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Viking MDIM of Mare Tyrrhenum quadrangle. Hesperia is the intermediate-toned (dusky) region (left of center) lying between the darker regions Mare Tyr
Viking MDIM of Mare Tyrrhenum quadrangle. Hesperia is the intermediate-toned (dusky) region (left of center) lying between the darker regions Mare Tyrrhenum (left) and Mare Cimmerium (right).
Closeup of the surface of northwestern Hesperia Planum, as seen by HiRISE camera on Mars Reconnaissance Orbiter (MRO).
Closeup of the surface of northwestern Hesperia Planum, as seen by HiRISE camera on Mars Reconnaissance Orbiter (MRO).
Viking orbiter view of wrinkle ridges in Hesperia Planum. North is at upper left. Image is about 107 km (66 mi) across.
Viking orbiter view of wrinkle ridges in Hesperia Planum. North is at upper left. Image is about 107 km (66 mi) across.
THEMIS daytime IR mosaic image of Tyrrhenus Mons. This ancient, eroded volcano was nicknamed the Dandelion when first seen in Mariner 9 images.
THEMIS daytime IR mosaic image of Tyrrhenus Mons. This ancient, eroded volcano was nicknamed the Dandelion when first seen in Mariner 9 images.
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HiRISE image illustrating superpositioning, a principle that lets geologists determine the relative ages of surface units. The dark-toned lava flow ov
HiRISE image illustrating superpositioning, a principle that lets geologists determine the relative ages of surface units. The dark-toned lava flow overlies (is younger than) the light-toned, more heavily cratered terrain at right. The ejecta of the crater at center overlies both units, indicating that the crater is the youngest feature in the image. (See cross section, above right.)
Geologic contact of Noachian and Hesperian Systems. Hesperian ridged plains (Hr) embay and overlie older Noachian cratered plateau materials (Npl). Th
Geologic contact of Noachian and Hesperian Systems. Hesperian ridged plains (Hr) embay and overlie older Noachian cratered plateau materials (Npl). The ridged plains partially bury many of the old Noachian-aged craters. Image is THEMIS IR mosaic, based on similar Viking photo shown in Tanaka et al. (1992), Fig. 1a, p. 352.
Viking orbiter view of Hesperian-aged surface in Terra Meridiani. The small impact craters date back to the Hesperian Period and appear crisp despite
Viking orbiter view of Hesperian-aged surface in Terra Meridiani. The small impact craters date back to the Hesperian Period and appear crisp despite their great age. This image indicates that erosion on Mars has been very slow since the end of the Noachian. Image is 17 km across and based on Carr, 1996, p. 134, Fig. 6-8.