The Apollo Program - Man on the Moon - Remote Sensing Application - Completely Remote Sensing, GPS, and GPS Tutorial
The Apollo Program - Man on the Moon

Either before or after reading through the next three pages, you may wish to consult an excellent online summary of the Apollo Expeditions to the Moon.

The culmination of the great push to the Moon, announced in 1962 by President John F. Kennedy as a major goal for all humankind, were the six manned landings between July 1969 and December 1972. The location of each site (A), along with the locations of the earlier Ranger (R) and Surveyor (S) spacecraft and the Soviet Luna (L) series of rovers, are plotted on this reference map of the Moon's front side:

Location of U.S. and Russian landing sites on the Moon.

The Lunar Orbiters had earlier imaged each site at various times; examples are seen in this next set of panels:

The six Apollo landing sites (Apollo 11 upper left; Apollo 12 upper right; �..Apollo 17 lower right) as imaged by Lunar Orbiters.

The following table summarizes the science rationale for visiting each site:

The Apollo 10 astronauts had previously reached and orbited the Moon without landing during Christmas of 1968. This emboldened NASA to send the first trio of astronauts, Neil Armstrong, Edwin "Buzz" Aldrin, and Michael Collins, in the summer of 1969 to attempt a landing near the south edge of Mare Tranquillitatis, chosen for its flatness and relative sparsity of larger craters. Here are the three "immortals" photographed before their journey that began on July 16, 1969:

Neil Armstrong, Michael Collins, and Buzz Aldrin, in a 'dress rehearsal'.
Their final approach was captured by a photo out the LM window which showed both the landing site ahead and the many guiding landmarks (given quaint names as was the custom) visible ahead:
Approach of Apollo 11 to its landing site.

The touchdown point (LM) at Apollo 11 is plotted on this Lunar Orbiter photomap:

The Apollo 11 site, located in this Lunar Orbiter photomap.

It was mid-afternoon (4:17 PM EDT) on July 20, 1969 that the Apollo 11 LM touched down safely on the lunar surface, much to the relief of the program people at Houston Mission Control and to an anxious but excited world. The descent phase is captured on this video site, narrated by Buzz Aldrin (it may not work on your computer, but try it; of course, you need to be connected to the Internet). There was drama and uncertainty in the final two minutes: a warning alarm sounded repeatedly (it was an overloaded computer) and descent fuel was down to its final minute). Here are six photos that show the scene sequentially just before touchdown:

The final approach.

Six hours later came one of the greatest moments in human history, immortalized in this TV image of the first astronaut to descend to the surface. (If you have forgotten his name and his famed quotation, check the caption; also, face the question: If he were first out, who was holding the TV camera?) Of course, you should remember his "immortal" first worlds: "One small step for (a) man; one giant leap for mankind!" (The 'a' in parenthesis is what he intended to say but this is not heard in the broadcast audio.)

Neil Armstrong, first Man on the Moon.
Astronaut Neil Armstrong descending the ladder of the Apollo 11 LM just before becoming the first human to set foot on another planetary body.)

This next photo captures an indelible image of what most Anericans consider one of the greatest triumphs of the science and technology of the USA, and a tremendous source of national pride - the planting by the astronauts of the American flag (appearing unfolded by making it as a metal sheet which preserves the "flapping" in the breeze) in the lunar soil.

Buzz Aldrin and the American flag.

The two astronauts spent only two hours on the surface (this was the planned duration since there was uncertainty about their safety in the hostile environment of the lunar surface). During this time, they collected rocks and soil and emplaced instruments including the first of three seismometers:

The seismometer, the landing craft, and Buzz Aldrin at the Apollo 11 site.

A view of a small, local crater near the Apollo 11 LM is typical of mare scenery at that site:

A small crater at the Apollo 11 site, taken during the mission there.

The upper part of the Lunar Lander (the LM) blasted off safely, leaving behind the base, which is just visible in this Lunar Reconnaissance Orbiter image:

Arrow points to the LM base which remains on the lunar surface.

One of the most famed of lunar landing photos is shown next. It is often cited when arguments resurface about the wisdom and need to return to the Moon. The photo is self-explanatory:

Astronaut footprint at Apollo 11.

