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Images of Jet Propulsion Laboratory (JPL) and California from 2007 and March 2007
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Internal Heat Drives Jupiter
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| Title |
Internal Heat Drives Jupiter's Giant Storm Eruption |
| General Information |
What is a News Nugget? News Nuggets are bulletins from the world of astronomy. Detailed analysis of two continent-sized storms that erupted in Jupiter's atmosphere in March 2007 shows that Jupiter's internal heat plays a significant role in generating atmospheric disturbances. Understanding this outbreak could be the key to unlock the mysteries buried in the deep Jovian atmosphere. An international team coordinated by Agustin Sánchez-Lavega from the Universidad del País Vasco in Spain presents its findings about this event in the January 24 issue of the journal Nature. The team monitored the new eruption of cloud activity and its evolution with an unprecedented resolution using NASA's Hubble Space Telescope, the NASA Infrared Telescope Facility in Hawaii, and telescopes in the Canary Islands (Spain). A network of smaller telescopes around the world also supported these observations. |
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Craters on South Polar Layer
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PIA09670
Sol (our sun)
HiRISE
| Title |
Craters on South Polar Layered Deposits |
| Original Caption Released with Image |
Click on image for larger version This subimage, about 2.5 km across, shows the south polar layered deposits exposed in a scarp illuminated from the lower right. This HiRISE image (PSP_002882_0940 [ http://hirise.lpl.arizona.edu/PSP_002882_0940 ]) was taken in the southern spring, when the surface was completely covered by carbon dioxide frost. Therefore, most of the brightness variations in this scene are caused by topography. The polar layered deposits are broken into blocks by fractures in two directions. Neither set of fractures is parallel to the current scarp face, suggesting that they were not formed as the scarp was eroded, but instead are due to pre-existing weaknesses in the polar layered deposits. The four craters at lower left appear to have formed at the same time by an impactor that broke up as it entered the Martian atmosphere. The presence of many craters such as these on the south polar layered deposits indicates that they are not as young as the north polar layered deposits, which have very few craters on them. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 7:06 PM Degrees latitude (centered): -85.9° Degrees longitude (East): 303.4° Range to target site: 246.9 km (154.3 miles) Original image scale range: 24.7 cm/pixel (with 1 x 1 binning) so objects ~74 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 6.7° Phase angle: 78.5° Solar incidence angle: 84°, with the Sun about 6° above the horizon Solar longitude: 196.9°, 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. |
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Craters on South Polar Layer
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PIA09670
Sol (our sun)
HiRISE
| Title |
Craters on South Polar Layered Deposits |
| Original Caption Released with Image |
Click on image for larger version This subimage, about 2.5 km across, shows the south polar layered deposits exposed in a scarp illuminated from the lower right. This HiRISE image (PSP_002882_0940 [ http://hirise.lpl.arizona.edu/PSP_002882_0940 ]) was taken in the southern spring, when the surface was completely covered by carbon dioxide frost. Therefore, most of the brightness variations in this scene are caused by topography. The polar layered deposits are broken into blocks by fractures in two directions. Neither set of fractures is parallel to the current scarp face, suggesting that they were not formed as the scarp was eroded, but instead are due to pre-existing weaknesses in the polar layered deposits. The four craters at lower left appear to have formed at the same time by an impactor that broke up as it entered the Martian atmosphere. The presence of many craters such as these on the south polar layered deposits indicates that they are not as young as the north polar layered deposits, which have very few craters on them. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 7:06 PM Degrees latitude (centered): -85.9° Degrees longitude (East): 303.4° Range to target site: 246.9 km (154.3 miles) Original image scale range: 24.7 cm/pixel (with 1 x 1 binning) so objects ~74 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 6.7° Phase angle: 78.5° Solar incidence angle: 84°, with the Sun about 6° above the horizon Solar longitude: 196.9°, 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. |
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Craters on South Polar Layer
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PIA09670
Sol (our sun)
HiRISE
| Title |
Craters on South Polar Layered Deposits |
| Original Caption Released with Image |
Click on image for larger version This subimage, about 2.5 km across, shows the south polar layered deposits exposed in a scarp illuminated from the lower right. This HiRISE image (PSP_002882_0940 [ http://hirise.lpl.arizona.edu/PSP_002882_0940 ]) was taken in the southern spring, when the surface was completely covered by carbon dioxide frost. Therefore, most of the brightness variations in this scene are caused by topography. The polar layered deposits are broken into blocks by fractures in two directions. Neither set of fractures is parallel to the current scarp face, suggesting that they were not formed as the scarp was eroded, but instead are due to pre-existing weaknesses in the polar layered deposits. The four craters at lower left appear to have formed at the same time by an impactor that broke up as it entered the Martian atmosphere. The presence of many craters such as these on the south polar layered deposits indicates that they are not as young as the north polar layered deposits, which have very few craters on them. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 7:06 PM Degrees latitude (centered): -85.9° Degrees longitude (East): 303.4° Range to target site: 246.9 km (154.3 miles) Original image scale range: 24.7 cm/pixel (with 1 x 1 binning) so objects ~74 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 6.7° Phase angle: 78.5° Solar incidence angle: 84°, with the Sun about 6° above the horizon Solar longitude: 196.9°, 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. |
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Kaiser Crater Dune Field
PIA09669
Sol (our sun)
HiRISE
| Title |
Kaiser Crater Dune Field |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003141_1330 [ http://hirise.lpl.arizona.edu/PSP_003141_1330 ]) shows a sand dune field in Kaiser Crater, a 210 km (130 miles) wide impact basin in the Hellespontus region of Mars. Winds have trapped massive quantities of sand on the floors of broad craters in this region. The steepest slopes on each dune, the slip faces, point to the east indicating that the dominant wind direction in this part of the dune field is from west to east. Patches of seasonal frost can be seen in the low areas between the dunes. The subimage reveals smaller secondary dunes superimposed on the surface of the large dunes and even smaller ripples that appear between and perpendicular to the secondary dunes. Avalanching or mass movement of sand has left deep scars on the slip face of the large dune in the upper left portion of the subimage. This may indicate that the sand is not loose but is weakly cemented. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -46.6° Degrees longitude (East): 19.3° 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: 17.5° Phase angle: 74.6° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 209.0°, 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. |
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Kaiser Crater Dune Field
PIA09669
Sol (our sun)
HiRISE
| Title |
Kaiser Crater Dune Field |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003141_1330 [ http://hirise.lpl.arizona.edu/PSP_003141_1330 ]) shows a sand dune field in Kaiser Crater, a 210 km (130 miles) wide impact basin in the Hellespontus region of Mars. Winds have trapped massive quantities of sand on the floors of broad craters in this region. The steepest slopes on each dune, the slip faces, point to the east indicating that the dominant wind direction in this part of the dune field is from west to east. Patches of seasonal frost can be seen in the low areas between the dunes. The subimage reveals smaller secondary dunes superimposed on the surface of the large dunes and even smaller ripples that appear between and perpendicular to the secondary dunes. Avalanching or mass movement of sand has left deep scars on the slip face of the large dune in the upper left portion of the subimage. This may indicate that the sand is not loose but is weakly cemented. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -46.6° Degrees longitude (East): 19.3° 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: 17.5° Phase angle: 74.6° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 209.0°, 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. |
