SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES ? NUMBER 30
Field and Laboratory Investigations
of Antarctic Meteorites Collected
by United States Expeditions,
1985-1987
Ursula B. Marvin
and Glenn J. MacPherson
EDITORS
ISSUED
DEC 1 8 1992
SMITHSONIAN INSTITUTION
SMITHSONIAN INSTITUTION PRESS
Washington, D.C.
1992
ABSTRACT
Marvin, Ursula B., and Glenn J. MacPherson, editors. Field and Laboratory Investigations of
Antarctic Meteorites Collected by United States Expeditions, 1985-1987. Smithsonian
Contributions to the Earth Sciences, number 30, 116 pages, frontispiece, 38 figures, 9 tables,
1992.?This monograph describes the meteorite collecting activities of the United States
Antarctic Search for Meteorites (ANSMET) expeditions during the 1984-1985, 1985-1986,
and 1986-1987 field seasons. Descriptions and classifications are given of most specimens
collected during those expeditions with the exceptions of the types 4, 5, and 6 ordinary
chondrites, whose properties are tabulated. Two articles are included that summarize data on the
terrestrial ages and thermoluminescence properties of Antarctic meteorites. The Appendix lists
all ANSMET specimens classified as of June 1987, in numerical order for each locality and by
meteorite class.
OFFICIAL PUBLICATION DATE is handstamped in a limited number of initial copies and is
recorded in the Institution's annual report, Smithsonian Year. SERIES COVER DESIGN: Volcanic
eruption at the island of Krakatau in 1883.
Library of Congress Cataloging-in-Publication Data
Field and laboratory investigations of Antarctic meteorites collected by United States expeditions, 1985-1987 / Ursula
B. Marvin and Glenn J. MacPherson, editors,
p. cm. - (Smithsonian contributions to the earth sciences ; no. 30)
Includes bibliographic references
1. Meteorites?Catalogs and collections?Antarctic regions. 2. Astronomy?Research?Antarctic re-
gions. 3. Scientific expeditions?United States. I. Marvin, Ursula B. II. MacPherson, Glenn J. III. Series.
QE1.S227 no. 30 [QB755.5.A6] 550 s-dc20 [523.5T09989] 92-10135
? The paper used in this publication meets the minimum requirements of the American
National Standard for Permanence of Paper for Printed Library Materials Z39.48?1984.
Contents
Page
1. EDITORS' INTRODUCTION, by Ursula B. Marvin and Glenn J. MacPherson 1
2. THE 1984-1985 ANTARCTIC SEARCH FOR METEORITES (ANSMET) FIELD
PROGRAM, by Scott A. Sandford 5
3. THE 1985-1986 AND 1986-1987 FIELD SEASONS, by William A. Cassidy .... 11
4. DESCRIPTIONS OF STONY METEORITES, by Brian Mason, Glenn J. MacPherson,
Roberta Score, Rene Martinez, Cecilia Satterwhite, Carol Schwarz,
and James L. Gooding 17
5. DESCRIPTIONS OF IRON METEORITES, by Roy S. Clarke, Jr 37
6. TERRESTRIAL AGES OF VICTORIA LAND METEORITES DERIVED FROM
COSMIC-RAY-PRODUCED RADIONUCLIDES, by John Evans, John Wacker,
and James Reeves 45
7. NATURAL THERMOLUMINESCENCE LEVELS AND THE RECOVERY LOCATION
OF ANTARCTIC METEORITES, by Fouad A. Hasan, Roberta Score,
Benjamin M. Myers, Hazel Sears, William A. Cassidy, and Derek W.G.
Sears 57
APPENDIX: Tables of ANSMET Meteorites 69
in
LEW86010
1 cm
FRONTISPIECE.?Two of the most interesting meteorites collected during the field seasons described in this
volume were also among the smallest. LEW86O1O (top) was initially believed to be a terrestrial igneous rock,
until examination of a thin section showed it to be the second example of one of the very rarest meteorite
types?an angrite. The photo shows the entire specimen prior to sampling. ALH85O85 (bottom, shown in a
"group photo" with the other ALH8508x specimens) was also not recognized as being unusual until thin section
examination and electron microprobe analyses revealed its unique characteristics.
Field and Laboratory Investigations
of Antarctic Meteorites Collected
by United States Expeditions,
1985-1987
1. Editors' Introduction
Ursula B. Marvin and Glenn J. MacPherson
This is the fifth publication in the Smithsonian Contributions
to the Earth Sciences series to present the results of the yearly
United States Antarctic Search for Meteorites (ANSMET)
expeditions to Antarctica. This issue describes the 1984-1985,
1985-1986, and 1986-1987 field seasons (Figure 1-1).
Descriptions and classifications are given of most of the
meteorites collected during those expeditions with the excep-
tions of types 4, 5, and 6 ordinary chondrites, whose properties
are tabulated in the Appendix. Two articles are included that
summarize data on the terrestrial ages and thermoluminescence
properties of Antarctic meteorites. Appendix Table A lists all
meteorites classified through June 1987 in numerical order for
each locality; Appendix Table B lists specimens in consecutive
order by meteorite class; Appendix Table C summarizes the
total numbers of meteorites collected by ANSMET through
1986, by type.
The numbers and main categories of meteorite specimens
collected in the 1984-1985, 1985-1986, and 1986-1987
seasons are listed in Table 1-1. Total numbers and aggregate
weights of specimens of each meteorite class are given in
Appendix Table B. The aggregate weights are of interest
because of the inherent intractibility of the pairing problem. We
are unlikely ever to obtain secure counts of the number of falls
of each meteorite class represented on the Antarctic stranding
surfaces, and so we cannot compare numbers of Antarctic falls
Ursula B. Marvin, Smithsonian Astrophysical Observatory, Mail Stop
52, 60 Garden Street, Cambridge, Massachusetts 02138. Glenn J.
MacPherson, Department of Mineral Sciences, National Museum of
Natural History, Smithsonian Institution, Washington, D.C. 20560.
with those in the rest of the world. We can, however, obtain
aggregate weights and, allowing for the vagaries of discovery,
gain a general idea of how relative proportions of meteorite
classes in the Antarctic collections compare with those found
elsewhere. The system for naming Antarctic meteorites was
changed in 1982 by the dropping of a letter (A, for example) to
designate the collecting expedition. When the system was
originally adopted, some members of the Nomenclature
Committee looked forward optimistically to a time when two or
more expeditions, from different countries or organizations,
might visit an area such as the Allan Hills during the same
season. They forsaw the need for a letter (A, B, C) to identify
each one. Hence, letters and numbers in a name such as
ALHA76001 were chosen to indicate place, expedition, year,
and specimen number: ALH (Allan Hills), A (Expedition A),
76 (1976), 001 (Specimen 1). In practice, however, meteoriti-
cists viewed the expedition number as incomprehensible and
unnecessary. It has been dropped for all meteorites collected
after the 1981 season; thus, the first Allan Hills specimen of
1982 was ALH82001.
The ANSMET program is governed by an interagency
agreement between the National Science Foundation, the
Smithsonian Institution, and the National Aeronautics and
Space Administration. At the request of the scientific commu-
nity, procedures (based on those used for lunar samples) were
adopted for collecting specimens by sterile techniques and
keeping them frozen until they are processed in nitrogen-filled
cabinets at the Johnson Space Center at Houston. Details of the
field and laboratory procedures are outlined in the first
SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
Syowa Base
Yamato Mts
Belgica
Neptune Mts.
Pecora Escarpment
Grosvenor Mountains
Queen Alexandra Range
Miller Range
Geologists Range
Bates Nunatak
Meteorite Hills
Purgatory Peak (Dry Valleys)
t. Baldr
Man Hills
eckling Peak
lephant Moraine
Outpost Nunatak
Bowden Neve
Derrick Peak
Antarctica
KEY:
Continental Boundary
Ice Shelf Border
Major Glaciers
Meteorite Find
McMurdo Station
Granite Harbor
500 km
FIGURE 1-1.?Outline map of Antarctica showing sites of meteorite finds.
publication in this series (Marvin and Mason, 1980). In order to
distribute research samples quickly and widely, all newly
classified specimens are described in the Antarctic Meteorite
Newsletters; these are mailed, on request, to investigators
throughout the world. Any scientist wishing to obtain samples
may submit a request, describing the proposed research and the
numbers, weights, and types of samples required, to the
Meteorite Working Group, a committee with a rotating
membership responsible for monitoring the program and
allocating samples. Requests for the Antarctic Meteorite
Newsletter or for research materials should be addressed to the
Secretary, Meteorite Working Group, NASA Johnson Space
Center, Code SN2, Houston, Texas 77058.
The Antarctic Meteorite Working Group meets twice each
year, usually in April and October. Each issue of the newsletter
publishes dates of meetings and deadlines for requests. Sample
requests are welcome from all qualified scientists and are
considered on the basis of their merit regardless of whether a
scientist is funded for meteorite research. The allocation of
Antarctic meteorite samples does not in any way commit a
funding agency to support the proposed research.
For references on Antarctic meteorites, see the earlier
publications in this series (Marvin and Mason, editors, 1980,
1982, 1984; Marvin and MacPherson, editors, 1989) and the
computerized lists of publications from the Antarctic Meteorite
Bibliography, which may be obtained on request from the
Lunar and Planetary Institute, 3600 Bay Area Blvd., Houston,
Texas 77058-1113. The Bibliography references articles in
NUMBER 30
TABLE 1-1.?Numbers of classified meteorite specimens collected in the
1984-1985,1985-1986, and 1986-1987 field seasons.
Meteorite Type
Achondrites
Enstatite Chondrites
Unique Chondrites
Ordinary Chondrites
Carbonaceous
Chondrites
Stony-Irons
Irons
Locality
Allan Hills
Elephant Moraine
Lewis Cliff
TOTAL
Allan Hills
TOTAL
Allan Hills
Lewis Cliff
TOTAL
Allan Hills
Bowden Neve
Dominion Range
Elephant Moraine
Geologists Range
Grosvenor Mountains
Lewis Cliff
Miller Range
Rekling Peak
TOTAL
Allan Hills
Lewis Cliff
MacAlpine Hills
Grosvenor Mountains
TOTAL
Lewis Cliff
Queen Alexandra Range
TOTAL
Allan Hills
Elephant Moraine
Grosvenor Mountains
Lewis Cliff
TOTAL
1984
22
1
23
8
8
0
204
7
211
27
27
0
2
1
3
1985
2
9
11
2
2
2
1
3
139
1
11
2
17
152
1
323
13
5
1
19
0
1
1
2
1986
5
5
0
0
13
3
491
6
513
7
7
1
1
2
4
4
Total
24
1
14
39
10
10
2
1
3
356
1
11
10
2
17
643
1
6
1047
40
5
7
1
53
1
1
2
2
1
1
5
9
Meteoritics, in the annual Proceedings of the Lunar and
Planetary Science Conferences at Houston, the Symposiums on
Antarctic Meteorites held by the National Institute of Polar
Research in Tokyo, and numerous other sources.
Libraries of polished thin sections are maintained in
Washington, Houston, and Tokyo for the use of visitors who
wish to make petrographic examinations. To obtain meteorite
samples collected by parties sponsored by the Japanese
Antarctic Research Expeditions, or to use the thin section
library in Tokyo, contact Dr. Keizo Yanai, Curator, at the
National Institute of Polar Research, 9-10 Kaga 1-chome,
Itabashi-ku, Tokyo 173, Japan. To use the thin section library
at the Johnson Space Center at Houston, contact the Secretary
of the Meteorite Working Group at the address given above. To
use the thin section library at the National Museum of Natural
History, Smithsonian Institution, Washington, D.C. 20560,
contact Roy S. Clarke, Jr., Curator.
Literature Cited
Marvin, Ursula B., and Brian Mason, editors
1980. Catalog of Antarctic Meteorites, 1977-1978. Smithsonian Contribu-
tions to the Earth Sciences, 23: 50 pages.
1982. Catalog of Meteorites from Victoria Land, Antarctica, 1978-1980.
Smithsonian Contributions to the Earth Sciences, 24: 97 pages.
1984. Field and Laboratory Investigations of Meteorites from Victoria
Land, Antarctica. Smithsonian Contributions to the Earth Sciences,
26: 138 pages.
Marvin, Ursula B., and Glenn J. MacPherson, editors
1989. Field and Laboratory Investigations of Meteorites from Victoria
Land and the Thiel Mountains Region, Antarctica, 1982-1983 and
1983-1984. Smithsonian Contributions to the Earth Sciences, 28:
146 pages.
2. The 1984-1985 Antarctic Search for
Meteorites (ANSMET) Field Program
Scott A. Sandford
The purpose of the 1984-1985 ANSMET (Antarctic Search
for Meteorites) expedition was to recover meteorites from the
Main, Near Western, Middle Western, and Far Western
icefields in the Allan Hills area and to carry out a reconnais-
sance of other nearby blue icefields. A brief summary of the
locations visited is provided in Table 2-1. Figures 2-1 and 2-2
contain maps of these locations and the routes taken between
them.
Expedition members included leader WA. Cassidy (Univer-
sity of Pittsburgh, Pittsburgh, Pennsylvania), Catherine King-
Frazier (James Madison University, Harrisonburg, Virginia),
John Schutt (University of Pittsburgh, Pittsburgh, Pennsylva-
nia), Roberta Score (National Aeronautics and Space Admini-
stration/Johnson Space Center, Houston, Texas), Carl Th-
ompson (Canterbury, New Zealand), Robert Walker (Washing-
ton University, St. Louis, Missouri), and the author (then at
Washington University, St. Louis, Missouri).
The expedition proper began in late November 1984 when
all the members except for Cassidy gathered at McMurdo
Station on Ross Island; Cassidy joined the party at a later date.
The first week was spent at McMurdo Station, undergoing
survival training (for two days, on the lower slopes of Mt.
Erebus) and gathering and preparing the expedition's gear for
transportation to the Allan Hills area.
During the 6 weeks of the expedition the party lived entirely
in Scott tents, two persons to a tent. Typical "non-storm" day
temperatures were in the -5? to -10? F range with windchill
factors generally falling between -10? and -40? F. Since it was
the austral summer, the sun never set during the entire
expedition. As a result, work days tended to be long, weather
permitting. The entire day was usually spent away from camp.
Cooking was done over portable, single burner gas stoves.
Scott A. Sandford, NASA/Ames Research Center, Moffett Field,
California 94035.
Water was obtained by melting snow and ice. Lunches were
generally very simple affairs, because most food froze solid
once it was taken from the tents (although the author did
determine that thinly sliced pastrami, when put in a plastic bag
and taped against the engine block of a snowmobile, would
remain partially thawed until lunchtime). Typical lunches
consisted of chocolate bars, raisins, and similar items.
After a delay of several days due to bad weather, the party
was transported to the Allan Hills on December 8 using UH-1N
Huey helicopters with an intermediate refueling stop at Marble
Point on the Antarctic mainland (Figure 2-1). The group was
accompanied by a two man photography team from public
television station WQED (Pittsburgh) who were filming
sequences for a documentary. Some of this footage was
subsequently shown in the seven part film series PLANET
EARTH. The film crew left on 10 December.
