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Waspie_Dwarf
Mars Odyssey Mission
Marte Vallis


Location: 15.8N, 184.2E
Released: 2008-09-26
Image Size: 18.6 x 65.9 km, 1024 x 3648 px
Resolution: 18m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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Marte Vallis is a large, complex lava channel. This VIS image shows how the lava is able to create features, such as streamlined islands, that are more commonly seen in water carved channels.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Hebrus Vallis


Location: 19.0N, 126.9E
Released: 2008-09-29
Image Size: 18.8 x 66.4 km, 1024 x 3648 px
Resolution: 18m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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The channels seen in this image are all part of Hebrus Vallis. Hebrus Vallis is just one of the many channel systems in Utopia Planitia.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Landslide


Location: 13.3N, 341.9E
Released: 2008-09-30
Image Size: 18.6 x 65.7 km, 1024 x 3648 px
Resolution: 18m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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The landslide seen in this VIS image is located in an unnamed crater in Arabia Terra.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Faulting


Location: 35.7N, 229.8E
Released: 2008-10-01
Image Size: 19.3 x 68.1 km, 1024 x 3648 px
Resolution: 19m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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The ridge in the upper portion of this image is located in Acheron Fossae, a large, arcuate set of faulted ridges north of Lycus Sulci and Olympus Mons.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Candor Chasma


Location: -8.0N, 295.2E
Released: 2008-10-02
Image Size: 18.0 x 63.7 km, 1024 x 3648 px
Resolution: 18m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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This VIS image shows some of the floor deposits within Candor Chasma. These deposits have been eroded by wind, and possibly by water.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Landslide


Location: -19.3N, 149.4E
Released: 2008-10-03
Image Size: 17.9 x 63.2 km, 1024 x 3648 px
Resolution: 17m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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The landslide seen in this VIS image occurs within an unnamed crater in Terra Cimmeria.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Yardangs


Location: 1.1N, 150.9E
Released: 2008-10-06
Image Size: 18.3 x 64.6 km, 1024 x 3648 px
Resolution: 18m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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The linear features in this VIS image are called yardangs. Yardangs are formed when winds erode poorly cemented materials, like those that form Zephyria Planum.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Polar Dunes


Location: 73.8N, 310.3E
Released: 2008-10-07
Image Size: 20.3 x 71.7 km, 1024 x 3648 px
Resolution: 20m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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This VIS image of north polar dunes illustrates how individual dunes cluster into large sand seas.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Collapse Features


Location: 20.1N, 253.9E
Released: 2008-10-08
Image Size: 18.7 x 66.2 km, 1024 x 3648 px
Resolution: 18m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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The connected oval depressions are locations where the surface has collapsed into voids in the underlying lava flow. This image is located in the Tharsis region north of Ascraeus Mons.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Surface Texture


Location: -0.2N, 280.0E
Released: 2008-10-09
Image Size: 18.2 x 64.3 km, 1024 x 3648 px
Resolution: 18m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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This VIS image shows part of the floor of Echus Chasma. The unusual texture is likely a result of lava flows.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
October 09, 2008

NASA's Mars Odyssey Shifting Orbit for Extended Mission


PASADENA, Calif. -- The longest-serving of six spacecraft now studying Mars is up to new tricks for a third two-year extension of its mission to examine the most Earthlike of known foreign planets.

NASA's Mars Odyssey is altering its orbit to gain even better sensitivity for its infrared mapping of Martian minerals. During the mission extension through September 2010, it will also point its camera with more flexibility than it has ever used before. Odyssey reached Mars in 2001.

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Artist concept of Odyssey.
Image credit: NASA/JPL
Larger Image


The orbit adjustment will allow Odyssey's Thermal Emission Imaging System to look down at sites when it's mid-afternoon, rather than late afternoon. The multipurpose camera will take advantage of the infrared radiation emitted by the warmer rocks to provide clues to the rocks' identities.

"This will allow us to do much more sensitive detection and mapping of minerals," said Odyssey Project Scientist Jeffrey Plaut of NASA's Jet Propulsion Laboratory, Pasadena, Calif.

The mission's orbit design before now used a compromise between what works best for the Thermal Emission Imaging System and what works best for another instrument, the Gamma Ray Spectrometer.

On commands from its operations team at JPL and at Denver-based Lockheed Martin Space Systems, Odyssey fired thrusters for nearly 6 minutes on Sept. 30, the final day of the mission's second two-year extension.

