PRECED!NG
RESOURCES
ROCKS,
OF THE
Lawrence
FOR A LUNAR
MINERALS,
MOON
AND
P,.'IGE E,LANK
NOT
FI!..MEb
361
BASE:
SOIL
N93-
1
973
A. Taylor
Department
of Geological Sciences
The University of Tennessee
Knoxville TN37996-1410
The rrmks and minerals of the Moon uqll he included among the raw materials used to constr_'t
a
lunar base. The lunar regolith, the fragmental
maten_ present on the surface of the Moon, is composed
mostly of disaggregated
rocks and minerals, but also includes glassy fragments
fused together by
meteorite impacts, lhe finer fraction of the regolith (i.e., <1 cm) is inf, mmally referred to as soil. The
soil is Im)bably the most important lx_rtion of the regolith for use at a lunar base. For example, soil
can be used as insulation against cosmic rays, for lunar ceramics and ab_Mes, (w fiw grouSng plants.
The soil contains abundant solar-ugna_i_nted
elements as well as various minerals, particzdarly o.xfule
phases, that are of potential economic importance. For example, these components
of the soil are sources
of oxygen and hydrogen for rocket fuel, helium for nuclear energy, and metals such as Fe, A1, St_ and
1t.
INTRODUCTION
CONDITIONS
OF ROCK
MINERAL
Based
upon
Apollo,
the
three
of returned
nature
Moon's
nine
from
lunar
Luna),
lunar
sample
we have
samples
and
return
over
missions
(six
380 kg (almost
an excellent
from
840 Ib)
knowledge
of the
of the rocks and regolith
over a limited
portion
of the
frontside.
These are the raw materials
that a lunar base
can utilize.
They
may also be the source
which
help
justify
to
hydrogen,
oxygen,
There
have been
petrology
an
of certain
many
excellent
returned
Taylor
lunar
(1975,
1982)
Steele,
shall
not
1976;
Papike
attempt
previously.
to
Instead,
petrology
and
attention
repeat
I will
what
present
mineralogy
to those
Bence,
of the
aspects
that
lunar
of the mineralogy
and
cometary
infall. Consequently,
which
the ix)oks
In addition,
Wiihelms,
there
been
so
well
synopsis
samples,
written
of the
with
respect
basic
recent
publication
Lunar
Bases
essential.
and
by the Lunar
Space
In addition,
coordinated
lished by
future
a book
through
Cambridge
entitled
the Lunar
University
knowledge
of the Moon,
base endeavors.
which
Institute
of the 21st
Lunar
has been
studies
actually
that
compiled
designed
experiment
should
engineering
and is presented
and add
In addition,
the
the
),
(1985),
is
(1991),
for future
in this paper.
to utilize
lunar
materials,
with
lunar
samples.
be followed
in order
or industrial
investigations.
lunar
a listing of
by mission,
With
certain
it may be necessary
A brief outline
to apply
for lunar
because
of the complete
so dominant
on Earth,
to
is given
,samples
for
(hydrogen),
nents into
components,
a significant
myriad
minute
of lunar
aspects:
mineral
( ! ) temperatures
components
corresponding
Moon.
only
Also,
mineral
are
soil.
protons
the presence
fragments
metamorphism,
one of the disof "agglutinates"
and #ass)
with
their
(i.e., Fe °) grains.
of lunar
rocks,
most notably
the
from those on Earth in two basic
of formation
during
of the
ones
to the
notably
shock
produce
formation.
and ( 2 ) the oxygen
Largely
of water and its great "fluxing"
abilit)' and
mineralizers
(e.g., E Cl), the cryst',dlization
than
40,000the
the minerals,
signature
particles,
soil, namely
and
iron metal
prevailing
the
in
introduce
exogenous
compoand meteorite
and micromete-
associated
ultimately
The formation
conditions
volcanic
ones, are different
pressures
principally
solar-wind-implanted
of rock
on
chemical
helium,
and carbon,
the soiL These particles
as'pects
(aggregates
(e.g.,
result
erosion
and
have bombarded
speeds
impacts
and
undergoes
to -130°C),
sizes)
and
and
lack of any water, chemical
weathering,
is nonexistent
on the lunar
surface.
orite
impacts,
with
their
including
complete
melting,
tinctive
hence,
of solar energy
and meteoritic
of the Moon
at fantastic
meteorite
of weathering
the meteorite
and Planetary
Institute
and pubPress, summarizes
our current
In addition
to the nature
of lunar components,
catalogs and documents
on lunar samples,
organized
process
for aeons
discemable
Sourt-eb_)k
will be important
effective
mas,s and,
(+135°C
to submicron
The_
Therefore,
( Houston
Century
km/hr).
for lunar
use of lunar materials,
and Planetary
Activities
kilometers
continually
250,000
the surface
in temperature
particular
may be of significance
to the possible
(from
the surface
I
torr)
changes
meteorites
1984).
-7
tremendous
exploitation.
With
of its smaller
cannot
maintain
a significant
atmothe result that it has no "insulating
that would
(1)aid
the retention
it from cosmic
rays, solar wind,
1979;
has
Because
Moon
with
blanket"
(2)shield
among
a brief
the
,¢40here
are paramount.
and
(<10
and soils.
3He,
are several fine review articles from which I have drawn liberally
(e.g., Smith, 1974; Frondel, 1975; Palyike et al., 1976, 1982; Smith
and
velocity,
with
endeavor,
reviews
samples,
minerals,
escape
in the environments
conditions
of their
e.g.,
ambitious
products
The Earth and its moon differ significantly
at their surfaces
and also in the formation
rocLs,
Fe metal.
of the
by Ross
such
AND
FORMATION
rocks are
on
Earth.
about
The
because
parti;d
of the lack
the paucity of other
temperatures
(ff the
100°-150°C
conditions
higher
of ox3'gen
362
2nd
partial
Conference
pressure
distinctly
in
any
conditions
the
in
elements
unusual
in
have
minerals
states
of
are
all
effect
the
kinds.
to Earth
on
I
the
Fe 3+
formation
curve,
native
Likewise,
some
a reduced
state
situations
I
are
is no
buffer
in
fO2)
there
because
present
compared
as
fugacity,
iron/wiistite
samples
Activities
a pronounced
Indeed,
the
Space
abbreviated
oxygen
minerals.
lunar
and
fugacity;
low
below
the
valance
the
the
at and
is ubiquitous
Bases
1 ) and
of
of
are
Lunar
oxygen
(Fig.
Because
present
Fe
(called
different
mineralogy.
on
(e.g.,
of
with
Ti 3+ vs.
Ti4+; Cr2+ vs. Cr3+; Fe 0 vs. Fe2+; p3+ vs. P_+.
t2
3
ROCKS
Most
U.S.
missions
Apollo
landed
flows.
Some
rocks.
the
Taylor
this
and
(1975,
most
areas
consisting
rock,
1982),
portion
on
importance
for
be
rocks
An
base
written
Bence
Steele
(1984).
brief.
of highland
and
and
16
basalt
been
Papike
Smith
is that
lunar
young
have
them
Wilhelms
will
(unmanned)
largely
papers
(1978),
and
here
Luna
comparatively
among
Vaniman
presented
shortened
of
of
review
lunar
Papike
Russian
areas
to
excellent
concerning
discussion
were
O
and
maria,
missions
Several
(1979),
(manned)
within
O)
Therefore,
additional
it is the
the
reason
minerals
endeavors,
not
20
(1976),
that
the
1/T(°K) x 104
85
I
for
are
rocks
per
I
'
800°C
900°C
10
'o
O°C
se.
Representative
,sampled
mission
the
portions
by
Apollo
brought
between
of
of
and
20%
two
of
breccias,
created
a
rocks
and
metamorphosed
Indeed,
few
igneous
rocks.
remelted
of the
highlands,
nym
there
for
basalts
land
great
elements
that
polymict
The
basalts,
and
some
less
potassium
(VHK)
for
vs. Mg'
oxide
makes
to
refers
bulk
or
up
that
are
lava
of
the
In
(an
acro-
in
some
most
50%
and
1%.
actually
of the
shows
number"
low
from
most
by volume
and
and
ubiquitous
(Note:
"modal
present
in the
theoretical
and
equal
Fe
percent"
rock;
mineralogy,
commonly
best
to
within
depicting
(lower
area)
the fayalite/quartz
this lunar
area.
range
basalts.
complete
from
"normative
starting
the
percent"
with
the
in weight
shocked
plutonic,
of
"pristine"
these
rocks
identifying
(Ir
and
and
melt
elements.
of
the
Au).
rocks
melt
is
impactor
by
meteorites
by
in
the
classifica-
to
impact.
all
always
the
The
which
Breccias
the
way
similar
to
and
the
soil
easy
to
identify
least
ambiguous
analysis
of
siderophile
high
siderophile
have
meteorites
of
these
to
resemble
either
of
are
and
matrix.
degree
texturally
impacting
form
complex
mineral,
debris,
compositions
The
17. After
Breccias
rock,
rocks
It is not
(e.g.,
and
of
the
of
rocks.
formed
15
meteorite
compositions
Most
particularly
working
of
the
rocks
are
component
upon
products.
"pristine"
contents,
signature
as melt
but
by a fine-grained
have
to
and
Composi-
accepted.
fragments
during
generally
and
olivine.
the
generally
These
rocks
clinopyroxene,
schemes
rocks,
aggregates
rocks.
but
many
depends
indurated
intermediate
and
highland
together
been
elements
a
of
matrix
has
rocks,
for
consist
welded
poorly
or
some
been
in the
and
as at Apollo
lunar
has
impact-melt
soil
lunar,
to
rock
from
the
in
and
fragments
igneous
a few
is present
(1980)
highland
of plagioclase
sites,
large
with
brecciated
cratered
plagioclase
in Fig. 3.
sample
as well
associated
for
of glass
a given
volatile
opaque
20),
rocks
amount
atomic
Luna
amounts
shown
a
of
clinopyroxene,
plagioclase
all
16, and
of Stfffler
meteorite
at
with
turmoil
of
heavily
other
plagioclase
are
sites
14,
in
up
those
Apollo
in
to plagioclase,
orthopyroxene,
rocks
present
ancient,
mainly
of unequal
is made
are
in the
contains
highland
at
complex
regardless
The
refers
expressed
plot
lunar
around
composed
of
gabbro
of these
abundant
are
is composed
troctolite
tions
tion
(VLT)
the
basalts,
vary
native
centers
abundant
in addition
orthopyroxene,
while
are
amounts
norite
nomenclature
seen
olivine.
olivine;
much
terrestrial
of the
O-20%
varying
three
very-high-
of
However,
contain
based
variations
be
contents
chromite.nlvOspinel,
The
rock,
the
can
feldspar.
are
as
rocks
Breccias
high-
very-low-Ti
such
and
the lunar activity
is located
entirely
field where
metallic
Fe is stable. No
Fe 3.) is stable
Anorthosites
types
There
These
possess
about
20%.
)
2
types.
distinction
a "calculated,"
percent.
Figure
a
various
varieties
Fe (i.e.,
Anorthositic
troctolites.
KREEP
and
region
buffer curve,
whereas
Fe/wiistite
curve, in the
highlands.
flows
of
is present
into
The terrestrial
area)
soil
simple
rocks
patterns
Iow-Ti,
abundant
plagioclase,
than
composition
volume
P)
"magnesium
ilmenite
percent
to
K,
over
less
volume
and
breccias,
and
shaded
and
aggregates.
plutonic
chemistry.
high-Ti,
rocks
20-30%
phases,
amounts
rocks
Earth
called
classified
main
[called
and
with
percent
three
These
Na
type,
the
activity.
vs. temperature
(fO2)
(upper
whereby
iron-rich
norites,
bulk
basalt.
the
Mg/(Mg+Fe)].
