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Mars' permanent North Polar cap is ringed by sand dunes. In the winter and spring the dunes are covered by a seasonal cap of dry ice as seen by NASA's by NASA's Mars Reconnaissance Orbiter spacecraft. | Map Projected Browse ImageClick on the image for larger versionMars' permanent North Polar cap is ringed by sand dunes. In the winter and spring the dunes are covered by a seasonal cap of dry ice.Here, we see the dark dunes in the summer, bare of seasonal frost. Two classic barchan dunes march across the rugged terrain. The long dark dune is crossing transverse aeolian ridges probably formed in a previous climate regime.The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colo. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. | |
This image from NASA's Mars Odyssey shows multiple channel systems located in Terra Sabaea. | Context imageToday's VIS image shows multiple channel systems located in Terra Sabaea. Two of the channels are named: Clasia Vallis and Hypsas Vallis, visible in the lower half of the image. Clasis Vallis is 125km long (77 miles), while Hypsas Vallis is only 33km long (20 miles).Orbit Number: 88121 Latitude: 34.6864 Longitude: 57.9318 Instrument: VIS Captured: 2021-10-26 04:41Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
This image from NASA's Mars Odyssey shows a sand sheet with surface dune forms as well as smaller sand dunes within an unnamed crater in Noachis Terra. | Context imageThis VIS image shows a sand sheet with surface dune forms as well as smaller sand dunes within an unnamed crater in Noachis Terra. These dunes are composed of basaltic sand that has collected in the bottom of the crater. The topographic depression of the crater forms a sand trap that prevents the sand from escaping. Dune fields are common in the bottoms of craters on Mars and appear as dark splotches that often lean up against the downwind walls of the craters. Dunes are useful for studying both the geology and meteorology of Mars. The sand forms by erosion of larger rocks, but it is unclear when and where this erosion took place on Mars or how such large volumes of sand could be formed. The dunes also indicate the local wind directions by their morphology.Orbit Number: 91766 Latitude: -52.1525 Longitude: 33.3362 Instrument: VIS Captured: 2022-08-22 07:22Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
Olympia Undae is a vast dune field in the north polar region of Mars. The dune field covers an area of approximately 470,000 km2 (bigger than California, smaller than Texas). This image was captured by NASA's 2001 Mars Odyssey spacecraft. | Context image Olympia Undae is a vast dune field in the north polar region of Mars. It consists of a broad sand sea or erg that partly rings the north polar cap from about 120° to 240°E longitude and 78° to 83°N latitude. The dune field covers an area of approximately 470,000 km2 (bigger than California, smaller than Texas). Olympia Undae is the largest continuous dune field on Mars. Olympia Undae is not the only dune field near the north polar cap, several other smaller fields exist in the same latitude, but in other ranges of longitude, e.g. Abolos and Siton Undae. Barchan and transverse dune forms are the most common. In regions with limited available sand individual barchan dunes will form, the surface beneath and between the dunes is visible. In regions with large sand supplies, the sand sheet covers the underlying surface, and dune forms are found modifying the surface of the sand sheet. In this case transverse dunes are more common. Barchan dunes "point" down wind, transverse dunes are more linear and form parallel to the wind direction. The "square" shaped transverse dunes in Olympia Undae are due to two prevailing wind directions.The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 71,000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, channels carved by water and lava, and a variety of other feature, THEMIS has imaged them all. For the next several months the image of the day will focus on the Tharsis volcanoes, the various chasmata of Valles Marineris, and the major dunes fields. We hope you enjoy these images!Orbit Number: 27652 Latitude: 80.983 Longitude: 170.458 Instrument: VIS Captured: 2008-03-09 04:03Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
The Ingenuity helicopter's carbon fiber blades can be seen spinning up to in this video taken by the Mastcam-Z instrument aboard NASA's Perseverance Mars rover on April 8, 2021, the 48th Martian day, or sol, of the mission. | Click here for animationThe Ingenuity Mars Helicopter's carbon fiber blades can be seen in this video taken by the Mastcam-Z instrument aboard NASA's Perseverance Mars rover on April 8, 2021, the 48th Martian day, or sol, of the mission. The four blades are arranged into two 4-foot-long (1.2-meter-long) counter-rotating rotors that can spin at roughly 2,400 rpm. The video shows the blades performing a wiggle test before the actual spin-up to ensure they were working properly.The helicopter weighs about 4 pounds (1.8 kilograms) on Earth, and about 1.5 pounds (0.68 kilograms) on Mars. It stands 1.6 feet (0.49 meters) high. It's four specially made carbon fiber blades are arranged into two 4-foot-long (1.2-meter-long) counter-rotating rotors that spin at roughly 2,400 rpm. The helicopter's fuselage is 5.4 inches by 7.7 inches by 6.4 inches (13.6 centimeters by 19.5 centimeters by 16.3 centimeters); it has four carbon composite landing legs, each 1.26 feet (0.384 meters) long, giving the helicopter about 5 inches (13 centimeters) of clearance above the ground. It is powered by a solar array on top of the rotor system, which charges six lithium-ion batteriesA key objective for Perseverance's mission on Mars is astrobiology, including the search for signs of ancient microbial life. The rover will characterize the planet's geology and past climate, pave the way for human exploration of the Red Planet, and be the first mission to collect and cache Martian rock and regolith (broken rock and dust).Subsequent NASA missions, in cooperation with ESA (European Space Agency), would send spacecraft to Mars to collect these sealed samples from the surface and return them to Earth for in-depth analysis.The Mars 2020 Perseverance mission is part of NASA's Moon to Mars exploration approach, which includes Artemis missions to the Moon that will help prepare for human exploration of the Red Planet.NASA's Jet Propulsion Laboratory, which is managed for NASA by Caltech in Pasadena, California, built and manages operations of the Perseverance rover. The Mastcam-Z investigation is led and operated by Arizona State University in Tempe, working in collaboration with Malin Space Science Systems in San Diego, California on the design, fabrication, testing, and operation of the cameras.For more about Perseverance: mars.nasa.gov/mars2020/ | |
NASA's Mars Exploration Rover Opportunity reached an outcrop in August 2005 and began investigating exposures of sedimentary rocks, intriguing rind-like features that appear to cap the rocks, and cobbles that dot the martian surface locally. | After months spent roving across a sea of rippled sands, Opportunity reached an outcrop in August 2005 and began investigating exposures of sedimentary rocks, intriguing rind-like features that appear to cap the rocks, and cobbles that dot the martian surface locally. Opportunity spent several sols analyzing a feature called "Lemon Rind," a thin surface layer covering portions of outcrop rocks poking through the sand north of "Erebus Crater." In images from the panoramic camera, Lemon Rind appears slightly different in color than surrounding rocks. It also appears to be slightly more resistant to wind erosion than the outcrop's interior. To obtain information on how this surface layer (or weathering rind) may have formed and how it compares to previously analyzed outcrops, Opportunity is using the microscopic imager, alpha particle X-ray spectrometer and Moessbauer spectrometer to analyze surfaces that have been brushed and ground with the rock abrasion tool. Scientists will compare these measurements with similar measurements made on the underlying rock material.This is a false-color composite generated by draping enhanced red-green-blue color from the panoramic camera's 753-nanometer, 535-nanometer and 482-nanometer filters over a high-fidelity violet, 432-nanometer-filter image. The image was acquired on martian day, or sol 552 (Aug. 13, 2005) around 11:55 a.m. local true solar time. In this representation, bright sulfur-bearing sedimentary rocks appear light tan to brown, depending on their degree of dust contamination, and small dark "blueberries" and other much less dusty rock fragments appear as different shades of blue. Draping the color derived from the blue to near-infrared filters over the violet filter image results in a false color view with the sharpest color and morphology contrasts. | |
This image from NASA's 2001 Mars Odyssey spacecraft shows a small region between Olympus Mons and Sulci Gordii. There are lava flows, tectonic depressions and channels visible in the image. All the features are related to the volcanism. | Context imageThis VIS image shows a small region between Olympus Mons and Sulci Gordii. There are lava flows, tectonic depressions and channels visible in the image. All the features are related to the volcanism.Orbit Number: 53647 Latitude: 17.6235 Longitude: 233.319 Instrument: VIS Captured: 2014-01-17 04:37Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
Spirit Rover on 'Husband Hill' | Figure 1: Location of SpiritTwo Earth years ago, NASA's Mars Exploration Rover Spirit touched down in Gusev Crater. The rover marked its first Mars-year (687 Earth days) anniversary in November 2005. Shortly before Spirit's Martian anniversary, the Mars Orbiter Camera on NASA's Mars Global Surveyor acquired an image covering approximately 3 kilometers by 3 kilometers (1.9 miles by 1.9 miles) centered on the rover's location at that time in the "Columbia Hills." "Husband Hill," the tallest in the range, is just below the center of the image. The image has a resolution of about 50 centimeters (1.6 feet) per pixel. North is up; illumination is from the left. The location is near 14.8 degrees south latitude, 184.6 degrees west longitude. The image was acquired on Nov. 2, 2005. A white box (see Figure 1) indicates the location of an excerpted portion on which the location of Spirit on that date is marked. Dr. Timothy J. Parker of the Mars Exploration Rover team at the NASA's Jet Propulsion Laboratory, Pasadena, Calif., confirmed the location of the rover in the image. The region toward the bottom of the image shows the area where the rover is currently headed. The large dark patch and other similar dark patches are accumulations of windblown sand and granules. | |
This image from NASA's Mars Odyssey shows a small section of Nirgal Valles. Located in Noachis Terra, Nirgal Valles is 610km long (379 miles). | Context imageToday's VIS image shows a small section of Nirgal Valles. Located in Noachis Terra, Nirgal Valles is 610km long (379 miles).Orbit Number: 83308 Latitude: -27.164 Longitude: 315.114 Instrument: VIS Captured: 2020-09-24 21:22Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
NASA's Mars Global Surveyor shows crisp details in a suite of mid-latitude gullies on a crater wall taken on October 12, 2006. | 20 November 2006Crisp details in a suite of mid-latitude gullies on a crater wall are captured in this Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) view obtained in southern winter on 12 October 2006. During southern winter, shadows are more pronounced and the atmosphere is typically quite clear. These gullies, which may have formed in relatively recent martian history by erosion caused by flowing, liquid water, are located in a crater on the east rim of Newton Crater near 40.4°S, 155.3°W. Sunlight illuminates the scene from the upper left. The picture covers an area about 3 km (1.9 mi) wide; the crater rim is on the right side of the image, the crater floor is on the left. North is toward the top/upper left. | |
