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<text>This bulls-eye view of Neptune's small dark spot (D2) was obtained by Voyager 2's narrow-angle camera on Aug. 24, 1989, when Neptune was within 1.1 million km (680,000 miles) of the planet. The smallest structures that can be seen are 20 km (12 miles) across. This unplanned photograph was obtained when the infrared spectrograph was mapping the planet, and is the highest-resolution view of the feature taken during the flyby. Banding surrounding the feature indicates unseen strong winds, while structures within the bright spot suggest both active upwelling of clouds and rotation about the center. A rotation rate has not yet been measured, but the V-shaped structure near the right edge of the bright area indicates that the spot rotates clockwise. Unlike the Great Red Spot on Jupiter, which rotates counterclockwise, if the D2 spot on Neptune rotates clockwise, the material will be descending in the dark oval region. The fact that infrared data will yield temperature information about the region above the clouds makes this observation especially valuable.</text>
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<text>This photograph shows the last face-on view of the Great Dark Spot that Voyager will make with the narrow-angle camera. The image was shuttered 45 hours before closest approach at a distance of 2.8 million kilometers (1.7 million miles). The smallest structures that can be seen are of an order of 50 kilometers (31 miles). The image shows feathery white clouds that overlie the boundary of the dark and light blue regions. The pinwheel (spiral) structure of both the dark boundary and the white cirrus suggest a storm system rotating counterclockwise. Periodic small-scale patterns in the white cloud, possibly waves, are short-lived and do not persist from one Neptunian rotation to the next. This color composite was made from the clear and green filters of the narrow-angle camera.</text>
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<text>This cylindrical projection view of Neptune uses five narrow-angle images equally spaced around the planet. They were taken over the course of a Neptunian day, an interval of about 18 hours. Latitude lines are horizontal in the image, and range from 80 degrees south to 30 degrees north of the equator. Near the center, the Great Dark Spot leaves a disturbed wave-like pattern that stretches around Neptune. Features further south move eastward at speeds up to 400 mph relative to the Great Dark Spot. The features are storms -- moving cloud systems that persist for months or longer. The weather forecast for Neptune is therefore continued high winds and cold with little change in temperature. The images were taken through the green filter from a distance of 10.5 million kilometers (6.5 million miles).</text>
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<text>This photograph of Neptune's southern hemisphere was taken by the narrow-angle camera on NASA's Voyager 2 when the spacecraft was 4.2 million km (2.6 million miles) from the planet. The smallest features that can be seen are 38 km (24 miles) across. The almond-shaped structure at the left is a large cloud system that has been seen for several weeks. Internal details in the feature have become increasingly apparent as Voyager 2 has approached. Systems with similar shapes in Jupiter's atmosphere rotate about their centers, rolling in the local winds that increase toward the south. However, the wispy nature of the white central clouds in this Neptunian feature make confirmation of the system's rotation difficult.</text>
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<text>In this false-color image of Neptune, objects that are deep in the atmosphere are blue, while those at higher altitudes are white. The image was taken by Voyager 2's wide-angle camera through an orange filter and two different methane filters. Light at methane wavelengths is mostly absorbed in the deeper atmosphere. The bright, white feature is a high-altitude cloud just south of the Great Dark Spot. The hard, sharp inner boundary within the bright cloud is an artifact of computer processing on Earth. Other, smaller clouds associated with the Great Dark Spot are white or pink, and are also at high altitudes. Neptune's limb looks reddish because Voyager 2 is viewing it tangentially, and the sunlight is scattered back to space before it can be absorbed by the methane. A long, narrow band of high-altitude clouds near the top of the image is located at 25 degrees north latitude, and faint hazes mark the equator and polar regions.</text>
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<text>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 Aug. 25, 1989. The picture was stored on the tape recorder and relayed to Earth later. Taken from a distance 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.</text>
