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Browse All : Images of Jet Propulsion Laboratory (JPL) and California from 2007 and January 2007

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Edge of the Olympus Mons
PIA09920
Sol (our sun)
HiRISE
Title Edge of the Olympus Mons
Original Caption Released with Image Click on image for larger version Olympus Mons, the largest volcano in the Solar System, has a mysterious halo (aureole) of material on its western and northern sides. There have been many ideas about how this feature may have formed over the years, but the hypothesis that this is a giant landslide deposit has gained favor. Many large volcanoes on the Earth collapse under their own weight, so it seems reasonable that Olympus Mons would do the same. The edge of the aureole is seen at the top (northern) part of the image (PSP_002184_2005 [ http://hirise.lpl.arizona.edu/PSP_002184_2005 ]). It is interesting that the main part of the aureole seems sunk down compared to the edge. It is possible that the ridge along the outer margin of the aureole formed as the flow turned around after pushing uphill for a ways. Imagine a giant wave of rock pushing up onto the "beach" and then receding. It might leave a deposit like this. Alternatively, glaciers push up a ramp of rock at their fronts. After they retreat, the ridge of rock is left at the furthest extent of the glacier. These are called "terminal moraines" by geologists. Many large volcanoes on the Earth collapse under their own weight, so it seems reasonable that Olympus Mons would do the same. The edge of the aureole is seen at the top (northern) part of the image. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:36 PM Degrees latitude (centered): 20.1° Degrees longitude (East): 219.7° Range to target site: 282.2 km (176.4 miles) Original image scale range: 56.5 cm/pixel (with 2 x 2 binning) so objects ~169 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.8° Phase angle: 51.7° Solar incidence angle: 54°, with the Sun about 36° above the horizon Solar longitude: 166.1°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Edge of the Olympus Mons
PIA09920
Sol (our sun)
HiRISE
Title Edge of the Olympus Mons
Original Caption Released with Image Click on image for larger version Olympus Mons, the largest volcano in the Solar System, has a mysterious halo (aureole) of material on its western and northern sides. There have been many ideas about how this feature may have formed over the years, but the hypothesis that this is a giant landslide deposit has gained favor. Many large volcanoes on the Earth collapse under their own weight, so it seems reasonable that Olympus Mons would do the same. The edge of the aureole is seen at the top (northern) part of the image (PSP_002184_2005 [ http://hirise.lpl.arizona.edu/PSP_002184_2005 ]). It is interesting that the main part of the aureole seems sunk down compared to the edge. It is possible that the ridge along the outer margin of the aureole formed as the flow turned around after pushing uphill for a ways. Imagine a giant wave of rock pushing up onto the "beach" and then receding. It might leave a deposit like this. Alternatively, glaciers push up a ramp of rock at their fronts. After they retreat, the ridge of rock is left at the furthest extent of the glacier. These are called "terminal moraines" by geologists. Many large volcanoes on the Earth collapse under their own weight, so it seems reasonable that Olympus Mons would do the same. The edge of the aureole is seen at the top (northern) part of the image. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:36 PM Degrees latitude (centered): 20.1° Degrees longitude (East): 219.7° Range to target site: 282.2 km (176.4 miles) Original image scale range: 56.5 cm/pixel (with 2 x 2 binning) so objects ~169 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.8° Phase angle: 51.7° Solar incidence angle: 54°, with the Sun about 36° above the horizon Solar longitude: 166.1°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Sample Tharsis Tholus Calder …
PIA09619
Sol (our sun)
HiRISE
Title Sample Tharsis Tholus Caldera Wall
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002169_1940 [ http://hirise.lpl.arizona.edu/PSP_002169_1940 ]) captures one of the cleaner portions of the interior wall of the caldera at the top of Tharsis Tholus. Tharsis Tholus is an intermediate sized shield volcano, much smaller than giants such as Olympus Mons, but still large by terrestrial standards. While relatively dust-free, this section of the caldera wall is still extensively covered by dust that is being sculpted into curious shapes by the wind and by gravity. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:33 PM Degrees latitude (centered): 13.6° Degrees longitude (East): 268.8° Range to target site: 274.4 km (171.5 miles) Original image scale range: 54.9 cm/pixel (with 2 x 2 binning) so objects ~165 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 13.3° Phase angle: 66.1° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 165.5°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Sample Tharsis Tholus Calder …
PIA09619
Sol (our sun)
HiRISE
Title Sample Tharsis Tholus Caldera Wall
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002169_1940 [ http://hirise.lpl.arizona.edu/PSP_002169_1940 ]) captures one of the cleaner portions of the interior wall of the caldera at the top of Tharsis Tholus. Tharsis Tholus is an intermediate sized shield volcano, much smaller than giants such as Olympus Mons, but still large by terrestrial standards. While relatively dust-free, this section of the caldera wall is still extensively covered by dust that is being sculpted into curious shapes by the wind and by gravity. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:33 PM Degrees latitude (centered): 13.6° Degrees longitude (East): 268.8° Range to target site: 274.4 km (171.5 miles) Original image scale range: 54.9 cm/pixel (with 2 x 2 binning) so objects ~165 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 13.3° Phase angle: 66.1° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 165.5°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Dusty Lava Flows on Ascreaus …
PIA09618
Sol (our sun)
HiRISE
Title Dusty Lava Flows on Ascreaus Mons
Original Caption Released with Image Click on image for larger version Ascreaus Mons is one of the giant shield volcanoes in the Tharsis region of Mars. Based on earlier lower resolution images, this location seemed to be ideal for examining how different types of lava flows interacted. The smoother ground on the northwest side of the image is probably a lava flow with a relatively smooth crust much like "pahoehoe" lava flows in Hawaii. The rugged terrain in the southwestern part of the image is indicative of a highly disrupted crust, possibly like what Hawaiians call an "aa" flow. Instead of confirming these hypotheses, HiRISE shows that the lava flow details are obscured by dust. The dust is carved into a curious network of scallops that are too small to have been seen by previous cameras. This is HiRISE image PSP_002209_1865 [ http://hirise.lpl.arizona.edu/PSP_002209_1865 ]. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:38 PM Degrees latitude (centered): 6.6° Degrees longitude (East): 26.6° Range to target site: 265.5 km (165.9 miles) Original image scale range: 26.6 cm/pixel (with 1 x 1 binning) so objects ~80 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 1.0° Phase angle: 55.3° Solar incidence angle: 54°, with the Sun about 36° above the horizon Solar longitude: 167.2°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Dusty Lava Flows on Ascreaus …
PIA09618
Sol (our sun)
HiRISE
Title Dusty Lava Flows on Ascreaus Mons
Original Caption Released with Image Click on image for larger version Ascreaus Mons is one of the giant shield volcanoes in the Tharsis region of Mars. Based on earlier lower resolution images, this location seemed to be ideal for examining how different types of lava flows interacted. The smoother ground on the northwest side of the image is probably a lava flow with a relatively smooth crust much like "pahoehoe" lava flows in Hawaii. The rugged terrain in the southwestern part of the image is indicative of a highly disrupted crust, possibly like what Hawaiians call an "aa" flow. Instead of confirming these hypotheses, HiRISE shows that the lava flow details are obscured by dust. The dust is carved into a curious network of scallops that are too small to have been seen by previous cameras. This is HiRISE image PSP_002209_1865 [ http://hirise.lpl.arizona.edu/PSP_002209_1865 ]. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:38 PM Degrees latitude (centered): 6.6° Degrees longitude (East): 26.6° Range to target site: 265.5 km (165.9 miles) Original image scale range: 26.6 cm/pixel (with 1 x 1 binning) so objects ~80 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 1.0° Phase angle: 55.3° Solar incidence angle: 54°, with the Sun about 36° above the horizon Solar longitude: 167.2°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Scalloped Topography in Pene …
