Mission Mars Odyssey - 4

<h1>PIA07010: North Polar Cap</h1><div class="PIA07010" lang="en" style="width:554px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07010_fig1.jpg"> </a><br /><p>This week we will be looking at five examples of laminar wind flow on the north polar cap. On Earth, gravity-driven south polar cap winds are termed "catabatic" winds. Catabatic winds begin over the smooth expanse of the cap interior due to temperature differences between the atmosphere and the surface. Once begun, the winds sweep outward along the surface of the polar cap toward the sea. As the polar surface slopes down toward sealevel, the wind speeds increase. Catabatic wind speeds in the Antartic can reach several hundreds of miles per hour.</p><p>In the images of the Martian north polar cap we can see these same type of winds. Notice the streamers of dust moving downslope over the darker trough sides, these streamers show the laminar flow regime coming off the cap. Within the trough we see turbulent clouds of dust, kicked up at the trough base as the winds slow down and enter a chaotic flow regime.</p><p>The horizontal lines in these images are due to framelet overlap and lighting conditions over the bright polar cap.</p><p>Image information: VIS instrument. Latitude 84.2, Longitude 57.4 East (302.6 West). 40 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07010" onclick="window.open(this.href); return false;" title="Voir l'image PIA07010: North Polar Cap sur le site de la NASA">Voir l'image PIA07010: North Polar Cap sur le site de la NASA.</a></div>
PIA07010: North Polar Cap
<h1>PIA07011: North Polar Cap</h1><div class="PIA07011" lang="en" style="width:506px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07011_fig1.jpg"> </a><br /><p>This week we will be looking at five examples of laminar wind flow on the north polar cap. On Earth, gravity-driven south polar cap winds are termed "catabatic" winds. Catabatic winds begin over the smooth expanse of the cap interior due to temperature differences between the atmosphere and the surface. Once begun, the winds sweep outward along the surface of the polar cap toward the sea. As the polar surface slopes down toward sealevel, the wind speeds increase. Catabatic wind speeds in the Antartic can reach several hundreds of miles per hour.</p><p>In the images of the Martian north polar cap we can see these same type of winds. Notice the streamers of dust moving downslope over the darker trough sides, these streamers show the laminar flow regime coming off the cap. Within the trough we see turbulent clouds of dust, kicked up at the trough base as the winds slow down and enter a chaotic flow regime.</p><p>The horizontal lines in these images are due to framelet overlap and lighting conditions over the bright polar cap.</p><p>Image information: VIS instrument. Latitude 84.3, Longitude 314.4 East (45.6 West). 40 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07011" onclick="window.open(this.href); return false;" title="Voir l'image PIA07011: North Polar Cap sur le site de la NASA">Voir l'image PIA07011: North Polar Cap sur le site de la NASA.</a></div>
PIA07011: North Polar Cap
<h1>PIA07012: North Polar Cap</h1><div class="PIA07012" lang="en" style="width:490px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07012_fig1.jpg"> </a><br /><p>This week we will be looking at five examples of laminar wind flow on the north polar cap. On Earth, gravity-driven south polar cap winds are termed "catabatic" winds. Catabatic winds begin over the smooth expanse of the cap interior due to temperature differences between the atmosphere and the surface. Once begun, the winds sweep outward along the surface of the polar cap toward the sea. As the polar surface slopes down toward sealevel, the wind speeds increase. Catabatic wind speeds in the Antartic can reach several hundreds of miles per hour.</p><p>In the images of the Martian north polar cap we can see these same type of winds. Notice the streamers of dust moving downslope over the darker trough sides, these streamers show the laminar flow regime coming off the cap. Within the trough we see turbulent clouds of dust, kicked up at the trough base as the winds slow down and enter a chaotic flow regime.</p><p>The horizontal lines in these images are due to framelet overlap and lighting conditions over the bright polar cap.</p><p>Image information: VIS instrument. Latitude 86.5, Longitude 64.5 East (295.5 West). 40 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07012" onclick="window.open(this.href); return false;" title="Voir l'image PIA07012: North Polar Cap sur le site de la NASA">Voir l'image PIA07012: North Polar Cap sur le site de la NASA.</a></div>
