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This artist's rendering show
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| Description |
This artist's rendering shows the Magellan spacecraft in an elliptical orbit around Venus and illustrates the mapping and data transmission phases of the mission. During the mapping phase, the spacecraft turns its large antenna toward Venus. For 37 minutes, the Synthetic Aperture Radar (SAR) maps the 15 mile wide swath from the north pole to 66 degrees south latitude, acquiring imaging, altimetry and radiometry data. As the spacecraft reaches the high point of its orbit, the antenna is turned toward Earth and, for 115 minutes, the data is transmitted to Earth receiving stations. Magellan Mission Launched May 4, 1989, the Magellan spacecraft was designed to conduct the most comprehensive observation of the surface and gravitational features of Venus ever undertaken. During its 243 day (one Venus rotation) primary mission, the spacecraft will map up to 90 percent of the planet with high resolution imaging radar and will return more digital imaging data than all previous U.S. planetary missions combined. Lifted into Earth orbit by a shuttle, Magellan was sent on its 15 month journey to Venus by an Inertial Upper Stage (IUS) booster rocket. On arrival at Venus, a solid rocket motor will insert the spacecraft into an elliptical orbit and then will be jettisoned. For 37 minutes of each orbit, the imaging radar, called Synthetic Aperture Radar or SAR, will image a 15 mile wide swath of Venus' surface while also acquiring altimetry and radiometry data to determine the altitudes and temperatures of surface features. Then as the spacecraft moves toward the high point of its orbit, Magellan will turn its large antenna toward Earth and, for 115 minutes, transmit the radar data at 268 kilobits (1 kilobit equals 1,000 bits of data) per second to Earth receiving stations. Also during this period, gravity data will be acquired as small accelerations of the spacecraft are measured from Earth. ##### JPL 400·344C, Rev 1 12189 This artist's rendering shows the Magellan spacecraft in an elliptical orbit around Venus and illustrates the mapping and data-transmission phases of the mission. During the mapping phase, the spacecraft will turn its large antenna toward Venus. For 37 minutes, the Synthetic Aperture Radar (SAR) will map a 15-mile-wide swath from the north pole to 66 degrees south latitude, acquiring imaging, altimetry, and radiometry data. As the spacecraft reaches the high point of its orbit, the antenna will turn toward Earth and, for 115 minutes, the data will be transmitted to Earth receiving stations. Magellan Mission On arrival at Venus in August 1990, the Magellan spacecraft will begin the most comprehensive observation of the surface and gravitational features of Venus ever undertaken. During its 243-day (one Venus rotation) primary mission, the spacecraft will map up to 90 percent of the planet with high-resolution imaging radar and will return more digital imaging data than all previous U.S. planetary missions combined. For 37 minutes of each three-hour elliptical orbit, the imaging radar, called Synthetic Aperture Radar or SAR, will image a 15-mile-wide swath of Venus' surface while also acquiring altimetry and radiometry data to determine the altitudes and temperatures of surface features. Then, as the spacecraft moves toward the high point of its orbit, Magellan will turn its large antenna toward Earth and, for 115 minutes, will transmit the radar data at 268 kilobits (1 kilobit equals 1,000 bits of data) per second to Earth receiving stations. Also during this period, gravity data will be acquired as ground engineers measure slight changes in the spacecraft's orbital motion. |
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Magellan MGN37
This Magellan image is of an
…
3/5/91
| Date |
3/5/91 |
| Description |
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. ##### |
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Magellan
The Magellan spacecraft has
…
10/6/94
| Date |
10/6/94 |
| Description |
The Magellan spacecraft has been collecting Doppler radio tracking data on the gravity field of Venus since completing radar mapping in 1992 After Magellan's successful aerobaking in August 1993, high resolution gravity data were acquired over the high latitude regions, providing relatively uniform global coverage with feature resolution between 200 kilometers and 400 kilometers and a sensitivity of I to 5 milligals (100 milligals equals I millimeter per second squared) By recording slight varations in the spacecraft's orbit as it passes over Venusian mountain belts, volcanoes and valleys, scientists are able to construct a "picture" of the distribution of density variations in the planet's interior. Those density differences are shown as color hues on this global image of Venus (red is high, blue is low). The globe is centered at 30 degrees west longitude and has been tipped forward by 30 degrees to better display the gravity differences in the Ishtar and Maxwell regions Slight differences in the gravity field provide clues about the geological processes responsible for shaping features observed at the surface The surface topography is displayed as three dimensional highs and lows on this image. The surface topography has been exaggerated by a factor of 100 to emphasize variations in elevation. It is evident that there is significant correlation of gravity with topography Maxwell Montes appears as a yellow and red area near the top right of the globe. Maxwell is the highest region of the planet and is of critical importance to geophysicists who must know the gravity field to make realistic inferences about the planet's internal structure. The high mountains of Beta Regio (left center) are shown in red. The topographic lows occur in the same regions where the dark blue color indicates that the gravity is low ##### |
