Analysis of lunar soil samples returned by Apollo 12 fligh

Mason, B.

English

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Produced by the NASA Center for Aerospace Information (CASI) 
https://ntrs.nasa.gov/search.jsp?R=19710008086 2020-03-12T00:22:17+00:00Z
fFinul Report, Contract NAS 9-8016
Principal Xuves tigator:
	 11rian Mason
Address:	 Dept. of Mineral Sciences
Smithsonian Institution
Washington, D. Ce 20560
Telephone:	 202-381-5314
• No. of pages:	 12
No. of tables:	 3
No. of figures:	 l
a Abbrevi4tions and symbols:
ppm	 parts per million
	 Fa mole per cent Fe2Sio4
min	 millimeter
	 ^	 Wo	 " "	 CasiO3
cm	 centimeter	 En	 " o'	 M8Sio3
8	 gram	 Fe	 of fo	 FeSio3
D	 specific gravity
	 An	 'o 10	 CaAI Si220
^Wv --;	 --*•--^-----	 Ab	 so
''``
a	 NaAlSi 0 8
8
Or	 n of	 KA1Si 0
Cn	 /0 ff	 BaAl Si 02	 2 $.rn a^ r
• Key words: .
k Apollo 12	 Pi.geonite
'Mineralogy	 Augite
Petrography	 Hedenbergite
Chemical analyses ' 	 Pyroxferroit•e
Water-soluble cations
	 Fayali.te-
' Cranophyre •
	Quartz
Feldspar	 Ilmenite
• .Plagioclase
	 Nickel-iron
• Sanidtine	 Zircon
Olivine
	 ' Apatite,
Pyroxone	 Whit:lockite
^-^ ►'+^ir+`;•;^^,;^• (ACCESS'	 UMBER)
Gr
} p	 (p	 ) (CODE)	 1
.•	 • . 	 •
_
a (NASA CR OR tMX OR AD NUMBER) (CATEGORY)
,
..r
0	 Nvo, O )i	
t	 ,^
Ajilwi-.alogy a1ld pot:a:o i;raphy of Sol)ch A; c%J,l.c) 12
Dr-ioll 1'tasorly 14, G. INQ-1-soil, Ia. P. 1' wacicr.,,,Oal 13. .1 17: CISC,l^ j.Glly aild J. ttiel vil,
1; ► 	 5oll j.slll Llst j .t• ut j.olty 1>ashirlgt:rri, D. C. 20` 60
iiIM! 1.0-5 o f the Apollo 12 f:i.iv1 s co;lt:aill :(:.Isa r. -ilents.
 ol: r,.•^l;;t ?1.^:1110
rcckv- and b i:occj.as, m ti-A- l graj.r.-; y ra y . d ^Aa.sr,y par tic lC .s. 1111)C!
mlvioral. f,a:al.i s a
.
re 11!%.1I.)Ay	 (pj•fic=or	 and augit c) and
o:Lj.vj.tcc:, ta:;. Ia 1a^:inc,^. alxolmt^; of p1ri-gi.ocla.ie i n.cl a.11:ic:nJ.t c, and a:^:re
:ilet:al f;ra ns. The cUi p.,):>j.L^Cl s of the rjit*."-J. f;;7."ains j.l. li-cat'c: thai:
fioUIC! are. of IrCt eo'!; j.t iC vri.c,, In and s?ome are dcr j.VC;d from 1.U7'111r '1:oC'jc:i..
A single pyroxone crystal has a pig,., nni to corn, rin augi.te inch le,
and a ].ifa of . E:3 roiiedc:]'t.b(:,rgi e, with a 7.1ar ov, zone of
along a central fissure.. One rack fl:agivc-ntr from a sample of coa rse
fines (12032) is a si..i.i.c.a-rich 'hcdenbe-;°g .tc granophyre, consisting
of sonidi.nc. (50%),, quartz (30%), hedevibergite (10"/0), plagioclase (1%),
fa.yal itc (37.), and accessory apatite, whit Io,-kit-e, and zircon. A
complete chemical analysis of 12001 fines has been made, 'and also
a cleterlaj.nat .on of the: water-soluble cations, a noteworthy feature
being the presence of 103 pp ►n water•-solu7ble calcium.
We received the. fol.l.owi)v, samples ftom the Apollo 12 Collections:,
Tines (-I . 1mn) : 12001 (3.0 r,); 12003• (0.5 g) ; 1263.3 (0.5
12042 (0.5 S); 12057 (2.0 g) ; 12.070 •(2.0 ^)
	 .
Coarse fines: (1 nun - 1 cm): 12032 (0.5 g)
Rock sections: 12009, 12012, 12045 0 12051
Each si-simple, of the fiva s' vas siavod throu^;lt 60 mesh (0.250 mm
opening) and 200 iresh (0.074 uan opoping) si.aves. The grain-size,
dist,ributipii was si milar in all, tlio wt ialit: proportions being: •5.60
mesh, 10•-20%a; , 60-200 weish, 20 ­3a.; ­200  mesh, 50-60%,. The fines
eont^iliaed f°r:agra;., gilts of ergs t xl.l. Lne roc kv, and bx-ecclas, mineral -Val is,
and glassy particles. The c*oarser .gxactions were dr:.- a,Lty-s(,,p rated,
using methylene, Iodide (A = 3.32). The fraction w3,L•h D > 3.32 com-
prised about 30%,, and cortslsted almo -;t entt.xely of grams of pyroxene
E
	
