Mineralogy inferred from the Viking X-ray fluorescence spectrometry (XRFS) is compared with mineralogy indicated by spectral data. The comparison is done by taking laboratory spectra of Viking analog minerals. Both XRFS and infrared data are consistent with clays as the dominant SiO2 containing minerals on Mars. The X-ray fluorescence data might also be consistent with the dominance of certain mafic SiO2 igneous minerals, but the spectral data are probably inconsistent with such materials. Sulfates, inferred by XRFS, are consistent with the spectral data. Inferences following Mariner 9 that high-SiO2 minerals were important on Mars may have been biased by the presence of sulfates. Calcium carbonate, in the quantities indirectly suggested by XRFS are inconsistent with the spectral data, but smaller quantities of CaCO3 are consistent, as are large quantities of other carbonates

Sagan, C.

Toon, O. B.

English

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Produced by the NASA Center for Aerospace Information (CASI) 
https://ntrs.nasa.gov/search.jsp?R=19790003814 2020-03-22T02:16:31+00:00Z
t
S^eptember 1978
J
N79-11985	 it'(NA c'A	 -	 92--	 INF 	 RnSC, Y OF
SIMULATED MARTIAN SURFACE MATLE+IALS
Final Repott, 1 Sep. 1977 - 30 May 1978
(Cornell Univ., Ithaca, N. Y.)	 10 p ITC
A02/MF A01	 CSCL 03E G3/91
zinc Ias
36955
CORNELL UNIVERSITY
Center for Radiophysics and Space Research
ITHACA, W. Y.
FILIAL REPORT
I'
Infrared Spectroscopy of Simulate=d
.Martian Surface Materials
NASA Ames Grant No. NSG-2277
9/1/77 to 5/30/78
Cwen B. Toon/Carl Sagan
^^^p^112131q js>^
1	 ^^h uniar^ r^s rsr  ,
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Own B. Toon
Carl Sagan (!'rint • 111al Ittvent igator)
Laborr► tor y lot Planctar y titutlit's
Corno l l I'n lvt • rs i t v
Illu ►ra. Nt-w fork	 14853
Inlraitcd s live trorsrol+v of SinittIatotl
Martian Sur tavo ".aerials
I'in.t l Itoport rover in 1 ,  flit , lit-riot) 1 11 11177 to 5/3(1/78
^r
it
NASA :\Du gs Ctr ml No. NS(,-'''77
	
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X-ray fluorescence spectrometry (\KFS) by Vikin t; ham determit.A many of
the major elemcutm composing; the surface materials on Mars, but .toes not directly
specify the mineralogy of the Martian surface, although it may allow mincralog;y
to be inferred. Many minerals have characteristic spectral features in the it
(5 to 50 um). ,Analyses of M.trincr 9 it transmission spectra of dust in the
great 1971 Martian dust storm arc informative ;shout mineralogv. here we comp.tre
mineralogy inferred from the Viking XKFS with mineralogy indicated by spectral
dat.l. The comparison is done by taking laboratory spectra of Viking analog min-
orals. W  find XKFS and it data arc consistent with clays as the uominant Sio,,-
containing; minerals on Marrs.	 I'he X-rvy fluorescence data might .1180 be consis-
tent with the dominattre of curtain mat is SiO,, igneo"S minerals, but the spectral
dat.t are probably inconslsternt with Stich materials. 	 Sultates, interred by \l.l`•,
are consistent with the spectral data; indeed inferences following; Mariner 9
that high-Sio., minerals were important on Mars may have been biased by the
presollee of sulfates.
	
