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Zusammenstellung ausgewählter Bilder zur Venus, die um weiterführenden Links mit der Möglichkeit des Downloads ergänzt wurden.

  • Venus, globale Ansicht zentriert auf 180° O

    Venus, globale Ansicht zentriert auf 180° O

    This global view of the surface of Venus is centered at 180 degrees east longitude. Magellan synthetic aperture radar mosaics from the first cycle of Magellan mapping are mapped onto a computer-simulated globe to create this image. Data gaps are filled with Pioneer Venus Orbiter data, or a constant mid-range value. Simulated color is used to enhance small-scale structure. The simulated hues are based on color images recorded by the Soviet Venera 13 and 14 spacecraft. The image was produced by the Solar System Visualization project and the Magellan science team at the JPL Multimission Image Processing Laboratory and is a single frame from a video released at the October 29, 1991, JPL news conference.

    Bild: NASA/JPL

  • Venus, Teil der Eistla-Region

    Venus, Teil der Eistla-Region

    This Magellan full resolution mosaic, centered at 12.3 north latitude, 8.3 degrees east longitude, shows an area 160 kilometers by 250 kilometers in the Eistla region of Venus. The prominent circular features are volcanic domes, 65 kilometers in diameter with broad, flat tops less than one kilometer in height. Sometimes referred to as 'pancake' domes, they represent a unique category of volcanic extrusions on Venus formed from viscous (sticky) lava. The cracks and pits commonly found in these features result from cooling and the withdrawal of lava. A less viscous flow was emitted from the northeastern dome toward the other large dome in the southwest corner of the image.

    Bild: NASA/JPL

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  • Krater im nordwestlichen Teil von Lavinia Planitia

    Krater im nordwestlichen Teil von Lavinia Planitia

    Three impact craters are displayed in this three-dimensional perspective view of the surface of Venus. The center of the image is located at approximately 27 degrees south latitude, 339 degrees east longitude in the northwestern portion of Lavinia Planitia. The viewpoint is located southwest of Howe Crater, which appears centered in the lower portion of the image. Howe is a crater with a diameter of 37.3 kilometers located at 28.6 degrees south latitude, 337.1 degrees east longitude. Danilova, a crater with a diameter of 47.6 kilometers, located at 26.35 degrees south latitude, 337.25 degrees east longitude, appears above and to the left of Howe in the image. Aglaonice, a crater with a diameter of 62.7 kilometers, located at 26.5 degrees south latitude, 340 degrees east longitude, is shown to the right of Danilova. Magellan synthetic aperture radar data is combined with radar altimetry to develop a three-dimensional map of the surface. Rays cast in a computer intersect the surface to create a three-dimensional perspective view. Simulated color and a digital elevation map developed by the U.S. Geological Survey are used to enhance small-scale structure. The simulated hues are based on color images recorded by the Soviet Venera 13 and 14 spacecraft.

    Bild: NASA/JPL

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  • Venus, Krater in der Region Lavinia

    Venus, Krater in der Region Lavinia

    One of the most useful Magellan standard data products is the full resolution mosaic, the F-MIDR (Full-Resolution Mosaiced Image Data Record). These products are mosaics of about 500 kilometer segments of 30 or more individual image strips. This image is an F-MIDR made from orbits 376 to 407, obtained between September 15 and September 19, 1990, part of the first orbits in which the Magellan flight team operated the radar system in the mapping mode. The mosaic is centered at 27 degrees south latitude, 339 degrees longitude, in the Lavinia region of Venus. Three large impact craters with diameters ranging from 37 kilometers to 50 kilometers can be seen located in a region of fractured plains. The craters show many features typical of meteorite impact craters, including rough, radar-bright ejecta, terraced inner walls and central peaks. Numerous domes of probable volcanic origin can be seen in the southeastern corner of the mosaic. The domes range in diameter from 1-12 kilometers, and some have central pits typical of volcanic shields or cones. Resolution of the Magellan data is about 120 meters.