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These images are composites
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3/16/95
| Date |
3/16/95 |
| Description |
These images are composites of the complete radar image collection obtained by the Magellan mission. The Magellan spacecraft was launched aboard space shuttle Atlantis in May 1989 and began mapping the surface of Venus in September 1990. The spacecraft continued to orbit Venus for four years, returning high-resolution images, altimetry, thermal emissions and gravity maps of 98 percent of the surface. Magellan spacecraft operations ended on October 12, 1994, when the radio contact was lost with the spacecraft during its controlled descent into the deeper portions of the Venusian atmosphere. The surface of Venus is displayed in these five global views. The center image (A) is centered at Venus’s north pole. The other four images are centered around the equator of Venus at (B) 0 degrees longitude, (C) 90 degrees east longitude, (D) 180 degrees and (E) 270 degrees east longitude. Magellan synthetic aperture radar mosaics 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 bright region near the center in the polar view is Maxwell Montes, the highest mountain range on Venus. Ovda Regio is centered in the (C) 90 degrees east longitude view. Atla Regio is seen prominently in the (D) 180 east longitude view. The scattered dark patches in this image are halos surrounding some of the younger impact craters. This global data set reveals a number of craters consistent with an average Venus surface age of 300 million to 500 million years. The image was produced by the Solar System Visualization Project and the Magellan science team at the Jet Propulsion Laboratory'’s Multimission Image Processing Laboratory. ##### |
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This image is a composite of
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3/16/95
| Date |
3/16/95 |
| Description |
This image is a composite of the complete radar image collection obtained by the Magellan mission. The Magellan spacecraft was launched aboard space shuttle Atlantis in May 1989 and began mapping the surface of Venus in September 1990. The spacecraft continued to orbit Venus for four years, returning high- resolution images, altimetry, thermal emissions and gravity maps of 98 percent of the surface. Magellan spacecraft operations ended on October 12, 1994, when the radio contact was lost with the spacecraft during its controlled descent into the deeper portions of the Venusian atmosphere. Venus is displayed in this simple cylindrical map of the planet's surface. The right and left edges of the image are 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 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. At the top, left of center, the bright region is Maxwell Montes, the highest mountain range on Venus. Extending along the equator to the right of center is Aphrodite Terra, a large highland region on Venus. The scattered dark patches in this image are halos surrounding some of the younger impact craters. This global data set reveals a number of craters consistent with an average Venus surface age of 300 million to 500 million years. The image was produced by the Solar System Visualization Project and the Magellan science team at the Jet Propulsion Laboratory'’s Multimission Image Processing Laboratory. ##### |
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Magellan
This hemispheric view of Ven
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3/16/95
| Date |
3/16/95 |
| Description |
This hemispheric view of Venus, as revealed by more than a decade of radar investigations culminating in the 1990-1994 Magellan mission, is centered at 270 degrees east longitude. The Magellan spacecraft imaged more than 98 percent of Venus at a resolution of about 100 meters, the effective resolution of this image is about 3 kilometers. 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 degrees 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. The Magellan mission was managed for NASA by the Jet Propulsion Laboratory (JPL), Pasadena, CA. Data processed by JPL, the Massachusetts Institute of Technology, Cambridge, MA, and the U.S. Geological Survey, Flagstaff, AZ. ##### |
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Magellan
This hemispheric view of Ven
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3/16/95
| Date |
3/16/95 |
| Description |
This 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 percent of Venus at a resolution of about 100 meters, the effective resolution of this image is about 3 kilometers. 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 degrees 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. The Magellan mission was managed for NASA by the Jet Propulsion Laboratory (JPL), Pasadena, CA. Data processed by JPL, the Massachusetts Institute of Technology, Cambridge, MA, and the U.S. Geological Survey, Flagstaff, AZ. |
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Magellan
This hemispheric view of Ven
…
3/16/95
| Date |
3/16/95 |