The first camp was made between the Allan Hills Main
Icefield and the Near Western Icefield (Figure 2-2). The camp
remained in its first location for 8 days, during which the two
nearest icefields were searched for meteorites (Table 2-1,
Figure 2-2). Approximately 80 meteorite fragments were found
during this period. The collection procedure consisted of
search, collection, and surveying. During the search phase the
snowmobiles were driven en echelon (similar to the pattern
used by the fighter plane squadrons of WWII) in order to cover
the maximum possible area in each sweep. This line formation
swept back and forth over the icefield until a meteorite was
spotted. Once found, meteorites were photographed, assigned a
sample number, and enclosed in several successive sample
bags (Figure 2-3). The position of the meteorite was then
determined relative to survey reference points. All the
meteorites were kept frozen until they arrived at the curatorial
facility at the Johnson Space Center in Houston.
On December 17 the camp was moved to a new site at the
Middle Western Icefield (Figure 2-2). The Middle Western
SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
Argentina Range
I Anderson Hills
McMurdo Station
Marble Point
ANTARCTICA KEY
Continental boundary 180*
Ice shelf border
FIGURE 2-1.?A map of the continent of Antarctica. Major sites visited by expedition members during the
1984-1985 field season are marked on the map. The positions of many of these sites are also listed in Table 2-1.
The boxed portion represents the extent of the area enclosed in the map in Figure 2-2.
TABLE 2-1.?Antarctic locations mentioned in the text
Icefield Location Dates and camps
McMurdo Station
Near Western Icefield
(77?30'S, 166?40'E)
(76?44'S, 158?49'E)
Middle Western Icefield (76?50'S, 158?26'E)
Far Western Icefield
Elephant Morraine
Allan Hills Main Icefield
Battlement Nunataks
Trinity Nunataks
Odell Glacier Camp
Carapace Nunatak
Natural Rock Arch
Geologists Range
Anderson Hills
(76?54'S, 157?01'E)
(76?11'S, 157?10'E)
(76?41'S, 159?17'E)
(76?32'S, 159?21'E)
(76?26'S, 160?38'E)
(76?47'S, 159?35'E)
(76?53'S, 159?24'E)
(76?45.5'S, 159?57.7'E)
(82?30'S, 155?30'E)
(84?30'S, 84?00'W)
8-17 Dec 1984
(Camp 1)
17-21 Dec 1984
(Camps 2 and 4)
21 Dec 1984-6 Jan
1985 (Camp 3)
8-10 Jan 1985
9-15 Jan 1985
13 Jan 1985
Not Reached
15-19 Jan 1985
(Camp 7)
16 Jan 1985
Discovered 17 Jan 1985
Aerial Recon 25 Jan
1985
Aerial Recon 25 Jan
1985
Icefield was searched from December 18 to December 21 and
approximately 30 additional meteorites were found. All
traverses were made using snowmobiles to pull trains consist-
ing of 1 to 3 Nansen or Knudsen sleds. Traverses at this
location were made with the snowmobiles in single file to
minimize risks associated with crevasses. On December 21, the
camp was moved to the Far Western Icefield (Figure 2-2). The
southeastern arm of the icefield was extensively searched and
about 120 meteorites were found. The northwestern arm of the
icefield was quickly surveyed but not thoroughly searched.
Christmas Eve was celebrated by cramming 6 people in one
Scott tent and sharing a meal of ham, lobster, shrimp, and yams.
On January 6 the party returned to the Middle Western
Icefield and made an additional search for meteorites. On the
8th, Schutt and Sandford made a trip to Elephant Morraine
(Figure 2-2) in order to meet with two geologists (Gunther
Faure and Karen Taylor of Ohio State University, Columbus,
Ohio) and to escort them back to the Allan Hills area. The rest
of the party proceeded on to the Allan Hills Main Icefield.
NUMBER 30
Far Western Icefield
SOUTH
/ / Middle Western
/Jfc- Icefield
^ Near Western1> Icefield
V
FIGURE 2-2.?A map of the Allan Hills area. Major traverses made during the 1984-1985 field season are shown
as dashed lines and the camp sites are given as numbered dots. The positions of many of the features on the map
can be found in Table 2-1.
While at Elephant Morraine, Sandford and Schutt found an
additional 9 meteorites, including one of the season's few iron
meteorites.
The Elephant Moraine party then proceeded to the Allan
Hills Main Icefield where the entire expedition was reunited on
January 10. Bill Cassidy joined the party on January 12. The
Main Icefield camp was maintained until January 15. During
this time the party searched the nearby icefield and visited the
blue icefield associated with the Battlement Nunataks; no
meteorites were found there.
While at the Allan Hills Main Icefield, an experiment was set
up to determine the extent to which wind moves rocks and
meteorites on the ice. Rocks spanning a range of sizes (about 1
to 10 cm in diameter) were placed on the icefield in two lines
SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
FIGURE 2-3.?The author with the largest meteorite found during the 1984-1985 field season. This meteorite is
an ordinary chondrite.
perpendicular to the prevailing wind direction. One line of
rocks was placed directly on the ice while the other line of rocks
was buried just below the surface of the ice. Both lines were
examined during the next year to see how various sized rocks
were excavated and moved by the wind. After one year the
buried rocks were found to have been entirely exposed by wind
ablation of the ice. While the larger rocks had been moved very
little, some of the middle-sized rocks had moved downwind by
distances in excess of 100 meters. Many of the smaller rocks
were never found again.
On the 15th, camp was broken and a traverse to the Trinity
Nunatak area was begun. Unfortunately, this traverse had to be
abandoned since a recent snowfall had covered up many of the
crevasses along the way and travelling conditions were
hazardous. The party therefore proceeded instead up the Odell
Glacier and established camp at its head. Additional reconnais-
sance trips from this camp were made to the Odell Glacier and
the blue ice near the Carapace Nunatak (see Figure 2-2). It was
during one of these day trips that the author discovered the
natural rock arch shown in Figure 2-4. As far as the author has
been able to ascertain, this is the only known rock arch in
Antarctica.
TABLE 2-2.?Summary of identified meteorites found.
Meteorite class
Ordinary Chondrites
H
L
LL
Enstatite Chondrites
E3
E4
Carbonaceous Chondrites
C2
C3V
C4
Irons
Ureilites
Diogenites
Aubrites
Unique Achondrites
Number found
112
63
15
1
7
24
2
2
3
1
1
18
3
The entire party was airlifted out of the field and returned to
McMurdo Station on January 19. Overall, the expedition
enjoyed generally good weather, and most of the time was
spent successfully hunting for meteorites. A total of 274
NUMBER 30
FIGURE 2-4.?This natural rock arch lies on the western slopes of the Coombs Hills overlooking the Odell Glacier
in southern Victoria Land. The arch is at approximately 76?45.5'S, 159?57.7'Eand is the only formation of its type
known to exist on the southern continent. The arch is estimated to be about 15 meters in height and width.
meteorite fragments were found, ranging in size from about 0.5
x 0.5 x 0.1 cm (0.4 g) to one stone measuring 32 x 22 x 18 cm
(16,000 g) (see Figure 2-3). Most of these samples have now
been examined and a summary of the breakdown by type is
given in Table 2-2. Of special interest are a 17 x 9.5 x 6.5 cm
diogenite and 3 unique achondrites.
At this point, most of the expedition personnel returned to
the United States. Three of the party members (Cassidy, Score,
and Sandford) remained and on January 25 participated in an
airborne reconnaissance (using a C-13O Hercules aircraft) of
potential meteorite-bearing icefields near the Geologists Range
and the Anderson Hills in the Patuxent Range (see Figure 2-1).
The latter site looks promising and future expeditions to this
area are being planned. Additional reconnaissance of icefields
near the Argentina Range had to be cancelled when an
exploratory "ski-drag" landing in the Anderson Hills damaged
the landing gear of the aircraft and it was forced to return to
McMurdo Station.
On January 28 an additional flight was made to the
Amundsen-Scott Station at the south pole. This trip was made
in order to change the sample surface of an electrostatic dust
collector which is in continuous operation at the pole. The
collection surface was returned to the University of Pittsburgh
for examination for extraterrestrial dust particles.
ACKNOWLEDGMENTS.?I would like to thank co-expedition
member Robbie Score for providing the latest summary of the
meteorite types found in the 1984-1985 field season, and for
spurring my memory concerning various details of the trip. My
thanks go also to Mike Zolensky for updating me on the status
of the rock movement experiment at the Alan Hills Main
Icefield.
3. The 1985-1986 and 1986-1987 Field Seasons
William A. Cas sidy
The 1985-1986 Field Season in the Allan Hills
Region and Reckling Peak
Four members of the 1985-1986 Antarctic Search for
Meteorites (ANSMET) field party went to the Allan Hills, a
proven source of meteorites in Southern Victoria Land, and
also made an exploratory trip to Reckling Peak: J. Schutt
(University of Pittsburgh), Ludolph Schultz (Max Planck
Institute, Mainz, Federal Republic of Germany), Michael
Zolensky (NASA/Johnson Space Center), and Ernst Zinner
(Washington University). The geography of this area, and
ANSMET expeditions to it, have been described in detail
previously (e.g., Cassidy, 1989), so only a summary of the
results during the 1986-1986 season are presented here.
Starting in 1976 the Allan Hills yielded meteorites in 10
consecutive austral summers, and by the start of the 1985-
1986 field season only about 40% of the available blue ice area
in the Far Western Icefield remained to be systematically
searched. This was done over the course of approximately 6
weeks from 7 December 1985 on, during which over 140
meteorites were recovered. A reconnaissance visit to another
nearby small icefield yielded only one specimen. Two
reconnaissance searches for meteorites on blue icefields near
Reckling Peak during this season produced no meteorite finds.
Finally, at the end of the season, the field party returned to the
Allan Hills Main Icefield and during the course of random
searches and traverses there 17 more meteorites were recov-
ered.
The 1985-1986 Field Season near Beardmore Glacier
The other four members of the 1985-1986 field party were
stationed at Beardmore Camp: Peter Englert (San Jose State
University), Twyla Thomas (United States National Museum),
Carl Thompson (Methven, New Zealand), and the author. From
William A. Cassidy, Department of Geology, University of Pittsburgh,
Pittsburgh, Pennsylvania 15260.
this base we investigated possible occurrences of meteorites
near Lewis Cliff, Otway Massif, Grosvenor Mountains,
Dominion Range, Geologists Range, and Milan Ridge (Figure
3-1). Only sparse meteorite occurrences were discovered at
Otway Massif and other sites in the Grosvenor Mountains. A
potentially more productive location lies adjacent to Dominion
Range. A few specimens were recovered at Geologists Range
and one at Milan Ridge. Many were found on the surface of an
ice tongue immediately to the east of Lewis Cliff; this area was
exceptionally productive.
On December 11 we made a 69-mile round trip on
snowmobiles out of Beardmore Camp and discovered our first
meteorites: 5 specimens lying on ice about one kilometer east
of the ice tongue below Lewis Cliff. We returned to this site,
and to the ice tongue itself, three times between December 12
and December 16 and collected 13 additional specimens.
On December 20, we were put in by helicopter at Otway
Massif, where we occupied the site called Camp 1 (Figures 3-1
and 3-2). GRO85203 (Figure 3-2) marks a site where we left at
least 20 large and small meteorite fragments undisturbed on the
ice. They all appeared to belong to the same fall. If we had
collected them the total mass would have added unduly to the
cargo we had to transport.
On December 23, we abandoned Camp 1 and made the
36-mile traverse to Camp 2, near Mt. Raymond (Figure 3-3).
This picturesque campsite is located in a shallow, somewhat
protected valley between rounded, dunelike snow masses. We
remained at Camp 2 from December 23 to December 28.
On December 28 we traversed 40 miles to Camp 3, above the
Scott Icefalls (Figures 3-1 and 3-4), where a large area of
exposed ice between our camp and the Icefalls is visible on
aerial photos. The ice, unfortunately, was covered by a thin
layer of snow. Little searching was done because of the snow
cover and semi-whiteout conditions; moreover, crevasses are
common in this area and some were difficult to identify under
the existing conditions. Nonetheless, we found four specimens
11
12 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
164'
170?30'
FIGURE 3-1.?Map showing locations in the vicinity of Dominion Range and the Grosvenor Mountains that were
visited during the 1985-1986 field season.
(shown on Figure 3-4). We plan to return to this site in the
future in the hope of finding the ice swept clean.
On December 31 we made the traverse to Camp 4 (Figure
3-5), a 52-mile trip, and remained there until January 4. Our
reconnaissance searches and recoveries are detailed in Figures
3-4 and 3-5. We were picked up by helicopter at Camp 4 on
January 4 and returned to the Beardmore Camp.
The period between December 20 and January 4 was notable
for the large proportion of fresh-appearing meteorites that we
collected. Many had fusion crusts intact or nearly so. Many
were larger than those we had been accustomed to finding. It
will be interesting to determine whether or not these individuals
have younger-than-average terrestrial ages.
On January 7 we established a new base of operations near
Coalsack Bluff at the site of the old "Hard Times " camp, where
paleontologists processed the first vertebrate fossils found in
Antarctica. The fossil site was discovered in November, 1969,
and the carnp was occupied during that summer. Traces of the
old camp remain: the generator shack was full of snow to its
roof but had a wind scoop on two sides; a number of double
?34'
FIGURE 3-2.?Enlarged map of the region around Otway Massif. Meteorite
recovery locations at Otway Massif, Mt. Raymond (Figure 3-3), and south of
Scott Icefalls (Figure 3-4) are labelled GRO (for Grosvenor Mountains).
NUMBER 30 13
174C
5?34'
85?45'
86?OO'
FIGURE 3-3.?Map of the ML Raymond area of the Grosvenor Mountains.
two-by-fours, nailed together and sticking up out of the snow,
still had electrical wiring stapled to them; and the tops of
55-gallon drums were exposed at the current snow surface.
Large cans of mandarin oranges and grated cheese had been left
in a cache, and were still edible. This is a convenient campsite,
because when storms threaten a party can quickly drive the 28
miles to the Beardmore Camp which never seems to have bad
weather in the summer. Throughout that season the heavy
windstorms stopped north of Mt. Sirius.
We used a scheduled helicopter flight on January 12 to make
a reconaissance survey along the Ice Plateau/Transantarctic
Mountains boundary line, as far north as the Geologists Range.
Meteorites associated with this site have the symbol GEO on
the map (Figure 3-6). We found three specimens on a small ice
patch west of Mt. Summerson, and collected two of them in a
20 mph wind with blowing snow. We later recovered one
fragment on the ice above the valley next to Milan Ridge
(symbol MIL, for Miller Range; Figure 3-7).
On January 16 a four-person party from the U.S. Geological
Survey, led by Gary Parasso, arrived at the Lewis Cliff Ice
Tongue from the Beardmore Camp and established a baseline
for us. They put in two stations on rocky hilltops that describe
a line running approximately north-south, parallel to the eastern
side of the upper part of the ice tongue. All mapping of this area
will be done with reference to these two points.
We systematically searched the entire upper level of the ice
tongue, collecting numerous specimens and mapping their
locations. Recovered specimens at the Lewis Cliff site were
typically small, with very few completely fusion-encrusted
individuals. Many of the specimens were severely weathered,
which made it difficult to distinguish them from the ferrugi-
nous Ferrar dolerites that are scattered liberally across the ice
surface. Weathered coal fragments and pieces of grey shaly
sandstone, both common on the ice surface, presented
additional difficulties because they tend to resemble carbona-
ceous chondrites. These terrestrial rocks made systematic
searching highly tedious and added pleasure to the rare
discovery of an exceptionally large meteorite specimen. Two
14
168*
DOM 85502 </
SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
170?
