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Changes near the Volcano Lok
…
PIA00710
Jupiter
Solid-State Imaging
| Title |
Changes near the Volcano Loki Patera on Io |
| Original Caption Released with Image |
Four views of the volcano Loki Patera on Jupiter's moon Io showing changes seen on June 27th, 1996 by the Galileo spacecraft as compared to views seen by the Voyager spacecraft during the 1979 flybys. Clockwise from upper left is a Voyager 1 high resolution image, a Voyager 1 color image, a Galileo color image, and a Voyager 2 color image. North is to the top of the picture. During the Voyager flybys large dense volcanic plumes erupting from each end of the dark linear "fissure" to the northeast of the dark caldera and plume deposits obscured much of the surrounding surface. These dark jets are not visible in the Galileo image, and other images have confirmed that the Loki plumes were inactive during this Galileo encounter. Ground-based observers have determined that the Loki hot spot, historically the most energetic on Io, has been unusually dim. The fissure appears extended and elongated to the east and southwest, perhaps also resulting in a migration of the plume vents. There is an enlarged dark spot to the west of Loki. The materials just south and northeast of the caldera appear more reddish color. Images are 894 km wide. The Jet Propulsion Laboratory, Pasadena, CA manages the mission for NASA's Office of Space Science, Washington, DC. This image and other images and data received from Galileo are posted on the World Wide Web, on the Galileo mission home page at URL http://galileo.jpl.nasa.gov. Background information and educational context for the images can be found at URL http://www.jpl.nasa.gov/galileo/sepo |
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Massive Resurfacing of the I
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PIA00709
Jupiter
Solid-State Imaging
| Title |
Massive Resurfacing of the Ionian Volcano Ra Patera |
| Original Caption Released with Image |
Four views of the volcano Ra Patera on Jupiter's moon Io showing changes seen on June 27th, 1996 by the Galileo spacecraft as compared to views seen by the Voyager spacecraft during the 1979 flybys. Clockwise from upper left is a Voyager 1 high resolution image, a Voyager 1 color image, a Galileo color image, and a Voyager 2 color image. North is to the top of the picture. Observations obtained by J. Spencer and others with the Hubble Space Telescope had indicated a major change in recent years. The Galileo images reveal the detailed morphology of new deposits. Dark materials, previously confined to a summit caldera, appear to have overflowed the caldera walls to produce a small flow to the south and a larger flow to the southeast. New bright deposits covering an area of about 40,000 square kilometers (the size of New Jersey) surround the dark materials. The morphology of the bright materials suggests emplacement as lava flows rather than pyroclastics. Notice the lobate margins and how the bright materials embay a plateau in the upper left. The Voyager 1 images also reveal relatively bright lava flows emanating from Ra Patera, especially to the northeast. The colors of the flows match those of sulfur plus SO2 frost. Images are 953 km wide. The Jet Propulsion Laboratory, Pasadena, CA manages the mission for NASA's Office of Space Science, Washington, DC. This image and other images and data received from Galileo are posted on the World Wide Web, on the Galileo mission home page at URL http://galileo.jpl.nasa.gov. Background information and educational context for the images can be found at URL http://www.jpl.nasa.gov/galileo/sepo |
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Valleys on Northwest Flank o
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PIA01679
Sol (our sun)
Mars Orbiter Camera
| Title |
Valleys on Northwest Flank of Alba Patera Volcano |
| Original Caption Released with Image |
In 1972, Mariner 9 images revealed a variety of branched and networked valleys on Alba Patera, a volcano in northern Tharsis. Since then, the question has always been, "what made these valleys, water or lava?" Because the Alba Patera volcano was considered to be a relatively young feature on Mars, it seemed that if waterways involved in the formation of the valleys, then it would imply that liquid water flowed on this part of Mars at a relatively recent time in the planet's history. Thus, it was hoped that Mars Global Surveyor (MGS), with its super-high resolution Mars Orbiter Camera (MOC), would help answer this key question about evidence for past water on the red planet. However, when MOC peered down upon these valleys it became clear that the camera might not help answer the question of their origin. As the picture above shows, these valleys--which trend from lower right to upper left in the picture--are old and have been cut by younger faults that created graben--e.g., the wide, straight valley running diagonally from upper right to lower left. Worse, the close-up views revealed that the valleys are covered up by a lumpy-textured material that also partly fills nearby impact craters. The origin of the textured material is unknown but might result from years and years of wind erosion of surface "soil" or volcanic ash. However it formed, this covering obscures so much of the details of the valleys that high resolution pictures are unlikely to solve this mystery. The picture above covers an area approximately 8 kilometers (5 miles) wide by 15 kilometers (9 miles) high. Illumination is from the right. The picture was acquired in August 1998 during the MGS Science Phasing Orbits imaging campaign, and was presented at the 30th Lunar and Planetary Science Conference in Houston, Texas, March 1999. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Lower Northeastern Flank of
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PIA02012
Sol (our sun)
Mars Orbiter Camera
| Title |
Lower Northeastern Flank of Tyrrhena Patera |
| Original Caption Released with Image |
Tyrrhenna Patera is thought to be an ancient volcano. It is located in Hesperia Planum in the martian southern hemisphere. The Mars Orbiter Camera recently acquired this view of escarpments and valleys on the lower northeast flank of the volcano. Small, bright dunes cover low areas such as valley and crater floors. The picture is illuminated from the lower right and covers an area 3 kilometers (1.9 miles) across. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Apollinaris Patera, Mars
PIA02006
Sol (our sun)
Mars Orbiter Camera
| Title |
Apollinaris Patera, Mars |
| Original Caption Released with Image |
This month (April 1999), the Mars Global Surveyor Mars Orbiter Camera (MOC) passed over the Apollinaris Patera volcano and captured a patch of bright clouds hanging over its summit in the early martian afternoon. This ancient volcano is located near the equator and--based on observations from the 1970s Viking Orbiters--is thought to be as much as 5 kilometers (3 miles) high. The caldera--the semi-circular crater at the volcano summit--is about 80 kilometers (50 miles) across. The color in this picture was derived from the MOC red and blue wide angle camera systems and does not represent true color as it would appear to the human eye (that is, if a human were in a position to be orbiting around the red planet). Illumination is from the upper left. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Amphitrites Patera
PIA00410
Sol (our sun)
| Title |
Amphitrites Patera |
| Original Caption Released with Image |