	 (major), olivine (minor) , and opcaque r►d.n.erals (small auzouat) . The
fraction with D < 3.32 (about 70%) caizsisted of rock. and breccia
fraginents, glass spherulas and framnents, and feldspar grains, 	 j
The -200 mesh fraction-of 12001 was further separated with a 	 ^'I
""	 ( opening), 
	
p	
_
^	 325 lr.^ah sieve 0. 04 M mm	 and a onion of the -325 mesh
fraction analysed. The results are given in Table 1, along with
two analyses of Apollo 11 fines. The compositions of the Apollo 12
and the Apollo 11 fines are rather similar, except that the Apollo 12
fines contain about half as much titanium as the Apollo 11 ruaterial;
this has already been noted in earlier reports (L§PET, 1970). Our
analyses also shore distinctly higher potassium and cbromi.tun`in
Apollo 12 fines. Since microscopic examination-showed minute
particles of metallic ' iron in the glassy fraction of the fines, we
attempted to determine this in the Apollo 12 fines (by dissoluttOn 	 .
in K+CuCl3 solution). The figure obtained, 0.33% Fe, is certainly
N.	 wi	 kt	 h	 tom+	 1	 {'s	 Gs	 t"^	 rp	 t4k	 pFF
UP0	 W
tees
C.
t . r
4
t.+
i
M '
tat
.
«►
W
''
W
to	 '^"`
h+ Q w t C7 Ca C s tat ^?	 ^^
4. till
N
1 •Oat V W
w
co %D V r W
1-'
a W .,1 t M
to
ta.
a t" t1	 p..
1^
aQa•
^^	 1 1 p 1",, h.r C>	 t M .t:► W QCs Vl W ON ON3 d-^C^ t?'
At W l,? •.^1 V1 q V Vt 11^ h7 +SJ
O:i W
w M
tiq
•
w
^	 ^ ^ Q C5 t;? 4 C5	 t3 C^ Q ^ y ^ Ln ^'` L Q«^ C^,^ ffi,^	 u^!!..,.
•
G7
• •	 i } W C^	 ►-' h^ ,^ti' VI 0% %0 ^l`' CrJ i3 C^	 [ ^ N th
%A y N W W C'7 (?a ^	 V ^!? C/a t7r W Fa W W b0 ^ •t` fD	 f^
1 P
` trot
He
In rt
-
W
t­ W W t ►2 O41
0.
In to	 vti v o u+ ° `° v' ¢ 4_4
'
W
e ,
^
1	 ^ © N O^ Q ^ Q- W ^,1 W C^ 'f
cn w N tv `° 4a ^-^ Vta °. ' eh ,
u
c5 e :	 ^a, Cr ^ MN "0", r lel o ,
i 5 •	 ^
,^ #	 ;	 .,	
' ..	 i .	 _	 r ..	 art  • ^. ^	
-^
_
r
''^
tx
Ma N oll « 4 "
11 llli.Ililnum vaal,tv. , sina•e the proc:c durc: voul e, C ►l ly di say of ve thosac mat:tal
pta^., l• e l et) C• : Por-od oil t. 1 Vler f.aco of t h.t 1" 1 ' :^ ^ ^`.'?t; a.:C'.11t;:*, "Ind xac^C those.► C;
totally om:losnd. 'liar: hiZ h f1uTr;m ati on cr,f Cho analyO.s of the Apollo 12
fines probably result :s f om tlaci ropoi• r:tng, of soma matall.ic iron as,
VeO1 amid po.,!; :;Ibl.y
	