    Bild: NASA/JPL

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  • Perspektivischer Blick auf Maat Mons

    Perspektivischer Blick auf Maat Mons

    Maat Mons is displayed in this computer generated three-dimensional perspective of the surface of Venus. The viewpoint is located 634 kilometers north of Maat Mons at an elevation of 3 kilometers above the terrain. Lava flows extend for hundreds of kilometers across the fractured plains shown in the foreground, to the base of Maat Mons. The view is to the south with the volcano Maat Mons appearing at the center of the image on the horizon and rising to almost 5 kilometers above the surrounding terrain. Maat Mons is located at approximately 0.9 degrees north latitude, 194.5 degrees east longitude with a peak that ascends to 8 kilometers above the mean surface. Maat Mons is named for an Egyptian Goddess of truth and justice. Magellan synthetic aperture radar data is combined with radar altimetry to develop a three-dimensional map of the surface. The vertical scale in this perspective has been exaggerated 10 times. Rays cast in a computer intersect the surface to crate a three-dimensional perspective view. Simulated color and a digital elevation map developed by the U.S. Geological Survey are used to enhance small-scale structure. The simulated hues are based on color images recorded by the Soviet Venera 13 and 14 spacecraft.

    Bild: NASA/JPL

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  • Krater Barton

    Krater Barton

    During orbits 404 through 414 on 19-20 September 1990, Magellan imaged a peak-ring crater that is 50 kilometers in diameter located at latitude 27.4 degrees north and longitude 337.5 degrees east. Barton is just at the diameter size that Venus craters appear to begin to possess peak-rings instead of a single central peak or central peak complex like does 75 percent of the craters with diameters between 50 and about 15 kilometers. The floor of the crater is flat and radar-dark, indicating possible infilling by volcanic deposits sometime following the impact event. Barton's central peak ring is discontinuous and appears to have been disrupted or separated during or following the cratering process. The extremely blocky crater deposits (ejecta) surrounding Barton appear to be most extensive on the southwest to southeast (lower left to right) side of the crater.

    Bild: NASA/JPL

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  • Globale Ansicht der Venus in Falschfarben

    Globale Ansicht der Venus in Falschfarben

    This colorized picture of Venus was taken February 14, 1990, from a distance of almost 1.7 million miles, about 6 days after Galileo's closest approach to the planet. It has been colorized to a bluish hue to emphasize subtle contrasts in the cloud markings and to indicate that it was taken through a violet filter. Features in the sulfuric acid clouds near the top of the planet's atmosphere are most prominent in violet and ultraviolet light. This image shows the east-to-west-trending cloud banding and the brighter polar hoods familiar from past studies of Venus. The features are embedded in winds that flow from east to west at about 230 mph. The smallest features visible are about 45 miles across. An intriguing filamentary dark pattern is seen immediately left of the bright region at the subsolar point (equatorial 'noon'). North is at the top and the evening terminator is to the left. The Galileo Project is managed for NASA's Office of Space Science and Applications by the Jet Propulsion Laboratory; its mission is to study Jupiter and its satellites and magnetosphere after multiple gravity-assist flybys at Venus and Earth.

    Bild: NASA/JPL

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  • Yavine Corona

    Yavine Corona

    The view shows a 100-km-wide nova superposed on Yavine Corona, a 500-km-wide asymmetric feature at latitude 5 degrees S., longitude 248.5 degrees; looking northeast. Coronae are roughly circular, volcanic features believed to form over hot upwellings of magma within the Venusian mantle. Yavine corona contains 2 novae; nova are circular hills with star-shaped fractures. The view is a close-up of the southern nova showing its fractures to be grabens or fault bound depressions. Novae may represent an intermediate stage in coronae formation.

    This is a three-dimensional perspective view of Venusian Terrains composed of reduced resolution left-looking synthetic-aperture radar images merged with altimetry data from the Magellan spacecraft.

