View allAll Photos Tagged MarsReconnaissanceOrbiter
Edited Mars Reconnaissance Orbiter image of part of Gale Crater and Curiosity sitting a bit above the middle of the image. Processing variant.
The yellow circle shows where you can see Curiosity.
This image, taken by HiRISE, shows a lobate tongue on the Northwest Hellas rim.
Lobate features such as these are located in the mid-latitudes (30-60 degrees), indicative of viscous flow, are reminiscent of terrestrial glaciers and have long been interpreted as evidence for subsurface ice.
Recent ground penetrating radar observations by SHARAD (Shallow Subsurface Radar) of other lobate features in this latitude belt also support the notion that these features have cores with ice.
Edited Mars Reconnaissance Orbiter PR image of a blue sand dune on Mars. Color/processing variant.
Image source: photojournal.jpl.nasa.gov/catalog/PIA22512
Original caption: Sand dunes often accumulate in the floors of craters. In this region of Lyot Crater NASA's Mars Reconnaissance Orbiter (MRO) shows a field of classic barchan dunes.
Just to the south of the group of barchan dunes is one large dune with a more complex structure. This particular dune, appearing like turquoise blue in enhanced color, is made of finer material and/or has a different composition than the surrounding.
The map is projected above at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 34.7 centimeters (13.7 inches) per pixel (with 1 x 1 binning); objects on the order of 104 centimeters (40.9 inches) across are resolved.] North is up.
This is a stereo pair with ESP_053406_2295.
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 Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.
Image Credit:
NASA/JPL-Caltech/Univ. of Arizona
Image Addition Date:
2018-06-11
Edited Mars Reconnaissance Orbiter image of a mound surrounded by (and affecting) an ancient flow of lava.
Edited Mars Reconnaissance Orbiter image (very big!) of lobes of material in a crater on Mars. Color/processed variant.
Edited Mars Reconnaissance Orbiter image of part of Candor Chasma showing swirly rock and sand layers. Color/processing variant.
Edited Mars Reconnaissance Orbiter image of part of Gale Crater and Curiosity sitting a bit above the middle of the image.
This is probably the largest (in terms of file size) image I've ever uploaded to Flickr.
Edited Mars Reconnaissance Orbiter image of a small mound (for unmeasured amounts of "small") mound in Chryse Planitia.
Edited Mars Reconnaissance Orbiter image of a possible location of a geyser on Mars (but no geyser visible).
Edited Mars Reconnaissance Orbiter image of part of Candor Chasma showing swirly rock and sand layers.
Although the rim of this well-preserved crater and its smooth walls are very impressive, note also the spectacular collection of ridges draping the underlying topography on the floor of this crater.
What can account for the formation of the terrain at the crater floor? One possible reason might be the former icy flows at this latitude. High-resolution images like this can give us better insight
into these features.
Edited Mars Reconnaissance Orbiter PR image layers of sulfates with varying levels of hydration on the surface of Mars.
Image source: photojournal.jpl.nasa.gov/catalog/PIA21935
Original caption: In this image from NASA's Mars Reconnaissance Orbiter, layering within the light-toned sulfate deposit is the result of different states of hydration. Some of the layers have sulfates with little water (known as monohydrated sulfates) whereas other layers have higher amounts of water (called polyhydrated sulfates). The different amounts of water within the sulfates may reflect changes in the water chemistry during deposition of the sulfates, or may have occurred after the sulfates were laid down when heat or pressure forced the water out of some layers, causing a decrease in the hydration state.
Many locations on Mars have sulfates, which are sedimentary rocks formed in water. Within Valles Marineris, the large canyon system that cuts across the planet, there are big and thick sequences of sulfates.
The CRISM instrument on MRO is crucial for telling scientists which type of sulfate is associated with each layer, because each hydration state will produce a spectrum with absorptions at specific wavelengths depending upon the amount of water contained within the sulfate.
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 Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.
Image Credit:
NASA/JPL-Caltech/Univ. of Arizona
Image Addition Date:
2017-09-04
Edited Mars Reconnaissance Orbiter image of part of Gale Crater and Curiosity sitting a bit above the middle of the image. Processing variant.