Pyroxene
and
and
been
and
types,
of
basalts,
component
REE,
have
mineralogy
basalt
elements
mare
trace-element
mare
TiO2
melt,
metamorphosed
anorthosites,
general
the
to
of oxygen
terrestrial
through
cemented
returned
basins,
K,
basalts
their
chemistry
of
dominates
other
magmatic
highly oxidized
Moon
pressure
for
the
a silicate
with
Partial
regions
+ magnetite
below
the
breccias.
mare
upon
mixed
up
1.
the
constitute
impacts
coherent,
in
make
on
Fig.
soil.
is a chemical
the
and
of
maria
only
formed
from
been
every
originating
rocks
meteorite
of complex
impact
darker
basalts
rocks,
samples
consist
composed
addition,
and
fine-grained
rocks
the
of
have
However,
as
The
minerals
into
consist
or
igneous
filled
broken
Most
Moon.
result
highland
regolith,
The
that
are
the
mare
igneous
of
as
that
the
crystallization
preexisting
shock
of
20.
identified
surface,
types:
highlands
Luna
samples
the
basic
processes
and
it appears
portion
15%
consist
ancient
16,
some
Although
a substantial
the
Apollo
back
highlands.
of
14,
means
retain
siderophile
Taylor:
I
Materials
I
for
T
a lunar
363
base
I
12
_-I-
10
_o 8
i
144
p
3:6
0
4
o_
J
2-
0.7
0.6
0.5
0.4
0.3
I
I
0.4
0.3
0.2
Mg/(Mg+Fe)
I
14
m
I
..... /_.....
I
1
.6
12
.5
I--,
-!0
t,--
10
0
m
3
8-
o
6-
e(
4-
.4
m
3:
.:3
Q
cL.2
20.7
I
I
i
I
0.6
0.5
0.4
0.3
0.2
0.7
0.6
0.5
Mg/(Mg+Fe)
0.2
Mg/(Mg+Fo)
Fig. 2.
Oxide
variations
vs. Mg" for mare basalLs (adapted
low-Ti basalt.s; diagonal
line shadings
are for very Iow-Ti (VLT)
from BV3/P, 1981 ). Horizontal
ba.salts.
line
shadings
SiO2
are for
high-Ti
SILICATE
Most
and
of the
are
igneous
is
rocks
the
of
when
the
lunar
are
highland
igneous
amounts
of
viewed
consist
and
silicate
minerals
of
in
in
rocks
are
which
thin
fi_r
it
are
"opaque"
to
that
Fig. 4.
As
mentioned
mostly
of
plagioclase,
chemistry
is presented
below.
mafic,
plagioclase,
are
of the
The
silicates
in
and
section,
abundances
olivine.
are
found
pyroxene,
The
depicted
lunar
commonly
olivine,
rocks.
rocks
the
those
most
pyroxene
rock-forming
as
phases,
light
basalts
comprise
i.e.,
shadings
MINERALS
same
Earth,
nonsilicate
distinctive
that
the
on
transmitted
mare
minerals
essentially
basalL, i; dot
most
minerals
in
above,
of
the
with
le&ser
these
three
Pyroxene
Pyroxene
displays
is
compositions
Ca,
Fe,
Mg)
of
are
Quadrilateral"
OL
AN
(Mg Fe)2 SiO4
Fig.
3.
Compositional
Ca At 2 Si 2 0 8
fields
the olivine (OL)-anorthosite
(adapted
from Tay/or, 1982).
of lunar
(AN)-silica
highland
(SiO2)
igneous
rocks
pseudoternary
plotted
on
diagram
the
considerable
name
.solid
solution
in
represented
the
(CaFeSizO¢,),
as shown
enstatite-ferrosilite
symmetry
compositions
are
termed
and
are
represent
terms
comers
of
group
range
the
by
are
ferrosilite
or
the
a
(i.e.,
pyroxenes
(Mg2Si2Oc,),
on
for
commonly
where
hedenbergite
general
termed
"clinopyroxenes."
major
use
of
diopside
with
have
with
Pyroxenes
that
). The
elements
the
(i.e.,
"Pyroxene
(CaMgSizO6)
and
compositions
whereas
monoclinic
with
near
crystal
all
symmetry
4-7%
,
enstatitc
orthorhombic
"orthop)a'oxenes,"
pyroxenes
minerals
(Fe2Si20(_),
in Fig. 5. Pyroxenes
join
of
in chemistr3,
Ca()
other
and
are
364
2nd
Conference
on
Lunar
Bases
and
Space
Activities
lOO
A
Ca Mg
Ca Fe
Si02
AI203
CaO
FeO
Mg Mg
MgO
Fe Fe
Ca Mg
B
8O
Ca Fe
Feldspar
2O
Mg Mg
Fig.
4.
ordered
(adapted
Mare
from
from
basalt
left
major-element
to right
BVSP,
chemistry
by decreasing
TiO2
and
(or
modal
opaque
Fig.
mineralogy,
oxide)
5.
Lunar
"pyroxene
content
(CaMgSizO6),
enstatite
A-11 LOW
CoMg
K
A-I!
HIGH
major-element
The
comers
hedenbergite
chemistry
clockwise
plotted
from
(CaFeSi206),
the
ferrosilite
(MgzSi206).
A-15 PIGEONITE
K
pyroxene
quadrilateral/'
diopside
1981 ).
Fe Fe
"StOWER....
FASTER"
CoFe
Me
Fe
A-I7
A-12 OLIVINE
A-12 PIGEONITE
A-12 ILMENITE
A-12 FELDSPATHIC
LOW K
A-17 VERY HIGH
"SLOWER"
A-14 FELDSPA THIC
LUNA-16
14053
A-IS
Fig.
OLIVINE
6.
Mare
"SLOWER....
b;L_alt pyroxenc
FASTER"
variations
with
arrows
A-17 VLT "SLOWER....
indicating
important
cr_.,stallization
Ti
"FASTER"
BI
FASTER" LUNA
trends
(adapted
from
24 VLT
BVSP,
1981 ).
on
upper
the
left are
(Fc2Si20¢,),
Taylor:
called
"pigeonltes,"
augites,"
and
a mineral
those
those
that
composition
was
near
minor
with
12-16%
with
>16%
first
discovered
the
CaO
Fe-rich
in lunar
end
are
of the
"subcalcic
Pyroxferroite
samples
and
is
has a
hedenbergite-ferrosilite
The
include
AI, Ti, Cr,
and
tan
trace amounts
of Na. Their use as diseriminant
usually be more
effective
for basalt petrogenesis
parameters
than the
chemistry.
As shown
range
in Fig. 5, the pyroxenes
in composition
to the
of the mare basalts.
contents
[usually
highland
rocks
and
(2)the
of equilibrium,
The
extensive
more
and
depletion,
do not
rates
that
aid
chemical
overall
resulting
in mare
This
well
to ferropyroxenes,
in the
pyroxenes
by
Plagioclase
cores
(range
in chemical
material
not
the Apollo
that displays
composition
without
Mg2SiO 4 (forsterite,
abbreviated
abbreviated
Compositions
as
Fa).
as
a solid
phase
Fo)
are
only
rims.
Furthermore,
solely
origin
The
trace-element
chemistry
MARE
,4 - 17
solution
series
between
constitute
0-35%
by volume
has compositions
ranging
in
many
FezSiO4
(fayalite,
in terms
of mole
basahs
of the rocks.
from
where
As shown
20% to 70% Fa (Fo
it
LOW
observed
in the
pyroxenes,
crystallization
of these
subsequent
Fe-enrichment
phases
results
in the melt.
0% to 100%
rocks,
of highland
where
caicic
In
in mare basalt.s,
to over 1% in the
basalt
plagloclase
feldspars.
Thus,
the
vs. highland
mare
plagioclase
is
based
is important
Plagioclase
frequently
contains
rare earth elements
(REE). This
BASALT
I
I
I
]
I
i
I
1
I
I
I
I
l
1
I
1
I
1
1
I
I
I
I
I
I
i
,4-/1
H/GH
l
_
t
I
I
I
I
1
I
l
I
I
I
K
VERY
H/GH
TI
I
I
t
I
I
I
I
I
1
I
1
I
I
1
i
I
I
I
l
i
l
I
I
I
1
I
i
I
t
i
I
l
1
I
I
I
I
1
I
I
I
I
I
I
1
I
I
1
1
1
I
I
l
I
I
I
I
I
I
I
in Fig. 7, it
80 to Fo 30),
where
OLIVINE
K
may'
always zoned from Mg-rich cores to more Fe-rich rims, e.g., from
Fo 80 to Fo 30 (Fa 20 to Fa 70). This Fe-enrichment
in olivine
to that
of lunar
with
compositions.
VLT FERROBASALTS
,a- 12 OL IVINE
with some near-pure
fayalite in the late-stage
mesostatis
(final
residue
from crystallization)
of the basahs.
Olivine in basalts is
is similar
of the
VLT
_t-II
A-IT'
mineral
of mare
of the plagioclase,
can be determined.
evolutionary
models.
more Eu than other
a
are Mn, Ni, Ca, Cr, Co, and Al.
is a major
K-rich
those of highland
on the Fe content
of a single particle
contents
zonation,
Na- and
Fe content
than
percent
of Fo or Fa. All other elements
are present
in amounts
<1 wt%. The most abundant
of these minor elements
in olivine
Olivine
chemical
to more
the
higher
15 basahs
change)
and
given
alkali
addition,
Fe content
of plagioclase,
particularly
can range from as much as 0.5% in the cores
LUNA 24
is a silicate
365
rocks.
displays
outward
Olivine
Olivine
of the low
the lunar
commonly
grading
as shown
are
but more importantly,
the cooling
of the crystal-melt
.system. These
displayed
base
Fe enrichment
a single
in turn
grading
are a consequence
that formed
for lunar
relatively
pyroxferroite.
trends
in
the
variation.
of the pyroxenes
plagioclase
considerably
in the basalts, sometimes
within
cores
mantled
by pigeonlte,
commonly
chemical
particularly
cooling
by their
result of the melt composition,
rates (and associated
kinetics)
effects are
(Fig. 6).
rocks
so characteristic
restricting
zonation
frequently
by auglte,
in Fig. 6. The
slower
represented
zonation
can be observed
grain, as orthopyroxene
mantled
FeO contents
thereby
chemical
is commonly
Ca
in the highland
high
This is largely a result of ( 1) the higher MgO
expressed
as Mg/(Mg+Fe)
ratios[
of the
attainment
basalts
in lunar pyroxenes
for a lunar
in highland
rocks commonly'
contain
even fewer alkalis, e.g., An
99 to An 90, Or 0 to 2. The low Ab and Or contents
of lunar
magmas
join.
major-element
elements
CaO
are augites.
Materials
A-12
PIGEON/TE
continued
in Mg-depletion
Olivine constitutes
with
from
it has compositions
from
Fa 7 to Fa 18 (Fo 93 to Fo 82). Olivine is less than 10% by volume
in anorthosite,
10-20%
in troctolite,
0-15% in gabbronorite,
and
up to 100% in dunite.
A-12
A-15
_-15
IL MENITE
OLIVINE
PIGEONITE
1
Plagiodase
Feldspar
I
I
The majority
of lunar
feldspars
are calcic
(CaAI2Si2Os; anorthite,
abbreviated
as An) in solid
sodic
plagioclase
plagioclase
also
(NaAISi3Os;
contains
albite,
trace
amounts
abbreviated
plagioclases
solution
with
ms Ab).
(ff K-feldspar
Lunar
(KAISi_Os;
orthoclase,
abbreviated
as Or) in solid solution.
The compositions
of felctspars are commonly
given as mole percent
of them three
comlx)nents,
plagioclase
contents
are
An, Ab, Or. AS shown in Fig. 8, the comtx)sitions
in mare basahs range from An 98 to An 74. The
minor
(0-3%).
