened to ripples produced on a pond by a rock striking the water. The great number of rings observed around this basin on Callisto is consistent with its low planetary density and probable low internal strength.</text>
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<text>This color picture as acquired by Voyager 1 during its approach to Ganymede on Monday afternoon (the 5th of March) at ranges between about 230 to 250 thousand km. The images show detail on the surface with a resolution of four and a half km. Picture 2 (P-21262) is just south of Picture 1 and shows more craters. It also shows the two distinctive types of terrain found by Voyager, the darker ungrooved regions and the lighter areas which show the grooves or fractures in abundance. The most striking features are the bright ray craters which have a distinctly "bluer" color appearing white against the redder background. Ganymede's surface is known to contain large amounts of surface ice and it appears that these relatively young craters have spread bright fresh ice materials over the surface. Likewise, the lighter color and reflectivity of the grooved areas suggests that here too, there is cleaner ice. We see ray craters with all sizes of ray patterns, ranging from extensive systems of the crater in the southern part of Picture 1 (northern part of Picture 2), which has rays at least 300-500 kilometers long, down to craters which have only faint remnants of bright ejecta patterns (such as several of the craters in the southern half of Picture 2). This variation suggests that, as on the Moon, there are processes which act to darken ray material, probably "gardening" by micro meteoroid impact.</text>
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<text>This photo mosaic of Ganymede, Jupiter's largest satellite, was taken on the morning of July 9, 1979, by Voyager 2 at a range of about 100,000 kilometers (62,000 miles). It shows numerous impact craters, many with bright ray systems. The rough mountainous terrain at lower right is the outer portion of a large fresh impact basin which post-dates most of the other terrain. At bottom, portions of grooved terrain transect other portions indicating they are younger. This may be the result of the intrusion of new icy material which comprises the crust of Ganymede. The dark patches of heavily cratered terrain (right center) are probably ancient icy material formed prior to the grooved terrain. The large rayed crater at upper center is about 150 kilometers (93 miles) in diameter.</text>
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<text>Voyager 1's cameras captured two of Jupiter's moons, Ganymede (right center) and Europa (top right) in this picture taken the morning of Jan. 17, 1979, from a distance of 47 million kilometers (29 million miles). Despite the small images of the moons, this photo and others are beginning to show details on the satellites not seen before in photos from Earth. Europa, an unusually bright satellite a little smaller than the Moon, is revealed to have a dark equatorial band. Although scientists believe Europa is a rocky satellite, its surface appears to be covered with a layer of ice or frost of undetermined thickness. Ganymede is larger than the planet Mercury. This photo shows only the darker side of the big satellite. The hidden half seen in other photos of Ganymede is marked by a large bright region. Ganymede is believed to be composed of a mixture of rock and water ice with a surface of ice or frost with a scattering of darker soil. Scientists at Jet Propulsion Laboratory have been observing rapid changes in Jupiter's atmosphere -- some occurring within 20 hours (two Jovian days). An example is changes in the long series of wave-like patterns trailing Jupiter's Great Red Spot. The bright zone stretching across the northern hemisphere may be clouds of frozen ammonia similar to cirrus clouds of water ice in Earth's atmosphere. Voyager 1 will fly by Jupiter on March 5 and continue on to a 1980 encounter with Saturn. This black and white photo was taken through a blue filter. </text>
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<text>This photo of Ganymede was taken Feb. 27, 1979, by Voyager 1 when the spacecraft was about 3.7 million miles (6 million kilometers) from the satellite. North is up and the central longitude is about 120 degrees west. Ganymede is slightly larger than the planet Mercury, but is much less dense (only about twice the density of water). Its surface brightness is about four times that of Earth's Moon. The picture shows dark features that remind scientists of the dark mare regions on our Moon, but on Ganymede those features are twice as bright as lunar mare and are unlikely to be composed of rock or lava. The north polar region appears to be covered with brighter material, probably water frost. If later pictures of this polar area show blanketing of underlying terrain, it could indicate movement of water on .Ganymede's surface, possibly in a very thin atmosphere. Brighter spots are scattered over this hemisphere of Ganymede. These may be related to impact craters or may represent source areas of fresh ice.</text>