"This was our biggest maneuver since 2002, and it went well," said JPL's Gaylon McSmith, Odyssey mission manager. "The spacecraft is in good health. The propellant supply is adequate for operating through at least 2015."

Odyssey's orbit is synchronized with the sun. The local solar time has been about 5 p.m. at whatever spot on Mars Odyssey flew over as it made its dozen daily passes from between the north pole region to the south pole region for the past five years. (Likewise, the local time has been about 5 a.m. under the track of the spacecraft during the south-to-north leg of each orbit.)

The push imparted by the Sept. 30 maneuver will gradually change that synchronization over the next year or so. Its effect is that the time of day on the ground when Odyssey is overhead is now getting earlier by about 20 seconds per day. A follow-up maneuver, probably in late 2009 when the overpass time is between 2:30 and 3:00 p.m., will end the progression toward earlier times.

While aiding performance of the Thermal Emission Imaging System, the shift to mid-afternoon is expected to stop the use of one of three instruments in Odyssey's Gamma Ray Spectrometer suite. The suite's gamma ray detector needs a later-hour orbit to avoid overheating of a critical component. The suite's neutron spectrometer and high-energy neutron detector are expected to keep operating.

The Gamma Ray Spectrometer provided dramatic discoveries of water-ice near the surface throughout much of high-latitude Mars, the impetus for NASA's Phoenix Mars Lander mission. The gamma ray detector has also mapped global distribution of many elements, such as iron, silicon and potassium, a high science priority for the first and second extensions of the Odyssey mission. A panel of planetary scientists assembled by NASA recommended this year that Odyssey make the orbit adjustment to get the best science return from the mission in coming years.

Increased sensitivity for identifying surface minerals is a key science goal for the mission extension beginning this month. Also, the Odyssey team plans to begin occasionally aiming the camera away from the straight-down pointing that has been used throughout the mission. This will allow the team to fill in some gaps in earlier mapping and also create some stereo, three-dimensional imaging.

Odyssey will continue providing crucial support for Mars surface missions as well as conducting its own investigations. It has relayed to Earth nearly all data returned from NASA rovers Spirit and Opportunity. It shares with NASA's Mars Reconnaissance Orbiter the relay role for Phoenix. It has made targeted observations for evaluating candidate landing sites.

Mars Odyssey, launched in 2001, is managed by JPL, a division of the California Institute of Technology, Pasadena, for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. Investigators at Arizona State University, Tempe, operate the Thermal Emission Imaging System. Investigators at the University of Arizona, Tucson, head operation of the Gamma Ray Spectrometer. Additional science partners are located at the Russian Aviation and Space Agency, which provided the high-energy neutron detector, and at Los Alamos National Laboratories, New Mexico, which provided the neutron spectrometer.

For more about the Mars Odyssey mission, visit: http://mars.jpl.nasa.gov/odyssey.
###

Guy Webster 818-354-6278
Jet Propulsion Laboratory, Pasadena, California
guy.webster@jpl.nasa.gov

Dwayne Brown 202-358-1726
Headquarters, Washington, D.C. dwayne.c.brown@nasa.gov

NEWS RELEASE: 2008-191

Source: NASA/JPL - Odyssey - Press Releases
Waspie_Dwarf
Mars Odyssey Mission
Dunes


Location: 58.2N, 58.9E
Released: 2008-10-10
Image Size: 19.9 x 70.4 km, 1024 x 3648 px
Resolution: 19m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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The dunes in this image are located in an unnamed crater in western Utopia Plainitia.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Slope Streaks


Location: 4.7N, 34.8E
Released: 2008-10-13
Image Size: 18.3 x 64.8 km, 1024 x 3648 px
Resolution: 18m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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This VIS image shows an unnamed crater in Terra Sabaea with prominent dark slope streaks.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Gullies


Location: 53.1N, 57.6E
Released: 2008-10-14
Image Size: 19.8 x 69.9 km, 1024 x 3648 px
Resolution: 19m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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This unnamed crater in western Utopia Planitia contains both gullies and a landslide deposit that may be related to the formation of some gullies.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Dunes


Location: 45.3N, 69.8E
Released: 2008-10-15
Image Size: 19.5 x 69.1 km, 1024 x 3648 px
Resolution: 19m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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The dunes in this image are located in an unnamed crater in Utopia Planitia.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Fractures and Collapse


