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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-29512 BW Range: 36,000 kilometers (22,000 miles) Miranda, innermost of Uranus' large satellites, is seen at close range as part of a Voyager 2 high-resolution mosaicking sequence. This clear-filter, narrow-angle image shows an area about 250 km (150 mi) across, at a resolution of about 800 meters (2,600 feet). Two distinct terrain types are visible; a rugged, higher-elevation terrain (right) and a lower, striated terrain. Numerous craters on the rugged, higher terain indicate that it is older than the lower terrain. Several scarps, probably faults, cut the different terrains. The impact crater in the lower part of this image is about 25 km (15 mi) across. ARC-1986-A86-7028
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-29519BW Range: 500,000 kilometers (300,000 miles) Several craters are seen on the surface of 1986U1, one of the several small moons of Uranus discovered by Voyager 2. This single image, a clear-filtered, narrow-angle picture with a resolution of about 10 km (6 mi), is the only closeup the spacecraft obtained of any of the new moons. The moon was found December 30, 1985; it was the first and largest of nine satellites discovered by the spacecraft's cameras. This image shows 1986U1 to be a dark, nearly spherical object, with a diameter of about 150 km (90 mi); the dark surface reflects only 7 percent of the incident light. The picture was inserted into the Voyager encounter sequence late in its development.This image has had a complex history, having been recorded on the spacecraft tape recorder and first played back during the late afternoon of its recording. An antenna-pointing problem at one of the Austrailian tracking stations led to the loss of the data, so the image had to be retransmitted. ARC-1986-A86-7035
P-29521 BW Range: 557,000 kilometers ( 346, 000 miles) The southern hemisphere of Umbriel displays heavy cratering in this Voyager 2 image. This frame, taken through the clear-filter of Voyager's narrow-angle camera, is the most detailed image of Umbriel, with a resolution of about 10 km (6 mi). Umbriel is the darkest of Uranus' larger moons and the one that appears to have experienced the lowest level of geological activity. It has a diameter of about 1,200 km (750 mi) and reflects only 16 percent of the light striking its surface; in the latter respect, Umbriel is similiar to lunar highland areas. Umbriel is heavily cratered but lacks the numerous bright-ray craters seen on the other large Uranian satellites; this results in a relatively uniform surface albedo (reflectivity). The prominent crater on the terminator (upper right) is about 110 km (70 mi) across and has a bright central peak. The strangest feature in this image (at top) is a curious bright ring, the most reflective area seen on Umbriel. The ring is about 140 km (90 mi) in diameter and lies near the satellite's equator. The nature of the ring is not known, although it might be a frost deposit, perhaps associated with an impact crater. Spots against the black background are due to 'noise' in the data. ARC-1986-A86-7037
P-29511 BW Range: 130,000 kilometers (80,000 miles) This clear-filter, narrow-angle picture is part of the high-resolution Voyager 2 imaging sequence of Ariel, a moon of Uranus about 1,300 kilometers (800 miles) in diameter. The complexity of Ariels' surface indicates that a variety of geologic processes have occured. The numerous craters, for example, are indications of an old surface bombarded by meteroids over a long periond. Also conspicuous at this resolution, about 2.4 km (1.5 mi), are linear grooves (evidence of tectonic activity that has broken up the surface) and smooth patches (indicative of deposition of material). ARC-1986-A86-7027
P-21756 BW only Range: 120,000 km (right) 169,000 km (left) Right: In the foreground of this picture taken by Voyager 2, the part of the surface of Ganymede shown is the typical grooved terrain as seen by Voyager 1. It consists of mutually intersecting bands of closely-spaced, parallel ridges and grooves. In the background is newly-cratered dark terrain across which can be traced several widely spaced parellel linear features. When viewed from a distance the line features appear to trace broad circular areas. The features resemble the circular ridges on Callisto that surround an almost complete annealed impact basin. The feature on Ganymede may be of similar origin but all traces of the impact itself have been destroyed. Left: This picture of Ganymede shows that the dark contrast terrain is separated by bright bands of grooved terain. The band of closely spaced linear grooves in the foreground is 150 km across and appears to be offset by another narrow band at right angles, as though by faulting. A variety of ray patterns are seen around the craters. One is in the left of the picture, it has prominent dark rays around an inner bright halo. Other craters have dark haloes; others have diffuse bright rays. The variation of albedo patterns around the craters may be indications of layering in the surface materials. The intensity of the craters suggests the dark areas are extremely old. The bright grooved terrain is less cratered and probably somewhat younger. ARC-1979-A79-7085