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<text>This photo of Ganymede, largest of Jupiter's Galilean satellites and the third from the planet, was taken shortly after midnight March 1, from a distance of 2.6 million miles (4.2 million kilometers). Ganymede is slightly larger than the planet Mercury, but is much less dense; it has roughly twice the density of water. Ganymede's surface brightness is four times that of Earth's Moon. This photo shows dark features reminiscent of the dark, mare regions on the Moon. On Ganymede, however, these features have twice the brightness of lunar mare. Scientists believe they are unlikely to be composed of rock or lava as the Moon's mare regions are. Ganymede's north polar region appears to be covered with brighter material, and scientists say it could be water frost. Later photos of Ganymede will be taken from closer range and will therefore have higher resolution if those photos of the polar region show underlying terrain blanketed by frost, it could indicate movement of water across Ganymede's surface, possibly in a very thin atmosphere. Brighter spots are also scattered across this hemisphere of Ganymede. They may be related to impact craters, or may represent source regions of fresh ice. </text>
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<text>This Voyager 1 picture of the outermost Galilean satellite, Callisto, was taken Feb. 28, through a violet filter from a distance of about 5 million miles (7 million kilometers). Callisto is the darkest of the four Galilean satellites of Jupiter, but is still nearly twice as bright as Earth's Moon. It shows a mottled appearance consisting of bright and dark patches. The bright spots remind scientists of rayed or bright halved craters, similar to those seen on our Moon. This face of Callisto is always turned toward Jupiter. </text>
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<text>This photo of Ganymede, largest of Jupiter's Galilean satellites and the third from the planet, was taken shortly after midnight March 1, from a distance of 2.6 million miles (4.2 million kilometers). Ganymede is slightly larger than the planet Mercury, but is much less dense; it has roughly twice the density of water. Ganymede's surface brightness is four times that of Earth's Moon. This photo shows dark features reminiscent of the dark, mare regions on the Moon. On Ganymede, however, these features have twice the brightness of lunar mare. Scientists believe they are unlikely to be composed of rock or lava as the Moon's mare regions are. Ganymede's north polar region appears to be covered with brighter material, and scientists say it could be water frost. Later photos of Ganymede will be taken from closer range and will therefore have higher resolution if those photos of the polar region show underlying terrain blanketed by frost, it could indicate movement of water across Ganymede's surface, possibly in a very thin atmosphere. Brighter spots are also scattered across this hemisphere of Ganymede. They may be related to impact craters, or may represent source regions of fresh ice. </text>
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<text>This photo of Ganymede was taken Feb. 27, 1979, by Voyager 1 when the spacecraft was about 3.7 million miles (6 million kilometers) from the satellite. North is up and the central longitude is about 120 degrees west. Ganymede is slightly larger than the planet Mercury, but is much less dense (only about twice the density of water). Its surface brightness is about four times that of Earth's Moon. The picture shows dark features that remind scientists of the dark mare regions on our Moon, but on Ganymede those features are twice as bright as lunar mare and are unlikely to be composed of rock or lava. The north polar region appears to be covered with brighter material, probably water frost. If later pictures of this polar area show blanketing of underlying terrain, it could indicate movement of water on .Ganymede's surface, possibly in a very thin atmosphere. Brighter spots are scattered over this hemisphere of Ganymede. These may be related to impact craters or may represent source areas of fresh ice.</text>