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Kaiser Crater Dune Field
PIA09669
Sol (our sun)
HiRISE
| Title |
Kaiser Crater Dune Field |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003141_1330 [ http://hirise.lpl.arizona.edu/PSP_003141_1330 ]) shows a sand dune field in Kaiser Crater, a 210 km (130 miles) wide impact basin in the Hellespontus region of Mars. Winds have trapped massive quantities of sand on the floors of broad craters in this region. The steepest slopes on each dune, the slip faces, point to the east indicating that the dominant wind direction in this part of the dune field is from west to east. Patches of seasonal frost can be seen in the low areas between the dunes. The subimage reveals smaller secondary dunes superimposed on the surface of the large dunes and even smaller ripples that appear between and perpendicular to the secondary dunes. Avalanching or mass movement of sand has left deep scars on the slip face of the large dune in the upper left portion of the subimage. This may indicate that the sand is not loose but is weakly cemented. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -46.6° Degrees longitude (East): 19.3° 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: 17.5° Phase angle: 74.6° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 209.0°, 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. |
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Monitoring South Polar Cap S
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PIA09625
Sol (our sun)
HiRISE
| Title |
Monitoring South Polar Cap Swiss-Cheese Terrain Change |
| Original Caption Released with Image |
) is taken in one of the troughs that are typical within the stack of Martian south polar layered deposits. Viewed at low resolution, sequences of layers of different albedos, or brightnesses, and/or textures can be seen. At full resolution, the different tones and textures can be seen to be due to different shapes and sizes of polygonal fractures, surface knobiness, and surface cover and concentration of frost, often within polygonal fractures. Faint criss-crossing troughs and dimples can be discerned on even the smoothest surfaces. Perhaps the most notable features in the image are the distinct round to heart-shaped to blob-shaped depressions scattered throughout the smooth areas, dubbed "swiss-cheese terrain." The smooth material is solid carbon dioxide ice representing the uppermost layer of the south polar residual cap. The retention of carbon dioxide ice throughout the year by the southern polar cap is one characteristic that distinguishes it significantly from Mars' north polar cap. The swiss-cheese depressions are areas in which sublimation of the carbon dioxide ice was initiated at a particular location and spread laterally from that point, creating rounded depressions typically several to 10 meters deep. In HiRISE images, it is evident that this carbon dioxide-rich material is actually comprised of several individual horizontal layers. In this particular location, several images had been acquired over the previous decade by the Mars Orbiter Camera (MOC) at slightly lower resolutions. In a series of those MOC images, the swiss-cheese depressions were seen to enlarge radially, or grow over a time period of several years. Part of the HiRISE imaging campaign includes continued monitoring of these features (at higher resolution) to understand their growth rates and patterns. In turn, we can better comprehend the role of carbon dioxide -- the main component of the Mars atmosphere -- in the current Mars climate regime. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 7:42 PM Degrees latitude (centered): -87.0° Degrees longitude (East): 281.8° Range to target site: 247.8 km (154.9 miles) Original image scale range: 49.6 cm/pixel (with 2 x 2 binning) so objects ~149 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 1.6° Phase angle: 87.0° Solar incidence angle: 86°, with the Sun about 4° above the horizon Solar longitude: 193.3°, 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_002804_0930 [ http://hirise.lpl.arizona.edu/PSP_002804_0930 ] |
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Monitoring South Polar Cap S
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PIA09625
Sol (our sun)
HiRISE
| Title |
Monitoring South Polar Cap Swiss-Cheese Terrain Change |
| Original Caption Released with Image |
) is taken in one of the troughs that are typical within the stack of Martian south polar layered deposits. Viewed at low resolution, sequences of layers of different albedos, or brightnesses, and/or textures can be seen. At full resolution, the different tones and textures can be seen to be due to different shapes and sizes of polygonal fractures, surface knobiness, and surface cover and concentration of frost, often within polygonal fractures. Faint criss-crossing troughs and dimples can be discerned on even the smoothest surfaces. Perhaps the most notable features in the image are the distinct round to heart-shaped to blob-shaped depressions scattered throughout the smooth areas, dubbed "swiss-cheese terrain." The smooth material is solid carbon dioxide ice representing the uppermost layer of the south polar residual cap. The retention of carbon dioxide ice throughout the year by the southern polar cap is one characteristic that distinguishes it significantly from Mars' north polar cap. The swiss-cheese depressions are areas in which sublimation of the carbon dioxide ice was initiated at a particular location and spread laterally from that point, creating rounded depressions typically several to 10 meters deep. In HiRISE images, it is evident that this carbon dioxide-rich material is actually comprised of several individual horizontal layers. In this particular location, several images had been acquired over the previous decade by the Mars Orbiter Camera (MOC) at slightly lower resolutions. In a series of those MOC images, the swiss-cheese depressions were seen to enlarge radially, or grow over a time period of several years. Part of the HiRISE imaging campaign includes continued monitoring of these features (at higher resolution) to understand their growth rates and patterns. In turn, we can better comprehend the role of carbon dioxide -- the main component of the Mars atmosphere -- in the current Mars climate regime. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 7:42 PM Degrees latitude (centered): -87.0° Degrees longitude (East): 281.8° Range to target site: 247.8 km (154.9 miles) Original image scale range: 49.6 cm/pixel (with 2 x 2 binning) so objects ~149 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 1.6° Phase angle: 87.0° Solar incidence angle: 86°, with the Sun about 4° above the horizon Solar longitude: 193.3°, 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_002804_0930 [ http://hirise.lpl.arizona.edu/PSP_002804_0930 ] |
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Aram Chaos Sediments
PIA09624
Sol (our sun)
HiRISE
| Title |
Aram Chaos Sediments |
| Original Caption Released with Image |
Click on image for larger version Aram Chaos appears to be a former impact crater. The terrain is disrupted, giving it a chaotic appearance (hence the name "chaos"). Scientists have postulated that a lake may have once existed inside the crater and sediments were laid down within the lake. The mineral hematite (rich in iron) has been detected by orbiting spacecraft within Aram Chaos. Hematite has been identified in several other locations on Mars, including at the Mars Exploration Rover landing site in Meridiani Planum. The hematite at both Meridiani and Aram Chaos most likely formed by precipitation in water. This HiRISE image (PSP_002839_1825 [ http://hirise.lpl.arizona.edu/PSP_002839_1825 ]) shows the light-toned sediments inside Aram Chaos that could have formed in a former lake. Unfortunately, dark debris now obscures much of this sediment, making it difficult to view and interpret the rocks. The light-toned layered deposit in the south (bottom) of the image is higher standing and has a pitted surface. Circular structures with dark centers are likely to be impact craters that have been partly filled with dark debris, including sand. More irregular depressions appear to result from erosion of layered beds within the sediments. Wind could erode materials that are slightly weaker more quickly and produce the irregular topography seen along the surface of the deposit. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:41 PM Degrees latitude (centered): 2.7° Degrees longitude (East): 339.3° Range to target site: 272.3 km (170.2 miles) Original image scale range: 27.2 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: 0.0° Phase angle: 56.1° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 194.9°, 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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Aram Chaos Sediments