Rare K- and Ba-feldspars
in late-stage
mesostasis
in some
those rich in KREEP components.
of the mare basalts,
The comtx)sitions
of
Or
I
,a -/4 FE L DSPA
/4 053
I
I
l
I
•
[
I
I
I
I
l
I
TlllO
1
0
l
I
l
20
t
I
40
1
60
I
I
80
_
I
I00
%Fa
are present
particularly
of felds'pars
Fig. 7. Fa_,'alitc content ah)ng the join Fe2SiO4-MgzSiO a fi)r marc basalts
(adapted from Papike aml Vaniman, 1978 ).
366
2rid Conference
positive
Eu anomaly,
compared
with
minerals
in the
that
caused
the
other
must
have
anorthosites
anomalies.
This
on Lunar
of
by the dual valance
REE,
indicates
negative
to
the
that
of Eu (2+,
there
Eu anomalies.
the lunar
led
Bases and Space Activities
highlands
"magma
arc
The
tx)sitivc
theory,"
consequently,
it should
did the derivative
bc possible
anomalies
plagioclase
contains
ocean
3+)
other
Eu
which
is one
istry, and
of lunar
that
of the
this
(and
basalts.
to realize
that
important
signature
terrestrial)
From
the
this brief
recognition
narrative,
of these
Eu
of lunar geochem-
discoveries
has permitted
major
interpretations
evolution.
postulates
that during the first 1O0 m.y. after the formation
of the
Moon, the outer Ix)rtions
melted to depths
of 100 km or so, and
as this
magma
cooled,
plagioclase
crystallized
and floated
to the
top of the melt to eventually
aggregate
into large masses forming
the early lunar crust, now referred to as the highlands.
The other,
more Mg- and Fe-rich,
forming
the residual
However,
this
minerals
settled to the depths of the ocean
from which
basalts were later generated.
lower
portion
had
a negative
Eu
anomaly
as,
OXIDE
The
nonsilicate
constituents
whitlockite,
metal
minerals
amounts.
I
L-24
I
I
I
baddeleyite,
and
other
phases
minerals
1
and chlor-
phases,
cohenite,
in hmar
in
of formation
basically
which
important
of _'arious
fluorapatite
and
and
lunar
native
niningerite,
(e.g.,
rocks and soils.
rocks
fO2)
are
of the
signatures
rocks
occur.
They also have tremendous
potential
any future lunar base activities. Whereas
lunar
I
yet
spinels
sulfide
Schreibersite,
imtx)rtant
oxide
conditions
VERY LOW Ti
r
rutile,
minor
ilmenite,
largely of meteoritic
origin,
are present
only in trace
The first ,several minerals
in this list, namely the oxides,
The
FELDSPAR
are
include
troilite
phases.
are the most
BASALT
which
rocks,
armalcolite,
apatite,
FeNi
MARE
minerals,
of lunar
chemistry,
MINERALS
the same
as those
are "opaque"
the Moon
of Earth,
minerals,
that prevailed
the
reflect
during
the
they
for utilization
with
silicate minerals are
oxide
phases,
the reducing
their
of
in which
most
of
conditions
on
formation.
A-17 VERY LOW Ti
Ilmenite
T_T--
I
,d-I/LOW
K
Ilmenite
is the
most
It has hexagonal
A-I/HIGH
K
lunar
ilmenite
which
exists
geikielite).
A-IP
VERY
-HIGH
i
77
I
I
I
I
<1%.
A-/20L
IV/NE
I
I
A-12
i
l
PIGEON/TE
A-12
I_LMENI'TE
I
I
I
of
the ilmenite
I
that
the
Mg content
I
PIGEONITE
I
I
I
Mg
contents
the
composition
rock,
LUNA-16
i
B I
1
I
a reflection
FEL DSPA
I
70
I
80
THIC
I
l
90
some
the
the
Moon.
The
of the
bulk
ilmenite
content
ilmenite
general
has
of the
contents
rock,
of 15-
ilmenite
vary
high
to terrestrial
formation,
ilmenites
was
Apollo
of the primary
also
the lunar
correlates
plot
along
the
contents
of
ilmenites from kimberlites,
it was originally
thought
however,
from
and
magnesium
17
with
magma.
a reflection
ilmenites
mare
with
volcanic
of
the
rocks.
the bulk
composition
Indeed,
the distribution
of
of Mg between
ilmenite
and silicates
is related
to the position
of ilmenite
within the crystallization
sequence,
which itself is a
I
function
A-/2
are
which
the TiOz
The
of lunar
Instead,
on
a function
Indeed,
lunar
of formation;
highest
contains
of the
11 and 17 basalts.
(Fig. 9).
many ilmenites are similar
which
are of high-pressure
I
from
content.
of
join
conditions
higher
for Apollo
compositions
FeTiO.c-MgTiO3
I
the
always
a reflection
is largely
magma
the higher
high pressure
A-15
the
Effectively,
20% are common
i
I
OLIVINE
magmatic
mineral
Cr, Mn, V, and Zr, are
almost
none,
in a rock
crystallized.
The
4-15
of the
of ilmenite
composition
ilmenite
FeTiO 3. Most
of the soUd solution
and MgTiO 3 (the
including
contains
in lunar rocks.
near
Mg, the result
FeTiO 3 (ilmenite)
terrestrial
mineral
compositions
elements,
ilmenite
state
amount
opaque
and
some
between
Although
reducing
i
contains
All other
Fe _÷, lunar
abundant
,symmetry
of cooling
rate
However,
it is doubtful
equilibrium
conditions,
and
oxygen
that
these
since
partial
MgO
pressure
contents
the composition
of ilmenite
significantly
even within one rock (Fig. 10).
The stability curve of pure ilmenite
is below
I
100
% An
the spinel
with
In fact, ilmenite
reduction
The
Fig. 8. Anorthite content (CaAlzSizOs) of mare basalt feldspars (adapted
from Papike and Vaniman, 1978).
phase
it is commonly
is commonly
formed
of this high-33spinel
production
is important
to rutile
which
of oxygen
in establishing
plus
iron
with
the
a lunar
the
release
Moon
fO2).
represent
can vary
that for ulvOspinel,
associated
as a product
(discussion
on
(i.e.,
all
(Fig. 11 ).
of subsolidus
below).
from
base. Ilmenite
of oxygen
lunar
materials
can be reduced
(l_tlliams
et al.,
7_O,Ior:
Materials
Jbr
a lunar
base
367
ILMENITE
WEIGHT
3
2
I
I
% MgO
4
!
I
5
6
|
I
?
m
-I
nn
m
i
m
iln
m
2
!
i
WEIGHT
3
% MgO
4
5
6
7
'
I
'
L
t
'
'
t
'
t
'
t
1
]
Apollo t l Low K
OlmiIm
1
I
i_/n
t.
0
I.,
! 12 llmenite
!
,4pO#o
,
1°1-
u
i
5t
0 I-l_
10 1
,
!
!
Apollo t50tw!ne
'
T
'
,
llI
'
,
Apo#o
sI0 I
I
i
!
,
'
t7
i
m
i
!
mm
loin
II
i
•
|
'
Luna t6
O--
!
i
|
i
A|
1
_"
p_.
o
':a =.g,,,r"_.,.'a,,_,a_
L
_JR
I
B Fek_spath¢
!
!
!
i
I
!
17114053
Im14072
Fig. 9.
MgO (x_ItL)
content
fi)r various
marc I)a.salt ilmcnitc,s
(adapted
J
1201 8
CO
(1)
CO
>,
I
I
I
I
1111
I
I
I
I
I
firom Pcq_ike el al., 1976).
L
T
[I
•
"_u
I
o
•
Uap
11¢I
•
T_
L I
I
I
T
1
i
Ru+I
U'_P_
"_
114 I
II_FpbtI
1
Web,let
R
(196q)
I
i
II/Fpb'
JBrioht
//"
L) I
FpblRu+I
i
O_
C"
<IS
"' Usp/D*l
tE
;
I
!
w¢..-
0
.2
d
I
Z
I I I l llJ[
n
i
i
10
I
i
BOo'c
Fig.
10.
MgO
El Goresy
(wt%)
Weight
variations
from
one
I/T('_)
rock (adapted
from
et al., 1971 ).
Fig.
11.
in the
Fugacity
Fe-Ti-O
1979).
This
on
reaction
Fig.
is that
I I, determined
associated
by
with
Taylor
eta/.
the
lower
( 1972
)
univariant
(hydrogen),
method
FeTiO3:TiO
z + Fe + 1/202
These
10.5w1%
O2
The
amount
This
ilmenite
of
reaction
using
oxygen
could
produced
be
indigenous
by
accomplished
this
reduction
by
solar-wind-implanted
the
reaction
hydrogenation
protons
is
Indeed,
soil
1990).
may
studies
ilmenite,
complications
and
have
which
as,sociated
particularly
even
not
the
be
from
beneficiation
a simple,
70
plot
Taylor
abundant
on
that
1985;
have
with
the
of an
of
Wu -
remain
process
lunar
of
feedstock
(Taylor
be
this
1985).
with
Fc _+. The
high-MgO
to
_)il.
by
largely
amounts
Fe-_+-free,
ilmenite
the
Knudsen,
conducted
17,
curves
Abbrcv.:
production
and
wafting
Alx)lio
one-step
grains
oxygen
been
uni_-ariant
1972).
Fpb = ferrop,_udobrook-
Gibson
contains
of the
et al..
I1 - ilmenitc;
shown
(Williams,
preliminary
ilmenite,
large.
is feasible
terrestrial
(1)
from
Usp = ulv6s'pincl;
studies
1200"C 1300°C
?
1
, i
_
x 104
vs. temperature
of ox)gen
s3,,stcm (adapted
adsorbed
Preliminary
r
rl_c
i
BO
Percent
in iLmenite
looo'c
T L
"Jr
T
90
wiistitc;
I - iron;
itc: Ru = ruffle.
curve
9oo'c
r_
--
--
MgO
ll/flu+l
18_
= I I I,li
10
0.1
of
T
i
lunar
e_-aluated.
from
lunar
and
Oder,
368
2nd Conference
Another
on Lunar
possible
utv6spinel
source
(Fe2TiO4),
Bases and
of
according
oxygen
Space Activities
is
the
spinel
phase,
12002
to the reaction
..c.....
•,
.Jl,
U_vo_lnel
Fe2TiO4 = TiO2 + 2Fe + O z
O
(2)
14.3 wt% 02
• dg .......-at
The
02 yield
from
for the ilmenite
is present
and
the
reduction
reaction.
up
to several
"Spinel
more
abundant.
section
The
complications
variable
below),
than
this spinel
phase
from
Apollo
12, 15,
compared
with
and
compositional
into its large-scale
is greater
though
in basalts
is quite
Group"
even
percent
17, its composition
(see
of ulvOspinel
However,
ilmenite
variability
?
E
A=
ilmenite
is generally
could
use for lunar oxygen
introduce
,'l[laU.#
production.
i°°#=,,
Spinel
Group
°IIIM.L
A
•|
I
Spinel
is the name
display
formula
for
represents
for a group
extensive
solid
these
minerals
2+ cations
Mg 2+) and
coordination
of minerals
solution.
with
The
is AiVB2"iO4,
in tetrahedral
(iv)
iv and
(sensu
as
vi coordination),
strtcta)
these
end
(MgAl204).
members
"chromian"
solution
In lunar
are
°
)o
basalts,
(e.g.,
spinels
than
ulv6spinels,
have
with
chromite
by
is
by the
distinct
names,
MgAl204
higher
V203
one
of
its inclusion
major
such
FeO,
contents
near
in Fo-rich
phases
olivine.
MgO,
such
If the
included
melt
and
change.
However,
for
if the
chromites
and
chromian
on
chemistry.
appears
as brown
contact
between
Cr203,
and
and
VzO 3
a discontinuity
mare
break
chromite
chromite
by renewed
is
the nuclei.
the
ulvOspinels
to tan
Some
crystallization
solid-state
The spinel
/
spinel
ulv6spinel
sharp
as
chromite.
