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<text>Before VoyagerΓÇÖs imaging of Uranus, Miranda was the smallest and closest moon known. Based on knowledge acquired during the fly-bys of Jupiter and Saturn, as well as the ongoing work and experience of NASA engineers, the Voyager photos of Miranda were of higher resolution than any taken since launch.Miranda is a scarred world, with an appearance unlike any other satellite in the solar system. It is possibly composed of the fragments of a larger body which was broken apart after it had formed and partially differentiated. The pieces could have regrouped into the body we see today, but it is also possible that Miranda was fractured by impacts more than once.</text>
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<text>This color composite of the Uranian satellite Miranda was taken by Voyager 2 on Jan. 24, 1986, from a distance of 147,000 kilometers (91,000 miles). This picture was constructed from images taken through the narrow-angle camera's green, violet and ultraviolet filters. It is the best color view of Miranda returned by Voyager. Miranda, just 480 km (300 mi) across, is the smallest of Uranus' five major satellites. Miranda's regional geologic provinces show very well in this view of the southern hemisphere, imaged at a resolution of 2.7 km (1.7 mi). The dark- and bright-banded region with its curvilinear traces covers about half of the image. Higher-resolution pictures taken later show many fault valleys and ridges parallel to these bands. Near the terminator (at right), another system of ridges and valleys abuts the banded terrain; many impact craters pockmark the surface in this region. The largest of these are about 30 km (20 mi) in diameter; many more lie in the range of 5 to 10 km (3 to 6 ml) in diameter.</text>
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<text>Before VoyagerΓÇÖs imaging of Uranus, Miranda was the smallest and closest moon known. Based on knowledge acquired during the fly-bys of Jupiter and Saturn, as well as the ongoing work and experience of NASA engineers, the Voyager photos of Miranda were of higher resolution than any taken since launch.Miranda is a scarred world, with an appearance unlike any other satellite in the solar system. It is possibly composed of the fragments of a larger body which was broken apart after it had formed and partially differentiated. The pieces could have regrouped into the body we see today, but it is also possible that Miranda was fractured by impacts more than once.</text>
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<text>Text for both pictures:The fifteen moons of Uranus, named for Shakespearean characters, are mostly under 160 km (100 miles) in diameter. The diagram of the inner orbits starts with the closest to the planet, Cordelia, at a distance of about 49,000 km. Moving outward, we find Ophelia, followed by five moons whose orbits appear as a band, because their orbits are too close together (between 59,200 and 66,100 km from the planet) to resolve at this scale. Rosalind, Belinda, and Puck (86,000 km from Uranus) are the last of the small moons; the outermost moon in the diagram, Miranda, is almost 500 km in diameter.The graphic of the outer orbits begins with Miranda, nearly 130,000 km from Uranus, and at increasing distances from the planet we find the four largest moons (all over 1,000 km in diameter). Oberon, the outermost satellite, orbits over 580,000 km from Uranus.</text>
<text>In this time of budget constraints, no new missions to Uranus and Neptune are being planned. However, the wealth of information provided by the Voyager spacecraft is still providing new information; these images and data have piqued our interest in these beautiful outer worlds. Major missions have been launched and designed for Jupiter and Saturn, respectively, so surely time will bring comprehensive missions to the other gas giants.</text>
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<text>Uranus was discovered in 1781 by William Herschel, who later discovered the satellites Titania and Oberon in 1787. William Lassell rediscovered Umbriel, which had been previously glimpsed by Herschel, and discovered Ariel in 1851. Gerard P. Kuiper discovered Miranda in 1948. Voyager 2 did first, as thus far only, close-up survey of Uranus in January 1986.</text>
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<text>All nine previously known rings of Uranus were photographed and measured by the Voyager spacecraft, as were other new rings and ringlets in the Uranian system. These observations showed that Uranus's rings are distinctly different from those at Jupiter and Saturn.Radio measurements showed the outermost ring, the epsilon ring, to be composed mostly of ice boulders several feet across. However, a very tenuous distribution of fine dust also seems to be spread throughout the ring system.Incomplete rings and the varying thicknesses in several of the main rings leads scientists to believe that the ring system may be relatively young and did not form at the same time as Uranus. The particles that make up the rings may be remnants of a moon that was broken by a high-velocity impact or torn up by gravitational effects.The number of known rings may eventually grow as a result of observations by the Voyager 2 photopolarimeter instrument. The sensor revealed what may be a large number of narrow rings -- or possibly incomplete rings or ring arcs -- as small as 50 meters (160 feet) in width. The individual ring particles were found to be of low reflectivity. At least one ring, the epsilon, was found to be gray in color. Important clues to Uranus's ring structure may come from the discovery that two small moons -- Cordelia and Ophelia -- straddle the epsilon ring. This finding lends credence to theories that small moonlets may be responsible for confining or deflecting material into rings and keeping it from escaping into space. Eighteen such satellites were expected to have been found, but only two were photographed.</text>