PIA07012: North Polar Cap
<h1>PIA07013: North Polar Cap</h1><div class="PIA07013" lang="en" style="width:516px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07013_fig1.jpg"> </a><br /><p>This week we will be looking at five examples of laminar wind flow on the north polar cap. On Earth, gravity-driven south polar cap winds are termed "catabatic" winds. Catabatic winds begin over the smooth expanse of the cap interior due to temperature differences between the atmosphere and the surface. Once begun, the winds sweep outward along the surface of the polar cap toward the sea. As the polar surface slopes down toward sealevel, the wind speeds increase. Catabatic wind speeds in the Antartic can reach several hundreds of miles per hour.</p><p>In the images of the Martian north polar cap we can see these same type of winds. Notice the streamers of dust moving downslope over the darker trough sides, these streamers show the laminar flow regime coming off the cap. Within the trough we see turbulent clouds of dust, kicked up at the trough base as the winds slow down and enter a chaotic flow regime.</p><p>The horizontal lines in these images are due to framelet overlap and lighting conditions over the bright polar cap.</p><p>Image information: VIS instrument. Latitude 86.5, Longitude 64.5 East (295.5 West). 40 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07013" onclick="window.open(this.href); return false;" title="Voir l'image PIA07013: North Polar Cap sur le site de la NASA">Voir l'image PIA07013: North Polar Cap sur le site de la NASA.</a></div>
PIA07013: North Polar Cap
<h1>PIA07014: North Polar Cap</h1><div class="PIA07014" lang="en" style="width:130px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07014_fig1.jpg"> </a><br /><p>This image shows clouds and one of the many storm fronts common in the north polar region during spring and early summer. Note the linear nature of the clouds towards the top of the image, and the appearance of a large crater barely visible beneath the cloud cover.</p><p>Image information: VIS instrument. Latitude 86.5, Longitude 64.5 East (295.5 West). 40 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07014" onclick="window.open(this.href); return false;" title="Voir l'image PIA07014: North Polar Cap sur le site de la NASA">Voir l'image PIA07014: North Polar Cap sur le site de la NASA.</a></div>
PIA07014: North Polar Cap
<h1>PIA07015: Cloudy Pole</h1><div class="PIA07015" lang="en" style="width:129px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07015_fig1.jpg"> </a><br /><p>This image shows clouds and one of the many storm fronts common in the north polar region during spring and early summer. Note the linear nature of the clouds towards the top of the image, and the appearance of a large crater barely visible beneath the cloud cover.</p><p>Image information: VIS instrument. Latitude 75, Longitude 194 East (166 West). 40 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07015" onclick="window.open(this.href); return false;" title="Voir l'image PIA07015: Cloudy Pole sur le site de la NASA">Voir l'image PIA07015: Cloudy Pole sur le site de la NASA.</a></div>
PIA07015: Cloudy Pole
<h1>PIA07016: Cloudy Pole</h1><div class="PIA07016" lang="en" style="width:128px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07016_fig1.jpg"> </a><br /><p>This image shows clouds and one of the many storm fronts common in the north polar region during spring and early summer. Note the linear nature of the clouds towards the top of the image, and the appearance of a large crater barely visible beneath the cloud cover.</p><p>Image information: VIS instrument. Latitude 75, Longitude 194 East (166 West). 40 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07016" onclick="window.open(this.href); return false;" title="Voir l'image PIA07016: Cloudy Pole sur le site de la NASA">Voir l'image PIA07016: Cloudy Pole sur le site de la NASA.</a></div>
PIA07016: Cloudy Pole
<h1>PIA07028: Storm and Clouds</h1><div class="PIA07028" lang="en" style="width:131px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07028_fig1.jpg"> </a><br /><p>Yesterday's storm front was moving westward, today's moves eastward. Note the thick cloud cover and beautifully delineated cloud tops.</p><p>Image information: VIS instrument. Latitude 72.1, Longitude 308.3 East (51.7 West). 40 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07028" onclick="window.open(this.href); return false;" title="Voir l'image PIA07028: Storm and Clouds sur le site de la NASA">Voir l'image PIA07028: Storm and Clouds sur le site de la NASA.</a></div>
