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Changes at Edges of Dark Dunes in Nili Patera, Mars
Changes at Edges of Dark Dunes in Nili Patera, Mars
Dunes and Inverted Crater in Arabia Terra
Dunes and Inverted Crater in Arabia Terra
Glacial Ice Deposits in Mid-Latitudes of Mars
Glacial Ice Deposits in Mid-Latitudes of Mars
Stages in the seasonal disappearance of surface ice from the ground around the Phoenix Mars Lander are visible in these images taken on Feb. 8, 2010, (left) and Feb. 25, 2010, during springtime on northern Mars.
Ice Around Phoenix Lander Continues to Lessen in Spring
A digital terrain model generated from a stereo pair of images provides this synthesized, oblique view of a portion of the wall terraces of Mojave Crater in the Xanthe Terra region of Mars.
Terrain Model of Mars' Mojave Crater
NASA's Phoenix Mars Lander, its backshell and its heatshield are visible within this enhanced-color image of the Phoenix landing site taken on Jan. 6, 2010 by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter. With early spring at the Phoenix landing site comes progressive sublimation of carbon-dioxide frost that has blanketed the lander and surrounding terrain throughout the winter. During the long polar-winter night, atmospheric carbon dioxide freezes onto the surface, building up a layer of frost roughly 30 centimeters (about one foot) thick. In the spring this frost returns to atmosphere gas (sublimates) over the course of several months. This image, part of a seasonal frost monitoring sequence, shows some areas of bare ground are beginning to be exposed. However, extensive frost patches remain in the topographic lows, such as the troughs of the local polygonally patterned surface.
Phoenix Lander Amid Disappearing Spring Ice
Polar Layered Deposits Stratigraphy Near Chasma Australe
Polar Layered Deposits Stratigraphy Near Chasma Australe
Well-Preserved Crater with Central Peak in Chryse Planitia
Well-Preserved Crater with Central Peak in Chryse Planitia
Gullies and Flow Features along Crater Wall in Promethei Terra
Gullies and Flow Features along Crater Wall in Promethei Terra
Syrtis Major Region
Syrtis Major Region
This image shows an outcrop of the south polar layered deposits (SPLD). The SPLD consist of layers of ice and admixed dust and make up the bulk of the dome-shaped Planum Australe. Planum Australe is, in some ways, analogous to the Antarctic ice sheet. Troughs and scarps carved into Planum Australe by erosional processes have exposed SPLD layers within it. In this image, the darkest area at the bottom of the image is the bottom of the scarp. Except for the dark material at the bottom of the slope, much of the changes in brightness in this image are due to the lighting angle, the direction from which the sun is illuminating the slope. Much like ice cores from Greenland and Antarctica and deep sea sediment cores, the icy-dusty layers of the SPLD may have preserved a record of recent Mars climate history. Understanding that record is a complex process and involves, among many other types of analyses, examining the differences and similarities in appearance between each layer and attempting to classify layer types. This image shows nice examples of different layer textures. But what is especially interesting about this image are the faults cutting through the layers. These faults appear as diagonal lines, on either side of which, the layering is offset. Note that the faults are not clean, single lines, but appear in long groups of short lines. What caused these faults is still under investigation, but, among other possibilities, they could be related to an earlier time when temperatures were higher and the ice was flowing at a much faster rate than it is today.
Troughs and Scarps in Planum Australe
Geologically young gullies are a prime target for the HiRISE camera. Gullies are located in a variety of settings and are found all over Mars. This "ring trough" or eroded pit crater, is located in the rugged southern highland terrain known as Noachis Terra. The HiRISE image shows the layered, boulder-rich wall rock facing to the northeast and gullies that are transporting material downslope. The material collects into debris aprons along the walls, which often exhibit narrow channels along its surface.
Gullies on Southwest Slope of Ring Trough in Noachis Terra
Impact Crater in Tempe Terra
Impact Crater in Tempe Terra
Drainage Near Crater in Terra Sabaea.
Drainage Near Crater in Terra Sabaea
Gullied Crater Slope with Rocky Outcrops Northeast of Hellas Region
Gullied Crater Slope with Rocky Outcrops Northeast of Hellas Region
Endeavour Crater in Context
Endeavour Crater in Context
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A Martian Valentine for 2009
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Martian Weather Activity on Short Timescales
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Sand Dunes and Ripples in Proctor Crater, Mars
These color-enhanced views of Deimos, the smaller ot the two moons of Mars, result from imaging on Feb. 21, 2009.
Martian Moon Deimos in High Resolution
This image shows an exposure of layered rock that exhibits a type of fracturing -- called columnar jointing -- that results when cooling lava contracts.
First Observation of Columnar Jointing on Mars
This image shows part of the floor of an impact crater on the northern rim of the giant Hellas Basin. Hellas includes the lowest elevations on Mars, and may have once held lakes or seas; layered rock outcrops occur around much of the edge of the basin. At this site, a large impact crater (about 90 kilometers across) was partly filled by layered rocks. These rocks on the crater floor are now eroding and forming strange pits. Here, the layers are mostly exposed on a steep slope which cuts across much of the image. On this slope, they crop out as rocky stripes, some continuous and others not. The material between the stripes is mostly covered by debris, but some areas of exposed rock are visible. The slope is capped by a thick, continuous layer that armors it against erosion; once this cap is gone, the lower material is removed rapidly, forming the steep slope. At the base of this slope, rocks on the floor of the pit appear bright and heavily fragmented by cracks known as joints. The variation in rock types suggests that the rocks here were deposited by multiple processes or in different environments. Sites like this may preserve a record of conditions on early Mars.
Layered Outcrops on Crater Floor
This fresh crater is located in the northern mid-latitudes. It is designated as fresh because of its very sharp rim. The crater has experienced some modification since it formed, including a few tiny craters on the south wall. The rough texture of the floor is suggestive of ground ice, which is expected to exist in the mid-latitudes. Ground ice aids gravity in moving material from the crater walls towards the center. Material is visible slumping off the northwest crater wall in this fashion. The wavy texture of the center of the crater floor suggests that material has been transported from the walls and merged in the center.
Fresh Impact Crater in Utopia Planitia
Periodic Layering in Martian Sedimentary Rocks
Periodic Layering in Martian Sedimentary Rocks
This image shows layers of rock stacked like a staircase, their edges extending diagonally from top left to bottom right and stepping downward from the lower left to the top right. At the far left of the image is an eroded, round crater filled with a row of nearly parallel sand dunes. To the right of the crater, a pinkish-colored layer of light-toned rock within the staircase contains opal.
A Gem of a Find
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