NASA's Mars Global Surveyor shows rugged hills and mountains mantled by a blanket of fine dust in Sulci Gordii on Mars. Ripple-like dunes in the troughs between each hill or mountain have also been covered with dust. | 3 July 2004The Sulci Gordii are a grouping of ridges -- almost like small, rocky mountains -- located east of the giant volcano, Olympus Mons. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a 3 km (1.9 mi) -wide portion of the Sulci Gordii region. The rugged hills and mountains have been mantled by a blanket of fine dust. Ripple-like dunes in the troughs between each hill or mountain have also been covered with dust, indicating that they are inactive in the present martian environment. This image is located near 21.2°N, 124.2°W. Sunlight illuminates the scene from the lower left. | |
NASA's Mars Global Surveyor shows collapse pits in the Tractus Fossae region on Mars. Dark streaks on the slopes of the pit result from avalanches of dry, fine-grained debris (probably dust). | MGS MOC Release No. MOC2-419, 12 July 2003Extensional faulting, wherein some fraction of the martian crust is pulled apart and faults are formed where the bedrock breaks, has also led to formation of collapse pits in the Tractus Fossae region. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows one such pit and the layered bedrock exposed in its walls. Dark streaks on the slopes of the pit result from avalanches of dry, fine-grained debris (probably dust, as these streaks are only found in the dust-mantled regions of Mars). This pit is located near 23.5°N, 103.8°W. Sunlight illuminates the scene from the lower left. | |
This image from NASA's Mars Odyssey shows an impressive drainage system emptying into Semeykin Crater on the northern margin of Arabia Terra on Mars. | Context image for PIA11259Semeykin DrainageThis impressive drainage system empties into Semeykin Crater on the northern margin of Arabia Terra.Image information: VIS instrument. Latitude 41.1N, Longitude 7.8E. 19 meter/pixel resolution.Please see the THEMIS Data Citation Note 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. | |
This image from NASA's 2001 Mars Odyssey released on Sept 10, 2004 shows the martian surface of Ius Chasma taken during the southern summer season. An old landslide is visible to the right of the image, coming off the northern wall of the canyon. | The Odyssey spacecraft has taken some great pictures of Valles Marineris, the largest canyon in the solar system. If this canyon were on Earth, it would stretch from New York to Los Angeles. For the next several weeks, the Image of the Day will tour some of the canyons that make up this vast system. We will start with Ius Chasma in the west, and end with Coprates Chasma to the east. For more information on Vallis Marineris, please see http://mars.jpl.nasa.gov/mep/science/vm.html.This image of Ius Chasma was taken during the southern summer season. An old landslide is visible to the right of the image, coming off the northern wall of the canyon.Image information: VIS instrument. Latitude -7.4, Longitude 279.6 East (80.4 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. | |
Stitched together from 79 individual images, this Mars 2020 Mastcam-Z right-eye 110-mm zoom mosaic is from the camera's first high-resolution panorama imaging sequence. | Photojournal Note: Also available is the full-width high-resolution file in TIF or PNG format, PIA23727_ultrawide.tif (93355 x 2127 pixels, 211 MB) or PIA23727_ultrawide.png (93355 x 2127 pixels, 161 MB). These files may be too large to view from a browser; they can be downloaded onto your desktop by right-clicking on the previous links and viewed with image viewing software.Stitched together from 79 individual images, this Mastcam-Z right-eye 110-mm zoom mosaic is from the camera's first high-resolution panorama imaging sequence. These images were taken on the afternoon of Sol 4 (Feb. 22, 2021) of the mission; a sol is a Martian day.The camera was commanded to take these images by scanning the mast, or "head," a full 360-degrees around the horizon visible from the landing site. The top of some of the distant crater rim is cut off in some images to ensure the images would cover the front ridge of the Jezero Crater's ancient delta, which is only about 1.25 miles (2 kilometers) away from the rover in the center of this panorama. At that distance and focal length, Mastcam-Z can resolve features as small as about 50 centimeters (1.6 feet) across along the front of the delta. The mosaic is not white balanced but is instead displayed in a preliminary calibrated version of a natural color composite, approximately simulating the colors of the scene that we would see if we were there viewing it ourselves.Arizona State University in Tempe leads the operations of the Mastcam-Z instrument, working in collaboration with Malin Space Science Systems in San Diego.A key objective for Perseverance's mission on Mars is astrobiology, including the search for signs of ancient microbial life. The rover will characterize the planet's geology and past climate, pave the way for human exploration of the Red Planet, and be the first mission to collect and cache Martian rock and regolith (broken rock and dust).Subsequent NASA missions, in cooperation with ESA (European Space Agency), would send spacecraft to Mars to collect these sealed samples from the surface and return them to Earth for in-depth analysis.The Mars 2020 Perseverance mission is part of NASA's Moon to Mars exploration approach, which includes Artemis missions to the Moon that will help prepare for human exploration of the Red Planet.JPL, which is managed for NASA by Caltech in Pasadena, California, built and manages operations of the Perseverance rover.For more about Perseverance go to: mars.nasa.gov/mars2020 or nasa.gov/perseverance | |
This image from NASA's Mars Odyssey spacecraft is of a small dune field inside an unnamed crater south of Nili Fossae on Mars. | 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.Our final dune image shows a small dune field inside an unnamed crater south of Nili Fossae.Image information: VIS instrument. Latitude 20.6, Longitude 79 East (281 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. | |
This image from NASA's Mars Odyssey shows a landslide deposit in Tiu Valles. | Context imageToday's VIS image shows a landslide deposit in Tiu Valles. The impact that created the crater likely caused the landslide, either during the impact event or shortly after. Located in Margaritifer Terra, Tiu Valles is part of a large system of channels that arise from Vallis Marineris and flow northward to empty into Chryse Planitia. Tiu Valles is 1720km long (1069 miles).Orbit Number: 88299 Latitude: 14.6135 Longitude: 325.705 Instrument: VIS Captured: 2021-11-09 20:20Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
This image from NASA's Mars Odyssey shows the floor of Matara Crater. A large sand sheet with surface dune forms dominates the floor of this crater located in Noachis Terra. | Context imageToday's VIS image shows the floor of Matara Crater (center of image). A large sand sheet with surface dune forms dominates the floor of this crater located in Noachis Terra. A similar dune complex is visible in an unnamed crater near the top of the image. Matara Crater is 48km (30 miles) in diamenter.Orbit Number: 83087 Latitude: -48.3688 Longitude: 34.0401 Instrument: VIS Captured: 2020-09-06 16:04Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
NASA's Mars Global Surveyor shows sand dunes in the martian north polar region in mid-spring, July 2004. In summer, the dunes will be dark. As they defrost, dark spots form on their surfaces. | 23 August 2004This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows sand dunes in the martian north polar region in mid-spring, July 2004. In summer, the dunes will be dark. As they defrost, dark spots form on their surfaces. This image is located near 82.8°N, 219.6°W. The image covers an area about 3 km (1.9 mi) across and sunlight illuminates the scene from the lower left. | |
NASA's Mars Global Surveyor shows the state of defrosting north polar sand dunes on Mars on 3 August 2004. Dark areas on the dunes are patches of bare sand; bright areas are remnants of frost deposited during the previous winter. | 07 August 2004The springtime retreat of the north polar seasonal frost cap is progressing on schedule. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows the state of defrosting north polar sand dunes just three days ago on 3 August 2004. Dark areas on the dunes are patches of bare sand; bright areas are remnants of frost deposited during the previous winter. Summer will arrive on 20 September 2004. These dunes are located near 76.3°N, 263.5°W. Their steepest slopes, known as the slip face of each dune, point toward the northeast (upper right), indicating wind transport of sand from the southwest (lower left). The image covers an area about 3 km (1.9 mi) across and is illuminated by sunlight from the lower left. | |
This image captured by NASA's 2001 Mars Odyssey spacecraft show part of the dune field located on the floor of Rabe Crater. | Context image Today's VIS image show part of the dune field located on the floor of Rabe Crater.Orbit Number: 67412 Latitude: -43.5303 Longitude: 34.6741 Instrument: VIS Captured: 2017-02-23 15:25Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the caldera at the summit of Arsia Mons. | Context imageToday's VIS image shows part of the caldera at the summit of Arsia Mons.Orbit Number: 56313 Latitude: -9.26897 Longitude: 240.031 Instrument: VIS Captured: 2014-08-24 13:33Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
NASA's Mars Exploration Rover Opportunity took images combined into this cylindrical full-circle view of Mars' Meridiani Planum region includes dark-toned sand ripples and small exposures of lighter-toned bedrock during March 12, 2009. | NASA's Mars Exploration Rover Opportunity used its navigation camera to take the images combined into this full-circle view of the rover's surroundings during the 1,825th Martian day, or sol, of Opportunity's surface mission (March 12, 2009). North is at the top. The rover had driven half a meter (1.5 feet) earlier on Sol 1825 to fine-tune its location for placing its robotic arm onto an exposed patch of outcrop including a target area informally called "Cook Islands." On the preceding sol, Opportunity turned around to drive frontwards and then drove 4.5 meters (15 feet) toward this outcrop. The tracks from the SOl 1824 drive are visible near the center of this view at about the 11 o'clock position. For scale, the distance between the parallel wheel tracks is about 1 meter (about 40 inches). Opportunity had previously been driving backward as a strategy to redistribute lubrication in a wheel drawing more electrical current than usual.The outcrop exposure that includes "Cook Islands" is visible just below the center of the image. The terrain in this portion of Mars' Meridiani Planum region includes dark-toned sand ripples and lighter-toned bedrock.This view is presented as a cylindrical projection with geometric seam correction. | |
This view NASA's Curiosity Mars Rover shows the rover's drill in position for a mini-drill test to assess whether a rock target called 'Mojave' is appropriate for full-depth drilling to collect a sample. It was taken on Jan. 13, 2015. | This view from the wide-angle Hazard Avoidance Camera (Hazcam) on the front of NASA's Curiosity Mars Rover shows the rover's drill in position for a mini-drill test to assess whether a rock target called "Mojave" is appropriate for full-depth drilling to collect a sample. It was taken on Jan. 13, 2015, during the 867th Martian day, or sol, of Curiosity's work on Mars.The rover team selected Mojave as the mission's second drill-sampling candidate on Mount Sharp. A higher portion of the mountain is visible on the horizon. A key appeal of this target is an abundance of crystal-shaped features evident when Curiosity used its dust-removal tool here in November 2014, as shown in PIA19077. The target is in the "Pink Hills" area near the lower edge of the "Pahrump Hills" outcrop in the basal layer of Mount Sharp. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, manages the Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington. JPL designed and built the project's Curiosity rover and the rover's Hazcams.More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/. | |