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<text>This picture of Ganymede, Jupiter's largest satellite, was taken on the afternoon of March 2, 1979, by Voyager 1 from a distance of about 3.4 million kilometers (2.1 million miles). This photograph was assembled from three black-and-white pictures in the Image Processing Laboratory at JPL. This face of Ganymede is centered on the 260┬░ meridian. Ganymede is slightly larger than the planet Mercury but has a density almost three times less than Mercury. Therefore, Ganymede probably consists in large part of ice. At this resolution the surface shows light and dark markings interspersed with bright spots. The large darkish area near the center of the satellite is crossed by irregular light streaks somewhat similar to rays seen on the Moon. The bright patch in the southern hemisphere is reminiscent of some of the larger rayed craters on the Moon caused by meteorite impacts.</text>
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<text>This color picture of Ganymede, Jupiter's largest satellite, was taken on the afternoon of March 2, 1979, by Voyager 1 from a distance of about 3.4 million kilometers (2.1 million miles). This photograph was assembled from three black-and-white pictures in the Image Processing Laboratory at JPL. This face of Ganymede is centered on the 260o meridian. Ganymede is slightly larger than the planet Mercury but has a density almost three times less than Mercury. Therefore, Ganymede probably consists in large part of ice. At this resolution the surface shows light and dark markings interspersed with bright spots. The large darkish area near the center of the satellite is crossed by irregular light streaks somewhat similar to rays seen on the Moon. The bright patch in the southern hemisphere is reminiscent of some of the larger rayed craters on the Moon caused by meteorite impacts.</text>
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<text>Voyager 1 took this photo of Jupiter and two of its satellites (Io, left, and Europa) on Feb. 13, 1979. Io is about 350,000 kilometers (220,000 miles) above Jupiter's Great Red Spot; Europa is about 600,000 kilometers (375,000 miles) above Jupiter's clouds. Although both satellites have about the same brightness, Io's color is very different from Europa's. Io's equatorial region show two types of material -- dark orange, broken by several bright spots -- producing a mottled appearance. The poles are darker and reddish. Preliminary evidence suggests color variations within and between the polar regions. Io's surface composition is unknown, but scientists believe it may be a mixture of salts and sulfur. Europa is less strongly colored, although still relatively dark at short wavelengths. Markings on Europa are less evident than on the other satellites, although this picture shows darker regions toward the trailing half of the visible disk. Jupiter is about 20 million kilometers (12.4 million miles) from the spacecraft. At this resolution (about 400 kilometers or 250 miles) there is evidence of circular motion in Jupiter's atmosphere. While the dominant large-scale motions are West-to-east, small-scale movement includes eddy-like circulation within and between the bands. 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.</text>
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<text>Voyager 1 took this picture of Europa, Jupiter's second Galilean satellite, early on the morning of March 1, 1979, from a distance of 3.66 million miles (5.9 million kilometers). The photo was taken through a violet filter and shows faint swirls and linear patterns in Europa's equatorial region. The hemisphere shown here is that which always faces Jupiter. North is up. The equatorial region is slightly darker than the poles. Although Europa is the brightest of the Galilean satellites, it exhibits low contrast on this hemisphere. Like Io, Europa has a density and size comparable to Earth's Moon. But unlike Io which is apparently dry, Europa shows Earth-bound observers many indications of water ice or ground water on its surface. JPL manages and controls the Voyager project for NASA's Office of Space Science.</text>
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<text>Voyager 1 took this picture of Europa, Jupiter's second Galilean satellite, early on the morning of March 1, 1979, from a distance of 3.66 million miles (5.9 million kilometers). The photo was taken through a violet filter and shows faint swirls and linear patterns in Europa's equatorial region. The hemisphere shown here is that which always faces Jupiter. North is up. The equatorial region is slightly darker than the poles. Although Europa is the brightest of the Galilean satellites, it exhibits low contrast on this hemisphere. Like Io, Europa has a density and size comparable to Earth's Moon. But unlike Io which is apparently dry, Europa shows Earth-bound observers many indications of water ice or ground water on its surface. </text>