A color image of the Amphitrites Patera region of Mars, north toward top. The scene shows several indistinct ring structures and radial ridges of an old volcano named Amphitrites Patera. A patera (Latin for shallow dish or saucer) is a volcano of broad areal extent with little vertical relief. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 55 degrees S. to 62 degrees S. and from longitude 292 degrees to 311 degrees, Lambert projection. Amphitrites Patera is a 138-km-diameter feature on the south rim of Hellas impact basin and is one of many indistinct ring structures in the area. The location of the paterae in this area of Hellas indicates that their source magma may have been influenced by the transition fractures of the basin. The radial ridges of Amphitrites extend for about 400 km north into the Hellas basin. |
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Apollinaris Patera
PIA00411
Sol (our sun)
| Title |
Apollinaris Patera |
| Original Caption Released with Image |
A color image of the Apollinaris Patera Region of Mars, north toward top. The scene shows the 80-km-wide central caldera of Apollinaris, a plume of young flows extending south down the flank of the volcano, a cliff and chaotic terrain west of the volcano, and the surrounding younger deposits of the Medusae Fossae Formation (north and east). A patera (Latin for shallow dish or saucer) is a volcano of broad areal extent with little vertical relief. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 12 degrees S. to 6 degrees S. and from longitude 182 degrees to 189 degrees, Mercator projection. Apollinaris Patera is an isolated volcano (about 400 km across) lying on the Martian highlands just north of Gusev impact crater and the termination of Ma'adim Vallis. After the main edifice was built, eruption continued on the volcano's southern flank to form a broad ridge overlapping the original shield. Breakdown of ice-rich materials formed chaos on its western edge. Finally the friable materials (possible ash?) of the Medusae Fossae Fm were deposited. |
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Hadriaca Patera
PIA00415
Sol (our sun)
| Title |
Hadriaca Patera |
| Original Caption Released with Image |
A color image of Hadriaca Patera on the northeast rim of Hellas basin of Mars, north toward top. The scene shows a central circular depression surrounded by low radial ridges and, at the bottom of the image, the channel of Dao Vallis. A patera (Latin for shallow dish or saucer) is a volcano of broad areal extent with little vertical relief. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 27 degrees S. to 37 degrees S. and from longitude 263 degrees to 273 degrees, Mercator projection. Hadriaca Patera is less than 2 km high, has a 60-km-diameter caldera at its center, and is surrounded by a 300-km-wide ring of low ridges. The radial ridges may be lava flows with lava channels at their crests. South of Hadriaca, Dao Vallis begins at a steep-walled depression 40 km across but forms a much shallower channel that extends 800 km southwest into the floor of the Hellas basin. The channel is very likely fluvial in origin, with the release of water being triggered by volcanic activity. |
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Alba Patera
PIA00409
Sol (our sun)
| Title |
Alba Patera |
| Original Caption Released with Image |
A color image of the Alba Patera region of Mars, north toward top. The scene shows a central circular depression surrounded by splays of fractures, named Alba Fossae (west of Alba Patera) and Tantalus Fossae (east of Alba Patera). A patera (Latin for shallow dish or saucer) is a volcano of broad areal extent with little vertical relief, a fossa is a linear depression. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 30 degrees N. to 50 degrees N. and from longitude 95 degrees to 125 degrees, Lambert projection. Alba Patera has a 100-km-diameter caldera at its center surrounded by a fracture ring. In total, the approximately 1,200- km-diameter Alba Patera far exceeds any other known volcano in areal extent, it covers eight times the area of Olympus Mons (the highest volcano in the Solar System) but reaches only about 6 km in height. The patera lies directly north of the Tharsis bulge, which encompasses the most intensely and most recently active volcanic region of the planet. The fossae of the Alba area are fault-bound graben that can be traced south through the Tharsis bulge and therefore likely formed by upwarping of the Tharsis bulge as well as the coeval upwelling of Alba Pateria magma. |
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Tyrrhena Patera
PIA00421
Sol (our sun)
| Title |
Tyrrhena Patera |
| Original Caption Released with Image |
A color image of the Tyrrhena Patera Region of Mars, north toward top. The scene shows a central circular depression surrounded by circular fractures and highly dissected horizontal sheets. A patera (Latin for shallow dish or saucer) is a volcano of broad areal extent with little vertical relief. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 17 degrees S. to 25 degrees S. and from longitude 250 degrees to 260 degrees, Mercator projection. Tyrrhena Patera has a 12-km-diameter caldera at its center surrounded by a 45-km-diameter fracture ring. Around the fracture ring, the terrain is highly eroded forming ragged outward-facing cliffs, as though successive flat-lying layers had been eroded back. Cut into the sequence are several flat-floored channels that extend outward as far as 200 km from the center of the volcano. The structure may be composed of highly erodible ash layers and the channels may be fluvial, with the release of water being triggered by volcanic activity (Carr, 1981, The surface of Mars, Yale Univ. Press, New Haven, 232 p.). |
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Alba Patera
PIA05023
Sol (our sun)
Mars Orbiter Camera
| Title |
Alba Patera |
| Original Caption Released with Image |
28 December 2003 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) red wide angle image shows much of Alba Patera, a low, broad shield volcano in northern Tharsis. The caldera complex--the pits formed by collapse at the volcano summit -- is located toward the bottom center of this image. Alba Patera is located at 41°N, 111°W. The area shown here is approximately 430 km (~270 mi) across and illuminated from the lower left. |
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Recent Eruption at Gish Bar
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PIA03884
Jupiter
Solid-State Imaging
| Title |
Recent Eruption at Gish Bar Patera on Io |
| Original Caption Released with Image |
This image taken by NASA's Galileo spacecraft reveals fresh lava in a wide pit named Gish Bar Patera on Jupiter's moon Io. The patera, or depression, is quite large: 106.3 kilometers (66 miles) by 115.0 kilometers (71 miles). Galileo has detected volcanic activity at this site in the past, particularly in late 1996. Galileo took this image on Oct. 16, 2001, during its 32nd orbit of Jupiter. Effects of a new eruption at Gish Bar can be seen in a comparison with images from 1999 (see figure below). The new eruption was first detected in infrared imaging by Galileo's near-infrared mapping spectrometer in August 2001. This visible-light image shows a pair of new lava flows. The largest runs to the western boundary and extends to the central and northern portions of the patera. The other flow corresponds to a secondary depression in the southeastern portion of the patera. Based on changes seen at this depression between July and October 1999, this is thought to be the site of an outburst seen by Earth-based observers in August 1999. Gish Bar Patera lies at the base of an 11-kilometer (36,000-foot) mountain at 15.6 degrees north latitude, 89.1 degrees west longitude on Io. This image was taken from a distance of 25,000 kilometers (15,500 miles) and has a resolution of 250 meters (820 feet) per pixel. The Sun is straight behind the observer, an illumination angle that minimizes shadows and emphasizes inherent brightness variations rather than topography. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Galileo mission for NASA's Office of Space Science, Washington, D.C. Additional information about Galileo and its discoveries is available on the Galileo mission home page at http://galileo.jpl.nasa.gov [ http://galileo.jpl.nasa.gov ]. Background information and educational context for the images can be found at http://galileo.jpl.nasa.gov/gallery/io.cfm [ http://galileo.jpl.nasa.gov/gallery/io.cfm ]. |
