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30 calibabor Vertical Gun Range in horizontal loading position. Dr. William Quaide and Donald Gault of Ames planetology branch used this gun range to study the formation of impact craters on the Moon. N-204A Verticle Gun is used to simulate the physics and mechanics of planetaryimpact cratering phenomena. ARC-1965-A-33996

30 calibabor Vertical Gun Range in horizontal loading position. Dr. William Quaide and Donald Gault of Ames planetology branch used this gun range to study the formation of impact craters on the Moon. N-204A Ve More

Range : 6 million kilometers (3.7 million miles) Central Longitude 120 degrees west, North is up. and 3rd from the planet. Photo taken after midnight 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. ARC-1979-A79-7019

Range : 6 million kilometers (3.7 million miles) Central Longitude 120 degrees west, North is up. and 3rd from the planet. Photo taken after midnight Ganymede is slightly larger than Mercury but much less de More

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. ARC-1979-A79-7020

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 More

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) ARC-1979-A79-7027

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 More

Range : 4.2 million kilometers (2.6 million miles) Ganymede is Jupiter's Largest Galilean satellites and 3rd from the planet. Photo taken after midnight 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. ARC-1979-A79-7016

Range : 4.2 million kilometers (2.6 million miles) Ganymede is Jupiter's Largest Galilean satellites and 3rd from the planet. Photo taken after midnight Ganymede is slightly larger than Mercury but much less More

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 235Â° 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. ARC-1979-AC79-7078

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 cov More

Range : 4.2 million km. ( 2.6 million miles ) Jupiter's moon Europa, the size of earth's moon, is apparently covered by water ice, as indicated by ground spectrometers and its brightness. In this view, global scale dark sreaks discovered by Voyager 1 that criss-cross the the satelite are becoming visible. Bright rayed impact craters, which are abundant on Ganymede and Callisto, would be easily visible at this range, suggesting that Europa's surface is young and that the streaks are reflections of currently active internal dynamic processes. ARC-1979-A79-7103

Range : 4.2 million km. ( 2.6 million miles ) Jupiter's moon Europa, the size of earth's moon, is apparently covered by water ice, as indicated by ground spectrometers and its brightness. In this view, global More

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. ARC-1979-AC79-7104

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 componen More

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. ARC-1979-A79-7097

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 youn More

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. ARC-1979-A79-7093

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 cu More

100,000 kilometers (62,000 miles) This photomosaic of Ganymede, Jupiter's largest satellite, shows many impact craters, some 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 indication 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. ARC-1979-A79-7096

100,000 kilometers (62,000 miles) This photomosaic of Ganymede, Jupiter's largest satellite, shows many impact craters, some with bright ray systems. The rough mountainous terrain at lower right is the outer p More

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. ARC-1979-AC79-7083

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 l More

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. ARC-1979-A79-7092

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 densi More

P-21760 C 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. ARC-1979-AC79-7088

P-21760 C 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 streak More

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. ARC-1979-A79-7088

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 strea More

Range : 2.77 million miles (1.72 million miles) resolution : 51 km. (32 mi.) P-29495C This Voyager 2 photograph of the outermost Uranian satellite, Oberon is a computer reconstruction of three frames , exposed through the narrow angle camera's blue, green, and orange filters. the grayness or apparent lack of strong color is a distinctive characteristic of the satellites and the rings of Uranus and can serve as one indicator of the possible composition of the satellites' surfaces. Oberon has a diameter of about 1,600 km. (1,000 mi.) and orbits the planet at a radial distance of 586,000 km. (364,000 mi.). Oberon's surface displays areas of lighter and darker material, probably associated in part with impact craters formed during its long exposure to bombardment by cosmic debris. Thr resolution of this particular image is not sufficient, however, to reveal with confidece the nature of these features. ARC-1986-AC86-7012

Range : 2.77 million miles (1.72 million miles) resolution : 51 km. (32 mi.) P-29495C This Voyager 2 photograph of the outermost Uranian satellite, Oberon is a computer reconstruction of three frames , expose More

