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Geotimes
 Published by the American Geological Institute
Newsmagazine of the Earth Sciences

August 2000


Feature
The Making of Lunar Explorers

by Peter Margolin

It was 1961, and John F. Kennedy challenged the nation to reach the moon before the end of the decade. Would America simply go there and return, just to show the world we could beat the Russians? Or would we use the chance to explore Earth’s neighbor and learn something about its composition, history and origin? Twelve U.S. astronauts walked on the moon between July 1969 and December 1972.  Only one was a scientist.
 

On Aug. 1, 1971, astronauts David Scott and James Irwin were exploring the Apennine Mountains on the moon, a few kilometers from their Apollo 15 landing site. They weren’t geologists, but they had received seven years of training from geologists, so they knew what kinds of rocks they would find on the moon. Scott noticed a rock characterized by large, shiny crystal faces and parallel striations — what he thought were signs of plagioclase. He told Mission Control in Houston he thought the rock might be composed entirely of plagioclase, and remembered from his training that this was the definition of anorthosite. He was right.

What Scott found boosted geologists’ hunch that the oldest lunar crust consisted largely of anorthosite. Elated by Scott’s discovery, news reporters back at Houston promptly dubbed his find “Genesis Rock.”


 Above: Apollo 17 astronauts Jack Schmitt (left) and Ron Evans 
 (right) training in the Lunar Rover Vehicle mock-up at Sunset 
 Crater, Ariz., June 1972. All photos courtesy of Don Wilhelms.

Scott was one of 12 astronauts who brought back almost 850 pounds of rock and soil from the moon during the six moon landings. Analyses of these samples revealed the chemistry of the lunar crust and showed that it contained lower concentrations of silicon and volatile elements and higher concentrations of titanium than Earth’s crust. Some of the samples were also enriched in a unique suite: potassium, phosphorous, certain rare-earth elements, uranium and thorium.

Working with these facts, in 1975 astronomer William Hartmann of the University of Arizona suggested a solution to the mystery of the moon’s origin. Characterized by some as the Big Whack, Hartmann’s theory was that the impact of a Mars-sized planetesimal with Earth about 4.5 billion years ago lofted enough debris into Earth orbit to coalesce and form the moon. By 1985, this had become the most widely accepted theory of the moon’s origin. Today, it rests solidly on a foundation built by 11 test pilots and a geologist.

In 1962, charged with carrying out the mission President Kennedy had envisioned, NASA decided it made better sense to teach test pilots the rudiments of geology than to expect geologists to learn to fly rockets. Thus it turned to the nation’s preeminent earth-science organization, the U.S. Geological Survey (USGS), to provide geologic training for astronauts bound for the moon. NASA money had begun flowing into the survey two years before, when $200,000 was allotted for an infant lunar studies program that included investigating tektites and mapping the moon photogeologically.

Geology 101: Flagstaff

The astronauts got their introduction to geology with a flight over Flagstaff, Ariz., in January 1963. Observing Flagstaff’s many examples of Pleistocene and recent volcanism, they peered down into the pristine bowl of cinder cones such as Sunset Crater, which had erupted only 900 years before. Geology seemed to agree with them, especially from the air.

In 1948, when Eugene Shoemaker decided he wanted to be the first geologist to land on the moon, he took his first steps in the Flagstaff area. (Shoemaker, who died in a car crash in 1997, didn’t make it to the moon in his lifetime. His ashes were made to crash land on the moon last year aboard the Lunar Orbiter.) Working as a USGS geologist in the 1950s, he showed how Meteor Crater had formed by the impact of a meteorite, and he estimated the size, mass and terminal velocity of the impacting object. The crater thus became the first scientifically documented structure of its kind. At Hopi Buttes, a Miocene-Pliocene volcanic field of more than 300 eruptive centers, he studied maars and diatremes as possible examples of explosive lunar volcanism.
 

  Apollo 11 astronaut Buzz Aldrin at a view point along the 
  Bright Angel Trail, Grand Canyon, in 1964.
Classroom training of the Apollo astronauts started in 1964 at the Manned Spacecraft Center in Houston. Thirty astronauts had been selected for the Apollo program, including Alan Shepard, America’s first man in space; John Glenn, first to orbit Earth; and Gemini veteran Neil Armstrong. USGS geologists Dale Jackson, Al Chidester, Don Wilhelms, Dan Milton and Gordon Swann introduced 29 test pilot astronauts to basic geologic concepts and the mechanics of impact cratering. NASA geologists gave lectures on how to recognize different types of rocks and minerals.

