'Albedo' and the surface geology of the 'Moon's Near-side'

The nearside of the Moon using false colour to show the differences in albedo (reflection of sunlight) .
Image compiled from AVI video files - 66mm Altair Astro Refractor - QHY5-11 colour planetary camera - Credit: Archie Mendes

" The changes in albedo, quite literally reflect the variations in surface geology of the Moon. The  different  mineral content of the highlands (shades of green) and the Maria or Seas (shades of blue and red) is clearly displayed in the above colour enhanced images.

The lunar maria  have a lower albedo and therefore appear darker to the eye than do the highlands. They are generally lower lying and as a result of their younger age are less heavily cratered. The lunar maria cover approximately one third of the nearside and are large basaltic-lava filled plains. The majority of maria lavas formed between 3 and 3.5 billion years ago. A large amount of the maria were formed by lavas erupting in or flowing into very large impact basins. It should be noted that the impact basins are 500 million years older than the lava which fills them. There is therefore, no real evidence that the volcanism was connected to impact events. Oceanus Procellarum, the largest  Mare, does not correspond with any known impact basin.

The maria are predominantly basalt whilst the highlands are anorthosite composed of calcium-rich plagioclase feldspar. Plagioclase feldspar is mainly found in the lunar crust whilst pyroxene and olivine are primarily found in the underlying mantle. . With respect to the highlands, the maria are comprised from basaltic lava with higher abundances of olivine and pyroxene and less plagioclase. With respect to terrestrial lavas, the lunar lavas have lower viscosities and a lower iron content. Some mare lavas contain high levels of titanium (ilmenite)." - George Hammer - Geologist  

Credit: Wikipedia