t rivalcat. titanium :s V.020
1
The caki ll,axted mincra1l cowposit,i.ons (iaok•m3) o2 Ohs;;;a anal.y::c•s
Mimi aabo-vt 40% fei].clspar of aaa ort~li t;ic ccmtpo.,;i.tim uald About 45%
py^.•c..r:^c:. 	 '^:}lc	 ^^tt:,t7s;.t:^.Ulisi	 naafi	 f.li.^,1,t;7.y	 u:'adta^"stxi:ur..^ted	 i.la	 S3,()2,
' gi.v3ra	 :;ln;all. t1i,?ntlilt:	 of olivine.	 '^}lC Apollo 12 Mier, contain  the
"Y
w
egmivaal.entr• of about 5% i.Ira:arii.t o, co mpR1rad to about I W' in the Apollo 11
material.	 Aft or subt:):acting the i.11t12nitc f	 the PCO/ '(:U 'i'^ 0 na:•l;:c t.a,ta^
NG^.'CC:ftt:a c i,s xC:i«1a^ ;. ^^? .y sl,rn3.l r;a; in all thic sc aazaaly,camr;	 (42 for the
Apollo 1-9, 41 and 43 for the Apollo I.I. analyses) .
Vle also dat:erminod the water- extri) ct&tile cations in both Apz it o 11
and Apollo 12 f inns..	 A control 	 :,ampar: Yi.4,ldc_d' Iovs .
'
than 1 ppm of thr cot~.i.ons determined. 	 A sampla of the Al e-nde mct-tc>orlt:e
• was extracted for comparison.
	
The results are as follows (in ppi a)
N,	 I	 M	 Cry	 Fe	 Ni
12001	 14	 < 5	 31'	 143	 .4 5,	 .t 5
10084
	 21	 •C 5	 16	 325	 < 5	 45
Allende	 238 `	 ' < 5	 `25	 20	 45	 '45 {
The notable feature is the comparatively high amount of extra:ctahle
calcium, considerably less, howaKvex, in 12001 than in 10084.	 The
extractable cations are not present in the fines as halides, since
•
Reed and Jovanovic (1970)- report less than 2 ppm. water •-s ol.ubl a halogens
in 10084.	 The high surface. area and rt'actvty of the fresh lunar
.' glass may Ice respoftiible..' The water-extractable calcium perhaps
,
F
~
t416—.. ^,rgr r:Oes *^V ♦ qr .+1`^.y.s' y-.. •^V'N e+ ; .e +.	 • -.....qf....,^.	 .'4.4re ,.
t !
Mason - 5
explaitics they
 ropc3k• ual ro ntttlatittt;t f.fect; of. lumar (lui;t on plvi L
gro%W) .
f
ZIti.a:try 8rai.n s of olivine in Oic, Apollo 12 fintos were ru;tl.^•c;c:cl
with the microprobe. Vie ronte in composition, in mole per cent
Ve2Sio4 (Va), is 
ra'26-609 with tto markod composi,t:JonnI proxir^ronce;
the r. t:: tois F 41' Tai nor CIc.:OCnts detceted %lith tl)a mi.c:roproba ware
Ca (avitraL!p 0., 2t.%) , Mn (0.24%) )
 Cr (0.147,) and Ti (0.04%) . Tho
cont-ont:s of calcivrn and cha,owitt,vt are notably hi, lh for uli.vines ill
mate'Drit I.0 o1j"vines3 which we bave maasurc.d Ca is vc:ual.l,yr 0,01-0.02%1,
and Cr 0.02-0.04%. This probably refl.et f ts a high to-,:z1jarat"ure of
crystallization for the lu:car of ivina, and rapid chilling prevont:tng
rendjiistmc-ni: at lower t:empera,t~uores.
Some. sixty pyfroxenr graiaa in the Apollo 1.2 fines were also analysed.
They shoed two compositional clusters, on for pigeonito and the other
for au8i.te-• sabcaleia aaei.te. The mean composition of the pij;eoni.te
cluster i s Wo 1 n l"s, , , of the au0i,i:c^•- stcbca.lci.c au -I to cluster
VoEn Fs	 The principal minorr. elements are aluminum And twi.tani to33 li0 27
:.x The pigeonite grains average 1.4% Al 03 and 0.9% T^ .02 , the auSitie and
Ta i.	 •	 suhcalci a auSite 2.3/. Al203 And 1.37. Ti02.
The range
 