PIA09611
Sol (our sun)
HiRISE
Title Scalloped Topography in Peneus Patera Crater
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002296_1215 [ http://hirise.lpl.arizona.edu/PSP_002296_1215 ]), near the southeast rim of Peneus Patera crater, is marked by depressions in the mantle with scalloped edges. Several of the depressions have apparently coalesced together. These features are most commonly found at approximately 55 degrees north and south latitude. Their presence has led to hypotheses of the removal of subsurface material, possibly interstitial ice by sublimation (evaporation). Steep scarps consistently face the south pole while more gentle slopes face in the direction of the equator. This is most likely due to differences in solar heating. A polygonal pattern of fractures, commonly associated with "scalloped terrain," can be found on the surface surrounding and within the depressions. The fractures indicate that the surface has undergone stress that may have been caused by subsidence, desiccation, or thermal contraction. Scallop formation is believed to be an ongoing process at the present time. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 4:01 PM Degrees latitude (centered): ):-58.0° Degrees longitude (East): 53.7° Range to target site: 250.7 km (156.7 miles) Original image scale range: 50.2 cm/pixel (with 2 x 2 binning) so objects ~150 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.7° Phase angle: 73.8° Solar incidence angle: 78°, with the Sun about 12° above the horizon Solar longitude: 170.9°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Scalloped Topography in Pene …
PIA09611
Sol (our sun)
HiRISE
Title Scalloped Topography in Peneus Patera Crater
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002296_1215 [ http://hirise.lpl.arizona.edu/PSP_002296_1215 ]), near the southeast rim of Peneus Patera crater, is marked by depressions in the mantle with scalloped edges. Several of the depressions have apparently coalesced together. These features are most commonly found at approximately 55 degrees north and south latitude. Their presence has led to hypotheses of the removal of subsurface material, possibly interstitial ice by sublimation (evaporation). Steep scarps consistently face the south pole while more gentle slopes face in the direction of the equator. This is most likely due to differences in solar heating. A polygonal pattern of fractures, commonly associated with "scalloped terrain," can be found on the surface surrounding and within the depressions. The fractures indicate that the surface has undergone stress that may have been caused by subsidence, desiccation, or thermal contraction. Scallop formation is believed to be an ongoing process at the present time. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 4:01 PM Degrees latitude (centered): ):-58.0° Degrees longitude (East): 53.7° Range to target site: 250.7 km (156.7 miles) Original image scale range: 50.2 cm/pixel (with 2 x 2 binning) so objects ~150 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.7° Phase angle: 73.8° Solar incidence angle: 78°, with the Sun about 12° above the horizon Solar longitude: 170.9°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Proposed MSL Site in Margari …
PIA09641
Sol (our sun)
HiRISE
Title Proposed MSL Site in Margaritifer Basin
Original Caption Released with Image Click on image for larger version HiRISE image (PSP_002193_1670 [ http://hirise.lpl.arizona.edu/PSP_002193_1670 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Margaritifer Basin. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -12.9° Degrees longitude (East): 337.9° Range to target site: 263.9 km (164.9 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.5° Phase angle: 58.0° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 166.5 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Proposed MSL Site in Margari …
PIA09641
Sol (our sun)
HiRISE
Title Proposed MSL Site in Margaritifer Basin
Original Caption Released with Image Click on image for larger version HiRISE image (PSP_002193_1670 [ http://hirise.lpl.arizona.edu/PSP_002193_1670 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Margaritifer Basin. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -12.9° Degrees longitude (East): 337.9° Range to target site: 263.9 km (164.9 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.5° Phase angle: 58.0° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 166.5 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
White Rock Landform in Polla …
PIA09640
Sol (our sun)
HiRISE
Title White Rock Landform in Pollack Crater
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002244_1720 [ http://hirise.lpl.arizona.edu/PSP_002244_1720 ]) shows a portion of a relatively bright landform named "White Rock" on the floor of Pollack crater in the Sinus Sabaeus region of Mars. Data from the Mars Global Surveyor Thermal Emission Spectrometer (TES) [ http://tes.asu.edu/ ] indicates that this landform is not anomalously bright, relative to other bright Martian regions. Further, the apparent brightness seen here is due to contrast with other materials on the crater floor. Dunes and ripples are visible in the dark material between the bright ridges. Their orientations appear to be influenced by wind directionally channeled by the ridges. Material appears to have been shed from the white landform and deposited on the darker bedforms indicating that the light-toned outcrops break down into fine materials. Its high albedo and location in a topographic basin have led to suggestions that White Rock is an erosional remnant of an ancient lacustrine evaporate deposit. Other interpretations include an eroded accumulation of compacted or weakly cemented aeolian sediment. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -8.0° Degrees longitude (East): 25.0° Range to target site: 263.1 km (164.4 miles) Original image scale range: 26.3 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 1.3° Phase angle: 55.7° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 168.7°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
White Rock Landform in Polla …
PIA09640
Sol (our sun)
HiRISE
Title White Rock Landform in Pollack Crater
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002244_1720 [ http://hirise.lpl.arizona.edu/PSP_002244_1720 ]) shows a portion of a relatively bright landform named "White Rock" on the floor of Pollack crater in the Sinus Sabaeus region of Mars. Data from the Mars Global Surveyor Thermal Emission Spectrometer (TES) [ http://tes.asu.edu/ ] indicates that this landform is not anomalously bright, relative to other bright Martian regions. Further, the apparent brightness seen here is due to contrast with other materials on the crater floor. Dunes and ripples are visible in the dark material between the bright ridges. Their orientations appear to be influenced by wind directionally channeled by the ridges. Material appears to have been shed from the white landform and deposited on the darker bedforms indicating that the light-toned outcrops break down into fine materials. Its high albedo and location in a topographic basin have led to suggestions that White Rock is an erosional remnant of an ancient lacustrine evaporate deposit. Other interpretations include an eroded accumulation of compacted or weakly cemented aeolian sediment. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -8.0° Degrees longitude (East): 25.0° Range to target site: 263.1 km (164.4 miles) Original image scale range: 26.3 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 1.3° Phase angle: 55.7° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 168.7°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Layered Mesa in Coprates Cha …
PIA09651
Sol (our sun)
HiRISE
Title Layered Mesa in Coprates Chasma
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002036_1655 [ http://hirise.lpl.arizona.edu/PSP_002036_1655 ]) shows a mesa within Coprates Chasma, a large trough in the Valles Marineris canyon system. Multiple layers, some only a few meters in thickness, are visible on the slopes descending from the edges of the flat-topped mesa. The layered rocks could have formed from volcanic, lacustrine, or aeolian sediments that were deposited in portions of the Valles Marineris trough. Variations in the brightness of the layers may represent compositional differences. In particular, the slopes contain a prominent layer of dark material that is seemingly composed of materials more resistant to erosion than the overlying brighter layers. Dunes and ripples can also visible on the top of the mesa. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:40 PM Degrees latitude (centered): -14.4° Degrees longitude (East): 304.2° Range to target site: 258.8 km (161.7 miles) Original image scale range: from 25.9 cm/pixel (with 1 x 1 binning) to 51.8 cm/pixel (with 2 x 2 binning) Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.3° Phase angle: 61.4° Solar incidence angle: 59°, with the Sun about 31° above the horizon Solar longitude: 160.0°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Layered Mesa in Coprates Cha …