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Recent Eruption at Gish Bar
…
PIA03884
Jupiter
Solid-State Imaging
| Title |
Recent Eruption at Gish Bar Patera on Io |
| Original Caption Released with Image |
This image taken by NASA's Galileo spacecraft reveals fresh lava in a wide pit named Gish Bar Patera on Jupiter's moon Io. The patera, or depression, is quite large: 106.3 kilometers (66 miles) by 115.0 kilometers (71 miles). Galileo has detected volcanic activity at this site in the past, particularly in late 1996. Galileo took this image on Oct. 16, 2001, during its 32nd orbit of Jupiter. Effects of a new eruption at Gish Bar can be seen in a comparison with images from 1999 (see figure below). The new eruption was first detected in infrared imaging by Galileo's near-infrared mapping spectrometer in August 2001. This visible-light image shows a pair of new lava flows. The largest runs to the western boundary and extends to the central and northern portions of the patera. The other flow corresponds to a secondary depression in the southeastern portion of the patera. Based on changes seen at this depression between July and October 1999, this is thought to be the site of an outburst seen by Earth-based observers in August 1999. Gish Bar Patera lies at the base of an 11-kilometer (36,000-foot) mountain at 15.6 degrees north latitude, 89.1 degrees west longitude on Io. This image was taken from a distance of 25,000 kilometers (15,500 miles) and has a resolution of 250 meters (820 feet) per pixel. The Sun is straight behind the observer, an illumination angle that minimizes shadows and emphasizes inherent brightness variations rather than topography. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Galileo mission for NASA's Office of Space Science, Washington, D.C. Additional information about Galileo and its discoveries is available on the Galileo mission home page at http://galileo.jpl.nasa.gov [ http://galileo.jpl.nasa.gov ]. Background information and educational context for the images can be found at http://galileo.jpl.nasa.gov/gallery/io.cfm [ http://galileo.jpl.nasa.gov/gallery/io.cfm ]. |
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Major Martian Volcanoes from
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PIA02803
Sol (our sun)
MOLA
| Title |
Major Martian Volcanoes from MOLA - Alba Patera |
| Original Caption Released with Image |
Two views of Alba Patera with topography draped over a Viking image mosaic. MOLA data have clarified the relationship between fault location and topography on and surrounding the Alba construct, providing insight into the volcanological and geophysical processes that shaped the edifice. The vertical exaggeration is 10:1. |
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Tyrrhena Patera
PIA06946
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Tyrrhena Patera |
| Original Caption Released with Image |
This week we will be examining images of Tyrrhena Patera and its surroundings. Tyrrhena Patera is one of several moderate sized volcanoes located in the Martian southern highlands. While the volcanic edifice is only moderate in size (when compared to the larger Tharsis volcanoes), the surrounding volcanic materials cover an extensive area. Deep eroded channels on the slope of the volcano indicate that the volcano itself is likely composed of pyroclastic materials rather than flow materials. Image information: IR instrument. Latitude -21.8, Longitude 106.4 East (253.6 West). 100 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Alba Patera Valleys
PIA06965
Sol (our sun)
Mars Orbiter Camera
| Title |
Alba Patera Valleys |
| Original Caption Released with Image |
24 October 2004 The northwest flanks of the broad, northern Tharsis volcano, Alba Patera, have been known since the 1970s to exhibit a plethora of what appeared to be branching valley networks running down the volcano slopes. Some investigators suggested that these valleys were evidence for precipitation and runoff of liquid water on the volcano flanks. It was hoped that high resolution images from the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) would provide new details that would confirm or refute the hypothesis. The problem is, MGS MOC images instead showed a surface largely covered by an eroded, rough-textured mantle that obscured the valley floors. The images, such as the one shown here, also showed that the valleys are discontinuous and indistinct when viewed at high resolution (although, when shrunk to fit within the reduced-scale view on this web page, they may seem continuous -- click on the image to view the full-scale picture). The valleys in the lower quarter of this image have been cut by a fault. This image is located on Alba Patera near 45.8°N, 111.8°W. The image covers an area about 3 km (1.9 mi) wide. Sunlight illuminates the scene from the lower left. |
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NIMS Observes Increased Acti
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PIA00856
Jupiter
Near Infrared Mapping Spectr
…
| Title |
NIMS Observes Increased Activity at Loki Patera, Io |
| Original Caption Released with Image |
Loki Patera, historically the most active and persistent hot spot on Io, is located on the hemisphere of Io always facing Jupiter. Loki Patera was the site of two plumes during the Voyager encounters, which were not seen during the early orbits of Galileo. Ground-based observers reported Loki Patera to be unusually dim during this time, marking a period of low volcanic activity. On 21 February 1997, during Galileo's sixth orbit, the Near Infrared Mapping Spectrometer (NIMS) on the Galileo spacecraft observed Io in daylight from a range of approximately 703,000 km (440,000 miles). The image on the left shows Io at a wavelength of 2.95 microns. Loki Patera is seen to be relatively quiescent (at longer wavelengths which are more sensitive to thermal emission, Loki Patera is more noticeable). A few weeks later, on March 12th 1997, ground based observers using the Infra-Red Telescope Facility (IRTF) on Mauna Kea, Hawaii, observed an intense brightening in the Loki region, so much that Loki was contributing 75% of Io's in-eclipse flux for this hemisphere. A large eruption was taking place! Other ground-based observations through March, April and May tracked the course of the activity and confirmed its location at Loki Patera. On 4 April 1997, NIMS again observed Io during the seventh orbit from a range of 556,000 km (348,000 miles), with Loki Patera positioned in darkness, close to the limb. The image on the right shows the increase in activity at Loki Patera, again at 2.95 microns. A preliminary single temperature fit to NIMS orbit seven Loki Patera hot spot data yields a temperature of 500 K and an area of over 800 square kilometers. That the image is so bright at this wavelength is an indication of the areal extent of the activity. It is also probable that some part of the volcanic material being erupted or exposed is at considerably higher temperatures than that of the 500 K single-temperature fit. Io is under observation by ground-based observers under the auspices of the International Jupiter Watch, which has a web site at http://www.lowell.edu/users/ijw/ijwhome.html The Jet Propulsion Laboratory, Pasadena, CA manages the mission for NASA's Office of Space Science, Washington, DC. This image and other images and data received from Galileo are posted on the World Wide Web, on the Galileo mission home page at URL http://galileo.jpl.nasa.gov. |