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<text>This picture of Uranus is a composite of four images returned Nov. 27, 1985, by the narrow-angle camera of Voyager 2. The spacecraft was about 74 million kilometers (46 million miles) from Uranus, inbound toward a Jan. 24, 1986, closest approach to the planet. At this range, Voyager 2 could detect clouds or other features in the atmosphere as small as 1,370 km (851 mi) across; no such features are yet visible. This view is toward the illuminated south pole of Uranus. The predominant blue color is the result of atmospheric methane, which absorbs the red wavelengths from incoming sunlight, thus rendering the planet bluish-green in hue. The spot at the upper left edge of the planet's disk resulted from the removal of a mark used in making measurements on the photograph. Three of Uranus' five known satellites are visible: Miranda (at far right, closest to the planet), Ariel (next out, at top) and Umbriel (lower left). Titania and Oberon are now outside the narrow-angle camera's field of view when it is centered on the planet. This color composite was made from images shuttered through blue, green, orange and clear filters.</text>
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<text>These two pictures of Uranus -- one in true color (left) and the other in false color -- were compiled from images returned Jan. 17, 1986, by the narrow-angle camera of Voyager 2. The spacecraft was 9.1 million kilometers (5.7 million miles) from the planet, seven days from closest approach. The picture at left has been processed to show Uranus as human eyes would see it from the vantage point of the spacecraft. The picture is a composed of images taken through blue, green and orange filters. The darker shadings at the upper right of the disk correspond to the day-night boundary on the planet. Beyond this boundary lies the hidden northern hemisphere of Uranus, which currently remains in total darkness as the planet rotates. The blue-green color results from the absorption of red light by methane gas in Uranus' deep, cold and remarkably clear atmosphere. The picture at right uses false color and extreme contrast enhancement to bring out subtle details in the polar region of Uranus. Images obtained through ultraviolet, violet and orange filters were respectively converted to the same blue, green and red colors used to produce the picture at left. The very slight contrasts visible in true color are greatly exaggerated here. In this false-color picture, Uranus reveals a dark polar hood surrounded by a series of progressively lighter concentric bands. One possible explanation is that a brownish haze or smog, concentrated over the pole, is arranged into bands by zonal motions of the upper atmosphere. Several artifacts of the optics and processing are visible. The occasional donut shapes are shadows cast by dust of the camera optics; the processing necessary to bring out faint features also brings out these camera blemishes. In addition, the bright pink strip at the lower edge of the planet's limb is an artifact of the image enhancement. In fact, the limb is dark and uniform in color around the planet.</text>
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<text>These two pictures of Uranus were compiled from images recorded by Voyager 2 on Jan. 10, 1986, when the NASA spacecraft was 18 million kilometers (11 million miles) from the planet. The images were obtained by Voyager's narrow-angle camera; the view is toward the planet's pole of rotation, which lies just left of center. The picture on the left has been processed to show Uranus as human eyes would see it from the vantage point of the spacecraft. The second picture is an exaggerated false-color view that reveals details not visible in the true-color view -- including indications of what could be a polar haze of smog-like particles. The true-color picture was made by combining pictures taken through blue, green and orange filters. The dark shading of the upper right edge of the disk is the terminator, or day-night boundary. The blue-green appearance of Uranus results from methane in the atmosphere; this gas absorbs red wavelengths from the incoming sunlight, leaving the predominant bluish color seen here. The picture on the right uses false color and contrast enhancement to bring out subtle details in the polar region of the atmosphere. Images shuttered through different color filters were added and manipulated by computer, greatly enhancing the low-contrast details in the original images. Ultraviolet-, violet- and orange-filtered images were displayed, respectively, as blue, green and red to produce this false-color picture. The planet reveals a dark polar hood surrounded by a series of progressively lighter convective bands. The banded structure is real, though exaggerated here. The brownish color near the center of the planet could be explained as being caused by a thin haze concentrated over the pole -- perhaps the product of chemical reactions powered by ultraviolet light from the Sun. One such reaction produces acetylene from methane -- acetylene has been detected on Uranus by an Earth-orbiting spacecraft -- and further reactions involving acetylene are known to produce reddish-brown smog-like particles. A similar haze envelopes Saturn's moon Titan; ground-based observations have predicted such a haze in the polar regions of Uranus. The exact identification of the reactions and their products will require additional study.</text>