PIA09651
Sol (our sun)
HiRISE
Title Layered Mesa in Coprates Chasma
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002036_1655 [ http://hirise.lpl.arizona.edu/PSP_002036_1655 ]) shows a mesa within Coprates Chasma, a large trough in the Valles Marineris canyon system. Multiple layers, some only a few meters in thickness, are visible on the slopes descending from the edges of the flat-topped mesa. The layered rocks could have formed from volcanic, lacustrine, or aeolian sediments that were deposited in portions of the Valles Marineris trough. Variations in the brightness of the layers may represent compositional differences. In particular, the slopes contain a prominent layer of dark material that is seemingly composed of materials more resistant to erosion than the overlying brighter layers. Dunes and ripples can also visible on the top of the mesa. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:40 PM Degrees latitude (centered): -14.4° Degrees longitude (East): 304.2° Range to target site: 258.8 km (161.7 miles) Original image scale range: from 25.9 cm/pixel (with 1 x 1 binning) to 51.8 cm/pixel (with 2 x 2 binning) Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.3° Phase angle: 61.4° Solar incidence angle: 59°, with the Sun about 31° above the horizon Solar longitude: 160.0°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Mantles and Flows in Moreux …
PIA09650
Sol (our sun)
HiRISE
Title Mantles and Flows in Moreux Crater
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002098_2220 [ http://hirise.lpl.arizona.edu/PSP_002098_2220 ]) shows part of the central uplift of Moreux Crater, at about 42 degrees north of the equator. In several parts of the image, the underlying topography appears mantled by a later deposit. This appears mostly in topographic lows and has lineations which suggest that it has flowed downslope, suggesting that this mantle may have been ice-rich. In one point near the center of the image, some of this material appears detached in a local topographic minimum, however, this patch is still lineated. North of the image center there are several patches of dark material which appear smooth at low resolution (zoomed out). A closer look reveals that these areas are broken into polygonal patterns, which may be due to stresses created by temperature variations. Such polygons often indicate the presence of ground ice near the surface. Sites like this provide a wealth of information about processes affecting the the surface of Mars. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:29 PM Degrees latitude (centered): 41.7° Degrees longitude (East): 44.4° Range to target site: 297.7 km (186.0 miles) Original image scale range: from 29.8 cm/pixel (with 1 x 1 binning) to 59.6 cm/pixel (with 2 x 2 binning) Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.8° Phase angle: 57.0° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 162.5 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Mantles and Flows in Moreux …
PIA09650
Sol (our sun)
HiRISE
Title Mantles and Flows in Moreux Crater
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002098_2220 [ http://hirise.lpl.arizona.edu/PSP_002098_2220 ]) shows part of the central uplift of Moreux Crater, at about 42 degrees north of the equator. In several parts of the image, the underlying topography appears mantled by a later deposit. This appears mostly in topographic lows and has lineations which suggest that it has flowed downslope, suggesting that this mantle may have been ice-rich. In one point near the center of the image, some of this material appears detached in a local topographic minimum, however, this patch is still lineated. North of the image center there are several patches of dark material which appear smooth at low resolution (zoomed out). A closer look reveals that these areas are broken into polygonal patterns, which may be due to stresses created by temperature variations. Such polygons often indicate the presence of ground ice near the surface. Sites like this provide a wealth of information about processes affecting the the surface of Mars. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:29 PM Degrees latitude (centered): 41.7° Degrees longitude (East): 44.4° Range to target site: 297.7 km (186.0 miles) Original image scale range: from 29.8 cm/pixel (with 1 x 1 binning) to 59.6 cm/pixel (with 2 x 2 binning) Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.8° Phase angle: 57.0° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 162.5 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Mound of South Polar Layered …
PIA09609
Sol (our sun)
HiRISE
Title Mound of South Polar Layered Deposits
Original Caption Released with Image Click on image for larger version The south polar layered deposits are a stack of layered ice up to 3000 meters (9800 feet) thick which is similar to terrestrial ice sheets. In places, this stack extends up to 1100 kilometers (680 miles) from the pole and many of the impact craters surrounding this ice-sheet appear to be filled with mounds of similar icy material and also sand dunes. This image shows the material within one of these near-polar craters. The crater is about 44 kilometers (27 miles) across and contains a mound of material about 23 kilometers (14 miles) across and 300 meters (1000 feet) thick on its northern (south facing) wall. The dark material at the top (north) of the image shows the northern wall of the crater, the bright material that begins near the image top and extends toward the bottom is the surface of the mound. This surface is covered with sand dunes that appear bright as they are still covered by seasonal carbon dioxide frost. Smaller dunes and ripples can be seen on the surfaces of the larger linear dunes. In the low lying areas between dunes, one can see a network of cracks that are reminiscent of the surface of the polar layered deposits, indicating that this mound is probably mostly ice with a thinner and incomplete covering of dunes. The dark spots in the frost cover are characteristic of how this terrain defrosts, and are commonly observed in these locations during this season. This HiRISE image is PSP_002345_1095 [ http://hirise.lpl.arizona.edu/PSP_002345_1095 ]. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 10:00 PM Degrees latitude (centered): -70.2° Degrees longitude (East): 159.0° Range to target site: 248.4 km (155.3 miles) Original image scale range: 49.7 cm/pixel (with 2 x 2 binning) so objects ~149 cm across are resolved Map-projected scale: 50 cm/pixel Map-projection: POLAR STEREOGRAPHIC Emission angle: 0.4° Phase angle: 83.9° Solar incidence angle: 84°, with the Sun about 6° above the horizon Solar longitude: 173.0°, N NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Mound of South Polar Layered …
PIA09609
Sol (our sun)
HiRISE
Title Mound of South Polar Layered Deposits
Original Caption Released with Image Click on image for larger version The south polar layered deposits are a stack of layered ice up to 3000 meters (9800 feet) thick which is similar to terrestrial ice sheets. In places, this stack extends up to 1100 kilometers (680 miles) from the pole and many of the impact craters surrounding this ice-sheet appear to be filled with mounds of similar icy material and also sand dunes. This image shows the material within one of these near-polar craters. The crater is about 44 kilometers (27 miles) across and contains a mound of material about 23 kilometers (14 miles) across and 300 meters (1000 feet) thick on its northern (south facing) wall. The dark material at the top (north) of the image shows the northern wall of the crater, the bright material that begins near the image top and extends toward the bottom is the surface of the mound. This surface is covered with sand dunes that appear bright as they are still covered by seasonal carbon dioxide frost. Smaller dunes and ripples can be seen on the surfaces of the larger linear dunes. In the low lying areas between dunes, one can see a network of cracks that are reminiscent of the surface of the polar layered deposits, indicating that this mound is probably mostly ice with a thinner and incomplete covering of dunes. The dark spots in the frost cover are characteristic of how this terrain defrosts, and are commonly observed in these locations during this season. This HiRISE image is PSP_002345_1095 [ http://hirise.lpl.arizona.edu/PSP_002345_1095 ]. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 10:00 PM Degrees latitude (centered): -70.2° Degrees longitude (East): 159.0° Range to target site: 248.4 km (155.3 miles) Original image scale range: 49.7 cm/pixel (with 2 x 2 binning) so objects ~149 cm across are resolved Map-projected scale: 50 cm/pixel Map-projection: POLAR STEREOGRAPHIC Emission angle: 0.4° Phase angle: 83.9° Solar incidence angle: 84°, with the Sun about 6° above the horizon Solar longitude: 173.0°, N NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Newly-Formed Slope Streaks