PIA07028: Storm and Clouds
<h1>PIA07029: Storm over Dunes</h1><div class="PIA07029" lang="en" style="width:129px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07029_fig1.jpg"> </a><br /><p>Today's image shows a storm front moving across an area of the north pole populated with hundreds of small dark sand dunes. The north polar region contains large regions of sand dunes, perhaps providing the some of the material raised into these clouds.</p><p>Image information: VIS instrument. Latitude 75.7, Longitude 323.7 East (36.3 West). 40 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07029" onclick="window.open(this.href); return false;" title="Voir l'image PIA07029: Storm over Dunes sur le site de la NASA">Voir l'image PIA07029: Storm over Dunes sur le site de la NASA.</a></div>
PIA07029: Storm over Dunes
<h1>PIA07037: Collapse Pits in Bernard Crater</h1><div class="PIA07037" lang="en" style="width:514px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07037_fig1.jpg"> </a><br /><p>We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in serveral ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire ediface to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form.</p><p>These pits occur in the floor of Bernard Crater. These collapse pits were likely formed by the release of volatiles from the materials deposited in the crater floor.</p><p>Image information: VIS instrument. Latitude -24, Longitude 205.5 East (154.5 West). 19 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07037" onclick="window.open(this.href); return false;" title="Voir l'image PIA07037: Collapse Pits in Bernard Crater sur le site de la NASA">Voir l'image PIA07037: Collapse Pits in Bernard Crater sur le site de la NASA.</a></div>
PIA07037: Collapse Pits in Bernard Crater
<h1>PIA07038: Sulci Collapse Pits</h1><div class="PIA07038" lang="en" style="width:522px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07038_fig1.jpg"> </a><br /><p>We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in serveral ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire ediface to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form.</p><p>These collapse pits are found in an area of "sulci" ridges east of Olympus Mons. Graben cut the ridges, and one graben hosts the collapse pits. It is likely that these collapse pits are related to volatile release from material that filled the lows at some point after graben formation.</p><p>Image information: VIS instrument. Latitude 18.6, Longitude 234.6 East (125.4 West). 19 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07038" onclick="window.open(this.href); return false;" title="Voir l'image PIA07038: Sulci Collapse Pits sur le site de la NASA">Voir l'image PIA07038: Sulci Collapse Pits sur le site de la NASA.</a></div>
PIA07038: Sulci Collapse Pits
<h1>PIA07042: Sulci Collapse Pits</h1><div class="PIA07042" lang="en" style="width:519px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07042_fig1.jpg"> </a><br /><p>We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form.</p><p>This is the Noctis Labyrinthus region of Mars. These collapse pits are forming along structural fractures that are allowing the release of volatiles from the subsurface. This is believed to be the way that chaos terrain forms on Mars. This area represents the early stage of chaos formation.</p><p>Image information: VIS instrument. Latitude -12.6, Longitude 264 East (96 West). 19 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07042" onclick="window.open(this.href); return false;" title="Voir l'image PIA07042: Sulci Collapse Pits sur le site de la NASA">Voir l'image PIA07042: Sulci Collapse Pits sur le site de la NASA.</a></div>
PIA07042: Sulci Collapse Pits
<h1>PIA07053: Tharsis Collapse Pits</h1><div class="PIA07053" lang="en" style="width:526px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07053_fig1.jpg"> </a><br /><p>We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form.</p><p>These collapse pits are found within the extensive lava flows of the Tharsis region. They are related to lava tubes, likely coming from Ascraeus Mons.</p><p>Image information: VIS instrument. Latitude 22.8, Longitude 266.8 East (93.2 West). 19 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07053" onclick="window.open(this.href); return false;" title="Voir l'image PIA07053: Tharsis Collapse Pits sur le site de la NASA">Voir l'image PIA07053: Tharsis Collapse Pits sur le site de la NASA.</a></div>
PIA07053: Tharsis Collapse Pits
