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Venera 14 Lander
| title |
Venera 14 Lander |
| date |
11.04.1981 |
| description |
Venera 14 was identical to its twin, Venera 13. The spacecraft carried out three midcourse corrections on the way to Venus: on 14 November 1981, 23 November 1981, and 25 February 1982. Russian sources indicate that one of the corrections was incorrect (probably the first) and could have jeopardized the mission. The lander probe separated from its flyby parent on 3 March 1982 before the entry cycle began. The probe's main parachute opened at an altitude of 62 to 63 kilometers, thus activating the atmospheric instruments. The parachute was released at an altitude of 47 kilometers, and the 760-kilogram lander fell to the surface using only the atmosphere as a retarding medium. The probe made safe contact with the Venusian surface at 07:00:10 UT on 3 March 1982 and continued with 57 minutes of transmissions. Landing coordinates were 13.25° south latitude and 310° longitude, about 1,000 kilometers from the Venera 13 landing site. As with its twin, Venera 14 returned color photographs of its surroundings and examined a soil sample (about 1 cubic centimeter taken from a 30-millimeter-deep sample). Soil was deposited in a chamber sealed off from the outside environment and was then progressively transferred through a series of chambers by blowing air until the sample was deposited in its final chamber with a temperature of only 30°C. Here it was examined by the x-ray fluorescence spectrometer. Temperature and pressure outside were considerably higher than at the Venera 13 site: 470°C and 93.5 atmospheres, respectively. The flyby probe, meanwhile, passed Venus at a range of 36,000 kilometers and entered heliocentric orbit, continuing to provide data on solar x-ray flares. It performed one trajectory change on 14 November 1982. |
|
The Desert Surface of Venus
| title |
The Desert Surface of Venus |
| date |
03.01.1982 |
| description |
Venera 13 Lander image of the surface of Venus at 7.5 S, 303. E, east of Phoebe Regio. Venera 13 survived on the surface for 2 hours, 7 minutes, long enough to obtain 14 images on 1 March, 1982. This color 170 degree panorama was produced using dark blue, green and red filters and has a resolution of 4 to 5 min. Part of the spacecraft is at the bottom of the image. Flat rock slabs and soil are visible. The true color is difficult to judge because the Venerian atmosphere filters out blue light. The surface composition is similar to terrestrial basalt. On the ground in foreground is a camera lens cover. (Venera 13 Lander, VG00261,262) *Image Credit*: NASA |
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Venus - 3D Perspective View
…
| title |
Venus - 3D Perspective View of Maat Mons |
| date |
04.22.1992 |
| description |
Maat Mons is displayed in this computer generated three-dimensional perspective of the surface of Venus. The viewpoint is located 634 kilometers (393 miles) north of Maat Mons at an elevation of 3 kilometers (2 miles) 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 (3 miles) 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 (5 miles) 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. 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. *Image Credit*: JPL |
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Venus - 3D Perspective View
…
| Title |
Venus - 3D Perspective View of Eistla Regio |
| Description |
A portion of western Eistla Regio is displayed in this three-dimensional perspective view of the surface of Venus. The viewpoint is located 1,310 kilometers (812 miles) southwest of Gula Mons at an elevation of 0.78 kilometer (0.48 mile). The view is to the northeast with Gula Mons appearing on the horizon. Gula Mons, a 3 kilometer (1.86 mile) high volcano, is located at approximately 22 degrees north latitude, 359 degrees east longitude. The impact crater Cunitz, named for the astronomer and mathematician Maria Cunitz, is visible in the center of the image. The crater is 48.5 kilometers (30 miles) in diameter and is 215 kilometers (133 miles) from the viewer's position. 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. The image was produced at the JPL Multimission Image Processing Laboratory and is a single frame from a video released at the March 5, 1991, JPL news conference. |
| Date |
05.28.1991 |
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Venus - 3D Perspective View
…
| Title |
Venus - 3D Perspective View of Gula Mons |
| Description |
Gula Mons is displayed in this computer-simulated view of the surface of Venus. The viewpoint is located 110 kilometers (68 miles) southwest of Gula Mons at the same elevation as the summit, 3 kilometers (1.9 miles) 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 (1.9 mile) 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. The image was produced by the JPL Multimission Image Processing Laboratory and is a single frame from a video released at the March 5, 1991, JPL news conference. |
