Galerie de photos de la planète Vénus

<h1>PIA00479: Venus - Complex Crater 'Dickinson' in NE Atalanta Region</h1><div class="PIA00479" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This Magellan image is centered at 74.6 degrees north latitude and 177.3 east longitude, in the northeastern Atalanta Region of Venus. The image is approximately 185 kilometers (115 miles) wide at the base and shows Dickinson, an impact crater 69 kilometers (43 miles) in diameter. The crater is complex, characterized by a partial central ring and a floor flooded by radar-dark and radar-bright materials. Hummocky, rough-textured ejecta extend all around the crater, except to the west. The lack of ejecta to the west may indicate that the impactor that produced the crater was an oblique impact from the west. Extensive radar-bright flows that emanate from the crater's eastern walls may represent large volumes of impact melt, or they may be the result of volcanic material released from the subsurface during the cratering event.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00479" onclick="window.open(this.href); return false;" title="Voir l'image PIA00479: Venus - Complex Crater 'Dickinson' in NE Atalanta Region sur le site de la NASA">Voir l'image PIA00479: Venus - Complex Crater 'Dickinson' in NE Atalanta Region sur le site de la NASA.</a></div>
PIA00479: Venus - Complex Crater 'Dickinson' in NE Atalanta Region
<h1>PIA00250: Venus - Wanda Crater in Akna Montes</h1><div class="PIA00250" lang="en" style="width:721px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This Magellan full-resolution images show the northern part of the Akna Montes (mountains) of Venus. The Akna range is a north-south trending ridge belt that forms the western border of the elevated smooth plateau of Lakshmi Planum (plains). The Lakshmi plateau plains are formed by extensive volcanic eruptions and are bounded by mountain chains on all sides. The plains appear to be deformed near the mountains. This suggests that some of the mountain building activity occurred after the plains formed. An impact crater (Official International Astronomical Union name 'Wanda,' mapped first by the Soviet Venera 15/16 mission in 1984 at low resolution) with a diameter of 22 kilometers (14 miles) was formed by the impact of an asteroid in the Akna mountains. The crater has a rugged central peak and a smooth radar-dark floor, probably volcanic material. The crater does not appear to be much deformed by later crustal movement that uplifted the mountains and crumpled the plains. Material from the adjacent mountain ridge to the west, however, appears to have collapsed into the crater. Small pits seen to the north of the crater may be volcanic collapse pits a few kilometers across (1-2 miles). The ridge of the Akna mountains immediately to the west of the crater is 8 kilometers wide (5 miles). The area imaged is approximately 200 kilometers long and 125 kilometers wide (130 by 80 miles). This area is centered at 71.5 degrees north latitude, 324 degrees east longitude. The resolution of the Magellan radar system is 120 meters (400 feet). At this latitude the radar views the surface from an angle of 23 degrees off vertical, creating a perspective as though a viewer were looking at the scene from the right (east) at an angle of 23 degrees above the surface.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00250" onclick="window.open(this.href); return false;" title="Voir l'image PIA00250: Venus - Wanda Crater in Akna Montes sur le site de la NASA">Voir l'image PIA00250: Venus - Wanda Crater in Akna Montes sur le site de la NASA.</a></div>
PIA00250: Venus - Wanda Crater in Akna Montes
<h1>PIA00149: Venus - Maxwell Montes and Cleopatra Crater</h1><div class="PIA00149" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This Magellan full-resolution image shows Maxwell Montes, and is centered at 65 degrees north latitude and 6 degrees east longitude. Maxwell is the highest mountain on Venus, rising almost 11 kilometers (6.8 miles) above mean planetary radius. The western slopes (on the left) are very steep, whereas the eastern slopes descend gradually into Fortuna Tessera. The broad ridges and valleys making up Maxwell and Fortuna suggest that the topography resulted from compression. Most of Maxwell Montes has a very bright radar return; such bright returns are common on Venus at high altitudes. This phenomenon is thought to result from the presence of a radar reflective mineral such as pyrite. Interestingly, the highest area on Maxwell is less bright than