    Bild: NASA/JPL/USGS

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  • Globale Ansicht der Venus zentriert auf 0° O, Höhe farbkodiert

    Globale Ansicht der Venus zentriert auf 0° O, Höhe farbkodiert

    The hemispheric view of Venus, as revealed by more than a decade of radar investigations culminating in the 1990-1994 Magellan mission, is centered at 0 degrees east longitude. The Magellan spacecraft imaged more than 98% of Venus at a resolution of about 100 meters; the effective resolution of this image is about 3 km. A mosaic of the Magellan images (most with illumination from the west) forms the image base. Gaps in the Magellan coverage were filled with images from the Earth-based Arecibo radar in a region centered roughly on 0 degree latitude and longitude, and with a neutral tone elsewhere (primarily near the south pole). The composite image was processed to improve contrast and to emphasize small features, and was color-coded to represent elevation. Gaps in the elevation data from the Magellan radar altimeter were filled with altimetry from the Venera spacecraft and the U.S. Pioneer Venus missions. An orthographic projection was used, simulating a distant view of one hemisphere of the planet.

    Bild: NASA/JPL/USGS

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  • Westlicher Teil der Eistla Regio mit Sif und Gula Mons

    Westlicher Teil der Eistla Regio mit Sif und Gula Mons

    A portion of western Eistla Regio is shown in this three dimensional, computer-generated view of the surface of Venus. The viewpoint is at an elevation of 1.2 kilometers at a location 700 kilometers southeast of Gula Mons, the volcano on the right horizon. Gula Mons reaches 3 kilometers high and is located around 22 degrees north latitude and 359 degrees east longitude. Sif Mons, the volcano on the left horizon, has a diameter of 300 kilometers (186 miles) and a height of 2 kilometers. Magellan imaging and altimetry data are combined to develop a three-dimensional computer view of the planet's surface. Simulated color based on color images from the Soviet Venera 13 and 14 spacecraft is added to enhance small-scale structure.

    Bild: NASA/JPL

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  • Ostrand der Alpha Regio mit domartigen Hügeln

    Ostrand der Alpha Regio mit domartigen Hügeln

    The eastern edge of Alpha Regio is shown in this image centered at 30 degrees south latitude and 11.8 degrees east longitude (longitude on Venus is measured from 0 degrees to 360 degrees east). Seven circular, dome-like hills, averaging 25 kilometers in diameter with maximum heights of 750 meters dominate the scene. These features are interpreted as very thick lava flows that came from an opening on the relatively level ground, which allowed the lava to flow in an even pattern outward from the opening. The complex fractures on top of the domes suggest that if the domes were created by lava flows, a cooled outer layer formed and then further lava flowing in the interior stretched the surface. The domes may be similar to volcanic domes on Earth. Another interpretation is that the domes are the result of molten rock or magma in the interior that pushed the surface layer upward. The near-surface magma then withdrew to deeper levels, causing the collapse and fracturing of the dome surface. The bright margins possibly indicate the presence of rock debris on the slopes of the domes. Some of the fractures on the plains cut through the domes, while others appear to be covered by the domes. This indicates that active processes pre date and post date the dome-like hills. The prominent black area in the northeast corner of the image is a data gap. North is at the top of the image.

    Bild: NASA/JPL

  • Maat Mons in 3D

    Maat Mons in 3D

    Maat Mons is displayed in this three-dimensional perspective view of the surface of Venus. The viewpoint is located 560 kilometers north of Maat Mons at an elevation of 1.7 kilometers above the terrain. Lava flows extend for hundreds of kilometers across the fractured plains shown in the foreground, to the base of Maat Mons. The view is to the south with Maat Mons appearing at the center of the image on the horizon. Maat Mons, an 8-kilometer high volcano, is located at approximately 0.9 degrees north latitude, 194.5 degrees east longitude. Maat Mons is named for an Egyptian goddess of truth and justice. Magellan synthetic aperture radar data is combined with radar altimetry to develop a three-dimensional map of the surface. The vertical scale in this perspective has been exaggerated 22.5 times. Rays cast in a computer intersect the surface to create a three-dimensional perspective view. Simulated color and a digital elevation map developed by the U.S. Geological Survey, are used to enhance small-scale structure. The simulated hues are based on color images recorded by the Soviet Venera 13 and 14 spacecraft.

    Bild: NASA/JPL

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  • Globale Ansichten der Venus in Echtfarbe und farbverstärkt aus neu prozessierten Daten

    Globale Ansichten der Venus in Echtfarbe und farbverstärkt aus neu prozessierten Daten

    As it sped away from Venus, NASA's Mariner 10 spacecraft captured this seemingly peaceful view of a planet the size of Earth, wrapped in a dense, global cloud layer. But, contrary to its serene appearance, the clouded globe of Venus is a world of intense heat, crushing atmospheric pressure and clouds of corrosive acid.