The
and is reflected
core
followed
chromite
in
to rim. This
grains
Fig. 13) contain
later
acted
spinel
or
subsolidus
as
grains
reequilibration
of lunar rocks are typically
system:
FeCr204-Fe2TiO4-FeAI204.
major
a third
dimension
to this .system
cation
substitutions
component
(actually,
MgAIzO _) prov_de.s
(Figs. 12 and
14). The
of the .solid solution
in these
by Fe z++ Ti 4+ = 2(CrAi)
3+. The
of the
spinels
represented
The addition
lunar
principal
phases
generalized
in lunar mare
basalts
can
com-
are shown
in Fig. 14. Spinels are ubiquitous
in mare basalts where
they
display various
textures
and associations.
They are ,second in
abundance
only to ilmenite
gabbros,
abundance
rocks
and
than
tend
TiO2
and
1972 ).
Cr-rich
those
contain
14).
thin
because
isotropism.
troctolite.s,
basalts.
mineral
with
This spinel
spinels
lesser
in basalts. The)'
is not
of its pink
highland
called
along
the
opaque,
color,
in
high
much
in the
amounts
Certain
phase
midpoint
although
The
in basalts.
a spinel
of the
Figs. 12 and
section
and
in mare
to be chromites
than
troctolites,
for lunar spincls (adapted from Haggerty,
as the opaque
make up to 10-12% of some basalts (e.g., those from Apollo 12).
Spinels
-aLso occur in nonmare
rocks such
as anorthosites,
anorthositJc
Nomenclature
phase
the
also reflected in gradational changes
solution.
This could result from con-
of
compositions
trends
toward
titanian
latter
the bluish
earlier
12018,
of Mg as another
positional
it
diffusion.
the ternary
be represented
FeAb
Fig. 12.
melt,
the
in crystallization,
the
rocks (e.g.,
involving
within
,'I1\\
the
light,
trend from
a cessation
in that
tinuous
about
is commonly
compositional
reflects
growth
possess
In reflected
rims
the two
that display diffuse contacts,
in the chemistry
of the solid
/\
with
in TtO2 and FeO and decreasing
chromite.
in the
probably
as
it
is in contact
increasing
isolated
chemical
in A1203, MgO, and Cr20_, the overall composition
moving
ulvOspinel (Fig. 14). Most of the basalts that contain both
overgrowths
crystallize,
within the olivine, it is effectively
undergoes
no further
growth
or
to grow,
(Fig. 12 ).
1%. In typical
to
completely
from the
will continue
solid
as pleonaste
and varied
oxides
of AIzO3,
first
spinel
between
Some
and FeAl204
contents
the
(vi)
of the
use of modifiers
chromite.
have complicated
the
Fe 2+,
(FeAlzO4),and
compositions
"titanium"
between
in Fig. 13, besides
chromites
evidenced
or
ioo
F_r c ent
Fig. 13. Elemental distribution diagrams for chromites and ulvOspincls
in typical Apollo 12 basalt (adapted from El Goresy eta/., 1971 ).
A typically
chromite
(FeCr204)
,
as Fe2TiO4; Fe 2+ is in
solution
designated
have
essentially
1302,
basalts,
structural
coordination
hercynite
Solid
ulvOspinel
compositions
compositions
As shown
where
_'_
symmetry
general
B represents
3+ or 4+ cations
in octahedral
(e.g., Cr 3÷, A1-3+,Ti4+). The various members
spinel group
of minerals
(Fig. 12) include
uivOspinel
(FeFeTiO4,
commonly
written
both
cubic
....
)o
ol
We)ght
that
_
of MgO,
rocks,
pleonaste
lower
anorthositic
AIzO_,
notably
(slightly
MgAI204-FeA1204
but
it stands
refraction
Fejoin,
out
index,
in
and
Taylor..
FT
its composition
.
APOLLOt1
_'_
]
reduction
Fe
is important
the
soil
by
impacting
Fc
heated
as
and
Apollo
11
basalts.
(Fe0sMg0.5)Ti20
describe
the
FeTi2Os-MgTizOs
17
Fig.
Perspective
views
mare
basalt
lunar
base
carbon,
high
Ks well
when
which
impart
In
the
fact,
is driven
notably
a reducing
native
spinel
the
by
the
elements
environment
by the
in
metamorphosed
reduction
caused
evidence
of
shock
particles,
369
as being
material.
This
temperatures
base
generation
raw
reduction
a lunar
when
impacts.
of the
spinel
was
first
site
where
recognized
it occurs
Although
its
s, the
a mineral
an
is also
portions
(Fig.
16).
used
of
Detailed
in
accessory
composition
name
intermediate
as
as
samples
from
mineral
in Ti-
is
strictly
in
a broader
the
solid
chemical
defined
as
sense
solution
to
series
analyses
of
LUNA 24
15.
Spinel
a silicate melt
et al., 1972).
16
for
a
solar-wind-implanted
to the
rich
14.
secondary
undergoes
Armalcolite
the
MgAl204
chromite.
this
for
Armalcolite
.5 MC
Fig.
toward
.spinel,
micrometeorites.
of
hydrogen
_
of
readily
presence
5 M,1
moves
for
Materials
3-D system
comi-_)sitions
comix_sitional
and (b)
variations
sub_)lidus
during
reduction
(a)
(adapted
from
crystallization
from
El Gore_,
FeCr204-Fcz'[iO4-FcAI20_(modified
from
Haggerty,
1972).
Normal
tion
processes
and
are
rocks
soil, the normal
often
reduced
futile
+ native
lunar
rocks
a few
is
accompanying
in terrestrial
rocks
to
Fe.
Figure
crystallization
chromite
growth
and
continues.
the
last-formed
the
residual
subsequent
oxidation;
This
is the
14053,
a Ti-poor
normal
these
,spinel,
15 addresses
this
of spinel
from
changes
its
The
effect
uh'6spinel
components
Ti-rich
titanian
a melt,
the
spinel
of
is to
enriching
the
later
"exsolvc"
the
to
with
(Fig.
spinel,
1S).
In
ulv6spinel,
ilmenite,
(ff reaction.
composition
grains
sequence
chromite,
type
r(x.-ks
UlvOspinel
and
sometimes
reactior_s
the
crystalliza-
in lunar
paragenetic
subsolidus
14072),
to
however,
situation
involves
reduction.
to
ilmenite
+ native
Fe
involves
(e.g.,
reduced
native
Fe.
and
and
involve
During
typically
begins
as
ulv6spinel
as
subsolidus
reduction
on
ilmenite
+ native
spinel,
\,
normal
toward
remaining
'\,
and
Fe with
such
that
FeC
Fig. 16.
_'gO
AJrmalcolRe coml_)sitions (wt",,,)/lolled in the s},_lcm FeO-
MgO-Ti() 2 (adapted from A _>Pson
el _d. 1970 ).
370
2nd
Conference
armalcolite,
with
balance
the
the
formation
of
lunar
17).
rocks.
This
since
it sets
armalcolites
subsequently
found
on
occurrence
the
that
have
reaction
of
nesian
or
first
and
of
most
abundant
compositions
described
17
Two
gray
and
appear
be
in color.
type
ilmenite.
Although
identical.
either,
by
being
crystal
Because
the
are
second
having
CaO
ZrO
armalcolite.
titanate,
olite
and
is termed
the
wt%).
These
important
last
as resources
has
these
been
were
to
be
different
CaZrTi207
is characterized
is
and
called
Cr-Zr-Ca-
between
titanate.
definitive
the
This
are
Fig. 18.
Compositions
(wt%)
for
Cr-Zr-Ca-armalcolite
(C-Z-A),
Phase
Haggerty,
s
Oxide
The
in
Rutile
other
ha:ks
and
of ZrO2.
tx:curs
is generally
soils
minerals
are
of
rutile
associated
any
(TiO2)
with
volumetric
and
ilmenite
significance
baddeleyite
and
most
(ZrO2).
commonly
as a reaction
armalcolite.
the
oxide
1973).
(0.26-
Minerals
only
lunar
initial
as discrete,
rutile
Nb,
Ta,
which
melt
recrystaUizes
different
from
the
various
other
amounts
14
rock
14310,
schreibersite
Where
appreciable
Zr-bearing
forms
Troilite
zirconium
and/or
ilmenite
troilite
'_/
0
(i.e.,
may
°'
Ti305
v
04
MgTi20_,
v
05
v
06
o
07
microprobe
analyses
compositions
from
mare
basalts
anosovite
(TisOs)
as calculated
(adapted
from
Papike
et aft., 1976).
depicting
the
from
electron
the
there
of troilite
is usually
phase
most
in mare
of
are
common
basalts,
pnMuct.
It is commonly
also
with
native
Fe.
of
the
with
eutectic
origins
others.
than
is
and
residual
0.6%
from
commonly
ZrOz),
and
the
present.
sulfide
minerals
originally
native
between
of
troilite
in
In
all occurrences,
lunar
native
thought
that
Fe
Fe
in
with
in
and
the
Fe
the
a
texture
FeS.
This
lunar
the
is
rocks;
amount
1% by volume.
occurrence
where
it does
baddeleyite
associated
associated
the
much
example
iimenite
to
be
commonly
It was
several
less
up
also
spinel.
988°C
one
however,
The
Fig.
17.
Arm',dcolite
amount
of Ti _+ as
always
of
undoubtedly
FeTi205
and
An
likely,
the
that
not
MINERALS
common
and/or
was
reminiscent
o
most
is ubiquitous
most
(x:curs,
meteorite
However,
abundant
This
magma
rock,
rocks.
occurs
commonly
large
constituents.
both,
of armalcolite
is the
It
a silicate
contains
SULFIDE
rocks.
by
into
igneous
after
and
Baddeleyite
igneous
and/
ilmenite.
formed
an
baddeleyite
with
are
meteoritic
[(Fe,Ni)_P],
meteorites.
is rare
REE.
into
which
rutile
associated
soil
ilmenite
forming
and
the
normal
of
of
is secondary,
Primary
typically
rocks,"
reduction
futile
rock.
Cr,
effectively
subsequently
contains
the
the
this
grains,
"melt
that
Apollo
of
contains
in
from
cases,
euhedral
often
occurs
have
product
In such
formation
impacts
Oo
(Z-A),
from
l_)tentially
or
Other
armalcolitc
(A), Zr-armalcolitc
ZI, and zirconolite
(Z) (adapted
of ZrO2
Nbz()
armalcolite
first,
armaloc-
amounts
and
of
high-Mg
of armalcolite.
a composition
types
most
(4.3-11.5wt%),
(O. 15-0.53wt%),
two
of
distinctly
type
has
all
but
the
varieties
armalcolite
Cr-Zr-(La
and
characterized
determined
not
Cr203
and
series
from
rims
polymorphs
of
This
second,
YzO 3
been
that
are
The
11
returned
which
have
has
solution
in Apollo
with
not
Zr-armalcolite
(2.0-4.4wt%),
0.65
type
18).
is represented
compositions
compositions
third
(Fig.
solid
have
in
mag-
compositional
overlapping
variety,
type
from
form
petrographies,
suggested
contents.