NASA's Mars Global Surveyor shows some typical relations between impact craters and light-toned, layered rock on Mars. The larger circular feature marks the location of a filled, buried crater on intermountain terrain north of Hellas Planitia. | 11 March 2006This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows some typical relations between impact craters and light-toned, layered rock on Mars. The larger circular feature at the north (top) end of the image marks the location of a filled, buried crater on intermountain terrain north of Hellas Planitia. The larger crater at the southeast (lower right) corner formed by meteor impact into the layered material in which the buried crater is encased. The layered rock, in this case, has a light tone similar to the sedimentary rocks being explored by the Mars Exploration Rover, Opportunity, thousands of kilometers away in Sinus Meridiani.Location near: 24.9°S, 299.3°W Image width: ~3 km (~1.9 mi) Illumination from: upper left Season: Southern Summer | |
This image from NASA's Mars Global Surveyor (MGS) view (lower right, above), released on April 24, 2000, shows a 1.5 kilometer-(0.9 mile)-wide portion of the floor of Vishniac in the process of defrosting during southern spring. | Click for full-resolution image | |
This image from NASA's Mars Odyssey shows a complex channel, part of Mangala Fossae. | Context imageThe complex channel at the top of the image is part of Mangala Fossae. At the top of this image the main graben is interacting with a preexisting impact creater. Other depression towards the bottom of the image are simple linear features. Mangala Fossae are long linear depressions called a graben and were formed by extension of the crust and faulting. When large amounts of pressure or tension are applied to rocks on timescales that are fast enough that the rock cannot respond by deforming, the rock breaks along faults. In the case of a graben, two parallel faults are formed by extension of the crust and the rock in between the faults drops downward into the space created by the extension. Mangala Fossae is 828 km long (514 miles).Orbit Number: 91348 Latitude: -20.1261 Longitude: 207.108 Instrument: VIS Captured: 2022-07-18 21:30Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
NASA's Mars Exploration Rover Opportunity shows the shapes of the vugs, or small cavities, located on the region dubbed 'El Capitan.' The region is part of the rock outcrop at Meridiani Planum, Mars. | This image, taken by the microscopic imager on the Mars Exploration Rover Opportunity, illustrates the shapes of the vugs, or small cavities, located on the region dubbed "El Capitan." The region is part of the rock outcrop at Meridiani Planum, Mars, which the rover is currently examining.The image provides insight into the nature of the rock matrix -- the rock material surrounding the vugs. Several vugs have disk-like shapes with wide midpoints and tapered ends. This feature is consistent with sulfate minerals that crystallize within a rock matrix, either pushing the matrix grains aside or replacing them. These crystals are then either dissolved in water or eroded by wind activity to produce vugs.The rock matrix here exhibits a granular texture, delicately enhanced through wind abrasion. The primary sediment particles making up this granular layer are relatively uniform in size, ranging up to 1 millimeter (.04 inches). Note that some of these grains are well rounded, which could result from transport of rock fragments in air or water, or precipitation of mineral grains in water. | |
Extensive wind-swept plains of the Medusae Fossae formation on Mars. This southern subframe image, frame 3104, is of a 3.0 x 4.7 km area centered near 2.0 degrees north, 163.8 degrees west, taken by NASA's Mars Global Surveyor Orbiter. | Extensive wind-swept plains of the Medusae Fossae formation on Mars. This southern subframe image, frame 3104, is of a 3.0 x 4.7 km area centered near 2.0 degrees north, 163.8 degrees west.Figure caption from Science Magazine. | |
The small channel at the top of this image from NASA's 2001 Mars Odyssey spacecraft is located on the rim of an unnamed crater in Terra Sabaea. | Context imageThe small channel at the top of this VIS image is located on the rim of an unnamed crater in Terra Sabaea.Orbit Number: 50995 Latitude: -24.3698 Longitude: 27.795 Instrument: VIS Captured: 2013-06-12 21:30Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
NASA's Mars Global Surveyor shows volcanic plains to the east, southeast, and south of the giant Tharsis volcano, Pavonis Mons on Mars, dotted by dozens of small volcanoes. | MGS MOC Release No. MOC2-549, 19 November 2003The volcanic plains to the east, southeast, and south of the giant Tharsis volcano, Pavonis Mons, are dotted by dozens of small volcanoes. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows an example located near 2.1°S, 109.1°W. The elongate depression in the lower left (southwest) quarter of the image is the collapsed vent area for this small, unnamed volcano. A slightly sinuous, leveed channel runs from the depression toward the upper right (north-northeast); this is the trace of a collapsed lava tube. The entire scene has been mantled by dust, such that none of the original volcanic rocks are exposed--except minor occurrences on the steepest slopes in the vent area. The scene is 3 km (1.9 mi) wide and illuminated by sunlight from the left/upper left. | |
This image from NASA's 2001 Mars Odyssey spacecraft shows a portion of Naktong Vallis in Terra Sabaea. | Context imageToday's VIS image shows a portion of Naktong Vallis in Terra Sabaea.Orbit Number: 43765 Latitude: 0.099626 Longitude: 36.5548 Instrument: VIS Captured: 2011-10-26 22:10Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
This anaglyph, acquired by NASA's Phoenix Lander's Surface Stereo Imager on June 8, 2008, shows a stereoscopic 3D view of the Martian surface near the lander. 3D glasses are necessary. | This anaglyph, acquired by NASA's Phoenix Lander's Surface Stereo Imager on Sol 14, the 14th Martian day of the mission (June 8, 2008), shows a stereoscopic 3D view of the Martian surface near the lander.The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.Photojournal Note: As planned, the Phoenix lander, which landed May 25, 2008 23:53 UTC, ended communications in November 2008, about six months after landing, when its solar panels ceased operating in the dark Martian winter. | |
This image from NASA's 2001 Mars Odyssey spacecraft shows a portion of Nanedi Valles in Xanthe Terra. | Context imageThis VIS image shows a portion of Nanedi Valles in Xanthe Terra.Orbit Number: 44542 Latitude: 3.58436 Longitude: 310.851 Instrument: VIS Captured: 2011-12-29 20:58Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
This image indicates the locations of NASA's Perseverance rover, as well as the Kodiak butte and several prominent steep banks known as escarpments, or scarps, along the delta of Jezero Crater. | Provided by the High Resolution Imaging Experiment (HiRISE) aboard NASA's Mars Reconnaissance orbiter, this overhead image captures a portion of Mars' Jezero Crater. The yellow dot on lower right indicates the location of NASA's Perseverance rover. The remnant of Jezero Crater's rover delta the science team refers to as "Kodiak" is to the lower left. Long, steep slopes, called scarps, along the delta are on the upper left, labeled A through D.The University of Arizona, in Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., in Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.A key objective for Perseverance's mission on Mars is astrobiology, including the search for signs of ancient microbial life. The rover will characterize the planet's geology and past climate, pave the way for human exploration of the Red Planet, and be the first mission to collect and cache Martian rock and regolith.The Mars 2020 Perseverance mission is part of NASA's Moon to Mars exploration approach, which includes Artemis missions to the Moon that will help prepare for human exploration of the Red Planet.Subsequent NASA missions, in cooperation with ESA (European Space Agency), would send spacecraft to Mars to collect these sealed samples from the surface and return them to Earth for in-depth analysis.NASA's Jet Propulsion Laboratory in Southern California built and manages operations of the Mars 2020 Perseverance rover for NASA.For more information about the mission, go to:https://mars.nasa.gov/mars2020 | |
NASA's Mars Exploration Rover Opportunity observed this outcrop on the 'Murray Ridge' portion of the rim of Endeavour Crater as the rover approached the 10th anniversary of its landing on Mars. | Horizontal cropVertical cropClick on an individual image for full resolution figures imageNASA's Mars Exploration Rover Opportunity observed this outcrop on the "Murray Ridge" portion of the rim of Endeavour Crater as the rover approached the 10th anniversary of its landing on Mars. Opportunity used its Panoramic Camera (Pancam) during the 3,494th to 3,496th Martian days, or sols, of its work on Mars (Nov. 21 to Nov. 23, 2013) to take the images combined into this approximately true-color view. The scene includes an outcrop called "Moreton Island," which the rover imaged to help researchers chose a target for contact investigation with tools on the rover's robotic arm. The view merges exposures taken through three of the Pancam's color filters, centered on wavelengths of 753 nanometers (near-infrared), 535 nanometers (green) and 432 nanometers (violet). Opportunity landed on Mars on Jan. 25, 2004, Universal Time (Jan. 24, 2004, PST). Spirit, the other twin rover sent by NASA's Mars Exploration Rover Project, landed on Jan. 4, 2004, UT (Jan. 3, 2004, PST). Both missions were planned for durations of three months on Mars. Spirit worked for six years and Opportunity is still exploring in January 2014. | |
This image from NASA's Mars Odyssey spacecraft shows the western floor of Liu Hsin Crater containing many, small, isolated dark dunes on Mars. | Context image for PIA10152Liu Hsin CraterThe western floor of Liu Hsin Crater contains many, small, isolated dark dunes.Image information: VIS instrument. Latitude -53.1N, Longitude 188.0E. 17 meter/pixel resolution.Please see the THEMIS Data Citation Note 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. | |
The arcuate fractures and broken up surface shown in this image from NASA's 2001 Mars Odyssey spacecraft is called Avernus Colles. This unique surface has developed on the southeast margin of Elysium Plainitia. | Context image The arcuate fractures and broken up surface shown in this image is called Avernus Colles. This unique surface has developed on the southeast margin of Elysium Plainitia.Orbit Number: 69502 Latitude: 0.0441848 Longitude: 175.395 Instrument: VIS Captured: 2017-08-14 20:32Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
The hills in this image from NASA's Mars Odyssey are part of mound located in Arcadia Plantia. Just west of these hills is a long region of grouped hills called Phlegra Montes. | Context imageThe hills in this VIS image are part of mound located in Arcadia Plantia. Just west of these hills is a long region of grouped hills called Phlegra Montes.Orbit Number: 72221 Latitude: 31.1044 Longitude: 166.723 Instrument: VIS Captured: 2018-03-26 20:50Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
This image from NASA's Mars Odyssey shows the western side of the summit caldera on the volcano called Uranius Mons. | Context imageToday's VIS image shows the western side of the summit caldera on the volcano called Uranius Mons. Uranius Mons is 4.8 kilometers (3 miles) high with shallow slopes. The surrounding volcanic plains are younger than the volcano itself and originated at other volcanic centers in the Tharsis region.Orbit Number: 85356 Latitude: 25.5498 Longitude: 266.521 Instrument: VIS Captured: 2021-03-12 12:40Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
NASA Mars Pathfinder's rear rover ramp can be seen successfully unfurled in this image, taken at the end of July 5, 1997 Sol 2 by the Imager for Mars Pathfinder (IMP). | Mars Pathfinder's rear rover ramp can be seen successfully unfurled in this image, taken at the end of Sol 2 by the Imager for Mars Pathfinder (IMP). This ramp was later used for the deployment of the microrover Sojourner, which occurred at the end of Sol 2. Areas of a lander petal and deflated airbag are visible at left. The image helped Pathfinder scientists determine that the rear ramp was the one to use for rover deployment. At upper right is the rock dubbed "Barnacle Bill," which Sojourner will later study.Mars Pathfinder is the second in NASA's Discovery program of low-cost spacecraft with highly focused science goals. The Jet Propulsion Laboratory, Pasadena, CA, developed and manages the Mars Pathfinder mission for NASA's Office of Space Science, Washington, D.C.
