Get closer to the surface with these stunning images of the surface of Mars.
This image pack contains 3 UHD 8K images from HiRISE (High Resolution Imaging Science Experiment) onboard the Mars Reconnaissance Orbiter, NASA. HiRISE is the most powerful camera ever sent to another planet, letting us see the surface of Mars at 30 cm/pixel.
Each image has been refined using Topaz Labs state of the art image upscaler Gigapixel AI to further refine the image for high quality printing at 300dpi. Further refinements are made using Topaz Labs Sharpener AI and Denoiser AI tools.
Martian Internet then meticulously scours the image by eye to ensure that interpolation is smooth and there are no artefacts.
:. 7680×4320 8K ultra high definition resolution
:. PNG Lossless file format
:. 300 dpi industry standard pixel density for high quality large prints
North Polar Scarp
Sculpted Cool – This is part of a steep scarp within the North Polar layered deposits. Scarps like this have the potential for active avalanches.(319 km above the surface, less than 10 km left to right.)
Polar Sand Dunes
Mars has a vast sea of sand dunes in the high latitude region encircling its north polar cap, known as the North Polar erg. These dunes are made up of basalt and gypsum sand grains. In some regions of the North Polar erg where the sand supply is limited they take on an elongated crescent shape. The icy ground that the dunes are on top of has irregular polygonal patterns. In other areas with an abundant supply of sand the dunes are continuous. Image is less than 1 km (0.67 mi) top to bottom and is 320 km (199 mi) above the surface.
Meridiani Planum
This image of the Meridani Planum is an example of “Mass wasting and Slope Processes“, a broad science theme dealing with the downhill movement of rocks and debris. Many different types of mass movement fall into the general category of mass wasting, from large landslides and debris avalanches to rockfalls, debris flows and soil creep. On Mars, mass wasting landforms are seen at a range of scales, from giant rock avalanches to tiny slumps and single rockfalls. One of the most exciting discoveries of recent spacecraft exploration is the assortment of changes that we can see occurring on Martian slopes today. Dark flows termed “Recurring slope lineae” (or RSL) are seen slowly advancing down warm slopes in the summer. New mass movements are seen in Martian gully landforms, and generally occur in the late winter or spring, potentially triggered by the carbon dioxide frost that coats the surface in the winter. Avalanches are seen in action on steep slopes at the edge of the North Polar Layered Deposits when they are warming in Northern spring. Slope streaks are seen in dusty regions of Mars and are thought to be the result of dust avalanches, sometimes triggered by impact craters or rockfalls. Image acquired: November 2016, approximately 269 kilometers above the surface. Scene is 5 km across.
Image Credit: NASA/JPL/UArizona
Modification: © 2022 Martian Internet
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