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<text>This photo of Europa, brightest of Jupiter's four Galilean satellites, was taken by Voyager 1 March 2, 1979, from a distance of 1.75 million miles (2.87 million kilometers). In this image a bizarre collection of dark streaks are becoming visible. They are about 30 miles (50 kilometers) wide, and typically 1,200 miles (2,000 kilometers) to 1,800 miles (3,000 kilometers) long. They show a variety of forms: straight, arcuate, linear and branching. Scientists believe they may represent some tectonic system of large fractures or faults. At this resolution it is still too early to tell. In July Voyager 2 will see, at much closer range, the same hemisphere of Europa. </text>
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<text>View of Europa taken from a range of 2,869,252 kilometers (1.6 million miles) on March 2 at 2:00 PM. The 1700 longitude is at the center of the picture; this is the face away from Jupiter. Irregular dark and bright patches on the surface are different from the patterns on the other satellites of Jupiter and those on the Moon, Mars and Mercury. Dark intersecting lines may be faults that break the crust. </text>
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<text>View of Europa taken from a range of 2,869,252 kilometers (1.6 million miles) on March 2 at 2:00 PM. The color composite is made from three black and white images taken through the orange, green and violet filters. The 1700 longitude is at the center of the picture; this is the face away from Jupiter. Irregular dark and bright patches on the surface are different from the patterns on the other satellites of Jupiter and those on the Moon, Mars and Mercury. Dark intersecting lines may be faults that break the crust. </text>
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<text>These images of Io's South Pole show several volcanic features. All of the somewhat circular marks on the surface are volcanoes which have erupted fairly recently. The largest of these volcanoes near the South Pole is Haemus Mons. It has a base which measures approximately 100 by 200 km. Peaks such as Haemus Mons can be as much as 10 km tall. The lighter rings surrounding the dark circles are volcanic material, probably some form of sulfur, which has been spewed from the central vent.</text>
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<text>Pateras are very large, but low, volcanoes with large calderas. The calderas form when magma chambers underneath the volcano are rapidly emptied by an eruption. The empty chamber cannot support the rock above, and the roof collapses. Pateras are different from the tall shield volcanoes such as Olympus Mons on Mars or the volcanoes which formed the Hawaiian islands on Earth.The Mbali, Mihr, Maasaw, Loki, Ra and Babbar Patera are all volcanoes which have recently erupted. Though they are similar to one another, each of them has its own unique features. The Ra Patera has many long flows emanating from it. These lava "fingers" stretch for as much as 200 km across Io's surface.The Loki Patera is larger than the island of Hawaii. It is possible that the large black region is a lake of liquid sulfur which is about 250 km across. Another remarkable thing about the Loki Patera is the striking change in its appearance in the time between the Voyager 1 and 2 flybys. The eruptions of these pateras are less violent and large than volcanoes like Pele, but they last much longer. The base of the plumes of these eruptions generally measures 300 to 400 km. Volcanism is associated with heating of Io by tidal pumping. Europa and Ganymede, two large satellites nearby, perturb Io in its orbitand Jupiter pulls Io back again. The pumping action causes tidalbulging up to 100 meters (330 feet) on Io's surface, comparedwith typical tidal bulges on Earth of one meter (three feet).Voyager 1 identified nine currently active (erupting) volcanoes on Io, probably driven by tidal heating. Many more are suspected. Voyager 2 observed eight of the nine; the largest shut down by the time Voyager 2 arrived at Jupiter. Plumes from the volcanoes reach more than 300 kilometers (190 miles) above the surface. The material was being ejected at velocities up to1.05 kilometers a second (2,300 miles an hour). By comparison, ejection velocities at Mount Etna, one of Earth's most explosive volcanoes, hit 50 meters a second (112 miles an hour). </text>