    This newly processed image revisits the original data with modern image processing software. A contrast-enhanced version of this view, also provided here, makes features in the planet's thick cloud cover visible in greater detail. The clouds seen here are located about 60 kilometers above the planet's surface, at altitudes where Earth-like atmospheric pressures and temperatures exist. They are comprised of sulfuric acid particles, as opposed to water droplets or ice crystals, as on Earth. These cloud particles are mostly white in appearance; however, patches of red-tinted clouds also can be seen. This is due to the presence of a mysterious material that absorbs light at blue and ultraviolet wavelengths. Many chemicals have been suggested for this mystery component, from sulfur compounds to even biological materials, but a consensus has yet to be reached among researchers.

    Bild: NASA/JPL-Caltech

  • Gula Mons in Eistla Regio

    Gula Mons in Eistla Regio

    Gula Mons is displayed in this computer-simulated view of the surface of Venus. The viewpoint is located 110 kilometers southwest of Gula Mons at the same elevation as the summit, 3 kilometers above Eistla Regio. Lava flows extend for hundreds of kilometers across the fractured plains. The view is to the northeast with Gula Mons appearing at the center of the image. Gula Mons, a 3 kilometer high volcano, is located at approximately 22 degrees north latitude, 359 degrees east longitude in western Eistla Regio. Magellan synthetic aperture radar data is combined with radar altimetry to produce a three-dimensional map of the surface. Rays cast in a computer intersect the surface to create a three-dimensional perspective view. Simulated color and a digital elevation map developed by the U.S. Geological Survey are used to enhance small-scale structure. The simulated hues are based on color images recorded by the Soviet Venera 13 and 14 spacecraft.

    Bild: NASA/JPL

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  • Krater Aurelia mit terrassierten Wänden und Zentralberg

    Krater Aurelia mit terrassierten Wänden und Zentralberg

    This Magellan image shows a complex crater, 31.9 kilometers in diameter with a circular rim, terraced walls, and central peaks, located at 20.3 degrees north latitude and 331.8 degrees east longitude. Several unusual features are evidenced in this image: large dark surface up range from the crater; lobate flows emanating from crater ejecta, and very radar-bright ejecta and floor. Aurelia has been proposed to the International Astronomical Union, Subcommittee of Planetary Nomenclature as a candidate name. Aurelia is the mother of Julius Caesar.

    Bild: NASA/JPL

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  • Alpha Regio in 3D, Teil des östlichen Randes

    Alpha Regio in 3D, Teil des östlichen Randes

    A portion of the eastern edge of Alpha Regio is displayed in this three-dimensional perspective view of the surface of Venus. The viewpoint is located at approximately 30 degrees south latitude, 11.8 degrees east longitude at an elevation of 2.4 kilometers. The view is to the northeast at the center of an area containing seven circular dome-like hills. The average diameter of the hills is 25 kilometers with maximum heights of 750 meters. Three of the hills are visible in the center of the image. Fractures on the surrounding plains are both older and younger than the domes. The hills may be the result of viscous or thick eruptions of lava coming from a vent on the relatively level ground, allowing the lava to flow in an even lateral pattern. The concentric and radial fracture patterns on their surfaces suggests that a chilled outer layer formed, then further intrusion in the interior stretched the surface. An alternative interpretation is that domes are the result of shallow intrusions of molten lava, causing the surface to rise. If they are intrusive, then magma withdrawal near the end of the eruptions produced the fractures. The bright margins possibly indicate the presence of rock debris or talus at the slopes of the domes.