| Description |
This hemispheric view of Venus, as revealed by more than a decade of radar investigations culminating in the 1990-1994 Magellan mission, is centered at 90 degrees east longitude. The Magellan spacecraft imaged more than 98 percent of Venus at a resolution of about 100 meters, the effective resolution of this image is about 3 kilometers. 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 degrees 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. The Magellan mission was managed for NASA by the Jet Propulsion Laboratory (JPL), Pasadena, CA. Data processed by JPL, the Massachusetts Institute of Technology, Cambridge, MA, and the U.S. Geological Survey, Flagstaff, AZ. |
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Magellan
This hemispheric view of Ven
…
3/16/95
| Date |
3/16/95 |
| Description |
This hemispheric view of Venus, as revealed by more than a decade of radar investigations culminating in the 1990-1994 Magellan mission, is centered at the North Pole. The Magellan spacecraft imaged more than 98 percent of Venus at a resolution of about 100 meters, the effective resolution of this image is about 3 kilometers. 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 degrees 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. The Magellan mission was managed for NASA by the Jet Propulsion Laboratory (JPL), Pasadena, CA. Data processed by JPL, the Massachusetts Institute of Technology, Cambridge, MA, and the U.S. Geological Survey, Flagstaff, AZ. ##### |
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NASA Destination Tomorrow -
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NASA Destination Tomorrow Se
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6/1/03
| Description |
NASA Destination Tomorrow Segment exploring the function of aerobraking and how this helps reduce costs and create more room in aircraft. |
| Date |
6/1/03 |
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NASA Destination Tomorrow -
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NASA Destination Tomorrow Vi
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6/1/03
| Description |
NASA Destination Tomorrow Video containing three segments as described below. NASA Destination Tomorrow Segment exploring the function of aerobraking and how this helps reduce costs and create more room in aircraft. NASA Destination Tomorrow Segment exploring new materials technology development and how it has revolutionized the world of science and technology. NASA Destination Tomorrow Segment exploring a newly discovered moon called Titan that revolves around the planet Saturn. |
| Date |
6/1/03 |
|
NASA TV's This Week at NASA,
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Scientists now believe Earth
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04/09/10
| Description |
Scientists now believe Earth's nearest neighbor Venus is more like our planet than they previously thought. New findings based on pictures and infrared imagery captured by the European Space Agency's Venus Express mission and NASA's Magellan spacecraft confirm that Venus is not a cold rock but a dynamic host of active volcanoes like those found in Hawaii. * Opportunity, the Mars Exploration Rover, has reached another milestone in its travels around the Red Planet. The rover has covered more than twelve-and-a-half miles since landing on Mars six years ago. * The first, full-scale, friction stir welded and spun-formed tank dome was unveiled by NASA and its partners at a special ceremony at the Marshall Space Flight Center. * Four members of the STS-130 Endeavour space shuttle crew expressed their appreciation for employees of the Marshall Space Flight Center during a recent visit. The crew thanked employees for supporting the successful February mission to the International Space Station. Among other contributions, Marshall provided the three main engines that powered the crew on their 14-day mission. * Twenty-nine years ago, on April 12, 1981, space shuttle Columbia was launched from the Kennedy Space Center. Commanded by Gemini and Apollo veteran John Young and piloted by first-time flyer Bob Crippen, this first space shuttle mission, STS-1, was also the first U.S. manned orbital space flight since the Apollo-Soyuz Test Project almost six years earlier. |
| Date |
04/09/10 |
|
Wheatley Crater, Venus
| title |
Wheatley Crater, Venus |
| description |
Magellan radar image of Wheatley crater on Venus. This 72 km diameter crater shows a radar bright ejecta pattern and a generally flat floor with some rough raised areas and faulting. The crater is located in Asteria Regio at 16.6N,267E. (Portion of Magellan C1-MIDR 15N266;1,framelets 21 and 22) *Image Credit*: NASA |
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Volcano Southeast of Phoebe
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| title |
Volcano Southeast of Phoebe Regio,Venus with Emissivity Data |
| date |
11.11.1992 |
| description |
Magellan press release image showing radio-thermal emission (emissivity). Red represents high emissivity and blue low. The image is centered at 12.5S,261E, southeast of Phoebe Regio, Venus and is 587 km on a side. The unnamed volcano is about 2 km high and shows low emissivity at the summit, which could indicate the presence of pyrrohtite or pyrite, minerals which may not be stable at lower altitudes. (Magellan press release P-40698) *Image Credit*: NASA |
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Nova in Themis Regio,Venus
| title |
Nova in Themis Regio,Venus |