Scott
crev
falls 85U36'
crevasses
GRO85220*
xGRO 85219
GRO
85216
GRO85210-
85?45'
sses
85?49'
FIGURE 3-4.?Map of the region near Camp 3 where four meteorites were found. At upper left is the ML \Vard_
area, where a number of meteorites were found during the traverse to Camp 4.
166' 168(
85?15'
5?30'
FIGURE 3-5.?Map of the Dominion Range (DOM) in the vicinity of Camp 4.
NUMBER 30 15
154? 155^
GISTS
R A
?-GEO85701
156?
82?30'
N G E
crevasses
>Mt. Summerson
82?45'
FIGURE 3-6.?Map of the Geologists Range where two meteorites (GEO) were
recovered during a reconnaissance survey in the 1985-1986 field season.
such finds were LEW85320 (110 kg) and LEW85319 (11 kg),
both H5 chondrites found on the slope between the upper level
and the lower level of the ice tongue. These specimens may
represent a paired fall.
The meteorite specimens on the upper ice tongue are very
heterogeneously distributed. They occupy a narrow zone at the
southern (upstream) end and a much wider zone at the northern
end, just above the slope down to the lower level. These
distributions are real, and the boundary between the zones is
sharp, but the cause is not obvious.
A symmetrically patterned suite of ice samples was collected
for 818O determinations by Peter Englert. Unfortunately, the
samples were lost in transit to, or at, McMurdo Station.
In summary, the 1985-1986 field season was very success-
ful and the Lewis Cliff Ice Tongue was established as a major
new source of Antarctic meteorites.
The 1986-1987 Field Season
Members of the 1986-1987 party were Christian Koeberl
(University of Vienna), Louis Lindner (National Institute for
Nuclear Physics and High Energy Physics, Amsterdam),
Austin Mardon (Texas A&M University), John Schutt (Univer-
sity of Pittsburgh), Keizo Yanai (National Institute of Polar
Research, Tokyo), and the author. The entire field season was
154?
83?15'
FIGURE 3-7.?Map of the Miller Range (MIL), showing the location where a meteorite was found near Milan
Ridge during the 1985-1986 field season.
16 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
spent at the Lewis Cliff Ice Tongue because of the importance
of this newly discovered stranding surface. We were in the field
from December 6 to January 21. We concentrated mainly on
foot searches in the southern part of the lower ice tongue, just
below the step, where relatively high densities of small
meteorite fragments were found. We collected and mapped all
of our finds.
We also began finding meteorites along the southern edge of
an extensive moraine that lies east of the ice tongue. Fragments
occurred among the rocks as far as 20 meters into the moraine,
making the search procedure particularly difficult; this was the
first time any of us had had to search on our hands and knees.
Most of the specimens we collected are weathered fragments of
ordinary chondrites with minor patches of fusion crust; most of
them probably are paired. We named this area Meteorite
Moraine.
Ordinary chondrites dominate the accumulations on the
lower ice tongue as well as in Meteorite Moraine. Interesting
distributions of specimens with differing thermoluminescence
properties are described by Hasan et al. (Article 7).
We carried out an ice sampling program in which we
duplicated Englert's pattern of the previous season and also
sampled at 10-meter intervals along a line crossing the
boundary of the meteorite distribution field on the upper ice
tongue. On a reconnaissance survey we discovered a significant
accumulation of meteorites on exposed ice around Goodwin
Nunataks, about 50 kilometers south (i.e., upstream) of the
Lewis Cliff Ice Tongue. That accumulation was left in place for
a future field season when we can put in a camp nearby.
The total number of probable meteorite specimens from
Lewis Cliff Ice Tongue and Meteorite Moraine is now over
700.
Stratigraphic Features at the Lewis Cliff Ice Tongue
Lewis Cliff Ice Tongue is a promising site for establishing an
ice-stratigraphic series that would provide a new reference
framework within which to evaluate the observed distribution
of meteorites on the stranding surface. The main time markers
are dust bands composed of volcanic ash that dip into the ice.
It appears that an essentially horizontal series of tephra deposits
have been tilted and exposed at the surface by wind ablation.
We have been mapping and sampling these bands.
Other interesting features at the ice tongue are bed-load dust
bands and regelated ice. Ice at the bed of a glacier or moving ice
sheet can be melted for short periods and refrozen. The melted
stage lasts long enough for extensive, but not complete,
degassing to occur. As a result, the regelated (recrystallized) ice
is mostly bubble-free; the remaining bubbles often form linear
trains suggestive of streaming. Dust and rocks, the latter often
rounded and glacially striated, can be entrained in regelated ice
and carried slowly downstream parallel to the bed of the
glacier. If the ice reaches a barrier it may buckle or shear, and
in either case regelated ice, with its load of sediment, then can
be thrust to the surface. If only the finer particles reach the
surface, they form dust bands composed of basal rock detritus
instead of tephra. If larger rocks are brought to a surface where
ablation is taking place, a mass of unsorted glacial debris soon
litters the ice on either side of the dust band. This sedimentary
cover effectively slows the ablation process and the result, after
a period of time, is an ice ridge strewn with a thin veneer of
boulders and cobbles with a planar core of glacial debris. This
is a so-called ice-core moraine. Ice-core moraines are structural
features that can yield stratigraphic information because they
preserve a record of forces that have acted to distort the original
simple stratigraphic sequence.
Much less well understood at the Lewis Cliff Ice Tongue are
bands of evaporite-type mineral deposits that apparently extend
in a planar array along levels stratigraphically higher than the
interface between regelated ice and unmelted ice. They seem to
be parallel and close to this boundary, but detached from it.
They may be related to the regelation process but the nature of
this relation is not clear. In any case, although they may not
represent time horizons, the evaporite deposits probably give
stratigraphic data, at least over the short range.
With the available stratigraphic and structural clues at the
Lewis Cliff Ice Tongue, it should be possible to establish a
relative stratigraphic sequence across the meteorite stranding
surface. If we then can determine absolute ages for some of the
marker horizons we will have what amounts to an ice core laid
out horizontally at the surface. Such an expanse of ice, where
dated dust bands can be mapped in context with distributions of
meteorite terrestrial ages, will provide an excellent testing
ground for the different models of the meteorite stranding
mechanism.
ACKNOWLEDGMENTS.?During the 1986-1987 field season,
Gunter Faure of Ohio State University led a party to the Allan
Hills, Reckling Moraine, and Elephant Moraine, principally to
study moraines associated with meteorite stranding surfaces.
During the course of their field work, they came across 22
meteorites (plus 2 possible meteorites), collected them in a
careful manner, and turned them over to our group at the end of
the season. We are very grateful for this action on their part.
Members of their group were G. Faure, D. Buchanan, E. Hagen,
and M. Strobel.
We also acknowledge with thanks the efforts of the U.S.G.S.
group that surveyed our mapping baseline. The members of
that field team were G. Parasso, E. Eckel, M. Hower, and G.
Sandul. We are indebted to all the dedicated professionals listed
above. This work was supported by NSF Grant DPP 83-14496.
Literature Cited
Cassidy, W.A.
1989. The 1982-1983 Antarctic Search for Meteorites (ANSMET) Field
Program. In U.B. Marvin and G.J. MacPherson, editors, Field and
Laboratory Investigations of Meteorites from Victoria Land and the
Thiel Mountains Region, Antarctica, 1982-1983 and 1983-1984.
Smithsonian Contributions to the Earth Sciences, 28:5-8.
4. Descriptions of Stony Meteorites
Brian Mason, Glenn J. MacPherson, Roberta Score, Rene Martinez,
Cecilia Satterwhite, Carol Schwarz, and James L. Gooding
This article gives descriptions of the achondrites, mesosider-
ites, and the more unusual chondrites (unique, carbonaceous,
enstatite, and type 3 ordinary chondrites) collected during the
1984-1985, 1985-1986, and 1986-1987 field seasons. Sum-
mary data for the other ordinary chondrites are included in the
Appendix. Within the carbonaceous and enstatite chondrites,
the specimens are grouped according to the Van Schmus-Wood
(1967) classification, and the descriptions follow the order of
increasing petrographic type. The descriptions are based
largely on those published in the Antarctic Meteorite Newslet-
ter, with additional information as available. The letter-number
designation concurs with the guidelines recommended by the
Committee on Nomenclature of the Meteoritical Society, and
carries the following information: location, e.g., ALH, Allan
Hills; field season, e.g., 84, 1984-1985 field season; xxx,
digits indicating sequential number of the specimen. The
original weight of the specimen is given to the nearest 0.1 gram.
Chondrites
UNCLASSIFIED OR UNIQUE
FIGURES 4-1,4-2,4-3
ALH85085 (11.9 g).?This small stone is entirely covered
with an iridescent brown fusion crust. The interior is black with
abundant small (~1 mm) white inclusions. Some oxidation is
present.
Brian Mason and Glenn J. MacPherson, National Museum of Natural
History, Smithsonian Institution, Washington, D.C. 20560. Roberta
Score, Rene Martinez, Cecilia Satterwhite, Carol Schwarz, and James
L. Gooding, National Aeronautics and Space Administration, Johnson
Space Center, Houston, Texas 77058.
Detailed petrographic studies of this unusual meteorite have
been published by Scott (1988), Weisberg et al. (1988), and
Grossman et al. (1988); the following description is taken from
these three papers. ALH85085 consists of ~5%-10% chon-
drules (mostly of the radial pyroxene and cryptocrystalline
varieties), -5% dark lithic clasts, 20%-23% metal, and
~60%-70% silicate fragments. There is little or no true matrix.
Electron microscope examination reveals the presence of
numerous (100 or more per thin section) but tiny (<120 pm)
and volumetrically-minor refractory inclusions. Weisberg et al.
(1988) and Scott (1988) found rare grains of osbornite (TiN).
Silicate phases in chondrules and fragments are very iron poor:
the olivine composition is FaQ_40, with most FaQ_5 and only rare
grains as Fe-rich as Fa50; low calcium pyroxene is Fso_25. Many
lithic clasts appear to be Cl fragments or C2 matrix lumps rich
in sulfide, magnetite framboids, platelets and spheroids, and a
presumably hydrous matrix that gives low microprobe analysis
totals; also present are "reduced" clasts that are rich in tiny
metal grains.
Estimates of bulk composition from broad- or rastered-beam
electron microprobe analyses show that ALH85085 has
roughly chondritic ratios of refractory lithophile elements, is
greatly depleted in volatile elements such as Na, Mn, and S, and
is greatly enriched in siderophile elements such as Fe and Ni.
Grossman et al. (1988) and Weisberg et al. (1988) note that
ALH85085 has close affinities with the Renazzo-type carbona-
ceous chondrites, although only the former authors advocate
classifying it as such; Weisberg et al. (1988) and Scott (1988)
regard ALH85085 as a new variety of chondrite. The oxygen
isotope composition of bulk ALH85085 (Clayton and Mayeda,
1988) is similar to those of bulk Renazzo and Al Rais. Wasson
and Kallemeyn (1990) give trace and minor element data for
17
18 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
FIGURE 4-1.?Photomicrograph of the unique chondrite ALH85085. Micro-
chondrules, chondrule fragments, and mineral grains are the main features
visible in this photo. The largest chondrule is cryptocrystalline; the largest
fragment is a piece of a porphyritic chondrule. The dark background is not
matrix but, rather, abundant metal plus underexposed silicate grains. Width of
field is 1.1 mm.
ALH85085 and argue that it is not a true chondrite at all but,
rather, predominantly the product of an impact ejecta cloud.
Grady and Pillinger (1989) found ALH85085 to have the
highest enrichment of 15N ever measured in any whole-rock
meteorite.
ALH85151 (13.9 g).?Traces of dull black fusion crust
remain on an exterior surface that is otherwise dull brownish-
gray and heavily pitted; clasts and inclusions are present in
relief. One notable clast is black with small white inclusions.
FIGURE 4-2.?Photomicrograph of the chondrite ALH85151. A mixture of
chondrules, chondrule fragments, dark clasts, and mineral grains are dispersed
throughout the dark matrix. Opaque grains are almost exclusively sulfide, with
sparse chromite; metal is absent. Width of field is 2.3 mm.
FIGURE 4-3.?Photomicrograph of the unique chondrite LEW85332. Abundant
chondrules of a wide range of sizes, chondrule fragments, iron-nickel metal,
sulfide, and mineral grains are scattered in the darker matrix. The tiny
chondrule at lower left center is roughly 80 (Am in diameter. At left is a small,
irregularly-shaped, rimmed, hibonite-bearing refractory inclusion. Width of
field is 2.3 mm.
The interior is medium-gray with white inclusions; oxidation is
extensive in some areas. A thin section shows numerous
chondrules (up to 1.2 mm across) and chondrule fragments in
a fine-grained matrix. Most of the chondrules consist mainly of
porphyritic and barred olivine; pyroxene is rare. Minor
amounts of nickel-iron and sulfide are present, mainly as very
small grains scattered through the matrix. Microprobe analyses
give the following compositions: olivine, FaQ4_41, with a mean
of Fa34; pyroxene, Fs6_30.
Weisberg et al. (1989) report oxygen isotope data for
ALH85151 that show it belongs to a previously unknown
chondrite group that includes the meteorite Carlisle Lakes.
Rubin and Kallemeyn (1989) give detailed petrologic and bulk
chemical data that also demonstrate the unusual nature of this
chondrite; those authors note the similarity of ALH85151 to
Carlisle Lakes and, possibly, Y-75302.
LEW85332 (113.7 g).?Dark fusion crust covers all but one
surface of this meteorite. The interior has a dark gray
fine-grained matrix with a few light-colored inclusions. A thin
section shows an aggregate of small chondrules (up to 1.2 mm
across, but most are less than 0.5 mm), chondrule fragments,
and irregular granular masses set in a translucent yellow-brown
matrix. Chondrules are mainly porphyritic olivine and radial
pyroxene/cryptocrystalline. Minor amounts of nickel-iron and
sulfide are present, as small grains scattered through the matrix,
and locally concentrated around chondrule rims. Including
microprobe data from Rubin and Kallemeyn (1990), olivine has
a wide composition range, Fa2_37, with a mean of Fa^ less
abundant pyroxene has a composition range Fsj_30.
Rubin and Kallemeyn (1990) report petrologic and bulk
NUMBER 30 19
FIGURE 4-4.?Photomicrographs of C2 chondrites: a, ALH84029; b,
ALH84033; c, GRO85202. The photos show an assortment of chondrules,
inclusions, and mineral grains dispersed within abundant dark matrix; in
ALH84029 the visible grains are mostly phyllosilicate, in ALH84033 most are
olivine, and in GRO85202 both phyllosilicates and olivine are present The
matrices in all three consist of green-brown phyllosilicate. Width of field in
each photo is 2.3 mm.
chemical data for LEW85332 that show it is probably a
carbonaceous chondrite of a unique type.
CLASS C2
FIGURE 4-4
ALH84029, 84030, 84031, 84032, 84034, 84035, 84040,
84041, 84042, 84043, 84044, 84045, 84047, 84048, 84049,
84051, 85004, 85012 (total weight 542.5 g).?These are all
small fragments, some with fusion crust, the largest of which
(ALH84044) weighs 147.4 g. They were found close together
on the SE edge of the Allan Hills Far Western Icefield, and this,
together with their unique mineralogy (almost entirely phyllos-
ilicate), indicates that they are likely paired (probably also with
ALH831OO, ALH83102, and ALH83106). The major compo-
nent is a brown to black phyllosilicate matrix that encloses
green to pale brown phyllosilicate pseudomorphs of chon-
drules, crystals, and inclusions. Calcite is abundant. Sporadic
primary olivine crystals (composition FaQ_2 ) are preserved,
although a few as iron-rich as Fa37 were found. Chondrules and
inclusions range up to a little over 1 mm in diameter, and are
completely altered to phyllosilicates. Chromite, pentlandite,
and (?) magnetite are accessory. Gibson (1987) measured
carbon abundances in ALH83100 (1.948%) and ALH84029
(1.863%). McSween (1987) determined matrix compositions in
ALH831OO and ALH84034 and agreed that they are probably
paired.