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<text>This view of the region just to the Southeast of the Great Red Spot was taken by Voyager 1 on March 4, 1979 at a distance of 1,100,000 miles (1,800,000 kin). Differences in cloud color may indicate relative heights of the cloud layers but the exact relationship between color and height has not yet been established. The smallest clouds seen in this picture are approximately 20 miles (30 km) across</text>
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<text>Pateras are very large, but low, volcanoes with large calderas. The calderas form when magma chambers underneath the volcano are rapidly emptied by an eruption. The empty chamber cannot support the rock above, and the roof collapses. Pateras are different from the tall shield volcanoes such as Olympus Mons on Mars or the volcanoes which formed the Hawaiian islands on Earth.The Mbali, Mihr, Maasaw, Loki, Ra and Babbar Patera are all volcanoes which have recently erupted. Though they are similar to one another, each of them has its own unique features. The Ra Patera has many long flows emanating from it. These lava "fingers" stretch for as much as 200 km across Io's surface.The Loki Patera is larger than the island of Hawaii. It is possible that the large black region is a lake of liquid sulfur which is about 250 km across. Another remarkable thing about the Loki Patera is the striking change in its appearance in the time between the Voyager 1 and 2 flybys. The eruptions of these pateras are less violent and large than volcanoes like Pele, but they last much longer. The base of the plumes of these eruptions generally measures 300 to 400 km. Volcanism is associated with heating of Io by tidal pumping. Europa and Ganymede, two large satellites nearby, perturb Io in its orbitand Jupiter pulls Io back again. The pumping action causes tidalbulging up to 100 meters (330 feet) on Io's surface, comparedwith typical tidal bulges on Earth of one meter (three feet).Voyager 1 identified nine currently active (erupting) volcanoes on Io, probably driven by tidal heating. Many more are suspected. Voyager 2 observed eight of the nine; the largest shut down by the time Voyager 2 arrived at Jupiter. Plumes from the volcanoes reach more than 300 kilometers (190 miles) above the surface. The material was being ejected at velocities up to1.05 kilometers a second (2,300 miles an hour). By comparison, ejection velocities at Mount Etna, one of Earth's most explosive volcanoes, hit 50 meters a second (112 miles an hour). </text>
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<text>Pele is the first volcanic eruption discovered on Io. It was viewed by Voyager 1, but had returned to a dormant state by the time Voyager 2 passed Io four months later. While it erupted, however, it sprayed molten sulfur and other material in a plume which reached 300 km above the surface. In some ways, the eruption of volcanoes on Io is more like terrestrial geysers than terrestrial volcanoes. This is due to the lower density of the "lava", lower surface gravity, and lower atmospheric pressure on Io. For comparison, however, if "Old Faithful" in Yellowstone Park could erupt in an environment like that of Pele, its plume would only reach 35 km high. Therefore it is not just the conditions of Io that allow such large eruptions--the force driving the volcanoes must be much stronger than that which causes terrestrial volcanoes.</text>
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<text>Voyager 2 completed a dramatic ten-hour time lapse photographic sequence July 9, to monitor the active volcanos on Jupiter's dynamic 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. The sequence of pictures was acquired at a range of approximately 1 million kilometers. On the bright limb, two of the plumes (P-5 and P-6) discovered in March by Voyager 1 are again visible. The plumes are spewing materials to a height of about 100 kilometers.</text>
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<text>This photograph of Jupiter's satellite Io shows what appears to be a volcanic caldera that is venting gasses (the bright blue patch at left center). In the photo is a network of volcanic calderas with dark floors linked by bright red materials. The northernmost caldera has a bright blue patch on the floor. Scientists believe the bright blue patch may be clouds of gas issuing from volcanic vents. The gas clouds may condense to form extremely fine particles that appear blue. Since Voyager 1's infrared spectrometer has discovered sulfur dioxide on Io, it is possible that sulfur dioxide is 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 molten sulfur, a very dark form of sulfur.The picture was taken March 5, 1979, as Voyager 1 approached Io. Photo was taken from 80,500 miles (129,600 kilometers). The Voyager project is managed and controlled for NASA's Office of Space Science by the Jet Propulsion Laboratory.</text>