the surrounding slopes, suggesting that the phenomenon is limited to a particular elevation range. The pressure, temperature, and chemistry of the atmosphere vary with altitude; the material responsible for the bright return probably is only stable in a particular range of atmospheric conditions and therefore a particular elevation range. The prominent circular feature in eastern Maxwell is Cleopatra. Cleopatra is a double-ring impact basin about 100 kilometers (62 miles) in diameter and 2.5 kilometers (1.5 miles) deep. A steep-walled, winding channel a few kilometers wide breaks through the rough terrain surrounding the crater rim. A large amount of lava originating in Cleopatra flowed through this channel and filled valleys in Fortuna Tessera. Cleopatra is superimposed on the structures of Maxwell Montes and appears to be undeformed, indicating that Cleopatra is relatively young.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00149" onclick="window.open(this.href); return false;" title="Voir l'image PIA00149: Venus - Maxwell Montes and Cleopatra Crater sur le site de la NASA">Voir l'image PIA00149: Venus - Maxwell Montes and Cleopatra Crater sur le site de la NASA.</a></div>
PIA00149: Venus - Maxwell Montes and Cleopatra Crater
<h1>PIA00107: Venus - 3D Perspective View of Sapas Mons</h1><div class="PIA00107" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Sapas Mons is displayed in the center of this computer-generated three-dimensional perspective view of the surface of Venus. The viewpoint is located 527 kilometers (327 miles) northwest of Sapas Mons at an elevation of 4 kilometers (2.5 miles) above the terrain. Lava flows extend for hundreds of kilometers across the fractured plains shown in the foreground to the base of Sapas Mons. The view is to the southeast with Sapas Mons appearing at the center with Maat Mons located in the background on the horizon. Sapas Mons, a volcano 400 kilometers (248 miles) across and 1.5 kilometers (0.9 mile) high is located at approximately 8 degrees north latitude, 188 degrees east longitude, on the western edge of Atla Regio. Its peak sits at an elevation of 4.5 kilometers (2.8 miles) above the planet's mean elevation. Sapas Mons is named for a Phoenician goddess. The vertical scale in this perspective has been exaggerated 10 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. 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 April 22, 1992 news conference.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00107" onclick="window.open(this.href); return false;" title="Voir l'image PIA00107: Venus - 3D Perspective View of Sapas Mons sur le site de la NASA">Voir l'image PIA00107: Venus - 3D Perspective View of Sapas Mons sur le site de la NASA.</a></div>
PIA00107: Venus - 3D Perspective View of Sapas Mons
<h1>PIA00089: Venus - Eistla Region</h1><div class="PIA00089" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This Magellan image is of an area located in the Eistla Region of Venus in the southern hemisphere and is centered at 5.5 degrees east longitude, 18 degrees south latitude. It is 122 kilometers (76 miles) across east to west and 107 kilometers (66 miles) north to south. North is at the top of the image. Shown is an unusual volcanic edifice unlike all others previously observed. It is approximately 66 kilometers (41 miles) across at the base and has a relatively flat, slightly concave summit 35 kilometers (22 miles) in diameter. The sides of the edifice are characterized by radiating ridges and valleys that impart a fluted appearance. To the west, the rim of the structure appears to have been breached by dark lava flows that emanated from a shallow summit pit approximately 5 kilometers (3 miles) in diameter and traveled west along a channel approximately 5 kilometers wide and 27 kilometers (17 miles) long. A series of coalescing, collapsed pits 2 to 10 kilometers (1.2 to 6.2 miles) in diameter are located 10 kilometers (6 miles) west of the summit. The edifice and western pits are circumscribed by faint, concentric lineaments up to 70 kilometers (43 miles) in diameter. A series of north northwest trending graben are deflected eastward around the edifice; the interplay of these graben and the fluted rim of the edifice produce a distinctive scalloped pattern in the image. Several north northwest trending lineaments cut directly across the summit region. This peculiar volcanic construct is located 25 to 30 kilometers (15 to 19 miles) north of Alpha Regio, a highly deformed region of tessera terrain. A collection of at least six similar volcanoes has been observed near Thetis Regio, a region of tessera within Aphrodite Terra. Thus, these unusual constructs tentatively appear to be spatially associated with regions of tessera. A tessera is a complex, deformed terrain on Venus consisting of at least two sets of intersecting ridges and troughs. The implications of this spatial association on the unusual morphology of these constructs are being investigated.