of compositions shown by the isolated pyroxene grains
are essentially duplicated in a single pyroxene crystal fragment
•	 picked from 12057. This crystal fragment, 1.1 nom by 0.7 mm, liar
a central core of pigeonite of rather uniform composition (too Fn >s )10 57 32
with a mantle-of subcalcic augite ('Wo 3`7 37 26)2En Fs 	and on one edge. a
narrow rim of ferroheder.'bergite (Wo30En7Fs63) * A narrow rift in the
° Y
	
	 central cure is lined with a thin zone; of pyroxferroi.te. The
individual minerals are clearly di.sti,nSuished in crossed polars by
the increase in birefri,gence in Passing fxom pyroxferrofte to
•
pi.geoni.t:o to ttterit a to	 con►pon—Wonlal
t	 ,
variation taro...; trlti.-; trc,in is u ven i.tK S`i-, ^I 1-ii tut i.w of t•lic
pyroxene Ilan' mothers.	 A similar.' pyt•`o:;onc c-vY:;Ln l from Apollo 12
material, ha.., brett dancri.l ad by Dena: ot ,
 al..	 (1.970) .
Plagi,oclsase grains from Mo. Apollo 1.2 f i.ru;s show a vlupp of
composition from At'82 tc, 1'^X96t with a Irsavty of A1190 0 Thcs
coatai.ns datect«iblc► irvi (avera-r-a 0,40% roo), poluva-i; tim (average
0. l°I. X 0) , and ti.t::an;i un (raveraj,,c 0.08% TW
Several nu:tal-r•i•rlt psrt:,i.r.l.c wcro. entt;acted from the Apollo 12
fines by m--saris of a haiid ma-ijot. Ille tot ,-.1 ancaullt in ary Sample is
I	 small, voking, up rnnch lass t~hati 1%. Two typos of n:?t.al wevo
dist:irsgu:tslv., ; 0%ne type is i inal.y gj:ar . l.ar and shows! defontiatfion
structures, the otbor•
 is coarse-grained and undeform, .d. Microprobe
analyses of the def.•o,:wed ft:ains give f• igu efy for. xtichal• and cobalt
comparable %,:It h those► for n1etQoj,*13.LJ,C n,icltel-iron, suggesti,xig that
t:hctre grains-, lit:ve baer darived from mrit~eori.t a Inpact : on the lunar
surface. Vie coaxs'e»grai.ned utUlcfcAMed 1a.1.t4 usually has lower
nickel concentrations than mat eor iti.c nickal-:i.ron, and sometimes
more cobalt than a al--ol; these fragptents are presumably indigenous
to the 1+10011, Probably formed by; localized reduction of basaltic
e
m terial. One such fragment is essentially petu Iron,, with no detectable
•
amounts of other elegy ants; It is extremely soft, comparable with	 j
w have be ± 'able to obtain. This metale	  enr	 the purest strain-free.. iron	 h
fragment contains inclusions of ol.ivine^ and ilmenit:e similar to
.	 ,
these minerals in the lunar basal,t:s, from which it was presumably
• derived.
i
4k °,^.{.^^k.x,•..a.Aws«m...e._ .^w.+a,^_we'4 m..t -. -.
	
» ..^,,T . ... t. .:.as,.
	 ..
i	 • i
F
Mason « 7
9s:
'	 Our 0.5 g sa ►.,pl a cif coax ne fines (12032, from thr. rim of
Bunch Crater) Was washed w1th nectona to remove dust, nud theil
Y
density-fraetimil ted in nwit:hylone iod 140- a0v toile Mixtures. 	 Tile
dc-nait.y frr'1tr%^ jons waves hiitlt7-sort etd u tader a binoCt la.-- ClLc:roscopo
,
into braccia frragni,e mts and crysLall iue rock fraBmants.	 The results
aro set out in 'table 2.	 ',ilia avaraae weight: of individual fray ,ants };
' J.s 3..5 vii, and tha percent rps of ar.C:ocia and cryst all inp: racks -Are
82  and 18 respectively.
Several erysLal.lina rock f +..ovnenits warro seloated for detv—!Ied
ex: inina,tion.
	
