MESSENGER: MErcury Surface, Space ENvironment, GEochemistry, and Ranging
| Date Created: February 10, 2012 Instrument: Mercury Dual Imaging System (MDIS) Latitude Range: 49.6° N to 60.9° N Longitude Range: 16.5° E to 48.5° E Resolution: 400 meters/pixel Scale: Hokusai, the large, fresh impact crater at top left, is 90 km (56 mi.) in diameter. Projection: Azimuthal equidistant
Of Interest: This image is a portion of the MDIS global mosaic basemap that was acquired during MESSENGER's first year in orbit. The scene shows a region of smooth, volcanic plains that have been heavily modified by tectonic structures termed "wrinkle ridges". Occurring on the Moon and Mars as well as on Mercury, wrinkle ridges are low, sinuous features that form when lavas cool and subside, causing the crust to contract horizontally. These landforms are often concentrated around buried crater rims, forming circular wrinkle ridges like those in the center right of the image.
While the innermost planet hosts thousands of wrinkle ridges, they are largely confined to its smooth plains, and are morphologically different to the larger, longer faults that comprise Mercury's fold-and-thrust belts. By studying the how different types of tectonic features are distributed across Mercury, MESSENGER scientists can begin to document in detail how the planet has deformed through time. | |
| Credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington |
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