Photojournal note: Sojourner spent 83 days of a planned seven-day mission exploring the Martian terrain, acquiring images, and taking chemical, atmospheric and other measurements. The final data transmission received from Pathfinder was at 10:23 UTC on September 27, 1997. Although mission managers tried to restore full communications during the following five months, the successful mission was terminated on March 10, 1998. | |
NASA's Ingenuity Mars Helicopter is seen in shadow in an image captured by its navigation camera during the rotorcraft's 52nd flight on April 26, 2023. This image was finally received after Perseverance and Ingenuity were out of communication for 63 days. | NASA's Ingenuity Mars Helicopter's navigation camera captured the rotorcraft in shadow during its 52nd flight on April 26, 2023. This image was finally received after Perseverance and Ingenuity were out of communication for 63 days.The Ingenuity Mars Helicopter was built by NASA's Jet Propulsion Laboratory, which manages the project for NASA Headquarters. It is supported by NASA's Science Mission Directorate. NASA's Ames Research Center in California's Silicon Valley and NASA's Langley Research Center in Hampton, Virginia, provided significant flight performance analysis and technical assistance during Ingenuity's development. AeroVironment Inc., Qualcomm, and SolAero also provided design assistance and major vehicle components. Lockheed Martin Space designed and manufactured the Mars Helicopter Delivery System. | |
This image from NASA's Mars Odyssey shows Hebrus Valles, a complex channel system that flowed to the north. | Context imageLocated west of the Elysium Volcanic complex, Hebrus Valles is a complex channel system that flowed to the north. In this VIS image the there are fluid created channels and tectonic formed depressions. In other portions of the valles, there are pits and collapse features which appear to have formed by material falling into subsurface voids. This is a common feature in regions of volcanic activity where lava tubes run below the surface. Both water and lava contributed to the formation of Hebrus Valles.Orbit Number: 78248 Latitude: 17.8704 Longitude: 128.118 Instrument: VIS Captured: 2019-08-05 06:11Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
This mosaic taken by NASA's Mars Curiosity rover looks uphill at Mount Sharp. Highlighted is an area in white with clay-bearing rocks that scientists are eager to explore. | This mosaic taken by NASA's Mars Curiosity rover looks uphill at Mount Sharp, which Curiosity has been climbing. Highlighted in white is an area with clay-bearing rocks that scientists are eager to explore; it could shed additional light on the role of water in creating Mount Sharp. The mosaic was assembled from dozens of images taken by Curiosity's Mast Camera (Mastcam). It was taken on Sol 1931 back in January.Mount Sharp stands in the middle of Gale Crater, which is 96 miles (154 kilometers) in diameter. This mound, which Curiosity has been climbing since 2014, likely formed in the presence of water at various points of time in Mars ancient history. That makes it an ideal place to study how water influenced the habitability of Mars billions of years ago.The scene has been white-balanced so the colors of the rock materials resemble how they would appear under daytime lighting conditions on Earth.Malin Space Science Systems, San Diego, built and operates the Mastcam. NASA's Jet Propulsion Laboratory, a division of the Caltech in Pasadena, California, manages the Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington. JPL designed and built the project's Curiosity rover. More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/. | |
This image captured by NASA's 2001 Mars Odyssey spacecraft spans from Tithonium Chasma (top of image) to Ius Chasma (bottom of image). | Context imageThis VIS image spans from Tithonium Chasma (top of image) to Ius Chasma (bottom of image).Orbit Number: 56187 Latitude: -6.18316 Longitude: 273.792 Instrument: VIS Captured: 2014-08-14 04:36Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
This image from NASA's Mars Odyssey shows tan unnamed crater located in Terra Sirenum. The surface of the ejecta contains radial grooves, visible on the thicker ejecta near the crater rim. | Context imageThis VIS image shows an unnamed crater located in Terra Sirenum. The surface of the ejecta contains radial grooves, visible on the thicker ejecta near the crater rim. The formation mechanism for the grooves is still unknown but several theories exist including basal surge flows and air pressure rock entrainment. Several gullies dissect the inner crater rim.Orbit Number: 84865 Latitude: -43.7455 Longitude: 222.519 Instrument: VIS Captured: 2021-01-31 01:32Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
These plots, or spectra, show that a rock dubbed 'McKittrick' near the Mars Exploration Rover Opportunity's landing site at Meridiani Planum, Mars, possesses the highest concentration of sulfur yet observed on Mars. | These plots, or spectra, show that a rock dubbed "McKittrick" near the Mars Exploration Rover Opportunity's landing site at Meridiani Planum, Mars, possesses the highest concentration of sulfur yet observed on Mars. These data were acquired with the rover's alpha particle X-ray spectrometer, which produces a spectrum, or fingerprint, of chemicals in martian rocks and soil. This instrument contains a radioisotope, curium-244, that bombards a designated area with alpha particles and X-rays, causing a cascade of reflective fluorescent X-rays. The energies of these fluorescent X-rays are unique to each atom in the periodic table, allowing scientists to determine a target's elemental composition.The spectra shown here are taken from "McKittrick" and a soil patch nicknamed "Tarmac," both of which are located within the small crater where Opportunity landed. "McKittrick" measurements were acquired after the rover drilled a hole in the rock with its rock abrasion tool. Only portions of the targets' full spectra are displayed. The data are expressed as X-ray intensity (linear scale) versus energy. The measured area is 28 millimeters (1 inch) in diameter.When comparing two spectra, the relative intensities at a given energy are proportional to the elemental concentrations, however these proportionality factors can be complex. To be precise, scientists extensively calibrate the instrument using well-analyzed geochemical standards.Both the alpha particle X-ray spectrometer and the rock abrasion tool are located on the rover's instrument deployment device, or arm. | |
NASA's Mars Global Surveyor shows a rounded knob in the Propontis region of Mars. Dark dots on the hilltop and slopes are house-sized (and larger) boulders. | 22 April 2004This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) picture shows a rounded knob in the Propontis region of Mars near 43.1°N, 182.3°W. Dark dots on the hilltop and slopes are house-sized (and larger) boulders. The picture covers an area about 3 km (1.9 mi) across. Sunlight illuminates the scene from the lower left. | |
NASA's Mars Global Surveyor shows a dust storm raging in Syria Planum, south of the Labyrinthus Noctis troughs on Mars. Water ice clouds are present over each of the five largest Tharsis volcanoes. | MGS MOC Release No. MOC2-366, 20 May 2003A dust storm rages in Syria Planum, south of the Labyrinthus Noctis troughs (at lower center) in this Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) composite of daily global images taken during the recent southern winter. In this view, water ice clouds are present over each of the five largest Tharsis volcanoes, Olympus Mons (right center), Alba Patera (upper center), Ascraeus Mons (near center), Pavonis Mons (toward lower left), and Arsia Mons (lower left). The summertime north polar residual water ice cap can be seen at the top of this picture. Sunlight illuminates the planet from the left. | |
This image from NASA's Mars Odyssey shows a channel associated with Hecates Tholus, part of the Elysium volcanic complex. | Context image for PIA10880Buvinda VallisThis channel is associated with Hecates Tholus, part of the Elysium volcanic complex.Image information: VIS instrument. Latitude 32.4N, Longitude 152.0E. 19 meter/pixel resolution.Please see the THEMIS Data Citation Note 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. | |
This color thumbnail image was obtained by NASA's Curiosity rover revealing surface features including relatively dark dunes, degraded impact craters and other geologic features including small escarpments. | This color thumbnail image was obtained by NASA's Curiosity rover during its descent to the surface of Mars on Aug. 5 PDT (Aug. 6 EDT). This image from Curiosity's Mars Descent Imager reveals surface features including relatively dark dunes, degraded impact craters and other geologic features including small escarpments that range in size from a few feet (meters) to many tens of feet (meters) in height. | |
This crater on Mars is located at 37°N, a latitude far enough north that ground ice is present, and it sculpts the terrain when it moves. This image is from NASA's Mars Odyssey. | Released 20 May 2003This crater is located at 37°N, a latitude far enough north that ground ice is present, and it sculpts the terrain when it moves. In this image, the western rim of the crater has been deformed from its original, presumably circular, shape. Note, however, that lobes of material and grooves (seen best at full resolution) in the crater's ejecta blanket are still pristine: perhaps ground ice moves the most on steep topography, such as on a crater rim.Image information: VIS instrument. Latitude 37.6, Longitude 159.1 East (200.9) 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. | |
This image from the Navigation Camera (Navcam) on NASA's Curiosity Mars rover shows two holes at top center drilled into a sandstone target called 'Windjana.' The farther hole, with larger pile of tailings around it, is a full-depth sampling hole. | This image from the Navigation Camera (Navcam) on NASA's Curiosity Mars rover shows two holes at top center drilled into a sandstone target called "Windjana." The farther hole, with larger pile of tailings around it, is a full-depth sampling hole. It was created by the rover's hammering drill while the drill collected rock-powder sample material from the interior of the rock. The nearer hole was created by a shallower test drilling into the rock in preparation for the sample collection. Each hole is 0.63 inch (1.6 centimeters) in diameter. The full-depth hole is about 2.6 inches (6.5 centimeters) deep, drilled during the 621st Martian day, or sol, of Curiosity's work on Mars (May 5, 2014). The test hole is about 0.8 inch (2 centimeters) deep, drilled on Sol 615 (April 29, 2014). This image was taken on Sol 621 (May 5).The sandstone target's informal name comes from Windjana Gorge in Western Australia. The rock is within a waypoint location called "The Kimberley," where sandstone outcrops with differing resistance to wind erosion result in a stair-step pattern of layers. Windjana is within what the team calls the area's "middle unit," because it is intermediate between rocks that form buttes in the area and lower-lying rocks that show a pattern of striations.NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, manages the Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington. JPL designed and built the project's Curiosity rover and the rover's Navcam.
