Geological Field Investigation in Early Apollo Manned Lunar

60 Pages·2007·4.54 MB·English

APOLLO MANNED LUNAR LANDING

SCIENTIFIC EXPERIMENT PROPOSAL

GEOLOGICAL FIELD INVESTIGATION IN EARLY

APOLLO MANNED LUNAR LANDING MISSIONS

Abstract

and

Techi~icalS ection

E. M.Shoemaker, U.S. Geological Survey

Principal Illvestigator

E. N. Goddard, Uiliversity of Michigan

Co-investigator

J. H. Mackin, University of Texas

Co- investigator

H.M. Schrnitt, National Aeroilautics

and Space Adrninis tration

Co-investigator

A. C.Waters, Uiliversity of California

at Sai~taBarbara

Co- investigator

November 1965
APOLLO MANNED 1,UNAR I,ANDING

SCIENTIFIC EXPERIMENT PROPOSAL

GEOLOGICAL FIETADI NiTESTXGATTON IN EARLY

APOELO MANNED LUNAR LANDING MISSIONS

Sponsor

U. S. Geological Survey

GSA Building

Washington, D. C. 20242

Harold L. James

Chief Geologist

U. S. Geological Survey

GSA Building

Washington, D. C. 20242

202-343-2125

Investigators

Eugene M. Shoemaker Center of Astrogeology 602-774-5261
Principal Iilvestigator U. S. Geological Survey
601 East Cedar Avenue
Flagstaff, Arizona 86001
Edwirl N. Coddard Department of Geology 313-764- 1444
Co-investigator University of Michigan
Ann Arbor, Michigall
J. I-Ioover Mackiil Department of Geology 512-471 -3055
Co-investigator University of Texas
Austin, Texas
1Iarrisoi? 1-1. Schmitt P. 0. BOX 276 602-969-8933
Co-investigator Williams Air Force Base
Arizona
Aaron C. Watcrs Department of Geology 805 -968- 1511
Co-investigator University of California
at Salzta narbara
Santa Barbara, California

Page
Abstract 1
1. Purpose and objectives of geologic iilvestigatioils
in early Apollo luilar landing missions 3
A. Scie~ltifico bjectives 3
B. Fine structure of the plains surfaces 4
C. Chemical and physical surface alteration 8
2. State of present developmeilt of Apollo
geologic field i~lvestigatioil 12
3. Characteristics of the geologic field instrumellts 15
Stereometric film camera
Staff
G11om
011
Televisioil camera
Sampling trowel
Sampling tubes
Sampliilg hammer
Sample scriber/brush
Field sample bags
Special sample containers
Tool and sample carrier
Hand magnifying glass
Hand- held flashlight
N. Audio communicatioils equipment 19

ABSTRACT
The principal geological objectives of -E-arly Apollo missions
will be study of the fine structure of the lunar surface, mainly
in the plains areas favorable for early lauding, and study of the
ilature of the plains materials. Plains areas of interest include
not only the maria, but also the plains of certain upland regions.
These plains are depositional surfaces, modified by post-
depositional processes of several The primary questions
to be answered are 1)the lithologic composition, structure, at~d
thicklless of the superficial layer of fragmental material believed
to cover most parts of the plains and other areas on the moon
and 2) the composition and origin of the material underlying the
plains.
Allswers to these questions will be obtained from the geo-
logical observations of the astro~lauts,f ronl photographs, and
from sarnp1.e~ta ken along a series of foot traverses from the
lunar excursion module. The geological instruments to be used
by the astronauts are light, simple hand tools and cameras. The
topographic and geologic relations observed along the traverses
of the astronauts will be determined primarily from numerous
stereoscopic photographs supplemented by the astronautsq
descriptions alld by data obtai~ledf rom returned samples. The
photographs provide a detailed record of the surface features,
which can later be analyzed quantitatively, and will provide the
geologic context at the site of each sample locality. The orien-
tation of the cameras during exposure of each photograph will
be automatically recorded for use in later photogrammetric and
photometric data reduction.
TECHNICAL SECnON
A. Scientific objectives
The early Apollo lullar landing sites will probably be on
maria floors or other lunar plains, remote from rugged topo-
graphy. These plains are depositional surfaces, modified by
post-depositio~lalp rocesses of several kinds. The primary
geological questions to be answered by early Apollo lu~lar
lailding missions are I) the nature and origill of the material
underlying these plains, and 2) the nature and rates of the
processes that have taken place on the lunar surfa.ce. Were the
plains materials formed as flows of liquid lava that now range
from solid rock to rock froth, or were they deposited as ash or
granular material, and now range from unconsolidated to solid
depending on the degree of heat or vacuum welding? The rates
of processes modifyillg the surfaces of the plains are exceed-
ingly slow; these processes call best be approached by study of
their long-term effects materials and topographic forms of
011
the plains.
The most immediate question will be the composition, fine
structure, and thickness of a superficial layer of fragmental
material believed by many studellts of the moo11 to have been
formed by the impact of objects of various sizes over a very
loilg period of time. Closely related to the origin of this
material, is the distribution and range in size and shape of
craters which pockmark the surface, as seen in the Railger VII,
VIII and IX photographs.
B. Fine structure of the plains surfaces
Models of the local fine structure of the plains can be
derived from physical studies of the moon's surface, by means
of telescopic photometry, radiometry and reflected microwave
signals, and observations of the lunar crater distribution in
combination with empirical knowledge of the phenomenology of
cratering, cratering theory, curreilt data 011 the flux of meteor-
oids in the vicinity of the earth, and estimates of the effects of
other processes acting on the lunar surface, such as sputtering
produced by solar wind bombardment. Prom such stuclies we already
know that the lunar crust is demoilstrably heterogeneous in com-
position. The fine structure of the surface also may be expected
to be heterogeneous.
On the basis of the available data, it appears highly probable
that most parts of the moon's surface are covered with a layer of
finely broke11 rock fragmeilts, the upper surface of which is
pitted with craters. The thicklless of the layer, the size distri-
bution of the rock fragments, and the size and spacing of super-
imposed craters probably all vary abruptly from place to place.
Employiilg the data available from the photographs acquired from
the Iiailger missions, in addition to the illformation obtained at
the telescope, a reasonable model of the fine structure of a
typical local area on a plains surfacec an be described in the
following way:
1. A layer of shattered and pulverized rock probably
covers more than 95 percent of the plains. It is of variable
thickness and rests with irregular contact on the uilderlying
substailce of the plains.
2. The fragments in this layer or blanket of shattered
rock have been derived by ejectioil from craters, most of
thcrn nearby, but some lying great distances away. About
50 percent or more of the fragments have come from within
one kilometer of the site, but there is a fiilite probability,
decreasiilg with the distance to the source, of findiilg a rock
fragmeilt derived from any place on the moon. Except alollg
the margins of a plain, therefore, the pieces of debris will
be composed predomi~lantlyo f plaiils material. Those frag-
ments that have come from beymd the plains will probably
represellt highly diverse geologic environments. In addition,
a small admixture of meteoritic material will probably be
represellted among the rock debris.
3. Fragme~ltso ccurring at the base of the debris layer
will, on the average, have been transported on ballistic
trajectories a smaller ilumber of times than pieces near the
middle or top of the layer. Progressing upward from the
base, the layer has been stirred or recoilstituted an