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Hadriaca Patera
PIA03798
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Hadriaca Patera |
| Original Caption Released with Image |
(Released 17 May 2002) The Science Although the largest volcanoes on Mars (and the solar system) are located in the geologically young Tharsis region, there are many other martian volcanoes that display equally interesting features, such as Hadriaca Patera, shown in this image. Hadriaca Patera is located to the northeast of the Hellas Planitia impact basin in the southern hemisphere. Unlike the Tharsis volcanoes, Hadriaca Patera has very low relief, standing only about 1-2 km above the surrounding plains. Many scientists believe that Hadriaca Patera and other patera volcanoes (e.g., Tyrrhena) had significant interaction with subsurface water that produced mostly explosive ash deposits (pyroclastic flows), rather than just lava flows. Nearby sources of water might have included Dao Vallis on the southern flank of the volcano. The upper portion of this image shows relatively smooth terrain located in the central caldera, which has been nearly filled in with late-stage lava flows. The lower half of the image shows lobate flows as well as furrows in the ash deposits that make up the volcano's southern flank, these erosional furrows may have formed by surface runoff or sapping by groundwater. Just below the center of the image, a few small sinuous troughs are visible, and may be collapsed lava tubes or collapse features related to subsurface water. The number of impact craters on a planetary surface is commonly used as a proxy for the age of the surface -- an old surface has had time to accumulate more craters than a young surface. The relatively small number of large craters in the image indicates that the surface in this area is younger than the nearby heavily cratered ancient terrains outside the Hellas basin, but there are more craters on this surface than would be found on the average volcanic surface in Tharsis (there are some very large old craters on the volcano's flank to the southeast of this image). Paterae in general are older than the Tharsis volcanoes. At the far right edge of the central portion of the image, an ovoid-shaped crater is visible. Such craters are believed to form by extremely low-angle impact events. The Story If you look at the context image to the right, you'll see a large round circle. That's the ancient mouth of the volcano, not a crater. This volcano is named Hadriaca Patera. Even though Mars is known as the home of the largest volcanoes in the solar system, this mile-high volcano isn't very tall compared to its cousins in a region of Mars called Tharsis. As a result, you might think that paterae volcanoes like this one are relatively undistinguished as Martian volcanoes go, but it turns out they are probably much older. The number of craters on the surface in the area tells us so. Older surfaces have had time to accumulate many more craters. Not all craters, however, are almost perfectly round. Look for the egg-shaped crater (far right edge of the central portion of the image). Crater shapes like this one are, caused when an impacting body comes in toward the surface at an extremely low angle. More than being older, paterae volcanoes are really interesting to scientists because they may have interacted with subsurface water. With that "ingredient," these volcanoes spat out explosive ash deposits instead of just lava flows. Mars may look calm now, but wow! It sure wasn't in the past. There are many signs of the volcano's past activity. In the upper portion of the image, the mouth of the volcano has been filled in with late-stage lava flows. Down below, a layering of flows is further scored with erosional furrows formed either by surface runoff or when groundwater eroded the surface from underneath, causing it to sink. Near the center of the image, collapsed lava tubes (or other collapse features related to subsurface water) texture the surface as well. |
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Hadriaca Patera
PIA03798
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Hadriaca Patera |
| Original Caption Released with Image |
(Released 17 May 2002) The Science Although the largest volcanoes on Mars (and the solar system) are located in the geologically young Tharsis region, there are many other martian volcanoes that display equally interesting features, such as Hadriaca Patera, shown in this image. Hadriaca Patera is located to the northeast of the Hellas Planitia impact basin in the southern hemisphere. Unlike the Tharsis volcanoes, Hadriaca Patera has very low relief, standing only about 1-2 km above the surrounding plains. Many scientists believe that Hadriaca Patera and other patera volcanoes (e.g., Tyrrhena) had significant interaction with subsurface water that produced mostly explosive ash deposits (pyroclastic flows), rather than just lava flows. Nearby sources of water might have included Dao Vallis on the southern flank of the volcano. The upper portion of this image shows relatively smooth terrain located in the central caldera, which has been nearly filled in with late-stage lava flows. The lower half of the image shows lobate flows as well as furrows in the ash deposits that make up the volcano's southern flank, these erosional furrows may have formed by surface runoff or sapping by groundwater. Just below the center of the image, a few small sinuous troughs are visible, and may be collapsed lava tubes or collapse features related to subsurface water. The number of impact craters on a planetary surface is commonly used as a proxy for the age of the surface -- an old surface has had time to accumulate more craters than a young surface. The relatively small number of large craters in the image indicates that the surface in this area is younger than the nearby heavily cratered ancient terrains outside the Hellas basin, but there are more craters on this surface than would be found on the average volcanic surface in Tharsis (there are some very large old craters on the volcano's flank to the southeast of this image). Paterae in general are older than the Tharsis volcanoes. At the far right edge of the central portion of the image, an ovoid-shaped crater is visible. Such craters are believed to form by extremely low-angle impact events. The Story If you look at the context image to the right, you'll see a large round circle. That's the ancient mouth of the volcano, not a crater. This volcano is named Hadriaca Patera. Even though Mars is known as the home of the largest volcanoes in the solar system, this mile-high volcano isn't very tall compared to its cousins in a region of Mars called Tharsis. As a result, you might think that paterae volcanoes like this one are relatively undistinguished as Martian volcanoes go, but it turns out they are probably much older. The number of craters on the surface in the area tells us so. Older surfaces have had time to accumulate many more craters. Not all craters, however, are almost perfectly round. Look for the egg-shaped crater (far right edge of the central portion of the image). Crater shapes like this one are, caused when an impacting body comes in toward the surface at an extremely low angle. More than being older, paterae volcanoes are really interesting to scientists because they may have interacted with subsurface water. With that "ingredient," these volcanoes spat out explosive ash deposits instead of just lava flows. Mars may look calm now, but wow! It sure wasn't in the past. There are many signs of the volcano's past activity. In the upper portion of the image, the mouth of the volcano has been filled in with late-stage lava flows. Down below, a layering of flows is further scored with erosional furrows formed either by surface runoff or when groundwater eroded the surface from underneath, causing it to sink. Near the center of the image, collapsed lava tubes (or other collapse features related to subsurface water) texture the surface as well. |