The
distinct
samples
2 (3.8-6.2wt%),
(3.0-3.5wt%)
Fe-Mg
have
varieties,
lunar
results
to
observed)
type
structures
simply
cooling
samples
the
in
first
gray
was
Ti 3÷ in
varieties
liquid
occurrence
found
compositional
high
of
different
the
it
three
to
These
of
the
to high-TiO2-content
slow
lunar
typical
this
in
the
these
The
is
of
present
common
polymorphs,
it
varieties
tan
to
are
(>95%
is the
although
mi&sions.
as
type
This
lunar
and
in
intermediate
above.
basalts,
there
result
Earth.
rapidly;
armalcolite
of
during
of
the
armalcolite
In practice,
varieties
is another
presence
off
FeO
charge
presence
prevailed
is restricted
relatively
early-formed
ilmenite.
types
by
of armalcolite
cooled
the
This
that
is noteworthy
The
Activities
of
shown
environment
igneous
Space
considerations
armalcolite
rocks
and
have
Ti 3÷ (Fig.
reducing
of
Bases
structure,
amounts
distinctly
Lunar
crystal-chemical
within
appreciable
on
of
troilite
it is usually
associated
Its
formation
is as
a late-stage
with
is
ilmenitc
a result
an
accessory
crystallization
and spinel,
o.f the
but
bulk
Taylor:
composition
of the
of S controls
the
induced
shock
notably
(_6095,
formed
as
the
"Rusty
result
The
been
found
basalts.
of
that
as
that
of
troilite
probably
been
16
rocks,
most
likely
sulfur
during
shock
grains
and
that
identified
Them
60016
61016
as
a result
in
have
some
Apollo
of
Iron
present
lunar
of
the
as
rocks,
low
oxygen
crystallization
_0-
various
Ni)
prol'x)rtiorts
and
as
15.
taenite
Apollo
(1)indigenous,
reduction
of
metal,
certain
metamorphism
highland
lunar
Figure
soil
that
60335
diagonal
and
Yakouqtz
a plot
lines
not
imply
lunar.
that
Here,
The
Ni
erably,
it
these
and
from
20
shows
16
highland
the
over
chemical
,samples.
of
and
lunar
of
metal
easiest
"
_i%
_ _ ,o__
,,....... _
,
8
_ * _6 I
68415
9955=•
field"
that
native
,samples,
Goldstein
to
metal
this
field
does
can
0%
to
Fe
for
indigenous
In
.. ":
_o_5 Popk
Rocks
65o_5
_'°
i
Nickel
and
Co contents
(wt%)
of native
Fc grains
in numerous
16 r(x:ks (adapted
from M/sra and
Tay/or,
1975).
lines are used for reference
(see Fig. 19 caption).
vary
several
it is reasonable
the
notably
been
used
Using
samples
Apollo
must
to
sup-
to
estimate
soils
the
return
of
be
in the
The
diagonal
the
than
considerably
material,
this
proces,s
of
additional
the
Fe
signal
something
the
it was
soils
(i.e.,
that
lunar
soil
Therefore,
Fe °)
in the
¢x:curring
unraveling
to
the
there
soils
than
of disaggregated
unique
led
inherent
in
noticed
the
samples.
Fe
matter.
material
from
comt'x)sed
Indeed,
in
processes
.samples,
r¢x:k
have
1-3%.
lunar
were
formation.
native
complicated
to
only
the
that
of extralunar
meteoritic
(FMR)
from
metal.
in
signatures
t3pe
of
metallic
soils
l_)inted
soil
that
more
Since
this
to be
first
meteoritic
elements
meteoritic
of
estimated
most
the
siderophile
amount
resonance
greater
r¢_:ks.
are
influx
the
been
was
etc.,
the
has
contain
(ff certain
signatures,
ferromagnetic
Figure
rocks
contents
It, W, Re, Au,
such
With
the
highland
the
soil,
highland
consid-
Co.
that
practice,
reference.
4%
20.
Apollo
parallel
pose
Fe metal.
unique
for
..
is
_
Fe
as
be
•
lunar
native
within
may
Rocks
impact
of
native
Melt
of
soil
for
metal
from
by
to recover.
simply
Fc
Fig.
,samples
it is the
used
and
lunar
lunar
It
are
variation
Of all
_
in
formed
origin.
native
Ni
68al6
(0-8?/,,
(3)fragments
designated
of
50%
66095
magma
ct3_tallization
"meteoritic
lines
contents
_
_,0j
phases
(2)Fe
practice,
common
meteoritic
boundary
to
in
from
normal
In
composition
is of
Co
0%
the
of
two
kamacite
occurs
ulvOspinel),
mistakenly
The
Fe
crystallized
the
63335
•
#m)
because
time
as
of Co vs. Ni contents
outline
(1971)
meteorites.
the
(e.g.,
most
Rocks
S
however,
largely
intergrown,
rocks.
is the
at
metal,
during
igneous
19 shows
The
from
mare
and
(<20
rocks;
phase
igneous
metal
formed
and
in the
(4)
69935
12
Zn
as small
present
Native
minerals
and
is
usually
Ni).
of
in terrestrial
common
Fe
normal
meteoritic
68115
where
'_
prevailing
are
(8-50%
67955
vol%).
common
Native
that
67915
Melt
62295
"
60017
IRON
extremely
fugacities
(Fig.
present
(<O.Ol
Fe ° is not
it is an
65095
of
only
16 breccias
mobilization
it is only
quantities
NATIVE
in
63355
°
include
phases
grains
in some
metamorphism,
in minor
371
during
is essentially
positively
sphalerite.
observed
formed
base
Breccias
!s
105
it was
a lunar
volatility
meteorite-
Apollo
remobilization
(<lO-15#m)
was
the
troilite
of
The
during
for
components.
and
small
Sphalerite
the
have
cubanite,
of
contain
chemistry
of all other
sulfides
S content.
troilite
Some
Rock,"
process.
chalcopyrite,
the
of ,secondary
metamorphism.
<1 wt%
Other
in particular,
a direct
impact
FeS with
melt,
formation
Materials
the
our
in lunar
rock
during
origin
understanding
soil
the
of
this
of
formation
the
(dimu_sed
below).
25
LUNAR SOIL FORMATION
OF SINGLE-DOMAIN
20
AND THE ORIGIN
NATIVE IRON
0
0
A.s mentioned
815
native
Fe
apparent
lunar
origin
and
largely
from
What
5
A_m
10
15
WEIGHT % NICKEL
ii
t,a_a._
on
Fig.
19.
literature.
metal
and
Native
The
Fe metal
region
originating
Tayl¢w, 1975
from
).
compositions
labeled
by mission
"meteoritic"
a meteorite,
but
is not
is u._d
as compiled
necessarily
fi)r reference
from
the
indicative
of
(me
M/sra
the
erable
soil
Taylor
damage,
smallest
crater.
to <1
of
given
of
and
Cirlin
with
The
of
free
was
clues
following
Fe
in
betu_,'n
UlXm
times
more
derived
This
toward
under-
di_-ussion
the
the
lunar
size
lunar
that
the
on
soils
the
is taken
surface
in
of the
particles
is about
particles
size
(i.e.,
with
from
of
soils?
possesses,
causing
that
10%
aml
Earth
thereby
ranging
small
rocks
the
lunar
km/hr,
pits")
the
.several
soil
(1986).
craters
("zap
flux
the
atmosphere
impinge
/_m.
contains
imt'x)rtant
The
this
40,0(R)-250,OO0
craters
The
us
different
shielding
of
soil
which
formation.
particles
order
kilometers
the
has
lunar
from
significance
the
meteoritic
the
rocks
is inherently
Without
20
the
paradox
standing
05
above,
than
velocities
consid-
thousands
produced
the
diameter
micrometeorites)
of
these
of
372
was
2nd
Conference
'always
greater
on
than
impacts
smash
large
material
great
distances
is largely
a function
Two
tion,
basic
flux
soil
from
the
to
tion
of
glass
and
Figure
lunar
21
pieces
but
soil
the
1,0
The
larger
and
move
0.8
and
of
increase,
by
are
called
at a small
the
a
resonance
characteristic
tinates
and
regolith
material).
This
numbers
size
of
range
the
soil.
breccias
grain
The
the
in some
the
The
of the
actual
within
of
of
the
the
single-domain
showed
elemental
size
on
has
is the
the
are
the
size
with
first
direct
range.
range
particles
of the
notably
to
that
The
this
FMR
are
_,
Curie
essentially
the_
that
Fe 2÷ in
glass
disseminated
melting
and
the
process
solar
the
impose
silicate
precipitates
within
cooling
of
the
quenched
is so
fast
.900
••00
250
(k)
22.
Size distribution
Apollo
11 sample
are for sizes <40
Mcxlified
from
of Fe° metal
10084.
,g,, which
Housl_.
spheres
in agglutinitic
glass
Data are from TEM photographs.
are too small to be counted
with
from
The .squares
any certaint3,.
et a/. ( ! 974 ).
22).
point
pure
Fen?
The
wind
and
soil
is melted
a very
melt
as
I
150
well
solar-wind-implanted
a lx)rtion
elements
that
with
with
C. When
Fe °
single_lomain
bombarded
impact,
elemental
are
abundant
saturated
H and
such
reduced
of
lO0
l
determination
100-2OO
Subsequent
these
50
DIAMETER
Fig.
before
Fe ° (Fig.
of
I
the
Fe ° in the
studies
I
large
in
agglutinates,
single-domain
the
by
Fe
single-domain
o
o•
the
native
Fe
particles.
is
reducing
melt
that
might
wind
and
the
be
to
due
Fe °
l_D2°7.eb
(i.e.,
the
correlation
206 ages
origin
based
vs.
was
of
"exposure
of
the
age"
length
rough
of
can
the
agglutinates
amount
was
at
be correlated
AS A MEASURE
was
a function
of
the
concept
a function
lunar
soil
study
the
as
and
apparent
to
Thus,
the
with
Rb-Sr
this
established
reworking
solar
solar-wind-
workers
.samples.
the
of
Although
other
lunar
individual
to
correlations
soils.
soil
of
time
reworking
of
a ltmar
this
IJFeO
impact
in
time
sedimentologists,
and
upon
it prompted
for
of
exposure
is, the
real,
the
in Fe ° contents
That
particles
in
sized
for
rocks.
in
Fe ° content
not
Fe metal
of
flux.
gases
was
the
larger
responsible
resides
variations
differences
meteoritic
This
tiny
from
into
is
Fe ° that
the
to
aggregating
process"
soils
that
reducing
time.
and
additional
suggested
soils
of
it prevents
the
distinguishes
It was
diffusing
"autoreduction
of
implanted
effectively
myriad
and
from
This
production
become
environment
¸ --
agglu-
anticipated
(TEM)
the
in
is continually
by micrometeorite
spheres
not
numerous
that
origin
Moon
effectively
elements,
glass).
abundant
__
0.4--
detected
produced
the
of
soils
is, metallic
was
L
of
Fe in composition.
What
soil
is
soil
provided
the
WELDED
of
impact-produced
that
lunar
much
grains
measurements
of
Fe°, '' that
microscopic
agglutinates
sizes
majority
of
SPHERES
GLASS
#ass-welded
and
samples
It seems
electron
METAL
IN
0.6--
agglutina-
associated
resonance
in the
carriers
Transmission
rocks
only
(larger
(SD)
_..
of which
are
was
characteristic
of 40-300
of the
that
"single-domain
presence
Apollo,
of
resonance
Fe
O0
studies
-
I0084,85
"agglutinates."
Ferromagnetic
f
processes
and
,_ale.
_
--
0.2
particles
I
AGGREGATES
mineral
quenching
two
comminution
I
smaller
and
the
respectively,
the
into
lithic
These
•
comminu-
minerals
welding
melt.
f
development
( 1 ) simple
pr(_luced
depicts
,soil particles
meteorites.
smaller
soil:
of rocks
impact
decrease
the
lunar
the
the
Activities
impacts.
breaking
by
5pace
large
origin,
agglutination,
together
and
into
its
form
or
(2)
particles.
of the
material
micrometeorite-produced
compete
Bases
of micrometeorite
processes
and
fragments
the
rock
dL_tggregation
particles
Lunar
surface.
To
maturity.
OF SOIL
MATURITY
NILNOMETEORI!E
The
ferromagnetic
dominated
330
by
_t).
The
suggested
index
age
the
silicate
the
increase
a
Fig. 21.
Schematic
representation
of lunar
soil formation.
agglutinate
of
is/F••
for
from
soils.
function
of
agglutinate
maturity
of
As
content
(exposure)
at
the
an
and
to the
as
well
of
the
lunar
an
increase
(Fig.
