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Many martian dunes strongly resemble terrestrial dunes but images acquired by the High-Resolution Imaging Science Experiment on the Mars Reconnaissance Orbiter have shown that martian dunes in the north polar region are subject to modification via grainflow triggered by seasonal CO 2 sublimation, a process not seen on Earth. [12]
Areography, also known as the geography of Mars, is a subfield of planetary science that entails the delineation and characterization of regions on Mars. [1] [2] [3] Areography is mainly focused on what is called physical geography on Earth; that is the distribution of physical features across Mars and their cartographic representations.
Compared to Earth's atmosphere, thermal tides have a larger influence on the Martian atmosphere because of the stronger diurnal temperature contrast. [168] The surface pressure measured by Mars rovers showed clear signals of thermal tides, although the variation also depends on the shape of the planet's surface and the amount of suspended dust ...
Mars is the fourth planet from the Sun.The surface of Mars is orange-red because it is covered in iron(III) oxide dust, giving it the nickname "the Red Planet". [22] [23] Mars is among the brightest objects in Earth's sky, and its high-contrast albedo features have made it a common subject for telescope viewing.
The geology of Mars is the scientific study of the surface, crust, and interior of the planet Mars. It emphasizes the composition, structure, history, and physical processes that shape the planet. It emphasizes the composition, structure, history, and physical processes that shape the planet.
Fretted terrain – Surface feature common to certain areas of Mars; Geology of Mars – Scientific study of the surface, crust, and interior of the planet Mars; Glacier – Persistent body of ice that moves downhill under its own weight; Glaciers on Mars – Extraterrestrial bodies of ice; Lobate debris apron – Geological features on Mars
Topographic map of Mars showing the highland-lowland boundary marked in yellow, and the Tharsis rise outlined in red (USGS, 2014).[1]Like the Earth, the crustal properties and structure of the surface of Mars are thought to have evolved through time; in other words, as on Earth, tectonic processes have shaped the planet.
The average surface pressure on Mars is 0.6-0.9 kPa, compared to about 101 kPa for Earth. This results in a much lower atmospheric thermal inertia, and as a consequence Mars is subject to strong thermal tides that can change total atmospheric pressure by up to 10%. The thin atmosphere also increases the variability of the planet's temperature.