The raost remarl-Ale one was a lone Aiite fraa,-',Cn,t ill
. the D < 2.70 fraction, i4hieh otherwise c:onsIst• ed of hiAhlY
vesic ir1r 1.at d black f. r aVeia J.racp. ones.	 This crys. ` t41. l>I ins f r,,gtra:ln tws .
3 im long	 to consist,* largely ok sc,nidino, ult,-h i itoz avouut:s;prov0d
of quartz, plaaiuclaso 	 fayalit:e, and	 ar;d 4=L-Story ;L
zircon, apatite., and this lockitMa.	 The c6mpvsitiott of the iwdividutitl  'I
minerals, dat;ermint ed by the ml croprobo, is given .im Table 3, along
II
with the calculated bulk composition.
A
r
i
it
A.!
I
Mason "' B
Tabre.. 2 Fractionation of 0.5
€t coarse fines Krom the rim of
Rench Crater (12052, 46) .
Numbor of fragments
• Density [Weight per cent.	 breeci.0	 Crystalline rocks
2.70 8 11	 1
t
2.70-2.90 33 43	 3
2.103.10 44 58	 6
3.:10-3.32 '12 5	 12	 a
3.32 3 4
Totals 100 117	 26
I
li
3
•
e
Mm
Table 3.	 Analysex (mica-apa.o3^e) of infito.ral . fs in hcdoubc:5rrite
gratiophyre (12032, 46-2)
1	 2	 3 4 5 6
SO)2	 65.4	 57.0	 19.7 (diff.) 48.8 29.8 72.0
TiO2 	 N	 - 0.75 0.7.1. 0.1
Al203 	1€3.6	 2608	 0.20 o.41 0.04 11.1
Cr203 	..	 w	 w 0.06 0.13 w
1'00	 0.82	 1110	 n.d. 28.0 67.8 513
M110	 n.ct*	 no el.	 n.d,' 0039 0095 0.1
t1g0	 nod*	 11.d.	 nod. 1.55 1.22 0.2
Gao
	
0.31
	 8.74	 nod. 19.3 0467 2.7
NS 2b	 2.96	 6«85	 n.d. 0.10 nod. 2.1
K10	 11.6	 0115 5.8
^ra	 nod,	 nod,	 - -
Da0
	
i	 1121	 nod.	 ~ " 016
10009
	
100.6	 (130.0) 99.4 100.8 10000
n.d,	 not detected (.4 0105/¢)
1.	 Sanidine (or 69Ab28 n2lln1 	 507.
2	 Plagioclase feldspar (Ab,SM4j0rl) f 7%
3.	 quartz; 3010
4.	 liedenbexgite' (Wo45En5Fs5U)
5.	 Fayalite (Fa95)	 3`/1
6.	 Bulk composition (calculated)
is	
...	 .
t
Y	
...
. . .°^'^`^	 ^^;^^^^'Yfl^^ilR 6 ai$MwN.•vi «tlr:£^'ar' . f . ..' .#fi+^ ♦
ply . 4	 ^ t
f3
111a bedvf• ber:glue vnc foyal fi.t.e are t'r^ ';k^:i11: ou ph t^t^vvty.;tr., up try l- rr.t
long , in a fine-rr awed grounclmati of hu:crLz and foldrt>ar, umucli of it in
vi.crogrnpbia inL rgrovy t.h. The perec-ntngns of r3ar idi'me	 qutirt+r i ci
this nt,^rf;ro nh are P.ppro%iira tel y 65 : 35, a c ompos 3.t1 cain close. to Lhe
f
temporat:ure rtl,rrimiwc on Ov'-- liqu dus in the system KAISI308 M hnAl S PS
Sio2 . The rock it; comparable to 	 t errost.rial. gravoriiyrr.s, specr.ffcylly,
the
	