PIA09608
Sol (our sun)
HiRISE
Title Newly-Formed Slope Streaks
Original Caption Released with Image Click on image for larger version HiRISE image (PSP_002396_1900 [ http://hirise.lpl.arizona.edu/PSP_002396_1900 ]) features three newly-formed slope streaks. These are features which occur on crater walls, hills, and other slopes on Mars. They always begin at a point source and widen downslope, sometimes weaving around existing topographic features (such as dunes or craters), but other times they flow over them. Many slope streaks do not show topographic relief in available images, and there are no observable deposits of displaced materials surrounding their borders. In general, slope streaks tend to be many hundreds of meters long and less than 200 meters wide. They are observed in varying shades of darkness, where lighter-toned streaks appear to be older than darker ones. The formation mechanism responsible for slope streaks is still under debate, theories range from dry dust avalanches (most widely-accepted theory) to briney water seepage. Slope streak formation is among the few surface processes known to be currently active on Mars, making slope streaks some of the youngest features on Mars. A comparison of this HiRISE image with the Mars Orbiter Camera (MOC) image E04-01817 [ http://www.msss.com/moc_gallery/e01_e06/images/E04/E0401817.html ] shows that three new slope streaks have formed during the six years separating these images (2001-2007). The shortest time frame in which new slope streaks have been observed to form is six months (MOC images SP2-37303 and E02-02379), though it is not yet known how long it actually takes for a slope streak to form. MOC image E04-01817 courtesy of NASA/JPL/Malin Space Science Systems. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:40 PM Degrees latitude (centered): 10.1° Degrees longitude (East): 193.2° Range to target site: 278.7 km (174.2 miles) Original image scale range: 55.8 cm/pixel (with 2 x 2 binning) so objects ~167 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 3.7° Phase angle: 51.7° Solar incidence angle: 55°, with the Sun about 35° above the horizon Solar longitude: 175.2°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Newly-Formed Slope Streaks
PIA09608
Sol (our sun)
HiRISE
Title Newly-Formed Slope Streaks
Original Caption Released with Image Click on image for larger version HiRISE image (PSP_002396_1900 [ http://hirise.lpl.arizona.edu/PSP_002396_1900 ]) features three newly-formed slope streaks. These are features which occur on crater walls, hills, and other slopes on Mars. They always begin at a point source and widen downslope, sometimes weaving around existing topographic features (such as dunes or craters), but other times they flow over them. Many slope streaks do not show topographic relief in available images, and there are no observable deposits of displaced materials surrounding their borders. In general, slope streaks tend to be many hundreds of meters long and less than 200 meters wide. They are observed in varying shades of darkness, where lighter-toned streaks appear to be older than darker ones. The formation mechanism responsible for slope streaks is still under debate, theories range from dry dust avalanches (most widely-accepted theory) to briney water seepage. Slope streak formation is among the few surface processes known to be currently active on Mars, making slope streaks some of the youngest features on Mars. A comparison of this HiRISE image with the Mars Orbiter Camera (MOC) image E04-01817 [ http://www.msss.com/moc_gallery/e01_e06/images/E04/E0401817.html ] shows that three new slope streaks have formed during the six years separating these images (2001-2007). The shortest time frame in which new slope streaks have been observed to form is six months (MOC images SP2-37303 and E02-02379), though it is not yet known how long it actually takes for a slope streak to form. MOC image E04-01817 courtesy of NASA/JPL/Malin Space Science Systems. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:40 PM Degrees latitude (centered): 10.1° Degrees longitude (East): 193.2° Range to target site: 278.7 km (174.2 miles) Original image scale range: 55.8 cm/pixel (with 2 x 2 binning) so objects ~167 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 3.7° Phase angle: 51.7° Solar incidence angle: 55°, with the Sun about 35° above the horizon Solar longitude: 175.2°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
A Field of Secondary Craters
PIA09584
Sol (our sun)
HiRISE
Title A Field of Secondary Craters
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002281_2115 [ http://hirise.lpl.arizona.edu/PSP_002281_2115 ]) shows a secondary crater field. Secondary craters form when material ejected from a larger impact event impacts the Martian surface. One impact event, depending on the size of the impactor, can form hundreds of millions of secondary craters at essentially the same time. Primary craters (those created directly from an impactor from space) can be the same size as secondary craters, which makes dating surfaces based on the number of accumulated craters difficult to near-impossible. Secondary craters are distinguished from primaries based on their morphologies. They are sometimes irregularly shaped, as seen in this image, because they form at relatively low velocities. The velocity of the impactor determines a crater's size, shape, and depth, with lower energy impacts forming shallow, less-developed craters and higher energy impacts forming deeper, more regular craters. Secondary craters often occur in clusters, as seen here, as a piece of ejecta breaks up before hitting the surface. Primary craters form at random locations globally. Secondary clusters are more likely to be found in groups because of their formation mechanism. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:34 PM Degrees latitude (centered): 31.1 ° Degrees longitude (East): 89.7 ° Range to target site: 291.1 km (181.9 miles) Original image scale range: 29.1 cm/pixel (with 1 x 1 binning) so objects ~87 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.2 ° Phase angle: 57.1 ° Solar incidence angle: 57 °, with the Sun about 33 ° above the horizon Solar longitude: 170.2 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
A Field of Secondary Craters
PIA09584
Sol (our sun)
HiRISE
Title A Field of Secondary Craters
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002281_2115 [ http://hirise.lpl.arizona.edu/PSP_002281_2115 ]) shows a secondary crater field. Secondary craters form when material ejected from a larger impact event impacts the Martian surface. One impact event, depending on the size of the impactor, can form hundreds of millions of secondary craters at essentially the same time. Primary craters (those created directly from an impactor from space) can be the same size as secondary craters, which makes dating surfaces based on the number of accumulated craters difficult to near-impossible. Secondary craters are distinguished from primaries based on their morphologies. They are sometimes irregularly shaped, as seen in this image, because they form at relatively low velocities. The velocity of the impactor determines a crater's size, shape, and depth, with lower energy impacts forming shallow, less-developed craters and higher energy impacts forming deeper, more regular craters. Secondary craters often occur in clusters, as seen here, as a piece of ejecta breaks up before hitting the surface. Primary craters form at random locations globally. Secondary clusters are more likely to be found in groups because of their formation mechanism. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:34 PM Degrees latitude (centered): 31.1 ° Degrees longitude (East): 89.7 ° Range to target site: 291.1 km (181.9 miles) Original image scale range: 29.1 cm/pixel (with 1 x 1 binning) so objects ~87 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.2 ° Phase angle: 57.1 ° Solar incidence angle: 57 °, with the Sun about 33 ° above the horizon Solar longitude: 170.2 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Sinuous Ridges Near Aeolis M …
PIA09580
Sol (our sun)
HiRISE
Title Sinuous Ridges Near Aeolis Mensae