<h1>PIA07054: Alba Patera Collapse Pits</h1><div class="PIA07054" lang="en" style="width:395px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07054_fig1.jpg"> </a><br /><p>We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form.</p><p>These collapse pits are found within graben surrounding Alba Patera. Alba Patera is an old volcano that has subsided after it's magma chamber was evacuated.</p><p>Image information: VIS instrument. Latitude 43.1, Longitude 259.4 East (100.6 West). 19 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07054" onclick="window.open(this.href); return false;" title="Voir l'image PIA07054: Alba Patera Collapse Pits sur le site de la NASA">Voir l'image PIA07054: Alba Patera Collapse Pits sur le site de la NASA.</a></div>
PIA07054: Alba Patera Collapse Pits
<h1>PIA07055: Lava Tube Collapse Pits</h1><div class="PIA07055" lang="en" style="width:513px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07055_fig1.jpg"> </a><br /><p>We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form.</p><p>These collapse pits are found in the southern hemisphere of Mars. They are likely lava tube collapse pits related to flows from Hadriaca Patera.</p><p>Image information: VIS instrument. Latitude -36.8, Longitude 89.6 East (270.4 West). 19 meter/pixel resolution.</p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07055" onclick="window.open(this.href); return false;" title="Voir l'image PIA07055: Lava Tube Collapse Pits sur le site de la NASA">Voir l'image PIA07055: Lava Tube Collapse Pits sur le site de la NASA.</a></div>
PIA07055: Lava Tube Collapse Pits
<h1>PIA07056: Ascraeus Mons Collapse Pits</h1><div class="PIA07056" lang="en" style="width:228px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07056_fig1.jpg"> </a><br /><p>We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form.</p><p>These collapse pits are found on the flank of Ascraeus Mons. The pits and channels are all related to lava tube formation and emptying.</p><p>Image information: IR instrument. Latitude 8, Longitude 253.9 East (106.1 West). 100 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07056" onclick="window.open(this.href); return false;" title="Voir l'image PIA07056: Ascraeus Mons Collapse Pits sur le site de la NASA">Voir l'image PIA07056: Ascraeus Mons Collapse Pits sur le site de la NASA.</a></div>
PIA07056: Ascraeus Mons Collapse Pits
<h1>PIA07068: Arsia Mons Collapse Pits in IR</h1><div class="PIA07068" lang="en" style="width:319px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07068_fig1.jpg"> </a><br /><p>We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form.</p><p>These collapse pits are found on the flank of Arsia Mons and are related to lava tube collapse.</p><p>Image information: IR instrument. Latitude -8.8, Longitude 240.4 East (119.6 West). 100 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07068" onclick="window.open(this.href); return false;" title="Voir l'image PIA07068: Arsia Mons Collapse Pits in IR sur le site de la NASA">Voir l'image PIA07068: Arsia Mons Collapse Pits in IR sur le site de la NASA.</a></div>
PIA07068: Arsia Mons Collapse Pits in IR
<h1>PIA07069: Alba Patera Collapse Pits</h1><div class="PIA07069" lang="en" style="width:320px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07069_fig1.jpg"> </a><br /><p>We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form.</p><p>This image of the Alba Patera region has both lava tube collapse pits (running generally east/west) and subsidence related collapse within structural grabens.</p><p>Image information: IR instrument. Latitude 26.9, Longitude 256.5 East (103.5 West). 100 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07069" onclick="window.open(this.href); return false;" title="Voir l'image PIA07069: Alba Patera Collapse Pits sur le site de la NASA">Voir l'image PIA07069: Alba Patera Collapse Pits sur le site de la NASA.</a></div>
PIA07069: Alba Patera Collapse Pits
<h1>PIA07070: Tractus Catena Collapse Pits</h1><div class="PIA07070" lang="en" style="width:614px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07070_fig1.jpg"> </a><br /><p>We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form.</p><p>These collapse pits are found in graben located in Tractus Catena. These features are related to subsidence after magma chamber evacuation of Alba Patera.</p><p>Image information: VIS instrument. Latitude 35.8, Longitude 241.7 East (118.3 West). 19 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07070" onclick="window.open(this.href); return false;" title="Voir l'image PIA07070: Tractus Catena Collapse Pits sur le site de la NASA">Voir l'image PIA07070: Tractus Catena Collapse Pits sur le site de la NASA.</a></div>