PIA09624
Sol (our sun)
HiRISE
| Title |
Aram Chaos Sediments |
| Original Caption Released with Image |
Click on image for larger version Aram Chaos appears to be a former impact crater. The terrain is disrupted, giving it a chaotic appearance (hence the name "chaos"). Scientists have postulated that a lake may have once existed inside the crater and sediments were laid down within the lake. The mineral hematite (rich in iron) has been detected by orbiting spacecraft within Aram Chaos. Hematite has been identified in several other locations on Mars, including at the Mars Exploration Rover landing site in Meridiani Planum. The hematite at both Meridiani and Aram Chaos most likely formed by precipitation in water. This HiRISE image (PSP_002839_1825 [ http://hirise.lpl.arizona.edu/PSP_002839_1825 ]) shows the light-toned sediments inside Aram Chaos that could have formed in a former lake. Unfortunately, dark debris now obscures much of this sediment, making it difficult to view and interpret the rocks. The light-toned layered deposit in the south (bottom) of the image is higher standing and has a pitted surface. Circular structures with dark centers are likely to be impact craters that have been partly filled with dark debris, including sand. More irregular depressions appear to result from erosion of layered beds within the sediments. Wind could erode materials that are slightly weaker more quickly and produce the irregular topography seen along the surface of the deposit. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:41 PM Degrees latitude (centered): 2.7° Degrees longitude (East): 339.3° Range to target site: 272.3 km (170.2 miles) Original image scale range: 27.2 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: 0.0° Phase angle: 56.1° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 194.9°, 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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Proposed MSL Site in Mawrth
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PIA09647
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Mawrth Vallis |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003063_2050 [ http://hirise.lpl.arizona.edu/PSP_003063_2050 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Mawrth Vallis. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:32 PM Degrees latitude (centered): 24.9° Degrees longitude (East): 340.2° Range to target site: 292.0 km (182.5 miles) Original image scale range: 29.2 cm/pixel (with 1 x 1 binning) so objects ~88 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 10.0° Phase angle: 72.2° Solar incidence angle: 63°, with the Sun about 27° above the horizon Solar longitude: 205.3°, 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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Proposed MSL Site in Mawrth
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PIA09647
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Mawrth Vallis |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003063_2050 [ http://hirise.lpl.arizona.edu/PSP_003063_2050 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Mawrth Vallis. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:32 PM Degrees latitude (centered): 24.9° Degrees longitude (East): 340.2° Range to target site: 292.0 km (182.5 miles) Original image scale range: 29.2 cm/pixel (with 1 x 1 binning) so objects ~88 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 10.0° Phase angle: 72.2° Solar incidence angle: 63°, with the Sun about 27° above the horizon Solar longitude: 205.3°, 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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Proposed MSL Site in Elysium
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PIA09636
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Elysium/Avernus Colles |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_002832_1770 [ http://hirise.lpl.arizona.edu/PSP_002832_1770 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Elysium/Avernus Colles. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -3.1° Degrees longitude (East): 170.7° Range to target site: 270.5 km (169.1 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: 5.0° Phase angle: 60.2° Solar incidence angle: 55°, with the Sun about 35° above the horizon Solar longitude: 194.6°, 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. |
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Proposed MSL Site in Elysium
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PIA09636
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Elysium/Avernus Colles |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_002832_1770 [ http://hirise.lpl.arizona.edu/PSP_002832_1770 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Elysium/Avernus Colles. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -3.1° Degrees longitude (East): 170.7° Range to target site: 270.5 km (169.1 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: 5.0° Phase angle: 60.2° Solar incidence angle: 55°, with the Sun about 35° above the horizon Solar longitude: 194.6°, 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. |
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South Polar Layered Deposits
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PIA09630
Sol (our sun)
HiRISE
| Title |
South Polar Layered Deposits and Residual Cap |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002856_0875 [ http://hirise.lpl.arizona.edu/PSP_002856_0875 ]) shows a variety of surface texture within the south polar residual cap of Mars. It was taken during the southern spring, when the surface was covered by seasonal carbon dioxide frost, so that surface relief is easily seen. Illumination is from the bottom left, highlighting long troughs at to the right and round pits and irregular mesas to the left of center. These unique landforms are common in the south polar residual cap, which is known from previous Mars Global Surveyor images to be eroding rapidly in places. Right of center, polar layered deposits are exposed on a sun-facing scarp. These deposits are older than the residual ice cap, and the layers are thought to record climate variations on Mars similar to ice ages on Earth. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 10:14 PM Degrees latitude (centered): -87.2° Degrees longitude (East): 340.3° Range to target site: 244.7 km (152.9 miles) Original image scale range: 24.5 cm/pixel (with 1 x 1 binning) so objects ~73 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 0.1° Phase angle: 85.8° Solar incidence angle: 86°, with the Sun about 4° above the horizon Solar longitude: 195.7°, 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. |
|
South Polar Layered Deposits
…
PIA09630
Sol (our sun)
HiRISE
| Title |
South Polar Layered Deposits and Residual Cap |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002856_0875 [ http://hirise.lpl.arizona.edu/PSP_002856_0875 ]) shows a variety of surface texture within the south polar residual cap of Mars. It was taken during the southern spring, when the surface was covered by seasonal carbon dioxide frost, so that surface relief is easily seen. Illumination is from the bottom left, highlighting long troughs at to the right and round pits and irregular mesas to the left of center. These unique landforms are common in the south polar residual cap, which is known from previous Mars Global Surveyor images to be eroding rapidly in places. Right of center, polar layered deposits are exposed on a sun-facing scarp. These deposits are older than the residual ice cap, and the layers are thought to record climate variations on Mars similar to ice ages on Earth. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 10:14 PM Degrees latitude (centered): -87.2° Degrees longitude (East): 340.3° Range to target site: 244.7 km (152.9 miles) Original image scale range: 24.5 cm/pixel (with 1 x 1 binning) so objects ~73 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 0.1° Phase angle: 85.8° Solar incidence angle: 86°, with the Sun about 4° above the horizon Solar longitude: 195.7°, 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. |
|
Glacier-Like Flow on Arsia M
…
PIA09648
Sol (our sun)
HiRISE
| Title |