Each astronaut involved in excursions after landing was well-equipped to operate in the low gravity (1/6th that of Earth), airless surficial environment, as depicted in this figure:

The well-dressed astronaut in his space suit with tools and gear.

Apollo 11 and 12 sites were both in mare terrain. Apollo 11 rocks were mostly mare basalts extruding 3.7 b.y. ago. Apollo 12 also sat astride ejecta within a ray coming from the crater Copernicus. Apollo 12 represented a remarkable achievement in navigation, setting down within easy walking distance of the Surveyor III spacecraft remaining from an earlier mission,; pieces of Surveyor were returned to Earth to study the wear on its surface from micrometeorite bombardment. Here it is, with the LM in the background:

Photo taken by an astronaut showing the Surveyor III on the Moon, with the Apollow 12 LM on a rise in the background.

In the opinion of many, the salvaging of the Apollo 13 mission ranks Number 1 on the list defining the capacity of dedicated humans to master modern technology gone astray, requiring extraordinary self-control and innovation to avoid a disaster and save precious lives. The story is told in the movie masterpiece "Apollo 13" with Tom Hanks as Astronaut Jim Lovell - a must-see.

Apollo 14 was in Fra Mauro ejecta emanating from the huge cratering event that produced the Mare Imbrium Basin about 3.9 b.y. ago. Basalts from Oceanus Procellarum were also present. Some of Imbrium Basin ejecta was scattered about Cone Crater, in the top view of this next illustration; a close-up of this ejecta is in the bottom view:

Cone crater and a close-up of an ejecta boulder at the Apollo 14 site.

Apollo 15 landed on basalt flows near the Apennine Mountains, made of rim rocks, which are lunar crust, pushed up when the Imbrium Basin formed. These mountains, shown in the background of the next (top) view that also pictures the LM, rose as high as 4.2km (about 2.8 miles). The highest on the Moon, Mt Hadley (bottom), reaches to 4.5 km (14765 ft).

Apollo 15 near Hadley Rille, with the Apennines in the background; LM in background; David Scott and the Lunar Rover at the right.

If the mountains are indeed uplifted lunar crust, then they expose rocks that were buried at every other Apollo site. Unfortunately, their distance from the Apollo 15 landing area precluded direct examination. But telephoto lens pictures revealed one distinctive characteristic. In the next two images are photos of Mt. Hadley; in the top one faint layering (inclined to the left) is evident and in the contrast-enhanced lower photo this uniformly-spaced set of layers seems to be crosscut by a second set of lesser dipping (lower angle) layers.

Mt. Hadley; note the faint inclined layering
Close-up photo of Mt. Hadley, which seems to suggest two sets of layers.

The precise nature of these layers is still the subject of speculation. But the telephoto below of a terrain extension named Silver Spur in the Hadley Mountains shows a sequence of thick (20-30 m) layers that may be a strong clue. These are dark and resemble the layering in flood basalts such as those in the Columbia plateau. Dr. Paul Lowman (author of Section 12) interprets them as the succession of flow layers involved in filling Mare Imbrium.

Layering in Silver Spur in the Hadley range; some layers may be recessed from the spur face, forming terraces.

A mobile, self-powered vehicle, the Lunar Rover, was first used at the Apollo 15 site to transport the astronauts on long (kilometers) excursions to vist places too far for foot excursions. The Rover, also called the "Lunar Buggy" is equipped as indicated in this schematic:

Schematic drawing of the Lunar Rover and its principal working equipment.

The Rover is shown in this next photo that also shows the Lander and astronaut James Irwin: when

James Irwin and the Lunar Rover.

Apollo 15 also carried the third seismometer emplaced on the Moon. After it was deployed and sent back good data, the simultaneous operation of the three working instruments permitted calculations of the seismic properties of the lunar interior. Several models have been proposed: here is one put forth by M. Toksöz (other investigators argue for a small metallic core); read its caption for more details.

 One of several interpretations for the lunar interior: in this view, the highlands (anorthositic) crust averages 60 km in thickness and has surface extrusions of mare lava (black); a thick mantle overlies an asthenosphere (hot, plastic, partially molten rock in which seismic S waves are slowed); moonquakes occur near the base of the mantle where still rigid rock adjusts to the interior flow.