More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/. | |
This graphic shows the general activities the team behind NASA's Ingenuity Mars Helicopter hopes to accomplish on a given test flight on the Red Planet. | This graphic shows the general activities the team behind NASA's Ingenuity Mars Helicopter hopes to accomplish on a given test flight on the Red Planet. The helicopter will have 31 Earth days (30 sols, or Martian days) for its test flight program. The Ingenuity Mars Helicopter technology demonstration activity is supported by NASA's Science Mission Directorate, the NASA Aeronautics Research Mission Directorate, and the NASA Space Technology Mission Directorate. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the helicopter technology demonstration for NASA. | |
This image from NASA's Mars Rover Opportunity shows the rover's view of Meridiani Planum as it headed to Endurance Crater on Mars. | This cylindrical projection was constructed from a sequence of three images taken by the navigation camera on the Mars Exploration Rover Opportunity. The images were acquired on sol 94 (April 29, 2004) of Opportunity's mission to Meridiani Planum. The camera acquired the images at approximately 12:40 local solar time, or around 9:15 a.m. Pacific Daylight Time. The images were taken from the rover's new location about 20 meters (65 feet) away from the rim of Opportunity's next target, "Endurance Crater." | |
This image taken by NASA;s Mars Exploration Rover Opportunity shows the rock called 'Pilbara' located in the small crater dubbed 'Fram.' The rock appears to be dotted with the same 'blueberries,' or spherules, found at 'Eagle Crater.' | This approximate true-color image taken by the panoramic camera on the Mars Exploration Rover Opportunity shows the rock called "Pilbara" located in the small crater dubbed "Fram." The rock appears to be dotted with the same "blueberries," or spherules, found at "Eagle Crater." Spirit drilled into this rock with its rock abrasion tool. After analyzing the hole with the rover's scientific instruments, scientists concluded that Pilbara has a similar chemical make-up, and thus watery past, to rocks studied at Eagle Crater. This image was taken with the panoramic camera's 480-, 530- and 600-nanometer filters. | |
This image released on Oct 29, 2004 from NASA's 2001 Mars Odyssey shows the Martian north polar cap. Streamers of dust moving downslope over the darker trough sides showing the laminar flow regime coming off the cap. | This week we will be looking at five examples of laminar wind flow on the north polar cap. On Earth, gravity-driven south polar cap winds are termed "catabatic" winds. Catabatic winds begin over the smooth expanse of the cap interior due to temperature differences between the atmosphere and the surface. Once begun, the winds sweep outward along the surface of the polar cap toward the sea. As the polar surface slopes down toward sealevel, the wind speeds increase. Catabatic wind speeds in the Antartic can reach several hundreds of miles per hour.In the images of the Martian north polar cap we can see these same type of winds. Notice the streamers of dust moving downslope over the darker trough sides, these streamers show the laminar flow regime coming off the cap. Within the trough we see turbulent clouds of dust, kicked up at the trough base as the winds slow down and enter a chaotic flow regime.The horizontal lines in these images are due to framelet overlap and lighting conditions over the bright polar cap.Image information: VIS instrument. Latitude 86.5, Longitude 64.5 East (295.5 West). 40 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. | |
This false-color image released on June 8, 2004 from NASA's 2001 Mars Odyssey was collected September 5, 2003 during southern spring season. The image shows an area near the Thaumasia Planum region on Mars. | Released 8 June 2004This image was collected September 5, 2003 during southern spring season. The local time at the image location was about 4:45 pm. The image shows an area near the Thaumasia Planum region.The THEMIS VIS camera is capable of capturing color images of the martian surface using its five different color filters. In this mode of operation, the spatial resolution and coverage of the image must be reduced to accommodate the additional data volume produced from the use of multiple filters. To make a color image, three of the five filter images (each in grayscale) are selected. Each is contrast enhanced and then converted to a red, green, or blue intensity image. These three images are then combined to produce a full color, single image. Because the THEMIS color filters don't span the full range of colors seen by the human eye, a color THEMIS image does not represent true color. Also, because each single-filter image is contrast enhanced before inclusion in the three-color image, the apparent color variation of the scene is exaggerated. Nevertheless, the color variation that does appear is representative of some change in color, however subtle, in the actual scene. Note that the long edges of THEMIS color images typically contain color artifacts that do not represent surface variation.Image information: VIS instrument. Latitude -24.3, Longitude 299 East (61 West). 38 meter/pixel resolution.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
Light-toned deposits forming in two gully sites in Terra Sirenum on Mars during NASA's Mars Global Surveyor mission in the 1999-2005 period are considered to be a result of sediment transport by a fluid with the physical properties of liquid water. | The light-toned deposits that formed in two gully sites on Mars during the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) mission in the 1999 to 2005 period are considered to be the result of sediment transport by a fluid with the physical properties of liquid water. The young, light-toned gully deposits were found in a crater in Terra Sirenum (see PIA09027 or MOC2-1618) and in a crater east of the Hellas basin in the Centauri Montes region (see PIA09028 or MOC2-1619). In their study of how the light-toned gully deposits may have formed, the MOC team considered their resemblance to light- and dark-toned slope streaks found elsewhere on Mars. Slope streaks are most commonly believed to have formed by downslope movement of extremely dry, very fine-grained dust, through processes thought by some to be analogous to terrestrial snow avalanche formation. Figure 1 shows the light-toned gully deposit in the crater in the Centauri Montes region, compared with typical slope streaks and several examples in which the slope streak gives a strong impression of having been produced by fluid-like flow. Figure 1AAnnotated ImageNo AnnotationFigure 1BAnnotated ImageFigure 1CAnnotated ImageNo AnnotationFigure 1DAnnotated ImageNo AnnotationFigure 1. The fresh, light-toned gully deposits have some resemblance to slope streaks. (A) Light-toned gully deposit that formed between August 1999 and February 2004 in a crater in the Centauri Montes region of Mars. (B) Typical dark slope streaks, as seen in a valley in central Arabia Terra. Hundreds of MOC images have shown that the darkest streaks are the youngest; commonly, the darkest streaks are less than a few years old. (C) Dark slope streaks on a slope surrounding a pedestal crater in Tikhonravov Crater in Arabia Terra. These streaks, particularly the two near the center of the image, show evidence that the downslope movement of debris was diverted around obstacles, particularly large boulders. (D) Dark slope streaks, including some that diverted around obstacles, on knobs in the Aeolis region of Mars. The 300 meter scale bars are about 328 yards across; the 150 meter bar is 164 yards.As shown in Figure 2, slope streaks can be lighter or darker than their surroundings. The majority of them are dark, and nearly always when light streaks are present, dark ones are nearby. This observation differs from the two light-toned gully deposits observed in Terra Sirenum and the Centauri Montes regions. In the case of the light-toned gully deposits, no dark slope streaks are present anywhere within the craters that they formed. As far as can we can tell, based on MGS MOC and Mars Odyssey Thermal Emission Imaging System (THEMIS) coverage, there are no dark slope streaks within hundreds of kilometers of the two gully deposits. Figure 2Annotated ImageNo AnnotationFigure 2. Slope streaks of both light and dark tone, relative to their surrounding surfaces, in centralArabia Terra. Where light slope streaks are found, dark ones are almost always nearby. The 500 meter scale bar is about 547 yards across.Figure 3 shows that light and dark slope streaks occur in very specific regions (brown-shaded areas; particularly Tharsis, Amazonis, and near Elysium), and the gullies occur in different regions (pink-shaded areas; particularly middle northern and southern latitudes). In other words, the two fresh, light-toned gully deposits observed by MOC occur very far from the regions in which light and dark slope streaks are found. Indeed, the regions in which slope streaks occur are those that are most thickly covered with mantles of dust. Experience from driving the Sojourner and Mars Exploration Rover, Spirit, on dusty surfaces shows that when the uppermost coating of fine, bright dust is disturbed, the underlying surface is darker. Thus, dark slope streaks are considered to be areas where dust has been disturbed and slid downhill by dry, granular flow. The dust is extremely fine, like the flour used to bake bread. Figure 3Annotated ImageFigure 3. This map of Mars shows areas where gullies occur, shaded in pink, and where light and dark slope streaks occur, shaded in brown. The location of the two craters in which MGS MOC observed new, light-toned gully deposits are indicated. Except for a small portion of Tempe Terra (northeast of Tharsis), gullies and slope streaks do not occur together in the same regions. Slope streaks occur in regions that have been known since the Viking orbiter missions to be thickly mantled with dust. Gullies occur at middle and high latitudes, where dust mantles are not so thick. The pink-shaded gully area is based upon the MOC team's survey of over 96,000 MOC narrow angle camera images. The brown-shaded area, representing light and dark slope streak occurrences, comes from a combination of the MOC team's assessment and the published results of O. Aharonson, N. Schorghofer, and M. F. Gerstell (2003) Slope streak formation and dust deposition rates on Mars, Journal of Geophysical Research, v. 108, no. E12, doi:10.1029/2003JE002123.New dark slope streaks are forming on Mars all the time. MGS MOC images have captured hundreds of before-and-after examples. Figure 4 shows one site that MOC monitored in the Elysium/Cerberus region. Figure 4Annotated ImageNo AnnotationFigure 4. The MOC narrow angle camera has acquired hundreds of images that repeat locations where slope streaks occur. In so doing, MOC captured hundreds of cases where new slope streaks formed. New streaks are always dark, not light. Several examples on hillslopes in the Elysium/Cerberus region are shown here, spanning a period from April 1998 through January 2005. The 300 meter scale bar equals about 328 yards.New slopes streaks are always dark. No new light slope streaks have been observed by MOC, despite monitoring over the past 7-9 years at dozens of locations. Figure 5 shows one such example on the wall of Bahram Vallis, in which a suite of light slope streaks remained unchanged over a period spanning September 2000 through December 2005.Figure 5Annotated ImageNo AnnotationFigure 5. Light slope streaks are more rare than dark slope streaks. Curious as to whether new light streaks form under present conditions, just as new dark streaks do, the MOC team monitored dozens of light slope streak sites. But no new light slope streaks have been observed. This time series includes images from 2000, 2003, and 2005; no new streaks formed during this period. The 400 meter scale bar is about 437 yards across. Not only have no new light slope streaks been observed, dark streaks have been seen to superpose (i.e., formed or were deposited on top of) light streaks. Figure 6a shows a case where several dark streaks are superimposed on several light streaks. Figure 6b shows a before-and-after example, in which a new dark streak wiped out underlying, older light slope streaks.Figure 6AAnnotated ImageNo AnnotationFigure 6BAnnotated ImageNo AnnotationFigure 6. MOC images show that dark slope streaks always superpose light slope streaks, never the other way around. This observation reinforces the view that light slope streaks are not formed by the downslope movement of dust -- when dust moves, it creates a dark streak. Light streaks might therefore be old dark streaks, perhaps trapping light-toned dust better than the adjacent, intermediate-toned slopes. (A) Light and dark slope streaks on the wall of an unnamed valley in central Arabia Terra. Dark streaks in some cases superpose light streaks. (B) Light and dark slope streaks in Arabia Terra in an example where a new, large dark streak formed sometime between January 2001 and August 2003. The new dark streak formed on top of older light slope streaks. The 500 meter scale bars are about 547 yards across. The MGS MOC team's experience, gained from examining all of the more than 96,000 MOC narrow angle camera images -- and seeking evidence for changes among gullies, slope streaks, and other variable