Glacier-Like Flow on Arsia Mons Flank |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002922_1725 [ http://hirise.lpl.arizona.edu/PSP_002922_1725 ]) shows glacier-like flow in a depression in the flanks of Arsia Mons. Arsia Mons is one of the large Martian volcanoes that sits near the equator on the Tharsis Rise. Downslope is towards the top left of the image, and flow is in this direction. It is interesting to note that the depression being viewed is not directly radial from the volcano's peak, but rather oriented approximately 45 degrees away from radial, along the flanks of the volcano. The pitted texture of the material suggests that sublimation is occurring or has occurred. Sublimation is when a substance, such as water ice, goes directly from a solid state to a gaseous state without going through an intermediate liquid phase. The surface temperature and pressure on Mars are such that water in ice-rich material can easily sublimate leaving behind a depression where the volatiles were removed. It is possible that the flow features in this image are relict glaciers. The flow lobes and surface lineations are similar to those found on glaciers on Earth. The merging of the lobes seen in the bottom of the image and the subimage (approximately 3.2 km across) implies that multiple walls are shedding material. It's possible that the flanks of Arsia Mons contain ice-rich material possibly deposited during a different obliquity (tilt of Mars' spin axis) or climate regime. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:49 PM Degrees latitude (centered): -7.3° Degrees longitude (East): 236.2° Range to target site: 276.7 km (179.9 miles) Original image scale range: 27.7 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: 22.9° Phase angle: 34.1° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 198.7°, 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. |
|
Glacier-Like Flow on Arsia M
…
PIA09648
Sol (our sun)
HiRISE
| Title |
Glacier-Like Flow on Arsia Mons Flank |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002922_1725 [ http://hirise.lpl.arizona.edu/PSP_002922_1725 ]) shows glacier-like flow in a depression in the flanks of Arsia Mons. Arsia Mons is one of the large Martian volcanoes that sits near the equator on the Tharsis Rise. Downslope is towards the top left of the image, and flow is in this direction. It is interesting to note that the depression being viewed is not directly radial from the volcano's peak, but rather oriented approximately 45 degrees away from radial, along the flanks of the volcano. The pitted texture of the material suggests that sublimation is occurring or has occurred. Sublimation is when a substance, such as water ice, goes directly from a solid state to a gaseous state without going through an intermediate liquid phase. The surface temperature and pressure on Mars are such that water in ice-rich material can easily sublimate leaving behind a depression where the volatiles were removed. It is possible that the flow features in this image are relict glaciers. The flow lobes and surface lineations are similar to those found on glaciers on Earth. The merging of the lobes seen in the bottom of the image and the subimage (approximately 3.2 km across) implies that multiple walls are shedding material. It's possible that the flanks of Arsia Mons contain ice-rich material possibly deposited during a different obliquity (tilt of Mars' spin axis) or climate regime. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:49 PM Degrees latitude (centered): -7.3° Degrees longitude (East): 236.2° Range to target site: 276.7 km (179.9 miles) Original image scale range: 27.7 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: 22.9° Phase angle: 34.1° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 198.7°, 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. |
|
Proposed MSL Site in NE Syrt
…
PIA09637
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in NE Syrtis Major |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_002809_1965 [ http://hirise.lpl.arizona.edu/PSP_002809_1965 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Northeast Syrtis Major. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:39 PM Degrees latitude (centered): 16.5° Degrees longitude (East): 76.6° Range to target site: 278.1 km (173.8 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: 0.2° Phase angle: 58.7° Solar incidence angle: 59°, with the Sun about 31° above the horizon Solar longitude: 193.5°, 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. |
|
Proposed MSL Site in NE Syrt
…
PIA09637
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in NE Syrtis Major |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_002809_1965 [ http://hirise.lpl.arizona.edu/PSP_002809_1965 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Northeast Syrtis Major. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:39 PM Degrees latitude (centered): 16.5° Degrees longitude (East): 76.6° Range to target site: 278.1 km (173.8 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: 0.2° Phase angle: 58.7° Solar incidence angle: 59°, with the Sun about 31° above the horizon Solar longitude: 193.5°, 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. |
|
Proposed MSL Site in Southwe
…
PIA09649
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Southwest Arabia Terra |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_002812_1855 [ http://hirise.lpl.arizona.edu/PSP_002812_1855 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Southwest Arabia Terra. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:39 PM Degrees latitude (centered): 5.6° Degrees longitude (East): 355.6° Range to target site: 274.5 km (171.5 miles) Original image scale range: 27.5 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: 6.0° Phase angle: 62.0° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 193.7°, 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. |
|
Proposed MSL Site in Southwe
…
PIA09649
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Southwest Arabia Terra |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_002812_1855 [ http://hirise.lpl.arizona.edu/PSP_002812_1855 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Southwest Arabia Terra. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:39 PM Degrees latitude (centered): 5.6° Degrees longitude (East): 355.6° Range to target site: 274.5 km (171.5 miles) Original image scale range: 27.5 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: 6.0° Phase angle: 62.0° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 193.7°, 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. |
|
Dissected Mantled Terrain
PIA09661
Sol (our sun)
HiRISE
| Title |
Dissected Mantled Terrain |
| Original Caption Released with Image |
Click on image for larger version A northern mid-latitude scene consisting of craters, intercrater plains, and mantled material is seen in this HiRISE image (PSP_002917_2175 [ http://hirise.lpl.arizona.edu/PSP_002917_2175 ]). The mantled material seen here covers much of the middle latitudes in both hemispheres of Mars, it has been visibly removed in some locations. It's called "mantled" because it looks as if it's just draped over, or mantling, the topography underneath. The mantled material is what causes the craters to have a muted, softened appearance. It's thought to be ice-rich material deposited in a climate different from that of today. The mantled unit is dissected here, meaning that is not pristine and has likely undergone modification since it was originally laid down. The intercrater plains have a pitted texture (see subimage, full resolution, approx. 200 m [218 yards]) thought to be caused by water ice sublimating and leaving depressions behind. Unlike that of Earth, the obliquity (tilt of the planet's rotation axis) of Mars changes wildly. Earth has the Moon to keep its axis stable, but Mars' satellites, Phobos and Deimos, are not massive enough to do the same. Today Mars' obliquity (25.19°) is similar to that of Earth's (23.45°), but this has not always been the case. As the obliquity changes, the portions of Mars that receive the most sunlight shift. During periods of high obliquity, polar regions receive the most sunlight. This causes polar ices, including water ice and carbon dioxide ice, to sublimate (evaporate) into the atmosphere. They would then potentially be re-deposited in the mid-latitudes, similar to where this image is located. It is believed that this process is responsible for the mid-latitude mantled unit. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:34 PM Degrees latitude (centered): 37.0° Degrees longitude (East): 5.3° Range to target site: 295.6 km (184.7 miles) Original image scale range: 29.6 cm/pixel (with 1 x 1 binning) so objects ~89 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.3° Phase angle: 67.3° Solar incidence angle: 67°, with the Sun about 23° above the horizon Solar longitude: 198.5°, 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. |
|
Dissected Mantled Terrain
PIA09661
Sol (our sun)
HiRISE
| Title |
Dissected Mantled Terrain |
| Original Caption Released with Image |