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Alba Patera
PIA03774
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera |
| Original Caption Released with Image |
(Released 22 April 2002) The Science This image, centered near 46.5 N and 119.3 W (240.7 E), is on the northwestern flank of a large, broad shield volcano called Alba Patera. This region of Mars has a number of unique valley features that at first glance look dendritic much in the same pattern that rivers and tributaries form on Earth. A closer look reveals that the valleys are quite discontinuous and must form through a different process than surface runoff of liquid water that is common on Earth. A number of processes might have taken place at some point in the Martian past to form these features. Some of the broad valley features bear some resemblance to karst topography, where material is removed underground by melting or dissolving in groundwater causing the collapse of the surface above it. The long narrow valleys resemble surfaces where groundwater sapping has occurred. Sapping happens when groundwater reaches the surface and causes headward erosion, forming long valleys with fewer tributaries than is seen with valleys formed by surface water runoff. The volcano itself might have been a source of heat and energy, which played a role in producing surfaces that indicate an active groundwater system. The Story Fluid, oozing lava poured somewhat lazily over this area long ago. It happened perhaps thousands of times, over hundreds of thousands of Martian years, creating the nearly smooth, plaster-of-Paris-looking terrain seen today. (Small craters also dent the area, though they may deceive you and look like raised bumps instead. That's just a trick of the eye and the lighting - tilt your head to your left shoulder, and you should see the craters pit the surface as expected.) The lava flows came from a Martian "shield" volcano named Alba Patera. Shield volcanoes get their name from their appearance: from above, they look like large battle shields lying face up to the sky as if a giant, geological warrior had lain them down. Perhaps one did if you think of a volcano as a "geologic warrior," that is. These volcanoes aren't too fierce, however. Because of the gentle layering of lava over time, they don't stand tall and angry against the horizon, but instead have relatively gentle slopes and are spread out over large areas. (On Earth, the Hawaiian Islands are examples of shield volcanoes, but you can't see much of their expanse, since they rise almost three miles from the ocean floor before popping out above the water's surface.) What's most interesting in this picture are all of the branching features that lightly texture the terrain. The patterns may look like those caused by rivers here on Earth, but geologists say that no surface streams on Mars were responsible. That's no disappointment, however, to those who'd like to find water on Mars, because there are still intriguing water-related possibilities here. Some of the broad valley features in this image look like karsts, a terrain found on Earth in Karst, a limestone area on the Adriatic, Sea in modern-day Croatia, and in other world regions including France, China, the American Midwest, Kentucky, and Florida. Karst terrain on Earth is barren land with all kinds of caves, sinkholes, and underground rivers that excavate the subsurface, causing the surface above it to collapse. So, perhaps it's like that in this region on Mars as well. Future Martian spelunkers should be excited, because most caves on Earth are in karst areas. Other suggestions of water here are some long, narrow valleys that resemble Earth surfaces where groundwater has sapped away the terrain. Sapping occurs when groundwater erodes slopes, creating valleys. Water action can be concentrated at valley heads, leading to what is called their "headward growth." That may be what has happened here on Alba Patera as well. All of these features suggest the action of liquid water, but Mars is so cold, you might wonder if any water would have to be as frozen as the world it is on. Well . . . that depends! Remember that this area is part of a volcano, and volcanoes can put out enough heat and energy below the surface to keep water warm enough to flow - if not now, then at least in the past when the volcano was more active. |
|
Alba Patera
PIA03774
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera |
| Original Caption Released with Image |
(Released 22 April 2002) The Science This image, centered near 46.5 N and 119.3 W (240.7 E), is on the northwestern flank of a large, broad shield volcano called Alba Patera. This region of Mars has a number of unique valley features that at first glance look dendritic much in the same pattern that rivers and tributaries form on Earth. A closer look reveals that the valleys are quite discontinuous and must form through a different process than surface runoff of liquid water that is common on Earth. A number of processes might have taken place at some point in the Martian past to form these features. Some of the broad valley features bear some resemblance to karst topography, where material is removed underground by melting or dissolving in groundwater causing the collapse of the surface above it. The long narrow valleys resemble surfaces where groundwater sapping has occurred. Sapping happens when groundwater reaches the surface and causes headward erosion, forming long valleys with fewer tributaries than is seen with valleys formed by surface water runoff. The volcano itself might have been a source of heat and energy, which played a role in producing surfaces that indicate an active groundwater system. The Story Fluid, oozing lava poured somewhat lazily over this area long ago. It happened perhaps thousands of times, over hundreds of thousands of Martian years, creating the nearly smooth, plaster-of-Paris-looking terrain seen today. (Small craters also dent the area, though they may deceive you and look like raised bumps instead. That's just a trick of the eye and the lighting - tilt your head to your left shoulder, and you should see the craters pit the surface as expected.) The lava flows came from a Martian "shield" volcano named Alba Patera. Shield volcanoes get their name from their appearance: from above, they look like large battle shields lying face up to the sky as if a giant, geological warrior had lain them down. Perhaps one did if you think of a volcano as a "geologic warrior," that is. These volcanoes aren't too fierce, however. Because