Calcium carbonate, in the quantities indirectly sug;g;estc,l
b y XR S (-u TZ), are inconsistent with the spectral data. but smaller quantities 	 it
of CaCO 3 are consistent, as are largo quantities of other carbonantes.	 I'
	
t	 i
.	 r-
.a
j
Resu lts
'1'hc' 1' il.ln t, X- ray t I tit s rt'Nt • t`tlt't` (XRF,) t rant tl i rt't't Iv nl. l awu['t'd t ht` t' It'n1t'nt .t l
t0111positikill
	 I t 	 Iwt+ sItvs .111 tllr +I.I1'ttall :curt art`.
	 '1',111t-	 I	 llrt'st'ntS tIl.' t'It'n10'ntal
.t 1 1111.t 1 :lit it'll,	 t 1 Xl1t ' t 1 SHt 1 t1 its is -Ades,
	 ( UI' tllrt't , sa till +It':.	 I 	 (lit- V ihillp;	 I	 I and vr lilt.`
I,S1, tit, 9.1) 0 trt' 0111' rulIIII , I ' (U1) at	 tllt' Vil.iu l; 2 tantlt l t al(s` ('1't+ulnllu t' t .Il.t
1 1)77; IlaIr.l tat .tl., 1`117) antl 1t 1r twt+ MaI- t Ian .tit. II ogs W4  - Ilt.tIrd v
	 .II..
1'171; Toll l tit ltt ^1 L al..	 1 1) 7 7) .mil It.' - (Itaird 1 l r Nil tt' t't111l1nulicat I kill) . Ta1,1t 	 1
slit + wt ;	 t hat	 t IIt' t' I t'lllI'II It .11	 . • 01111 4 1 :; it I t I tlS 01	 it l l	 l ht' :t.1111111 t':; ,I t	 la1 t 11	 1,111,1 t li t '.	 t t t':;
tits	 ;i Ill I iIF .I:; A1 , t, Illy t`lt'llIt'IIt.II 00111po..;It Ikill	 .'1	 tI10 twt l tt'rr& I Nll- I.II	 .111aItie's
o04 	 and it 	 t ►nt' tit' t ht' groat ativ.Itlt at,.` : Ot \RFS 1110;k rirt'111t • fl( :; I:; t 110' I I	 :t'n:: t -
tivIty t 	 ill t lit, U t'It'11u'nlal 4`0111P011t'nt!; :;11 ''11 114 1'I, V., t'l, M t `,. t'a. 1101wt`vrt. as 0'.011
l 't. :;t`.t'n b y t v oid' lrinp, flit` ill I lit , I'.IIt1+ •,v 0 1 1	 analtl t-, It: and o04 
	 itt	 I'a1 1 1t	 l	 It	 Is not
0:1Sv tI' kit , F Ivt l list-I %I	 tnin.`r.l it + ,;icaI	 IitI oI -utat It+ll I rtlnl t ho \KFS 01.0'.1. 	 I'll0't'.`t t lrt'.
ll	 i:: nt't't 1 Ss.,kr y t.1 , ;t11 1 1 1 10'ult-11t	 XRI'S tl.It,t wItII . 1 tIIt'1	 1 , 10005 tit	 lilloi1u.It ioil
	
' 1 110' valu.lhlt', ml It' ralt+ t;lt'all y soll::it Ivt'.
	
1nttlrulat it'll m'ut't' ' ' I:; tllt' I lit rart`tl
tltt'.L•;ill ,'Illt'IlI
	
ll!:Itlt' .1111 ill', ,l
	 ^1.Irt 1.111 .111:;t
	 . ;t'+1'111	 (0''111 Mil  111or t) 1'v	 t ht'	 1111 l art'tl
I lit t'l'I t 1 1'0111t't r it' S 1) t't't rt'Kc t'l'v ( I K l ti) exl +t'1' IowIIt .	 Tit 0;it• ::1+t`t'l 1.1	 111111CAt t` Ntrtllll•,
tlu:;t
	 .tl l :tOI I't i.`Il 110'.'1	 10 tun ,111.1 : U 11111.	 FO I I OW 1110, l ht' MAI . 11101. tt I I 1 o.IIt .; scvt`r I I
lltv.`::tl t;ator	 :;t11,11o1 tht , I1%1S ,lu:;t
	 +1 1 t`.tra .ultl ,0111 ' Illdc.1 that	 tltr N.Irtlan
Ntll - tact . 111.111'l' I:1 I:; O'. 1 11 Itl he .III	 it;llt`OUS rOck wit 11 .111 510. 1 . • t'llt I'll I	 Ul	 (il ► t	 10.. o 
t'I,t y ,	 but	 tllt'	 , ,It l'l Ak , 0 t • tlll Iit	 110t	 t • t 1 1l1 .1 l it	 :;tllltit.11ll 
I 
a I
	