PIA07070: Tractus Catena Collapse Pits
<h1>PIA07071: Nighttime IR Channels</h1><div class="PIA07071" lang="en" style="width:155px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07071_fig1.jpg"> </a><br /><p>This night time IR image shows Parana Vallis. Parana Vallis is one of many channels located in the Martian highlands SE of Eos Chasma (the eastern end of Valles Marineris). Parana Vallis is likely to have been formed by fluvial activity. </p><p>NOTE: in nighttime images North is to the bottom of the image.</p><p>Image information: IR instrument. Latitude -24.6, Longitude 349.7 East (10.3 West). 100 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07071" onclick="window.open(this.href); return false;" title="Voir l'image PIA07071: Nighttime IR Channels sur le site de la NASA">Voir l'image PIA07071: Nighttime IR Channels sur le site de la NASA.</a></div>
PIA07071: Nighttime IR Channels
<h1>PIA07072: Tinto Vallis Fluvial Channel</h1><div class="PIA07072" lang="en" style="width:282px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07072" onclick="window.open(this.href); return false;" title="Voir l'image PIA07072: Tinto Vallis Fluvial Channel sur le site de la NASA">Voir l'image PIA07072: Tinto Vallis Fluvial Channel sur le site de la NASA.</a></div>
PIA07072: Tinto Vallis Fluvial Channel
<h1>PIA07080: Tyrrhena Patera Nighttime IR</h1><div class="PIA07080" lang="en" style="width:134px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07080_fig1.jpg"> </a><br /><p>Like yesterday's image, the small unnamed channel in this nighttime IR image is located near Tyrrhena Patera. This channel is located to the northwest of the volcanic complex and likely formed by fluvial action.</p><p>NOTE: in nighttime images North is to the bottom of the image.</p><p>Image information: IR instrument. Latitude -24.6, Longitude 349.7 East (10.3 West). 100 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07080" onclick="window.open(this.href); return false;" title="Voir l'image PIA07080: Tyrrhena Patera Nighttime IR sur le site de la NASA">Voir l'image PIA07080: Tyrrhena Patera Nighttime IR sur le site de la NASA.</a></div>
PIA07080: Tyrrhena Patera Nighttime IR
<h1>PIA07158: Nirgal Vallis Nighttime IR</h1><div class="PIA07158" lang="en" style="width:320px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07158_fig1.jpg"> </a><br /><p>This nighttime IR image is of Nirgal Vallis, a long fluvial channel that flows south (towards top of image) into the margin of Argyre Basin.</p><p>NOTE: in nighttime images North is to the bottom of the image.</p><p>Image information: IR instrument. Latitude -28.4, Longitude 317.6 East (42.4 West). 100 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07158" onclick="window.open(this.href); return false;" title="Voir l'image PIA07158: Nirgal Vallis Nighttime IR sur le site de la NASA">Voir l'image PIA07158: Nirgal Vallis Nighttime IR sur le site de la NASA.</a></div>
PIA07158: Nirgal Vallis Nighttime IR
<h1>PIA07159: Granicus Vallis Channels</h1><div class="PIA07159" lang="en" style="width:220px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07159_fig1.jpg"> </a><br /><p>This day time IR image shows a group of channels that originate from the Elysium volcanic field. Called Granicus Vallis, these channels are related to the volcanic activity of Elysium Mons and may be lava channels rather than fluvial. Note the lava flows at the top of the image.</p><p>Image information: IR instrument. Latitude 27.5, Longitude 132.9 East (227.1 West). 100 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07159" onclick="window.open(this.href); return false;" title="Voir l'image PIA07159: Granicus Vallis Channels sur le site de la NASA">Voir l'image PIA07159: Granicus Vallis Channels sur le site de la NASA.</a></div>
PIA07159: Granicus Vallis Channels
<h1>PIA07160: Minio Vallis Channel</h1><div class="PIA07160" lang="en" style="width:533px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07160_fig1.jpg"> </a><br /><p>This VIS image is of the southern reach of Minio Vallis, a small fluvial channel located near the larger Mangala Vallis. Both channels are in the Tharsis region, in the area west of Arsia Mons and southeast of Medusae Fossae.</p><p>Image information: VIS instrument. Latitude -8.2, Longitude 208.1 East (151.9 West). 19 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07160" onclick="window.open(this.href); return false;" title="Voir l'image PIA07160: Minio Vallis Channel sur le site de la NASA">Voir l'image PIA07160: Minio Vallis Channel sur le site de la NASA.</a></div>
