This region extends from the Birkhoff Basin to the Hertzsprung Basin (see Figure 10.5 for detailed coverage).
The Eastern Far Side Region was photographed by Lunar Orbiter 5 in order to complete coverage of the far side. Because of mission constraints, the photographs were taken at an early, high orbit, which reduced the resolution. That is n why this chapter covers a relatively large area with the usual oo number of photographs.
0 Remote sensing instruments have established that the area is unusually uniform in the distribution of chemical elements of and minerals. Few areas of mare basalt have been identified. Apart from topography, the only major patterns visible to remote sensing are due to bright rays associated with young -§ craters like Jackson and Ohm. The upper layers of the surface have been deposited by ejecta from a number of basins. As in ° the other far side regions, the lowest layers above the pristine he crust were deposited by the proposed Near Side Megabasin and the South Pole-Aitkcen Basin early in the pre-Nectarian Period, then came the Coulomb-Sarton Basin and the Birkhoff Basin later in the pre-Nectarian Period. The Korolev Basin came in the Nectarian Period and the Hertzsprung Basin came later in the Nectarian Period; its ejecta blanket overlays that of Korolev. Light ejecta came from the Imbrium Basin at the start of the Early Imbrian Period. Finally, the Orientale Basin covered most of this region at the end of the Early Imbrian Period.
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