Apollo 17

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The landing site selected for Apollo 17 was in the Taurus-Littrow Valley on the eastern rim of Mare Serenitatis. The two primary objectives were obtaining samples of ancient highland material that were older than the Imbrium impact and investigating the possibility of young, explosive volcanism in this region.

The mission lasted 12 days, with a stay on the lunar surface of 75 hours. During this time the crew embarked on three extravehicular activities, which lasted a total of 22 hours. They collected 741 individual rock and soil samples with a total mass of 111 kilograms.

Apollo 17 was launched on December 7th 1972.

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When you look at the Moon on a clear night with the naked eye, you can see colour variations. The overall pattern that they make is sometimes called ‘the man in the Moon’ because some people think they see a face. The lighter areas are the highlands and the darker areas are maria (mare is the singular form).

The lunar highlands represent the original lunar crust, as seen in the previous step. The oldest highland rocks are more than 4.15 billion years old and sometimes as old as 4.4 billion years, which is older than any rock found on Earth. They are mainly anorthosite, but also include dunite and gabbro with increasing depth. These are the oldest rocks on the Moon and are evidence for a magma ocean, as discussed earlier.

In contrast, the maria are basins filled in with basalt and were formed mostly between roughly 3.0 and 3.5 billion years ago. However, there are some small patches that are thought to be as young as around 1.0 billion years. The mare basalts are secondary to the Moon’s formation, in the sense that they did not form from the magma ocean stage like anorthosite, but by later heating and melting of the mantle in the same way that volcanoes are formed on Earth.

Two other types of deposit are found on the surface of the Moon:

regolith: the crushed remains of other rock types that coat much of the surface
breccia: a rock formed of regolith that has been welded together at high temperature and pressure.
Regolith is the mixture of dust, mineral fragments and rock fragments that lies on the surface. Breccia is formed in the explosions when large asteroids hit the Moon.

The Moon has no atmosphere, so even the smallest meteorites just millimetres across reach the surface and form craters. (Such meteorites are called micrometeorites.) Some of the Moon rocks returned to Earth by the Apollo astronauts have small pock marks formed when tiny particles hit them. Each is filled by a thin layer of rock that melted in the impact and then re-solidified.

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Apollo 17 crew: Harrison Schmitt, Gene Cernan & Ron Evans (courtesy of NASA)
Apollo 17 lunar module - Challenger (courtesy of NASA)
Apollo 17 Rover (courtesy of NASA)
Apollo 17 sampling (courtesy of NASA)
Apollo 17 Tracy's Rock (courtesy of NASA)
Apollo 17 sample location map

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When you look at the Moon on a clear night with the naked eye, you can see colour variations. The overall pattern that they make is sometimes called ‘the man in the Moon’ because some people think they see a face. The lighter areas are the highlands and the darker areas are maria (mare is the singular form).

The lunar highlands represent the original lunar crust, as seen in the previous step. The oldest highland rocks are more than 4.15 billion years old and sometimes as old as 4.4 billion years, which is older than any rock found on Earth. They are mainly anorthosite, but also include dunite and gabbro with increasing depth. These are the oldest rocks on the Moon and are evidence for a magma ocean, as discussed earlier.

In contrast, the maria are basins filled in with basalt and were formed mostly between roughly 3.0 and 3.5 billion years ago. However, there are some small patches that are thought to be as young as around 1.0 billion years. The mare basalts are secondary to the Moon’s formation, in the sense that they did not form from the magma ocean stage like anorthosite, but by later heating and melting of the mantle in the same way that volcanoes are formed on Earth.

Two other types of deposit are found on the surface of the Moon:

regolith: the crushed remains of other rock types that coat much of the surface
breccia: a rock formed of regolith that has been welded together at high temperature and pressure.
Regolith is the mixture of dust, mineral fragments and rock fragments that lies on the surface. Breccia is formed in the explosions when large asteroids hit the Moon.

The Moon has no atmosphere, so even the smallest meteorites just millimetres across reach the surface and form craters. (Such meteorites are called micrometeorites.) Some of the Moon rocks returned to Earth by the Apollo astronauts have small pock marks formed when tiny particles hit them. Each is filled by a thin layer of rock that melted in the impact and then re-solidified.