| Date |
10.29.1991 |
|
Venus - Simulated Color of U
…
| Title |
Venus - Simulated Color of Ushas Mons |
| Description |
Ushas Mons, a 2-kilometer-high (1.25 mile) 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 (360 miles) 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. The image was produced by the Solar System Visualization Project and the Magellan Science Team at the Jet Propulsion Multimission Image Processing Laboratory. The Magellan mission is managed by JPL for NASA's Office of Space Science. |
| Date |
05.26.1993 |
|
Venus - Computer Simulated G
…
PIA00271
Sol (our sun)
Imaging Radar
| Title |
Venus - Computer Simulated Global View of the Northern Hemisphere |
| Original Caption Released with Image |
The northern hemisphere is displayed in this global view of the surface of Venus. The north pole is at the center of the image, with 0 degrees, 90 degrees, 180 degrees, 270 degrees east longitudes at the 6, 3, 12, and 9 o'clock positions, respectively, of an imaginary clock face. Magellan synthetic aperture radar mosaics from the three eight-month cycles of Magellan radar mapping are mapped onto a computer-simulated globe to create this image. Magellan obtained coverage of 98 percent of the surface of Venus. Remaining gaps are filled with data from previous missions, (the Soviet Venera 15 and 16 radar and Pioneer Venus Orbiter altimetry) and data from Earth-based radar observations from the Arecibo radio telescope. 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. Maxwell Montes, the planet's highest mountain at 11 kilometers (6.6 miles) above the average elevation, is the bright feature in the lower center of the image. Other terrain types visible in this image include tessera, ridge belts, lava flows, impact craters and coronae. The image was produced by the Solar System Visualization Project and the Magellan Science team at the Jet Propulsion Laboratory Multimission Image Processing Laboratory. The Magellan mission is managed by JPL for NASA's Office of Space Science. |
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Venus - Computer Simulated G
…
PIA00270
Sol (our sun)
Imaging Radar
| Title |
Venus - Computer Simulated Global View Centered at 90 Degrees East Longitude |
| Original Caption Released with Image |
This global view of the surface of Venus is centered at 90 degrees east longitude. Magellan synthetic aperture radar mosaics from the three eight-month cycles of Magellan radar mapping are mapped onto a computer-simulated globe to create this image. Magellan obtained coverage of 98 percent of the surface of Venus. Remaining gaps are filled with data from previous Venus missions -- the Venera 15 and 16 radar and Pioneer-Venus Orbiter altimetry -- and data from Earth-based radar observations from the Arecibo radio telescope. Simulated color is used to enhance small-scale structures. The simulated hues are based on color images obtained by the Venera 13 and 14 landing craft. The bright feature near the center of the image is Ovda Regio, a mountainous region in the western portion of the great Aphrodite equatorial highland. The dark areas scattered across the Venusian plains consist of extremely smooth deposits associated with large meteorite impacts. The image was produced by the Solar System Visualization Project and the Magellan Science team at the Jet Propulsion Laboratory Multimission Image Processing Laboratory. The Magellan mission is managed by JPL for NASA's Office of Space Science. |
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Global view of Venus from Ma
…
| Title |
Global view of Venus from Magellan, Pioneer, and Venera data |
| Description |
Global view of Venus is created from Magellan, Pioneer, and Venera data. The northern hemisphere of Venus is displayed in this global view of Venus' surface. The north pole is at the center of the image. Zero degrees, 90 degrees, 180 degrees, and 270 degrees east longitude are at the 6, 3, 12, and 9 o'clock positions, respectively, of an imaginary clock face. 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 at the Jet Propulsion Laboratory (JPL) Multimission Image Processing Laboratory and is a single frame from a video released at the JPL news conference, 10-29-91. |
| Date Taken |
1991-11-07 |
|
Global view of Venus from Ma
…
| Title |
Global view of Venus from Magellan, Pioneer, and Venera data |
| Description |
This global view of Venus, centered at 270 degrees east longitude, is a compilation of data from several sources. Magellan synthetic aperature radar mosaics from the first cycle of Magellan mapping are mapped onto a computer-simulated globe to create the 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 at the Jet Propulsion Laboratory (JPL) Multimission Image Processing Laboratory and is a single frame from a video released at the JPL news conference, 10-29-91. View provided by JPL with alternate number P-39225 MGN81. |
| Date Taken |
1991-11-07 |
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