Edited Mars Reconnaissance Orbiter image of Shalbatana Valles on Mars. Color/processing variant.
Image source: photojournal.jpl.nasa.gov/catalog/PIA22182
Original caption: Layers, probably sedimentary in origin, have undergone extensive erosion in this image from NASA's Mars Reconnaissance Orbiter (MRO) of Shalbatana Valles, a prominent channel that cuts through Xanthe Terra.
This erosion has produced several small mesas and exposed light-toned material that may differ in composition from the surrounding material.
The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 27.5 centimeters (10.8 inches) per pixel (with 1 x 1 binning); objects on the order of 82 centimeters (32.3 inches) across are resolved.] North is up.
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 Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.
Image Credit:
NASA/JPL-Caltech/Univ. of Arizona
Image Addition Date:
2018-01-23
Edited Mars Reconnaissance Orbiter image of snow (I presume carbon dioxide snow but certainly could be wrong) on the tops of sand dunes on Mars. Color/processing variant, cropped to better show the snow.
Edited Mars Reconnaissance Orbiter image of the monitoring of slopes in what looks like a crater. Color variant.
Edited Mars Reconnaissance Orbiter image of avalanches from a cliff on a the north polar ice cap on Mars. (Larger version of what I posted earlier.) Inverted grayscale variant.
Edited Mars Reconnaissance Orbiter image of a crater floor in Tempe Fossae. Color/processing variant.
The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) took this image of sulfate- and pyroxene-containing deposits in the Candor Chasma region of Mars at 0747 UTC (2:47 a.m. EST) on December 2, 2006, near 6.7 degrees south latitude, 75.8 degrees west longitude. The image was taken in 544 colors covering 0.36-3.92 micrometers, and shows features as small as 40 meters (132 feet) across. The image is about 10 kilometers (6.2 miles) wide at its narrowest point. The top panel in the montage above illustrates the location of CRISM data on a mosaic taken by the Mars Odyssey spacecraft's Thermal Emission Imaging System (THEMIS). CRISM data cover an area centered on the southwestern part of Candor Chasma, where highland crust was depressed by faulting and buried by a kilometers-thick stack of layered deposits. The bottom two images are views of CRISM data. The lower left image is an infrared false color image, while at lower right is a spectral image that illustrates the distribution of sulfates in the layered deposits, the olivine and pyroxene that make up the faulted highland crust, and highcalcium pyroxene in the highland crust.
Edited Mars Reconnaissance Orbiter image by way of the European Space Agency of Oxia Planum on Mars, which is a leading candidate for the landing spot for the ExoMars rover in the future.
Edited Mars Reconnaissance Orbiter image of a crater with sand dunes at the bottom, being monitored for slope changes.
Edited Mars Reconnaissance Orbiter image of the suspected landing site of the European Space Agency's Beagle 2 lander (which failed before or on landing).
Edited Mars Reconnaissance Orbiter image of a crater on Mars in grayscale with a strip of color imagery overlaid it, showing the pretty (if subtle (at least until I get a hold of it)) colors. Color/processing variant.
Edited Mars Reconnaissance Orbiter PR image of a layer of rocky material cut by some process (perhaps flowing water a billion or two years ago) and now filled by sand dunes. Inverted Grayscale variant.
Edited Mars Reconnaissance Orbiter image of a lava-filled crater (long since cooled off) in Elysium Planitia.
Edited NASA PR image from Mars Reconnaissance Orbiter showing the Curiosity Rover near the base of Mount Sharp in Gale Crater. Inverted grayscale variant.
Image source: photojournal.jpl.nasa.gov/catalog/PIA23341
Original caption: NASA's Curiosity Mars rover can be seen in this image taken from space on May 31, 2019, by the High Resolution Imaging Science Experiment (HiRISE) camera aboard the Mars Reconnaissance Orbiter (MRO). In the image, Curiosity appears as a bluish speck.