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00089" onclick="window.open(this.href); return false;" title="Voir l'image PIA00089: Venus - Eistla Region sur le site de la NASA">Voir l'image PIA00089: Venus - Eistla Region sur le site de la NASA.</a></div>
PIA00089: Venus - Eistla Region
<h1>PIA00100: Venus - Fractured Somerville Crater in Beta Regio</h1><div class="PIA00100" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This Magellan radar image is of a 'half crater' located in the rift between Rhea and Theia Montes in Beta Regio on Venus. The unnamed crater is 37 kilometers (23 miles) in diameter and is located at 29.9 degrees north latitude and 282.9 degrees east longitude. It has been cut by many fractures or faults since it was formed by the impact of a large asteroid. The eastern half of the crater was destroyed during the formation of a fault valley that is up to 20 kilometers (12 miles) wide and apparently quite deep. A north-south profile through the very center of this crater is visible as a result of the down dropping and removal of the eastern half of the crater. Magellan scientists expect to get a better view of the crater's geological features during a later mapping cycle of Venus.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00100" onclick="window.open(this.href); return false;" title="Voir l'image PIA00100: Venus - Fractured Somerville Crater in Beta Regio sur le site de la NASA">Voir l'image PIA00100: Venus - Fractured Somerville Crater in Beta Regio sur le site de la NASA.</a></div>
PIA00100: Venus - Fractured Somerville Crater in Beta Regio
<h1>PIA00087: Lavinia Region Ridge Belts, Plains and Lava Flows</h1><div class="PIA00087" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p>This is a Magellan full resolution radar mosaic of the Lavinia region of Venus. The mosaic is centered at 50 degrees south latitude, 345 degrees east longitude, and spans 540 kilometers (338 miles) north to south and 900 kilometers (563 miles) east to west. As with all Magellan images acquired thus far, the illumination of the radar is from the left hand side of the image. This area shows a diverse set of geologic features. The bright area running from the upper right to the lower left is interpreted as part of a belt of ridges, formed by compression and thickening of the upper layers of the planet. The areas between ridges suggest flooding by radar dark (and thus presumably) smoother lavas. The varied texture of the lavas can be seen in the mottled appearance of the plains which are cut by the ridges; brighter, rougher flows are also quite common. The particularly bright flows in the lower right corner are the northern extension of Mylitta Fluctus. The bright ridges adjacent to Mylitta Fluctus at the bottom center of the image also appear to have been affected by the volcanic activity. Some of these bright features have been interpreted as down dropped areas roughly 5 kilometers (3 miles) wide. This would imply a region of extension where the crust has been pulled apart and thus was more easily flooded by the later lava flows. The thinner fractures running from the upper left seem to end at the ridge belt in the center of this mosaic. These thinner fractures are a continuation of a pattern seen throughout much of Lavinia and suggest a pattern of compression over a very large region. At the bottom of the image, overlying the ridges, is an impact crater 10 to 15 kilometers (6 to 10 miles) in diameter. The double or overlapped crater structure and asymmetrical ejecta pattern suggests that the incoming body broke up shortly before it hit, leaving closely spaced craters. The placement of the crater on top of the ridges implies it is younger than the ridges; in fact, the crater may be one of the youngest features in this image.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00087" onclick="window.open(this.href); return false;" title="Voir l'image PIA00087: Lavinia Region Ridge Belts, Plains and Lava Flows sur le site de la NASA">Voir l'image PIA00087: Lavinia Region Ridge Belts, Plains and Lava Flows sur le site de la NASA.</a></div>