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<text>This Voyager 2 photograph of Uranus is the first picture to show clear evidence of latitudinal banding in the planet's atmosphere and one of the first indicating atmospheric structure of any sort. The computer-enhanced picture is a summation of five images returned Dec. 27, 1985 by Voyager's narrow-angle camera. The spacecraft was 36 million kilometers (22 million miles) from Uranus. The concentric pattern emanates 1ike a bull's-eye from the planet's pole of rotation, which in this view lies 1eft of center. (Uranus lies almost on its side with respect to the other planets and is rotating in a counterclockwise direction as seen here.) Clouds in the Uranian atmosphere give rise to the pattern, the first clear photographic evidence of banding similar to that seen previously on Jupiter and Saturn. The banding on Uranus, however, shows much less contrast. At the distance at which the images were acquired, Voyager's camera could have detected individual features as small as 660 kilometers (410 miles) across, but no such clouds or markings were apparent. Scientists cannot yet say what properties -- such as cloud height, composition or particle size -- are giving rise to the varying 1evels of brightness visible here. The images composing this picture were shuttered through a filter that transmits only violet light. In the original, unprocessed images, the contrast of the features producing the banding is low -- no more than 10 percent. In order to reduce "noise" and enhance the visibility of the features, processors at JPL combined five raw images and then compared the resulting composite to a hypothetical featureless planet illuminated by the Sun from the proper direction. Only the ratio between the original data and the hypothetical image is shown.</text>
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<name>MAGNETIC FIELD</name>
<script>on mouseUpframeHilitelock screengo to cd "D8"unlock screenend mouseUp</script>
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<name>RINGS</name>
<script>on mouseUpframeHilitelock screengo to cd "D9"unlock screenend mouseUp</script>
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<type>field</type>
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<text>UranusPlanet statisticsDistance from the SunMaximum: 1,867 million miles 3,004 million km 20.088 AUMinimum: 1,699 million miles 2,735 million km 18.275 AUMean:1,783 million miles 2,870 million km 19.82 AUPeriod of revolution: 84.01 yearsPeriod of rotation (equatorial): 17 hr. 14 min.Mean orbital velocity: 4.2 miles (6.8 km) per secondInclination of axis: 97.9 degreesOrbital eccentricity: 0.047Orbital inclination: 0.774 degreesDiameter at equator: 31,770 miles (51,118 km) 4.01 x EarthΓÇÖs diameterOblateness: 0.023Mass: 8.66 x 10^25 kg 14.6 x EarthΓÇÖs massVolume: 7.26 x 10^13 km^3 67 x EarthΓÇÖs volumeDensity: 1.17 g/cm^3 0.23 x EarthΓÇÖs densitySurface gravity: 11.44 m/s^2 1.17 x EarthΓÇÖs gravityEscape velocity: 13.2 miles (21.3 km) per secondMean surface temperature: -353 F / -214 C / 59 K (at cloud tops)Maximum apparent diameter as seen from Earth (seconds of arc): 3.7"Number of known satellites: 15Mean diameter of Sun as seen from the planet: 1' 41"</text>
<script>on mouseUpframeHilitelock screengo to cd "D1"unlock screenend mouseUp</script>
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<font>Chicago</font>
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<name>MOONS</name>
<script>on mouseUpframeHilitelock screengo to cd "M1"unlock screenend mouseUp</script>
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<textAlign>center</textAlign>
<font>Chicago</font>
<textSize>12</textSize>
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<name>EXPLORATION</name>
<script>on mouseUpframeHilitelock screengo to cd "E1"unlock screenend mouseUp</script>
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<font>Chicago</font>
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<name>TOUR</name>
<script>on mouseUpframeHilitelock screengo to cd "T1"unlock screenend mouseUp</script>
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<name>main menu</name>
<script>on openCardlock screencolorizeHC "Add","PLANETS:URANUS:UI_MAC:URANUS.PIC"noPaintWhitepalette "uraMMenu","0,417"unlock screenend openCardon closeCardlock screencolorizeHC "colorFill" -- redraw previous screensunlock screenif there is a window "URANUS211KHz Movie" then ¬close window "URANUS211KHz Movie"noPaintWhiteif there is a window "uraMMenu" then ¬close window "uraMMenu"end closeCard</script>
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 (1994).iso/pc/uranus/uranus.hc/PATs.png){kind=link}