Apollo 11 Lunar Science Conference abstracts

167 Pages·2017·41.62 MB·English

by  Lunar Science Institute

NATIONAL AERONAUTICS AND
SPACE ADMINISTRATION
(cid:43)(cid:50)(cid:56)(cid:54)(cid:55)(cid:50)(cid:49)(cid:15)(cid:3)TEXAS
APOLLO 11
LUNAR SCIENCE CONFERENCE
ABSTRACTS

INDEX
Name Page No. Name Page No.
Abell, P, I. 1 Davis, R. 30
Adams, J. B. 2 Doell, R. R. 31
Agrell, S. 0, 3 Douglas, J. A. V. 32
Albee, A, L. 4 Duke, M. B. 33
Alley, C. O. 5 Edgington, J. A. 34
Alvarez, L. 6 Ehmann, W. D. 35
Anderson, A. 7 Engel, C. G. 36
Arrhenius, G. 8 Engelhardt, W .,v. 38
Baedecker, P. 9 Epstein, S. 39
Bailey, J. C. 10 Evans, H. T. 40
Barghoorn, E. 11 Fernandez-Maran, H. 41
Birkebak, R. C. 12 Fields, P, R. 43
Bochsler, P. 13 Fireman, E. L. 44
Brown, G. M. 14 Fleischer, R. L. 45
Burlingame, A. 15 Fox, S. W. 47
Cameron, E. N. 17 Fredriksson, K. 48
Carter, J. L. 19 Friedman, I. 49
Carter, N. L. 20 Frondel, C. 51
Chao, E. C. T. 21 Fryxell, R. 52
Cloud, P, 22 Gast, P. W. 53
Coegg, P. E. 24 Gay, P. 54
Collett, L. S. 25 Geake, J. E. 55
Compston, W. 26 Gold, T. 56
Castes, N. C. 27 Gales, G. G. 57
Crozaz, G. 28 Gopalan, K. 58
Dalrymple, G. 29 Greenman, N. N. 59
I N D EX (continued)
Name Page No. Name Page No.
---
Grossman. J. 60 Marti. K. 87
s.
Haggerty. 61 Mason, B. 88
Hargraves. R. 62 Maxwell. J.A. 89
Haskin, L.A. 63 Meinschein. W. G. 90
Helsley. C. E. 64 Moore, c. B. 91
Helz. A. 65 Morrison. G. H. 92
c.
Herzenberg. 66 Muir, A. H. 93
c.
Heymann. D. 67 Murphy. R. 94
Hintenberger. H. 69 Nagata. T. 95
Hodgson, G. W. 70 Nagy. B. 96
Hurley. P. 71 Nash, D. B. 98
Jedwab, J. 72 O'Hara. M. J. 99
Johnson. R. D. 73 O'Kelley. G. D. 101
Kanamori. H. 74 Onuma. N. 102
Kaplan, I. R. 75 Oro, J. 104
Keays, R. R. 76 Oyama, V. I. 105
o.
Keil. K. 77 Pepin. R. 106
King, E. A. 78 Perkins. R. W. 107
Kirsten. T. 79 Philpotts, J. A. 109
Kohman. T. P. 80 Ponnamperuma. c. 110
Kushiro. I. 81 Quaide, W. L. 112
v.
Larochelle, A. 82 Murthy, R. 113
Latham. G. 83 Simmons, G. 115
Lovering. J. F. 84 Ramdohr. P. 116
s.
McKay. D. 85 Reed, G. W. 117
s.
Manatt. L. 86 Reynolds. J. H. 118
INDEX (continued)
Name Page No. Name Page No.
Richardson, K. A. 119 Strangway, D.W. 144
Rho, J. H. 120 Tatsumoto, M. 146
Ringwood, A. E. 121 Taylor, R. 147
Roedder, E. 123 Tolansky, s. 149
Rose, H. J. 124 Turek ian, K. K. 150
Ross, M. 126 Turner, G. 151
Runcorn, S. K. 127 Walter, L. s. 152
Schaeffer, (cid:50). 128 Wanke, H. 154
Schmitt, R. A. 129 Wanless, R. K. 155
Schopf, J. w. 130 Warren, N. 156
Sclar, C. B. 131 Weeks, R. A. 157
Scoon, J. H. 132 Weill, D. F. 158
Shedlovsky, J. 133 Wiik, H. B. 159
Shoemaker, E. M. 134 Wood, J. A. 160
Short, N. M. 135
Silver, L. T. 136
Simmons, G. 115
Simpson, P. R. 137
Sippel, R. F. 138
Skinner, B. J. 139
Smales, A. A. 140
Stephens, D. R. 141
Stewart, D. B. 142