PIA00087: Lavinia Region Ridge Belts, Plains and Lava Flows
<h1>PIA00219: Venus - Lada Terra Region</h1><div class="PIA00219" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This is a Magellan radar image mosaic of part of Venus, centered at 51 degrees south latitude, 21 degrees east longitude. Each pixel, or picture element, represents 225 meters. The scene is approximately 200 kilometers (124 miles) east to west by 160 kilometers (99 miles) north to south. Running from west to east across the center of the image is part of a 1,200 kilometer (744 miles) long by 20 kilometer (12 mile) wide lava channel in the Lada Terra region of Venus. Numerous streamlined structures within the channel attest to the very high temperature, very fluid lavas (resulting in both thermal and mechanical erosion) responsible for carving the channel.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00219" onclick="window.open(this.href); return false;" title="Voir l'image PIA00219: Venus - Lada Terra Region sur le site de la NASA">Voir l'image PIA00219: Venus - Lada Terra Region sur le site de la NASA.</a></div>
PIA00219: Venus - Lada Terra Region
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<h1>PIA00096: Three-dimensional perspective views of Venusian Terrains composed of reduced resolution left-looking synthetic-aperture radar images merged with altimetry data from the Magellan spacecraft.</h1><div class="PIA00096" lang="en" style="width:723px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">The view shows most of Galindo (V-40) quadrangle looking east; Atete Corona, in the foreground, is a 600-km-long and about 450-km-wide, circular volcano-tectonic feature. Coronae are believed to form over hot upwellings of magma within the Venusian mantle.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00096" onclick="window.open(this.href); return false;" title="Voir l'image PIA00096: Three-dimensional perspective views of Venusian Terrains composed of reduced resolution left-looking synthetic-aperture radar images merged with altimetry data from the Magellan spacecraft. sur le site de la NASA">Voir l'image PIA00096: Three-dimensional perspective views of Venusian Terrains composed of reduced resolution left-looking synthetic-aperture radar images merged with altimetry data from the Magellan spacecraft. sur le site de la NASA.</a></div>
PIA00096: Three-dimensional perspective views of Venusian Terrains composed of reduced resolution left-looking synthetic-aperture radar images merged with altimetry data from the Magellan spacecraft.
<h1>PIA00201: Venus - Volcanic features in Atla Region</h1><div class="PIA00201" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This Magellan image from the Atla region of Venus shows several types of volcanic features and superimposed surface fractures. The area in the image is approximately 350 kilometers (217 miles) across, centered at 9 degrees south latitude, 199 degrees east longitude. Lava flows emanating from circular pits or linear fissures form flower-shaped patterns in several areas. A collapse depression approximately 20 kilometers by 10 kilometers (12 by 6 miles) near the center of the image is drained by a lava channel approximately 40 kilometers (25 miles) long. Numerous surface fractures and graben (linear valleys) criss-cross the volcanic deposits in north to northeast trends. The fractures are not buried by the lavas, indicating that the tectonic activity post-dates most of the volcanic activity.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00201" onclick="window.open(this.href); return false;" title="Voir l'image PIA00201: Venus - Volcanic features in Atla Region sur le site de la NASA">Voir l'image PIA00201: Venus - Volcanic features in Atla Region sur le site de la NASA.</a></div>
PIA00201: Venus - Volcanic features in Atla Region
<h1>PIA00461: Venus - Mosaic of Bahet and Onatah Coronae</h1><div class="PIA00461" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">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 (138 miles) long and 150 kilometers (90 miles) across. A portion of Onatah Corona, over 350 kilometers (210 miles) 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 (400 feet).<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00461" onclick="window.open(this.href); return false;" title="Voir l'image PIA00461: Venus - Mosaic of Bahet and Onatah Coronae sur le site de la NASA">Voir l'image PIA00461: Venus - Mosaic of Bahet and Onatah Coronae sur le site de la NASA.</a></div>
PIA00461: Venus - Mosaic of Bahet and Onatah Coronae