Apollo 16 was the only lunar manned mission to visit true highlands terrain. The spacecraft landed in the Descartes Mountains; the site is shown in this Apollo photograph:

The Apollo 16 landing site (star *) in the Descartes Mountains.

This Apollo 16 view encompasses the plains, a terrace, and low mountains in the background:

The scene at the Apollo 16 site.

The Apollo 16 astronauts main goal was to sample Highlands units, both in the hills (the Descartes Formation) and the lower units consisting of the Cayley Formation, making up part of what the USGS astrogeologists believed to make up the Cayley Plains. As interpreted by planetary geologists, these supposedly were volcanic deposits, perhaps of pyroclastic nature, but they were shown during and after the mission to be consolidated impact ejecta. A small crater and hills beyond, as shown below, are typical of this highlands landscape:

Another view of the Cayley Plains and nearby hills.

This Apollo 16 sample is typical of the breccias occurring at the site:

An Apollo 16 breccia sample.

The largest breccia sample found at the Descartes site is House Rock:

House Rock.

The Apollo 17 landing site was in the Taurus-Littrow region, where the last visit to the Moon occurred in December, 1972. Here is the approach to this site as photographed from the orbiting Command Module.

The Taurus-Littrow valley and surrounding hills photographed as the Apollo 17 CM neared the landing site.

This vertical photo shows the landing site for Apollo 17 and some key features in the area including the dark, flatter volcanic units which proved to be mare basalts in nature.

Apollo 17 photograph of the landing site in the Taurus-Littrow region, December 1972.

Apollo 17 also sought volcanic pyroclasic units, predicted to occur around the Taurow-Littrow Mountains but, except for the notable orange layers (glass droplets splashed out of mare lavas before they hardened) within the regolith (debris "soil"), the rocks exposed in the massifs (high hills) were again made of ejecta. Some of the rocks at the 17 site were huge, as indicated by this view of "Split Rock" which consisted of a consolidated ejecta (a breccia); astronaut-geologist Harrison H. "Jack" Schmitt is standing nearby:

House Rock at Apollo 17; Astronaut Jack Schmitt is sampling it; note the terrain in the background.

Against the backdrop of the site photo, this map shows the paths followed by astronauts Jack Schmitt and Eugene Cernan as they used the Lunar Rover to traverse to various sampling and instrument emplacement locations.

Lunar Rover paths around the LM at the Apollo 17 site.

Familiarize yourself with the geography of this scene, and note especially the patterns of the massifs (hills in the highlands) that stand out as bright against the darker central lava-covered plains around the touchdown site. Now, look at this ground scene:

Apollo 17 photograph showing the Lunar Module and the Lunar Rover, December 1972.

Astronaut Jack Schmitt (a geologist and the only career scientist to walk on the Moon) took the photo, partly to show the Lunar Module (LM) sitting safely on the plains against a background of a massif (mountain block) composed of breccias (see below). Astronaut Eugene Cernan is at the controls of the mobile Lunar Rover, used for excursions up to several miles from the LM.

One of the prime goals for discovery at the Apollo 17 site was evidence of volcanism other than invasion by mare basalts. The U.S. Geological Survey had forecast that volcanic deposits transported above the surface should be present. There was a moment of high excitement when one of the astronauts suddenly spotted an orange layer in the regolith (surface "soil" debris), as photographed by him here:

The 'notorious' orange soil in place in the regolith at the Apollo 17 site.

When samples of the orange layer were studied after return to Earth, the material was seen to consist of small black glass spherules and chips of orange glass. These are believed to be splash droplets tossed out of cooling lava during impacts into still fluid target lavas (probably with a solid surface crust). This is what they looked like back on Earth:

The particles of black and orange glass, principally of volcanic origin (crater ejecta

You may be interested in this Web site prepared byJack Schmitt in which he has summarized his Apollo 17 experiences, with emphasis on the observations and results made during the mission.