.Illlt ltlllt:;	 (^,	 Il l ..)	 of
t'.t It' 111111 CAI'lh l lt.It t'
	
01.111'' I
	
t't	 :11	 I tI	 ,	 111111t	 t't	 al.	 I 0 73,	 Ttn ln vt	 .11. ,	 1 0)77) .
M, t't l ntrast tlit , XKFS rostiIt	 ll'al , It , I, ,md km I III 
I 
it  t't al
-
. . Itli7) :;ut;tost suhstant i.11
tltl.ultitIt`:; tit t•at'11t11atos are 111'e;t'nt, t 1I.I1 1 h soII IS c0111110::t"I 1.11O;t`l y t i t t'lav
lit 11101.1l y tit	 1 1 .'111.11);, .1	 1t1w 
~ill	
I ►;11t'0lth Illatt`t 1.11,	 anti that t.ultAtt`:. at t` Llit',nit Ik%Ill(	 I
Illiut- r.lIS.
a
1
I
6
^j
1
i
1
	
t
I
	
1
_. ; —1
	rr--1 ms ►*; -'-7^' t-r----.^	
.idA^"^1
4
lit order to resolve some of thest' contradict. totls we obtained infrared
spectra of the Viking 82 and 11041 at.alogs and of each of their mineralogic
constituents. We used it Perkin Eimer 1121 spectron ►ctcr ,md suspended the analoi;s
and minerals as dust in t'sl pellets. Spectra are shown for the analogs and for
orbit 8 of the Mariner 9 spacecraft It- Figure I. Figure ': it lw trates spectra
Of the minerals contposinl; the It' :utalol:•
it is clear from Figure 1 that neither 6041 nor 112 is an acceptal l: allillo8
fur the orbit 8 emission spectrum. 	 I'he ll2 an.1 log Ilas two st rong; ha ads near 150.0
	
1 ^	 rm- I that are not found in the orbit 8 spectrum. The 6041 analog has onl y weak
i`
Ihands treat 1500 cm^ I +ut the shag+t of t lit , 1000 cm - I hand does not match we I I
with the observations.
,\n cxplan.it ion for the:;, , problem:; can be sovi ► in figure 2.	 Calcite I ►as ;t
-1
strong band at 1500 rill	 1110 l:tr);t' yuant ity of calcite (CACO 3 ) in 112 does not
,,cord with the observations. The second teature In 112 near 1500 cm -I is due
to II,,0 which is partly In the MgSo . ►nd partly in the clay s - iimitronite and
lit-it t kill lte.
	
Water ill clays and Ni1lt;lt('N is expected to he scasonahl y varying; on
Mars so the discrepancy is not s:'rious. 'rite 6041 anaIo), has two d I I ficult ivs.
Nont roil I to doer: not have i t r: I 000 cin - I hand we I l l ova t od to agree with the data
so tilt- larger yu.ult ity of noniron i to in 6041 than It-' y Ields :1 worse t i t for
	
i	 6041 near 1000 cm- I .	 Ill add i t ion 6041 1 ►as 1 ess MI,SO, thall 1 1	 l ti;. ' shows
MgSO4 hats it strong band at the edgO of e 1000 cm
-I 
stlicate hand, which ten.(::,
	
i. '	 to broadon the 1000 cn1
-I
 hand. 'Phis can also be seen by comparing It' and It2
minus MgsoN 
In Figure 1 with the orbit 8 data.
111:'se results imil1v that clay mill.•rals such as those In the B2 analoi; are
	