<h1>PIA00241: Venus - Lakshmi Planum and Maxwell Montes</h1><div class="PIA00241" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This Magellan full resolution radar image is centered at 65 degrees north latitude, zero degrees east longitude, along the eastern edge of Lakshmi Planum and the western edge of Maxwell Montes. The plains of Lakshmi are made up of radar-dark, homogeneous, smooth lava flows. Located near the center of the image is a feature previously mapped as tessera made up of intersecting 1- to 2-km (0.6 to 1.2 miles) wide graven. The abrupt termination of dark plains against this feature indicates that it has been partially covered by lava. Additional blocks of tessera are located along the left hand edge of the image. A series of linear parallel troughs are located along the southern edge of the image. These features, 60- to 120-km (36- to 72- miles) long and 10- to 40- km (6- to 24- miles) wide are interpreted as graben. Located along the right hand part of the image is Maxwell Montes, the highest mountain on the planet, rising to an elevation of 11.5 km (7 miles) and is part of a series of mountain belts surrounding Lakshmi Planum. The western edge of Maxwell shown in this image rises sharply, 5.0 km (3.0 miles), above the adjacent plains in Lakshmi Planum. Maxwell is made up of parallel ridges 2- to 7-km (1.2- to 4.2 miles) apart and is interpreted to have formed by compressional tectonics. The image is 300 km (180 miles) wide.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00241" onclick="window.open(this.href); return false;" title="Voir l'image PIA00241: Venus - Lakshmi Planum and Maxwell Montes sur le site de la NASA">Voir l'image PIA00241: Venus - Lakshmi Planum and Maxwell Montes sur le site de la NASA.</a></div>
PIA00241: Venus - Lakshmi Planum and Maxwell Montes
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<h1>PIA00086: Mosaic of Large Impact Craters</h1><div class="PIA00086" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p>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 (300 mile) 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 (23 miles) to 50 kilometers (30 miles) 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 (0.6-7 miles), and some have central pits typical of volcanic shields or cones. Resolution of the Magellan data is about 120 meters (400 feet).<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00086" onclick="window.open(this.href); return false;" title="Voir l'image PIA00086: Mosaic of Large Impact Craters sur le site de la NASA">Voir l'image PIA00086: Mosaic of Large Impact Craters sur le site de la NASA.</a></div>
PIA00086: Mosaic of Large Impact Craters
<h1>PIA00218: Venus - Interior of Ovda Regio</h1><div class="PIA00218" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This Magellan image shows part of the interior of Ovda Regio, one of the large highlands ringing the equator of Venus. Several tectonic events formed this complex block fractured terrain. An underlying fabric of ridges and valleys strikes northeast southwest. These ridges are spaced 10 to 20 kilometers (6 to 12 miles) apart and may have been caused by shortening of the crust at right angles to this trend. These structures are cut by thoroughgoing extension fractures trending northwest-southeast, suggesting a later episode of northeast southwest extension. Lastly, the largest valleys, particularly the 20 kilometer (12 mile) wide one extending across the image, were filled with dark material, probably lava. The complex internal fabric of Ovda Regio attests to a long history of tectonic deformation. This image, centered approximately at 1 degree south, 81 degrees east, measures 225 kilometers (140 miles) by 150 kilometers (90 miles) and was acquired by Magellan in November 1990.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00218" onclick="window.open(this.href); return false;" title="Voir l'image PIA00218: Venus - Interior of Ovda Regio sur le site de la NASA">Voir l'image PIA00218: Venus - Interior of Ovda Regio sur le site de la NASA.</a></div>
PIA00218: Venus - Interior of Ovda Regio