Apollo 17 also shed some proof on a prediction made by the writer (NMS). Just before the Apollo 15 mission, he had attempted to calculate the thickness of the ejecta deposits that he had proposed as the principal surface units in the Highlands. The basis for this calculation was simply to determine the amount of material that would be excavated and tossed out of lunar (impact) basins and craters larger than 1 km on the frontside of the Moon. A terrestrial cratering model was assumed. The result indicated thicknesses on the Highlands to range between < 1 km to just over 3 km. Maximum thicknesses would be near the edge of large basins; the central Highlands would contain, on average, about a kilometer of ejecta (also referred to as the ejecta blanket or megabreccia unit on the surface of which normally develops, both in the Highlands and the Maria, a thin surface layer - the regolith, produced mainly through constant diminution resulting from extralunar debris that impacts as micrometeorites). After Apollo 15's seismograph began operating, indications favored a widespread low velocity layer on the Highlands which seemed to correspond to this ejecta unit. The writer published this generalized isopach (thickness) map shortly thereafter:

Isopach map of calculated thickness variations of the lunar ejecta deposits on the front side of the Moon.

After the failure of Apollo 16 to find extensive volcanic deposits, the group within NASA responsible for site selection planned to meet to finalize selection of the Apollo 17 site. Rumor had it that the USGS would guarantee Taurus-Littrow as rich in volcanics. I consulted the above map and concluded that there would instead be about 3 km of lunar ejecta at and around the site (not counting the local mare basalts). I organized an "insurgency", after I had convinced Dr. Wm. Muehlberger (U. of Texas) who was on the selection committee to champion my argument against the USGS recommendation (my choice was Copernicus, the potential Apollo 18 site). Bill argued vociferously. But it came down to 'Nick Short vs USGS' - guess who won! Guess who was wrong! Read on.

On landing, astronaut Harrison H. (Jack) Schmitt noticed that North Massif was a 1.5 kilometer high mountain made up entirely of breccia (consolidated ejecta). A small portable seismometer then determined that there was a kilometer and a half of low velocity (ejecta) below the site. These two observations totaled 3 kilometers, either a remarkable confirmation of the isopach map at that point or a very lucky coincidence.

(NOTE added on March 25, 2003: The writer (NMS) spoke with Jack Schmitt when the latter visited Bloomsburg University to lecture, and I was able to gather additional details on the stratigraphy. First, he couldn't recall saying I was proved right. He said that the ~1.5 km ejecta deposits above the valley floor were from the Imbrium Basin. Below the floor the seismometer "thump" signal indicated a kilometer and a half of mare basalts. But that was covered by an earlier ejecta interval derived mainly from older Serenitatis Basin impact excavation was beneath that; its thickness exceeded a kilometer. If this is a correct update than the 3 km total is inaccurate [2.5 km being more likely] since the total would thus be 4 km of mixed breccia/flow units above, presumably, lunar highlands rock. But the 2.5 km ejecta prediction still is close.)

The dominance of breccias (most if not all being consolidated lunar ejecta) at Apollos 16 and 17, and the prevalence of this type of rock in the Fra Mauro formation at Apollo 14, supports the idea that the lunar highlands is composed of up to several kilometers of ejecta breccia, probably overlying an anorthositic crust. The unconsolidated regolith at the surface is a superficial deposit. Breccias likely were covering the crustal surface when huge impacts - the basins - removed them for redistribution, followed by invasion of the mare lavas that remain today.

The Apollo program remains the paramount achievement of Man in Space. The greatest reward from the journeys to the Moon lies in the nearly 368 kilograms (810 pounds) of rock samples collected by the astronauts. Almost three decades later, scientists continue the most intense analysis and scrutiny of any natural substances taken from a planetary body. Starting in 1970, every year in March, hundreds of geoscientists meet at the Johnson Space Center near Houston, Texas, for the annual Lunar and Planetary Science Conference, to report on new findings and exchange hypotheses on the interpretation and implications of recent data. From examining the lunar rocks several fundamental ideas have emerged: differentiation of a primitive planetary body, the nature of its early surface, the pre-eminence in non-mare rocks of shock effects from impact cratering, the age and history of the Moon, and its origin. The prevailing opinion is that it derived from accretion of terrestrial debris hurled into space after being ejected from a huge impact on the early Earth that resulted in crustal/mantle materials attaining orbital velocities. A variant of this model, held by some, is that much of the material came from the incoming body, probably an asteroid whose size approached that of Mars).