features on the planet's surface -- is that slope streaks form on very dusty slopes, the newest ones are dark, and older ones lighten with time as new dust is deposited on them. The origin of light slope streaks is not known, although we suspect they are related to dark slope streaks. Dark slope streaks may be dark because they have lost their light dust cover or because disturbed surfaces often have micro-relief that casts miniature shadows on the surface. Slope streaks that are lighter than their surroundings may have trapped newly-fallen dust within this microrelief, and may do so more effectively than adjacent, smooth slopes. Slope streaks have attributes that indicate they experienced fluidized motion, but the fluid was less viscous (more fluid) than water-lubricated dirt. As with snow avalanches, the "fluid" was probably atmospheric gas ingested and intimately mixed with the dust as it began and continued to move downslope. Such air-fluidized flows stop more abruptly than do water-fluidized flows on comparable slopes. In developing geologic interpretations from inspection of images, many factors are considered: size, relief, shape and pattern, color or brightness, texture, and association (context). Context is often the final discriminator between features that look similar. It is undeniable that the gully deposits resemble slope streaks, but they do not share the same context. If they are slopes streaks formed by downslope movement of dry, unconsolidated dust, then they are extremely rare features, because the new gully deposits (a) do not occur in regions where slope streaks occur, (b) are not found near any dark slope streaks, while typical light slope streaks have dark ones nearby, and (c) formed during the MGS MOC mission, while no new light slope streaks were observed to have formed anywhere else on the planet during the mission. Conversely, their presence within craters with gullies and the existence of similar light-toned features on other gullied (and in some cases on adjacent) slopes, with which they share geomorphic attributes, may be coincidental but is probably not. The gullies themselves provide the context for the gully deposits, and argue for a genetic relationship.The Mars Global Surveyor mission is managed for NASA's Office of Space Science, Washington, by the Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena. Lockheed Martin Space Systems, Denver, developed and operates the spacecraft. Malin Space Science Systems, San Diego, Calif., built and operates the Mars Orbiter Camera.For more information about images from the Mars Orbiter Camera, see http://www.msss.com/mgs/moc/index.html. | |
This type of 'broken-up' terrain on Mars is called chaos as seen by NASA's 2001 Mars Odyssey spacecraft. | Context image for PIA02196Aureum ChaosThis type of "broken-up" terrain is called chaos. At the bottom right corner of the image there is evidence of deposition of material.Image information: VIS instrument. Latitude -3.6N, Longitude 333.3E. 17 meter/pixel resolution.Please see the THEMIS Data Citation Note 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. | |
During the 33rd flight of NASA's Ingenuity Mars Helicopter, a small piece of foreign object debris can be seen attached to one of the rotorcraft's landing legs before falling away to the surface. There's no indication of damage to the helicopter. | Click here for animationA small piece of foreign object debris (FOD) is seen in footage from the navigation camera of NASA's Ingenuity Mars Helicopter during its 33rd flight on Mars on Sept 24, 2022. The FOD is seen attached to one of the rotorcraft's landing legs, then drifting away.The Ingenuity Mars Helicopter was built by JPL, which also manages the technology demonstration project for NASA Headquarters. It is supported by NASA's Science, Aeronautics Research, and Space Technology mission directorates. NASA's Ames Research Center in California's Silicon Valley, and NASA's Langley Research Center in Hampton, Virginia, provided significant flight performance analysis and technical assistance during Ingenuity's development. AeroVironment Inc., Qualcomm, and SolAero also provided design assistance and major vehicle components. Lockheed Martin Space designed and manufactured the Mars Helicopter Delivery System.At NASA Headquarters, Dave Lavery is the program executive for the Ingenuity Mars Helicopter. | |
This image from NASA's 2001 Mars Odyssey released on March 8, 2004 shows Mars' south polar capt during the southern summer season. Layering in the South polar cap interior is readily visible and may indicate yearly ice/dust deposition. | Released 8 March 2004The 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.This image was collected March 5, 2002 during the southern summer season. Layering in the South polar cap interior is readily visible and may indicate yearly ice/dust deposition.Image information: VIS instrument. Latitude -86.6, Longitude 156.8 East (203.2 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. | |
Rates of change in surface temperatures during a martian day indicate differences in particle size in and near 'Bonneville Crater' as shown in this image from NASA's Mars Exploration Rover (MER) taken in 2004. | Rates of change in surface temperatures during a martian day indicate differences in particle size in and near "Bonneville Crater." This image is the third in a series of five with color-coded temperature information from different times of day. This one is from 1:35 p.m. local solar time at the site where NASA's Mars Exploration Rover Spirit is exploring Mars. Temperature information from Spirit's miniature thermal emission spectrometer is overlaid onto a view of the site from Spirit's panoramic camera.In this color-coded map, quicker reddening during the day suggests sand or dust. (Red is about 270 Kelvin or 27 degrees Fahrenheit.) An example of this is in the shallow depression in the right foreground. Areas that stay blue longer into the day have larger rocks. (Blue indicates about 230 Kelvin or minus 45 Degrees F.) An example is the rock in the left foreground.See PIA05927 for a sequence of all five frames. | |
This image from NASA's Mars Odyssey shows a sinuous channel, Tinto Vallis. | Context imageThe sinuous channel in this VIS image is Tinto Vallis. This northward flowing channel is 180 km (112 miles) long and is located in northern Hesperia Planum. Tinto Vallis arises in the plains of Herperia Planum and empties into Palos Crater.Orbit Number: 79197 Latitude: -4.11256 Longitude: 111.326 Instrument: VIS Captured: 2019-10-22 09:32Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
NASA's Mars Global Surveyor shows light-toned, layered, sedimentary rock outcrops exposed on the floor of a trough that parallels Coprates Chasma in the Valles Marineris system on Mars. | MGS MOC Release No. MOC2-420, 13 July 2003This mosaic of two Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) narrow angle camera images, one from 2001, the other from 2003, shows light-toned, layered, sedimentary rock outcrops exposed on the floor of a trough that parallels Coprates Chasma in the Valles Marineris system. Layered rocks form the pages from which the history of a place can be read. It may be many years before the story is read, but or now at least we know where one of the books of martian history is found. This picture is located near 15.2°S, 60.1°W. Sunlight illuminates the scene from the left. | |
This image from NASA's Mars Odyssey shows part of Ius Chasma and one of its mega gullies. | Context imageToday's VIS image shows part of Ius Chasma and one of its mega gullies (bottom of image). Ius Chasma is unique from the other chasmata of Valles Marineris in possessing mega gullies on both sides of the chasma. The largest mega gullies are located in Sinai Planum, dissecting those plains and emptying into the canyon. Mega gullies are thought to be sapping channels caused by groundwater flow and erosion. The Earth analog is springs – water that flows underground and then breaches the surface creating channels. The morphology of the Mars gullies mirrors terrestrial springs. The channel is fairly uniform in width and the "head" of the channel is rounded like an amphitheater. The channel lengthens by erosion at the "head" backwards as the surface where the spring emerges is undercut. For Mars it is theorized that subsurface water would stay liquid due to underground heating. Ius Chasma is at the western end of Valles Marineris, south of Tithonium Chasma. Valles Marineris is over 4000 kilometers long, almost as wide as the United States. Ius Chasma is almost 850 kilometers long (528 miles), 120 kilometers wide and over 8 kilometers deep.Orbit Number: 91408 Latitude: -6.95449 Longitude: 274.37 Instrument: VIS Captured: 2022-07-23 20:09Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
This image acquired on August 15, 2020 by NASA's Mars Reconnaissance Orbiter, shows a brownish, dusty cliff wall, where the faint light-blue-colored ice shows through. | Map Projected Browse ImageClick on image for larger versionScientists have come to realize that, just below the surface, about one third of Mars is covered in ice. We study this ice to learn about Mars' ancient climate and astronauts' future water supplies.Sometimes we see the buried ice because cliffs form like the one in this image. On the brownish, dusty cliff wall, the faint light-blue-colored ice shows through. Some of these cliffs change before our eyes and boulders of ice can tumble downhill. We take repeat images of these scenes to check for changes like this.The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. (The original image scale is 25.1 centimeters [9.9 inches] per pixel [with 1 x 1 binning]; objects on the order of 75 centimeters [29.5 inches] across are resolved.) North is up.The University of Arizona, in Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., in Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. | |
This image from NASA's Mars Odyssey shows a portion of Sirenum Fossae. The linear features are tectonic graben. | Context imageToday's VIS image shows a portion of Sirenum Fossae. The linear features are tectonic graben. Graben are formed by extension of the crust and faulting. When large amounts of pressure or tension are applied to rocks on timescales that are fast enough that the rock cannot respond by deforming, the rock breaks along faults. In the case of a graben, two parallel faults are formed by extension of the crust and the rock in between the faults drops downward into the space created by the extension. Numerous sets of graben are visible in this THEMIS image, trending from north-northeast to south-southwest. Because the faults defining the graben are formed perpendicular to the direction of the applied stress, we know that extensional forces were pulling the crust apart in the west-northwest/east-southeast direction. The Sirenum Fossae graben are 2735km (1700 miles) long and stretch from eastern Terra Sirenum into western Daedalia Planum.Orbit Number: 91436 Latitude: -37.5623 Longitude: 190.938 Instrument: VIS Captured: 2022-07-26 03:19Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
Mesas and valleys form the terrain called Margaritifer Chaos as shown in this image captured by NASA's 2001 Mars Odyssey spacecraft. | Context imageMesas and valleys form the terrain called Margaritifer Chaos.Orbit Number: 43406 Latitude: -8.66529 Longitude: 337.077 Instrument: VIS Captured: 2011-09-27 07:04Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
This image from NASA's Mars Odyssey shows the westernmost extent of the Medusae Fossae Formation on Mars, a 5000+ km long belt of eroding sediments, the interleaving of erosional surfaces produces dramatic textural variations. | Released 7 May 2003Toward the westernmost extent of the Medusae Fossae Formation, a 5000+ km long belt of eroding sediments, the interleaving of erosional surfaces produces dramatic textural variations. In the lower third of this image, the cross-hatched MFF layer is being stripped back from a surface that was already heavily eroded before the MFF layer was deposited. Also, note the sinuous and, in places, dendritic ridges that are either linear dunes or inverted channels.Image information: VIS instrument. Latitude -3.9, Longitude 154.1East (205.9). 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. | |
NASA's Mars Global Surveyor shows several low, relatively flat-topped hills (mesas) on the floor of a broad valley among the mountains of the Nereidum Montes region, northeast of Argyre Planitia. | Some of the pictures returned from Mars by the Mars Orbiter Camera (MOC) onboard the Mars Global Surveyor (MGS) spacecraft show features that--at a glance--resemble familiar, non-geological objects on Earth. For example, the picture above at the left shows several low, relatively flat-topped hills (mesas) on the floor of a broad valley among the mountains of the Nereidum Montes region, northeast of Argyre Planitia. One of the mesas seen here looks like half of a butterfly (upper subframe on right). Another hill looks something like a snail or a hot dog wrapped and baked in a croissant roll (lower subframe on right). These mesas were formed by natural processes and are most likely the eroded remnants of a formerly more extensive layer of bedrock. In the frame on the left, illumination is from the upper left and the scene covers an area 2.7 km (1.7 miles) wide by 6.8 km (4.2 miles) high. The "butterfly" is about 800 meters (875 yards) in length and the "hot dog" is about 1 km (0.62 miles) long.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. | |