23),
which
a
soil.
this
FeO
surface
species,
IJFeO).
Thus,
mature
levels
classification
mean
above,
of
in
soil.
.same
as
Fe
accompanying
increase
submature,
was
surface
FeO
extent,
with
in the
equivalent
explained
total
solar-wind-implanted
increases
immature,
I_. it
micrometeorite-
of the
exposure
of
;is
the
include
some
are
(40-
relative
by
melting
agglutinates,
17
of the
to
the
(reflected
is roughly
to
to
soils
particles
designated
Fe ° generated
content
of petrographic
of
is
lunar
normalized
It is necessary
of
all
Fe °
measlzre
amount
Fe ° metal
Apollo
function
a
duration
the
development
in terms
for
soils.
formed
the
does
in the
range
of soil
as
,so
signal
is a function,
liquid
Effectively,
increases,
be
of
fine-grained
intensity,
amount
autoreduction
of the
the
of lunar
spectra
to
this
FMR
might
because
impact
due
of
this
(Is/F••),
exposure
and
signal
intensity
that
content
resonance
a
This
grain
in
in
Is/F••
size,
is
turn
is a
concept
of
Tavlor:
-
100
!
!
I
I
I
|
I
I
I
T"
' --r
,
T
r
for
a lunar
base
373
T
I
I__
Ib)
E
90
'_11, (t
#
_0
'_:"
r-_
12
_. r,0
r
8O
_ IT
Materials
•
N'I08
o l_a
A
7
t--
i ID
i
"'%"
n
,_
c] All
o
l0
•
o
ico
o D
V
i_0
C l,,q'_,
z_
tSO
E
t
60
0
nO
v
o
O
v
j7
o
oo
Fig.
24.
Correlation
modified
from
of
Morr/s
ls/FeO
with
_)lar-wind
gases.
Figure
has
been
(1976).
o
50
13
V o
O
V
Y.
40
V
does
V
3O
not
are
m
It,
V
as for
v_ v
2
0
!0
or'l
I
i
I
1
I
1
1
ZO
10
PERCENT
I
I
I
30
I
4O
PETROGRAPHIC
I
I
.50
I
6O
up
soils
with
the
highest
be
indicative
70
90-150t,
AGGLUTINATES.
pick
17
The
23.
Correlation
determined
by point
are
from
given
of lffFeO
counting
with
all Apollo missions.
in Fig. 24. Figure
with
contents
a petrographic
The
modified
agglutinate
legend
from
for
of
.soils
micromope.
the
s},mbols
as
4He
originate
here
is
MCrrr/s (1976).
radionuclides
Based
upon
Various
22Na,
26A1, and
data,
lunar
soil
FeO
_'Ar,
from
the
S6Mn,
(<1
ram)
Apollo
Fig.
24 ) have
would
seem
to
are
those
wind
and
not
from
as
to
quantify
of
cosmogenic
"track
agreed
formation
of soils.
_32Xe
use
well
age
and
include
as
wind
The
on
attempted
it is generally
even
solar
4He.
exposure
solar
These
derived
(FeTiO3).
1990).
-_4Kr,
have
are
to
content
and
2(_'qe,
soils
,same
Therefore,
of
( Taylor,
studies
formation.
4He.
squares
4°Ar/_'Ar
of soil
isotopic
fine-grained
for
4He,
directly
reactions.
the
content
exist
for
soils
exposure
(open
17
the
ilmenite
amounts
contents
Apollo
17
14%
enough
thus,
gases
the
it is almost
Apollo
to
(sink)
have
ilmenite
also
rate
up
contents;
that
nuclear
The
contain
appreciable
FeO
of the
rare
absolute
Samples
used
retain
when
in fact,
Fig. 24).
,soils
higher
trapped
gases
Fig.
and
but
a "sponge"
17
Correlations
m
go_xi,
is good;
and
to be
Apollo
to
very
(also
basalts
appears
immature
<t:
be
correlation
l ffFeO
high-Ti
Ilmenite
V
v
to
the
C vs.
from
v
2O
appear
omitted,
that
are
the
densities."
the
much
rates
less
of
than
1 can/yr.
exposure
age
trapped
showed
_°Ar.
Thus,
,soil maturity,
that
the
which
for
.some
parameter
soils,
IJFeO
I,JFeO
is a flmction
correlates
is an
of surface
with
effective
exposure
index
of
age.
The most detailed investigations applying IJFeO measurements
on lunar soils were performed on core samples taken during the
Apollo missions, particularly lS-17. Horizons of mature soil (high
IJFc_)) were di_overed
in these soil profiles. These mature soil
layers are the result of slow formation with extensive reworking
("gardening")
in the upper few centimeters or so of the regolith,
a process
Is/FeO
AS A MEASURE
OF SOLAR-WIND
ELEMENTAL
CONCENTRATIONS
IN
LUNAR
M_wrt_s
of
152
this
a
(1976)
,softs
large
measured
and
for
suite
variety
of
implanted
other
C,
the
direct
the
contents
of
the
l_FeO
Nuclear
and
its
small
an
extremely
the
fusion
of
reactants.
the
3('At
(i.e.,
of
With
ls/FeO
with
example,
were
IjFeO
desirable
radioactive
This
of several
and
soils.
For
shown
values.
Figure
exfx)sure
what
age)
practical
soil
bury
profile
slow
reworking" However, large
situ
the
_s
deposition,
of quie,_ent
soil
to
be
one
24
for
various
of
the
most
revealed
but
useful
commercial
"in
situ"
(i.e.,
in
cores
sporadic
does
It was
meteorite
mature)
events
development.
units in thc cores may be
layers with horizontal extent
of the secrets hidden within
continues today. However,
fraction
of 88
exposure.
I_FeO
or
horizons
not
represent
intermLxcd
with
recognized
that
the
only discontinuous pods, rather than
and time siguiticancc. The unraveling
the soils is complicated and research
the concept of IjFeO h_s proven to
in
lunar
endeaw_rs
mience
inwflved
and
with
will
a lunar
Ix*
of
u._
base.
with
use
are
SUMMARY
soils?
source
more
<25-#m-size
to correlate
However,
is a highly
important
contents
of
4He.
of lunar
4He
"in
the
periods
fraction
increasing
that
termed
obliterate
continuous
the
surface
gases
with
correlation
amounts
with
of
the
C and
fusion
of
correlated
values
for
it W',LS possible
in concentration
shows
vs. 4He
ls/FeO
indices
so
SOILS
90-150-#m-size
of .samples,
N,
increase
the
impacts
_)urce
products,
of
3He,
the
of
energy
and
lunar
most
solar-wind-implanted
abundant
soils.
4He.
At first
highly
species
Figure
glance,
24
the
shows
4He
The
because
soils
are
prized
of
can
be
l_/FeO
correlation
warious
constituents
minerals,
and
construct
a lunar
present
and
by
on
minerals,
impacts.
the
gla._ses,
base.
surface,
but
The
also
finer
of
will
The
be
the
anlong
lunar
fraction
the
regolith,
is composed
includes
Moon,
mostly
namely
raw
the
fragmental
of disaggregatcd
gla-ss 3' fragments
of
the
the
materials
regolith
fu.ca:d
(i.e.,
r(x:ks,
u._d
material
rocks
together
<1 cm),
to
374
,
2nd Conference
informally
referred
on Lunar
to
Bases and Space Activities
as soil,
is probably
the
most
imlx)rtant
tx)rtion
of the regolith
for use at a lunar base. This soil can be
used as insulation
against
cosmic
rays, for lunar ceramics
and
abodes,
etc.
for growing
The
well
soil contains
as various
potential
minerals,
.soil are
helium
for nuclear
particularly
sources
The
agglutinates
and
the
lunar
surface
a function
increases
products
of
elements,
is requisite
of
for rocket
.soil's
fuel,
Ti,
in the soil
maturity.
These
of metallic
maturity),
relative
the
Fe. The
He
and
plans
tff
IffFeO
solar-wind-
lunar
of all aspects
to any efficient
the
of
H, in the
knowledge
amount
Thus,
amounts
Apollo
11
soil.
It is
of the
for colonizing
lunar
Preliminary
The
lunar
samples
integrity.
11 Preliminary
Lunar
Sample
made
collection
usually
it must
is a national
and curated
frugal
use
treasure,
and
.samples,
the
with concern
for their
of ,samples
for various
scientific.
Therefore,
before
samples
be determined
that every attempt
has
to ( 1) use analog
either
.synthetic
are
been
or natural
(e.g.,
terrestrial
or meteoritic
.specimens)
and (2)design
experiments
such that the smallest amount of lunar material is needed without
jeapardizing
the quality
of the
of lunar
materials,
for allocation
protx)sal
to the
Planetary
address
(1)the
particularly
with
merits;
(2)preliminary
(4) the
); (5)the
associates;
for conducting
and
individual
situation,
needed;
therefore,
befiJre
request,
Planetary
tion
and
number
analog
of the
(6)a
of
the
request.
(LAPST),
to NASA concerning
the
Materials
who
will
request.
Curator
effort to assist an individual
experiment
merits its use.
Ulxm
and
upon
the
information
shotfld
be
receipt
by the
of the
Lunar
and
11 Organic
Lunar Surface
There
that
are
compilation
and
are
not
Documents
many
catalogs
commonly
a recommenda-
It should
be emphasized
the proper
of many
NASA publications
of these
to
the
and can be obtained
Planetary
at_mt
Materials
(713)
483-3274
Stereo_-opic
Sanlple
1969.
1 t. Lunar Receiving
I)ircctorate,
MSC, NASA,
(Flt)ry
D. A., Simoneit
Photography
(Greenwood
Informatkm
Examination
Examination
of
Lunar
1325-1339.
Team,
1970. )
Apollo
12 Preliminary
Science
Apollo
12 I.unar- "Sample
on
the
W. R. et al,
Catalog
_a
(ff
1971.)
(Revised).
JSC
Samples
(Lunar
from
Apollo
Sample
R_.qx)rt. NA_Dt SP-235,
Information.
NA.g4
12.
Preliminary,
1970.
TRR-353.
(Warner
J.,
1970. )
Electron
Microprobe
_%amples. Unit,.
Analyses
of Minerals
Net,, Mexico
._ec.
from
Apollo
Ptd_l. No..3.
12 Ltmar
(Bu_'he
E I). ct
ai., 1971.)
Apollo
12
Coarse
De_-ription,
and
Fines
(2-10
Inventory.
mm):
Sample
NA£4
JSC
14434.
Lunar
Samples
Locations,
(Marvin
U. B.,
! 979. )
Preliminary
Examination
Science,
Team,
14 Preliminary
Apollo
14
Lunar
58062.
(Lunar
Surface
(Alxfllo
arc
from
Apolh)
Prdiminary
14.
Examination
Report.
NASA MSCSP-272,
Information
Catalog
Office,
Stereoscopic
NA.Dt
1714X-
197 I. )
Photography
TMX-58072.
1971
MSC
at Fra Mauro
(Carrier
"_¢ D. and Heiken
G., 1972.)
Deseription,
Classification,
Apollo
14
Coarse
B., 1977.)
is a
Sample
_-C_mple Curator's
Closeup
ff the
of which
,_ience
Sample
14). NASAJSC
.sample,
,samples
(Lunar
1971.)
Apollo
Lunar
of
173, 681-693.
Classification.
lunar
Atx)llo
(4-10
mm)
12922.
(Kramer
Surtz Prof
14 Landing
Comprehensive
W. et al., 1975.)
Sample
Ix)cation
Apollo
;and
E E. and Twedell
Site in the Fva Mauro
Pal). 880. (Swarm
of Scqected
(TWedell
Rock
of the
(Phinney
Fines
Maps
14
Walton
Inventory
NA,g,t JSC
of the AlX)llo
JSC 13842.
and
14. NASAJSC
D.
Highlancts.
(;. A. et al., 1977. )
14 Breccia
,Samples.