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 Â° 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'. ARC-1986-AC86-7018

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 More

P-29504BW Range: 500,000 kilometers (300,000 miles) This full-disk view of Uranus' moon Titania in the early morning hours, a clear-filter image returned by the Voyager narrow-angle camera, shows many circular depressions-probably impact craters. Other bright spots are distinguished by radiating rays and are probably halo craters that mark relatively more recent impacts. Even more interesting are the linear troughs (right) that are probably fault canyons. The troughs break the crust in two directions, an indication of some tectonic extension of Titania's crust. These features indicate that this icy satellite has a dynamic, active interior. Titania is about 1,600 km (1,000 mi) in diameter; the resolution of this image is about 9 km (6 mi). ARC-1986-A86-7020

P-29504BW Range: 500,000 kilometers (300,000 miles) This full-disk view of Uranus' moon Titania in the early morning hours, a clear-filter image returned by the Voyager narrow-angle camera, shows many circula More

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. ARC-1986-A86-7029

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) re More

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. ARC-1986-A86-7034

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, More

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. ARC-1986-A86-7031

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. Gr More

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, it shows a surface dominated by many roughly circular, polygonal, and arcuate features between 30 and 50 km (18 and 30 miles ) across. Some resemble degraded impact craters of Mars, while others resemble the 'palimpsest' features of Jupiter's satellite Ganymede. Peculiar intersecting, double ridged lines are 15 to 20 km. or 9 to 12 miles wide and hundreds of kilometers long. Theyresemble some deformational belts of Ganymede. Patches of plainsforming material tend to occur in local depressions. The geologic features of Triton and spectroscopic information indicates that the surface of Triton is underlain by a mixture of ices. ARC-1989-A89-7030

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, it shows a More

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. ARC-1989-A89-7026

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 More

Voyager II Imagery, Neptune: This is one of the most detailed views of the surface of Triton taken by Voyager 2 on its flyby of the large satellite of Neptune early in the morning of August 25, 1989. The picture was stored on the tape recorder and relayed to Earth later. Taken from a distanT ce of only 40,000 km (25, 000 miles), the frame is about 220 kilometers (140 miles) across and shows details as small as 750 meters (0.5 miles). Most of the area is covered by a peculiar landscape of roughly circular depressions separated by rugged ridges. This type of terrain, which covers large tracts of Triton's northern hemisphere, is unlike anything seen elsewhere in the solar system. The depressions are probably not impact craters: They are too similar in size and too regularly spaced. Their origin is still unknown, but may involve local melting and collapse of the icy surface. A conspicuous set of grooves and ridges cuts across the landscape, indicating fracturing and deformation of Triton's surface. The rarity of impact craters suggests a young surface by solar-system standards, probably less than a few billion years old. The Voyager Mission is conducted by JPL for NASA's Office of Space Science and Applications. (JPL ref: P-34722 Voyager N-60 ) ARC-1989-AC89-7055

Voyager II Imagery, Neptune: This is one of the most detailed views of the surface of Triton taken by Voyager 2 on its flyby of the large satellite of Neptune early in the morning of August 25, 1989. The pictur More

P-34668 This narrow angled image of Neptune's Triton, part of a sequence recieved from Voyager 2 shows a large flooded basin about 200 km. or 120 miles wide and 400 km. or 240 miles long. It appears to have been formed chiefly by two large, ancient craters. The walls of the basin have retreated, possibly as a consequence of sapping or collapse into the fluid that filled the main floor. The vent from which the flood evidently erupted lies near the right hand end of the basin. The surface of the eruptive material is rough near the vent and along the center of the basin, perhaps as a consequence of the presence of large rafts of ice. The absence of resolved impact craters on the floor of the basin indicatyes a young age for the flood. ARC-1989-A89-7028

P-34668 This narrow angled image of Neptune's Triton, part of a sequence recieved from Voyager 2 shows a large flooded basin about 200 km. or 120 miles wide and 400 km. or 240 miles long. It appears to have bee More