Original Caption Released with Image ) covers part of a fan-shaped deposit of material in the Aeolis Mensae region of Mars. The dominant surface texture is a series of parallel linear ridges. In addition, there are several sinuous, flat-topped ridges. The sinuous ridges do not follow the trend of the linear ridges, and various intersecting relations are observed. The southernmost sinuous features in this image are partially buried by linear ridge material, while in the northern part of the image they appear to stand above it. This could indicate that the linear unit has been more eroded in the north than the south, but may also be due to a more complex geological history in which different sinuous ridges formed at different times. In the northeast part of the image one sinuous ridge appears superposed on another, supporting this hypothesis. The linear ridges may be yardangs. Yardangs form when material is eroded by wind, producing elongated features aligned with the prevailing wind. Many of the ridges expose layers and appear to have broken into boulders. Layering indicates multiple episodes or pulses of deposition, while the occurrence of boulders shows that the material has been consolidated to some degree. The sinuous ridges could be former stream channels outcropping in inverted relief, where a formerly low-lying feature is now relatively high-standing. This occurs when the stream channel is more resistant to erosion that the surroundings, either due to cementation by water or to the presence of large rocks which are not easily eroded. In this case, the sinuous ridges contain few boulders resolvable by HiRISE, generally appearing uniform and smooth. They also contain fractures which in places cut across the entire ridge. Both of these observations are consistent with cementation of former channel floors. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:51 PM Degrees latitude (centered): -6.2 ° Degrees longitude (East): 151.4 ° Range to target site: 302.7 km (189.2 miles) Original image scale range: from 30.3 cm/pixel (with 1 x 1 binning) to 60.6 cm/pixel (with 2 x 2 binning) Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 29.3 ° Phase angle: 31.2 ° Solar incidence angle: 59 °, with the Sun about 31 ° above the horizon Solar longitude: 170.1 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo., Click on image for larger version This HiRISE image (PSP_002279_1735 [ http://hirise.lpl.arizona.edu/PSP_002279_1735 ]
Sinuous Ridges Near Aeolis M …
PIA09580
Sol (our sun)
HiRISE
Title Sinuous Ridges Near Aeolis Mensae
Original Caption Released with Image ) covers part of a fan-shaped deposit of material in the Aeolis Mensae region of Mars. The dominant surface texture is a series of parallel linear ridges. In addition, there are several sinuous, flat-topped ridges. The sinuous ridges do not follow the trend of the linear ridges, and various intersecting relations are observed. The southernmost sinuous features in this image are partially buried by linear ridge material, while in the northern part of the image they appear to stand above it. This could indicate that the linear unit has been more eroded in the north than the south, but may also be due to a more complex geological history in which different sinuous ridges formed at different times. In the northeast part of the image one sinuous ridge appears superposed on another, supporting this hypothesis. The linear ridges may be yardangs. Yardangs form when material is eroded by wind, producing elongated features aligned with the prevailing wind. Many of the ridges expose layers and appear to have broken into boulders. Layering indicates multiple episodes or pulses of deposition, while the occurrence of boulders shows that the material has been consolidated to some degree. The sinuous ridges could be former stream channels outcropping in inverted relief, where a formerly low-lying feature is now relatively high-standing. This occurs when the stream channel is more resistant to erosion that the surroundings, either due to cementation by water or to the presence of large rocks which are not easily eroded. In this case, the sinuous ridges contain few boulders resolvable by HiRISE, generally appearing uniform and smooth. They also contain fractures which in places cut across the entire ridge. Both of these observations are consistent with cementation of former channel floors. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:51 PM Degrees latitude (centered): -6.2 ° Degrees longitude (East): 151.4 ° Range to target site: 302.7 km (189.2 miles) Original image scale range: from 30.3 cm/pixel (with 1 x 1 binning) to 60.6 cm/pixel (with 2 x 2 binning) Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 29.3 ° Phase angle: 31.2 ° Solar incidence angle: 59 °, with the Sun about 31 ° above the horizon Solar longitude: 170.1 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo., Click on image for larger version This HiRISE image (PSP_002279_1735 [ http://hirise.lpl.arizona.edu/PSP_002279_1735 ]
Gully Grab Bag in Crater Wal …
PIA09595
Sol (our sun)
HiRISE
Title Gully Grab Bag in Crater Wall in the Terra Sirenum Region
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002291_1335 [ http://hirise.lpl.arizona.edu/PSP_002291_1335 ]) shows the complex, gullied western wall of a kilometer-deep impact crater in the Terra Sirenum region. This is an interesting crater because it appears to be mantled by the fluidized ejecta blanket of a slightly smaller crater just to the west. A diverse set of gullies originate at multiple elevations along the crater wall. Prominent gullies have incised through the overlying ejecta into the upper walls to reveal numerous resistant dark layers. The floors of these gullies display a host of interesting features, including braided middle reaches, cut banks, channel bars, and stream terracing. These are all features suggestive of water flow. Miniature gully systems, less than a kilometer long, start much further downslope than the larger gullies yet display the usual gully attributes, including theater-headed alcove source regions, incised middle reaches, and overlapping alluvial fans at their lower reaches. Detailed studies of these and other gully systems should help to elucidate the gully formation mechanisms. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -46.2 ° Degrees longitude (East): 184.5 ° Range to target site: 272.0 km (170.0 miles) Original image scale range: 54.4 cm/pixel (with 2 x 2 binning) so objects ~163 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 23.6 ° Phase angle: 90.1 ° Solar incidence angle: 70 °, with the Sun about 20 ° above the horizon Solar longitude: 170.7 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Gully Grab Bag in Crater Wal …
PIA09595
Sol (our sun)
HiRISE
Title Gully Grab Bag in Crater Wall in the Terra Sirenum Region
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002291_1335 [ http://hirise.lpl.arizona.edu/PSP_002291_1335 ]) shows the complex, gullied western wall of a kilometer-deep impact crater in the Terra Sirenum region. This is an interesting crater because it appears to be mantled by the fluidized ejecta blanket of a slightly smaller crater just to the west. A diverse set of gullies originate at multiple elevations along the crater wall. Prominent gullies have incised through the overlying ejecta into the upper walls to reveal numerous resistant dark layers. The floors of these gullies display a host of interesting features, including braided middle reaches, cut banks, channel bars, and stream terracing. These are all features suggestive of water flow. Miniature gully systems, less than a kilometer long, start much further downslope than the larger gullies yet display the usual gully attributes, including theater-headed alcove source regions, incised middle reaches, and overlapping alluvial fans at their lower reaches. Detailed studies of these and other gully systems should help to elucidate the gully formation mechanisms. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -46.2 ° Degrees longitude (East): 184.5 ° Range to target site: 272.0 km (170.0 miles) Original image scale range: 54.4 cm/pixel (with 2 x 2 binning) so objects ~163 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 23.6 ° Phase angle: 90.1 ° Solar incidence angle: 70 °, with the Sun about 20 ° above the horizon Solar longitude: 170.7 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Portion of Isidis Planitia N …
PIA09598
Sol (our sun)
HiRISE
Title Portion of Isidis Planitia Near the Beagle 2 Landing Ellipse
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002136_1920 [ http://hirise.lpl.arizona.edu/PSP_002136_1920 ]) shows a portion of cratered plains in Isidis Planitia, near or perhaps within the landing ellipse for Beagle 2. There are some interesting bright-pixel artifacts that are due to cosmic-ray events detected by the HiRISE camera, similar to those seen when imaging black sky during cruise to Mars. The image shows two portions of the Isidis Planitia image with bright noise at top, and 6 examples of bright noise seen in the cruise images, all are from the original, unprocessed images. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:36 PM Degrees latitude (centered): 11.8 ° Degrees longitude (East): 90.9 ° Range to target site: 277.5 km (173.5 miles) Original image scale range: 27.8 cm/pixel (with 1 x 1 binning) so objects ~83 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 1.0 ° Phase angle: 54.7 ° Solar incidence angle: 54 °, with the Sun about 36 ° above the horizon Solar longitude: 164.1 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Portion of Isidis Planitia N …
PIA09598
Sol (our sun)
HiRISE
Title Portion of Isidis Planitia Near the Beagle 2 Landing Ellipse