NA,Dt
D. et al., 1977.)
Samples.
NA,Cet JSC
14240.
(Carlson
1. C and
J. A., 1978. )
to
Coordinator
NASA Johnson
Space Center - Code
Houston TX 77058
11.
E E. et al., 1977. )
167,
every
Following
several
by writing
Aixfllo
12
Lithological
public.
publications,
NA.g4 SP-214,
Apollo
Histo_'.
TMX-58077.
Lunar
(Kramer
make
Samples
and documents
known
Report.
Catalog
Contamination
NAX4
Il
Geology
on Lunar
with
D. H, 1969)
Closeup
Tranquility.
U.S. G_L
Catalogs
Returned
and Applications
-Sample from Apollo
make
and his staff will
in obtaining
be
facilities
Depending
there may be some additional
the Planetary
Materials
Curator
Team
needed;
as can
investigator
be rtwiewed
11.
Alx _llo 14
samples;
best
description
any
a short
.samples
(as
the experiment.
submitting
that the Planetary
on
size
Apollo
Preliminary.
pmpo.'-sal should
(ff the principal
the prtg)o.c, al will
Sample
to write
apply
to be conducted,
and/or
engineering
requested
credentials
necessary
to formally
This
obtained
mass
.sample
research
contacted
Curator.
the experiment
to its ._ientific
results
of the
sTmcific
determined
,sample
of
In order
it is nece._sary
Materials
nature
respect
(3) consideration
results.
Samples
_'ience
Science
B. R., and Smith
12522.
from
Sample
1969. )
Information
I,alx)r'ator3,,
1969.
Apollo
Samples
(Lunar
of the Lunar
Atx)llo
Apollo
Lunar
E. M. et ai., 1969.)
Science,
must be preserved
This
entails
the
purposes,
allocated,
Team,
(Shoemaker
of
1211-1227.
Setting
Preliminary
Samples
.sample
165,
Geologic
AlX)llo
Lunar
Examination
Science,
the Moon.
APPENDIX
Obtaining
Documents
Examination
as Fe, AI, Si, and
also increases.
the
notably
a thorough
are
components
products
the
(i.e.,
of solar-wind
regolith
of
that
as
IJFeO,
measures
the amount
of
as maturity
increases.
As exlx)sure
is indicative
that
hydrogen
such
quantities
signature
obvious
and
tremendous
absorption
implanted
these
impact-melt
FMR signature
of a soil,
agglutinates,
which
increases
at
phases,
metals
peculiar
are
contain
oxide
Sample
elements,
elements,
For example,
of oxygen
energy,
of valuable
solar-wind-implanted
importance.
for construction.
agglutinates
for the extraction
-abundant
economic
of the
called
plants,
Lunar
SN2
Apollo
15
Apollo
! 5 Preliminat
Atx)llo
15
1972.
Lunar
3' Science
Rclx)rt.
Samples--Collection
NASA MSC SP-289,
of
Papers.
1972.
Sc/enct;
175.
Taylor: Materials
Apollo
15
Coarse
De,_ription,
Fines
and
(4-10
Inventory.
mm):
Sample
Classification,
03228.
(Powell
NALg4 MSC
B. N.,
1972. )
Documentation
of Apollo
Rept. 47. (Sutton
Lunar
Sample
(Lunar
Apollo
R: Let
Mineral
NewMeMco
and
_ec.
Glass
Apollo
Analyses
15 Rake
of Separated
of Apollo
Spinel
Samples
Particles.
Lunar
1296
Regolith
1983.)
Breccia
Univ.
and
Origin.
Univ.
C. E. et al., 1973.)
and
M J., ! 974. )
Branch
Apollo
17 Lunar
Science
182,
Team,
16
Apollo
16 Preliminary
Apollo
De._-ription,
Apollo
_ience
Coarse
(4-10
and Inventory.
16 Rake ,Samples
De_ription,
and
P D. and Ryder
G.,
Sample
NA_g4 MSC
NASA
MSC
(Smith
Geologic
Cla:_sification,
182,
Samples from
et al., 1972.)
Lunar
Sample
Laboratory.
the
(Lunar
Samples
from
Lofgren
G., 1973.)
Stations
16
Description.
Catalog
Catalog
Team,
New
(Keii
MSC
K.
16
Receiving
of
Apollo
13. NASA JSC
16
(Phinney
Rake
W. and
Samples:
179,
Petrographic
23-34.
and
(Apollo
16
Chemical
Preliminary
! 973. )
16 Rake Sm'nples
Mexico
from
the LM Area and Station
,_Oec. PubL No.
Non-Mare
Rewired. NASAJSC
14565.
Catalog
of Pristine
Revimd. NASvtJSC
Apollo
13. (Warner
R D. et al.,
Catalog
16 Soil Catalog
of Alx)llo
Curatrwial
Materials
(Ryder
Part
1. Non-Anorthosites
G. and Norman
M. D., 1979.)
Non-Mare
Materials
Part
2. Anorthosites
14603. (Ryder G. and Norman M. D., 1979.)
61220
4 mm Fines. NASAJSC
U. B. and Mosie
Classification
Curatorial
Branch
and De,_ription
t_bl.
No.
of 1-
53. (Marvin
A. B., 1980. )
16 Rocks
Branch
17
De_-ription.
Preliminary
Examination
NA.g4JSCSP-330,
Trans
AGU,
1973.
Sample
(Meyer C,
54, 580-622.
of Taurus-Littrow:
Location,
1973. )
(Bence
Apollo
(Apollo
Field
Information
Catalog
Atx)llo
laboratory,
A. E.,
17 Ianding
Geology
Site.
Investigation
Classification,
from
Station
17. NA_g4 MSC4)3211.
1973. )
and
Inventory
of
6. NASA JSC (Phinney
Cla,_sification,
and Inventory
Stations
lA,
Studies
of
Samples
Apollo
Wet
17
8. NAX4 JSC
from
Rake
al., 1974. )
of 113 Apollo
2, 7, and
17, Vol. I; Vol 2. Smithsonian
Boulder
Astroph)_s.
i 7 Rake
(Keil
K. ct
1, Station
Obser
2,
(Adams
J. B. et al., 1974. )
Microprobe
from
Apollo
S/_,c. Pub/.
Analysis
17 Rake
No. I6. (Warner
Plagioclase
Catalug
from
New
Fe-Ti Oxides
Mart" Basalts.
Atx)llo
17
17 Rake
Me._co
lMiv.
and
New
Metal
Mexico
R. I). et al., 1976.)
Analysis
of
Rake
Olivine,
Samples
,_ec.
Pyroxene,
and
,'-Sample Mart = Basalts.
I_dOl. No. 16. (Warner
of Apollo
8. Unit,.
of Spincl,
Sample
Microprobe
Catalog
of Lunar
and
Trace
Unit,.
R. 1). et al., 1976.)
from
P_d_l. No.
Publ.
Part
1. 60015-62315.
No.
52. (Ryder
NASAJSC
Mare Ba,,_alts Greater
Element
and I.ofgren
Houston.
Guideb(x)k
17243,
of Pristine
and Petrographic
Rcix)rt.
672-(x-qO.
Neu, MexicoSPec.
P, 1972. )
Inventory
1, 4, and
Lunar
1976.)
Catalog
R. M,
Stations
1A, 2, 7, and
15. (Warner
R. I). et al.,
1978. )
Lunar
of Apollo
5. Univ.
5. NASA
Alx)llo
( Butler
and
Science,
Examination
16 Rake
Eos
Receiving
Electron
Classification,
Apollo
of 151 Apollo
and Station
NAL_ MSC 03210.
Description,
The
Inventory
LM Area
Information
(Fruland
1973.)
Sample
Apolh)
J. V. and Steele
,_ience
Exploration
Electron
and
(Apollo
Intcrdi,_iplinary
U. B., 1972.)
Sample
Chemical
_%amples from
al., 1974.)
Classification,
(Marvin
and 68537
Inventory.
1972.
Samples:
659-672.
17 Results.
Demription,
NASd SP-315,
mm):
67515
Classification,
10045.
ed., 1973. )
Lunar
I. M., 1972.)
Description,
JSC
Apollo
17 Coarse
Fines
(4-10
mm)
Classification,
and Photo Index. NA£4JSC
Team,
15 landing
Houston.
Report.
Fines
NASA
1973.)
I)e,_ription,
16
Workb(x)k.
17 Preliminary
_qence,
G., 1985.)
of the Apollo
(Spudis
17
Apollo
Description,
pp. (Ryder
Apollo
Samples
ApoUo
375
Workshop
on Apollo
16. LP! Tech. Rept. 814)1. (James
o. B. and
HO'z E, e4s., 1981. ) Lunar and Planetary Institute,
Houston.
Apollo
1, 2, and 3. Curatorial
Institute,
Bulk
Minerals
of Igneous
and Petrology
and Planetary
Analyses.
NA_g4 JSC ( Drake
Parts
Site. LPI Tech. Rpt. 8(>4).3. 126 pp.
! 986.)
Rocks:
Group
10. (Nehru
15 Rocks:
on the Geology
MSC 03209.
P E et al., 1973.)
Classification,
Ptdol. 5I¢>. 72,JSC2078Z
Workshop
Microprobe
of
Deep-Drill-Core:
Inventory
Catalog
15. NA£4
and Non-Mare
11. (Hlava
Spec. Publ. No.
15
Atx)ilo
Electron
Publ. No.
in Apollo
NewMexico
O,
1972. )
Microbreccias
Microprobe
Ilmenite
U.S. Geol. Surv. lnteragen
base
1972.)
Catalog
laboratory,
15 Rake ,Sample
Electron
al,
Information
Receiving
Rock,
15 Samples.
for a lunar
The
E
for
M.,
1981.)
the lk)ulders
Curatorial
Geologic
Chemistry.
Luna
Lunar
Investigation
458,
and
at Station
Branch
17 Ianding
Site (Maps).
E. Wet al., 1981.)
than 40 Grams
LPI Contr
Part
Planetary
6, Apollo
1. Major
(l.ofgren
G. E.
Institute,
17. NASA JSC-
I_d_l. No. 55. ( Phinney
W, 19e !. )
of the
Valley:
Apolh)
Pap. 1080.
(Wolfe
Taurus
I.ittrow
U.S. GeoL .gun,. I_>f
16
is,sue Especially
Earth Planet.
De_'otcd
to the Study of _)me
S(g. Let& 13, 223-472.
1972.
Luna
16 ?"_amples.
i_sue Espcially Dew)ted
to the Study of ,'_)me
Fxtrth Planet. ,_'i. Left., 17, 1-294. 1972.
Luna
20 ,_maples.
16_)4,
G. and Norman
M. D.,
Luna
20
1980.)
Catalog
of Apollo
Curatorial
16 Rocks
Branch
PubL
Part 2. 63335-66095.
No.
52. (Ryder
NASAJSC
16¢_ff)4,
G. and Norman
M. D.,
Luna 20--A
1980. )
Catalog
of Apollu
Curatorial
16 Rocks
Branch
Publ.
Part 3. 6701%69965.
5/¢>. 52. (Ryder
NA£4JSC
16004,
G. and Norman
M. D.,
Acta,
Further
1980. )
Geology of the Apollo 16 Area, Central Lunar Highlands.
Sum,. lXa>f. Pap. 1048. (Ulrich G. E. et al., 1981.)
by the
U& Geol.
hldia
eds.,
Study of £'_,ampics from
Unmanned
3 7, 719Advances
Nat.
Luna
1110.
1974. )
(Anders
in Lunar
,_'i. Acad.,
the l,unar
20 Spacecraft.
New
E. and Albcc
Re_-arch:
Delhi.
Highlands
Geoctn'm.
Luna
(Bhandari
Returned
Cosmocbim.
A. L., 1973. )
16 and
20
Samples.