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. ARC-1989-A89-7048

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. Th More

This image shows a comparison between a Magellan image (right) and the highest resolution Earth-based radar image of Venus, obtained by the US National Astronomy and Ionosphere Center's Arecibo Observatory in Puerto Rico. The small white bot in the Arecibo image on the left corresponds to the Magellan image. This portion of a Magellan radar image strip shows a small region on the east flank of a major volcanic upland called Beta Regio. The image is centered a t 23 degrees north latitude and 286.7 degrees east longitude. The ridge and valley network in the middle part of the image is formed by intersecting faults which have broken the Venusian crust into a complex deformed type of surface called tessera, the Latin word for tile. The parallel mountains and valleys resemble the Basin and Range Province kn the western United States. The irregular dark patch near the top of the image is a smooth surface, proboably formed by lava flows in a region about 10 km (6 mi.) across. Similar dark surfaces within the valleys indicate lava flows that are younger than the tessera. The Arecibo image contains probable impact craters, mapped in detail by Magellan. The Magellan image has a resolution of 120 meters, (400 feet). The image segment is 20 km (12.4 mi.) wide adn 150 km (90 mi.) long. The Arecibo image has a resolution of 1-3 km (0.6-1.8 mi.) and is approx. 900 km (550 mi.) across. ARC-1990-A90-3002

This image shows a comparison between a Magellan image (right) and the highest resolution Earth-based radar image of Venus, obtained by the US National Astronomy and Ionosphere Center's Arecibo Observatory in P More

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. ARC-1990-A90-3003

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 ( More

This three-dimensional representation of brightness variations in a Magellan radar image of Golubkina crater enhances the structural features of the crater. Golubkina is 34 kimometers (20.4 mi.) in diameter, and is located at about 60.5 degrees north latitude, 287.2 degrees east longitude. Golubkina is characterized by terraced inner walls and a central peak, typical of large impact craters on the Earth, Moon and Mars. The terraced inner walls form at late stages in the formation of an impact crater, due to collapse of the initial cavity formed by the meterorite impact. The central peak forms due to rebound of the inner crater floor. ARC-1990-A90-3005

This three-dimensional representation of brightness variations in a Magellan radar image of Golubkina crater enhances the structural features of the crater. Golubkina is 34 kimometers (20.4 mi.) in diameter, a More

This dynamic planet : world map of volcanoes, earthquakes, impact craters, and plate tectonics /

Available also through the Library of Congress Web site as a raster image.

Natural color view of Ganymede. NASA public domain image colelction.

Description Natural color view of Ganymede from the Galileo spacecraft during its first encounter with the satellite. North is to the top of the picture and the sun illuminates the surface from the right. The d More

Oberon at Voyager Closest Approach

This image of Oberon, Uranus outermost moon, was captured by NASA Voyager 2 on Jan. 24, 1986. Clearly visible are several large impact craters in Oberon icy surface surrounded by bright rays. http://photojourn More

Venus - Adivar Crater, NASA Magellan spacecraft

Many of the impact craters of Venus revealed by NASA Magellan spacecraft have characteristics unlike craters on any other planetary body. This crater, named Adivar, is located just north of the western Aphrodit More

Mosaic of Large Impact Craters. NASA public domain image colelction.

This mosaic from NASA Magellan data is in the Lavinia region of Venus. Three large impact craters can be seen located in a region of fractured plains. http://photojournal.jpl.nasa.gov/catalog/PIA00086 NASA/JPL

Callisto False Color, Voyager Program, NASA/JPL Photo

This false color picture of Callisto was taken by NASA's Voyager 2 on July 7, 1979 at a range of 1,094,666 kilometers (677,000 miles) and is centered on 11 degrees N and 171 degrees W. This rendition uses an ul More

Europa During Voyager 2 Closest Approach

This color image of the Jovian moon Europa was acquired by NASA Voyager 2 during its close encounter on Jul. 9, 1979. Europa, the size of our moon, is thought to have a crust of ice perhaps 100 kilometers thick More