The appearance of typical lunar rock specimens is shown in the next four photos:

First is a specimen of lunar basalt from the Apollo 12 site; it is fine-grained and pitted by micrometeorite bombardment. This is the prevalent rock type in the maria.

Sample of lunar basalt from the Apollo 12 site, on display at the Lunar Receiving Lab at Johnson Space Center in Houston, TX.

Next is an anorthositic gabbro, a whitish rock dominated by feldspar. It is probably typical of the bulk of the original lunar crust, representing crystals of plagioclase that floated upwards in the cooling magma that developed during the Moon's first general melting. Note the black glass that coats part of the sample, presumably plastered on the rock as it was transported from an impact crater that made the glass.

The 'Genesis Rock', composed mainly of Ca-Na plagioclase feldspar in a rock type called anorthosite, collected at the Apollo 15 site.

Third is an unusual rock found first at the Apollo 12 site (sample 12013). It contains two color phases: light (shown here) and dark:

Apollo sample 12013; the KREEP rock.
Exposed face from a slab of sample 12013; the felsitic phase is the lighter-toned middle patch.

The dark phase is a breccia composed of light-toned fragments in a basaltic matric. The light phase is described as a felsite (fine-crystalline equivalent to a granite) and has a higher silica (SiO2) content than most lunar samples. It contains potassium feldspar and needles of quartz. Because it is high in potassium (chemical symbol K), the rare earth elements (REE), and phosphorus (P), it is representative of the lunar rock class called KREEP. (Note its position in the diagram at the bottom of this page.) Other examples were found at later Apollo sites, particularly Apollo 14. Current thinking holds it to be the top differentiate of a magma that gave rise to a more general anorthositic crust beneath. A variant is that this very old rock may be a sample of the original lunar magma which suggests that crust formed from it was more granitic.

Finally, from the Apollo 17 site, the large central rock is a breccia, that is, a rock composed of fragments of other rocks that accumulate from various (usually distant) sources which are then welded together by heat and pressure.

A lunar breccia from the Apollo 17 site.

These fragments represent impact debris from more than one area of the Moon that makes up the principal deposits of the outer layers of the Moon, i.e., part of the 1-3 km (about 0.62-1.86 miles) thick, lunar-ejecta blanket. The dark material in this specimen is basalt, the solidified end product of iron-rich lava that fills lunar marias. The lighter rock fragments probably originated from the lunar highlands; Surveyor chemistry and Apollo samples show these rocks to have a high percentage of grayish feldspars (Ca-Na aluminosilicates) that cause the highlands to appear lighter in tone (higher albedo or reflectivity). The smaller rock samples surrounding the large specimen are vesicular basalt pieces (dark) and individual highlands rocks (light), collected nearby on the same mission.

At every Apollo site, the surface was covered with fine fragmental material, the lunar soil (technically called regolith) which lay atop the lunar ejecta blanket in deposits from meters to tens of meters thick. This material is the accumulation of debris brought in from near to distant sources after cratering tossed fragments of a wide size range to varying distances beyond the rims. The deposits were then further comminuted by constant micrometeorite bombardment.

An important task for the astronauts was to drive drills into the regolith that allowed core to be removed intact. Here is Astronaut David Scott in process of coring at the Apollo 15 site and below that are recovered core samples from the Apollo 12 site.

David Scott drilling a hole later used for a heat measurement probe.
Typically dark, fine-grained regolith in core retrieved at the Apollo 12 site.

The core samples were analyzed as intensely as the rocks returned from the Moon, but they told a different story. Their components roughly indicated the relative contributions from nearby versus faraway sources. Here is a plot of the relative proportions of different lithologies of coarser fragments in one core from Apollo 11 and several core samples from Apollo 12.

Comparison of lithologies in several Apollo 11 and 12 cores.

Basaltic rocks and breccias were predominant, indicating local sources provided most of the material. Anorthosites were carried to the sites from distant highlands. When mapped in detail, the cores clearly show multiple layers that differ in composition and size distribution, as expected whenever larger impacts tossed out significant ejecta to their surroundings.

