HRSC is a stereo camera system onboard Mars Express used to take angular pictures of geographic features on Mars. ESA then postprocesses these into 3D images.
The end result looks like these:
Rubble and boulder deposits in Reull Vallis
Ice flows have deposited rubble and boulders in the upper section of Reull Vallis outflow channel, some seven kilometres wide and 300 metres deep at this point, near to the Promethei Terra region that is. After the ice mass melted, a pattern was left in the sediments in which the movement of the glacier and its rocky cargo is clearly visible. A tributary valley flows into the main valley in the centre of the image.
Ophir Chasma, a northern parallel valley of the Valles Marineris
Perspective view of Ophir Chasma, a northern parallel valley of Valles Marineris.
Icefield in polar crater
Water ice at the bottom of a crater near the Martian north pole. In the centre of the crater, which is about 35 kilometres across, white water ice stands out clearly. The impact crater is located in the northern lowland area Vastitas Borealis. Water ice can remain in the centre of the crater throughout the year, as the temperature is low enough and atmospheric pressure is sufficient to prevent sublimation (direct transition from a solid to a gaseous state). At the time of image acquisition (later summer on Mars), carbon dioxide ice had already disappeared from the entire northern polar cap, leaving only water ice. The thickness of the ice is probably only in the decimetre range. This has been confirmed by some earlier measurements.
The Martian moon, Phobos
Black and white image of Phobos, a moon of Mars.
Martian North Pole - Chasma Boreale
Water ice in the northern polar region of Mars - perspective colour view.
More and in better resolution here: DLR Portal - Mars Express
Source: ESA/DLR/FU Berlin
The end result looks like these:
Rubble and boulder deposits in Reull Vallis
Ice flows have deposited rubble and boulders in the upper section of Reull Vallis outflow channel, some seven kilometres wide and 300 metres deep at this point, near to the Promethei Terra region that is. After the ice mass melted, a pattern was left in the sediments in which the movement of the glacier and its rocky cargo is clearly visible. A tributary valley flows into the main valley in the centre of the image.
Ophir Chasma, a northern parallel valley of the Valles Marineris
Perspective view of Ophir Chasma, a northern parallel valley of Valles Marineris.
Icefield in polar crater
Water ice at the bottom of a crater near the Martian north pole. In the centre of the crater, which is about 35 kilometres across, white water ice stands out clearly. The impact crater is located in the northern lowland area Vastitas Borealis. Water ice can remain in the centre of the crater throughout the year, as the temperature is low enough and atmospheric pressure is sufficient to prevent sublimation (direct transition from a solid to a gaseous state). At the time of image acquisition (later summer on Mars), carbon dioxide ice had already disappeared from the entire northern polar cap, leaving only water ice. The thickness of the ice is probably only in the decimetre range. This has been confirmed by some earlier measurements.
The Martian moon, Phobos
Black and white image of Phobos, a moon of Mars.
Martian North Pole - Chasma Boreale
Water ice in the northern polar region of Mars - perspective colour view.
More and in better resolution here: DLR Portal - Mars Express
Source: ESA/DLR/FU Berlin
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