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<text>Voyager 1 acquired this image of Io on March 4 at 5:30 p.m. (PST) about 11 hours before closest approach to the Jupiter moon. The distance to Io was about 490,000 kilometers (304,000 miles). An enormous volcanic explosion can be seen silhouetted against dark space over Io's bright limb. The brightness of the plume has been increased by the computer as it is normally extremely faint, whereas the relative color of the plane (greenish white) has been preserved. At this time solid material had been thrown up to an altitude of about 100 miles. This requires an ejection velocity from the volcanic vent of about 1200 miles per hour, material reaching the crest of the fountain in several minutes. The vent area is a complex circular structure consisting of a bright ring about 300 kilometers in diameter and a central region of irregular dark and light patterns. Volcanic explosions similar to this occur on the earth when magmatic gases expand explosively as material is vented. On earth, water is the major gas driving the explosion. Because Io is thought to be extremely dry, scientists are searching for other gases to explain the explosion. </text>
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<text>This picture of Io was taken on the morning of March 5 at a range of 75,445 kilometers. The area shown is at latitude 15┬░ south longitude 244┬░. Many depressions and elevations are shown. The light is coming from the left, so a depression has a bright right wall and shadow on the left wall. The depressions are complex in shape and do not resemble impact craters. Two of the depressions are joined by a shallow trough. The elevations are irregular and conical. They are cut by linear and irregular troughs. The surface is smooth and plain-like, that is, the surface is not pockmarked by abundant impact craters so are probably geologically young. The Voyager Project is managed and controlled by the Jet Propulsion Laboratory for NASA's Office of Space Science.</text>
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<text>Obtained on March 2, 1979, by Voyager 1, this picture of Io shows the region of the Jovian moon which will be monitored for volcanic eruptions by Voyager 2 during' the so-called "Io movie" sequence on July 9 and 10. The white and orange patches probably are deposits of sulfur compounds and other volcanic materials. The Voyager 2 pictures of this region will be much more detailed than this photo, taken from 2.6 million kilometers (1.6 million miles).</text>
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<text>This picture of Io, the innermost Galilean satellite, was taken by Voyager 1 on the morning of March 5, 1979 at a range of 377,000 kilometers (226,200 miles). The smallest features visible are about 10 kilometers (6 miles) across. The reddish, white and black areas are probably surface deposits, possibly consisting of mixtures of salts, sulfur and sublimate deposits of possible volcanic origin. Many of the black spots in these pictures are associated with craters of possible volcanic origin. The lack of impact craters on Io suggests that the surface is relatively young compared to the other Galilean satellites and some of the terrestrial planets such as Mercury and the Moon. JPL manages and controls the Voyager project for NASA's Office of Space Science.</text>
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<text>This photo of Io, innermost of the four large Galilean satellites of Jupiter, was taken through an ultraviolet filter by the narrow angle camera of Voyager 1. The photo was taken at 2 a.m. (PST) Feb. 27, when Voyager 1 was 4.3 million miles (7 million kilometers) from Io, seen against the background of a 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 generally very dark polar areas and numerous light and dark regions around the equator. At this resolution (about 100 miles or 160 kilometers), no topographic features, such as craters, can be seen. The brighter regions are believed to contain sulfur and various salts, making Io highly reflective (about six times brighter than Earth's Moon) in visible and enhanced light. This satellite of Jupiter has almost exactly the same size and density as our own Moon, but it apparently has followed a very different evolutionary path, influenced by its proximity to Jupiter and the intense bombardment it receives from the Jovian radiation belts of energetic charged particles.</text>