of the gentle layering of lava over time, they don't stand tall and angry against the horizon, but instead have relatively gentle slopes and are spread out over large areas. (On Earth, the Hawaiian Islands are examples of shield volcanoes, but you can't see much of their expanse, since they rise almost three miles from the ocean floor before popping out above the water's surface.) What's most interesting in this picture are all of the branching features that lightly texture the terrain. The patterns may look like those caused by rivers here on Earth, but geologists say that no surface streams on Mars were responsible. That's no disappointment, however, to those who'd like to find water on Mars, because there are still intriguing water-related possibilities here. Some of the broad valley features in this image look like karsts, a terrain found on Earth in Karst, a limestone area on the Adriatic, Sea in modern-day Croatia, and in other world regions including France, China, the American Midwest, Kentucky, and Florida. Karst terrain on Earth is barren land with all kinds of caves, sinkholes, and underground rivers that excavate the subsurface, causing the surface above it to collapse. So, perhaps it's like that in this region on Mars as well. Future Martian spelunkers should be excited, because most caves on Earth are in karst areas. Other suggestions of water here are some long, narrow valleys that resemble Earth surfaces where groundwater has sapped away the terrain. Sapping occurs when groundwater erodes slopes, creating valleys. Water action can be concentrated at valley heads, leading to what is called their "headward growth." That may be what has happened here on Alba Patera as well. All of these features suggest the action of liquid water, but Mars is so cold, you might wonder if any water would have to be as frozen as the world it is on. Well . . . that depends! Remember that this area is part of a volcano, and volcanoes can put out enough heat and energy below the surface to keep water warm enough to flow - if not now, then at least in the past when the volcano was more active. |
|
Dusty Top of Alba Patera Vol
…
PIA09395
Sol (our sun)
HiRISE
| Title |
Dusty Top of Alba Patera Volcano |
| Original Caption Released with Image |
This HiRISE image shows a small portion of the rim of the caldera at the top of the volcano Alba Patera. This volcano has shallower slopes than most of the other large volcanoes on Mars. Unfortunately, this image is not able to help us understand what is unique about Alba Patera because of the thick dust cover. Instead it shows that the dust has been carved into streamlined shapes by the wind, cut by small landslides. Interestingly, there are some isolated patches that appear smooth and undisturbed by the wind. Image PSP_001510_2195 [ http://hiroc.lpl.arizona.edu/images/PSP/PSP_001510_2195/ ] was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard the Mars Reconnaissance Orbiter spacecraft on November 22, 2006. The complete image is centered at 39.3 degrees latitude, 251.5 degrees East longitude. The range to the target site was 285.7 km (178.6 miles). At this distance the image scale ranges from 57.2 cm/pixel (with 2 x 2 binning) to 114.3 cm/pixel (with 4 x 4 binning). The image shown here has been map-projected to 50 cm/pixel and north is up. The image was taken at a local Mars time of 3:23 PM and the scene is illuminated from the west with a solar incidence angle of 50 degrees, thus the sun was about 40 degrees above the horizon. At a solar longitude of 139.0 degrees, the season on Mars is 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. |
|
Alba Patera Windstreaks
PIA03934
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera Windstreaks |
| Original Caption Released with Image |
Windstreaks are features caused by the interaction of wind and topographic landforms. The raised rims and bowls of impact craters causes a complex interaction such that the wind vortex in the lee of the crater can both scour away the surface dust and deposit it back in the center of the lee. If you look closely, you will see evidence of this in a darker "rim" enclosing a brighter interior. These windstreaks are located northeast of Olympus Mons and southwest of Alba Patera. The lava flows the windstreaks occur on most likely originated from Alba Patera. Image information: VIS instrument. Latitude 31.3, Longitude 235.1 East (124.9 West). 36 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Alba Patera Windstreaks
PIA03934
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera Windstreaks |
| Original Caption Released with Image |
Windstreaks are features caused by the interaction of wind and topographic landforms. The raised rims and bowls of impact craters causes a complex interaction such that the wind vortex in the lee of the crater can both scour away the surface dust and deposit it back in the center of the lee. If you look closely, you will see evidence of this in a darker "rim" enclosing a brighter interior. These windstreaks are located northeast of Olympus Mons and southwest of Alba Patera. The lava flows the windstreaks occur on most likely originated from Alba Patera. Image information: VIS instrument. Latitude 31.3, Longitude 235.1 East (124.9 West). 36 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Alba Patera Channels
PIA05666
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera Channels |
| Original Caption Released with Image |
Released 1 April 2004 The Odyssey spacecraft has completed a full Mars year of observations of the red planet. For the next several weeks the Image of the Day will look back over this first mars year. It will focus on four themes: 1) the poles - with the seasonal changes seen in the retreat and expansion of the caps, 2) craters - with a variety of morphologies relating to impact materials and later alteration, both infilling and exhumation, 3) channels - the clues to liquid surface flow, and 4) volcanic flow features. While some images have helped answer questions about the history of Mars, many have raised new questions that are still being investigated as Odyssey continues collecting data as it orbits Mars. The channel shown on the image is near the feature called Alba Patera. It was collected August 22, 2002 during northern spring season. The local time is 4:30pm. The image shows multiple possibly liquid formed channels. Image information: VIS instrument. Latitude 43.7, Longitude 241.5 East (118.5 West). 19 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Alba Patera Channels
PIA05666
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera Channels |
| Original Caption Released with Image |
Released 1 April 2004 The Odyssey spacecraft has completed a full Mars year of observations of the red planet. For the next several weeks the Image of the Day will look back over this first mars year. It will focus on four themes: 1) the poles - with the seasonal changes seen in the retreat and expansion of the caps, 2) craters - with a variety of morphologies relating to impact materials and later alteration, both infilling and exhumation, 3) channels - the clues to liquid surface flow, and 4) volcanic flow features. While some images have helped answer questions about the history of Mars, many have raised new questions that are still being investigated as Odyssey continues collecting data as it orbits Mars. The channel shown on the image is near the feature called Alba Patera. It was collected August 22, 2002 during northern spring season. The local time is 4:30pm. The image shows multiple possibly liquid formed channels. Image information: VIS instrument. Latitude 43.7, Longitude 241.5 East (118.5 West). 19 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Apollinaris Patera