| description |
Magellan image of a nova, a radial network of grabens, in Themis Regio, Venus. There have been about 50 novae identified on Venus, which consist of closely spaced graben radiating from a central area. This nova is about 250 km in diameter, concentrated to the south. (North is up.) (Magellan C1-MIDR 30S279;1,framelet 18) *Image Credit*: NASA |
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Venus - Magellan
| title |
Venus - Magellan |
| description |
Magellan radar image of the Venera 10 landing site on Venus. The exact coordinates of the Venera 10 lander site are not known, but the estimate is centered at 15.42N,291.51E, near the southeastern edge of Beta Regio which is also the center of this image. The Venera lander panorama shows Venera 10 landed on a plain (the dark region) and not the brighter tessera. This image is about 600 km across and north is up. (Magellan C1-MIDR 15N283;1,framelet 32) *Image Credit*: NASA |
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Venus - 3D Perspective View
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| 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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Magellan Preparations
| Title |
Magellan Preparations |
| Full Description |
The Magellan spacecraft with its attached Inertial Upper Stage booster is in the orbiter Atlantis payload bay prior to closure of the doors at T-3 days to launch from pad 39B. Launch of Magellan and Space Shuttle Mission STS-30 is targeted for Friday, April 28, 1989. The 23 minute launch window opens at 2:24 p.m. |
| Date |
4/25/1989 |
| NASA Center |
Kennedy Space Center |
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Solar System Montage
| Title |
Solar System Montage |
| Full Description |
This is a montage of planetary images taken by spacecraft managed by the Jet Propulsion Laboratory in Pasadena, CA. Included are (from top to bottom) images of Mercury, Venus, Earth (and Moon), Mars, Jupiter, Saturn, Uranus and Neptune. The spacecraft responsible for these images are as follows: the Mercury image was taken by Mariner 10, the Venus image by Magellan, the Earth image by Galileo, the Mars image by Viking, and the Jupiter, Saturn, Uranus and Neptune images by Voyager. Pluto is not shown as no spacecraft has yet visited it. The inner planets (Mercury, Venus, Earth, Moon, and Mars) are roughly to scale to each other, the outer planets (Jupiter, Saturn, Uranus, and Neptune) are roughly to scale to each other. Actual diameters are given below: Sun 1,390,000 km Mercury 4,879 km Venus 12,104 km Earth 12,756 km Moon 3,475 km Mars 6,794 km Jupiter 142.984 km Saturn 120,536 km Uranus 51,118 km Neptune 49,528 km Pluto 2,390 km |
| Date |
04/09/1999 |
| NASA Center |
Jet Propulsion Laboratory |
|
STS-30 Landing
| Title |
STS-30 Landing |
| Full Description |
The Space Shuttle Atlantis returns to Earth after mission STS-30 landing at Edwards Air Force Base, CA. At 3:43:38 EDT. The orbiter Atlantis was launched form Kennedy Space Center May 4, 1989 at 2:46:59 p.m. EDT carrying into low Earth orbit the spacecraft Magellan. It was Atlantis' fourth shuttle mission. Approximately six hours after launch, Magellan was deployed from the Atlantis payload bay beginning its 15 month long journey to the planet Venus. Crew members of STS-30 were: Commander David M. Walker, Pilot Ronald J. Grabe, and Mission Specialists Mark C. Lee, Norman E. Thagard, and Mary L. Cleave. |
| Date |
5/8/1989 |
| NASA Center |
Kennedy Space Center |
|
A90-3000
Photographer : JPL After tra
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8/21/90
| Description |
Photographer : JPL After traveling more than 1.5 billion km (948 million mi.), the Magellan spacecraft was inserted into orbit around Venus on Aug. 10, 1990. This mosaic consists of adjacent pieces of two magellan image strips obtained in the first radar test. The radar test was part of a planned In-Orbit Checkout sequence designed to prepare the magellan spacecraft and radar to begin mapping after Aug. 31. The strip on the left was returned to the Goldstone Deep Space Network station in California, the strip to the right was received at the DSN in Canberra, Australia. A third station that will be receiving Magellan data is locaterd near Madrid, Spain. Each image strip is 20 km (12 mi.) wide and 16,000 km (10,000 mi.) long. This mosaic is a small portion 80 km (50 mi.) long. This image is centered at 21 degrees north latitude and 286.8 degrees east longitude, southeast of a volcanic highland region called Beta Regio. The resolution of the image is about 120 meters (400 feet), 10 times better than revious images of the same area of Venus, revealing many new geologic features. The bright line trending northwest-southeast across the center of the image is a fracture or fault zone cutting the volcanic plains. In the upper lest corner of the image, a multiple-ring circular feature of probable volcanic origin can be seen, approx. 4.27 km (2.65 mi.) across. The bright and dark variations seen in the plains surrounding these features correspond to volcanic lava flows of varying ages. The volcanic lava flows in the southern half of the image have been cut by north-south trending faults. This area is similar geologically to volcanic deposits seen on Earth at Hawaii and the Snake River Plains in Idaho. |
| Date |
8/21/90 |
|
A90-3001
Photographer : JPL This port
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8/21/90
| Description |