The image shows Curiosity at a location called "Woodland Bay." It's just one of many stops the rover has made in an area referred to as the "clay-bearing unit" on the side of Mount Sharp, a 3-mile-tall (5-kilometer-tall) mountain inside of Gale Crater.
Look carefully at the inset image, and you can make out what it is likely Curiosity's "head," technically known as the remote sensing mast. A bright spot appears in the upper-left corner of the rover. At the time this image was acquired, the rover was facing 65 degrees counterclockwise from north, which would put the mast in about the right location to produce this bright spot.
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 Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.
Image Credit:
NASA/JPL-Caltech
Image Addition Date:
2019-07-12
Edited NASA PR image from Mars Reconnaissance Orbiter showing the Curiosity Rover near the base of Mount Sharp in Gale Crater. Color/processing variant.
Image source: photojournal.jpl.nasa.gov/catalog/PIA23341
Original caption: NASA's Curiosity Mars rover can be seen in this image taken from space on May 31, 2019, by the High Resolution Imaging Science Experiment (HiRISE) camera aboard the Mars Reconnaissance Orbiter (MRO). In the image, Curiosity appears as a bluish speck.
The image shows Curiosity at a location called "Woodland Bay." It's just one of many stops the rover has made in an area referred to as the "clay-bearing unit" on the side of Mount Sharp, a 3-mile-tall (5-kilometer-tall) mountain inside of Gale Crater.
Look carefully at the inset image, and you can make out what it is likely Curiosity's "head," technically known as the remote sensing mast. A bright spot appears in the upper-left corner of the rover. At the time this image was acquired, the rover was facing 65 degrees counterclockwise from north, which would put the mast in about the right location to produce this bright spot.
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 Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.
Image Credit:
NASA/JPL-Caltech
Image Addition Date:
2019-07-12
Edited Mars Reconnaissance Orbiter image of a crater on Mars whose slopes are being monitored for gully formation (a sign that something slide down the crater wall). Converted into a round image because, uh, it was fun. Actually, the result reminds me of a small moon of Jupiter or Saturn...
Edited Mars Reconnaissance Orbiter PR image of sand dunes in the center of Juventae Chasma.
Original caption: The ultimate origin of the sediment that forms Martian dunes has long been debated. While sand dunes on Earth are primarily sourced by quartz-bearing components of granitic continental crust, it's often suggested that sand on Mars derives from eroded volcanic flows or sedimentary deposits, but exact sources are often vague.
This image reveals a unique situation where this small dune field occurs along the summit of the large 1-mile-tall mound near the center of Juventae Chasma. The layered mound slopes are far too steep for dunes to climb, and bedform sand is unlikely to come from purely airborne material. Instead, the mound's summit displays several dark-toned, mantled deposits that are adjacent to the dunes and appear to be eroding into fans of sandy material.
Along with local HiRISE images, spectral data from other instruments on MRO have confirmed such units are likely to be the sand source for these mound summit dunes and reveal how landscape evolution on Mars might occur.
The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 27.8 centimeters (10.9 inches) per pixel (with 1 x 1 binning); objects on the order of 83 centimeters (32.7 inches) across are resolved.] North is up.
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 Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.
Image Credit:
NASA/JPL-Caltech/Univ. of Arizona
Image Addition Date:
2018-10-01
This graphic illustrates where Mars mineral-mapping from orbit has detected a few minerals -- sulfates (blue) and iron oxides (pink) -- that can indicate where a volcano erupted beneath an ice sheet.
These mountains are in a region called Sisyphi Montes. In this graphic, the base image shows a portion of the region about 130 miles (230 kilometers) across, centered at 17.73 degrees east longitude, 63.46 degrees south latitude. Red outlines indicate possible subglacial volcanic structures. CRISM data are presented in the overlay box at upper right, with an indication of the ground area covered by this CRISM observation. The color key at upper left shows how the spectrometer data correspond to the presence of sulfates and iron oxide minerals, which are characteristic of subglacial volcanism sites on Earth.
Edited Mars Reconnaissance Orbiter image of many many dust devil tracks messing up the surface of Mars.