ALH84033, 84036, 84039, 84046, 84050, 84053, 84054,
84191 (total weight 139.3 g).?These small fragments (the
largest, ALH84033, weighs 60.4 g), some with fusion crust,
were collected at widely scattered locations on the Allan Hills
Far Western Icefield; they are so similar in texture and
mineralogy that they are tentatively paired. Unlike the
ALH84029 group, these C2 carbonaceous chondrites contain
abundant preserved primary phases. Chondrules up to nearly 2
mm in diameter, along with abundant and varied inclusion
types, crystals, and crystal fragments, are dispersed in a black
20 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
matrix that is reddish brown on thin edges. Olivine is uniformly
Fa^ among the grains analysed. Rare pyroxene is nearly pure
MgSiO3. Troilite, pentlandite, nickel-iron, chromite, and (?)
magnetite are accessory phases. Many refractory inclusions are
present, containing spinel, perovskite, and in a few cases
blue-pleochroic hibonite.
Gibson (1987) determined the carbon content in ALH84033
to be 1.671%.
ALH85OO5, 85007, 85008, 85009, 85010, 85013, 85106
(total weight 326.5 g).?These specimens are very similar in
texture and mineralogy and are tentatively paired. Most are
fragments, some with fusion crust. The largest, ALH85O13, is
a completely crusted stone weighing 130.4 g. ALH85OO8,
ALH85009, ALH85O1O, and ALH85O11 were found close
together at the NW end of Allan Hills Far Western Icefield. In
thin section the meteorites are seen to consist largely of black
opaque matrix, through which are scattered small (up to 0.2
mm) mineral grains and sparse chondrules and chondrule
fragments. The chondrules and most of the mineral grains
consist of olivine, usually close to Mg2Si04 in composition but
some are more iron-rich. Pyroxene is less common, and is close
to MgSiO3 in composition. A few grains of calcite were noted.
GRO85202 (27.2 g).?Thin fusion crust covers two sides of
this stone; it is highly fractured, and disintegrated on chipping.
A thin section shows a dark brown to black matrix with
numerous mineral grains and aggregates and rare small
chondrules. Most of the mineral grains and aggregates consist
of an isotropic to weakly birefringent serpentine-like mineral.
A few grains of olivine near Mg2Si04 in composition were
analysed; some grains of calcite were noted.
LEW85306, 85307, 85309, 85311, 85312 (total weight
293.5 g).?These specimens are very similar in texture and
mineral compositions, and are tentatively paired. The largest,
LEW85311, weighs 199.5 g. Frothy black fusion crust is
present as patches on these stones. A thin evaporite deposit is
present on LEW853O9. The interiors show abundant light-
colored clasts and chondrules set in a black fine-grained matrix.
Some reddish-brown oxidation was noted. Thin sections show
numerous mineral grains and aggregates and a few small
(maximum diameter 0.6 mm) chondrules in a brown to black
matrix. Most of the mineral grains are olivine, usually near
Mg2Si04 in composition, but some are more iron-rich.
Pyroxene is less abundant, and is near MgSiO3 in composition.
LEW86004, 86005, 86007, 86008, 86009 (total weight 20.5
g).?These specimens are so similar that they are tentatively
paired. Some fusion crust remains on each of these stones.
White evaporite deposit speckles the crust-free surfaces of
LEW86005 and LEW86007. A brownish weathering rind
extends 1-2 mm into the interior of LEW86004, LEW86008,
and LEW86009. Unweathered interior matrix is jet black and
contains abundant rounded and irregular inclusions. Thin
sections show numerous small colorless grains (mainly
olivine), irregular aggregates, and rare chondrules in an opaque
to translucent brown matrix. Microprobe analyses of the
olivines show a composition range of FaQ_54 with a marked
peak at FaQ^. A few grains of clinoenstatite were analysed,
having a composition range of Fso_7.
CLASS C3
FIGURE 4-5
ALH84028 (735.9 g), 84037 (3.0 g).?These two meteorites
are so similar that they can confidently be paired. Bubbly black
fusion crust covers about 50% of ALH84O28; the interior is
gray with numerous 1-2 mm sized lighter inclusions, and
shows a few oxidation halos. A thin section shows a variety of
chondrules up to about 2 mm in diameter, together with clasts
and inclusions up to about 4 mm in maximum dimension, in a
pristine matrix consisting of abundant minute olivine plates
with composition Fa45_50, troilite, and awaruite. The chon-
drules are very well preserved, and many contain devitrified
glass. The olivine in chondrules, and larger matrix grains, has
a wide range of composition, FaQ_30, but most are FaQ_10.
Pyroxene grains having a composition close to WojEn^ were
analysed, although a wider range of compositions like that of
olivine is presumably present. Fine-grained and "coarse-
grained" refractory inclusions are present; one example found
is a type A, irregular in shape, that contains gehlenitic melilite,
spinel, and very Ti-rich fassaitic pyroxene. This is a C3V
carbonaceous chondrite.
ALH85OO3 (50.1 g).?Thick patchy fusion crust covers
approximately 70% of this meteorite. The interior is light gray
and chondrules or clasts are not distinguishable in the granular
matrix. A 1 mm thick weathering rind and small patches of rust
are present. A thin section shows an aggregate of small
chondrules (up to 0.9 mm diameter, but most are less than 0.6
mm), chondrule fragments, and irregular aggregates set in a
translucent yellow-brown matrix. Chondrules are mainly
granular or porphyritic olivine. Minor amounts of nickel-iron
are present, as small grains scattered throughout the section.
Microprobe analyses of olivine show a wide composition
range, Fa,_56, with a mean of Fa17; only a few grains of
pyroxene were found, having a composition range of Fs0 5_23.
This meteorite is a C3 chondrite of the Ornans subtype; it is
possibly paired with ALH82101 (they were found 2.5 km apart
at the northern margin of the Allan Hills Far Western Icefield).
ALH85006 (49.0 g).?Fusion crust is present on only one
surface of this coherent stone. The interior is made up of
chondrules up to 2 mm in diameter and irregular white
inclusions up to 3 mm long. A thin section shows a variety of
chondrules (up to 2.5 mm across), chondrule fragments, and
irregular clasts in a dark brown to black matrix. Fine-grained
opaques are dispersed throughout the matrix, and rim some of
the chondrules. The matrix consists largely of fine-grained
iron-rich (Fa45_47) olivine. Olivine in the chondrules and
mineral fragments is usually near Mg2Si04 in composition, but
more iron-rich grains are also present. Pyroxene is much less
NUMBER 30 21
FIGURE 4-5.?Photomicrographs of C3 chondrites: a, ALH84028 [C3V]; b,
ALH85OO6 [C3V]; c, ALH85OO3 [C3O]. Large chondrules, chondrule
fragments, mineral fragments, and irregularly-shaped inclusions are dispersed
within the abundant dark matrices. The chondrules in ALH85003 are smaller
and more numerous than in the two C3V meteorites shown. Width of field in
each photo is 2.3 mm.
abundant than olivine, and is close to MgSiO3 in composition.
The meteorite is a C3V chondrite.
LEW86006 (0.8g).?Forty percent of this small stone is
covered with dull black fusion crust; dark gray matrix with
some irregular white inclusions makes up the interior. The very
small thin section (5x3 mm) shows several chondrules, up to
1.5 mm across, and some irregular granular aggregates in a very
fine-grained translucent brown matrix. The chondrules consist
mainly of olivine, some with polysynthetically-twinned clino-
pyroxene. Microprobe analyses give olivine compositions in
the range Fao_27, with a mean of Fa6; pyroxene compositions
range from Fs0 to Fs5. The matrix appears to consist largely of
fine-grained iron-rich olivine (Fa40_50). The meteorite is
tentatively identified as a C3V chondrite.
CLASS C4
FIGURE 4-6
ALH84038 (12.3 g).?This fragment has black to reddish-
brown fusion crust on all but one surface; the interior is dark
gray and fine-grained with no features visible. Thin section
examination shows the meteorite to consist largely of finely
granular olivine (grains up to 0.1 mm) with rare chondrules and
chondrule fragments, and a little opaque material. Microprobe
analyses, including data from Kallemeyn et al. (1991), give the
following compositions: olivine, Fa25_30 (one grain was found
with a composition of Fa39), with a mean of Fa^; pyroxene
(Fs26_28); and plagioclase (An22_82). The minor element and
trace element data of Kallemeyn et al. (1991) support the
original proposal that this meteorite might be paired with
ALH82135. Kallemeyn et al. (1991) have proposed a new
group of carbonaceous chondrites, CK (after Karoonda), within
which ALH84038 is classified by them as CK4.
ALH85002 (437.7 g).?Most of the surface is covered with
reddish-brown polygonally-fractured fusion crust. The interior
is light gray with dark rounded inclusions as large as 1 mm and
white irregular inclusions up to 3 mm long. Thin section
examination reveals mostly fine-grained olivine (grains up to
22 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
FIGURE 4-6.?Photomicrographs of C4 chondrites: a, ALH85002. Chondrules,
chondrule fragments, magnetite, and sulfide are dispersed in the granular
olivine-rich matrix, b, LEW86258. Chondrules, chondrule fragments, mineral
grains, and some small irregular inclusions are visible in the granular
olivine-rich matrix. Width of field in each photo is 2.3 mm.
0.1 mm), with a little pyroxene, plagioclase, and opaques
(largely magnetite). A few chondrules, made up of coarser-
grained olivine, are present. Microprobe analyses, including
data from Kallemeyn et al. (1991), give the following
compositions: olivine, Fa30; pyroxene, Fs23_29; plagioclase,
An3066. Kallemeyn et al. (1991) give trace and minor element
data for ALH85OO2, and they classify it as CK4.
LEW86258 (24.1 g).?This stone is gray and friable with
black chondrules protruding from weathered surfaces; about
40% of the surface is covered with polygonally-fractured black
fusion crust. A thin section shows a few chondrules in a matrix
consisting largely of fine-grained olivine (grains up to 0.1 mm),
with a little pyroxene, plagioclase, and opaques (almost entirely
magnetite, with a little nickel-iron). Most chondrules are about
1 mm in diameter and consist of granular olivine; one large (2.5
mm) chondrule was found that consists of radiating plagioclase
laths up to 0.8 mm long in a matrix of granular olivine and
diopside. Microprobe analyses, including data from Kallemeyn
et al. (1991), give the following compositions: olivine, Fa32;
low-Ca pyroxene, Fs26; diopside, Wo42Fs5 with 4.8% A12O3,
1.9% TiO2; plagioclase, An3I_83. Kallemeyn et al. (1991) give
trace and minor element data for LEW86258, and they classify
it as probable type CK4 (weathered).
ENSTATITE CHONDRITES
FIGURE 4-7
ALH84170 (39.2 g).?Fifty percent of this fragment is
covered by extremely weathered fusion crust; the interior has a
black matrix with numerous white to gray rounded and
irregular inclusions. Seen in thin section, chondrules (0.3-2
mm) are abundant and consist of radiating or granular
pyroxene, some with olivine. The matrix is made up of
chondrule fragments and mineral grains, with a considerable
amount of opaques (nickel-iron and sulfides). Weathering is
extensive, with brown limonitic staining throughout. Micro-
probe analyses show many grains of olivine and pyroxene close
to Mg2Si04 and MgSiO3 in composition, but some contain a
considerable amount of iron. The nickel-iron contains 2.2%-
3.0% Si. This meteorite is classified as type EH3.
ALH84188, 84200, 84206, 84220, 84235, 84250, 84254,
85159 (total weight 64.1 g).?Most of these small fragments,
some of which are extremely weathered, were collected in a
limited area of the Allan Hills Near Western Icefield. In thin
section the chondrules and chondrule fragments are abundant
but mostly small (ranging up to 0.6 mm across with only a few
larger ones); they consist of fine-grained to coarsely granular
pyroxene. The matrix consists of small pyroxene grains and
opaques (mostly nickel-iron with some sulfides). Weathering is
indicated by brown limonitic staining throughout the sections.
Microprobe analyses give the following pyroxene composi-
tions: FsO6_4, with a mean of Fs18. The nickel-iron contains
2.3% Si. These fragments are classified as type E4.
ALH85119 (20.6 g).?This stone, found near the NW end of
the Allan Hills Far Western Icefield, is completely covered
with frothy black fusion crust; evaporite deposit is present
underneath the fusion crust in some areas. The interior is
charcoal gray with dark chondrules; oxidation is extensive in
some areas. A thin section shows a compact aggregate of
chondrules, chondrule fragments, and irregular clasts up to 3
mm across, together with about 25% nickel-iron in grains up to
1.5 mm and minor troilite. A blue -isotropic phase?possibly
ringwoodite?is present as isolated sporadic grains in the
matrix and as an interstitial phase (replacing glass?) within a
few chondrules. Pyroxene is the predominant silicate; minor
olivine occurs as small grains poikilitically enclosed in
pyroxene. Many of the pyroxene crystals are clouded with very
NUMBER 30 23
FIGURE 4-7.?Photomicrographs of enstatite chondrites: a, ALH84170 [EH3];
b, ALH84188 [E4]; c, ALH85119 [E4?]. Numerous chondrules, chondrule
fragments, and mineral grains are visible in the dark matrices of each meteorite.
All three show deformed and broken chondrules. Width of field in each photo
is 2.3 mm.
fine-grained opaque material; in addition, many pyroxenes are
intensely deformed and even granulated, suggesting?taken
together with a clear directional fabric visible in the section and
the possible presence of ringwoodite?that this meteorite has
been severely shocked. Coarsely crystalline graphite occurs
within some metal grains. Pyroxene compositions are Fs0 3_12,
mean Fs24. The nickel-iron contains 0.4%-0.6% Si. This
meteorite has been tentatively classified as an E4 chondrite in
the Antarctic Meteorite Newsletter, but the silicon content of
the metal is low for EH.
CLASS H3
FIGURE 4-8
ALH85121 (55.3 g).?Frothy brown and black fusion crust
covers the top surface of the "mushroom cap" shaped stone,
and thick (2 mm) viscous ropy fusion crust covers the lower (B)
surface. The interior is moderately to heavily weathered, with a
weathering rind up to 5 mm thick; numerous clasts and
chondrules are present. A thin section shows abundant
chondrules and chondrule fragments up to 3 mm across, in a
matrix of fine-grained olivine and pyroxene with moderate
amounts of nickel-iron and troilite (locally rimming chon-
drules). Chondrule types include granular and porphyritic
olivine and olivine-pyroxene, and radiating or cryptocrystalline
pyroxene. Weathering is extensive, with limonitic staining and
small areas of red-brown limonite throughout. Microprobe
analyses show olivine and pyroxene with a considerable range
in composition: olivine, Fa^g (the coefficient of variation,
c.v., for FeO is 16); pyroxene, Fs3_31. The meteorite is classified
as an H3 chondrite (estimated H3.8).