Venus - Possible Remnants of a Meteoroid in Lakshmi Region

This full resolution mosaiced image covers an area of approximately 100 kilometers by 120 kilometers (62 by 74 miles) and is located in the Lakshmi region of Venus at 47 degrees north latitude and 334 east long More

Northeast View from Viking Landing Site

This Mars view looks northeast from Nasa's Viking 1 and completes the 360 panorama of the landing site begun earlier with the spacecraft's other camera. A layer of haze can be seen in the Martian sky. Large dar More

Ganymede At 150,000 Miles, Voyager Program, NASA/JPL Photo

This picture of Ganymede, Jupiter's largest satellite, was taken by NASA's Voyager 1 on the afternoon of March 5, 1979, from a range of about 250,000 km (150,000 mi.). The center of the picture is at 60 north l More

A Chain of Impact Craters on Callisto

A portion of a chain of impact craters on Jupiter's moon Callisto is seen in this image taken by the Galileo spacecraft on November 4, 1996. This crater chain on Callisto is believed to result from the impact o More

Ridges on Europa, NASA / JPL Europa Image

This view of Jupiter's moon Europa shows a portion of the surface that has been highly disrupted by fractures and ridges. This picture covers an area about 238 kilometers (150 miles) wide by 225 kilometers (140 More

Dark-floored Impact Craters on Ganymede

Dark-floored Impact Craters on Ganymede NASA/JPL/Brown University

Impact Craters on Icy Callisto: Doh Crater and Asgard

Impact Craters on Icy Callisto: Doh Crater and Asgard NASA/JPL/ASU

Mars and Syrtis Major, NASA history collection

Taking advantage of Mars's closest approach to Earth in eight years, astronomers using NASA's Hubble Space Telescope have taken the space- based observatory's sharpest views yet of the Red Planet. The telescope More

Impact Craters on Xanadu - NASA Titan images

Impact Craters on Xanadu NASA/JPL-Caltech/ASI Public domain photograph of a solar system, planet, space exploration, free to use, no copyright restrictions image - Picryl description

Ten Newly Named Impact Craters on Mercury

Ten Newly Named Impact Craters on Mercury NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Taking the Measure of Impact Craters on Mercury

Taking the Measure of Impact Craters on Mercury NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Spatter Cone - free images of Idaho

Once thought to resemble the Moon, Craters of the Moon's features are borne from volcanic eruptions, not impact craters as on the lunar surface.

Fresh Cluster of Impact Craters on Mars

This set of images from cameras on NASA Mars Reconnaissance Orbiter documents the appearance of a new cluster of impact craters on Mars. The orbiter has imaged at least 248 fresh craters, or crater clusters, on More

Public domain stock image. Moon moon by night lunar.

A half moon in a blue sky with clouds. Moon moon by day lunar.

The moon in the sky / The moon in the sky public domain stock photo.

Bosumtwi Worldwind SW

Lake Bosumtwi, Ghana, view from Southwest. Bosumtwiis a lake-filled impact crater, about 10.5 km in size an 1.3 million years old. Vertical exaggeration 3x.

Voyage in Space page185

Relief models of part of the surface of the Moon (left), and Vesuvius and Bay of Naples (right).

Barringer Crater aerial photo by USGS

The origin of this classic, simple meteorite impact crater was long the subject of controversy. The discovery of fragments of the Canyon Diablo meteorite, including fragments within the breccia deposits that p More

Ausschnitt des Nördlinger Rieses aus der "Geognostischen Karte von Deutschland und den umliegenden Staaten in 42 Blättern, Berichtigt 1833, IV Auflage 1834

Deutsch: Geologisches Blatt „Mannheim“ der von dem Verlag von Simon Schropp et Comp. herausgegebenen, sehr großen Gesamtkarte Geognostische Karte von Deutschland und den umliegenden Staaten in 42 Blättern, Ber More