    Bild: NASA/JPL

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  • Nordrand der Ovda Regio

    Nordrand der Ovda Regio

    This Magellan image shows part of the northern boundary of Ovda Regio, one of the large highlands ringing the equator of Venus. The scene consists largely of low-relief, rounded linear ridges. These ridges, 8-15 kilometers in width and 30-60 kilometers long, lie mostly along a 100-200 kilometer wide slope where the elevation drops 3 kilometers from Ovda Regio to the surrounding plains. Some of the ridges have been cut at right angles by extension fractures. Dark material, either lava or windblown dirt, fills the region between the ridges. The curvilinear, banded nature of these ridges suggests that crustal shortening, roughly oriented north-south, is largely responsible for their formation. Such crustal shortening was unexpected by Magellan scientists, who believed that Ovda Region, a likely site of hot upwelling from the interior of Venus, should be dominated by volcanism and crustal extension. This image, centered approximately at 1 degree north, 81 degrees east, measures 300 kilometers by 225 kilometers and was acquired by Magellan in November 1990.

    Bild: NASA/JPL

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  • Wolken der Venus auf der Nachtseite im Infrarot

    Wolken der Venus auf der Nachtseite im Infrarot

    This image is a false color version of a near infrared map of lower level clouds on the night side of Venus, obtained by the Near Infrared Mapping Spectrometer aboard the Galileo spacecraft as it approached the planet February 10, 1990. Taken from an altitude of about 60,000 miles above the planet, at an infrared wavelength of 2.3 microns (about three times the longest wavelength visible to the human eye) the map shows the turbulent, cloudy middle atmosphere some 30-33 miles above the surface, 6-10 miles below the visible cloudtops. The image shows the radiant heat from the lower atmosphere (about 400 degrees Fahrenheit) shining through the sulfuric acid clouds, which appear as much as 10 times darker than the bright gaps between clouds. The colors indicate relative cloud transparency; white and red show thin cloud regions, while black and blue represent relatively thick clouds. This cloud layer is at about 30 degrees Fahrenheit, at a pressure about 1/2 Earth's atmospheric pressure. 2/3 of the dark hemisphere is visible, centered on longitude 350 West, with bright slivers of daylit high clouds visible at top and bottom left. Near the equator, the clouds appear fluffy and blocky; farther north, they are stretched out into East West filaments by winds estimated at more than 150 mph, while the poles are capped by thick clouds at this altitude.

    Bild: NASA/JPL

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  • Teil des längsten der bisher entdeckten Kanäle auf der Venus

    Teil des längsten der bisher entdeckten Kanäle auf der Venus

    This compressed resolution radar mosaic from Magellan at 49 degrees north latitude, 165 degrees east longitude with dimensions of 460 by 460 kilometers, shows a 600 kilometers segment of the longest channel discovered on Venus to date. The channel is approximately 1.8 kilometers wide. At more than 7,000 kilometers long, it is several hundred kilometers longer than the Nile River, Earth's longest river, thus making it the longest known channel in the solar system. Both ends of the channel are obscured, however, so its original length is unknown. The channel was initially discovered by the Soviet Venera 15-16 orbiters which, in spite of their one kilometer resolution, detected more than 1,000 kilometers of the channel. These channel-like features are common on the plains of Venus. In some places they appear to have been formed by lava which may have melted or thermally eroded a path over the plains' surface. Most are 1 to 3 kilometers wide. They resemble terrestrial meandering rivers in some aspects, with meanders, cutoff bows and abandoned channel segments. However, Venus channels are not as tightly sinuous as terrestrial rivers. Most are partly buried by younger lava plains, making their sources difficult to identify. A few have vast radar-dark plains units associated with them, suggesting large flow volumes. These channels, with large deposits appear to be older than other channel types, as they are crossed by fractures and wrinkle ridges, and are often buried by other volcanic materials. In addition, they appear to run both upslope and downslope, suggesting that the plains were warped by regional tectonism after channel formation. Resolution of the Magellan data is about 120 meters.

    Bild: NASA/JPL

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  • Ushas Mons mit simulierter Farbe

    Ushas Mons mit simulierter Farbe

    Ushas Mons, a 2-kilometer-high volcano in the southern hemisphere of Venus is shown in this Magellan radar image. The image is centered at 25 degrees south latitude, 323 degrees east longitude, and shows an area approximately 600 kilometers on a side. The volcano is marked by numerous bright lava flows and a set of north-south trending fractures, many of which appear to have formed after the lavas were erupted onto the surface. In the central summit area, however, younger flows remain unfractured. An impact crater can be seen among the fractures in the upper center of the image. The association of faulting and volcanism is common on this type of volcano on Venus, and is believed to result from a large zone of hot material upwelling from the Venusian mantle, a phenomenon known on Earth as a "hot spot." Simulated color is used to enhance small-scale structures. The simulated hues are based on color images recorded by the Venera 13 and 14 landing craft. The data were acquired during the third eight-month cycle of Magellan's radar mapping, which ended in September 1992. Several narrow gaps in the Magellan coverage are filled with low-resolution radar data obtained by the Earth-based Arecibo radio telescope.