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<text>This false color image of Triton is a composite of images taken through the violet, green and ultraviolet filters. The image was taken early on Aug. 25, 1989 when Voyager 2 was about 190,000 kilometers (118,000 miles) from Triton's surface. The smallest visible features are about 4 kilometers (2.5 miles) across. The image shows a geologic boundary between completely dark materials and patchy light/dark materials. A layer of pinkish material stretches across the center of the image. The pinkish layer must be thin because underlying albedo patterns show through. Several features appear to be affected by the thin atmosphere; the elongated dark streaks may represent particulate materials blown in the same direction by prevailing winds, and the white material may be frost deposits. Other features appear to be volcanic deposits including the smooth, dark materials alongside the long, narrow canyons. The streaks themselves appear to originate from very small circular sources, some of which are white, like the source of the prominent streak near the center of the image. The sources may be small volcanic vents with fumarolic-like activity. The colors may be due to irradiated methane, which is pink to red, and nitrogen, which is white.</text>
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<text>Voyager 2 took this picture of Neptune's largest satellite, Triton, from less than 80,000 km (50,000 miles). The image shows an area in Triton's northern hemisphere. The Sun is just above the horizon, so features cast shadows that accentuate height differences. The large, smooth area in the right-hand side of the image shows a single, fresh, impact crater. Otherwise there is no evidence of impacts such as those that have pocked the faces of most of the satellites Voyager 2 has visited. Many low cliffs in the area, bright where they face the Sun, and dark when they face away from it, suggest an intricate history for Triton. The cliffs might be due either to melting of surface materials or, possibly, caused by unusual fluid materials that flowed sometime in Triton's past. </text>
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<text>This Voyager 2 photo of Neptune's largest satellite, Triton, was part of a set received between 3:30 a.m. and 5:30 a.m., Aug. 25, 1989. 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, doubled ridge lines are 15 to 20 km (9 to 12 miles) wide and hundreds of kilometers long. They resemble some deformational belts of Ganymede. Patches of plains-forming material tend to occur in local depressions. The geologic features of Triton and spectroscopic information indicate that the surface of Triton is underlain by a mixture of ices.</text>
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<text>This photomosaic of Triton, assembled from 14 individual frames, shows the great variety of its surface features. At the bottom of the image are remnants of the south polar cap, containing "dark" streaks generally aligned towards the northeast (upper right: in the image). Even though these are darker than other features on Triton, they reflect nearly ten times as much light as the surface of the Earth's moon. North of the cap, in the western (left) half of the disk is the region which has been informally dubbed the "cantaloupe" terrain. Small dimples with upraised rims and shallow central depressions dot the area. Long fractures have opened allowing some icy material to ooze up and form a central ridge. These criss-cross the region and extend into parts of the polar cap region. Towards the south this terrain has a light covering of frost. Running east to the limb of Triton, just north of the polar cap, is an area of smooth plains and low hills which is the most densely cratered region seen. In the northeast (upper right) of this image are plains which show evidence for extensive resurfacing, including possible extrusions of flowing material onto the surface. This region also contains two large smooth areas reminiscent of the maria of the Earth's moon which were formed by large-scale volcanic flooding. Near the eastern (right) limb of Triton are three darker gray markings with sharply defined brighter borders. These are unlike anything else seen in the solar system, and their origin is not yet understood.</text>
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<text>Voyager violet, green, and ultraviolet images of Triton were map projected into cylindrical coordinates and combined to produce this false-color terrain map. Several compositionally distinct terrain and geologic features are portrayed. At center is a gray-blue unit referred to as "cantaloupe" terrain because of its unusual topographic texture. The unit appears to predate other units to the left. Immediately adjacent to the cantaloupe terrain, is a smoother unit, represented by a reddish color, that has been dissected by a prominent fault system. This unit apparently overlies a much higher albedo material, seen farther left. A prominent angular albedo boundary separates relatively undisturbed smooth terrain from irregular patches which have been derived from breakup of the same material. Also visible at the far left are diffuse, elongated streaks, which seem to emanate from circular, often bright-centered features. The parallel streaks may represent vented particulate materials blown in the same direction by winds in Triton's thin atmosphere.</text>
