Apollo Instrument Experiments - Remote Sensing Application - Completely Remote Sensing, GPS, and GPS Tutorial
Apollo Instrument Experiments

The top priority for Apollo 11 was just to get there (and back). Once successful, the principal effort was directed towards collecting rock/soil samples. But Apollo 11, and all of the subsequent 5 missions that touched down on the Moon, carried a wide variety of scientific instruments selected and designed to measure a diverse set of physical and chemical properties of the Moon - locally, internally, and in its external surroundings. These fell into two categories: equipment mounted in the SIM (Scientific Instruments Module) of the orbiting CSM (Command and Service Module) and surface-emplaced equipment . The instruments used in both activities and the missions on which they were employed are summarized in this table.

Table of Apollo orbital and surface experiments.

The CSM opens its SIM outer sheath to expose the instruments to the lunar surface, as seen in this photo:

Apollo 15 CSM with its SIM Bay open.

The instruments for the Apollo 15 SIM are labeled in this diagram:

The SIM instrument package on Apollo 15.

Many significant results have stemmed from operating both the orbital and the ground instruments. But in this Tutorial we are limited to just a few examples. First, several orbital findings, shown as images with minimal comment.

The x-ray fluorescence spectrometer is capable of determining fairly accurately the amounts of a number of elements, including most of the major ones in rocks and some minor or trace elements. This plot shows the variation in Al/Si ratio along paths traversed by the Apollo 14 CSM.

Al/Si ratios for the lunar surface under the Apollo 14 CSM, as measured by x-ray fluorescence spectroscopy.

The Moon has a weak magnetic field but one not caused by rotation of a melted zone like that on Earth. It has a small metallic core (about 20% of the radius of the entire Moon) but that is not now suffiently fluid (the outer part may be "mushy") to generate an internal field is probably ruled out. This core was developed when the Moon had accreted and then probably melted more or less completely. The differentiation, like that of the early Earth, yield a crust (anorthositic), a thick mantle, and a small iron core. This illustration is one model of the Moon's interior:

The lunar interior.

The present weak field is a "fossil" or paleomagnetic one. The source of the field may be remanent magnetism in the lunar rocks themselves, possibly induced by interactions with solar and/or terrestrial magnetic fields or induced in the rocks when/if the lunar core was once fluid in the early history of the Moon. That the Sun's magnetic field plays a large role in the current state of the Moon's field is demonstrated by the similarities (general correspondence) in the Β magnetic field vector onboard an Earth-orbiting Explorer 35 and simultaneous measurements on the ground at the Apollo 12 site.

Magnetic fields measured simultaneously by Explorer 35 and at the Apollo 12 site.

Magnetic field strengths as low as 38 and high as 341 γ were measured at the Apollo ground stations. Thus, there is notably variation from one area of the Moon to another. This is what Apollo 16 measured from orbit using the SIM magnetometer to show surface variations of two magnetic components:

Laser altimeters operated from several of the CSM's. Here is an Apollo 15 profile along one complete circumlunar orbit, expressing differences in elevation as ΔR's, or variations in radius from the mean lunar spheroid.

Apollo 15 elevation profile along a single orbit path, measured by CSM's laser altimeter.

Variations in lunar gravity were another important parameter to measure in detail. One way to do this is to use radio tracking to determine changes in spacecraft speeds which result almost entirely from fluctuations in gravitational pull. The S-band (radio) Transponder on Apollo 15 was used to obtain these measurements, from which these two profiles (and others) resulted:

S-band Transponder plots of variations in CSM velocities while passing over the lunar surface, translated in changes in gravitational magnitudes (in milligals).

The gravitational highs over Mare Serenitatus and Mare Crisium correspond to features earlier identified and named mascons (for mass concentrations). These gravity highs are believed due to increases in rock densities at depths where pressure converts the gabbro feeding the surface basalts into a denser rock called eclogite (see illustration at bottom of next page).

This map covering the entire Moon shows in red areas of mass concentration or mascons; these tend to be found underneath major mare-covered basins:

Bouguer gravity anomalies; those in red associated with mascons.

Now, turrning to experiments conducted on the lunar surface by the astronauts. Each Apollo LM carried a compact package of ground-deployable instruments known by the acronym ALSEP (Apollo Lunar Surface Experiments Package). Two good reviews of the ALSEP program are found at these Internet sites (1) and (2). Several instruments were on most flights but individual Apollo missions usually carried new ones, as evident in the table above. This next illustration, credited to a 1970 article in the National Geographic Society magazine, shows some of these instruments:

ALSEP instruments.

In front of the astronaut is the Lunar Ranging RetroReflector (LRRR) (incredibly, there to reflect a laser beam sent from Earth). Then, clockwise from his left are the Lunar Surface Gravimeter (LSG), the Lunar Atmospheric Composition Experiment (LACE), The Lunar Ejecta & Meteorite Experiment (LEAM) the Passive Seismic Experiment (PSE), the Charged Particle Lunar Environment Experiment; the Lunar Surface Magnetometer (LSM), the Suprathermal Ion Detector (SID), the Cold Cathode Ion Gauge, the Solar Wind Experiment (SWE), the Heat Flow Experiment (HFE), and the Active Seismic Experiment (ASE). Some ALSEP instruments are stand-alone, with their own power source. Others are tethered by cable to a central power source, the Radioisotope Thermoelectric Generator (RTG), shown here at the Central Station point at the Apollo 14 site.

The RTG power source for many of the ALSEP instruments, at the Apollo 14 site.

These many sophisticated instruments (some costing in the $millions to insure their spaceworthiness) have returned vast amounts of data that have enlarged our understanding of the Moon's interior and surface environment. One experiment must suffice to illustrate this versatility. Below are seismic records (seismograms) obtained by the Passive Seismic Experiment. The top two are produced when a spent Saturn IV-B casing was forced to crash on the Moon and when a LM (left behind as the CSM returns to Earth) was allowed to decay in orbit and hit the Moon. The bottom two records are of natural (and small; magnitudes of 2 or less) moonquakes from the interior.

All these records differ from those associated with terrestrial earthquakes in lacking S (secondary or shear) waves. They also last for much longer than earthquakes - up to an hour, as though the Moon were "ringing" like a bell. The bulk of the moonquakes originate from depths of 600 km or more (attributed to the seismic signals bouncing back and forth in the low velocity surface layers [ejecta blanket]). They tend to occur in swarms associated both with preferred spatial locations and specific time intervals (probably accounted for by stresses induced by terrestrial tidal forces).

Seismometers at Apollo 12, 14, 15, and 16 continued to operate for years, providing a wealth of data about the Moon's interior. One model for that interior is shown in this diagram:

Seismic profile of L wave velocities in the Moon's outer interior, with suggested rock types and densities that would account for these values.

Note the two velocity discontinuities at about 20 and 60 km. Velocities within this interval are consistent with anorthosites. The higher velocities deeper than 60 km are associated with a proposed pyroxene-olivine upper mantle. Velocities between 4 and 20 km are indicative of a fractured basaltic flow sequence responding to load pressure. The shallow velocities (lower left inset) are attributed to the lunar ejecta blanket units discussed on the preceding page, overlain by comminuted regolith.

A final word: Heat probe measurements showed a higher heat flow range, averaging 2.8 x 10-6 W/cm2, than was predicted before the landings (Earth's average is ~6.2 x 10-6 W/cm2). This implies a hotter interior than expected, perhaps related to higher uranium (heat-producer through radioactive decay) concentrations.

Source: http://rst.gsfc.nasa.gov