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002136_1920 [ http://hirise.lpl.arizona.edu/PSP_002136_1920 ]) shows a portion of cratered plains in Isidis Planitia, near or perhaps within the landing ellipse for Beagle 2. There are some interesting bright-pixel artifacts that are due to cosmic-ray events detected by the HiRISE camera, similar to those seen when imaging black sky during cruise to Mars. The image shows two portions of the Isidis Planitia image with bright noise at top, and 6 examples of bright noise seen in the cruise images, all are from the original, unprocessed images. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:36 PM Degrees latitude (centered): 11.8 ° Degrees longitude (East): 90.9 ° Range to target site: 277.5 km (173.5 miles) Original image scale range: 27.8 cm/pixel (with 1 x 1 binning) so objects ~83 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 1.0 ° Phase angle: 54.7 ° Solar incidence angle: 54 °, with the Sun about 36 ° above the horizon Solar longitude: 164.1 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Mantled Surface of Ascraeus …
PIA09596
Sol (our sun)
HiRISE
Title Mantled Surface of Ascraeus Mons
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002196_1920 [ http://hirise.lpl.arizona.edu/PSP_002196_1920 ]) shows a part of the western flank of Ascraeus Mons. Ascraeus Mons is one of the giant volcanoes of the Tharsis volcanic region of Mars. It is a shield volcano, so named because of the gently-sloped round shape. Terrestrial examples, like Mauna Loa and Kilauea on Hawaii, are formed mostly by repeated eruptions of fluid (basaltic) lava. Martian volcanoes can attain much larger sizes partiallly because Mars lacks plate tectonics, allowing eruptions to persist at the same site for a long time. In this HiRISE image, the surface is covered by a mantle of dusty material which obscured the underlying surface. This has been sculpted into regular textures, probably by aeolian (wind) erosion. It appears that there are multiple layers, as the southeast portion of the image shows textured knobs standing above a similarly patterned surface. The origin of the dusty mantle is unclear. It could be wind-blown dust, but it is also possible that some of it is volcanic ash erupted from Ascraeus Mons. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:36 PM Degrees latitude (centered): 11.7 ° Degrees longitude (East): 252.5 ° Range to target site: 271.4 km (169.6 miles) Original image scale range: 54.3 cm/pixel (with 2 x 2 binning) so objects ~163 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.1 ° Phase angle: 58.7 ° Solar incidence angle: 54 °, with the Sun about 36 ° above the horizon Solar longitude: 166.6 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Mantled Surface of Ascraeus …
PIA09596
Sol (our sun)
HiRISE
Title Mantled Surface of Ascraeus Mons
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002196_1920 [ http://hirise.lpl.arizona.edu/PSP_002196_1920 ]) shows a part of the western flank of Ascraeus Mons. Ascraeus Mons is one of the giant volcanoes of the Tharsis volcanic region of Mars. It is a shield volcano, so named because of the gently-sloped round shape. Terrestrial examples, like Mauna Loa and Kilauea on Hawaii, are formed mostly by repeated eruptions of fluid (basaltic) lava. Martian volcanoes can attain much larger sizes partiallly because Mars lacks plate tectonics, allowing eruptions to persist at the same site for a long time. In this HiRISE image, the surface is covered by a mantle of dusty material which obscured the underlying surface. This has been sculpted into regular textures, probably by aeolian (wind) erosion. It appears that there are multiple layers, as the southeast portion of the image shows textured knobs standing above a similarly patterned surface. The origin of the dusty mantle is unclear. It could be wind-blown dust, but it is also possible that some of it is volcanic ash erupted from Ascraeus Mons. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:36 PM Degrees latitude (centered): 11.7 ° Degrees longitude (East): 252.5 ° Range to target site: 271.4 km (169.6 miles) Original image scale range: 54.3 cm/pixel (with 2 x 2 binning) so objects ~163 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.1 ° Phase angle: 58.7 ° Solar incidence angle: 54 °, with the Sun about 36 ° above the horizon Solar longitude: 166.6 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Tongue-Shaped Flow Feature i …
PIA09594
Sol (our sun)
HiRISE
Title Tongue-Shaped Flow Feature in Hellas Planitia
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002320_1415 [ http://hirise.lpl.arizona.edu/PSP_002320_1415 ]) captures a tongue-shaped lobate flow feature along a interior crater wall located in eastern Hellas Planitia. The flow feature is approximately 5 kilometers long and 1 kilometer wide with a partial double inner ridge and raised outer margin. The flow feature's surface is generally devoid of impact craters and parts of its outer margin have deflected around obstacles. Similar flow features, though not as distinctively tongue-shaped as this one, are found in many other craters throughout the southern mid-latitudes of Mars. Recent studies of these flow features have determined a latitudinal dependence to which side of the crater interior these features are formed upon. For this particular flow feature, it has formed on the pole-facing slope. This polar or equatorial-facing preference has implications for the amount of solar isolation these slopes are receiving, which may be a result of recent climate change due to shifts from low to high obliquity. Although these Martian flow features may have Earth analogs such as rock glaciers, uncertainty remains as to what types of fluvial, glacial and mass-wasting processes are involved in their formation. This particular flow feature was imaged previously by the Mars Orbiter Camera (MOC) onboard NASA's Mars Global Surveyor spacecraft. Observation Geometry Acquisition date:1 January 2007 Local Mars time: 3:46 PM Degrees latitude (centered): -38.1 ° Degrees longitude (East): 113.2 ° Range to target site: 255.2 km (159.5 miles) Original image scale range: 25.5 cm/pixel (with 1 x 1 binning) so objects ~77 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 9.4 ° Phase angle: 75.0 ° Solar incidence angle: 67 °, with the Sun about 23 ° above the horizon Solar longitude: 171.9 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Tongue-Shaped Flow Feature i …
PIA09594
Sol (our sun)
HiRISE
Title Tongue-Shaped Flow Feature in Hellas Planitia
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002320_1415 [ http://hirise.lpl.arizona.edu/PSP_002320_1415 ]) captures a tongue-shaped lobate flow feature along a interior crater wall located in eastern Hellas Planitia. The flow feature is approximately 5 kilometers long and 1 kilometer wide with a partial double inner ridge and raised outer margin. The flow feature's surface is generally devoid of impact craters and parts of its outer margin have deflected around obstacles. Similar flow features, though not as distinctively tongue-shaped as this one, are found in many other craters throughout the southern mid-latitudes of Mars. Recent studies of these flow features have determined a latitudinal dependence to which side of the crater interior these features are formed upon. For this particular flow feature, it has formed on the pole-facing slope. This polar or equatorial-facing preference has implications for the amount of solar isolation these slopes are receiving, which may be a result of recent climate change due to shifts from low to high obliquity. Although these Martian flow features may have Earth analogs such as rock glaciers, uncertainty remains as to what types of fluvial, glacial and mass-wasting processes are involved in their formation. This particular flow feature was imaged previously by the Mars Orbiter Camera (MOC) onboard NASA's Mars Global Surveyor spacecraft. Observation Geometry Acquisition date:1 January 2007 Local Mars time: 3:46 PM Degrees latitude (centered): -38.1 ° Degrees longitude (East): 113.2 ° Range to target site: 255.2 km (159.5 miles) Original image scale range: 25.5 cm/pixel (with 1 x 1 binning) so objects ~77 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 9.4 ° Phase angle: 75.0 ° Solar incidence angle: 67 °, with the Sun about 23 ° above the horizon Solar longitude: 171.9 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Portion of Beagle 2 Landing …
PIA09592
Sol (our sun)
HiRISE
Title Portion of Beagle 2 Landing Ellipse in Isidis Planitia