P-29510BW Range: 150,000 kilometers (90,000 miles) Nearly the full disk of Miranda can be seen in this clear-filter image taken by Voyager's narrow-angle camera. At this resolution, about 2.7 km (1.7 mi), only two distinct terrain types are visible. One is a bright, rugged, heavily-cratered region seen along the bottom of the disk and extending to the top in a narrow band. The second terrain type is a topographically lower, darker, grooved terrain along the two upper sides in this image. The dark areas had been visible for several days before closest approach in lower-resolution views of the satellite. Scarps, or cliffs, visible along the limbs have a rugged relief of several kilometers in height. ARC-1986-A86-7026
P-21739 BW Range: 4.7 million kilometers (2.9 million miles) This picture of Io was taken as Voyager 2 closes in on the Jovian system. Scientists are studying these distant views of Io for evidences of changes since Voyager 1 observations in March of 79. Voyager 1 discovered that Io, the innermost of the Galilean satellites, is the most volcanically active body yet seen in the solar system, surpassing even earth. In this picture, the first volcano discovered by Voyager 1 is again visible in the lower left portion of the disk as a dark oval with a dark spot in the center. In March, this volcano appeared as a heart-shaped marking, not a symmetrical oval. Scientists believe that the non-symmetric markings earlier resulted from a constriction in the mouth of the volcanic vent causing erupting material to extrude preferentially in certain directions. Apparently, the volcanic eruptive activity, which sends material to altitudes of 280 kilometers (175 miles) or more above this volcano, has changed the vent geometry or dislodged an obstruction. Such changes in the form of eruptive fountains are common in terrestial volcanos, although on a much smaller scale than on Io. ARC-1979-A79-7074
P-29514 BW Miranda reveals a complex geologic history in this view acquired by Voyager 2 around its closest approach to the Uranian moon. At least three terrain types of different age and geologic style are evident at this resolution of about 700 meters (2,300 feet). Visible in this clear-filter, narrow-angle image are from left: 1) an apparently ancient, cratered terrain consisting of rolling, subdued hills and degraded medium-sized craters; 2) a grooved terrain with linear valleys and ridges developed at the expense of, or replacing, the first terrain type; and 3) a complex terrain seen along the terminator, in which intersecting curvillinear ridges and troughs are abrubtly truncated by the linear, grooved terrain. Voyager scientists believe this third terrain type is intermediate in age between the first two. ARC-1986-A86-7030
Summary
P-29514 BW Miranda reveals a complex geologic history in this view acquired by Voyager 2 around its closest approach to the Uranian moon. At least three terrain types of different age and geologic style are evident at this resolution of about 700 meters (2,300 feet). Visible in this clear-filter, narrow-angle image are from left: 1) an apparently ancient, cratered terrain consisting of rolling, subdued hills and degraded medium-sized craters; 2) a grooved terrain with linear valleys and ridges developed at the expense of, or replacing, the first terrain type; and 3) a complex terrain seen along the terminator, in which intersecting curvillinear ridges and troughs are abrubtly truncated by the linear, grooved terrain. Voyager scientists believe this third terrain type is intermediate in age between the first two.
In 1977, Voyager 1 and 2 started their one-way journey to the end of the solar system and beyond, now traveling a million miles a day. Jimmy Carter was president when NASA launched two probes from Cape Canaveral. Voyager 1 and its twin, Voyager 2, were initially meant to explore Jupiter, Saturn, and their moons. They did that. But then they kept going at a rate of 35,000 miles per hour. Each craft bears an object that is a record, both dubbed the Golden Records. They were the product of Carl Sagan and his team who produced a record that would, if discovered by aliens, represent humanity and "communicate a story of our world to extraterrestrials."
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arc
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ames research center
miranda
bw miranda
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voyager
approach
uranian
moon
uranian moon
terrain
types
three terrain types
style
resolution
meters
visible
clear filter
narrow angle
narrow angle image
hills
craters
valleys
ridges
expense
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third terrain type
first two
high resolution
p 29514 bw miranda
history
nasa
geography
travel and description
Date
24/01/1986
in collections
Location
Exit 398A
,
37.40750, -122.06528
Source
NASA
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Copyright info
Public Domain Dedication (CC0)