PIA06828
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Apollinaris Patera |
| Original Caption Released with Image |
Released August 23, 2004The THEMIS Image of the Day will be exploring the nomenclature of Mars [ http://photojournal.jpl.nasa.gov/catalog/PIA06821 ] for the next three weeks. "Apollinaris Patera" * "Patera: "an irregular crater, or a complex one with scalloped edges * "Apollinaris:" The Aquae Apollinares is a hot springs northwest of Rome in Etruria. This hot springs location was known to both the Etruscans and the Romans. Apollonaris Patera is the remains of a caldera located on the top of an old volcano near Gusev Crater. The image above is a mosaic of daytime IR frames. Nomenclature Fact of the Day: On Europa, another moon of Jupiter, linear features are named for Celtic stone rows, while ring features are named for Celtic stone circles. Image information: IR instrument. Latitude -9.8, Longitude 174.4 East (185.6 West). 100 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Apollinaris Patera
PIA06828
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Apollinaris Patera |
| Original Caption Released with Image |
Released August 23, 2004The THEMIS Image of the Day will be exploring the nomenclature of Mars [ http://photojournal.jpl.nasa.gov/catalog/PIA06821 ] for the next three weeks. "Apollinaris Patera" * "Patera: "an irregular crater, or a complex one with scalloped edges * "Apollinaris:" The Aquae Apollinares is a hot springs northwest of Rome in Etruria. This hot springs location was known to both the Etruscans and the Romans. Apollonaris Patera is the remains of a caldera located on the top of an old volcano near Gusev Crater. The image above is a mosaic of daytime IR frames. Nomenclature Fact of the Day: On Europa, another moon of Jupiter, linear features are named for Celtic stone rows, while ring features are named for Celtic stone circles. Image information: IR instrument. Latitude -9.8, Longitude 174.4 East (185.6 West). 100 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Tyrrhena Patera
PIA06933
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Tyrrhena Patera |
| Original Caption Released with Image |
This week we will be examining images of Tyrrhena Patera and its surroundings. Tyrrhena Patera is one of several moderate sized volcanoes located in the Martian southern highlands. While the volcanic edifice is only moderate in size (when compared to the larger Tharsis volcanoes), the surrounding volcanic materials cover an extensive area. Deep eroded channels on the slope of the volcano indicate that the volcano itself is likely composed of pyroclastic materials rather than flow materials. Image information: VIS instrument. Latitude -21.3, Longitude 106.7 East (253.3 West). 19 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Tyrrhena Patera
PIA06933
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Tyrrhena Patera |
| Original Caption Released with Image |
This week we will be examining images of Tyrrhena Patera and its surroundings. Tyrrhena Patera is one of several moderate sized volcanoes located in the Martian southern highlands. While the volcanic edifice is only moderate in size (when compared to the larger Tharsis volcanoes), the surrounding volcanic materials cover an extensive area. Deep eroded channels on the slope of the volcano indicate that the volcano itself is likely composed of pyroclastic materials rather than flow materials. Image information: VIS instrument. Latitude -21.3, Longitude 106.7 East (253.3 West). 19 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Tyrrhena Patera
PIA06945
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Tyrrhena Patera |
| Original Caption Released with Image |
This week we will be examining images of Tyrrhena Patera and its surroundings. Tyrrhena Patera is one of several moderate sized volcanoes located in the Martian southern highlands. While the volcanic edifice is only moderate in size (when compared to the larger Tharsis volcanoes), the surrounding volcanic materials cover an extensive area. Deep eroded channels on the slope of the volcano indicate that the volcano itself is likely composed of pyroclastic materials rather than flow materials. Image information: IR instrument. Latitude -21.8, Longitude 106.4 East (253.6 West). 100 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Tyrrhena Patera
PIA06945
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Tyrrhena Patera |
| Original Caption Released with Image |
This week we will be examining images of Tyrrhena Patera and its surroundings. Tyrrhena Patera is one of several moderate sized volcanoes located in the Martian southern highlands. While the volcanic edifice is only moderate in size (when compared to the larger Tharsis volcanoes), the surrounding volcanic materials cover an extensive area. Deep eroded channels on the slope of the volcano indicate that the volcano itself is likely composed of pyroclastic materials rather than flow materials. Image information: IR instrument. Latitude -21.8, Longitude 106.4 East (253.6 West). 100 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Tyrrhena Patera
PIA06934
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Tyrrhena Patera |
| Original Caption Released with Image |
This week we will be examining images of Tyrrhena Patera and its surroundings. Tyrrhena Patera is one of several moderate sized volcanoes located in the Martian southern highlands. While the volcanic edifice is only moderate in size (when compared to the larger Tharsis volcanoes), the surrounding volcanic materials cover an extensive area. Deep eroded channels on the slope of the volcano indicate that the volcano itself is likely composed of pyroclastic materials rather than flow materials. Image information: VIS instrument. Latitude -21.5, Longitude 106.9 East (253.1 West). 70 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Tyrrhena Patera
PIA06934
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Tyrrhena Patera |
| Original Caption Released with Image |
This week we will be examining images of Tyrrhena Patera and its surroundings. Tyrrhena Patera is one of several moderate sized volcanoes located in the Martian southern highlands. While the volcanic edifice is only moderate in size (when compared to the larger Tharsis volcanoes), the surrounding volcanic materials cover an extensive area. Deep eroded channels on the slope of the volcano indicate that the volcano itself is likely composed of pyroclastic materials rather than flow materials. Image information: VIS instrument. Latitude -21.5, Longitude 106.9 East (253.1 West). 70 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Tyrrhena Patera Mosaic
PIA06947
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Tyrrhena Patera Mosaic |
| Original Caption Released with Image |
This image of Tyrrhena Patera is a mosaic of daytime thermal infrared images colorized with a mosaic of nighttime temperature images (purple/blue is coldest, yellow/red is warmest). The colder nighttime temperatures (blue hues) in the caldera and on the flanks of the volcano indicate that this area is likely covered with finer-grained materals. This contrasts strongly against the warm (red) area to the northwest. These warmer temperatures indicate a rockier surface, possibly even exposed bedrock. This is especially probably where the red hues conform with the topography. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Tyrrhena Patera Nighttime IR
PIA07080
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Tyrrhena Patera Nighttime IR |