}	 consistent with the MIS observation::, htlt MOO, (or possibly outer sulfates)
Ni	 art, needed to yield a good t it with tic h h , h I reducncy side of the 1000 c;u-
hand. The hi i ji calcium earl+onate content ill 	 K2 mixture is not. consistent
r,
' 	
'^ 1
	 l	 1	 1	 ^	 I
1
'I
	
I
with t,b4t`rviltit+114.	 Pol-11.11's k i t 114 . 1 carbt,llatcs wt+tllit lit' % • kill:,ist•-III	 I . . wt,tlld It'44411'
tlu.rlll it it • 4 tit ,.I lc it t`.	 Add ln l; non t roll itit tt, I lit ixtitre st`vnw t 
	 make the I It t0
I lit' d.lt.l W01'40.
I'lle So4 ill (lit' Mart Lin sllrt.lrt` i:: Ill't,b.IhlV 1'1'4pt,tlsiblt' for tht • illct,rl-l't'I
c011Clu410114 1oIIowi11 i; M.11'lllt'r N p lat Illt` oust w.ls ItI k"llIy sll Icootis ::dive MiSO
t t 1 Iltl4 to I+rt,adt • n t hr 1000 cllt-1
 hand t o II i l;h 1 rt'(1ut'nt • 1rs as tit" 111 ) 1,111 v 4 I I I ct`t,t14
tit Inoral:;.	 I'ht • \RF'S data nli,',ht lit' tt+n4i4tt'nt Willi ?+111.'1' attalt l i;4 ct,nt,llnitir, very
I it t to Sit.1.,.
	 It a elms ltnl ikvIv t hit t thc4c would lit ,
 ct,rl:tl4t ell t with tlic Ihl::
d.1 ta,
 its, for t'ximil l Iv. nottt rim i t y kit I t , 4 Ilt + t sct'111 it i,t,t,d I it .11ld i t 11:14 .1 It+w
frrqucltt• v 1000 rill-I band is tit, basic 4iliratt • s.	 Ilt,wrvrl', Ilit • MP,titl, complicate
tilt' 1lrt,blcm .Ind makcs gtialit.lt ivr' .v+ull+act4t+ns 4uS1101 • 1 .
1'ht` rt`snit:: presented here can 11t' (urthcl' yuatttit icd b y rluulcrical calcula-
I i0ll4 01 C-111ISSIt,ll ::Ilct'1 1'.1 ll:;lilt', tllt' kill  ir.l1 t't + Il-,t. lIs of tlic InI lit ,
 I- ills (v.i;. 1't,t,ll
ct al., 1977).	 such wt,t1, is, ctit'notitly untierw:t y .	 Lac ant it- ip.ltI , that this, work
W i l I .111.it1I I fv t Ili' t"Wot 1111111,1. bt 1 t111d4 , bc( t i l l- ct,lL• : ldt • r t ilt- 4 igil it icallt • t' t i t Ml,titl
.11 l d 1+111	 I illllt4 on mil)"110t itr, t i tllt`r Lt,44tblt` :;ill l.11 t'>: and cal-11011ilt0.8.
Publ irat ions:
I'll, ,
 work ritrd will he stlbnlittt'd It,r pill'I scat it'll in 11w opt • n l iIoraturc.
1'hc work has bt , t'n rrpt,rtcd as
M.It t ian Stit'lact' l't,nll+t+::it I.t,n:	 Collil"it-ist,n , 1 1 	Ia'Intltt' "Ilt't • tr.tl Studics .111,1 Ill-
Situ X-Ral k, FItiorc:;crnce :lnalvs14, lt. R. 1'uun, B. N. Klmrc, J. I+. 1't,llack.
C. Sag.11l. Ninth I'I inctary lt't+It +i;V,	 I'I incil+.11	 ltlVI':;t i l ;att l l' tiy1111 1 t+::illill. 'i'lllson,
Arizona, 1978.
.\It abst ract 01 tilt' W011, has .11:;t , bt on 411bmi t t t`ti for 1 poster t.l i k .1t
	