<h1>PIA00088: Venus - Stein Triplet Crater</h1><div class="PIA00088" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p>The Magellan synthetic aperture radar (SAR) imaged this unique 'triplet crater,' or 'crater field' during orbits 418-421 on 21 September 1990. These craters are 14 kilometers, 11 kilometers, and 9 kilometers in diameter, respectively, and are centered at latitude -30.1 degrees south and longitude 345.5 degrees east. The Magellan Science Team has proposed the name Stein for this crater field after the American author, Gertrude Stein. This name has not yet been approved by the International Astronomical Union. The crater field was formed on highly fractured plains. The impacts generated a considerable amount of low viscosity 'flows' thought to consist largely of shock-melted target material along with fragmented debris from the crater. The three craters appear to have relatively steep walls based on the distortion in the image of the near and far walls of the craters in the Magellan radar look direction (from the left). The flow deposits from the three craters extend dominantly to the northeast (upper right).<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00088" onclick="window.open(this.href); return false;" title="Voir l'image PIA00088: Venus - Stein Triplet Crater sur le site de la NASA">Voir l'image PIA00088: Venus - Stein Triplet Crater sur le site de la NASA.</a></div>
PIA00088: Venus - Stein Triplet Crater
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<h1>PIA00148: Venus - Mead Crater</h1><div class="PIA00148" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This Magellan image mosaic shows the largest (275 kilometers in diameter [170 miles]) impact crater known to exist on Venus at this point in the Magellan mission. The crater is located north of Aphrodite Terra and east of Eistla Regio at latitude 12.5 degrees north and longitude 57.4 degrees east, and was imaged during Magellan orbit 804 on November 12, 1990. The Magellan science team has proposed to name this crater Mead, after Margaret Mead, the American Anthropologist (1901- 1978). All Magellan-based names of features on Venus are, of course, only proposed until final approval is given by the International Astronomical Union-Commission on Planetary Nomenclature. Mead is classified as a multi-ring crater with its innermost, concentric scarp being interpreted as the rim of the original crater cavity. No inner peak-ring of mountain massifs is observed on Mead. The presence of hummocky, radar-bright crater ejecta crossing the radar-dark floor terrace and adjacent outer rim scarp suggests that the floor terrace is probably a giant rotated block that is concentric to, but lies outside of, the original crater cavity. The flat, somewhat brighter inner floor of Mead is interpreted to result from considerable infilling of the original crater cavity by impact melt and/or by volcanic lavas. To the southeast of the crater rim, emplacement of hummocky ejecta appears to have been impeded by the topography of preexisting ridges, thus suggesting a very low ground-hugging mode of deposition for this material. Radar illumination on this and all other Magellan image products is from the left to the right in the scene.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00148" onclick="window.open(this.href); return false;" title="Voir l'image PIA00148: Venus - Mead Crater sur le site de la NASA">Voir l'image PIA00148: Venus - Mead Crater sur le site de la NASA.</a></div>
PIA00148: Venus - Mead Crater
<h1>PIA00478: Venus - Global View Centered at 180 degrees</h1><div class="PIA00478" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">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, and a 5 degree latitude-longitude grid, 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. The image was produced by the Solar System Visualization project and the Magellan Science team at the JPL Multimission Image Processing Laboratory.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00478" onclick="window.open(this.href); return false;" title="Voir l'image PIA00478: Venus - Global View Centered at 180 degrees sur le site de la NASA">Voir l'image PIA00478: Venus - Global View Centered at 180 degrees sur le site de la NASA.</a></div>
PIA00478: Venus - Global View Centered at 180 degrees
<h1>PIA00256: Venus - Simple Cylindrical Map of Surface (Eastern Half)</h1><div class="PIA00256" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">The eastern half of the planet is displayed in this simple cylindrical map of the surface of Venus. The left edge of the image is at 52.5 degrees east longitude, the right edge at 240 degrees east longitude. The top and bottom of the image are at 90 degrees north latitude and 90 degrees south latitude, respectively. Magellan synthetic aperture radar mosaics from the first cycle of Magellan mapping are mapped onto a rectangular latitude-longitude grid to create this image. Data gaps are filled with Pioneer Venus Orbiter altimetric 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.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00256" onclick="window.open(this.href); return false;" title="Voir l'image PIA00256: Venus - Simple Cylindrical Map of Surface (Eastern Half) sur le site de la NASA">Voir l'image PIA00256: Venus - Simple Cylindrical Map of Surface (Eastern Half) sur le site de la NASA.</a></div>