LEW85383 (18.5 g).?This angular stone is completely
covered with polished black fusion crust. The interior is heavily
oxidized, masking any structure present. The section shows
abundant chondrules and chondrule fragments, up to 1.5 mm
across, in a minor amount of finely granular matrix containing
considerable nickel-iron and lesser troilite. A variety of
24 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
FIGURE 4-8.?Photomicrograph of the H3 chondrite ALH85121. Chondrules,
chondrule fragments, and mineral grains are visible in a dark matrix. Part of the
"matrix" is in fact dark limonite staining. Width of field is 2.3 mm.
chondrule types is present, mostly porphyritic and granular
olivine and olivine-pyroxene, but some cryptocrystalline and
radiating pyroxene chondrules also occur. Weathering is
extensive, with brown limonitic staining throughout the
section. Microprobe analyses show olivine and pyroxene of
variable composition: olivine, Fa6_23 with a mean of Fa17 (c.v.
FeO is 26); pyroxene, Fs2_18. The meteorite is classified as an
H3 chondrite (estimated H3.7).
LEW86102 (21.8g), 86105 (6.4 g).?Shiny smooth brown/
black fusion crust completely covers both of these specimens.
The interiors consist of black matrix with abundant small
weathered chondrules. Oxidation is scattered throughout the
interiors with LEW86105 being the more weathered of the two
samples.
Thin section examination shows that the two specimens are
very similar and probably paired. Chondrules and chondrule
fragments are abundant, ranging up to 2.1 mm across; most are
porphyritic or granular olivine and olivine-pyroxene, but a few
radiating or cryptocrystalline pyroxene chondrules were noted.
They are surrounded by a dark finely granular groundmass
containing some metal and a little sulfide, often as rims to
chondrules; the metal is extensively altered to limonite.
Microprobe analyses show olivine and pyroxene of highly
variable composition; olivine, Faj_50 (c.v. FeO is 70);
pyroxene, Fs^j. The meteorites are classified as H3 chon-
drites (estimated H3.3).
CLASS L3
FIGURE 4-9
ALH84120 (129.0 g), 85045 (145.0 g).?Thirty percent of
ALH84120 is covered with fusion crust; fractured brown fusion
crust covers most of ALH85045. The interiors of these
unequilibrated chondrites are light to medium gray and show
abundant chondrules (up to 3 mm across ) and irregular
inclusions. Sections show an aggregate of chondrules (0.3-2.4
mm across) and chondrule fragments in a fine-grained matrix
of olivine and pyroxene with minor amounts of nickel-iron and
troilite. A variety of chondrule types is present; one barred
chondrule was found with transparent pale brown glass
between the olivine bars. Most of the pyroxene is polysyntheti-
cally twinned clinobronzite. Minor weathering is indicated by
brown limonitic staining around metal grains. Microprobe
analyses gave the following compositions: olivine, Fa^.^,
mean Fa23 (c.v. FeO is 8); pyroxene, Fs6_22. These L3
chondrites (estimated L3.9) are very similar and may be paired.
ALH84205 (25.2 g).?Fusion crust covers 60% of this stone.
The interior is made up of light to medium gray matrix with
abundant light and dark chondrules and inclusions. In thin
section chondrules and chondrule fragments are abundant,
ranging up to 2.1 mm across; most are granular olivine and
olivine-pyroxene, but barred olivine and cryptocrystalline
pyroxene chondrules are also present. Many have narrow black
rims. Nickel-iron and troilite are present in small amounts.
Microprobe analyses give the following compositions: olivine,
Fa12_33, with a mean of Fa19 (c.v. FeO is 27); pyroxene, Fs4_19.
The meteorite is classified as an L3.7 chondrite.
ALH85062 (167.3 g), 85155 (18.5 g).?These stones are
partly covered with dull black fusion crust. The interiors show
a gray matrix with abundant inclusions. Sections show a
close-packed aggregate of chondrules and chondrule fragments
(up to 2.1 mm across) in a dark finely granular matrix, which
includes minor amounts of nickel-iron and troilite. A variety of
chondrule types is present, including granular and porphyritic
olivine and fine-grained pyroxene. Both olivine and pyroxene
show a wide range in composition: olivine, Fa^g, mean Fa16
(c.v. FeO is 40); pyroxene, Fs3_20. These meteorites are very
similar and may be paired. They are classified as L3.5-3.6, and
may belong to the ALHA77011 pairing group.
ALH85070 (12.9 g).?Fusion crust covers about 75% of this
stone. The interior is light-gray and has abundant inclusions.
Oxidation is light. The section shows abundant chondrules and
chondrule fragments, up to 2 mm across, in a fine-grained
matrix containing a few coarser grains of nickel-iron and
troilite. A variety of chondrule types is present including
granular and porphyritic olivine and olivine-pyroxene, barred
olivine, and crypto-crystalline pyroxene. Much of the pyroxene
is polysynthetically-twinned clinobronzite. Minor weathering
is indicated by rusty halos around metal grains. Microprobe
analyses show olivine and pyroxene of variable composition:
olivine, Fa4_25 with a mean of Fa18 (c.v. FeO is 38); pyroxene,
Fs1_29. The meteorite is classified as an L3 chondrite (estimated
L3.6).
LEW85339 (28.8 g).?Polygonally fractured fusion crust
completely covers this small specimen. The interior is light
gray with chondrules and other inclusions measuring up to ~3
mm in diameter. One dark haloed inclusion (metallic?) is ~7
NUMBER 30 25
FIGURE 4-9.?Photomicrographs of L3 chondrites: a, ALH84120; b, ALH84205; c, LEW86018; d, LEW86127.
Abundant chondrules, chondrule fragments, and mineral grains are visible in the photos; only a little matrix is
actually present in any of these three meteorites, the dark regions in fact being mostly limonite weathering. Width
of field in each photo is 2.3 mm.
mm across. In thin section, chondrules and chondrule frag-
ments up to 2.1 mm across are closely-packed in a minimum
amount of dark matrix that contains some troilite and a little
nickel-iron. A variety of chondrule types is present, including
granular and porphyritic olivine and olivine-pyroxene, barred
olivine, and fine-grained radiating pyroxene. Considerable
weathering is indicated by brown limonitic staining throughout
the section. Microprobe analyses show olivine and pyroxene of
variable composition: olivine, Faj_30, with a mean of Fa14 (c.v.
FeO is 59); pyroxene, Fs3_13. The meteorite is classified as an
L3 chondrite (estimated L3.4).
LEW85396 (60.2 g), 85401 (3.9 g), 86018 (502.0 g), 86022
(351.7 g).?These stones are very similar and are possibly
paired. They all retain some fusion crust, but are extensively
weathered. Interiors are brown and show numerous chondrules
and inclusions up to 5 mm long. Thin sections show a
close-packed mass of chondrules (up to 2.9 mm across),
chondrule fragments, and irregular granular aggregates in a
small amount of opaque matrix which includes minor amounts
of nickel-iron and troilite. Most chondrules consist of granular
or porphyritic olivine, some with polysynthetically-twinned
clinopyroxene. Both olivine and pyroxene show a wide range
in composition: olivine, Fa^^; pyroxene, Fsj_31. The meteor-
ites are classified as L3.5 chondrites.
LEW85434 (19.4 g), 85437 (9.4 g).?Both specimens have
red-brown interiors covered with weathered fusion crust. Light
colored chondrules are visible in LEW85437.
Thin section examination shows that these two specimens
are very similar and probably paired. Chondrules and chon-
drule fragments, up to 1.8 mm across, are closely-packed in a
26 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
small amount of dark matrix containing a little troilite and
nickel-iron. Chondrule types include granular and porphyritic
olivine and olivine-pyroxene, barred olivine, and fine-grained
radiating pyroxene. Weathering is extensive, with brown
limonitic staining pervading the sections. Olivine and pyroxene
show a wide range in composition: olivine, Faj_23 with a mean
of Fa10 (c.v. FeO is 76); pyroxene, Fs2_n. The meteorite is
classed as an L3 chondrite (estimated L3.4).
LEW85452 (9.2 g).?Black fusion crust completely covers
LEW85452. Macroscopically, the interior structure has been
obscured by oxidation. The section shows a close-packed
aggregate of chondrules and chondrule fragments, up to 2.4
mm across, in a finely granular matrix containing some troilite
and nickel-iron. Chondrule types include granular and porphy-
ritic olivine and olivine-pyroxene, and fine-grained to cryptoc-
rystalline pyroxene. Olivine and pyroxene show a wide range in
composition: olivine, Fa5_23 with a mean of Fa15 (c.v. FeO is
35); pyroxene, Fs2_18. The meteorite is classed as an L3
chondrite (estimated L3.6).
LEW86021 (325.8 g).?This rounded stone is mostly
covered with iridescent fusion crust; evaporite deposit is
present on some surfaces. The interior is red-brown and heavily
weathered. A section shows a close-packed mass of chondrules
(up to 2.7 mm across), chondrule fragments, and irregular
crystalline aggregates, together with minor amounts of nickel-
iron and troilite. A variety of chondrule types is present,
including granular and porphyritic olivine and olivine-
pyroxene, barred olivine, and radiating pyroxene. Weathering
is extensive, with limonitic staining and areas of brown
limonite throughout. Microprobe analyses give the following
compositions: olivine, Fa18_28, mean Fa^ (c.v. FeO is 10);
pyroxene, Fs4_17. The meteorite is classified as an L3.9
chondrite.
LEW86127, 86134, 86144, 86158, 86207, 86246, 86270,
86307, 86367, 86408, 86417, 86436, 86505 (total weight 150.9
g).?All these small stones show light and dark chondrules and
angular fragments in a darker, very coherent matrix. They are
very similar in all respects and may be paired. Sections show a
close-packed aggregate of chondrules and chondrule frag-
ments, up to 3 mm across, in a minimum amount of
fine-grained dark matrix that contains a little nickel-iron and
troilite. Chondrule types include granular and porphyritic
olivine and olivine-pyroxene, barred olivine, and radiating and
cryptocrystalline pyroxene. Weathering is extensive, with
brown limonitic staining throughout. Composition ranges are:
olivine, Faj_30; pyroxene, Fsj_24. The meteorites are classified
as L3.5 chondrites.
LEW86549 (50.1 g).?A gray interior is overlain by a black
polygonally-fractured fusion crust that covers about 50% of the
surface of this specimen. The section consists mainly of
chondrules and chondrule fragments, with a minor amount of
dark finely-granular matrix containing a little nickel-iron and
troilite. The chondrules are relatively small, the largest found
being 0.9 mm across; most are granular olivine and olivine-
pyroxene, but barred olivine and radiating pyroxene chondrules
are also present. Weathering is extensive, with brown limonitic
staining throughout the section. Olivine and pyroxene are
variable in composition: olivine, Fa5_20, with a mean of Fa15
(c.v. FeO is 28); pyroxene, Fsj_29. This meteorite is classified
as an L3 chondrite (estimated L3.7).
RKP86700 (424.1 g).?Brown fusion crust spotted with
oxidation halos covers 90% of this stone. The interior is dark
gray with black inclusions up to 2 mm across; oxidation is
heavy along fractures. A thin section shows a close-packed
mass of chondrules (0.6-2.4 mm across) and irregular
aggregates. Some chondrules have dark rims consisting largely
of fine-grained troilite. The sparse matrix is fine-grained, with
a small amount of coarser nickel-iron and troilite scattered
throughout. A notable variety of chondrule types is present;
many are granular or porphyritic olivine and olivine-pyroxene
with transparent to turbid interstitial glass. The pyroxene is
polysynthetically-twinned clinobronzite. Brown limonitic
staining pervades the section. Composition ranges are as
follows: olivine, Fa17_27, mean Fa^ (c.v. FeO is 9.3); pyroxene,
Fs14_23. The meteorite is an L3 chondrite (estimated L3.9); it
resembles RKPA80256, and may be paired with it.
CLASS LL3
FIGURE 4-10
ALH84086 (234.0 g).?Fusion crust covers most of this
chondrite. Abundant inclusions, both chondrules and clasts
(one 0.7 x 0.9 cm), are present in the medium gray matrix. A
section shows a close-packed aggregate of chondrules, chon-
drule fragments, and irregular inclusions up to 3 mm across,
with a few grains of nickel-iron and sulfide and hardly any
matrix. A considerable variety of chondrules is present, the
commonest being porphyritic or granular olivine with or
without polysynthetically twinned clinobronzite. Some chon-
drules have intergranular transparent pale brown glass; in
others the glass is turbid and partly devitrified. Microprobe
analyses, including data from Rubin (1990), show a moderate
range in olivine composition (Fa25_29) with a mean of Fa^, and
a wider range in pyroxene (Fs17_26). The meteorite was
originally classified as an LL3.9 chondrite; Rubin (1990) has
suggested LL3.8.
ALH84126 (41.2 g).?This fragment retains four small
patches of fusion crust. Numerous chondrules and inclusions
show in relief on the brown weathered surface. A thin section
shows a close-packed aggregate of chondrules, chondrule
fragments, and angular clasts ranging up to 3 mm across. Many
chondrules have dark rims. A variety of chondrule types is
present, including porphyritic olivine, granular olivine and
olivine-pyroxene, and radiating pyroxene. A few grains of
troilite and nickel-iron are present. Mineral compositions are:
olivine, Fa^j, mean Fa16 (c.v. FeO is 46); pyroxene, Fs3_24,
mean Fs9. The meteorite is classified as an LL3.5 chondrite.
NUMBER 30 27
FIGURE 4-10.?Photomicrographs of LL3 chondrites: a, ALH84126; b,
ALH84086. Numerous chondrules, chondrule fragments, and mineral grains
are visible in very sparse dark matrices. Much of what appears to be dark matrix
in ALH84126 is actually limonite staining. Opaque (iron-nickel metal and
troilite) grains are visible in the photo of ALH84086. Width of field in each
photo is 2.3 mm.
Achondrites
BRACHINA-LIKE AND UNGROUPED
FIGURE 4-11
ALH 84025 (4.6 g).?This small meteorite is largely covered
with thick fusion crust. In composition it is essentially a dunite,
consisting of large (up to 1.5 mm) polygonal olivine crystals
that are uniformly Fo67_68 in composition, with lesser diopside
(Wo44En46) and sparse polygonal chromite grains. Criss-
crossing the meteorite are veins of troilite, within which are
tiny globules of Ni-rich (about 30% Ni) metal. In many cases
these sulfide veins are no more than trails of tiny sulfide grains
that outline crystal boundaries and define (presumably) healed
fractures within crystals. Only the larger and more continuous
veins contain metal. Neither the olivine nor the pyroxene show
significant undulatory extinction. A well-defined fusion crust,
0.6 mm thick, encloses much of the area of the thin section,
reflecting the small overall size of this meteorite. A very few
fractures show slight limonitic staining, indicating only minor
terrestrial weathering. This specimen most closely resembles
the unique achondrite Brachina in texture and mineralogy, but
unlike Brachina it is more coarsely crystalline and contains no
plagioclase.
Prinz et al. (1986) made a comprehensive study of the
mineralogy of ALH84025 and confirmed its close relationship
to Brachina. Warren and Kallemeyn (1987) compared
ALH84025 to Brachina and Chassigny, noting that in some
respects it bears little resemblance to either. It has far lower
contents of light REE, and also shows a small (barely
significant) positive Eu anomaly, which neither Brachina nor
Chassigny has. They interpret the texture and bulk composition
of this meteorite to reflect an origin as an igneous cumulate. Ott
et al. (1987) have measured the noble gases in ALH84025 and
conclude that it is like Brachina and unlike Chassigny.