1
ORGANIC ANALYSIS OF THE RETURNED LUNAR SAMPLE
P. I. Abell, G. H. Draffan, G. Eglinton*, J. M. Hayes,
J. R. Maxwell, C. T. Pillinger
The Organic Geochemistry Unit, School of Chemistry,
The University; Bristol, England
ABSTRACT
The analysis scheme was designed to detect and identify carbon compounds over a
wide molecular weight range.
Mass spectrometry has been used to examine a sample of I unar fines for trapped
volatile constituents. A variety of small organic molecules, including methane
and other hydrocarbons, accompanied the rare gases when the sample was heated
in a stepwise fashion to 900°C under vacuum. In addition, specially designed
apparatus has been constructed to perform the classical geochemical procedures
of extraction, separation, deri vati sation, chromatography and mass spectrometry,
using the smallest possible volumes of solvent, and with a minimum exposure of
the sample to the atmosphere.
Stringent precautions were taken in the laboratory but contamination introduced
during the course of the Apollo 11 mission undoubtedly made a major contribution
to the observed organic content of the fines. The much cleaner samples and
complete procedural blanks expected for subsequent missions must be awaited
before the true nature and extent of indigenous lunar organic matter can be determined.
*Speaker
2
SPEC'ih.i1L F.EF1.1CTI VI'l.'I 01' APOLLO 11 LUNAR f,M.4PLE.S
John B. bctams1
Robert L. Jcnes2
Apollo J.l cry::;tb.lline rocks containing P.J'Tt)Xt:ne but
no ulivine show h 36% absorption bi:nd centered at 0.94 microns and
~:;_ 19~ b~nd at 1::.0 microns. Crystalline rock Bamples containing
pyroxene and minor olivine !:lave a 23% bend at 1.00 microns end E:
10% b1md at LO microns, the expected bt=.md frequenciec for mixtures
of these minerals. Surface fine::s t-..nd breccies have on.1y traces of
olivine, and the combina.tion bcmds occur at approximately 0.95
!llicrons ( 5%) and 2.0 microns 5%). Band shallovmess in the fines
end breccias is related to their J.ower integr&l reflectivity. All
:ufJjor bbnds are f).ssigned to Fe2+ in clinopyroxene tlnd olivine. Glass,
feld.:;par and opaques apparently do not contribute meHS'.ll'E,ble 8b::;orption
bands in diffuse reflected lie,ht. Bend frequencies are not sensitive
to exposure of sumples to N2 or air, or to m:lcrofractur:i.ng and partial
vitrific&tion. Band depths, ho;7ever, f..re diminished by the micro-
fracturing and vitrification. Curves for surface fines agree in de-
tail ~ith McCord's 0.4-l.l micron telescopic reflectivity curve for
an 16 km. spot tbat includes the Apollo 11 site. Results confirm
ea.rlier predictions of lunar surfhce mineralogy based on telescopic
curves and strongly support the feasibility of obtuining mlneralo-
gic;;J. infontation remotely, using telescopic rei'J.ectiv i ty data.
1 CuribteBJJ. Research Institute, St. Croix, Virgin Islands
2 ftllanned Spa.cecrnft Center, Houston, Texas
3
Observations on the mineralogy and composition
of some lunar samples from Tranquility .Bo.sf: ·
S.O. Agrell, I. Drummon~, J.V.P. Long, J.D.C. McConnell and I.D. Muir,
Department of Mineralogy and Petrology,
University of Cambridge;
England.
Electron-probe, optical and electron-microscope data are
presented for minerals and glasses from:
a) Igneous rocks - individually collected samples and the
'fine31 material from the bulk sample container.
b) Microbreccins and regolith material including glassy
spheres, clast3 of shocked and unshocked material and
composite fragments welded together by vesicular glass.
The dark colour of the latter may in part be due to
submicroscopic droplets of metallic iron and possibly
troilite di3po~ed in a complex flow pattern.
c) Fragcents cf meteoric origin.
The bulk co~rosition of the glassy spheres scatters around that of
the lunar basaltic igneou-s rocks, with extreme types having the composition
of almost pure plagioclase (.~n 95). Iron crystals at the margins of glassy
or crystaline spheres tend to be richer in nickel (7 - 17%) than those well
within the spheres, where the nickel value of the kamacitic iron (~3%)
approaches that associated \olith the troilite €<'1%) in lunar basaltic
rocks.
Preliminary studies by scanning electron microscopy have been made
on micro-impact craters and the surface of some of the glassy sphe~es.