Click on image for larger version A northern mid-latitude scene consisting of craters, intercrater plains, and mantled material is seen in this HiRISE image (PSP_002917_2175 [ http://hirise.lpl.arizona.edu/PSP_002917_2175 ]). The mantled material seen here covers much of the middle latitudes in both hemispheres of Mars, it has been visibly removed in some locations. It's called "mantled" because it looks as if it's just draped over, or mantling, the topography underneath. The mantled material is what causes the craters to have a muted, softened appearance. It's thought to be ice-rich material deposited in a climate different from that of today. The mantled unit is dissected here, meaning that is not pristine and has likely undergone modification since it was originally laid down. The intercrater plains have a pitted texture (see subimage, full resolution, approx. 200 m [218 yards]) thought to be caused by water ice sublimating and leaving depressions behind. Unlike that of Earth, the obliquity (tilt of the planet's rotation axis) of Mars changes wildly. Earth has the Moon to keep its axis stable, but Mars' satellites, Phobos and Deimos, are not massive enough to do the same. Today Mars' obliquity (25.19°) is similar to that of Earth's (23.45°), but this has not always been the case. As the obliquity changes, the portions of Mars that receive the most sunlight shift. During periods of high obliquity, polar regions receive the most sunlight. This causes polar ices, including water ice and carbon dioxide ice, to sublimate (evaporate) into the atmosphere. They would then potentially be re-deposited in the mid-latitudes, similar to where this image is located. It is believed that this process is responsible for the mid-latitude mantled unit. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:34 PM Degrees latitude (centered): 37.0° Degrees longitude (East): 5.3° Range to target site: 295.6 km (184.7 miles) Original image scale range: 29.6 cm/pixel (with 1 x 1 binning) so objects ~89 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.3° Phase angle: 67.3° Solar incidence angle: 67°, with the Sun about 23° above the horizon Solar longitude: 198.5°, 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. |
|
Dissected Mantled Terrain
PIA09661
Sol (our sun)
HiRISE
| Title |
Dissected Mantled Terrain |
| Original Caption Released with Image |
Click on image for larger version A northern mid-latitude scene consisting of craters, intercrater plains, and mantled material is seen in this HiRISE image (PSP_002917_2175 [ http://hirise.lpl.arizona.edu/PSP_002917_2175 ]). The mantled material seen here covers much of the middle latitudes in both hemispheres of Mars, it has been visibly removed in some locations. It's called "mantled" because it looks as if it's just draped over, or mantling, the topography underneath. The mantled material is what causes the craters to have a muted, softened appearance. It's thought to be ice-rich material deposited in a climate different from that of today. The mantled unit is dissected here, meaning that is not pristine and has likely undergone modification since it was originally laid down. The intercrater plains have a pitted texture (see subimage, full resolution, approx. 200 m [218 yards]) thought to be caused by water ice sublimating and leaving depressions behind. Unlike that of Earth, the obliquity (tilt of the planet's rotation axis) of Mars changes wildly. Earth has the Moon to keep its axis stable, but Mars' satellites, Phobos and Deimos, are not massive enough to do the same. Today Mars' obliquity (25.19°) is similar to that of Earth's (23.45°), but this has not always been the case. As the obliquity changes, the portions of Mars that receive the most sunlight shift. During periods of high obliquity, polar regions receive the most sunlight. This causes polar ices, including water ice and carbon dioxide ice, to sublimate (evaporate) into the atmosphere. They would then potentially be re-deposited in the mid-latitudes, similar to where this image is located. It is believed that this process is responsible for the mid-latitude mantled unit. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:34 PM Degrees latitude (centered): 37.0° Degrees longitude (East): 5.3° Range to target site: 295.6 km (184.7 miles) Original image scale range: 29.6 cm/pixel (with 1 x 1 binning) so objects ~89 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.3° Phase angle: 67.3° Solar incidence angle: 67°, with the Sun about 23° above the horizon Solar longitude: 198.5°, 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. |
|
Proposed MSL Site in Nili Fo
…
PIA09646
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Nili Fossae Trough |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003086_2015 [ http://hirise.lpl.arizona.edu/PSP_003086_2015 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Nili Fossae Trough. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:38 PM Degrees latitude (centered): 21.1° Degrees longitude (East): 74.2° Range to target site: 282.4 km (176.5 miles) Original image scale range: 28.3 cm/pixel (with 1 x 1 binning) so objects ~85 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 7.4° Phase angle: 55.5° Solar incidence angle: 62°, with the Sun about 28° above the horizon Solar longitude: 206.4°, 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 Nili Fo
…
PIA09646
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Nili Fossae Trough |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003086_2015 [ http://hirise.lpl.arizona.edu/PSP_003086_2015 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Nili Fossae Trough. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:38 PM Degrees latitude (centered): 21.1° Degrees longitude (East): 74.2° Range to target site: 282.4 km (176.5 miles) Original image scale range: 28.3 cm/pixel (with 1 x 1 binning) so objects ~85 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 7.4° Phase angle: 55.5° Solar incidence angle: 62°, with the Sun about 28° above the horizon Solar longitude: 206.4°, 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 Xanthe/
…
PIA09634
Sol (our sun)
HiRISE
| Title |
Proposed MSL site in Xanthe/Hypanis Vallis |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_002919_1915 [ http://hirise.lpl.arizona.edu/PSP_002919_1915 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Xanthe/Hypanis Vallis. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:42 PM Degrees latitude (centered): 11.4° Degrees longitude (East): 314.7° Range to target site: 279.9 km (179.4 miles) Original image scale range: 28.0 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: 8.2° Phase angle: 50.5° Solar incidence angle: 59°, with the Sun about 31° above the horizon Solar longitude: 198.6°, 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. |
|
Proposed MSL site in Xanthe/
…
PIA09634
Sol (our sun)
HiRISE
| Title |
Proposed MSL site in Xanthe/Hypanis Vallis |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_002919_1915 [ http://hirise.lpl.arizona.edu/PSP_002919_1915 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Xanthe/Hypanis Vallis. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:42 PM Degrees latitude (centered): 11.4° Degrees longitude (East): 314.7° Range to target site: 279.9 km (179.4 miles) Original image scale range: 28.0 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: 8.2° Phase angle: 50.5° Solar incidence angle: 59°, with the Sun about 31° above the horizon Solar longitude: 198.6°, 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. |
|
Meanders in Nanedi Valles
PIA09635
Sol (our sun)
HiRISE
| Title |
Meanders in Nanedi Valles |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002840_1855 [ http://hirise.lpl.arizona.edu/PSP_002840_1855 ]) shows a portion of Nanedi Valles, an equatorial Martian valley network. Valley networks are thought to have formed by groundwater sapping either in conjunction with an ice layer to cover the running water or during a past warmer, wetter climate regime on Mars. Glacial activity has also been proposed to form the valley networks. Groundwater sapping is the leading theory because of the morphology of the valleys. They commonly have approximately constant width along their reaches, as seen here, as well as theater shaped heads, as seen in the tributary valley in the bottom right of the scene. The meandering nature of valleys suggests persistent or repeated flow as required to form meanders in streams on Earth. The subimage (approximately 1.1 km across) shows a potential remnant channel seen on the floor of Nanedi Valles just below the center of the image. If this is a remnant channel, it suggests that there was either repeated or waning flows in this valley. Winding dunes and abundant impact craters are found throughout the valley, as well as within this putative channel. Dunes are thought to be transient features on Mars, although no movement has been detected to date. It is interesting to note that some of the dunes are superposed by craters indicating that the dunes were stable long enough for craters to form and not be erased. It is possible that the craters on top of the dunes are secondary craters that formed as a product of a larger impact. Secondary craters from a single impact are clustered in space and form almost simultaneously, implying that the dunes were stable for a time period-long enough for a single crater, rather than multiple craters, to form. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:41 PM Degrees latitude (centered): 5.2° Degrees longitude (East): 311.8° Range to target site: 271.3 km (169.6 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: 2.2° Phase angle: 54.4° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 195.0°, 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. |