ALH84190 (7.9 g).?This small fragment probably fits on a
corner of a larger meteorite that is angular and has an ablation
flange. The section shows an aggregate of anhedral to
subhedral grains, 0.06-0.5 mm across, of olivine and pyrox-
ene, with about 15% of disseminated nickel-iron and minor
amounts of plagioclase and troilite. The proportion of pyroxene
to olivine is estimated as 4:1. Weathering is extensive, with
veinlets and small areas of brown limonite throughout the
section. Microprobe analyses gave the following compositions:
olivine, Fa4; plagioclase, An19; pyroxene, Wo3Fs6 (slightly
variable, with one grain of diopside, Wo43Fs3, analysed). This
ungrouped achondrite is essentially identical with
ALHA81187; in mineral compositions and texture these
meteorites closely resemble inclusions in iron meteorites, such
as in Campo del Cielo (Wlotzka and Jarosewich, 1977).
EET84302 (59.6 g).?The exterior of this specimen is
mostly covered with thin fusion crust. The section shows an
anhedral granular aggregate (grain size 0.1-0.4 mm) consisting
largely of olivine and orthopyroxene, with minor amounts of
plagioclase, diopside, nickel-iron, and troilite. Weathering is
extensive, with limonitic staining throughout the section.
Microprobe analyses gave the following compositions: olivine,
Fa5; orthopyroxene, Wo2Fs8; diopside, Wo42Fs3; plagioclase,
An23.
ANGRITE
FIGURE 4-12
LEW86010 (6.9 g).?Greenish brown crystals are visible in
relief on the polished black exterior surface of this tiny stone;
some flow-like features are also visible. In thin section the rock
28 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
FIGURE 4-11.?Photomicrographs of Brachina-like and ungrouped achon-
drites: a, ALH84025; b, ALH84190; c, EET84302. ALH84025 (Brachina-like)
shows mostly olivine and chromite (opaque). In ALH84190 olivine, pyroxene,
and metal and sulfide (both opaque) are visible in the photo. EET84302
contains olivine, abundant metal and sulfide, pyroxene, plagioclase, and
extensive limonitic staining. Width of field in each photo is 2.3 mm.
consists of a granular aggregate of subequal amounts of
plagioclase, pyroxene, and olivine, with minor amounts of
troilite, whitlockite, hercynite spinel, and rare merrilite. A
striking feature is the strongly zoned, reddish-purple pleo-
chroism of the pyroxene.
The pyroxene is a fassaite, with 10% A12O3 and 2% TiO2.
The olivine is Fa63 in composition and contains l%-3% CaO;
present within the olivines are optically-visible exsolution
lamellae of kirschsteinite. The plagioclase is An100 in composi-
tion.
Correlated studies of the petrologic and trace element
characteristics have been reported by McKay, Lindstrom, Le,
and Yang (1988), McKay, Lindstrom, Yang, and Wagstaff
(1988), and Crozaz and Lundberg (1988); Rb-Sr, Pb-Pb, and Ca
and Ti isotopic properties are reported by Lugmair et al. (1989).
McKay and co-workers conclude that there is little doubt that
LEW86010 is an igneous rock. The trace element studies of
Crozaz and Lundberg (1988) support such a conclusion;
moreover, the lower REE abundances and higher Fe/Mg in
LEW86010 relative to Angra Dos Reis (ADOR) makes it
unlikely that these two rocks are co-magmatic.
Lugmair et al. (1989) found that the initial "Sr/^Sr for
LEW86010 is slightly higher than that of ADOR and slightly
lower than that of the cumulate eucrite, Moore County. The Pb
isotopic composition of LEW86010 proved to be severely
contaminated by modern terrestrial lead; however, measure-
ments on plagioclase yielded model ages of 4.536 b.y. relative
to primordial lead. The aluminous composition of LEW86010
led to a proposal (Prinz et al., 1988) that it might somehow be
related to Ca-Al-rich inclusions such as those found in
carbonaceous chondrites; Lugmair et al. (1989) measured Ca
and Ti isotopic ratios in the angrite and found no anomalies.
On the basis of zoning in the pyroxene and olivine, McKay,
Lindstrom, Le, and Yang (1988) and McKay, Lindstrom, Yang,
and Wagstaff (1988) concluded that LEW86010 cooled more
rapidly than did ADOR.
NUMBER 30 29
FIGURE 4-12.?Photomicrograph of the angrite LEW86010. Plagioclase
(clear), olivine (clear with high relief), fassaitic pyroxene (grey), and sparse
troilite are visible. Width of field is 2.3 mm.
AUBRITES
FIGURE 4-13
ALH84007-84024 (total weight 3.6 kg).?These 18 speci-
mens were collected in the Middle Western Icefield over a
distance of some 6 km. The largest specimen, ALH84007,
weighs 705.6 g. All are fragments, some with minor amounts of
yellowish to black fusion crust, and are almost certainly pieces
of a single meteorite, along with ALH83OO9 and ALH83O15.
Macroscopically they are complex breccias of large white clasts
up to 2 cm across, some dark inclusions up to 5 mm across, and
occasional metal grains with rusty halos. Thin sections show
that the meteorite is made up almost entirely of large (up to ~4
mm) intensely shocked enstatite crystals (essentially pure
MgSiO3; FeO less than 0.2%). The dusty brown matrix consists
of granulated enstatite with minor forsterite (FeO 0.1%),
diopside (Wo41_44En56_59), and plagioclase (Anc,Or3). Diopside
occurs both as independent grains in the matrix and as rounded
inclusions within enstatite. Sparse kamacite grains, up to 3 mm
across, are invariably associated with a complex assemblage of
phases that includes troilite, schreibersite, daubreelite, and
alabandite.
Schwarz et al. (1986) have examined the chemistry of
mineral separates from ALH84007, ALH84008, and
ALH84011. The "enstatite" separates have V-shaped REE
patterns with positive Eu anomalies, and appear fairly uniform
in comparison with previous data on aubrites. Ryder and
Murali (1987) have continued the work on these meteorites,
and find that the REE patterns are influenced by several sulfide
phases, which are the principal carriers of these elements.
Random microprobe analyses of 55 enstatite grains in
ALH84011 give the following: Al203 is fairly uniform, mostly
in the range 0.06%-0.08%; CaO 0.22%-0.30%; FeO variable,
FIGURE 4-13.?Photomicrograph of the aubrite ALH84007. Most of the photo
is occupied by large deformed enstatite crystals, with scattered opaque sulfides.
Width of field is 2.3 mm.
with most less than 0.03%;
0.01%; Cr2O3 less than 0.015%.
and TiO2 both less than
DlOGENITES
FIGURE 4-14
ALH84001 (1930.9 g).?Much of this rectangular shaped
meteorite is covered with dull black fusion crust. Remnants of
flow marks are visible on two surfaces. Areas not covered by
fusion crust have a greenish-gray color and a blocky texture.
Cleavage planes are obvious on some large crystals and the
stone has a shocked appearance. Small areas of oxidation are
present, and small fractures are numerous.
A thin section shows orthopyroxene (Wo3Fs27) crystals up to
5 mm long forming a polygonal-granular mosaic. Despite the
fact that the pyroxene contains 1.5% CaO, no exsolution
lamellae were observed. Veins of intensely granulated pyrox-
ene cross cut the section. Other minerals include minor
chromite and irregular patches of maskelynite (An35_390r34).
The section does not show iron-oxide staining but does contain
patches of brown Fe-rich carbonate, (Fe29Mg6OCau)CO3.
Although this diogenite contains granulated areas, it does not
appear to be a breccia.
ALH85015 (3.2 g).?This small fragment is partly covered
with black fusion crust, shiny in some places and dull in others.
Part of the area devoid of fusion crust is highly polished. A
weathering rind extends 2 mm into the interior, which is
medium gray in color with white and dark clasts. The thin
section consists almost entirely of orthopyroxene clasts, up to
3 mm across, in a groundmass of comminuted orthopyroxene,
accessory plagioclase and opaques, and traces of olivine. The
pyroxene is fairly uniform in composition, Fs25, with CaO
0.8%-1.5%, MnO 0.45%-0.67%, Al203 0.32%-0.66%, and
30 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
FIGURE 4-14.?Photomicrographs of diogenites: a, ALH84001. The photo
shows the largely undeformed character of this meteorite, except for some
narrow granulated zones crossing the section. Clear maskelynite and opaque
chromite are accessory to the predominant orthopyroxene. b, ALH85015. In
contrast with ALH84001, this meteorite is highly brecciated. Orthopyroxene-
rich clasts are prominent in a comminuted matrix of pyroxene, plagioclase,
minor olivine, and opaques. Width of field in each photo is 1 cm.
TiO2 0.05%-0.17%. The plagioclase composition is An84_95.
One grain of olivine, Fa39, was analysed.
EUCRITES
FIGURE 4-15
ALH85OO1 (212.3 g).?This meteorite is an oriented stone
covered by a shiny black fusion crust with thick flow lines.
Areas devoid of fusion crust have weathered to a brownish-gray
color. A discontinuous weathering rind, up to 4 mm thick, was
exposed when the stone was chipped. The interior is made up
of abundant laths of chalky plagioclase in a light gray matrix.
The thin section shows angular fragments of orthopyroxene
and plagioclase, up to 2.4 mm across, in a comminuted
groundmass of these minerals. Some of the pyroxene has
lamellae and blebs of exsolved augite. A large gabbroic clast, 6
mm across with individual grains up to 3 mm, was found in one
section. Trace amounts of nickel-iron and troilite are present in
the groundmass. Microprobe analyses show that pyroxene
compositions are remarkably uniform, Wo2Fs32, with a few
more calcic grains, up to Wo8 (possibly incipient augite
exsolution). Plagioclase composition is also fairly uniform,
An92_94. The meteorite is a monomict eucrite with unusually
magnesian pyroxene, similar to that in the Binda eucrite.
Mittlefehldt and Lindstrom (1988) have provided REE data
on this meteorite.
LEW853OO (210.3 g), 85302 (114.5 g), 85303 (408.0
g).?These three specimens of a complex polymict eucrite are
clearly paired. Thin shiny fusion crust with flow marks coat
most of the top of LEW853OO; the bottom surface has some
fusion crust but most of this face is a fracture surface which
appears to have been moderately polished. Fusion crust appears
as dull patches on LEW85302 and LEW85303. Several large
semi-rounded polymineralic clasts (as large as 2 x 2 cm) have
sharply defined edges and are set in a black matrix.
Thin sections show numerous clasts with diverse textures
and mineralogy set in a dark matrix with numerous commi-
nuted grains of pyroxene and plagioclase. Some clasts have
gabbroic or basaltic textures, others are breccias, and one is
identified as a C3 chondrite. Microprobe analyses of section
LEW85300,14 give pyroxene compositions clustering around
Wo-jFs^, ranging to Wo43Fs26, with a mean (n = 15) of
Wo12Fs52; two grains were found having the composition
Wo3Fs33. The plagioclase composition is Ang4_93.
The C3 chondrite clast consists largely of fine-grained
olivine, with a composition of Faj^; one grain each of
clinoenstatite (Fs59) and spinel (FeO 0.8%) were found.
A detailed account of clasts in these meteorites has been
provided by Kozul and Hewins (1988). Mittlefehldt and
Lindstrom (1988) have provided REE and other trace element
data on some clasts from these meteorites.
LEW85305 (40.8 g).?This cuboidal stone is completely
covered with shiny fusion crust showing flow lines. It has been
described in detail by Delaney (1987), as follows: "Lewis Cliff
85305 is a granular fine grained eucrite ... containing pigeonite
and augite with homogeneous plagioclase (An8890r063) in
roughly equal proportions. A SiO2 polymorph is the most
abundant minor phase with troilite, metal and intimately
intergrown ilmenite and Ti-bearing chromite. The pyroxene has
a relict subophitic texture with a grain size of about 500-1000
(im, but the present pyroxene is very fine grained equant grains
(50-100 (im) developed by granulation and recrystallizion of
the earlier texture. Plagioclase does not show the same
comminution effects. Both the augite and the pigeonite have
well-defined exsolution lamellae and are unzoned. Unlike that
in most eucrites, the plagioclase in 85305 ... is also unzoned.
The SiO2 mineral in 85305 occurs in a distinctive textural
NUMBER 30 31
FIGURE 4-15.?Photomicrographs of eucrites: a, ALH85OO1. The photo shows a large gabbroic clast (upper left)
enclosed in a granulated matrix of pyroxene (grey) and feldspar (light), b, LEW86001. The photo shows
diverse-textured clasts in a granulated matrix, c, LEW85300. The photo shows several clast types enclosed in the
dark granulated matrix, d, LEW853O5. Fine- to coarse-grained pyroxene (grey) and plagioclase are prominent in
the photo of this unbrecciated eucrite. Width of field in a is 1 cm; in all others, 2.3 mm.
setting as fairly large poikilitic grains with abundant small
inclusions of both pyroxenes and tends to form secondary veins
or "pools" through the thin section."
In its texture and the lack of compositional zoning in its
constituent phases, LEW85305 resembles the Ibitira eucrite
(Steele and Smith, 1976); however, the mineral compositions
are different.
Mittlefehldt and Lindstrom (1988) report that this meteorite
has a relatively flat REE distribution pattern at about 7-9 x
ordinary chondrites.
LEW85353 (24.5 g).?This small stone has retained most of
its thin fusion crust. Weathering has removed some crust and
left a pitted surface. The interior is light gray and has a basaltic
texture. A thin section shows a fine-grained aggregate (grains
0.1-0.4 mm) of pale brown pyroxene and colorless plagio-
clase, with a few opaque grains. Minor weathering is indicated
by brown limonitic staining around the opaques. Plagioclase is
fairly uniform in composition, averaging An88. Pyroxene is
largely hypersthene with a mean composition of WbjFsgQ;
accessory augite (Wo48Fs22) has exsolution lamellae of
hypersthene.
LEW86001 (290.6 g).?Dull black fusion crust covers 80%
of this stone. Large vugs, typical of Antarctic eucrites, are
abundant. Interior surfaces have a light gray color and show
numerous clasts up to 0.5 cm across; some oxidation is present.
A thin section shows a groundmass of comminuted pyroxene
and plagioclase (grains up to 0.5 mm), with numerous clasts up
to 3 mm. The clasts consist of pyroxene and plagioclase, with
32 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
a variety of textures from fine-grained granular to ophitic to
gabbroic. A small amount of opaques is present. Microprobe
analyses show pyroxene compositions clustered around
Wo2Fs56 but ranging to Wo44Fs22, with a fairly uniform En
content. The plagioclase composition is An7688.
Mittlefehldt and Lindstrom (1988) report that this meteorite
is relatively enriched in REE (10-20x ordinary chondrites),
and shows a LREE enriched pattern with a negative Eu
anomaly.
LEW86002 (32.6 g).?This oblong stone is mostly covered
with thin black fusion crust. Thin section examination reveals
an ophitic intergrowth of pyroxene and plagioclase (plagioclase
laths up to 0.7 mm long). Pyroxene ranges in composition from
Wo3Fs61 to Wo37Fs31, with fairly uniform En content. The
plagioclase composition is An^.
LEW86003 (1.6 g).?This small stone is mostly covered
with dull black fusion crust. Ninety percent of the interior is
light gray in color with minor black inclusions; the remainder
is jet black with minor inclusions and is more oxidized than the
lighter material. The contact between the two areas is sharp.
Most of the thin section is an ophitic intergrowth of pyroxene
and plagioclase, the plagioclase laths being up to 0.9 mm long.