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<text>This photo of Io, innermost of the four large Galilean satellites of Jupiter, was taken through an ultraviolet filter by the narrow angle camera of Voyager 1. The photo was taken at 2 a.m. (PST) Feb. 27, when Voyager 1 was 4.3 million miles (7 million kilometers) from Io, seen against the background of a 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 generally very dark polar areas and numerous light and dark regions around the equator. At this resolution (about 100 miles or 160 kilometers), no topographic features, such as craters, can be seen. The brighter regions are believed to contain sulfur and various salts, making Io highly reflective (about six times brighter than Earth's Moon) in visible and enhanced light. This satellite of Jupiter has almost exactly the same size and density as our own Moon, but it apparently has followed a very different evolutionary path, influenced by its proximity to Jupiter and the intense bombardment it receives from the Jovian radiation belts of energetic charged particles. JPL manages and controls the Voyager project for NASA's Office of Space Science.</text>
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<text>These images are various projections of the data the Voyager spacecraft recorded about Io.The image in the lower right corner is a mosaic of images color enhanced in order to emphasize the various types and colors of the Io terrain. The other three images are mosaics of the entire surface of Io. They are aligned so that the same features are at identical places on each of the maps. The large "pock mark" in the bottom left quarter of the images is the volcano Pele. The whitish region in the center is the Colchis Regio; the light region just to the right of center is the Media Regio. In each of these projections, north is at the top and the zero point of longitude is at both the right and left edges.</text>
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<text>The orbits of Jupiter's sixteen moons occupy a large area about the planet. Metis, closest to Jupiter, is only 127,960 km from the planet while Sinope, the farthest out, is 23,700,000 km from Jupiter. The "Inner Orbits" graphic shows the innermost eight moons. The four largest orbits in this picture are those of the Galilean satellites Callisto, Ganymede, Europa, and Io (from the outside in). The outer satellites occur in two groups. For scale, the orbit of Callisto, is the dot in the middle of the bottom graphic. The next collection of satellites includes four moons between 11 and 12 million km from Jupiter. The outermost grouping contains satellites with the most eccentric orbits. There are four satellites with mean distances of 21 to 24 million km from Jupiter.</text>
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<text>The atmosphere of Jupiter shows light and dark bands of clouds in a range of colors. The light bands, called zones, are high in the atmosphere and indicate up welling gas; the dark bands, or belts, are lower and show where gas is descending. The zones and belts are driven by eastward and westward winds of up to 540 kilometers per hour. Adjacent cloud bands are often moving in opposite directions, driving turbulent eddies around the planet. Of these eddies, which appear as light or dark ovals, the most prominent is the Great Red Spot (16,280 x 8,575 miles). Located in the southern hemisphere, this storm is more than twice the size of Earth and rotates in a counterclockwise direction every four to six days. The Great Red Spot was observed over 300 years ago, but researchers believe it could be millions of years old. </text>
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<text>JupiterPlanet statisticsDistance from the Sun: Maximum: 505.7 million miles 815.7 million km 5.455 AUMinimum: 459.4 million miles 740.9 km 4.951 AU Mean: 482.6 million miles 778.3 million km 5.203 AUPeriod of revolution: 11.86 yearsPeriod of rotation (equatorial): 9 hr. 50 min. 30 sec.Mean orbital velocity: 8.1 miles (13.1 km) per secondInclination of axis: 3.1 degreesOrbital eccentricity: 0.048Orbital inclination: 1.31 degreesDiameter at equator: 88,800 miles (142,900 km) 11.2 x Earth's diameterOblateness: 0.064Mass: 1.9 x 10^30 kg 318 x EarthΓÇÖs massVolume: 1.43 x 10^15 km^3 1,323 x EarthΓÇÖs volumeDensity: 1.33 g/cm^3 0.239 x EarthΓÇÖs densitySurface gravity: 22.9 m/s^2 2.64 x EarthΓÇÖs gravityEscape velocity: 37.0 miles (59.5 km) per secondMean surface temperature:-238 F / -150 C / 123 K (at cloud tops)Maximum apparent diameter as seen from Earth: 50.1ΓÇ¥Albedo: 0.44Number of knwon satellites: 16Mean diameter of Sun as seen from the planet: 6' 09"</text>
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