|
Meanders in Nanedi Valles
PIA09635
Sol (our sun)
HiRISE
| Title |
Meanders in Nanedi Valles |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002840_1855 [ http://hirise.lpl.arizona.edu/PSP_002840_1855 ]) shows a portion of Nanedi Valles, an equatorial Martian valley network. Valley networks are thought to have formed by groundwater sapping either in conjunction with an ice layer to cover the running water or during a past warmer, wetter climate regime on Mars. Glacial activity has also been proposed to form the valley networks. Groundwater sapping is the leading theory because of the morphology of the valleys. They commonly have approximately constant width along their reaches, as seen here, as well as theater shaped heads, as seen in the tributary valley in the bottom right of the scene. The meandering nature of valleys suggests persistent or repeated flow as required to form meanders in streams on Earth. The subimage (approximately 1.1 km across) shows a potential remnant channel seen on the floor of Nanedi Valles just below the center of the image. If this is a remnant channel, it suggests that there was either repeated or waning flows in this valley. Winding dunes and abundant impact craters are found throughout the valley, as well as within this putative channel. Dunes are thought to be transient features on Mars, although no movement has been detected to date. It is interesting to note that some of the dunes are superposed by craters indicating that the dunes were stable long enough for craters to form and not be erased. It is possible that the craters on top of the dunes are secondary craters that formed as a product of a larger impact. Secondary craters from a single impact are clustered in space and form almost simultaneously, implying that the dunes were stable for a time period-long enough for a single crater, rather than multiple craters, to form. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:41 PM Degrees latitude (centered): 5.2° Degrees longitude (East): 311.8° Range to target site: 271.3 km (169.6 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: 2.2° Phase angle: 54.4° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 195.0°, 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. |
|
Meanders in Nanedi Valles
PIA09635
Sol (our sun)
HiRISE
| Title |
Meanders in Nanedi Valles |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002840_1855 [ http://hirise.lpl.arizona.edu/PSP_002840_1855 ]) shows a portion of Nanedi Valles, an equatorial Martian valley network. Valley networks are thought to have formed by groundwater sapping either in conjunction with an ice layer to cover the running water or during a past warmer, wetter climate regime on Mars. Glacial activity has also been proposed to form the valley networks. Groundwater sapping is the leading theory because of the morphology of the valleys. They commonly have approximately constant width along their reaches, as seen here, as well as theater shaped heads, as seen in the tributary valley in the bottom right of the scene. The meandering nature of valleys suggests persistent or repeated flow as required to form meanders in streams on Earth. The subimage (approximately 1.1 km across) shows a potential remnant channel seen on the floor of Nanedi Valles just below the center of the image. If this is a remnant channel, it suggests that there was either repeated or waning flows in this valley. Winding dunes and abundant impact craters are found throughout the valley, as well as within this putative channel. Dunes are thought to be transient features on Mars, although no movement has been detected to date. It is interesting to note that some of the dunes are superposed by craters indicating that the dunes were stable long enough for craters to form and not be erased. It is possible that the craters on top of the dunes are secondary craters that formed as a product of a larger impact. Secondary craters from a single impact are clustered in space and form almost simultaneously, implying that the dunes were stable for a time period-long enough for a single crater, rather than multiple craters, to form. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:41 PM Degrees latitude (centered): 5.2° Degrees longitude (East): 311.8° Range to target site: 271.3 km (169.6 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: 2.2° Phase angle: 54.4° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 195.0°, 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. |
|
Dark Dunes in Herschel Crate
…
PIA09657
Sol (our sun)
HiRISE
| Title |
Dark Dunes in Herschel Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image PSP_002860_1650 [ http://hirise.lpl.arizona.edu/PSP_002860_1650 ] shows part of the floor of Herschel Crater, a roughly 300 kilometer wide impact basin located in the southern cratered highlands of Mars. The subimage is a close-up of a dark-toned sand dune field located on the crater floor. These dunes are "barchan" dunes, which are also commonly found on Earth. Barchan dunes are generally crescent-shaped, with their "horns" oriented in the downwind direction. They have a steep slip face (the downwind side of the dune). Barchan dunes form by winds that blow mostly in one direction and thus are good indicators of the dominant wind direction. In this case, the strongest winds blow approximately north to south. The surface of the dunes has a generally pitted and grooved texture and, in some places, is covered with smaller ripples. The grooved texture has led researchers in the past to believe the dune sands are "lithified," or cemented together. The rock that formed as a result has since been eroded and scoured by wind. These dark dunes in Herschel Crater are most likely composed of basaltic sand. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:44 PM Degrees latitude (centered): -14.8° Degrees longitude (East): 127.9° Range to target site: 259.0 km (161.9 miles) Original image scale range: 25.9 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: 2.3° Phase angle: 57.9° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 195.9°, 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. |
|
Dark Dunes in Herschel Crate
…
PIA09657
Sol (our sun)
HiRISE
| Title |
Dark Dunes in Herschel Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image PSP_002860_1650 [ http://hirise.lpl.arizona.edu/PSP_002860_1650 ] shows part of the floor of Herschel Crater, a roughly 300 kilometer wide impact basin located in the southern cratered highlands of Mars. The subimage is a close-up of a dark-toned sand dune field located on the crater floor. These dunes are "barchan" dunes, which are also commonly found on Earth. Barchan dunes are generally crescent-shaped, with their "horns" oriented in the downwind direction. They have a steep slip face (the downwind side of the dune). Barchan dunes form by winds that blow mostly in one direction and thus are good indicators of the dominant wind direction. In this case, the strongest winds blow approximately north to south. The surface of the dunes has a generally pitted and grooved texture and, in some places, is covered with smaller ripples. The grooved texture has led researchers in the past to believe the dune sands are "lithified," or cemented together. The rock that formed as a result has since been eroded and scoured by wind. These dark dunes in Herschel Crater are most likely composed of basaltic sand. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:44 PM Degrees latitude (centered): -14.8° Degrees longitude (East): 127.9° Range to target site: 259.0 km (161.9 miles) Original image scale range: 25.9 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: 2.3° Phase angle: 57.9° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 195.9°, 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. |
|
Dark Dunes in Herschel Crate
…
PIA09657
Sol (our sun)
HiRISE
| Title |