NASA's Mars Global Surveyor shows | MGS MOC Release No. MOC2-522, 23 October 2003This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) picture shows a young, fresh meteor impact crater in southeast Arabia Terra acquired in August 2003. The crater is inferred to be young because it still has a finely detailed pattern of rays associated with its ejecta. These rays formed in a dusty mantle that covers the other craters and rocky terrain at this locale. The crater is young enough that there has not been sufficient time for new dust to cover the rays, or for winds to erase them. The small dark dots associated with the crater are boulders. The boulders were ejected by the impact event. This crater is located near 6.9°S, 317.1°W. The picture covers an area approximately 3 km (1.9 mi) wide and is illuminated by sunlight from the lower left. | |
This image of the sedimentary rocks of Enchanted Lake was taken by one of the Perseverance rover's Hazard Avoidance Cameras (Hazcams) near the base of Jezero Crater's delta on April 30, 2022. | This image of the "Enchanted Lake" rocky outcrop, informally named after a landmark in Alaska's Katmai National Park and Preserve, was taken by one of the Hazard Avoidance Cameras (Hazcams) on NASA's Mars Perseverance rover on April 30, 2022, the 424th Martian day, or sol, of the mission.The image of the outcrop, near the base of Jezero Crater's delta, provided the rover science team with its first up-close glimpse of sedimentary rocks. Such rocks consist of fine particles carried by the atmosphere and/or water and deposited in generally flat-lying layers, which become indurated, or turned into rock, over time.A key objective for Perseverance's mission on Mars is astrobiology, including the search for signs of ancient microbial life. The rover will characterize the planet's geology and past climate, pave the way for human exploration of the Red Planet, and be the first mission to collect and cache Martian rock and regolith (broken rock and dust).Subsequent NASA missions, in cooperation with ESA (European Space Agency), would send spacecraft to Mars to collect these sealed samples from the surface and return them to Earth for in-depth analysis.The Mars 2020 Perseverance mission is part of NASA's Moon to Mars exploration approach, which includes Artemis missions to the Moon that will help prepare for human exploration of the Red Planet.NASA's Jet Propulsion Laboratory, which is managed for the agency by Caltech in Pasadena, California, built and manages operations of the Perseverance rover.For more about Perseverance:mars.nasa.gov/mars2020/ | |
The floor of this crater near its southwestern rim is rougher that the rest of the crater floor. Some process of change is working only in this area on Mars as seen by NASA's Mars Odyssey spacecraft. | Context image for PIA08679Floor Changes>The floor of this crater near its southwestern rim is rougher that the rest of the crater floor. Some process of change is working only in this area.Image information: VIS instrument. Latitude -9.0N, Longitude 86.1E. 18 meter/pixel resolution.Please see the THEMIS Data Citation Note 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. | |
This image from NASA's Mars Odyssey shows Maunder Crater. Its floor has been filled by a significant amount of material. | Context imageOne of the most interesting features of Maunder Crater is the large trough seen in this image. The floor of Maunder Crater has been filled by a significant amount of material. At some time after the filling event, the large trough developed. The depression is located on the east side of the crater and parallels the crater rim. How and why the trough came to be is unknown.Orbit Number: 91505 Latitude: -49.2071 Longitude: 2.39522 Instrument: VIS Captured: 2022-07-31 19:36Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
Wallrock and Light-toned Layering in Candor Chasma | While the canyon walls that define Valles Marineris appear dark and blocky, the interior of the canyons can sometimes be filled with light-toned rocks that appear layered. This HiRISE image shows the two geologic units in Candor Chasma, one of several canyons that make up Valles Marineris. At the center of the image is the wall rock that appears as a linear hill running east-west and composed of spurs and gullies. Larger meter-size boulders can be resolved by HiRISE and indicate lithified rock units that break down to produce these boulders which then roll downhill. The light-toned layered deposits are visible in the lower portion of the image. They appear brighter than the wallrock and also have prominent layering, which is best seen near the bottom of the image where there is a steep exposure and dozens of layers are revealed. Dark debris covers the layered deposits along this cliff face and forms debris aprons as material is shed downhill. The processes that emplaced the light-toned layered deposits are still being debated and include volcanism, eolian, and lacustrine origins. HiRISE images combined with multispectral data from CRISM (also on MRO) should help narrow down the possible origins. Image PSP_001390_1735 was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard the Mars Reconnaissance Orbiter spacecraft on November 12, 2006. The complete image is centered at -6.2 degrees latitude, 290.8 degrees East longitude. The range to the target site was 264.4 km (165.3 miles). At this distance the image scale ranges from 26.5 cm/pixel (with 1 x 1 binning) to 105.8 cm/pixel (with 4 x 4 binning). The image shown here has been map-projected to 25 cm/pixel and north is up. The image was taken at a local Mars time of 3:30 PM and the scene is illuminated from the west with a solar incidence angle of 57 degrees, thus the sun was about 33 degrees above the horizon. At a solar longitude of 134.4 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. | |
NASA's Mars Global Surveyor shows boulders ejected by the impact that formed the crater seen in the ejecta blanket. | 28 March 2005 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a 1.5 meters per pixel (5 ft/pixel) view of a ~1 km wide crater. Boulders ejected by the impact that formed the crater can be seen in the ejecta blanket. Location near: 34.1°N, 247.7°W Image width: ~3 km (~1.9 mi) Illumination from: lower left Season: Northern Spring | |
This image from NASA's Mars Odyssey shows a region of channels dissecting the northwest margin of Alba Mons, an ancient volcano. | Context image for PIA11304ChannelsThis region of channels is dissecting the northwest margin of Alba Mons, an ancient volcano.Image information: VIS instrument. Latitude 44.8N, Longitude 245.4E. 19 meter/pixel resolution.Please see the THEMIS Data Citation Note 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. | |
This doublet crater was formed when two meteorites impacted at the same time. The shock waves interact to form the straight central rim and the 'wings' of ejecta on the outside of the rims. This image is from NASA's Mars Odyssey. | Context imageThis doublet crater was formed when two meteorites impacted at the same time. The shock waves interact to form the straight central rim and the 'wings' of ejecta on the outside of the rims.Orbit Number: 39989 Latitude: -16.7109 Longitude: 265.428 Instrument: VIS Captured: 2010-12-19 23:14Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
This image from NASA's 2001 Mars Odyssey spacecraft shows part of the southeastern flank of Pavonis Mons. Surface lava flows run down hill from the top left of the image to the bottom right. | Context image This image shows part of the southeastern flank of Pavonis Mons. Surface lava flows run down hill from the top left of the image to the bottom right. Perpendicular to that trend are several linear features. These are faults that encircle the volcano and also run along the linear trend through the three Tharsis volcanoes. This image illustrates how subsurface lava tubes collapse into the free space of the empty tube. Just to the top of the deepest depression are a series of circular pits. The pits coalesce into a linear feature near the left side of the deepest depression. The mode of formation of a lava tube starts with a surface lava flow. The sides and top of the flow cool faster than the center, eventually forming a solid, non-flowing cover of the still flowing lava. The surface flow may have followed the deeper fault block graben (a lower surface than the surroundings). Once the flow stops there remains the empty space lower than the surroundings, and collapse of the top of the tube starts in small pits which coalesce in the linear features.Pavonis Mons is one of the three aligned Tharsis Volcanoes. The four Tharsis volcanoes are Ascreaus Mons, Pavonis Mons, Arsia Mons, and Olympus Mars. All four are shield type volcanoes. Shield volcanoes are formed by lava flows originating near or at the summit, building up layers upon layers of lava. The Hawaiian islands on Earth are shield volcanoes. The three aligned volcanoes are located along a topographic rise in the Tharsis region. Along this trend there are increased tectonic features and additional lava flows. Pavonis Mons is the smallest of the four volcanoes, rising 14km above the mean Mars surface level with a width of 375km. It has a complex summit caldera, with the smallest caldera deeper than the larger caldera. Like most shield volcanoes the surface has a low profile. In the case of Pavonis Mons the average slope is only 4 degrees.The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 69000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, channels carved by water and lava, and a variety of other feature, THEMIS has imaged them all. For the next several months the image of the day will focus on the Tharsis volcanoes, the various chasmata of Valles Marineris, and the major dunes fields. We hope you enjoy these images!Orbit Number: 31330 Latitude: -1.26587 Longitude: 247.705 Instrument: VIS Captured: 2009-01-05 23:32Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
The season is officially spring on Mars in Inca City. This image was acquired by NASA's Mars Reconnaissance Orbiter. Large blotches of dust cover the araneiforms. | Map Projected Browse ImageClick on the image for larger versionIt is about two weeks later in Inca City and the season is officially spring. Numerous changes have occurred. Large blotches of dust cover the araneiforms. Dark spots on the ridge show places where the seasonal polar ice cap has ruptured, releasing gas and fine material from the surface below.At the bottom of the image fans point in more than one direction from a single source, showing that the wind has changed direction while gas and dust were flowing out. Was the flow continuous or has the vent opened and closed?HiRISE is one of six instruments on NASA's Mars Reconnaissance Orbiter. The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. | |
This landslide occurs in an unnamed crater on Mars southeast of Millochau Crater as seen by NASA's 2001 Mars Odyssey spacecraft. | Context image for PIA06088Crater LandslideThis landslide occurs in an unnamed crater southeast of Millochau Crater.Image information: VIS instrument. Latitude -24.4N, Longitude 87.5E. 17 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. | |
NASA's Mars Global Surveyor shows dark, windblown sand dunes have over-ridden a suite of low, somewhat rectilinear ridges on the floor of an impact crater on Mars. | MGS MOC Release No. MOC2-369, 23 May 2003Dark, windblown sand dunes have over-ridden a suite of low, somewhat rectilinear ridges on the floor of an impact crater near 36.5°S, 219.0° W, in this Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image acquired in May 2003. The dune field is located in Terra Cimmeria. The image is 1.2 km (3/4 mile) wide; sunlight illuminates the scene from the upper left. | |
The linear depression in this image from NASA's 2001 Mars Odyssey spacecraft is part of Nili Fossae. | Context imageThe linear depression in today's VIS image is part of Nili Fossae.Orbit Number: 60318 Latitude: 24.7944 Longitude: 80.7404 Instrument: VIS Captured: 2015-07-20 08:53Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
NASA's Mars Global Surveyor shows dark sand dunes overlying an eroded, layered substrate in Chasma Boreale, amid the materials of the martian north polar cap. | 9 February 2005 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows dark sand dunes overlying an eroded, layered substrate in Chasma Boreale, amid the materials of the martian north polar cap.Location near: 84.5°N, 358.3°W Image width: ~3.0 km (~1.9 mi) Illumination from: lower left Season: Northern Summer | |
NASA's Mars Global Surveyor shows gullies formed on an equator-facing slope among mounds in Acidalia Planitia. Similar gullies occur in a variety of settings at middle and polar latitudes in both martian hemispheres. | 20 May 2005This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows gullies formed on an equator-facing slope among mounds in Acidalia Planitia. Similar gullies occur in a variety of settings at middle and polar latitudes in both martian hemispheres.Location near: 49.8°N, 22.7°WImage width: ~3 km (~1.9 mi) Illumination from: lower left Season: Northern Summer | |