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<text>A several-kilometers-tall, geyser-like eruption of dark material is seen shooting almost straight up from the surface of Neptune's moon Triton in this Voyager 2 image, acquired on Aug. 24, 1989, from a distance of 99,920 kilometers (about 62,000 miles). This dark plume first discovered in stereo images taken by Voyager 2 consists of a narrow stem that rises vertically nearly eight kilometers (five miles), forming a cloud that drifts 150 kilometers (90 miles) westward in Triton's winds. The image shows the geyser-like column nearly in profile, as the spacecraft was only 16 degrees above the horizon as seen from Triton's surface at the base of the plume. While Voyager scientists are still trying to determine the mechanism responsible for the eruption, one possibility being considered is that pressurized gas, probably nitrogen, rises from beneath the surface and carries aloft dark particles, probably including carbon-rich materials and possibly ice crystals. The plume carries the particles to an altitude where they are left suspended as an westward-drifting cloud.</text>
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<text>Voyager 2 obtained this high-resolution color image of NeptuneΓÇÖs large satellite Triton during its close flyby on Aug. 25, 1989. Approximately a dozen individual images were combined to produce this comprehensive view of the Neptune-facing hemisphere of Triton. Fine detail is provided by high-resolution, clear-filter images, with color information added from lower-resolution frames. The large south polar cap at the bottom of the image is highly reflective and slightly pink in color; it may consist of a slowly evaporating layer of nitrogen ice deposited during the previous winter. From the ragged edge of the polar cap northward the satellite's face is generally darker and redder in color. This coloring may be produced by the action of ultraviolet light and magnetospheric radiation upon methane in the atmosphere and surface. Running across this darker region, approximately parallel to the edge of the polar cap, is a band of brighter white material that is almost bluish in color. The underlying topography in this bright band is similar, however to that in the darker, redder regions surrounding it. The Voyager Mission is conducted by JPL for NASA's Office of Space Science and Applications.</text>
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<text>Voyager 2 was 530,000 kilometers (330,000 miles) from Neptune's largest satellite, Triton, when this photo was taken, Aug. 24, 1989. With a resolution of 10 kilometers (6 miles), this is the first photo of Triton to reveal surface topography. The south pole, continuously illuminated by sunlight at this season, is at bottom left. The boundary between the bright southern hemisphere and the darker northern hemisphere is clearly visible. Both the darker regions to the north and the very bright sub-equatorial band show a complex pattern of irregular topography that somewhat resembles "fretted terrain" on parts of Venus and Mars. The pattern of dark and light regions over most of the southern hemisphere will require higher-resolution images for interpretation. Also evident are long, straight lines that appear to be surface expressions of internal, tectonic processes. No large impact craters are visible, suggesting that the crust of Triton has been renewed relatively recently -- that is, within the past billion years or less.</text>
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<text>This natural color image of the limb of Triton was taken early in the morning of Aug. 25 1989, when the Voyager 2 spacecraft was at a distance of about 210,000 kilometers (128,000 miles) from the icy satellite. The largest surface features visible are about 3 miles across. The picture is a composite of images taken through the violet, green and clear filters. The image shows a geologic boundary between a rough, pitted surface to the right and a smoother surface to the left. The change between surface types is gradual. The image also shows a color boundary between pinkish material in the upper part of the image and whiter material in the lower part. The geologic and color boundaries are not the same. That implies that whatever supplies the color is a very thin coating over a different underlying material in which the geologic boundary occurs. The colored coating may be a seasonal frost composed of compounds volatile enough to be sublimated at the very low temperatures (40 K to 50 K, or -387.4 F to -369.4 F) prevailing near Triton's surface. Possible compositions of the frost layer include methane (which turns red when irradiated), carbon monoxide or nitrogen. The color in this image is somewhat exaggerated: Triton is primarily a white object with a pinkish cast in some areas.</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> When Voyager flew within 5,000 kilometers (3,000 miles) of Neptune on August 25, 1989, the planet was the most distant member of the solar system from the Sun. (Pluto once again will become most distant in 1999.) Even though Neptune receives only three percent as much sunlight as Jupiter does, it is a dynamic planet and surprisingly showed several large, dark spots reminiscent of Jupiter's hurricane-like storms. The largest spot, dubbed the Great Dark Spot, is about the size of Earth and is similar to the Great Red Spot on Jupiter. A small, irregularly shaped, eastward-moving cloud was observed "scooting" around Neptune every 16 hours or so; this "scooter," as Voyager scientists called it, could be a cloud plume rising above a deeper cloud deck. Long, bright clouds, similar to cirrus clouds on Earth, were seen high in Neptune's atmosphere. At low northern latitudes, Voyager captured images of cloud streaks casting their shadows on cloud decks below. The strongest winds on any planet were measured on Neptune. Most of