Dark Dunes in Herschel Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image PSP_002860_1650 [ http://hirise.lpl.arizona.edu/PSP_002860_1650 ] shows part of the floor of Herschel Crater, a roughly 300 kilometer wide impact basin located in the southern cratered highlands of Mars. The subimage is a close-up of a dark-toned sand dune field located on the crater floor. These dunes are "barchan" dunes, which are also commonly found on Earth. Barchan dunes are generally crescent-shaped, with their "horns" oriented in the downwind direction. They have a steep slip face (the downwind side of the dune). Barchan dunes form by winds that blow mostly in one direction and thus are good indicators of the dominant wind direction. In this case, the strongest winds blow approximately north to south. The surface of the dunes has a generally pitted and grooved texture and, in some places, is covered with smaller ripples. The grooved texture has led researchers in the past to believe the dune sands are "lithified," or cemented together. The rock that formed as a result has since been eroded and scoured by wind. These dark dunes in Herschel Crater are most likely composed of basaltic sand. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:44 PM Degrees latitude (centered): -14.8° Degrees longitude (East): 127.9° Range to target site: 259.0 km (161.9 miles) Original image scale range: 25.9 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: 2.3° Phase angle: 57.9° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 195.9°, 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 Deposits in Aureum C
…
PIA09656
Sol (our sun)
HiRISE
| Title |
Layered Deposits in Aureum Chaos |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002892_1760 [ http://hirise.lpl.arizona.edu/PSP_002892_1760 ]) shows an outcrop of a large slab of layered deposits in Aureum Chaos. "Chaotic" terrains on Mars are disorganized regions of blocks and large mounds which appear to have been produced by the collapse of pre-existing terrain. They are often associated with giant outflow channels, and they may have been the source of the water that carved the channels. This link is an important part of understanding the history of water on Mars. One way to address this is to study the rocks left behind in the chaotic terrains. The outcrop in this image is several kilometers across and light-toned. It has a slab-like appearance, with relatively steep edges and a flat top, although the top has many small knobs and spires. In places (see subimage), particularly along the west (left) edge of the main slab, it is clear that the light material is composed of many fine layers, which are eroding in a stepped fashion due to the variable resistance of the layers. The flat surface of the outcrop is partially coated with dark dust, obscuring its light tone. Along the edges, the outcrop is breaking into boulders and eroding away, but it is strong enough that it preserves steep slopes, particularly on the eastern edge. Away from the large slab, the image consists of hills and mounds characteristic of chaotic terrain. Little detail is visible on the mounds. The low areas have been partially covered by wind-blown sand or dust, forming the pervasive ripples seen in the image. Light material can be seen under the ripples in a few places, indicating that the light layered deposits extend farther than just the slab. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -4.0° Degrees longitude (East): 333.1° Range to target site: 269.1 km (168.2 miles) Original image scale range: 53.8 cm/pixel (with 2 x 2 binning) so objects ~162 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.0° Phase angle: 55.5° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 197.3°, 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 Deposits in Aureum C
…
PIA09656
Sol (our sun)
HiRISE
| Title |
Layered Deposits in Aureum Chaos |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002892_1760 [ http://hirise.lpl.arizona.edu/PSP_002892_1760 ]) shows an outcrop of a large slab of layered deposits in Aureum Chaos. "Chaotic" terrains on Mars are disorganized regions of blocks and large mounds which appear to have been produced by the collapse of pre-existing terrain. They are often associated with giant outflow channels, and they may have been the source of the water that carved the channels. This link is an important part of understanding the history of water on Mars. One way to address this is to study the rocks left behind in the chaotic terrains. The outcrop in this image is several kilometers across and light-toned. It has a slab-like appearance, with relatively steep edges and a flat top, although the top has many small knobs and spires. In places (see subimage), particularly along the west (left) edge of the main slab, it is clear that the light material is composed of many fine layers, which are eroding in a stepped fashion due to the variable resistance of the layers. The flat surface of the outcrop is partially coated with dark dust, obscuring its light tone. Along the edges, the outcrop is breaking into boulders and eroding away, but it is strong enough that it preserves steep slopes, particularly on the eastern edge. Away from the large slab, the image consists of hills and mounds characteristic of chaotic terrain. Little detail is visible on the mounds. The low areas have been partially covered by wind-blown sand or dust, forming the pervasive ripples seen in the image. Light material can be seen under the ripples in a few places, indicating that the light layered deposits extend farther than just the slab. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -4.0° Degrees longitude (East): 333.1° Range to target site: 269.1 km (168.2 miles) Original image scale range: 53.8 cm/pixel (with 2 x 2 binning) so objects ~162 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.0° Phase angle: 55.5° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 197.3°, 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. |
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Interior Layered Deposits in
…
PIA09655
Sol (our sun)
HiRISE
| Title |
Interior Layered Deposits in Juventae Chasma |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002946_1765 [ http://hirise.lpl.arizona.edu/PSP_002946_1765 ]) shows a portion of interior layered deposits (ILD) in Juventae Chasma. Juventae Chasma is a large depression near the equatorial canyon system Valles Marineris. The scene is along the top of a mound of layered deposits on the floor of Juventae Chasma. Dunes are seen in the low-lying, darker regions. Very fine layers are also seen (see subimage, approximately 1 km across). Understanding what kinds of materials formed the layers, how they were set in place, and how they have evolved will provide insight into Martian geologic history. Many of the Martian chasmata (plural of chasma) contain ILD like these. The ILD were deposited a long time ago, but the actual method is unknown. It has been suggested that sedimentary layers in standing bodies of water or volcanic ash deposits comprise the ILD. The alternating layers could indicate regular, repeating cycles of deposition. It is possible that these layers once covered the entire chasma floor. The IDL shown here have been modified by wind erosion. The yardangs seen near the top right of the image are evidence for wind sculpting of the deposits. It is interesting to note that there are very few craters in this scene, especially in the areas with visible layers. One crater can be found about half-way down the left side of the image amidst layers, and several craters are seen in the dark material on the right side of the image. This suggests that the ILD are eroding here fast enough to erase small craters before large numbers of them can accumulate. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:40 PM Degrees latitude (centered): -3.3° Degrees longitude (East): 298.3° Range to target site: 267.9 km (167.5 miles) Original image scale range: 26.8 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: 6.7° Phase angle: 61.6° Solar incidence angle: 55°, with the Sun about 35° above the horizon Solar longitude: 199.8°, 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. |
|
Interior Layered Deposits in
…
PIA09655
Sol (our sun)
HiRISE
| Title |
Interior Layered Deposits in Juventae Chasma |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002946_1765 [ http://hirise.lpl.arizona.edu/PSP_002946_1765 ]) shows a portion of interior layered deposits (ILD) in Juventae Chasma. Juventae Chasma is a large depression near the equatorial canyon system Valles Marineris. The scene is along the top of a mound of layered deposits on the floor of Juventae Chasma. Dunes are seen in the low-lying, darker regions. Very fine layers are also seen (see subimage, approximately 1 km across). Understanding what kinds of materials formed the layers, how they were set in place, and how they have evolved will provide insight into Martian geologic history. Many of the Martian chasmata (plural of chasma) contain ILD like these. The ILD were deposited a long time ago, but the actual method is unknown. It has been suggested that sedimentary layers in standing bodies of water or volcanic ash deposits comprise the ILD. The alternating layers could indicate regular, repeating cycles of deposition. It is possible that these layers once covered the entire chasma floor. The IDL shown here have been modified by wind erosion. The yardangs seen near the top right of the image are evidence for wind sculpting of the deposits. It is interesting to note that there are very few craters in this scene, especially in the areas with visible layers. One crater can be found about half-way down the left side of the image amidst layers, and several craters are seen in the dark material on the right side of the image. This suggests that the ILD are eroding here fast enough to erase small craters before large numbers of them can accumulate. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:40 PM Degrees latitude (centered): -3.3° Degrees longitude (East): 298.3° Range to target site: 267.9 km (167.5 miles) Original image scale range: 26.8 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: 6.7° Phase angle: 61.6° Solar incidence angle: 55°, with the Sun about 35° above the horizon Solar longitude: 199.8°, 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. |