These dust avalanches occur in a crater within Iani Chaos on Mars as seen by NASA's 2001 Mars Odyssey spacecraft. | Context image for PIA02684Dust SlidesThese dust avalanches occur in a crater within Iani Chaos.Image information: VIS instrument. Latitude -0.7N, Longitude 35.8E. 18 meter/pixel resolution.Please see the THEMIS Data Citation Note 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. | |
NASA's Mars Global Surveyor shows | 25 March 2004This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a plethora of small wind tails or streaks in the lees of impact craters in northeastern Tharsis near 25.8°N, 89.0°W. The streak tails point toward the east/northeast (right), indicating that the dominant winds blow from the west/southwest (left). This February 2004 picture covers an area about 3 km (1.9 mi) across. Sunlight illuminates the scene from the lower left. | |
This image from NASA's Mars Reconnaissance Orbiter shows a dusty area of Mars. The dark streaks on the slopes are locations where the dust has slumped downhill revealing a less dusty surface underneath. | Map Projected Browse ImageClick on the image for larger versionMars is a dusty place and in some locations thick blankets of its characteristically red dust can slowly settle out of the atmosphere and accumulate on slopes. This dust is also a lot brighter than the dust-free terrain on Mars; so, if you scrape off the dust, you'll see a darker surface underneath.This particular image shows one of these dusty areas. The dark streaks on the slopes are locations where the dust has slumped downhill revealing a less dusty surface underneath. In some cases, these slope streaks might be triggered by Marsquakes or nearby meteorite impacts. Scientists think they form quickly: more like an avalanche than dust slowly creeping downhill.Look more closely and you'll notice that some streaks are darker than others. Dust is settling out of the atmosphere all the time and these dark streaks get slowly buried by fresh dust so that they fade back into their brighter redder surroundings. It's not certain how long this fading takes to happen, but it's probably close to a few decades.Dust is an important player in the weather and climate on Mars. Images like this are used to monitor slow changes in these streaks over time to better understand how much dust is settling on the surface.The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter Project and Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington. | |
NASA's Mars Global Surveyor shows sand dunes overlain by a layer of seasonal carbon dioxide frost in the north polar region of Mars. | 21 May 2006This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows sand dunes overlain by a layer of seasonal carbon dioxide frost in the north polar region of Mars. Sunlight illuminates the scene from the lower left, but slopes facing toward the upper right seem illuminated because of the thicker accumulation of frost on the slopes facing away from the sunlight.Location near: 76.3°N, 264.3°W Image width: ~3 km (~1.9 mi) Illumination from: lower left Season: Northern Winter | |
This image from NASA's Mars Odyssey shows numerous channels dissecting the inner rim of this unnamed crater in Noachis Terra. Several small, dark dunes are located in the center of the crater. | Context image for PIA11864ChannelsNumerous channels dissect the inner rim of this unnamed crater in Noachis Terra. Several small, dark dunes are located in the center of the crater.Image information: VIS instrument. Latitude -38.0N, Longitude 9.8E. 17 meter/pixel resolution.Please see the THEMIS Data Citation Note 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. | |
These layered deposits are located on the floor of a large canyon called Ganges Chasma which is a part of the Valles Marineris in this image captured by NASA's 2001 Mars Odyssey spacecraft. | (Released 29 March 2002)The ScienceThe Story These layered deposits are located on the floor of a large canyon called Ganges Chasma which is a part of the Valles Marineris. Dramatic layering can be seen throughout the deposit. Different styles of erosion are manifest in these different layers and at different locations within the layered material. For example, the southern portion of these deposits have a pronounced fluting, whereas in other areas the same layers are more intact. Relatively dark dunes and sand sheets can be observed surrounding the relatively brighter layered material in the upper right and lower portions of the image. Darker material also appears to mantle select areas of the layered deposits. The formation of the dunes is influenced by topography; this influence is best illustrated in the upper left of the image where a small hillock has interfered with the local wind flow. Impact craters of all sizes are noticeably absent in this image, indicating a relatively young age for this surface. This image is approximately 22 km wide and 60 km in length; north is toward the top.The StoryIf this wonderfully textured landform were on Earth, it would have to be designated as a "national park," much like the popular canyon parklands of the American Southwest. Look for the oblong plateau at the center right of this image, and see how the terrain descends from it on all sides. The southerly canyon wall (bottom third of the image) displays a visually beautiful canyon slope, with descending erosional flutes that cut pathways through the differently hued rock and mineral layers. While the northern side of the plateau might not look as dramatic, don't miss the dark-colored sand dunes that lie at the base of the canyon. Why did they form in just that place? To find out, look for the small hillock in the top left of the image that has interfered with the wind's flow, causing the ripply dunes to form. With so many interesting and physically stunning features, this spot will no doubt attract eager Mars tourists some day far in the future. | |
NASA's Mars Global Surveyor shows the Dao, Niger, and Harmakhis Valles on Mars. | The Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) opened its fourth year orbiting the red planet with this mid-autumn view of three major valley systems east of the Hellas plains. From left to right, the first major valley, Dao Vallis, runs diagonally from the upper left to just past the lower center of the image. Niger Vallis joins Dao Vallis just above the center of the frame. Harmakhis Vallis extends diagonally across the right half of the picture, toward the lower right. These valleys are believed by some to have been formed--at least in part--by large outbursts of liquid water some time far back in the martian past, though there is no way to know exactly how many hundreds of millions or billions of years ago this might have occurred. In each valley, water would have flowed toward the bottom of the image. Although their dimensions vary along their courses, the valleys are all roughly 1 km (0.6 miles) deep and range in width from about 40 km (25 miles) down to about 8 km (5 mi). Located around 40°S, 270°W, the picture covers an area approximately 800 km across and is illuminated by sunlight from the lower left. North is toward the left; the picture is a composite of red and blue wide angle images obtained by MOC on September 13, 2000. | |
This image from NASA's 2001 Mars Odyssey spacecraft shows fractures and channel-like features located in the Elysium Volcanic complex on Mars. | Context image for PIA09053FractureThe fractures and channel-like features in this image are located in the Elysium Volcanic complex.Image information: VIS instrument. Latitude 25.3N, Longitude 137.3E. 19 meter/pixel resolution.Please see the THEMIS Data Citation Note 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. | |
This image from NASA's Mars Odyssey shows a region of lava covered plains east of Olympus Mons. Winds are common in the area and have created windstreaks downwind of craters in the region and on the lava flows. | Context imageThis VIS image shows are region of lava covered plains east of Olympus Mons. Winds are common in the area and have created windstreaks downwind of craters in the region and on the lava flows.Orbit Number: 37693 Latitude: 22.596 Longitude: 240.567 Instrument: VIS Captured: 2010-06-13 23:39Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
The small channel and lava flows in this image NASA's 2001 Mars Odyssey spacecraft are located northeast of Olympus Mons. | Context imageThe small channel and lava flows in this VIS image are located northeast of Olympus Mons.Orbit Number: 53822 Latitude: 29.858 Longitude: 229.899 Instrument: VIS Captured: 2014-01-31 14:10Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, 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. | |
What Lies Below a Martian Ice Cap | Click on image for larger annotated versionThis image (top) taken by the Shallow Radar instrument on NASA's Mars Reconnaissance Orbiter reveals the layers of ice, sand and dust that make up the north polar ice cap on Mars. It is the most detailed look to date at the insides of this ice cap. The colored map below the radar picture shows the topography of the corresponding Martian terrain (red and white represent higher ground, and green and yellow lower).The radar image reveals four never-before-seen thick layers of ice and dust separated by layers of nearly pure ice. According to scientists, these thick ice-free layers represent approximately one-million-year-long cycles of climate change on Mars caused by variations in the planet's tilted axis and its eccentric orbit around the sun. Adding up the entire stack of ice gives an estimated age for the north polar ice cap of about 4 million years—a finding that agrees with previous theoretical estimates. The ice cap is about 2 kilometers (1.2 miles) thick.The radar picture also shows that the boundary between the ice layers and the surface of Mars underneath is relatively flat (bottom white line on the right). This implies that the surface of Mars is not sagging, or bending, under the weight of the ice cap—and this, in turn, suggests that the planet's lithosphere, a combination of the crust and the strong parts of the upper mantle, is thicker than previously thought.A thicker lithosphere on Mars means that temperatures increase more gradually with depth toward the interior. Temperatures warm enough for water to be liquid are therefore deeper than previously thought. Likewise, if liquid water does exist in aquifers below the surface of Mars, and if there are any organisms living in that water, they would have to be located deeper in the planet.The topography data are from Mars Orbiter Laser Altimeter, which was flown on NASA's Mars Global Surveyor mission.NPLD stands for the north polar layered deposits.BU stands for basal unit, an ice-sand deposit that lies beneath parts of the north polar layered deposits.The Shallow Radar instrument was provided by the Italian Space Agency. Its operations are led by the University of Rome and its data are analyzed by a joint U.S.-Italian science team. JPL, a division of the California Institute of Technology, Pasadena, manages the Mars Reconnaissance Orbiter for the NASA Science Mission Directorate, Washington. | |
The floor of Reull Vallis is filled with patterned material. The patterns indicate a volitile such as ice played a part in creating the interesting surface on Mars as seen by NASA's Mars Odyssey spacecraft. | Context image for PIA08640Reull VallisThe floor of Reull Vallis is filled with patterned material. The patterns indicate a volitile such as ice played a part in creating the interesting surface.Image information: VIS instrument. Latitude -40.3N, Longitude 109.1E. 17 meter/pixel resolution.Please see the THEMIS Data Citation Note 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. | |
This cylindrical projection was taken by the navigation camera onboard NASA's Mars Exploration Rover Opportunity. The view is a region dubbed 'Fram Crater' located .3 miles from 'Eagle Crater' and roughly 820 feet from 'Endurance Crater' (upper right). | This cylindrical-perspective projection was constructed from a sequence of four images taken by the navigation camera onboard the Mars Exploration Rover Opportunity. It was taken with the camera's left eye.The images were acquired on sol 85 of Opportunity's mission to Meridiani Planum. The camera acquired the images at approximately 14:28 local solar time, or around 6:30 a.m. Pacific Daylight Time, on April 20, 2004.The view is from the rover's new location, a region dubbed "Fram Crater" located some 450 meters (.3 miles) from "Eagle Crater" and roughly 250 meters (820 feet) from "Endurance Crater" (upper right).See PIA05783 for 3-D view and PIA05785 for right eye view of this left eye cylindrical-perspective projection. | |
This image from NASA's Mars Reconnaissance Orbiter spacecraft covers mesas, or high-standing plateaus, to the north and pits, or low-standing, depressions to the south. What formed these mesas and pits is a question not so easy to answer. | Map Projected Browse ImageClick on the image for larger versionWhat's up and what's down? This image covers mesas, or high-standing plateaus, to the north and pits, or low-standing, depressions to the south. If it looks the other way around, then you are not seeing the topography correctly.Remember that the Sun is coming from the left (west) at MRO's imaging time of about 3 p.m. What formed these mesas and pits is a question that is not so easy to answer. The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colo. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. |
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