    Bild: NASA/JPL

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  • Bahet und Onatah Coronae in der Region Fortuna

    Bahet und Onatah Coronae in der Region Fortuna

    This mosaic of Magellan data in the Fortuna region of Venus, centered at 49 degrees north latitude, 2 degrees longitude, shows two coronae. Coronae are large circular or oval structures first identified in Soviet radar images of Venus. The structure on the left, Bahet Corona, is about 230 kilometers long and 150 kilometers across. A portion of Onatah Corona, over 350 kilometers in diameter, can be seen on the right of the mosaic. Both features are surrounded by a ring of ridges and troughs, which in places cut more radially-oriented fractures. The centers of the features also contain radial fractures as well as volcanic domes and flows. Coronae are thought to form due to the upwelling of hot material from deep in the interior of Venus. The two coronae may have formed at the same time over a single upwelling, or may indicate movement of the upwelling or the upper layers of the planet to the west over time. A 'pancake' dome, similar to low-relief domes see in the southern hemisphere, is located just to the southwest of Bahet. Resolution of the Magellan data is about 120 meters.

    Bild: NASA/JPL

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  • Schrägblick auf Krater Riley

    Schrägblick auf Krater Riley

    This Magellan full resolution radar mosaic centered at 14 degrees north latitude, 72 degrees east longitude, shows an oblique view of the impact crater Riley, named for Margaretta Riley, a 19th Century botanist. This view was prepared from two left-looking Magellan radar images acquired with different incidence angles. Because the relief displacements of the two images are different, depths from the crater rim to the crater floor and heights of the crater rim and flanks above the surrounding plains can be measured. The crater is 25 kilometers in diameter. The floor of the crater is 580 meters below the plains surrounding the crater. The crater's rim rises 620 meters above the plains and 1,200 meters above the crater floor. The crater's central peak is 536 meters high. The crater's diameter is 40 times the depth resulting in a relatively shallow appearance. The topography is exaggerated by 22 times to emphasize the crater's features.

    Bild: NASA/JPL

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  • Komplexes Netzwerk kleiner Brüche nahe Hestia Rupes

    Komplexes Netzwerk kleiner Brüche nahe Hestia Rupes

    This is a Magellan radar image covering a 105- kilometer by 45-kilometer (27-mile) region near Hestia Rupes on the northwestern corner of Aphrodite Terra. The complex network of narrow (<1 kilometer) fractures in the center of the image extends for approximately 50 kilometers (31 miles). This network exhibits tributary-like branches similar to those observed in river systems on Earth. However, the angular intersections of tributaries suggest tectonic control. These features appear to be due to drainage of lava along preexisting fractures and subsequent collapse of the surface. The underlying tectonic fabric can be observed in the northeast trending ridges which predate the plains.

    Bild: NASA/JPL

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  • Latrona Corona und Dali Chasma

    Latrona Corona und Dali Chasma

    This computer-generated perspective view of Latona Corona and Dali Chasma on Venus shows Magellan radar data superimposed on topography. The view is from the northeast and vertical exaggeration is 10 times. Exaggeration of relief is a common tool scientists use to detect relationships between structure (i.e. faults and fractures) and topography. Latona Corona, a circular feature approximately 1,000 kilometers in diameter whose eastern half is shown at the left of the image, has a relatively smooth, radar-bright raised rim. Bright lines or fractures within the corona appear to radiate away from its center toward the rim. The rest of the bright fractures in the area are associated with the relatively deep (approximately 3 kilometers) troughs of Dali Chasma. The Dali and Diana Chasma system consist of deep troughs that extend for 7,400 kilometers and are very distinct features on Venus. Those chasma connect the Ovda and Thetis highlands with the large volcanoes at Atla Regio and thus are considered to be the "Scorpion Tail" of Aphrodite Terra. The broad, curving scarp resembles some of Earth's subduction zones where crustal plates are pushed over each other. The radar-bright surface at the highest elevation along the scarp is similar to surfaces in other elevated regions where some metallic mineral such as pyrite (fool's gold) may occur on the surface.

