The seismographs left on the moon's surface by the Apollo astronauts and the gravity measurements of the 1998 Lunar Prospector probe have provided enough data to explain why there are many
more craters on the moon's far side than on the near side.
Not exact matches
Since the 1960's scientists thought that only in permanently shadowed areas in
craters near the lunar poles was it cold enough to accumulate this volatile material, but recent observations by a number of spacecraft, including LRO, suggest that hydrogen
on the
moon is
more widespread.
In that sense, the researchers say, the
moon is unique: Its
craters are constantly erased by the solar system's most relentless volcanic activity — 25 times
more frequent than that seen
on Earth — which adds an estimated 1 centimeter of fresh material to Io's surface each year.
The kind of asteroid needed to form the Martian dichotomy would fall in between that size and those of the rocks that formed other large
craters, such as the South Pole — Aitken impact basin
on the
moon and the Hellas Basin in Mars's southern hemisphere, both
more than 1,30 miles (2,000 kilometers) wide.
Large
craters cover
more of the
moon's surface
on its nearside than its farside, according to new maps from NASA's GRAIL spacecrafts.
Maps from the GRAIL spacecrafts reveal
more large
craters (big circles) and thinner crust (blue)
on the
moon's nearside (left) than
on the farside (right), where the crust is thicker (red).
The strong reflection seen
on Mercury is too large to be caused by a momentary «glint» off a
crater wall, and when studied in
more detail, shares the characteristics of reflections from the water ice seen
on Mars and the icy
moons of Jupiter.