But Jackson realized there was only so much textbook geology that a test pilot could stomach, so in March 1964 he organized the first of an extensive series of field trips to use Earth as a laboratory for the moon. He took the astronauts to the Grand Canyon, where outcrops illustrate basic stratigraphic principles in ways more memorable than any textbook.

From 1964 to 1969, geologists took the astronauts to places where the rocks and structures displayed effects of either volcanism or impact mechanics. Guiding the astronauts were Howard Wilshire and Dave Roddy, who both studied the geology of ancient impact structures (astroblemes); Don Wilhelms, who devoted his career to photogeologic study of the moon; and others who studied the diatremes and maars thought to resemble lunar eruptive vents.

By the summer of 1969, weeks before the Apollo 11 landing, the training intensified. USGS geologists began giving astronaut crews highly detailed briefings on the terrain and geology they should expect at their assigned landing sites. Command module pilots also received instruction, organized by the survey’s Harold Mosursky and by Bellcomm geologist Farouk El-Baz, an expert on remote sensing and now director of the Center for Remote Sensing at Boston University. For the several days these pilots would orbit the moon, waiting for their moon-walking partners to return, they could take photographs and scout lunar terrain for tell-tale geologic clues. Such scouting by Apollo 15 command module pilot Alfred Worden in July 1971 provided information for selecting the last of the landing sites, the one targeted for Apollo 17 Commander Eugene Cernan and geologist-astronaut Jack Schmitt. While in orbit, Worden photographed dark-rimmed craters that geologists had told him were prime candidates in the hunt for evidence of explosive volcanism.

Dress rehearsals for the moon

As part of the intensified training, moon-like areas on Earth were the stage for dress rehearsals. The setting that most nearly duplicated lunar terrain was a replica prepared in a field of black volcanic cinders called Cinder Lake, a few miles northeast of Flagstaff, Ariz., within the ashfall from Sunset Crater’s last eruption.

At Cinder Lake, astronauts walked across craters of the same size, shape and position as those in a particular section of lunar terrain photographed a few years earlier by a robot space probe, Lunar Orbiter. By the summer of 1970, they were touring these crater replicas in a mockup of the 450-pound electric go-cart, the Lunar Roving Vehicle, that would be used on the three final moon landings. They maintained radio contact with a mock-up mission control in Flagstaff, where geologists monitored the astronauts’ progress, answered their questions and asked for clarifications as the astronauts described what they saw.
 
Geologists devised an ingenious design for the Cinder Lake training ground. First, explosive charges were buried in a pattern corresponding, on a one-to-one scale, to that visible in high-resolution photos of a section of the moon’s dark, flat plains, the maria. The size of each charge was adjusted so that the explosion would produce a crater roughly the same size as its lunar counterpart. But geologists also wanted to duplicate two basic aspects of lunar impact craters. For thorough realism, ejecta from newer craters had to overlap ejecta from older ones, and the site needed a continuum of crater “freshness,” with the youngest having the sharpest, most distinct features. Rather than set off all the charges at once, the oldest, most eroded craters (eroded on the moon by micrometeorite bombardment and other cratering processes) were blasted out first, with succeeding series of explosions producing younger, fresher craters.
   Apollo 8 and Apollo 13 astronaut Jim Lovell at a lava squeeze-
   up near Sunset Crater, Arizona, in May 1964.

These dress rehearsals continued after the first moon landing, as did field trips to major astroblemes. The astronauts familiarized themselves with impact breccias at the Sierra Madera uplift near Fort Davis, Texas. At this astrobleme, they could also see the cone-in-cone structures (shatter cones) characteristic of sedimentary rocks subjected to hypervelocity impact. An August 1970 trip to the Ries Crater (Rieskessel) in Bavaria gave astronauts Alan Shepard and Edgar Mitchell a chance to see what impact breccias might look like on Earth — a year before they would find the lunar equivalents while exploring the south flank of Cone Crater at the Apollo 14 landing site.

As early as 1946, Robert Dietz had called attention to the nickel-bearing Sudbury structure in Ontario as a feature that could have been formed by meteorite impact in Proterozoic time. In July 1971, astronauts John Young and Charles Duke got their first look at Sudbury’s ancient impact breccias in situ. Eight months later, they would sample lunar rocks of this origin in the vicinity of their Apollo 16 landing site, thus demolishing geolgists’ idea that the bright lunar highlands were scenes of significant volcanic activity.
 

