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Polar Dust Devil Streaks
PIA06334
Sol (our sun)
Mars Orbiter Camera
| Title |
Polar Dust Devil Streaks |
| Original Caption Released with Image |
30 June 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image of dunes in the martian north polar region is important because it shows one of the highest northern latitude views of streaks thought to be made by passing dust devils. The dark, thin, filamentary streaks on the dunes and on the adjacent plains were probably formed by dust devils. The dunes occur near 76.6°N, 62.7°W. Dust devil streaks are observed on Mars at very high latitudes, such as this, all the way down to the equator. They are also seen at all elevations, from the deepest parts of the Hellas Basin to the summit of Olympus Mons. This picture covers an area about 3 km (1.9 mi) wide. Sunlight illuminates the scene from the lower left. |
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Cloud-Ground Interaction
PIA06449
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Cloud-Ground Interaction |
| Original Caption Released with Image |
Released 30 June 2004The atmosphere of Mars is a dynamic system. Water-ice clouds, fog, and hazes can make imaging the surface from space difficult. Dust storms can grow from local disturbances to global sizes, through which imaging is impossible. Seasonal temperature changes are the usual drivers in cloud and dust storm development and growth. Eons of atmospheric dust storm activity has left its mark on the surface of Mars. Dust carried aloft by the wind has settled out on every available surface, sand dunes have been created and moved by centuries of wind, and the effect of continual sand-blasting has modified many regions of Mars, creating yardangs and other unusual surface forms. This image of the North Polar water-ice clouds shows how surface topography can affect the linear form. Notice that the crater at the bottom of the image is causing a deflection in the linear form. Image information: VIS instrument. Latitude 68.4, Longitude 100.7 East (259.3 West). 38 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Cloud-Ground Interaction
PIA06449
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Cloud-Ground Interaction |
| Original Caption Released with Image |
Released 30 June 2004The atmosphere of Mars is a dynamic system. Water-ice clouds, fog, and hazes can make imaging the surface from space difficult. Dust storms can grow from local disturbances to global sizes, through which imaging is impossible. Seasonal temperature changes are the usual drivers in cloud and dust storm development and growth. Eons of atmospheric dust storm activity has left its mark on the surface of Mars. Dust carried aloft by the wind has settled out on every available surface, sand dunes have been created and moved by centuries of wind, and the effect of continual sand-blasting has modified many regions of Mars, creating yardangs and other unusual surface forms. This image of the North Polar water-ice clouds shows how surface topography can affect the linear form. Notice that the crater at the bottom of the image is causing a deflection in the linear form. Image information: VIS instrument. Latitude 68.4, Longitude 100.7 East (259.3 West). 38 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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| General Description |
International Space Station Imagery |
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| General Description |
International Space Station Imagery |
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| General Description |
International Space Station Imagery |
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| General Description |
International Space Station Imagery |
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| General Description |
International Space Station Imagery |
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| General Description |
International Space Station Imagery |
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| General Description |
International Space Station Imagery |
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