grn11(1pI1Yrc=s of the Skai rgnuird ijitrusion. pir(- of t:lic n
(W 3021) hays cssentially identical minornl o n y=, consist' l!) of lac c?:;r^4^er^;f to
(WO 44l n6Ts50 	 fay4!1.3, c. (Va 95) f plagioclase (P,1)40) potra"11 fel dil ;pzlr " P-11d
vi qua?.-trr and .Ktr idynti te. Toindsl.ay at al.. (1969) estl,vat o ► r,.iPporat;ur or, of
ow 980 C fund nn oxyucln fugacit •^ y ranging from 1.0 ^+ 1` x '0 to lU~13.G50 	 atm
for the crystal.lizat;t.on of the Sacac:r f ar^rd rock, and tbns. r,^ ^1c,J^ros- should
be equally applicable to thc. lufiar granophyre.
The	 nr.f nor alogica%, ti d textu5-.0 fout:ire: cif. this ro!.k
strongly nui est that it represent.,-, the last liquid d:t.1 emntiat e y rom
the fractional. 'crystallizationi nation of a large body of lunar basaltic nA&vaa
(or: possibly an initial product: of partial melting). Its composition
is similar to that of the h3.;gli- s l ica Blassy mesost avv is of many of the
Apollo 11 igneous rocks, described by Roedder and Weiblen (1970)0 it
is also comparable with the l.igilt —colored, silica-rich parts of the
unique rock 12013. Whether it was formed at or near the l.ocal,e of the
Apollo 12
.
 landing, or whether it is an exotic fragment:, -possibly fr oau
a Copernicus ray, remains an open question.
4cs
F"
t?e^n:rer^c^► ^
Bencat A *
 E., J. J. Pulpikeo and C. T. Vrow,i,tt, Apollo 12 clinopyroxonjes:
chemical, trends. Lart-h P1,1tu k Sci.. T.c.,ut ers, 8, s' t, 1970.
Liwlsluy, D. It., G. It. Brown, and x. • U. M!xir, Cond i.ti.'na of the
r: I'C^;:^1 . 1ti^lr+ t;nt i.t.e- :r+^uEie c^nxbert, G+ inversiou in kite
Skao1 tlard ;t:i'1tY,'tt; iou, J?:tstr O'reen and.	 I"1i.1'-	 1l#•	 {I4'•
	 '-»2• «,i ^ C' <:•Y.- - ......	 ....
Pad► r 2, 193, 1969.
LsrrT (Lmiar Sample I?vellmi,niary E%hart1.iiat .oa Tt.am), 1?rel-Litibiary c-xamination
of lmma.r samples l:i.•om Arol l o 12o 	{,c^^^c;c.'., . 1,067, 1325, 1.970.
RnoJ2
 G. Wt. ud S. .jovat,,r),vich) °f3^lo 4 ens, v-n- :cu ►;y, l ithl,utz and osmium
in Apollo 11 94wil-Ins. { eoohim. Cq :-r,.% Mm. A",ta, St, l , 1, 1487.,YM#• . Nr•wrr^	 rN Y .Fn FI ..Fl.""^H	 ^^ ♦Y+Y+Y.!ti	 11M•A	 Y
1970.
Rocddar., 1",. P
 
and P. W. F10.1b ". 11 0
 J4t.nar pr-t.x• o1ca;;Y u^ ^► ^•1.^,^^^^;e melt:
111cluslon , Apollo 11 rocl,,s. Ceoclib'A,	 'Ant.'1 ^ m^	 1. j11.. I
801 1
 1970.
• i
low &Az
♦ ^'	 w
^. ^	 ^ ^
N a •,.a N ^
Ot 41
d 1. • u1 N ^ Ci,
C6
^"'
to 0
► 	 0 41r RO
' 4).,.000*9. O
G A
♦
.d
Lo
so
.. O	 0 Q•
04 •r4 to 14
•
r4 R^
♦14 a a0%.0
" o	 44
u
d1 W	 •^^	 ; . ^ r . +'t.1.
to
co
IS
93	 .14
NQ!a00.
•• _ 0
4j a
ice! td
•O 'r^1 rt 'Od
•	 •
•^•
•	 Q.
N 0 0 O
010 41 f•+
I. 	 N N
•
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Mineralogy and petrography of some Apollo 12 samples Final report

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