Original Caption Released with Image This image (PSP_002347_1915 [ http://hirise.lpl.arizona.edu/PSP_002347_1915 ]) was targeted to a dark spot seen in a MOC image that was suggested to be the Beagle 2 landing site (see Beagle 2 Landing Site Located [ http://www.planetary.org/blog/article/00000321/ ] for more information). The dark spot corresponds to an impact crater, shown here in color. The European Beagle 2 lander was carried by the Mars Express orbiting spacecraft and released into the Martian atmosphere in December 2003, but Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:40 PM Degrees latitude (centered): 11.7 ° Degrees longitude (East): 90.7 ° Range to target site: 278.3 km (173.9 miles) Original image scale range: 27.8 cm/pixel (with 1 x 1 binning) so objects ~84 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 3.3 ° Phase angle: 51.9 ° Solar incidence angle: 55 °, with the Sun about 35 ° above the horizon Solar longitude: 173.1 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Northern Meridiani Etched Te …
PIA09593
Sol (our sun)
HiRISE
Title Northern Meridiani Etched Terrain and Hematite Plains Contact
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002324_1815 [ http://hirise.lpl.arizona.edu/PSP_002324_1815 ]) shows the contact between the Hematite Bearing Plains and Etched Terrain in Northern Meridiani Planum. The Hematite Bearing Plains (exposed at the bottom left of this image) are dark, smooth and full of dune fields. This unit is laterally extensive and the same unit that the Mars Exploration Rover Opportunity is sitting on about 400 km to the southwest. Based on observations by Opportunity, this unit is interpreted to be a thin aeolian (wind-blown) mantle of basaltic sand and hematite concretions sitting on the Etched Terrain. The Etched Terrain in this image is split into two units. The darker unit at the top of the image is filling in a ~120 km NW-SE trending valley, while the brighter Etched Terrain in the middle of the image is stratigraphically and topographically higher than the lower Etched Terrain in the valley. This upper Etched Terrain is a plateau-forming unit with a geomorphic pattern that ranges from relatively flat plains to dissected plateaus and mesas. The lower Etched Terrain is flat with low albedo, and covered in dunes. It is in these Etched Terrains that CRISM, and previously OMEGA, have detected hydrated sulfates, which makes a sedimentary origin seems most likely for these layered deposits of Etched Terrain found in Meridiani. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:41 PM Degrees latitude (centered): 1.6 ° Degrees longitude (East): 359.8 ° Range to target site: 271.2 km (169.5 miles) Original image scale range: 27.1 cm/pixel (with 1 x 1 binning) so objects ~81 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.0 ° Phase angle: 53.4 ° Solar incidence angle: 55 °, with the Sun about 35 ° above the horizon Solar longitude: 172.1 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Northern Meridiani Etched Te …
PIA09593
Sol (our sun)
HiRISE
Title Northern Meridiani Etched Terrain and Hematite Plains Contact
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002324_1815 [ http://hirise.lpl.arizona.edu/PSP_002324_1815 ]) shows the contact between the Hematite Bearing Plains and Etched Terrain in Northern Meridiani Planum. The Hematite Bearing Plains (exposed at the bottom left of this image) are dark, smooth and full of dune fields. This unit is laterally extensive and the same unit that the Mars Exploration Rover Opportunity is sitting on about 400 km to the southwest. Based on observations by Opportunity, this unit is interpreted to be a thin aeolian (wind-blown) mantle of basaltic sand and hematite concretions sitting on the Etched Terrain. The Etched Terrain in this image is split into two units. The darker unit at the top of the image is filling in a ~120 km NW-SE trending valley, while the brighter Etched Terrain in the middle of the image is stratigraphically and topographically higher than the lower Etched Terrain in the valley. This upper Etched Terrain is a plateau-forming unit with a geomorphic pattern that ranges from relatively flat plains to dissected plateaus and mesas. The lower Etched Terrain is flat with low albedo, and covered in dunes. It is in these Etched Terrains that CRISM, and previously OMEGA, have detected hydrated sulfates, which makes a sedimentary origin seems most likely for these layered deposits of Etched Terrain found in Meridiani. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:41 PM Degrees latitude (centered): 1.6 ° Degrees longitude (East): 359.8 ° Range to target site: 271.2 km (169.5 miles) Original image scale range: 27.1 cm/pixel (with 1 x 1 binning) so objects ~81 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.0 ° Phase angle: 53.4 ° Solar incidence angle: 55 °, with the Sun about 35 ° above the horizon Solar longitude: 172.1 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Layers and Dark Debris in Me …
PIA09591
Sol (our sun)
HiRISE
Title Layers and Dark Debris in Melas Chasma
Original Caption Released with Image This HiRISE sub-image shows layering in a light-toned deposit in Melas Chasma. The layers are sedimentary in origin, but there are many processes that could have deposited them, such as volcanic airfall from explosive eruptions, dust-size particles settling out of the atmosphere due to cyclic changes, and deposition in standing bodies of water. By looking at the slopes in the layers and how the layers intersect each other, scientists can rule out various origins. A darker material can be seen covering much of the layered deposit. Some of this dark material is loose and can be seen accumulating as debris aprons at the base of steep slopes. Other dark material appears indurated and has been eroded by the wind to form etched edges with topographic expressions. The lack of impact craters on the layered deposit indicates that it is a relatively young deposit, or the craters have been removed by the wind, or the deposit was quickly buried and is now being exhumed. This HiRISE image is PSP_002419_1675 [ http://hirise.lpl.arizona.edu/PSP_002419_1675 ]. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -11.4 ° Degrees longitude (East): 287.6 ° Range to target site: 263.5 km (164.7 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.1 ° Phase angle: 57.1 ° Solar incidence angle: 57 °, with the Sun about 33 ° above the horizon Solar longitude: 176.2 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Vent at the Summit of Arsia …
PIA09597
Sol (our sun)
HiRISE
Title Vent at the Summit of Arsia Mons Volcano
Original Caption Released with Image Click on image for larger version Like the other major shield volcanoes on Mars, Arisa Mons has a caldera (large volcanic crater) at its summit. Calderas form when magma (molten rock) is removed from the magma chamber in the volcano, and the roof of the magma chamber collapses into the resulting void. In the case of Arsia Mons, there are relatively young lava flows that overtop the northeast rim of the caldera. This HiRISE image (PSP_002157_1715 [ http://hirise.lpl.arizona.edu/PSP_002157_1715 ]) samples some of these lava flows. The long elliptical depression is the summit crater of a small shield volcano that fed some of these lava flows. At HiRISE resolution, we see that even these younger lavas are covered by a thick layer of dust. The small dark-rayed crater in the southwest edge of the image shows that the rock under the dust is dark, as expected of lava. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -8.4 ° Degrees longitude (East): 240.1 ° Range to target site: 244.7 km (153.0 miles) Original image scale range: 49.0 cm/pixel (with 2 x 2 binning) so objects ~147 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.1 ° Phase angle: 57.1 ° Solar incidence angle: 57 °, with the Sun about 33 ° above the horizon Solar longitude: 165.0 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Vent at the Summit of Arsia …
PIA09597
Sol (our sun)
HiRISE
Title Vent at the Summit of Arsia Mons Volcano
Original Caption Released with Image Click on image for larger version Like the other major shield volcanoes on Mars, Arisa Mons has a caldera (large volcanic crater) at its summit. Calderas form when magma (molten rock) is removed from the magma chamber in the volcano, and the roof of the magma chamber collapses into the resulting void. In the case of Arsia Mons, there are relatively young lava flows that overtop the northeast rim of the caldera. This HiRISE image (PSP_002157_1715 [ http://hirise.lpl.arizona.edu/PSP_002157_1715 ]) samples some of these lava flows. The long elliptical depression is the summit crater of a small shield volcano that fed some of these lava flows. At HiRISE resolution, we see that even these younger lavas are covered by a thick layer of dust. The small dark-rayed crater in the southwest edge of the image shows that the rock under the dust is dark, as expected of lava. Observation Geometry Acquisition date: 1 January 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -8.4 ° Degrees longitude (East): 240.1 ° Range to target site: 244.7 km (153.0 miles) Original image scale range: 49.0 cm/pixel (with 2 x 2 binning) so objects ~147 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.1 ° Phase angle: 57.1 ° Solar incidence angle: 57 °, with the Sun about 33 ° above the horizon Solar longitude: 165.0 °, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Gullies and Ice-rich Materia …
PIA09712
Sol (our sun)