| Original Caption Released with Image |
Like yesterday's image, the small unnamed channel in this nighttime IR image is located near Tyrrhena Patera. This channel is located to the northwest of the volcanic complex and likely formed by fluvial action. NOTE: in nighttime images North is to the bottom of the image. Image information: IR instrument. Latitude -24.6, Longitude 349.7 East (10.3 West). 100 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Tyrrhena Patera Nighttime IR
PIA07080
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Tyrrhena Patera Nighttime IR |
| Original Caption Released with Image |
Like yesterday's image, the small unnamed channel in this nighttime IR image is located near Tyrrhena Patera. This channel is located to the northwest of the volcanic complex and likely formed by fluvial action. NOTE: in nighttime images North is to the bottom of the image. Image information: IR instrument. Latitude -24.6, Longitude 349.7 East (10.3 West). 100 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Alba Patera Graben
PIA07810
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera Graben |
| Original Caption Released with Image |
This VIS image is on the southern flank of Alba Patera -- a large, old volcano. These graben likely formed as the volcano collaped into the empty magma chamber beneath the surface. Image information: VIS instrument. Latitude 31.9, Longitude 251.4 East (108.6 West). 19 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Alba Patera Graben
PIA07810
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera Graben |
| Original Caption Released with Image |
This VIS image is on the southern flank of Alba Patera -- a large, old volcano. These graben likely formed as the volcano collaped into the empty magma chamber beneath the surface. Image information: VIS instrument. Latitude 31.9, Longitude 251.4 East (108.6 West). 19 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Alba Patera Collapse Pits
PIA07069
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera Collapse Pits |
| Original Caption Released with Image |
We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form. This image of the Alba Patera region has both lava tube collapse pits (running generally east/west) and subsidence related collapse within structural grabens. Image information: IR instrument. Latitude 26.9, Longitude 256.5 East (103.5 West). 100 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Alba Patera Collapse Pits
PIA07069
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera Collapse Pits |
| Original Caption Released with Image |
We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form. This image of the Alba Patera region has both lava tube collapse pits (running generally east/west) and subsidence related collapse within structural grabens. Image information: IR instrument. Latitude 26.9, Longitude 256.5 East (103.5 West). 100 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Alba Patera Collapse Pits
PIA07054
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera Collapse Pits |
| Original Caption Released with Image |
We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form. These collapse pits are found within graben surrounding Alba Patera. Alba Patera is an old volcano that has subsided after it's magma chamber was evacuated. Image information: VIS instrument. Latitude 43.1, Longitude 259.4 East (100.6 West). 19 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Alba Patera Collapse Pits
PIA07054
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera Collapse Pits |
| Original Caption Released with Image |
We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form. These collapse pits are found within graben surrounding Alba Patera. Alba Patera is an old volcano that has subsided after it's magma chamber was evacuated. Image information: VIS instrument. Latitude 43.1, Longitude 259.4 East (100.6 West). 19 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Nili Patera Dune Field
PIA07833
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Nili Patera Dune Field |
| Original Caption Released with Image |
Our topic for the weeks of April 4 and April 11 is dunes on Mars. We will look at the north polar sand sea and at isolated dune fields at lower latitudes. Sand seas on Earth are often called "ergs," an Arabic name for dune field. A sand sea differs from a dune field in two ways: 1) a sand sea has a large regional extent, and 2) the individual dunes are large in size and complex in form. This VIS image shows a dune field within Nili Patera, the northern caldera of a large volcanic complex in Syrtis Major. Image information: VIS instrument. Latitude 9, Longitude 67 East (293 West). 19 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Nili Patera Dune Field
PIA07833
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Nili Patera Dune Field |
| Original Caption Released with Image |
Our topic for the weeks of April 4 and April 11 is dunes on Mars. We will look at the north polar sand sea and at isolated dune fields at lower latitudes. Sand seas on Earth are often called "ergs," an Arabic name for dune field. A sand sea differs from a dune field in two ways: 1) a sand sea has a large regional extent, and 2) the individual dunes are large in size and complex in form. This VIS image shows a dune field within Nili Patera, the northern caldera of a large volcanic complex in Syrtis Major. Image information: VIS instrument. Latitude 9, Longitude 67 East (293 West). 19 meter/pixel resolution. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Biblis Patera
PIA10000
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Biblis Patera |
| Original Caption Released with Image |
Context image for PIA10000 Biblis Patera This VIS image crosses Biblis Patera. Note the large size and depth of the summit caldera in relation to the size of the entire construct. Image information: VIS instrument. Latitude 2.1N, Longitude 235.9E. 35 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Biblis Patera
PIA10000
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Biblis Patera |
| Original Caption Released with Image |
Context image for PIA10000 Biblis Patera This VIS image crosses Biblis Patera. Note the large size and depth of the summit caldera in relation to the size of the entire construct. Image information: VIS instrument. Latitude 2.1N, Longitude 235.9E. 35 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Alba Patera
PIA09129
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera |
| Original Caption Released with Image |
Context image for PIA09129 Alba Patera This region of Alba Patera is characterized by faulting with the down-dropped block on the southeast side of the fault. Image information: VIS instrument. Latitude 44.8N, Longitude 249.1E. 19 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Alba Patera
PIA09129
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Alba Patera |
| Original Caption Released with Image |
Context image for PIA09129 Alba Patera This region of Alba Patera is characterized by faulting with the down-dropped block on the southeast side of the fault. Image information: VIS instrument. Latitude 44.8N, Longitude 249.1E. 19 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Biblis Patera
PIA09997
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Biblis Patera |
| Original Caption Released with Image |
Context image for PIA09997 Biblis Patera This VIS image shows the summit of Biblis Patera. Image information: VIS instrument. Latitude 2.4N, Longitude 236.6E. 18 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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