the winds there blow westward, or opposite to the rotation of the planet. Near the Great Dark Spot, winds blow up to 2,000 kilometers (1,200 miles) an hour. Triton, the largest of the moons of Neptune, was shown to be not only the most intriguing satellite of the Neptunian system, but one of the most interesting in all the solar system. It shows evidence of a remarkable geologic history, and Voyager 2 images showed active geyser-like eruptions spewing invisible nitrogen gas and dark dust particles several kilometers into the tenuous atmosphere. Triton's relatively high density and retrograde orbit offer strong evidence that Triton is not an original member of Neptune's family but is a captured object. If that is the case, tidal heating could have melted Triton in its originally eccentric orbit, and the moon might even have been liquid for as long as one billion years after its capture by Neptune. Voyager 2 solved many of the questions scientists had about Neptune's rings. Searches for "ring arcs," or partial rings, showed that Neptune's rings actually are complete, but are so diffuse and the material in them so fine that they could not be fully resolved from Earth. From the outermost in, the rings have been designated Adams, Plateau, Le Verrier and Galle. </text>
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<text>Neptune was the first planet to be discovered through mathematical calculation. Its position was predicted in 1845 by English astronomer John Couch Adams and Urbain Jean Joseph LeVerrier of France. In 1846, the planet was identified by Johanne Galle and Heinrich D'Arrest in Berlin. Triton was discovered by William Lassell in 1846. Nereid was discovered by G. P. Kuiper in 1949. Modern-day exploration of Neptune was conducted in 1989 by Voyager 2, which came within 4,850 km (3,010 miles) of the planet on August 25.</text>
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<text>The Voyager spacecraft was 8.6 million kilometers (5.3 million miles) from Neptune when it took this 61-second exposure through the clear filter with the narrow angle camera on August 19, 1989. The Voyager cameras were programmed to make a systematic search for faint ring arcs and new satellites. The bright upper corner of the image is due to a residual image from a previous long exposure of the planet. The portion of the arc visible here is approximately 35 degrees in longitudinal extent, making it approximately 38,000 kilometers (24,000 miles) in length, and is broken up into three segments separated from each other by approximately 5 degrees. The trailing edge is at the upper right and has an abrupt end while the leading edge seems to fade into the background more gradually. This arc orbits very close to of the newly discovered Neptune satellites, 1989N4. Close-up studies of this ring arc will be carried out in the coming days which will give higher spatial resolution at different lighting angles.</text>
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<text>The Voyager spacecraft took this picture after closest approach to Neptune on Aug. 25 1989, using the clear filter of the wide-angle camera with an exposure time of 255 seconds. The view back towards Neptune at a phase angle of 135 degrees found the two known rings to be five to 10 times brighter than seen in backscattering during Voyager approach at much lower phase angle. This brightness increase implies a large percentage of microscopic particles within the rings. Although the dominant arc-like clump of the outer ring is not seen here, the inner ring appears brighter than the outer ring at the longitudes seen in this image. A faint sheet of material is also revealed that extends from the faint ring at a radius of 53,200 kilometers (33,000 miles). A new and even fainter ring was discovered in this image at about 41,000 kilometers (25,400 miles), seen running from the lower left corner to about one-third the way across the top of the frame. This ring is quite broad, about 2,500 kilometers (1,550 miles) in radial width. In contrast to the two previously discovered rings, this feature is quite diffuse and has no well defined radial boundaries. The Voyager stellar occultation experiments. The Voyager spacecraft was 720,000 kilometers (446,400 miles) from Neptune at the time of this exposure.</text>
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<text>This wide-angle Voyager 2 image, taken through the camera's clear filter, is the first to show Neptune's rings in detail. The two main rings, about 53,000 km (33,000 miles) and 63,000 km (39,000 miles) from Neptune, are 5 to 10 times brighter than in earlier images. The difference is due to lighting and viewing geometry. In approach images, the rings were seen in light scattered backward toward the spacecraft at a 15-degree phase angle. However, this image was taken at 135 degree phase angle as Voyager left the planet. That geometry is ideal for detecting microscopic particles that forward-scatter light preferentially. The fact that Neptune's rings are so much brighter at that angle means the particle-size distribution is quite different from most of Uranus' and Saturn's rings, which contain fewer dust-size grains. However, a few components of the Saturnian and Uranian ring systems exhibit forward-scattering behavior: The F ring and the Encke Gap ringlet at Saturn, and 1986U1R at Uranus. They are also narrow, clumpy ringlets with kinks, and are associated with nearby moonlets too small to detect directly. In this image, the main clumpy arc, composed of three features each about 6 to 8 degrees long,. is clearly seen. This image was obtained when Voyager was 1.1 million km (683,000 miles) from Neptune. Exposure time was 111 seconds.</text>