HiRISE
Title Gullies and Ice-rich Material
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002066_1425 [ http://hirise.lpl.arizona.edu/PSP_002066_1425 ]) shows gullies in a crater in the southern hemisphere. Gullies typically form when flowing water has sufficient energy to erode soil and soft rock in a channelized flow. The gullies in this image have narrow, overlapping channels and are deeply incised into the slope. Overlapping channels may suggest multiple flow events on this slope wall. It is unknown what happened to the water that flowed in these gullies. Some of the water may have evaporated or gradually sublimated into the atmosphere or became incorporated as ice in the gully debris aprons located downslope at their termini. Sublimation is a process similar to evaporation except that solid ice (instead of liquid water) returns to the atmosphere as a gas. Sublimation is common on Mars because the temperature and pressure are so low on Mars today that liquid water is only rarely stable. The crater floor is covered in boulders (see subimage, approximately 500 m across), dunes, and textured material. The boulders are likely a "sublimation lag" that provides evidence that material on the crater floor is, or once was, ice-rich. A sublimation lag forms when ice-rich material sublimates leaving the boulders and rocks behind. It is possible that the boulders on this crater floor represent such a process. The pitted texture around boulders may also be an indicator of ice sublimation. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -37.0° Degrees longitude (East): 207.0° Range to target site: 261.1 km (163.2 miles) Original image scale range: 26.1 cm/pixel (with 1 x 1 binning) so objects ~78 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 15.0° Phase angle: 81.1° Solar incidence angle: 68°, with the Sun about 22° above the horizon Solar longitude: 161.2°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Gullies and Ice-rich Materia …
PIA09712
Sol (our sun)
HiRISE
Title Gullies and Ice-rich Material
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002066_1425 [ http://hirise.lpl.arizona.edu/PSP_002066_1425 ]) shows gullies in a crater in the southern hemisphere. Gullies typically form when flowing water has sufficient energy to erode soil and soft rock in a channelized flow. The gullies in this image have narrow, overlapping channels and are deeply incised into the slope. Overlapping channels may suggest multiple flow events on this slope wall. It is unknown what happened to the water that flowed in these gullies. Some of the water may have evaporated or gradually sublimated into the atmosphere or became incorporated as ice in the gully debris aprons located downslope at their termini. Sublimation is a process similar to evaporation except that solid ice (instead of liquid water) returns to the atmosphere as a gas. Sublimation is common on Mars because the temperature and pressure are so low on Mars today that liquid water is only rarely stable. The crater floor is covered in boulders (see subimage, approximately 500 m across), dunes, and textured material. The boulders are likely a "sublimation lag" that provides evidence that material on the crater floor is, or once was, ice-rich. A sublimation lag forms when ice-rich material sublimates leaving the boulders and rocks behind. It is possible that the boulders on this crater floor represent such a process. The pitted texture around boulders may also be an indicator of ice sublimation. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -37.0° Degrees longitude (East): 207.0° Range to target site: 261.1 km (163.2 miles) Original image scale range: 26.1 cm/pixel (with 1 x 1 binning) so objects ~78 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 15.0° Phase angle: 81.1° Solar incidence angle: 68°, with the Sun about 22° above the horizon Solar longitude: 161.2°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Gullies and Ice-rich Materia …
PIA09712
Sol (our sun)
HiRISE
Title Gullies and Ice-rich Material
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002066_1425 [ http://hirise.lpl.arizona.edu/PSP_002066_1425 ]) shows gullies in a crater in the southern hemisphere. Gullies typically form when flowing water has sufficient energy to erode soil and soft rock in a channelized flow. The gullies in this image have narrow, overlapping channels and are deeply incised into the slope. Overlapping channels may suggest multiple flow events on this slope wall. It is unknown what happened to the water that flowed in these gullies. Some of the water may have evaporated or gradually sublimated into the atmosphere or became incorporated as ice in the gully debris aprons located downslope at their termini. Sublimation is a process similar to evaporation except that solid ice (instead of liquid water) returns to the atmosphere as a gas. Sublimation is common on Mars because the temperature and pressure are so low on Mars today that liquid water is only rarely stable. The crater floor is covered in boulders (see subimage, approximately 500 m across), dunes, and textured material. The boulders are likely a "sublimation lag" that provides evidence that material on the crater floor is, or once was, ice-rich. A sublimation lag forms when ice-rich material sublimates leaving the boulders and rocks behind. It is possible that the boulders on this crater floor represent such a process. The pitted texture around boulders may also be an indicator of ice sublimation. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -37.0° Degrees longitude (East): 207.0° Range to target site: 261.1 km (163.2 miles) Original image scale range: 26.1 cm/pixel (with 1 x 1 binning) so objects ~78 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 15.0° Phase angle: 81.1° Solar incidence angle: 68°, with the Sun about 22° above the horizon Solar longitude: 161.2°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Proposed MSL site in Holden …
PIA09711
Sol (our sun)
HiRISE
Title Proposed MSL site in Holden Crater Fan
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002154_1530 [ http://hirise.lpl.arizona.edu/PSP_002154_1530 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Holden Crater Fan. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:48 PM Degrees latitude (centered): -26.6° Degrees longitude (East): 325.2° Range to target site: 263.7 km (164.8 miles) Original image scale range: 52.8 cm/pixel (with 2 x 2 binning) so objects ~158 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 11.1° Phase angle: 54.9° Solar incidence angle: 64°, with the Sun about 26° above the horizon Solar longitude: 164.9°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Proposed MSL site in Holden …
PIA09711
Sol (our sun)
HiRISE
Title Proposed MSL site in Holden Crater Fan
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002154_1530 [ http://hirise.lpl.arizona.edu/PSP_002154_1530 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Holden Crater Fan. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:48 PM Degrees latitude (centered): -26.6° Degrees longitude (East): 325.2° Range to target site: 263.7 km (164.8 miles) Original image scale range: 52.8 cm/pixel (with 2 x 2 binning) so objects ~158 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 11.1° Phase angle: 54.9° Solar incidence angle: 64°, with the Sun about 26° above the horizon Solar longitude: 164.9°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Proposed MSL site in Meridia …
PIA09710
Sol (our sun)
HiRISE
Title Proposed MSL site in Meridiani Crater Lake
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002179_1855 [ http://hirise.lpl.arizona.edu/PSP_002179_1855 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Meridiani Crater Lake. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:40 PM Degrees latitude (centered): 5.4° Degrees longitude (East): 358.2° Range to target site: 273.5 km (171.0 miles) Original image scale range: 27.4 cm/pixel (with 1 x 1 binning) so objects ~82 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 4.0° Phase angle: 50.8° Solar incidence angle: 55°, with the Sun about 35° above the horizon Solar longitude: 165.9°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Proposed MSL site in Meridia …
PIA09710
Sol (our sun)
HiRISE
Title Proposed MSL site in Meridiani Crater Lake
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_002179_1855 [ http://hirise.lpl.arizona.edu/PSP_002179_1855 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Meridiani Crater Lake. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:40 PM Degrees latitude (centered): 5.4° Degrees longitude (East): 358.2° Range to target site: 273.5 km (171.0 miles) Original image scale range: 27.4 cm/pixel (with 1 x 1 binning) so objects ~82 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 4.0° Phase angle: 50.8° Solar incidence angle: 55°, with the Sun about 35° above the horizon Solar longitude: 165.9°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
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