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Mars
Valles Marineris, taken by the Viking 1 probe
Valles Marineris, taken by the Viking 1 probe
Artist concept showing sand-laden jets erupting from Martian geysers (published by NASA; artist: Ron Miller)
Artist concept showing sand-laden jets erupting from Martian geysers (published by NASA; artist: Ron Miller)
Mars without a dust storm in June 2001 (on left) and with a global dust storm in July 2001 (on right), as seen by Mars Global Surveyor
Mars without a dust storm in June 2001 (on left) and with a global dust storm in July 2001 (on right), as seen by Mars Global Surveyor
Difference of dust and water clouds: the yellow cloud at the bottom center of the image is a large dust cloud, the other white clouds are water clouds
Difference of dust and water clouds: the yellow cloud at the bottom center of the image is a large dust cloud, the other white clouds are water clouds.
Mariner 9 image of Ascraeus Mons. This is one of the first images to show that Mars has large volcanoes.
Mariner 9 image of Ascraeus Mons. This is one of the first images to show that Mars has large volcanoes.
THEMIS image of lava flows with lobate edges (from Arsia Mons volcano)
THEMIS image of lava flows with lobate edges (from Arsia Mons volcano)
First X-ray diffraction view of Martian soil – CheMin analysis reveals minerals (including feldspar, pyroxenes and olivine) suggestive of "weathered b
First X-ray diffraction view of Martian soil – CheMin analysis reveals minerals (including feldspar, pyroxenes and olivine) suggestive of "weathered basaltic soils" of volcanoes in Hawaii (Curiosity rover at "Rocknest", 2012). Each ring is a diffraction peak that corresponds to a specific atom-atom distance, which are unique enough to identify minerals. Smaller rings corresponds to larger features and vice versa.
Viking orbiter image of the three Tharsis Montes: Arsia Mons (bottom), Pavonis Mons (center), and Ascraeus Mons (top)
Viking orbiter image of the three Tharsis Montes: Arsia Mons (bottom), Pavonis Mons (center), and Ascraeus Mons (top)