Photographer : JPL This portion of a Magellan radar image strip shows a small region on Venus 20 km (12.4 mi.) wide and 75 km (50 mi.) long on the east flank of a major volcanic upland called Beta Regio. The image is centerd at 23 degrees north latitude and 286.7 degrees east longitude. The ridge and valley networkin the middle part of the image is formed by intersection faults which have broken the Venusian crust into a clomplex, deformed type of surface called tessera, the Latin word for tile. The parallel mountains and valleys resemble the Basin and Range Province in the western United States. The irregular dark patch near the top of the image is a smooth surface, probably formed by lava flows in a region about 10 km (6 mi.) across. Similar dark surfaces within the valleys indicate lava flows that are younger than the tessera giving an indication of the geologic time relationships of the events that formed the present surface. The image has a resolution of 120 meters (400 feet). |
| Date |
8/21/90 |
|
A90-3004
Photographer : JPL Two mosai
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8/24/90
| Description |
Photographer : JPL Two mosaicked pieces of Magellan image strips display the area east of the Rhea Mons volcano on Venus. This image is centered at about 32.5 degrees north latitude and 286.6 degrees east longitude. The mosaic is 47 km (28 mi.) wide and 135 km (81 mi.) long. This region has been previously identified as "tessera"from Earth-based radar (Arecibo) images. The center of the image is dominated by a network of intersection ridges and valleys. The radar-bright north-south trending features in this image range from 1 km (0.6 mi.) to 3 km (1.8 mi.) in length. The average spacing between these ridges is about 1.5 km (0.9 mi.). The dark patches at the top of the image are smooth surfaces and may be lava flows located in lowlands between the higher ridge and the valley terrain. This image is a mosaic of two orbits obtained in the first Magellan stations near Goldstone, CA and Canberra, Australia. The resolution of this image is approx. 120 meters (400 feet). |
| Date |
8/24/90 |
|
AC90-3007
Photographer : JPL This Mage
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11/16/90
| Description |
Photographer : JPL This Magellan image reveals Sacajawea Patera, a large, elongate caldera located in wester Ishtar Terra on the smooth plateau of Lakshmi Planum. The image is centered at 64.5 degrees north latitude adn 337 degrees east longitude. It is approx. 420 km (252 mi.) wide at the base Sacajawea is a depression approx. 1-2 km (0.6-1.2 mi.) deep and 120 by 215 km (74 by 133 mi.) in diameter, it is elongate in a sousthwest-northeast direction. The depression is interpreted to be graben adn fault scarps. These structures are space 0.5 to 4 km (0.3 to 2.5 mi.) apart, are 0.6 to 4 km (0.4 to 2.5 mi.) in width and up to 100 km (62 mi.) in length. Extending up to 140 km (87 mi.) in length from the southeast of the patera is a system of linear structures thought to represent a flanking rift zone along which the lateral injection and eruption of magma may have occurred. A shield edifice 12 km (7 mi.) in diameter with a prominent central pit lies along the trend of one of these features. The impact crater zlata, approx. 6 km (4 mi.) in diameter is located within the zone of graben to the northwest of the patera. Few flow features are observed in association with sacajawea, possibly due to age and state of degradation of the flows. Mottled bright deposits 4 to 20 km (2.5 to 12 mi.) in width are located near the periphery and in the center of the patera floor within local topographic lows. Diffuse patches of dark material approx. 40 km (25 mi.) in width are observed southwest of the patera, superimposed on portions of the surrounding graben. The formation of sacajawea is thought to be related to the drainage and collapse of a large magma chamber. Gravitational relaxation may have caused the resultant caldera to sag, producing the numerous complex, highly deformed tessera-like terrain are located north and east of the patera and are seen in the upper portion of the image. Color has been added to this image to simulate the appearance of the Venus surface. |
| Date |
11/16/90 |
|
AC91-3008
Photographer : JPL This glob
…
10/29/91
| Description |
Photographer : JPL This global view of the surface of Venus is centered at 270 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 inhance small-scale structure. The simulated hues are based on color images recorded by the Soviet Venera 13 and 14 spacecraft. |
| Date |
10/29/91 |
|
AC91-3009
Photographer : JPL The north
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10/29/91
| Description |
Photographer : JPL 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 6, 3, 12 and 9 0'clock positions, repectively, of an imagery clock face. Magellan synthetic aperture radar mosaics from the first cycle of Magelolan mapping are mapped onto a computer-simulated globe to create this image. Data gaps are filled with Pioneere-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 & 14 spacecraft. |
| Date |
10/29/91 |
|
Cassini Spacecraft / Titan I
…
| Name of Image |
Cassini Spacecraft / Titan IVB Centaur Launch |
| Date of Image |
1996-11-07 |
| Full Description |