One end of the section is sharply bounded by an area of
subophitic to gabbroic clasts, up to 1.8 mm across, in a dark
brown glassy matrix. Mineral compositions are similar
throughout. Pyroxene compositions range from WojFs^ to
Wo43Fs27, with fairly uniform En contents. Plagioclase
compositions are An87 91.
HOWARDITES
FIGURE 4-16
LEW85313 (191.2 g).?Dull fusion crust covers most of this
meteorite except where large pieces have been plucked out,
giving the appearance of a piece of Swiss cheese. A
brownish-gray weathering rind extends from less than 1 mm to
greater than 1 cm into the interior. The massive gray matrix
contains rounded and irregular inclusions ranging in color from
white to black. Some oxidation halos are present. This
meteorite was originally classified as a diogenite on the basis of
a non-representative section (LEW85313,5), which was a large
orthopyroxene clast. Berkley (1988) has shown that it is
actually a howardite. It is a microbreccia of pyroxene clasts
(orthopyroxene with minor clinopyroxene) and eucrite clasts,
up to 0.9 mm across, in a comminuted groundmass of pyroxene
grains, with minor plagioclase and accessory opaques (troilite
and nickel-iron). Microprobe analyses give the following
pyroxene composition range: Wo1_10Fs15_64En34_85, with a
mean of Wo8Fs33 (one grain of ferroaugite, Wo37Fs38, was
analyzed). The plagioclase composition range is An7894. Two
grains of a silica polymorph, probably tridymite, were found
during reconnaiscance examination.
LEW85441 (10.9 g).?Half of the surface of this meteorite is
FIGURE 4-16.?Photomicrographs of howardites: a, LEW85441; b,
LEW85313. Both photographs show heterogeneous aggregates of basaltic,
gabbroic, and diogenetic clasts in comminuted matrices. Width of field in each
photo is 2.3 mm.
covered with dull frothy fusion crust. Areas devoid of fusion
crust are brownish-gray and show numerous clasts. Some
oxidation halos are present. The section has a cataclastic
texture, with angular fragments of pyroxene and plagioclase up
to 2 mm across in a comminuted groundmass of the same
minerals. The pyroxene is mainly hypersthene, but ranges
widely in composition: Wo1_10Fs25_48En34_74, with a mean of
Wo3Fs28. Plagioclase composition is An^.^. This meteorite is
very similar to LEW85313 and is possibly paired with it.
UREILITES
FIGURE 4-17
ALH84136 (83.5 g).?This specimen is entirely covered
with flaky black fusion crust. The interior is dark gray and
NUMBER 30 33
FIGURE 4-17.?Photomicrographs of ureilites: a, LEW85238. Olivine and
pyroxene crystals are surrounded by dark, mostly carbonaceous material that
also includes minor metal and troilite. b, LEW86216. The rounded olivine
clasts have been transformed into fine-grained olivine mosaics, enclosed in a
dark granulated matrix. Width of field in each photo is 2.3 mm.
granular with crystals as large as 2 mm in a red-brown matrix.
A thin section shows an aggregate of anhedral to subhedral
grains (0.6-2.4 mm across) of olivine and pyroxene, with
about 10% of opaque material, in part disseminated throughout
and in part concentrated along grain boundaries. Olivine grains
are gray due to submicroscopic opaque inclusions, whereas
pyroxene grains are clear but are extremely fractured. Micro-
probe analyses give the following compositions: olivine,
somewhat variable, FaQ_5, mean Fa3; pyroxene, essentially
uniform, Wo5Fs3; one grain of endiopside, Wo34Fs25, was
analysed. This meteorite is so similar in all respects to
ALH82106 and ALH82130 that it can be confidently paired
with them; they were all found within 2-3 km of each other on
the Allan Hills Far Western Icefield. This pairing is also
supported by oxygen isotope data (Clayton and Mayeda, 1988).
LEW85328 (106.8 g).?The meteorite is covered by black
fusion crust, frothy in places and with well-defined ablation
marks. A thin section shows an aggregate of anhedral to
subhedral grains (0.3-2.4 mm across) of olivine and pyroxene,
in the approximate proportions of 2 : 1. Individual grains are
rimmed by carbonaceous material. Trace amounts of finely-
divided nickel-iron and troilite are present, mainly along grain
boundaries. Microprobe analyses indicate that the olivine is
uniform in composition, (Fa20), with notably high CaO content
(0.3%). The pyroxene is pigeonite with a composition of
Wo9Fs17. This meteorite is notably unshocked compared to
most ureilites.
LEW85440 (43.8 g).?Thin black fusion crust with green-
ish-gray streaks cover 60% of this stone. A thin section shows
an equigranular aggregate of rounded to subhedral olivine and
pyroxene grains, 0.3-0.6 mm across. The grains are rimmed
with black carbonaceous material, which also contains trace
amounts of nickel-iron (partly weathered to brown limonite)
and troilite. Microprobe analyses show olivine and pyroxene of
uniform composition: olivine Fag (CaO 0.3%); pyroxene,
Wo5Fs8. Takeda et al. (1988) have made a detailed study of this
meteorite and report one grain of augite, Wo36Fs5. Clayton and
Mayeda (1988) have determined the oxygen isotopic composi-
tion.
LEW86216 (6.5 g).?This small stone has black frothy
fusion crust on most surfaces. It is extremely weathered, and
much of the thin section is obscured by brown limonite. It
shows rounded olivine grains, up to 3 mm across, in a
finer-grained, probably comminuted matrix of olivine with
minor pyroxene. The probable presence of accessory diamond
is indicated by difficulties in cutting and polishing, and by
brightly fluorescent particles in an electron beam. The
meteorite is heavily shocked, the large olivines being converted
into a mosaic of tiny grains averaging 0.05 mm across.
Microprobe analyses show an olivine composition range of
Fa12_18, with a mean of Fa17 (CaO 0.2%-0.4%); pyroxene
compositions are in the range Wo^oFsj^g.
MESOSIDERITES
FIGURE 4-18
LEW86210 (9.2 g).?This is a reddish-brown weathered
pebble with a high content of metal. Thin section examination
reveals a granular aggregate of about 50% nickel-iron and 50%
silicates. Pyroxene is the predominant silicate, with lesser
amounts of plagioclase, as clastic grains up to 1.5 mm in
maximum dimension in a matrix of metal and comminuted
silicates. Minor weathering is indicated by small areas of brown
limonite. Microprobe analyses show pyroxene in the composi-
tion range Wo2_8Fs24_61; most grains are Fs24_31, with a mean
of Wo4Fs29. The plagioclase composition is An8992. One grain
of olivine, Fa45, was analysed.
QUE86900 (1532.3 g).?This meteorite, from the Queen
34
FIGURE 4-18.?Photomicrographs of mesosiderites: a, LEW86210; b,
QUE86900. Both photographs show clasts of orthopyroxene and plagioclase
enclosed in metal matrices. The metal in QUE86900 is heavily weathered.
Width of field in each photo is 2.3 mm.
Alexandra Range, has isolated blebs of dull black fusion crust
on about 10% of the surface, the remainder being weathered
red-brown. Shallow regmaglypts are present. Large green platy
pyroxene crystals are abundant, the largest being 1.5 cm long.
Cleaving the stone revealed an interior with numerous platy
and dark rounded inclusions in a highly weathered, red-brown,
metal-rich matrix. A thin section shows plagioclase and
pyroxene clasts, up to 1.5 mm across, in an opaque matrix of
nickel-iron and troilite; the nickel-iron is extensively weathered
to limonite. Most of the pyroxene is hypersthene, but some
pigeonite is present; the composition ranges are
Wo1_]1Fs21_64En31_78, with a mean of Wo3Fs33. Most plagio-
clase compositions are in the range An9096, but a few more
sodic grains were analysed.
Mittlefehldt (1988) has measured the REE distribution in a
gabbroic clast from this meteorite.
SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
Literature Cited
Berkeley J.L.
1988. LEW85313 Howardite: Clues to the Diogenite-Cumulate Eucrite
Connection? In Lunar and Planetary Science XIX, pages 63-64.
Houston: The Lunar and Planetary Institute.
Clayton, R.N., and T.K. Mayeda
1988. Ureilites Are Not Igneous Differentiates. In Lunar and Planetary
Science XIX, pages 197-198. Houston: The Lunar and Planetary
Institute.
Crozaz, G., and L. Lundberg
1988. Rare Earth Elements (REE) in the Unique Achondrite LEW86010.
In Lunar and Planetary Science XIX, pages 231-232. Houston: The
Lunar and Planetary Institute.
Delaney, J.S.
1987. The Lewis Cliff 85305 Eucrite, and Shock Effects in Eucrites.
Meteoritics, 22:365-366.
Gibson, E.K.
1987. Carbon and Sulfur Abundances in Antarctic Meteorites. Meteoritics,
22:384-385.
Grady, M.M., and C.T. Pillinger
1989. Nitrogen and Carbon in ALH85085?Links with Bencubbin? In
Lunar and Planetary Science XX, pages 351-352. Houston: The
Lunar and Planetary Institute.
Grossman, J.N., A.E. Rubin, and G.J. MacPherson
1988. ALH85085: A Unique Volatile-poor Carbonaceous Chondrite with
Possible Implications for Nebular Fractionation Processes. Earth
and Planetary Science Letters, 91:33-54.
Kallemeyn, G.W., A.E. Rubin, and J.T. Wasson
1991. The Compositional Classification of Chondrites, V: The Karoonda
(CK) Group of Carbonaceous Chondrites. Geochimica et Cosmo -
chimica Ada, 55:881-892.
Kozul, J., and R.H. Hewins
1988. LEW853OO, 02, 03 Polymict Eucrite Consortium. In Lunar and
Planetary Science XIX, pages 645-648. Houston: The Lunar and
Planetary Institute.
Lugmair, G.W., S.J.G. Galer, and R. Loss
1989. Rb-Sr and other Isotopic Studies of the Angrite LEW86010. In
Lunar and Planetary Science XX, pages 604-605. Houston: The
Lunar and Planetary Institute.
McKay, G., D. Lindstrom, L. Le, and S.-R. Yang
1988. Experimental Studies of Synthetic LEW86010 Analogs: Petrogene-
sis of a Unique Achondrite. In Lunar and Planetary Science XIX,
pages 760-761. Houston: The Lunar and Planetary Institute.
McKay, G., D. Lindstrom, S.-R. Yang, and J. Wagstaff
1988. Petrology of Unique Achondrite Lewis Cliff 86010. In Lunar and
Planetary Science XIX, pages 762-763. Houston: The Lunar and
Planetary Institute.
McSween, H.Y.
1987. Aqueous Alteration in Carbonaceous Chondrites: Mass Balance
Constraints on Matrix Mineralogy. Geochimica et Cosmochimica
Ada, 51:2469-2477.
Mittlefehldt, D.W.
1988. Petrogenesis of the Mesosiderite Regolith. In Lunar and Planetary
Science XIX, pages 788-789. Houston: The Lunar and Planetary
Institute.
Mittlefehldt, D.W., and M.M. Lindstrom
1988. Geochemistry of Diverse Lithologies in Antarctic Eucrites. In Lunar
and Planetary Science XIX, pages 790-791. Houston: The Lunar
and Planetary Institute.
Ott, U., H.P. Lohr, and F. Begemann
1987. Noble Gases in ALH84025: Like Brachina, Unlike Chassigny.
Meteoritics, 22:476-477.
NUMBER 30 35
Prinz, M., M.K. Weisberg, and C.E. Nehru
1988. LEW86010, a Second Angrite: Relationship to CAI's and Opaque
Matrix. In Lunar and Planetary Science XIX, pages 949-950.
Houston: The Lunar and Planetary Institute.
Prinz, M., M.K. Weisberg, C.E. Nehru, and J.S. Delaney
1986. A Second Brachina-like Meteorite. In Lunar and Planetary Science
XVII, pages 679-680. Houston: The Lunar and Planetary Institute.
Rubin, A.E.
1990. Kamacite and Olivine in Ordinary Chondrites: Intergroup and
Intragroup Relationships. Geochimica et Cosmochimica Ada,
54:1217-1232.
Rubin, A.E., and G.W. Kallemeyn
1989. Carlisle Lakes and Allan Hills 85151: Members of a New Chondrite
Grouplet. Geochimica et Cosmochimica Ada, 53:3035-3044.
1990. Lewis Cliff 85332: A Unique Carbonaceous Chondrite. Meteoritics,
25:215-225.
Ryder, G., and A.V. Murali
1987. Mineralogy and Chemistry of Antarctic Aubrites. Meteoritics,
22:495-496.
Schwarz, C, G. Ryder, and A.V. Murali
1986. Chemistry of Mineral Separates from Three Antarctic Aubrites from
Allan Hills. Meteoritics, 21:507.
Scott, E.R.D.
1988. A New Kind of Primitive Chondrite, Allan Hills 85085. Earth and
Planetary Science Letters, 91:1-18.
Steele, I.M., and J.V. Smith
1976. Mineralogy of the Ibitira Eucrite and Comparison with Other
Eucrites and Lunar Samples. Earth and Planetary Science Letters,
33:67-78.
Takeda, H., H. Mori, and H. Ogata
1988. Mineralogy of Magnesian and Calcic Groups and Formation
Conditions of Ureilites. In Lunar and Planetary Science XIX, pages
1173-1174. Houston: The Lunar and Planetary Institute.
Van Schmus, W.R., and J.A. Wood
1967. A Chemical-Petrologic Classification for the Chondritic Meteorites.
Geochimica et Cosmochimica Ada, 31:747-765.
Warren, P.H., and G.W. Kallemeyn
1987. A Trio of Meteoritic Dunites, and New Data for Shergotty. In Lunar
and Planetary Science XVIII, pages 1056-1057. Houston: The
Lunar and Planetary Institute.
Wasson, J.T., and G.W. Kallemeyn
1990. Allan Hills 85085: A Subchondritic Meteorite of Mixed Nebular and
Regolithic Heritage. Earth and Planetary Science Letters, 101:
148-161.
Weisberg, M.K., M. Prinz, and C.E. Nehru
1988. Petrology of ALH85085: A Chondrite with Unique Properties. Earth
and Planetary Science Letters, 91:19-32.
Weisberg, M.K., M. Prinz, C.E. Nehru, R.N. Clayton, and T.K. Mayeda
1989. ALH85151 and Carlisle Lakes 001: Members of a New Chondrite
Group. In Lunar and Planetary Science XX, pages 1191-1192.
Houston: The Lunar and Planetary Institute.
Wlotzka, F., and E. Jarosewich
1977. Mineralogical and Chemical Compositions of Silicate Inclusions in
the El Taco, Campo del Cielo, Iron Meteorite. In B. Mason, editor,
Mineral Science Investigations, 1974-1975. Smithsonian Contribu-
tions to the Earth Sciences, 19:104-125.
5. Descriptions of Iron Meteorites
Roy S. Clarke, Jr.
This section provides brief descriptions of four octahedrites,
a group IAB silicate-rich specimen, and three anomalous
meteorites. The descriptions are based on material prepared
previously for the Antarctic Meteorite Newsletter and on
recently published data. The specimens considered are listed
with their weights and classifications in Table 5-1.
Octahedrites
ALH84165 (94.7 g).?This is an aerodynamically shaped
specimen (4.3 x 3.3 x 1.5 cm) from the Allan Hills (Figure 5-1).