N. and Rao M. N.,
376
2nd
Luna
Conference
on
Lunar
Bases
and
Space
Activities
24
Occurrence
to
Luna
24
Samples
Presented
De_ription.
Preliminary
Data
Automatic
for
Crisium:
Station
The
USA:
Catalog
J. S. and
Regolith
(Barsukov
IL B., 1978.)
the
(Nagle
the
Lunar
3303-3318.
Mare
to
NASAJSC.
Core
Luna
24.
and
Walton
Warner
W. J. A., 1977.)
Brought
Proc.
Preliminary
to
Lunar
Earth
Sci.
The
by
the
Conf.
8th,
V. L, 1977.)
View
Luna
New
York.
24.
(Papike
J. J.
and
Merrill
Fragments
Thin
in Lunar
,Sections.
NASA
Soils
JSC
and
14394.
Breccias:
(Bickel
Guide
C.
E. and
J. L, 1978.)
Lunar
Regolith.
(Papike
Ret,.
J. J. et al.,
Handbook
of
(Morris
from
Pergamon,
of ANT
Polished
Geop_s.
Space
Phys.,
20,
761-826.
1982.)
Lunar
Softs
Part
1: Atxfllo
! 1-15.
NAX4JSC
!_169.
Part
2: Atxfllo
16-17.
NASAJSC
1_169.
R. V. et al., 1983.)
Handbook
of
(Morris
Lunar
Soils
R. V. et al.,
1983.)
Guidebooks
Breccia
Guidelx>ok
King
No.
1-14321.
NASAJSC
14753.
(Meyer
C. and
C. D., 1979.)
Breccia
Guidebook
R. and
Breccia
No.
Taylor
L. A.,
and
Mosie
NASA
JSC
16198.
(Garrison
J.
1979.)
Guidebook
Breccia
2-66095.
No.
NA,_4
JSC
16242.
(Taylor
G. J.
)
of
the
conscientiously
No.
4-67015.
NASAJSC
16671.
(Marvin
U. B.,
Guidelx_ok
No.
5-14305.
NAX4JSC
19267.
(Shervais
J. W.
(Taylor
G. J.
manuscript
Graham
supported
has
thorough
colleagues,
Guidebook
1 would
like to thank my good Tennessee
friend
inspiration
that he has provided
to me on numerous
occasions,
e.g., while compiling
the data for this review paper.
all mistakes
were
originally
due
to his influence.
However,
version
3-67915.
A. B., 1979.
Acknowledgments.
Jack Daniels for the
and
Ryder
and
by NASA Grant
been
critical
Paul
improved
reviews
Spudis.
Any and
this final
immensely
of
two
A portion
by
highly
the
respected
of this endeavor
was
9-62.
1980.)
Breccia
and
Taylor
Breccia
Guidebook
and
Mosie
Breccia
No.
KJ.,
Guidebook
for
M. D. and
Guidelx_k
Lunar
for
17243.
PublicatT'ons
Demription,
Breccia
the
on
NASA
Boulders
W.,
19492.
(Shervais
J. W.,
JSC
20416.
(Salpas
P. A.,
NA,_I
JSC
17393.
at
Station
6,
ApoLlo
17.
NASA
JSC
1981.)
NASA
Subsampling
TMX-58070.
of
Apollo
(Fryxell
14
R. and
Core
Heiken
G.,
of
58066.
Stratigraphy
of
(Heiken
Lunar
Core
(Lindsay
Samples
the
by
AIxfllo
12. NASet
TMX-
197 I. )
ApoLlo
G. ct al.,
(;ore
Returned
J. E et al.,
15
Core.
NASA
TMX-58101.
09252.
(Duke
M. B. and
Nagle
J. S.,
_ubcs
lunar
74002/74001
Dissection
and
De,_ription.
NASA
JSC
J. W. ( 19751
M. A. and
ilmenite.
(X_ X_
Houston.
Curattmial
Branch
NASAJSC
Table
of
NAX4
PubL
to the
Core
17659.
Sample
JS_
( Nagle
Samples
(Fruland
the
R. M. and
Depths
for
Curatorial
J. S., 1978.
from
Apollo
Branx'h
)
pp.
Reimold
15,
16,
16
landing
J. N.,
and
56.
1981.)
17
Publ.
No.
Core
60009/60010.
Site.
J.
(ALlton
Cores.
J.
et
al.,
1981.)
Catalog
of
17172.
the
Apollo
(Fruland
16
Lunar
R. M. et al.,
NASA
JSC
1982.)
A
on
Catalog
( Heiken
Petrology
pp.
Lunar
G., 1974.
of
(Heiken
Lunar
of
Lunar
G.,
Stratigraphy
(l,ind,sayJ.
,_ils.
NASA
JSC,
Curatorial
Branch
Publ.
and
Soils.
Rev.
Geophys.
Space
Phys.,
Elsevier
_i.
13,
567-587.
and
Sedimentology.
E, 1976.)
Publ.
Co.,
302
H.
12
Planet.
Wiley,
Al_fllo
Volcanism
opaque
Prrw.
on
minerals
Lunar
&_. Conf
New York. 323 pp.
Lunar
oxygen
production
from
Activities
of the 21st
Lunar
and
Planetary
(1971)
lunar
Metallic
_il.
Sci. Left.,
Armalcolite
samples.
Pr_'.
inclusions
Lunar
Centu O,
Institute,
and
So'.
metal
Conf.
2ml,
E.-H,
13, 328-352.
and genetically
Proc. Lunar
Paton
micrometeorite
Conf.
,_.
N. E., and
alteration
associated
Conf
(_eoldbcrg
of the
opaque
min-
4th, pp. 777-797.
lunar
I. B. (1974)
regolith.
Proc.
_flar
Lutvar
5th, pp. 2623-2642.
K. ('. and
Ta}4or
L. A. (1975)
16 r_2k,s. Proc. Lumtr
R. _¢_(1976)
Surface
J. J. and
Bence
Characteristics
&_. Conf
eXlX_sure
Proc. Lunar,_"
logy. Rev. Geop_.
Cr_st'um: The
Vieu,from
pp. 371-4(11.
Pergamon,
J. J., Simon
J. J.,
and
Hodges
Mare
._ce
Smith J. V (1974)
dential addres,s,
Smith J. v. and
story., Part
Luna
A comparati_x
basalts:
Chemimry,
and
petro-
Luna 24 ferrobasalts
and the mare
miner'altrgy,
and petrolog T. In Mare
24
(J.J.
Papike
Laul J. C. (1982)
petrology.
Ret,.
and
The
(A_p_s.
A. E., Cameron
chemistry',
IL B. Merrill,
ett,¢. ),
mineralogy,
lunar
regolith:
,_t_ace Phys.,
M., and
and
Chem20,
Rhtxles
761.I.M.
petrology.
Rt_,.
story,
presi-
14, 475-$40.
Lunar mineralogy:
Part I. Am. Mineral.,
Steele
II. Am.
rocks:
New '_k_rk.
Crystal
t'hys.,
in
17. 1612-1641.
E N., Bcnce
basalts:
tff lunar
Planetary
P_s.,
s. B., and
mineralogy,
particles
7th, pp. 315-335.
A. E. (1979)
s. ,_'e
of metal
6th. pp. 615-639.
indices
Omf
Papike J. J. and Vaniman
I). T (19781
basalt suite: Comparative
chemistry,
Geophys.
1975.)
Earth
FMR study.
Papike
the
Luna 16: An opaque
mineral study and a systematic
compositional
variations
of spinels
from
Mare
R. M., Cirlin
wind
(1976)
)
Basaltt2-
Procellarum
C. W. (1985)
Apollo
S. E. (1973)
istry,
826.
Soils
Oceanus
Yakowitz
the
in the lunar
Papike
l$dolications
(1981)
Lum-_rMineraloR),.
I. and
in
Fecunditatis.
Misra
from
Knudscn
Haggerty
S. E. (1972)
examination
of
Papike
Drill
from
177-191.
Morris
Apollo
Project)
In Lunar
Bases and
_mce
Mcndell,
ed.),
pp. 543-'_50.
particles
Aixfllo
Intrtxluction
rocks
Gibson
,_.
1976.)
Drive
Study
mineral
Conf.. pp. 55-63.
pp. 219-235.
Housley
NASAJSC
Volcanism
Frondel
erals
1972.)
Catak_g
A new
I1 Lunar,_.
the Terrestrial Planets. Pergamon,
New York. 1286 pp.
El Croresy A.. Ramdohr
E, and Taylor
L. A. ( 1971 ) The
Haggerty
Drill
Armalcolite:
Proc. Apollo
BVSP (Basaltic
Goldstein
and
1971.)
De,_ription
A. T. et al. (1970)
2rid
(Norman
)
Cores
14230.
Anderson
in the
67016.
1981.
Dissection,
Sample
JSC
L A., 1985.)
G. G.,
(Phinney
NASA
8-72275.
Taylor
Garcia
18743.
L. A., 1984.)
No.
and
JSC
11 samples.
7-14321.
Taylor
Guidebook
WiLlis
NASA
)
No.
S., and
Breccia
6-67435.
A. B., 1982.
Guidebook
Knapp
REFERENCES
L. A., 1983.)
I. M. (1976)
Mineral.,
A heavenly
59, 231-243.
Lunar
mineralogy:
61, 1059-1116.
detective
A heavenly
detective
T, oqor:
_iiftler
D et
al. (1980)
of lunar
Higblaml,
highland
s Crust
Pergamon,
New
'l;aylor
in
_fil:
Hydrogen,
1.. A
samples.
Taylor
and
._Jace
Taylor
Dating
Tokyo.
L. A. and
Odor
mart"
_1, 143-152.
I.. A., Williams
to lunar
and
nomenclature
and
and
Aerospaee/A_;E,
_flar-wind
Proc
components
._/_'e
_),
68-77.
in thc Fe-Ti-O
a.s,semblages.
(M.
and
of ESR studies
Ikeya
and
on lunar
T Miki,
beneficiation
ctts. ),
of highland
gla_s.s_, components.
P_w.
Albuquerque.
McCallister
#2trth
._t_we:
,4 t_*st-Al_dlo
other
Magnetic
mineral,
Lumtr
Planetary
Institute, Houston.
481 pp.
Wilhclms
D. E. (1984)
Mtxm. In The
A re,dew
I)osimeto,
Rt_:ks,
R J., and
ulv(}spincl
mineral
aml
S. R. (1975)
R H (1972)
Stability
relations
swstcm
and application
Planet.
StY. Leg2., 16, 282-288.
of the_-
for
a lunar
base
377
l._eu,.
Perganlon,
New
M_rk. 372 pp.
Taylor
predictions.
(198(0
R. R (19_})
_ils:
Taylor
S. K
(1982)
(M. H. Carr,
_'illiams
E.-H.
Ionics,
of ilmenite
data
Cirlin
In /_'R
high-'H
and
report,
t_roc. Conf
l, um_r
B. Merrill.
eds.),
pp. S1-70.
Albuquerque.
and
pp. 19-38.
helium,
Abundances
Acrospace/A_]E,
Taylor
clas,sification
York
I.. A. (1990)
lunar
Recommended
roclcs--A
committee
(J. J. Papike
and R.
Materials
R
cd.),
J.
experimental
._t_ce
Lunar
Williams
Planeta
Actir_ties
pp.
(1985)
test
bencficiation
l(X_-205.
OxTgen
of an ilmenite
of ttx, 21st
and Planetary'
R. J., McKay
O, ,_kgence:
A I.unar
('_doRl'
ores.
of
the
Lunar
Terrestrial
and
Planets
NASA 5P-469.
extraction
from
reduction
prt_.'css.
lunar
Bunch
In ,_M._I SP_28,
T
materials:
In Lunar
Cenm O, (W. W. Mendcll.
Institute,
Houston.
I). S., Giles D., and
of lunar
Perspecti,_,.
Bases
An
aml
ed ), pp. 551-558.
E. (1979)
pp. 275-288.
Mining
and