The journey back to Mars begins with a liftoff of the Mars Global Surveyor atop a Delta II 7925A expendable launch vehicle from the Cape Canaveral Air Station. After an approximate 10-month interplanetary odyssey, the spacecraft will arrive at Mars and begin a 4-month aerobreaking phase, an irnovative technique first demonstrated during the Magellan mission to Venus, to achieve a mapping orbit. It will take about 2 Earth years for Surveyor to circle above most of the planet, its suite of sophisticated remote-sensing instruments building a comprehensive global portrait of Mars by mapping its topography, magnetism, mineral composition and atmosphere. Among the locations the Surveyor will pass over are the landing sites where the two U.S. Viking landers have stood since 1975 as silent monuments to the most recent successful U.S. missions to Mars. The Global Surveyor is the first of a trio of spacecraft being launched to Mars, next is Russia's Mars `96 spacecraft, followed by the U.S.'s Mars Pathfinder. |
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STS-30 Mission Insignia
| Name of Image |
STS-30 Mission Insignia |
| Date of Image |
1989-03-08 |
| Full Description |
The STS-30 patch depicts the joining of NASA's manned and unmanned space programs. The sun and inner planets of our solar system are shown with the curve connecting Earth and Venus symbolizing the shuttle orbit, the spacecraft trajectory toward Venus, and its subsequent orbit around our sister planet. A Spanish caravel similar to the ship on the official Magellan program logo commemorates the 16th century explorer's journey and his legacy of adventure and discovery. Seven stars on the patch honor the crew of Challenger. The five-star cluster in the shape of the constellation Cassiopeia represent the five STS-30 crewmembers - Astronauts David Walker, Ronald Grabe, Norman Thagard, Mary Cleave and Mark Lee - who collectively designed the patch. |
|
STS-30 Launch
| Name of Image |
STS-30 Launch |
| Date of Image |
1989-05-05 |
| Full Description |
The STS-30 mission launched aboard the Space Shuttle Atlantis on May 4, 1989 at 2:46:59pm (EDT) carrying a crew of five. Aboard were Ronald J. Grabe, pilot, David M. Walker, commander, and mission specialists Norman E. Thagard, Mary L. Cleave, and Mark C. Lee. The primary payload for the mission was the Magellan/Venus Radar mapper spacecraft and attached Inertial Upper Stage (IUS). |
|
STS-30 Crew Portrait
| Name of Image |
STS-30 Crew Portrait |
| Date of Image |
1988-04-26 |
| Full Description |
Five astronauts composed the STS-30 crew. Pictured (left to right) are Ronald J. Grabe, pilot, David M. Walker, commander, and mission specialists Norman E. Thagard, Mary L. Cleave, and Mark C. Lee. The STS-30 mission launched aboard the Space Shuttle Atlantis on May 4, 1989 at 2:46:59pm (EDT). The primary payload was the Magellan/Venus Radar mapper spacecraft and attached Inertial Upper Stage (IUS). |
|
STS-30 Launch
| Name of Image |
STS-30 Launch |
| Date of Image |
1989-05-05 |
| Full Description |
The STS-30 mission launched aboard the Space Shuttle Atlantis on May 4, 1989 at 2:46:59pm (EDT) carrying a crew of five. Aboard were Ronald J. Grabe, pilot, David M. Walker, commander, and mission specialists Norman E. Thagard, Mary L. Cleave, and Mark C. Lee. The primary payload for the mission was the Magellan/Venus Radar mapper spacecraft and attached Inertial Upper Stage (IUS). |
|
STS-30 Launch
| Name of Image |
STS-30 Launch |
| Date of Image |
1989-05-05 |
| Full Description |
The STS-30 mission launched aboard the Space Shuttle Atlantis on May 4, 1989 at 2:46:59pm (EDT) carrying a crew of five. Aboard were Ronald J. Grabe, pilot, David M. Walker, commander, and mission specialists Norman E. Thagard, Mary L. Cleave, and Mark C. Lee. The primary payload for the mission was the Magellan/Venus Radar mapper spacecraft and attached Inertial Upper Stage (IUS). |
|
Arecibo/Magellan Composite o
…
| Title |
Arecibo/Magellan Composite of Quetzalpetlatl Corona |
| Description |
This composite image was created by inserting approximately 70 orbits of Magellan data into an image obtained at the Arecibo, Puerto Rico radiotelescope and shows a geologically complex region in the southern hemisphere of Venus. The region is centered on 65 degrees south, 359 degrees east and is about 1500 x 1500 km (900 x 900 miles) in extent. The large oval feature in the lower half of the image is Quetzalpetlatl Corona, approximately 700 km (420 miles) in diameter. Coronae are circular to oval regions defined by an annulus of ridges and are centers for tectonic and volcanic activity. Tectonic activity is largely observed in a relatively narrow rim region, which in this image is defined by a complex lineated terrain that surrounds much of the corona. Bright and dark volcanic flows are seen throughout the corona and surrounding terrain. Small shield volcanoes, 1-20 km (0.6-12 miles) in diameter, are seen near the southern limit of the Magellan data image. Narrow linear troughs (seen in the image as bright lines) trend to the north-northwest of Quetzalpetlatl. |
| Date |
11.07.1990 |
|
Art concept of Magellan spac
…
| Title |
Art concept of Magellan spacecraft in cruise configuration |
| Description |
Magellan spacecraft cruise configuration is illustrated in this artist concept. With solar panels deployed and having jettisoned the inertial upper stage (IUS), Magellan approaches the sun which it will orbit approximately 1.6 times before encountering Venus. Magellan, named after the 16th century Portuguese explorer, will orbit Venus about once every three hours, acquiring radar data for 37 minutes of each orbit when it is closest to the surface. Using an advanced instrument called a synthetic aperture radar (SAR), it will map more than 90 per cent of the surface with resolution ten times better than the best from prior spacecraft. Magellan is managed by the Jet Propulsion Laboratory (JPL), Martin Marietta Aerospace is developing the spacecraft and Hughes Aircraft Company, the advanced imaging radar. Magellan will be deployed from payload bay (PLB) of Atlantis, Orbiter Vehicle (OV) 104, during the STS-30 mission. |