    Bild: NASA/JPL

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  • Dunkle Lavaflüsse

    Dunkle Lavaflüsse

    This scene, which covers an area of 75 kilometers by 45 kilometers, shows an area of dark volcanic lava flows overlying the brighter surrounding plains which are thought to have been formed from older flows. Some of the dark flows terminate on the narrow bright sinuous feature to the right of the image and it is assumed that they originate from eruptions at fissures located along this bright feature. The image is located at latitude 4.6 degrees North and longitude 331.8 East. The horizontal banding is a processing artifact in this photo made from the first orbit after the start of systematic mapping.

    Bild: NASA/JPL

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  • Globale Ansicht der Venus zentriert auf 180° O, Höhe farbkodiert

    Globale Ansicht der Venus zentriert auf 180° O, Höhe farbkodiert

    The hemispheric view of Venus, as revealed by more than a decade of radar investigations culminating in the 1990-1994 Magellan mission, is centered at 180 degrees east longitude. The Magellan spacecraft imaged more than 98% of Venus at a resolution of about 100 meters; the effective resolution of this image is about 3 km. A mosaic of the Magellan images (most with illumination from the west) forms the image base. Gaps in the Magellan coverage were filled with images from the Earth-based Arecibo radar in a region centered roughly on 0 degree latitude and longitude, and with a neutral tone elsewhere (primarily near the south pole). The composite image was processed to improve contrast and to emphasize small features, and was color-coded to represent elevation. Gaps in the elevation data from the Magellan radar altimeter were filled with altimetry from the Venera spacecraft and the U.S. Pioneer Venus missions. An orthographic projection was used, simulating a distant view of one hemisphere of the planet.

    Bild: NASA/JPL/USGS

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  • Lavaflüsse in der Region Lada

    Lavaflüsse in der Region Lada

    This is a 225 meter per pixel Magellan radar image mosaic of Venus, centered at 47 degrees south latitude, 25 degrees east longitude in the Lada region. The scene is approximately 550 kilometers east-west by 630 kilometers (391 miles) north-south. The mosaic shows a system of east-trending radar-bright and dark lava flows encountering and breaching a north-trending ridge belt (left of center). Upon breaching the ridge belt, the lavas pool in a vast, radar-bright deposit (covering approximately 100,000 square kilometers [right side of image]). The source caldera for the lava flows, named Ammavaru, lies approximately 300 kilometers west of the scene.

    Bild: NASA/JPL

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  • Wolkenwirbel in der Atmosphäre am Südpol der Venus

    Wolkenwirbel in der Atmosphäre am Südpol der Venus

    This ghostly puff of smoke is actually a mass of swirling gas and cloud at Venus’ south pole, as seen by the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) aboard ESA’s Venus Express spacecraft.

    Venus has a very choppy and fast-moving atmosphere – although wind speeds are sluggish at the surface, they reach dizzying speeds of around 400 km/h at the altitude of the cloud tops, some 70 km above the surface. At this altitude, Venus’ atmosphere spins round some 60 times faster than the planet itself. This is very rapid; even Earth’s fastest winds move at most about 30% of our planet’s rotation speed. Quick-moving Venusian winds can complete a full lap of the planet in just four Earth days.

    Bild: ESA/VIRTIS/INAF-IASF/Obs. de Paris-LESIA/Univ. Oxford

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  • Wolken in der Venus-Atmosphäre

    Wolken in der Venus-Atmosphäre

    False-colour image of cloud features seen on Venus by the Venus Monitoring Camera (VMC) on Venus Express. The image was captured from a distance of 30 000 km on 8 December 2011.

    The VMC was designed and built by a consortium of German institutes lead by the Max-Planck Institute for Solar System Research in Katlenburg-Lindau.

    Venus Express has been in orbit around the planet since 2006.

    Bild: ESA/MPS/DLR/IDA

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