I .
I he llc tol+t'r 1478 Div I ,, It'll k it P i met .It, .v S c i tnict-, Meet Ill% ,  IIt I is Atil , c I c4, ( ' .i I i I
r^
I
I	 ^
T----
; -
	
-
-% 701*^	
- - - ^r -
6
Baird, A. K., A..I. CaRtro, B.C. Clark, R. Toulmin III, 11. Rose, Jr., K. Keil,
and J.L. Gooding, 'Cite Viking X-ray flourescence experiment: Sampling
strategies and laboratory simulations, J. Geop hys.Res., 82, 4595, 1977.
Hanel, R., B. Conrath, W. Hovis, V. Kunde, P. Lowman, W. Maguire, J. Pearl,
J. Pirraglia, C. Prabhakara, B. Schlachman, G. Levin, P. Staat, and 1'.
Burke, Investigation of the Martian environment by infrared spectroscopy
on Mariner 9, Icarus, 17, 423, 1972.
Hunt, G.R., L.M. Logan, and J. Salisbury, Mars: Components of infrared spectra
and the composition of the dust cloud, Icarus, 18, 459, 1973.
Toon, O.B., J.R. Pollack and C. Sagan, Physical properties of the particles
composing the Martian dust storm of 1971-2, Icarus, 30, 663, 1977.
Toulmin III, P., A.K. Baird, B.C. Clark, K. Keil, H. Rose, Jr., R.P. Christain,
P.H. Evans, and W.C. Kelliher, Geochemical and mineralogical interpretation
of the inorganic chemical results, J. Geophys. Res., 82, 4625, 1977.
FiEIT Captions
Figure 1: An emission spectrum taken during orbit 8 of the Mariner 9 Spa,:e-
craft is compared with transmission spectra of B2, 6041 and B2 ►ninus
MgSO4 analogs.
Figure 2: A transmission spectrum of the B2 analog is compared with
the minerals composing the analog.
k
6041 B2
Nontronite 49.5 17.5
Bentonite 18.2 29.8
Kieserite 13,7 18.5
Quartz 7.5 14.4
Calcite 4.9 7.0
Hematite 2.5
---
Magnetite 2.4
Maghemi t e
---- 1J..1
Halite 0.8 0.8
Rutile
--- 1.0
F
OXIDE COMPOSITION OF MARTIAN SX
.TLES AND ANALOGS
S1 S2 S3 U1 6041
'T P2
S102 44.7 44.5 43.9 42.8 44.6 42.2
Al203 5.7
---- 5.5 ---- 5.5 5.9
Fe; !^ 18.2 18.0 18.7 20.3 18.6 17.0
+1g0 8.3
---- 8.6
---- 5.4 7.0
cao 5.6 5.3 5.6 5.0 6.0 5.7
K20 <	 0.3 <	 0.3 < 0.3 <	 0.3
.12 0.2
T102 0.9 0.9 0.9 1.0 0.8 1.1
S03 7.7 9.5 9.5 6.5 8.4 12.3
cl 0.'f o.8 0.9 0.6 0.5 0.5
MINERAL COMPOSITION OF MARTIAN ANALOGS
e
UKIGIN AL YAK =I% IS
OF p(N)ft ()I 1 A I .ITY
'1 J
ZO
.-,
cn
F
U)Z
1-
4.
ORBIT 6 EMISSION
	 "1,1.1Jill	 ^
t
Or' YlX►R 11 LAfY
^^	 l	 'r	 l	 I	 l	 p'
^^	 a
BENT(E
	 U	 1 Jv	 ^
i
B-2 ANALOG
SCALE FACTO 103
	
"	 2.500	 2.000	 1.500	 1 .000	 .500	 - . OCO4.000	 3.500	 3  ('!'^
41 iaj".


Infrared spectroscopy of simulated Martian surface materials

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