PIA07160: Minio Vallis Channel
<h1>PIA07161: Channel/Crater Interaction</h1><div class="PIA07161" lang="en" style="width:530px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07161_fig1.jpg"> </a><br /><p>This small unnamed channel is just west of the large outflow region of Ares, Simud, and Tiu Valles. Note the interaction of the channel and the small crater that it has cut through. This channel is likely fluvial in origin.</p><p>Image information: VIS instrument. Latitude 9.6, Longitude 313.7 East (46.3 West). 19 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07161" onclick="window.open(this.href); return false;" title="Voir l'image PIA07161: Channel/Crater Interaction sur le site de la NASA">Voir l'image PIA07161: Channel/Crater Interaction sur le site de la NASA.</a></div>
PIA07161: Channel/Crater Interaction
<h1>PIA07162: Olympica Fossae</h1><div class="PIA07162" lang="en" style="width:537px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07162_fig1.jpg"> </a><br /><p>Today's image is of Olympica Fossae. Located between Olympus Mons and Alba Patera, this entire region is comprised of volcanic flows. All the channels seen in this image were created by volcanic activity. Many shallow channels surround the deeper main channel.</p><p>Image information: VIS instrument. Latitude 23.7, Longitude 244.2 East (115.8 West). 19 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07162" onclick="window.open(this.href); return false;" title="Voir l'image PIA07162: Olympica Fossae sur le site de la NASA">Voir l'image PIA07162: Olympica Fossae sur le site de la NASA.</a></div>
PIA07162: Olympica Fossae
<h1>PIA07163: Olympica Fossae Redux</h1><div class="PIA07163" lang="en" style="width:528px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07163_fig1.jpg"> </a><br /><p>This image is of Olympica Fossae, located further eastward than yesterday's image and closer to Alba Patera. Note the complexity of the deeper main channel and the nearby collapse channels. The deeper channel may represent an unroofed lava tube or open main lava channel. The floor texture seen in the main channel in both yesterday's and today's images may represent the surface of one of the last lava flows hosted by the channel.</p><p>Image information: VIS instrument. Latitude 24.5, Longitude 245.4 East (114.6 West). 19 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07163" onclick="window.open(this.href); return false;" title="Voir l'image PIA07163: Olympica Fossae Redux sur le site de la NASA">Voir l'image PIA07163: Olympica Fossae Redux sur le site de la NASA.</a></div>
PIA07163: Olympica Fossae Redux
<h1>PIA07164: Hebrus Vallis</h1><div class="PIA07164" lang="en" style="width:543px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07164_fig1.jpg"> </a><br /><p>This image shows a portion of Hebrus Vallis, a channel system located south of Granicus Vallis. Like Granicus Vallis, Hebrus Vallis originates close to the base of the Elysium volcanic complex. The crisscrossing of channels seen in the image is not typical for fluvial systems, indicating that this channel system was likely formed by volcanic activity.</p><p>Image information: VIS instrument. Latitude 20.8, Longitude 125.9 East (234.1 West). 19 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07164" onclick="window.open(this.href); return false;" title="Voir l'image PIA07164: Hebrus Vallis sur le site de la NASA">Voir l'image PIA07164: Hebrus Vallis sur le site de la NASA.</a></div>
PIA07164: Hebrus Vallis
<h1>PIA07165: Crater in Nighttime IR</h1><div class="PIA07165" lang="en" style="width:320px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p><a href="/figures/PIA07165_fig1.jpg"> </a><br /><p>This nighttime IR image is of a small crater. Note the bright and dark portions of it's ejecta blanket. With ballistic emplacement of ejecta, larger(heavier) material falls closer to the crater rim than smaller material. This is clearly represented in the nighttime IR, where rockier material is warmer/brighter and finer material is darker/cooler.</p><p>Image information: IR instrument. Latitude -6.5, Longitude 24 East (336 West). 100 meter/pixel resolution.</p><p>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.</p><p>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.</p><br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA07165" onclick="window.open(this.href); return false;" title="Voir l'image PIA07165: Crater in Nighttime IR sur le site de la NASA">Voir l'image PIA07165: Crater in Nighttime IR sur le site de la NASA.</a></div>
PIA07165: Crater in Nighttime IR

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