Mare Moscoviense Flyover
Provided by Japan Aerospace Exploration Agency (JAXA)
Geology
Mare Moscoviense is the largest mare on the lunar farside in the area beyond the rim of the South Pole-Aitken Basin. The mare fills the ~210 km diameter inner ring of the Moscoviense impact basin, which is >445 km in diameter and possibly 550 km in diameter. The mare appears to be formed by at least three basalt eruptions. Crater densities measured by Haruyama et al. (2009) suggest one of those mare flows erupted ~3.5 billion years ago and that the youngest flow erupted ~2.57 billion years ago. This implies basalt eruptions occurred over a period of nearly 1 billion years. Many of the craters that puncture the mare are fresh looking and relatively young. Some craters, however, are nearly filled by the youngest mare flows, indicating that they were produced by impacting asteroids after the first lava flow erupted and before the last flow erupted. The mare surface is much younger than the surrounding basin highlands, which can easily be seen by the sharp contrast in crater densities on those different surfaces.
Processing
The imagery for this virtual flyover comes from the KAGUYA Terrain Camera (TC). The TC is a push-broom stereoscopic imager with forward-looking and aft-looking optical heads with slant angles of ± 15° from nadir. The spatial resolution of TC is 10 m/pixel from the KAGUYA nominal altitude of 100 km. The digital terrain model underlying the virtual flyover is derived from the TC stereoscopic imagery of the region. For more information about the Terrain Camera (TC) and other KAGUYA instruments please visit JAXA's KAGUYA website.
Credit
Provided by Japan Aerospace Exploration Agency (JAXA)
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