| Date |
04.27.1988 |
|
Artist concept of Magellan s
…
| Title |
Artist concept of Magellan spacecraft in elliptical orbit around Venus |
| Description |
Magellan spacecraft is shown in elliptical orbit around Venus, collecting data (radar mapping), and then transmitting data back to Earth in this artist concept. When the spacecraft orbit is close to Venus the synthetic aperature radar (SAR) will image a swath between 9 and 15 nautical miles (10 and 17 statute miles) (highlighted in image), beginning at or near the north pole and continuing to the southern hemisphere. Subsequent swaths will slightly overlap and, during its primary mission, the spacecraft will map most of the planet. When the spacecraft moves into the part of its elliptical orbit farthest from Venus, the spacecraft high-gain antenna will be turned toward Earth and will send the data collected during the imaging to Earth. Magellan, named after the 16th century Portuguese explorer, will orbit Venus about once every three hours, acquiring radar data for 37 minutes of each orbit. Magellan is managed by the Jet Propulsion Laboratory (JPL), Martin Marietta is developing the sp |
| Date |
09.21.1988 |
|
Artist concept of Magellan s
…
| Title |
Artist concept of Magellan spacecraft orbiting Venus |
| Description |
Magellan spacecraft orbits Venus in this artist concept. The continued quest for detailed topographic measurements of Venus will again be undertaken in April 1989 by Magellan, named after the 16th century Portuguese explorer. Magellan will orbit Venus about once every three hours, acquiring radar data for 37 minutes of each orbit when it is closest to the surface. Using an advanced instrument called a synthetic aperature radar (SAR), it will map more than 90 per cent of the surface with resolution ten times better than the best prior spacecraft. Magellan is managed by the Jet Propulsion Laboratory (JPL), Martin Marietta is developing the spacecraft and Hughes Aircraft Company, the advanced imaging radar. Magellan will be deployed from the payload bay (PLB) of Atlantis, Orbiter Vehicle (OV) 104, during mission STS-30. |
| Date |
04.27.1988 |
|
Solar System Montage
| Title |
Solar System Montage |
| Description |
This is a montage of planetary images taken by spacecraft managed by the Jet Propulsion Laboratory in Pasadena, CA. Included are (from top to bottom) images of Mercury, Venus, Earth (and Moon), Mars, Jupiter, Saturn, Uranus and Neptune. The spacecraft responsible for these images are as follows: the Mercury image was taken by Mariner 10, the Venus image by Magellan, the Earth image by Galileo, the Mars image by Viking, and the Jupiter, Saturn, Uranus and Neptune images by Voyager. |
| Date |
02.01.1996 |
|
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 |
|
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 - Comparison of Initia
…
| Title |
Venus - Comparison of Initial Magellan Radar Test and Data Acquired in 4/91 |
| Description |
This image compares Magellan data acquired in August 1990 during the initial test of the radar system (black and white insets) with data acquired by the spacecraft in April 1991 (color background). The area is in the southern hemisphere of Venus, and represents an area about 540 kilometers (330 miles) on a side, centered on latitude 35 degrees south and longitude 294 degrees east. The Magellan radar illuminates the surface from the left. The northern and eastern parts of the area consist of plains which appear moderately dark to dark on the radar image because they are relatively smooth at a scale comparable to the wavelength of the radar, 12.5 centimeters (about 5 inches). The bright terrain in the southwestern part of the image is about 500 to 700 meters (1640 to 2300 feet) higher than the plains, it is characterized by abundant faults and fractures, which appear as straight to gently curved bright lines. Many of these linear features are large enough to infer that they are grabens, which are troughs bounded on both sides by faults. However, many of them are too narrow to determine if they are faults or simply fractures that have roughened the surface. This elevated faulted and fractured region is part of a large east-west elongated ridge mapped by the Pioneer Venus radar altimeter, the portion shown here is about midway between Themis Regio and Tefnut Mons. The plains are probably underlain by volcanic lavas. The various shades indicate that minor differences in surface roughness are present, and these may be used to map out the distribution of different lavas. The small, bright patches on the plains represent places where the lava surfaces are relatively rough. Just left of the center of the image is a sharply defined volcanic crater about 15 kilometers (9 miles) in diameter. Immediately north of this crater are numerous round spots about 204 kilometers (102 miles) across that are small volcanic domes. |
| Date |
04.28.1991 |
|
Venus - Crater Golubkina
| Title |
Venus - Crater Golubkina |
| Description |