Analysis of lunar samples brought to light several distinct features. Some breccias when individual fragments were examined disclosed definitive evidence of shock effects, indicating that these rocks were debris involved in major impacts. Shock effects were found also in lunar soil samples. The writer (NMS) in 1969 was one of the original 142 Principal Investigators selected to study the first lunar samples; my task was to search for shock effects, to be expected because of the prevalence of impacts into the outer surface. However, my earlier experience with shock features in basalt subjected to nuclear explosions led me to predict that these effects would be harder to find than in more silicic rocks such as granites. This proved true. Still, effects attributable to shock were observed rather frequently. This group of six photomicrographs (reread the page on shock metamorphism [p. 18-4]) depicts some examples (check the caption for descriptions):

Photomicrographs of shock effects in lunar rocks: a) planar features in feldspar; b) basalt sample with feldspar isotropized (to glass); c) Partially fused (melted) rock fragment in a shock breccia; d) Quench crystals of pyroxene recrystallized from a highly shocked basalt (?); e) matte of feldspar laths recrystallized in a clear glass spherule (shock splash); f) a spherule now composed of olivene, with texture similar to that observed in chondrites, presumably resulting from melting by shock waves.

I also prepared a second montage showing shock effects in color. Again, the description of each picture is in the caption.

Individual features in moon rock fragments showing shock effects: upper left - a feldspar fragment containing fine (not visible here) planar features and a 'toasted' appearance noted in shocked silicates found in terrestrial crater rocks; upper right - shock-lithified highlands rock (see paragraph below); lower left - kink bands in feldspar; lower right - an orange spherule made up of shock melt, similar to the materials found in the Apollo 17 orange layer (see above)

The upper right photo warrants further discussion. This is a small rock fragment found in a breccia sample that almost certainly was a part of the now-lithified outer ejecta blanket described above on this page. The fragment consists almost entirely of pieces of plagioclase feldspar. The writer first set eyes on this fragment, in a "Eureka!!" moment in late October of 1969, while working on my P.I. tasks. As I peered through the microscope at this this fragment, I was suddenly aware of how much its texture was like that of the shock-lithified sandstones ("instant rock") described on page 18-3. Shown below is a variation: instant rock made up entirely of feldspar fragments welded together by the implosion tube method described on page 18-3.

Instant feldspar rock, produced by shock-lithification of fragments contained in an implosion tube.
Compare this texture to that of the 'Eureka' lunar fragment that appears here:
A piece of a breccia fragment found within an ejecta breccia collected at the Apollo 11 site; this fragment is made up almost entirely of feldspar which NMS postulated in 1969 was shock-lithified lunar highlands regolith expelled a long distance by an impact event there.

I immediately formed a prescient postulate. What I was looking at is a piece of the highlands regolith that had been converted into instant rock by an impact that hurled this fragment a long distance from the highlands site only to land in the forming regolith at the Apollo 11 site. If this were correct, then I was in fact confirming the argument made by A. Turkevitch and his colleagues (see answer to question 19-13) that the highlands was made up of mostly anorthosites (feldspar dominant rock). This conclusion I reported during the first Lunar Science Conference (1970), as did John Wood of the Smithsonian Astrophysical Observatory.

Mineralogically, moon rocks are similar to several types found on Earth, except that the individual minerals are almost entirely unaltered by hydrothermal solutions, i.e., they are very "fresh" looking under the petrographic microscope. Basalts, anorthosites, and breccias (fragmental mixtures of several different rock types) are prevalent. The most common minerals are calcium plagioglase, several pyroxenes, olivine, and ilmenite (an iron-titanium oxide). Three new minerals, unknown on Earth, have been found: tranquillityite, armacolite, and pyroxferroite.

Chemically, the lunar rocks were mostly in a class by themselves, being different from their terrestrial rock type counterparts. They are highly variable in iron (as FeO), with mare basalts being richer in this metal than are terrestrial basalts; they are low in volatiles (including potassium and sodium), and are totally anhydrous (meaning that water was not present when they formed; water found on the Moon is discussed below). Compared with Earth rocks, they were exceedingly fresh, showing almost no signs of alteration. As two examples of their chemical specificity, examine these diagrams which plot 1) Fe vs Mg, and 2) the ratio of potassium (K) to uranium (U) versus changing potassium content; note that both meteorites (chondrites and carbonaceous chondrites) and terrestrial igneous rocks plot in different areas of the diagram than the lunar rocks. However, the meteorite class Eucrites plots partly within the lunar samples field, suggesting that these are actually ejecta from the Moon that reached Earth.