|
Sand Dunes in Rabe Crater
PIA09717
Sol (our sun)
HiRISE
| Title |
Sand Dunes in Rabe Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002824_1355 [ http://hirise.lpl.arizona.edu/PSP_002824_1355 ]) shows a sand dune field in Rabe Crater. Rabe crater is approximately 100 km in diameter and is located in the southern highlands of Mars. The dune field within the crater has dimensions of roughly 50 km x 35 km, making it one of the largest dune fields in the region. It is composed mostly of barchanoid and transverse dunes that formed from uni-directional winds from the southeast. The sand grains are believed to be basalt, a common volcanic rock, that eroded from sedimentary units (made of eroded lava) exposed in a pit on the floor of Rabe Crater. The dark toned streaks seen on the dune slip face in the subimage are believed to form from grain-flow events, or sand avalanches, that occur when wind carries sand grains over the crest of the dune and deposits them on the slip face oversteepening the slope. When compared with older images, the identification of new streaks in HiRISE images could indicate that these dunes are still active today. Also seen in the subimage are smaller secondary dunes superimposed on the surface of the large dunes. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:50 PM Degrees latitude (centered): -44.0° Degrees longitude (East): 34.5° Range to target site: 252.6 km (157.8 miles) Original image scale range: 25.3 cm/pixel (with 1 x 1 binning) so objects ~76 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.2° Phase angle: 67.7° Solar incidence angle: 63°, with the Sun about 27° above the horizon Solar longitude: 194.2°, 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. |
|
Sand Dunes in Rabe Crater
PIA09717
Sol (our sun)
HiRISE
| Title |
Sand Dunes in Rabe Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002824_1355 [ http://hirise.lpl.arizona.edu/PSP_002824_1355 ]) shows a sand dune field in Rabe Crater. Rabe crater is approximately 100 km in diameter and is located in the southern highlands of Mars. The dune field within the crater has dimensions of roughly 50 km x 35 km, making it one of the largest dune fields in the region. It is composed mostly of barchanoid and transverse dunes that formed from uni-directional winds from the southeast. The sand grains are believed to be basalt, a common volcanic rock, that eroded from sedimentary units (made of eroded lava) exposed in a pit on the floor of Rabe Crater. The dark toned streaks seen on the dune slip face in the subimage are believed to form from grain-flow events, or sand avalanches, that occur when wind carries sand grains over the crest of the dune and deposits them on the slip face oversteepening the slope. When compared with older images, the identification of new streaks in HiRISE images could indicate that these dunes are still active today. Also seen in the subimage are smaller secondary dunes superimposed on the surface of the large dunes. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:50 PM Degrees latitude (centered): -44.0° Degrees longitude (East): 34.5° Range to target site: 252.6 km (157.8 miles) Original image scale range: 25.3 cm/pixel (with 1 x 1 binning) so objects ~76 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.2° Phase angle: 67.7° Solar incidence angle: 63°, with the Sun about 27° above the horizon Solar longitude: 194.2°, 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. |
|
Sand Dunes in Rabe Crater
PIA09717
Sol (our sun)
HiRISE
| Title |
Sand Dunes in Rabe Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002824_1355 [ http://hirise.lpl.arizona.edu/PSP_002824_1355 ]) shows a sand dune field in Rabe Crater. Rabe crater is approximately 100 km in diameter and is located in the southern highlands of Mars. The dune field within the crater has dimensions of roughly 50 km x 35 km, making it one of the largest dune fields in the region. It is composed mostly of barchanoid and transverse dunes that formed from uni-directional winds from the southeast. The sand grains are believed to be basalt, a common volcanic rock, that eroded from sedimentary units (made of eroded lava) exposed in a pit on the floor of Rabe Crater. The dark toned streaks seen on the dune slip face in the subimage are believed to form from grain-flow events, or sand avalanches, that occur when wind carries sand grains over the crest of the dune and deposits them on the slip face oversteepening the slope. When compared with older images, the identification of new streaks in HiRISE images could indicate that these dunes are still active today. Also seen in the subimage are smaller secondary dunes superimposed on the surface of the large dunes. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:50 PM Degrees latitude (centered): -44.0° Degrees longitude (East): 34.5° Range to target site: 252.6 km (157.8 miles) Original image scale range: 25.3 cm/pixel (with 1 x 1 binning) so objects ~76 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.2° Phase angle: 67.7° Solar incidence angle: 63°, with the Sun about 27° above the horizon Solar longitude: 194.2°, 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. |
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Fans of Lava Flows on the Fl
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PIA09716
Sol (our sun)
HiRISE
| Title |
Fans of Lava Flows on the Flanks of Olympus Mons |
| Original Caption Released with Image |
Click on image for larger version Olympus Mons, the largest volcano in the Solar System is covered by lava flows. Most of these lava flows carried the liquid lava in open streams which geologists call channels. In some places these channels break down and the lava spreads across a broad area, like a fan. In the center of this HiRISE image (PSP_002909_2000 [ http://hirise.lpl.arizona.edu/PSP_002909_2000 ]), you can see the transition from well-confined lava channels into broad fans as the lava flowed down to the north. When viewed at full-resolution, the HiRISE image shows a fuzzy pitted surface. This is caused by a thick layer of very small particles that are being moved around by the wind. It is not clear at this point in time whether these particles are predominantly dust deposited from the global dust storms or if they are mostly volcanic ash. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:38 PM Degrees latitude (centered): 19.7° Degrees longitude (East): 226.1° Range to target site: 263.0 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: 0.2° Phase angle: 60.3° Solar incidence angle: 60°, with the Sun about 30° above the horizon Solar longitude: 198.1°, 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. |
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Fans of Lava Flows on the Fl
…
PIA09716
Sol (our sun)
HiRISE
| Title |
Fans of Lava Flows on the Flanks of Olympus Mons |
| Original Caption Released with Image |
Click on image for larger version Olympus Mons, the largest volcano in the Solar System is covered by lava flows. Most of these lava flows carried the liquid lava in open streams which geologists call channels. In some places these channels break down and the lava spreads across a broad area, like a fan. In the center of this HiRISE image (PSP_002909_2000 [ http://hirise.lpl.arizona.edu/PSP_002909_2000 ]), you can see the transition from well-confined lava channels into broad fans as the lava flowed down to the north. When viewed at full-resolution, the HiRISE image shows a fuzzy pitted surface. This is caused by a thick layer of very small particles that are being moved around by the wind. It is not clear at this point in time whether these particles are predominantly dust deposited from the global dust storms or if they are mostly volcanic ash. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:38 PM Degrees latitude (centered): 19.7° Degrees longitude (East): 226.1° Range to target site: 263.0 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: 0.2° Phase angle: 60.3° Solar incidence angle: 60°, with the Sun about 30° above the horizon Solar longitude: 198.1°, 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. |
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