    Apollo 11 astronaut Neil Armstrong, on mule, follows USGS
    geologist Don Wilhelms along the Bright Angel Trail, Grand
    Canyon, May 1964.
The astronauts also studied man-made craters, including the huge craters produced by underground nuclear explosions at the Nevada Test Site. These craters displayed features resembling those at Meteor Crater, such as overturned beds on crater rims. The missile-impact craters that geologist Henry Moore and Peter Margolin studied in 1967 and 1968 at New Mexico’s White Sands Missile Range helped the astronauts recognize particular impact features and to collect samples of ejecta.

Field trips also showed the astronauts plutonic rocks in a natural context. Anorthosite inspired a visit to Minnesota’s Duluth Complex in 1970 and a tour of California’s San Gabriel Mountains. The first hint that this terrestrially uncommon rock type might be widespread on the moon was found in lunar soil Neil Armstrong and Edwin “Buzz” Aldrin returned in 1969.

Recipes for success

Jack Scmitt was the sole geologist in the Apollo missions and rode with Gene Cernan in the Apollo 17 mission. But the Apollo program’s first and only geologist to go to the moon experienced his measure of disappointment. In December 1972, on his second excursion from the Apollo 17 landing site, he found what looked like orange volcanic ash on the rim of a crater named Shorty in the valley Taurus-Luttrow. He thought he had discovered a true volcanic vent in the crater. But, noticing the crater’s blocky ejecta, he soon began doubting this conclusion. The ash, although genuinely volcanic, turned out to be billions of years old, far older than the crater at which it was found.

How had the nonscientists who flew Apollo 15 and Apollo 16 reaped such major scientific rewards?  For one thing, they had a longer training period than did the astronauts of earlier landings. For another, the Apollo 15 landing vehicle had been upgraded to support a three-day stay. The couple of hours Armstrong and Aldrin spent outside of their Apollo 11 landing vehicle were barely enough for grabbing 50 pounds of material before heading home. On later missions, the astronauts had more time to judge which materials were of geologic interest and worth bringing home. And improved tracking methods let Earth-bound geologists follow the explorers from moment to moment, with no uncertainty about precisely where the samples were being collected.

The Apollo 15 pair, Scott and Irwin, were lucky in their landing site assignment. Situated on a mare plain at the foot of the Apennine Mountains, this site was the only one near the edge of a sinuous rille, Rima Hadley, longest of the moon’s winding canyons apparently produced by swiftly moving, highly fluid lava. Visible in the canyon walls were layers of basaltic bedrock, the only such layers any of the astronauts would see on the moon. As a result, samples of basalt that Scott and Irwin collected near the edge of the rille were closer to being in situ than any others brought back to Earth (the anorthosite that Scott collected was interpreted as talus, carried by downslope movement from the bedrock core of the mountain).

The scientific achievements of the Apollo 15 and Apollo 16 missions grew from seven years of geologic training and a rare combination of skill, determination and luck.



Margolin worked at the U.S. Geological Center for Astrogeology in Flagstaff, Ariz., from 1966 to 1969. Semi-retired now, he pursues his mineralogical interests working summers as a Park Ranger at the Blue Ridge Parkway’s Museum of North Carolina Minerals, while researching prehistoric mica mining and soapstone quarries near his home in the mountains.



 
Searching for impact craters

When Eugene Shoemaker decided to use the geology around Flagstaff, Ariz., as a stage for lunar geology, he was following the lead set 60 years before by USGS geologist Grove Karl Gilbert. Gilbert became interested in the moon and its craters near the end of the 19th century, two decades after his classic study of Utah’s Henry Mountains. In 1891, he ran magnetometer surveys across Meteor Crater, then called Coon Butte, hoping to locate a buried meteorite and prove the unearthly origin of the crater. Finding no such mass, he reluctantly concluded the crater was produced by exploding volcanic steam. The USGS found no reason to question this conclusion until Eugene Shoemaker explained the absence of a buried meteorite in his authoritative study of the origin of Meteor Crater. (The meteorite had exploded and disintegrated upon impact.)

Believing he had failed to locate a meteorite crater on Earth, Gilbert trained his sights directly on the moon, spending weeks looking at it through the telescope of the Naval Observatory in Washington.

For this he took flak from a congressman, who reportedly said that the uselessness of the USGS was evident in that “one of its most distinguished members has no better way to employ his time than to sit up all night gaping at the Moon.” Gilbert’s “gaping” produced the first modern geologic observations of the moon, a paper entitled  “The Moon’s Face,” in which he deduced an impact origin for most lunar surface features, large and small, while considering volcanic activity responsible for some of the smaller, Earth-scale craters. The latter he thought might turn out to resemble terrestrial landforms such as maars and calderas, produced by explosive volcanism and collapse.

Peter Margolin 
 



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