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<text>This Voyager 2 wide-angle photograph of the shadow of Neptune on the rings was taken Aug. 25, 1989 from a distance of 660,000 kilometers (412,000 miles). Because Neptune's pole is tilted toward the sun by about 27 degrees, Neptune's shadow casts a curved profile on the rings which does not quite reach out to the outermost ring at about 38,000 kilometers (24,000 miles) from the cloudtops. In this photo taken through the clear filter at a phase angle of about 135 degrees, the shadow does fall on the inner bright ring [at about 28,000 kilometers (18,000 miles) from the cloudtops]. The shadow also clearly delineates the radial extent of the broad sheet of material discovered extending from about halfway between the bright rings down to, and perhaps beyond the inner bright ring. A very thin, brighter component of the edge of this diffuse sheet can also be seen. Additional information from other images indicates that this faint material extends further in, to at least the position of the innermost faint ring discovered at about 17,000 kilometers (11,000 miles) from the cloudtops.</text>
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<text>This Voyager 2 high resolution color image, taken 2 hours before closest approach, provides obvious evidence of vertical relief in Neptune's bright cloud streaks. These clouds were observed at a latitude of 29 degrees north near Neptune's east terminator. The linear cloud forms are stretched approximately along lines of constant latitude and the sun is toward the lower left. The bright sides of the clouds which face the sun are brighter than the surrounding cloud deck because they are more directly exposed to the sun. Shadows can be seen on the side opposite the sun. These shadows are less distinct at short wavelengths (violet filter) and more distinct at long wavelengths (orange filter). This can be understood if the underlying cloud deck on which the shadow is cast is at a relatively great depth, in which case scattering by molecules in the overlying atmosphere will diffuse light into the shadow. Because molecules scatter blue light much more efficiently than red light, the shadows will be darkest at the longest (reddest) wavelengths, and will appear blue under white light illumination. The resolution of this image is 11 kilometers (6.8 miles per pixel) and the range is only 157,000 kilometers (98,000 miles). The width of the cloud streaks range from 50 to 200 kilometers (31 to 124 miles), and their shadow widths range from 30 to 50 kilometers (18 to 31 miles). Cloud heights appear to be of the order of 50 kilometers (31 miles). This corresponds to 2 scale heights.</text>
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<text>The bright cirrus-like clouds of Neptune change rapidly, often forming and dissipating over periods of several to tens of hours. In this sequence spanning two rotations of Neptune (about 36 hours) Voyager 2 observed cloud evolution in the region around the Great Dark Spot (GDS) at an effective resolution of about l00 kilometers (62 miles) per pixel. The surprisingly rapid changes which occur over the 18 hours separating each panel shows that in this region Neptune's weather is perhaps as dynamic and variable as that of the Earth. However, the scale is immense by our standards -- the Earth and the GDS are of similar size -- and in Neptune's frigid atmosphere, where temperatures are as low as 55 degrees Kelvin (-360 F), the cirrus clouds are composed of frozen methane rather than Earth's crystals of water ice.</text>
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<text>NeptunePlanet statisticsDistance from the Sun Maximum: 2,817 million miles 4,537 million km 30.316 AU Minimum: 2,769 million miles 4,456 million km 29.800 AU Mean: 2,793 million miles 4,497 million km 30.058 AUPeriod of revolution: 164.8 yearsPeriod of rotation (equatorial): 16 hr. 3 min. or 19 hr. 12 min.Mean orbital velocity: 3.4 miles (5.4 km) per secondInclination of axis: 29.6 degreesOrbital eccentricity: 0.009Orbital inclination: 1.77 degreesDiameter at equator: 30,780 miles (49,528 km) 3.96 x EarthΓÇÖs diameterOblateness: 0.017Mass: 1.02 x 10^26 kg 17.2 x EarthΓÇÖs massVolume: 6.18 x 10^13 km^3 54 x EarthΓÇÖs volumeDensity: 1.64 g/cm^3 0.32 x EarthΓÇÖs densitySurface gravity: 11.0 m/s^2 (Earth = 1): 1.12Escape velocity: 14.5 miles (23.3 km) per secondMean surface temperature: -364 F / -220 C / 53 K (at cloud tops)Maximum apparent diameter as seen from Earth (seconds of arc): 2.2"Albedo: 0.4Number of known satellites: 8Mean diameter of Sun as seen from the planet: 1' 04"</text>
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<script>on openCardlock screencolorizeHC "Add","PLANETS:NEPTUNE:UI_MAC:NEPTUNE.PIC"noPaintWhitepalette "nepMMenu","0,417"unlock screenend openCardon closeCardlock screencolorizeHC "colorFill" -- redraw previous screensunlock screenif there is a window "NEPTUNE211KHz Movie" then ¬close window "NEPTUNE211KHz Movie"noPaintWhiteif there is a window "nepMMenu" then ¬close window "nepMMenu"end closeCard</script>
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