

Because of its small size, the moon could never retain an atmosphere. Its surface gravity is only 0.2 that of Earth's and gas molecules simply escaped into space. Without an atmosphere, there are no winds or rain to erode the surface. The only factors that change the surface at all are heating and cooling of the rocks and the occasional impact.
The lunar surface
can be divided into two distinct regions, the lunar highlands and the lunar
lowlands. The lowlands are the smooth dark plains which have few craters.
We call these the lunar Maria, Mare from the Latin word for sea, because
it was first thought that these smooth areas were lunar seas. They are
really lowlands filled with ancient floods of dark lava. The first Apollo
mission landed on the Mare, and they found the surface covered with a thick
lava dust. The samples returned indicated that the lava solidified about
3.2
The lunar highlands
are about 3 km higher in elevation than the lowlands. These are the lighter
colored heavily cratered areas. It was because of the higher elevation
that these areas were not flooded with the basaltic lava. These areas are
therefore older than the lowlands. The last two Apollo missions landed
in these areas, though landing here was much trickier. These rocks proved
to be different in composition from the basaltic lava. Rocks here were
anorthosite, a mixture of aluminum and calcium silicates, less dense than
basalt.
Many lunar rocks have been altered from the extensive cratering. These rocks, called breccias, have been shattered fragments cemented back together. It is interesting to note that many people think that moon rocks must be light in color, no doubt because the moon looks so bright in the sky. In reality, all moon rock types are dark grayish brown in color!
Copyright © 1997 Kathy A. Miles and Charles F. Peters II