This Magellan image mosaic shows the impact crater Golubkina, first identified in Soviet Venera 15/16 data. The crater is named after Anna Golubkina (1864-1927), a Soviet sculptor. The crater is about 34 kilometers (20.4 miles) across, similar to the size of the West Clearwater impact structure in Canada. The crater Golubkina is located at about 60.5 degrees north latitude, 286.7 degrees east longitude. Magellan data reveal that Golubkina has many characteristics typical of craters formed by a meteorite impact including terraced inner walls, a central peak, and radar bright rough ejecta surrounding the crater. The extreme darkness of the crater floor indicates a smooth surface, perhaps formed by the pounding of lava flows in the crater floor as seen in many lunar impact craters. The radar bright ejecta surrounding the crater indicates a relatively fresh or young crater. Craters with central peaks in the Soviet data range in size from about 10.60 km (6.36 miles) across. The largest crater identified in the Soviet Venera data is 140 km (84 miles) in diameter. This Magellan image strip is approximately 20 km (12 miles) wide and this piece of the image is approximately 100 km (62 miles) long. The image is a mosaic of two orbits obtained in the first Magellan radar test and played back to Earth to the Deep Space Network stations near Goldstone, Calif. and Canberra, Australia, respectively. The resolution of this image is approximately 120 meters (400 feet). The see-saw margins result from the offset of individual radar frames obtained along the orbit. The spacecraft moved from the north (top) to the south, looking to the left. |
| Date |
08.24.1990 |
|
Venus - Interior of Ovda Reg
…
| Title |
Venus - Interior of Ovda Regio |
| Description |
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. |
| Date |
03.05.1991 |
|
Venus - Lada Terra Region
| Title |
Venus - Lada Terra Region |
| Description |
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. |
| Date |
04.12.1991 |
|
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 |
|
Visual aid titled "The Magel
…
| Title |
Visual aid titled "The Magellan Mission to Venus |
| Description |
Visual aid titled "The Magellan Mission to Venus" describes data that will be collected and science objectives. Images and brightness temperatures will be obtained for 70-90% of the surface, with a radar resolution of 360 meters or better. The global gravity field model will be refined by combining Magellan and Pioneer-Venus doppler data. Altimetry data will be used to measure the topography of 70-90% of the surface with a vertical accuracy of 120-360 meters. Science objectives include: to improve the knowledge of the geological history of Venus by analysis of the surface morphology and electrical properties and the processes that control them, and to improve the knowledge of the geophysics of Venus, principally its density distribution and dynamics. Magellan, named for the 16th century Portuguese explorer, will be deployed from the payload bay (PLB) of Atlantis, Orbiter Vehicle (OV) 104, during mission STS-30. |
| Date |
04.27.1988 |
|
Atlantis Tribute
nasa, spaceshuttlegallery
This is a printable version
…
488843main_2atlantis
| mediatype |
IMAGE |
| mediatype |
image |
| date |
2010-10-15 |
| creator |
NASA |
| identifier |
488843main_2atlantis |
|
Venus Rising
nasa, nasaimageofthedaygalle
…
This hemispheric view of Ven
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508439main_PIA00007
| mediatype |
IMAGE |
| mediatype |
image |
| date |
2011-01-05 |
| creator |
NASA |
| identifier |
508439main_PIA00007 |
|
Venus - Maxwell Montes and C
…
PIA00149
Sol (our sun)
Imaging Radar
| Title |
Venus - Maxwell Montes and Cleopatra Crater |
| Original Caption Released with Image |
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. |
|
Venus - Mead Crater
PIA00148
Sol (our sun)
Imaging Radar
| Title |
Venus - Mead Crater |
| Original Caption Released with Image |
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. |
|
Venus - Ovda Regio
PIA00146
Sol (our sun)
Imaging Radar
| Title |
Venus - Ovda Regio |
| Original Caption Released with Image |
This image covers much of Ovda Regio, which forms the western part of Aphrodite Terra. It covers an area about 2,250 kilometers (1,386 miles) wide by 1,300 kilometers (800 miles) north to south, and ranges in latitude from 8 degrees north to 12 degrees south and in longitude from 62 degrees east to 90 degrees east. Ovda Regio is a highland region that rises over 4 kilometers (2.5 miles) above the surrounding plain. Magellan images show a complex surface, with several generations of structures. A pervasive fabric of irregular broad domes and ridges and associated curvilinear valleys was flooded by lava, then fractured. The circular feature surrounded by dark lava flows in the western part of the image is a caldera, or large volcanic collapse pit. Late-stage extension created long graben, or fault-bounded valleys, is best seen near the center of the image. The northern boundary of Ovda Regio is a steep, curvilinear mountain belt made up of long, narrow, rounded ridges. These ridges are similar in appearance to folded mountain belts on Earth. Several impact craters, such as the circular features on the western margin of the image, are scattered across the area. The bright area in the southeast part of the image indicates the presence of a radar-reflective mineral such as pyrite. Most of the highland areas on Venus display a similar bright signal. Each pixel of this image covers an area on the surface 675 meters (2,215 feet) across, representing a 9- times reduction in resolution compared to full-scale resolution data. |
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