Location: 30.1N, 138.7E
Released: 2008-10-16
Image Size: 19.1 x 67.6 km, 1024 x 3648 px
Resolution: 19m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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The fracturing and collapse seen in this VIS image are related to the Elysium Volcanic Complex.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Lava Channel


Location: 38.3N, 269.6E
Released: 2008-10-17
Image Size: 19.5 x 68.9 km, 1024 x 3648 px
Resolution: 19m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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The channel in this VIS image is located in the Tharsis Volcanic region, east of Alba Patera and north of Mareotis Fossae.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Polar Dunes


Location: 80.5N, 308.9E
Released: 2008-10-20
Image Size: 35.3 x 353.4 km, 320 x 3600 px
Resolution: 110m
Instrument: IR

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Image Credit: NASA/JPL/ASU
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This IR image of the north polar region shows a long dune formation. The dunes in this image appear bright due to their warm temperature rather than the actual color of the material.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Polar Dunes


Location: 76.5N, 295.6E
Released: 2008-10-21
Image Size: 20.5 x 72.4 km, 1024 x 3648 px
Resolution: 20m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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This VIS image shows a small portion of the enormous sea of dunes located in and around the north polar cap.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Cerulli Channels


Location: 32.9N, 22.5E
Released: 2008-10-22
Image Size: 19.2 x 68.0 km, 1024 x 3648 px
Resolution: 19m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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The channels in this VIS image are located on the inner rim of Cerulli Crater.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Polar Dunes


Location: 74.3N, 308.2E
Released: 2008-10-23
Image Size: 20.2 x 71.6 km, 1024 x 3648 px
Resolution: 20m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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This VIS image shows a region of dunes near the north polar cap that are individual dune forms.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Dark Slope Streaks


Location: 21.5N, 178.8E
Released: 2008-10-24
Image Size: 18.8 x 66.6 km, 1024 x 3648 px
Resolution: 18m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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Dark slope streaks are prevalent on these isolated hills near the Tartarus Montes.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Channel


Location: 36.2N, 36.8E
Released: 2008-10-27
Image Size: 19.3 x 68.2 km, 1024 x 3648 px
Resolution: 19m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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This VIS image shows part of a channel located on the plains of Terra Sabaea.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Semeykin Drainage


Location: 41.1N, 7.8E
Released: 2008-10-28
Image Size: 19.6 x 69.4 km, 1024 x 3648 px
Resolution: 19m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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This impressive drainage system empties into Semeykin Crater on the northern margin of Arabia Terra.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Linear Ridges


Location: 27.2N, 74.6E
Released: 2008-10-29
Image Size: 19.0 x 67.3 km, 1024 x 3648 px
Resolution: 19m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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This region of criss-crossing linear ridges is located just north of Nili Fossae.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Dust Devil Tracks


Location: 54.6N, 179.8E
Released: 2008-10-30
Image Size: 19.9 x 70.6 km, 1024 x 3648 px
Resolution: 19m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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A multitude of dust devil tracks are visible on this image of the northern plains near Phlegra Montes.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Arcuate Fractures


Location: -2.1N, 173.2
Released: 2008-10-31
Image Size: 18.3 x 64.6 km, 1024 x 3648 px
Resolution: 18m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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Called Averuns Colles, these broken blocks and arcuate fractures mark the transition region between the southern highlands and the northern lowlands of Mars.

Source: THEMIS - Mars Odyssey Mission
Waspie_Dwarf
Mars Odyssey Mission
Dunes and Channel


Location: -6.0N, 114.9E
Released: 2008-11-03
Image Size: 18.2 x 64.3 km, 1024 x 3648 px
Resolution: 18m
Instrument: VIS

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Image Credit: NASA/JPL/ASU
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This VIS image shows part of Tagus Valles and a small field of dunes in an unnamed crater.

Source: THEMIS - Mars Odyssey Mission
Vertical Gunn
QUOTE (Waspie_Dwarf @ Aug 30 2006, 07:48 AM) *
Mars Odyssey Mission
Channel


Location: 1.3N,173.4E
Released: 2006-08-30
Instrument: VIS
Image Size: 18.1x64.1 km, 1024x3648 px
Resolution: 18m

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Image Credit: NASA/JPL/ASU
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This region of arcuate fractures and chaos development on the highland/lowland boundary is called Avernus Colles.

Source: THEMIS - Mars Odyssey Mission


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