Mg vs Fe for lunar samples.
Plot of K/U vs K in lunar rocks, terrestrial rocks, and ordinary and carbonaceous chondrites.

Geologists would, of course, favor getting additional samples from other locations on the Moon, so as to better define the variability of its exterior composition. Possible future expeditions to the lunar surface (unmanned; manned) may fulfill that desire. Meanwhile, a few meteorites among the thousands being found on the ice during collecting trips to the Antarctic have been confirmed as coming from the Moon. Two examples are shown below:

Calcalong Creek, a regolith breccia type of lunar meteorite.
Another lunar meteorite.

Here is a more recent discovery of a lunar meteorite in the Antarctic:

Another moon rock, carried as a meteorite to Earth and landing on the Antarctic surface.

None of the lunar rocks collected during Apollo show ages as old as some meteorites (4.6 billion years [b.y.]). Radiometric dating (U/Pb; Rb/Sr; K/A decay methods) gave both model ages (times when initial materials appear to have formed) and formation ages (time when these materials melted and solidified to their present state). These two diagrams show Rubidium (Rb)-Strontium (Sr) ages in (A) and Potassium (K)-Argon (A) ages in B:

Rb/Sr and K/A ages for selected Moon rocks.

The youngest basaltic rocks came from the Apollo 12 site (exception: Sample 12013 [Apollo 12 site] is more than 4 b.y. old - it is an exotic emplaced as ejecta from the highlands); the oldest from Apollo 16 and 17 . The maria formation ages spread from around 3.2 to 3.85 b.y (none older). The major ringed basins such as Orientale and Imbrium, most now filled with basalt, seem to have formed about 3.9 b.y. ago whereas Serenitatis may be as old as 4.2 b.y. Thus, these basins took several hundred million years or more to fill.

Many highlands rocks, mostly anorthosites, show ages in the 4.0 to 4.2 b.y. range but the primordial crust formed sometime between 4.4 and 4.6 b.y. ago. No model age (older) was as old as the 4.6 b.y. estimated for the Earth, but the Moon is still considered nearly that old. It could be a 100 million years or so younger if the Earth impact origin remains as the mode of origin for the Moon (see page 19-6b).

A few large lunar craters have been formed during an era beginning less than 1 billion years ago. Copernicus may be about 800 m.y. old and Tycho perhaps less than 300 m.y. in age. This is inferred by extrapolation from crater counts on surfaces elsewhere whose estimated ages have been calibrated by radiometrically dated rocks.

The Moon and the Earth differ distinctly in the ages of rocks found on their rocky surfaces. On Earth very few rocks are older than 3.2 billion years; on the Moon very few are younger than that. This plot summarizes the age distribution:

Radiometrically-determined rock ages on the Earth and the Moon.

As the Apollo program progressed, many planetary geologists argued for making Copernicus a key part in the Apollo mission series. None through Apollo 17 actually went to a very large crater. A visit to one of the "biggies" would add valuable information about rocks and morphological features associated with these large structures. Before Apollo 17, there was debate about where that last mission would go. Impacters supported Copernicus but problems as to where to land safely (the interior near the central peaks was proposed) caused it to be rejected in favor of Taurus-Littrow. Although Apollo 18 had been cancelled before 17 succeeded, the astronauts on that mission took this photo of Copernicus in hopes that the abbreviation of the program could be circumvented.

Copernicus photographed by an Apollo 17 astronaut.

Copernicus - or a comparable large crater - is still there, awaiting a visit in a hoped-for renewed manned lunar exploration program, that is a "must do" (this writer's opinion) in the foreseeable future, now that China and other countries are planning their own lunar programs. Meanwhile, with the success of the unmanned Rovers on Mars (page 19-13a), which proved the technical feasibility of traversing uneven surfaces and doing mineralogical/chemical analyses, sending a fleet of at least several to key locations of special interest on the Moon seems almost mandatory.