PIA00256: Venus - Simple Cylindrical Map of Surface (Eastern Half)
Venus_a_pole-nord.jpg
Venus_a_pole-nord.jpg
<h1>PIA00240: Venus - Lakshmi Planum</h1><div class="PIA00240" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This image is a full-resolution mosaic of several Magellan images and is centered at 61 degrees north latitude and 341 degrees east longitude. The image is 250 kilometers wide (150 miles). The radar smooth region in the northern part of the image is Lakshmi Planum, a high plateau region roughly 3.5 kilometers (2.2 miles) above the mean planetary radius. Lakshmi Planum is ringed by intensely deformed terrain, some of which is shown in the southern portion of the image and is called Clotho Tessera. The 64-kilometer (40 mile) diameter circular feature in the image is a depression called Siddons and may be a volcanic caldera. This view is supported by the collapsed lava tubes surrounding the feature. By carefully studying this and other surrounding images scientists hope to discover what tectonic and volcanic processes formed this complex region. The solid black parts of the image represent data gaps that may be filled in by the Magellan extended mission.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00240" onclick="window.open(this.href); return false;" title="Voir l'image PIA00240: Venus - Lakshmi Planum sur le site de la NASA">Voir l'image PIA00240: Venus - Lakshmi Planum sur le site de la NASA.</a></div>
PIA00240: Venus - Lakshmi Planum
 
<h1>PIA00099: East Part of Sapas Mons with Flooded Crater</h1><div class="PIA00099" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This Magellan image centered near 9.6 degrees north latitude, 189.5 degrees east longitude of an area 140 kilometers (87 miles) by 110 kilometers (68 miles) covers part of the eastern flank of the volcano Sapas Mons on the western edge of Atla Regio. The bright lobate features along the southern and the western part of the image, oriented in northeast to southwest directions, are lava flows that are rough at the 12.6 centimeter wavelength of the radar. These flows range in width from 5 kilometers to 25 kilometers (3 to 16 miles) with lengths of 50 kilometers to 100 kilometers (31 to 62 miles), extending off the area shown here. Additional radar-dark (smooth) flows are also present. The radar-bright linear structures in the northwest part of the image are interpreted to be faults and fractures possibly associated with the emplacement of magma in the subsurface. Located near the center of the image is a 20 kilometer (12 mile) diameter impact crater. This crater is superimposed on a northeast/southwest trending fracture while the southern part of the crater's ejecta blanket is covered by a 6 kilometer (4 mile) wide radar-bright lava flow. These relations indicate that the crater post dates an episode of fracturing and is older than the lava flows covering its southern edge. This is one of only a few places on Venus in which an impact crater is seen to be covered by volcanic deposits.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00099" onclick="window.open(this.href); return false;" title="Voir l'image PIA00099: East Part of Sapas Mons with Flooded Crater sur le site de la NASA">Voir l'image PIA00099: East Part of Sapas Mons with Flooded Crater sur le site de la NASA.</a></div>
PIA00099: East Part of Sapas Mons with Flooded Crater
Venus_d_pole-nord.jpg
Venus_d_pole-nord.jpg
Venus_d90.jpg
Venus_d90.jpg
<h1>PIA00209: Venus - 3D Perspective of Golubkina Crater</h1><div class="PIA00209" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">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 kilometers (20.4 miles) 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 meteorite impact. The central peak forms due to rebound of the inner crater floor.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00209" onclick="window.open(this.href); return false;" title="Voir l'image PIA00209: Venus - 3D Perspective of Golubkina Crater sur le site de la NASA">Voir l'image PIA00209: Venus - 3D Perspective of Golubkina Crater sur le site de la NASA.</a></div>
PIA00209: Venus - 3D Perspective of Golubkina Crater
Synthese_Venus.jpg
Synthese_Venus.jpg