Distinct anterior and posterior surfaces are present, both
covered with thin coatings of reddish brown secondary iron
oxides. The anterior surface is smoother than the posterior and
has a uniform radius of curvature over most of its area. The
posterior radius of curvature is uniform and larger than that of
the anterior surface. The anterior radius does, however,
decrease markedly approaching the join of the two surfaces.
Anterior surface ablation-melt has accumulated on the posterior
side of the join, resulting in an approximately 1 mm flange
around the specimen (Figure 5-1, bottom). Delicate streamers
of fusion crust remain on the edges of the anterior surface
recording the flow of melt away from the stagnation point at the
center the surface. The axis of oriented flight was perpendicular
to the surface as shown in Figure 5-1, top, at the stagnation
point.
A median slice perpendicular to both the plane of the flange
and the long axis of the specimen was taken to the left of the
Roy S. Clarke, Jr., Department of Mineral Sciences, National Museum
of Natural History, Smithsonian Institution, Washington, D.C. 20560.
small depression in Figure 5-1, bottom, providing an area of
approximately 3 cm2 for metallographic examination. The
anterior edge of the slice is essentially free of fusion crust, but
a heat-altered zone of kamacite transformed to o^ penetrates 1.5
to 2 mm into the body of the specimen. The posterior edge has
a continuous fusion crust accumulation 0.2 to 0.3 mm thick,
and the kamacite along this edge has also been penetrated to a
depth of 1.5 to 2 mm by o^ structure. At the flange
intersections, fusion crust accumulation is as thick as 1.5 mm.
Taenite lamellae, taenite-plessite areas, and cellular plessite
areas are present in a well developed Widmanstatten pattern.
The few opportunities for band width measurements suggest a
value of about 1 mm, and the bulk Ni value is 7.76 wt%
(Jarosewich, 1990). Grain boundary schreibersite is present, as
is schreibersite associated with taenite. Kamacite is mottled and
contains a pronounced e-structure and occasional remnant
Neumann bands. These observations suggest a chemical Group
IIIAB classification, as has been established by Wasson et al.
(1989).
GRO85201 (1401 g).?This specimen (13 x 8 x 3.5 cm)
from Grosvenor Mountains was even more dramatically shaped
by aerodynamic forces than ALH84165. It is roughly the shape
and size of an extended and slightly curved adult human hand
with closed fingers and thumb (Figure 5-2). The convex surface
was the anterior surface during stable oriented flight (Figure
5-2, top). A distinct stagnation point may be seen in the center
of this surface, from which streamers of melt flowed to a
circumferential lip that separates the anterior and posterior
surfaces (Figure 5-2, bottom). The anterior surface is dark and
has a reddish cast due to terrestrial oxidation. There are distinct
patches of black fusion crust and areas of bare, shiny metal
37
38 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
FIGURE 5-1.?ALH84165 is an aerodynamically shaped individual covered with a thin coating of secondary iron
oxides. (Top) Looking down on the anterior surface. The plane of the photograph is perpendicular to the
orientation of the individual during atmospheric passage. The long axis is 4.3 cm. (Bottom) Specimen rotated 180?
around the long axis and photographed from an oblique angle to show the accumulation of fusion crust forming
the flange separating anterior and posterior surfaces.
NUMBER 30 39
FIGURE 5-2.?GRO85201 is an unusually well preserved oriented individual. (Top) Looking down on the anterior
surface. The plane of the photograph is perpendicular to the orientation of the individual during stable
atmospheric flight. The stagnation point is in the center of the photograph. It is from this point that delicate
streamers of melt flowed radially to the edge of the surface. The long axis is 13 cm. (Bottom) Specimen rotated
about 60? around the long axis in (Top), showing the posterior surface and the accumulation of melt at the edge
of the anterior surface.
40 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE 5-1.?Antarctic iron meteorites, 1984-1986.
Sample
number
ALH84165
GRO85201
EET84300
LEW86220
LEW86540
ALH84233
LEW85369
LEW86211
Weight
(g)
94.7
1401
72.7
25.0
21.0
13.6
6.3
163
Classification
IIIAB, Om
IIIAB, Om
IAB, Off
Silicate-rich IAB
IIICD, Off
Ungr, Anom
Ungr, Anom
Ungr, Sulfide-rich
associated with the metal streamers. The posterior surface is
darker, also has a slight reddish cast, and has a uniform matte
appearance. The specimen appears to have had a long terrestrial
residence, but its delicate ablation-produced markings are
remarkably well preserved.
A slice, perpendicular to both the surface illustrated in Figure
5-2, top, and the long axis of the specimen, was removed
approximately one-third of the way from the small end,
yielding an 11 cm2 surface for examination. A regular
Widmanstatten pattern with kamacite band widths of 0.8 to 1.5
mm is present. Plessite areas and centers of taenite bands have
a martensitic structure. Grain boundary schreibersite and
occasional large rhabdites are present. Weathering has pene-
trated into the interior along grain boundaries. The anterior
edge has a rim of terrestrial oxide generally less than 0.1 mm
thick and containing a few areas of remnant fusion crust. The
posterior edge is uniformly covered with layered and slightly
weathered fusion crust 1.0 to 1.5 mm thick. Interior to both
edges is an o^ structure typical of heat-altered zones. This 02
structure blends into a much coarser martensite structure that is
present throughout the kamacite in the section. These observa-
tions, combined with a bulk Ni value of 8.59 wt% (Jarosewich,
1990), suggest that the specimen is cosmically heat-altered and
a member of group IIIAB as has been established by Wasson
(1990).
EET84300 (72.7 g).?This irregularly shaped specimen (3.5
x 3 x 2 cm) from Elephant Moraine is severely weathered and
is covered with a reddish brown coating of secondary oxides
containing small amounts of adhering soil material. After the
internal structure of the meteorite had been examined, it was
realized that surface silicates on one part of the surface are
meteoritic and not terrestrial silicates.
An off-center section through the specimen provided an area
of 4 cm2 for metallographic examination. About two-thirds of
this area is uninterrupted metal, while the remaining one-third
contains silicate clusters and individual silicate crystals
dispersed in metal. These silicate associations comprise about
5% of the total area. The metal is polycrystalline, containing
three cm-size areas of finest octahedrite structure with band
widths around 0.1 mm. These three large areas are separated by
two comparatively thin bands of kamacite containing median
grain boundary schreibersite. The silicate-rich areas are more
complex and contain smaller areas of finest octahedrite
structure. The slice is rimmed with an essentially continuous
band of secondary oxides about 0.2 mm thick. A few small
metal areas near the rim contain 0^ structure, its deepest
penetration being less than 0.5 mm.
Dominant features within the metal areas are a Widman-
statten pattern of taenite, cellular plessite, and kamacite
lamellae. Schreibersite is found at junctions of kamacite
lamellae, at centers of kamacite lamellae, and within plessite
areas. A number of graphite inclusions are present, ranging in
size from a few hundredths of a mm to 0.5 mm. Tiny inclusions
of daubreelite were tentatively identified.
Angular silicates occur as clusters of grains and as individual
grains within metal. They range from transparent to translucent,
and from water-clear to slightly colored. Some of the coloring
is probably due to weathering. A 0.5 mm transparent and
slightly green crystal proved on electron microprobe examina-
tion to be diopside. Other silicates identified were plagioclase
(An12), olivine (Fa^, and pyroxene (Fs6). The cluster silicates
are coarsely crystalline and associated with polycrystalline
troilite, small amounts of metal, and schreibersite and/or
cohenite.
This specimen is a silicate- and graphite-rich polycrystalline
finest octahedrite with a bulk Ni value of 9.71 wt%
(Jarosewich, 1990). It belongs to chemical group IAB (Wasson
et al., 1989) and is distinct from IAB meteorite EET83333 on
the basis of both structure and chemical composition (Clarke,
1989; Wasson et al., 1989; Jarosewich, 1990).
LEW86220 (25.0 g).?This weathered, elongated pebble (4
x 1 x 1.5 cm), was described as an iron meteorite with silicate
inclusions by Mason and Martinez (1988). Their macroscopic
description noted that the interior "appears to be coarse-grained
silicate minerals, some green, some yellow?all stained by
oxidation." The microscopic description noted that most
silicate grains are in the 0.3-1.2 mm range, and that they are
olivine and pyroxene with minor plagioclase and limonite
veining. "Microprobe analyses give the following composi-
tions: olivine, Fa^ pyroxene, Wo2Fs9; plagioclase, An15; one
grain of diopside, Wo43Fs4, was analyzed."
Additional information given here is based on low power
microscopic examination of specimen fragments resulting from
section preparation, and on the microscopic examination of a
second polished thin section (LEW86220.2; 0.8 cm2) and a
polished section LEW86220,3; 0.9 cm2).
The exteriors of the fragments are covered with a polished
terrestrial weathering crust of patchy reddish brown to black
material. Positive evidence for melt crust was not found, but
some of the black material appeares to represent the surface
expression of heat-altered silicates. Two small surface areas in
the mm-size range have a jade-green hue, while a third such
surface area was at an edge, revealing both exterior and interior
surfaces. Its interior expression was that of cleavage surfaces of
NUMBER 30 41
coarse, transparent green crystals, undoubtedly the diopside
mentioned above. Approximately 10 such areas were seen on
broken surfaces, one of which was 2.5 mm long. A crude
estimate based on two sawn surfaces and the two polished
section surfaces indicate that 30%-40% of the surface area
consists of irregularly distributed metal.
Polished section and polished thin section examination
revealed no melt crust, but there is a well developed
heat-altered zone. Several areas along silicate edges have
20-50 Jim rims of dendritic magnetite precipitated during the
ablative, high temperature vitrification of the silicates, indicat-
ing that very little material has been lost from this surface.
Sulfide veining and kamacite transformed to otj penetrate
approximately one mm into the specimen. Weathering veins
penetrate into the interior of the specimen, particularly along
the edges of metal areas; and areas of metal transformed to
oxide are prominent near exterior surfaces.
The metal is predominantly kamacite, with occasional well
developed Neumann bands. Several taenite-plessite areas
associated with schreibersite are present within kamacite. On
the basis of optical examination alone, the association observed
is kamacite in contact with a very thin border of "clear taenite
1" (~1 Jim), followed by a region of equal thickness of "cloudy
zone," followed by a comparatively broad area of "clear taenite
2," and finally transformation into a coarse martensite which
occupies most of the area of the structure. This thin border with
kamacite is probably tetrataenite, but the optical anisotropy
needed for confirmation can not be seen on such a thin rim.
Troilite is irregularly distributed, much less abundant than
metal, and mainly occurs as single crystals. Several small
chromites were also recognized.
The information available suggests that this specimen passed
through at least part of the atmosphere as an individual and that
it is a silicate-rich area from a group IAB iron meteorite.
LEW86540 (21.0 g).?This aerodynamically shaped, tektite-
like specimen is a slightly out-of-round (2.2 x 2.4 cm) disk (1.1
cm thick), with a small segment (2-3 mm wide, 2 mm deep)
missing from its edge. Anterior and posterior surfaces intersect
at a sharp edge which undulates only slightly from a plane.
Maximum thickness is approximately at the center of the disk.
The two surfaces are smooth, and they have essentially uniform
radii of curvature, the radius of the anterior surface being 2-3
cm and that of the posterior surface 6-8 cm.
Surfaces are predominantly reddish-brown due to weather-
ing, have small black patches or remnant fusion crust, and have
several patches of iridescent coloring near the edge. Fine
streamers of fusion crust (~0.1 mm) radiate from the stagnation
point at the center of the anterior surface to the edge, with a
very small accumulation of fusion crust at the edge. Indications
of a very fine Widmanstatten pattern stand in relief in several
areas of the posterior surface and can be seen under low
magnification. Wasson (1990) has classified the meteorite as a
finest octahedrite of chemical group IIICD. He reports bulk
values of 18.7 wt% Ni and 0.59 wt% Co.
A slice perpendicular to the plane defined by the edge of the
specimen, and slightly to one side of the center of the disk,
provided a surface area of 2 cm2 for metallographic examina-
tion. The edge of this section corresponding to the anterior
surface has a 10 to 100 |0,m thick rim of terrestrial weathering
products. Remnant fusion crust is present within it and is
partially invaded by terrestrial oxides. On the posterior edge,
similar fusion crust/terrestrial oxide associations extend along
about two-thirds of its length. A layered fusion crust
accumulation 120 |im thick has collected at an intersection of
anterior and posterior surfaces. Throughout the entire section,
kamacite has been heat-altered to o^. Widths of kamacite
lamellae range from 15 to 40 Jim, their lengths being 10 to 100
times their widths. Schreibersites within 800 jim of the anterior
surface have been heat-altered and survive in the form of
quenched eutectic melts. Within 800 Jim of the posterior
surface, both eutectic melts and schreibersites melted at their
edges are observed. Schreibersites are small (in the 50 to 100
jim range), numerous, and found within kamacite lamellae or at
lamellae junctions. A small number of electron microprobe
analyses indicate that schreibersite Ni contents range from 46
to 50 wt%. Taenite-bordered martensitic plessite occupies 60%
or more of the surface area, and its Ni content is 18 to 19 wt%,
in good agreement with Wasson's (1990) bulk Ni value.
Ungrouped Meteorites
ALH84233 (13.6 g).?This reddish-brown and rounded
specimen (2 x 1.5 x 1 cm) has a protrusion on one side giving
it a shape suggestive of a teardrop, suggesting atmospheric
ablation was an important shape-forming process. Several very
small areas of remnant fusion crust were tentatively identified,
but fusion crust has mainly been obliterated by weathering.
One side of the specimen has been more severely weathered,
suggestion it was the underside while exposed on the surface.
A median slice through the long axis of the specimen
provided an area of approximately 1.5 cm2 for metallographic
examination. Much of the edge of the specimen has been
penetrated by 0.1 mm of terrestrial weathering, and in a few
areas both remnant fusion crust and weathering products were
observed. The metal appears to have been single crystal
kamacite with an occasional subgrain boundary that has been
transformed throughout by atmospheric heating to a coarse
martensite or o^ structure. Its bulk Ni value as determined by
electron microprobe is somewhat greater than 6 wt%. No
significant troilite or schreibersite was observed in the metal.
At the base of the elongation where it joins the main body of
the specimen, there is a 1 mm2 area of weathered silicate
material. Its external edge has been melted by atmospheric
ablation and contains small bodies of troilite and kamacite. On
the basis of a small number of microprobe analyses, the
silicates seem to be uniform in composition. Olivine
42 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
pyroxene (Fs17), and plagioclase (Ab83An12Or4) are present.
Prinz et al. (1991) have recently given more detailed
information on the silicates.
The data given here does not place this meteorite into one of
the recognized structural of chemical classification catagories.
On the basis of trace element data on the metal, Wasson (1990)
has found this to be an ungrouped meteorite.
LEW85369 (6.3 g).?This specimen from Lewis Cliff is
small (1.5 x 1.5 x 0.8 cm), irregularly shaped, pitted,
weathered, and covered with a reddish-brown coating of
secondary oxides.
A median section through the specimen provided an area of
0.8 cm2 for metallographic examination. The surface is
comprised of about 8 roughly equidimensional metal grains in
the 1 to 3 mm2 size range. Two of these grains have a
martensite structure that contains martensite subgrains bor-
dered by thin, irregular bands of kamacite. The large kamacite
grains appear to be single crystal kamacite free of inclusions.
Individual kamacite grains react differently to nital etchant,
some becoming very dark on only brief exposure. Preliminary
electron microprobe analysis indicates that the kamacite
contains slightly more than one weight percent Si. Terrestrial
weathering has penetrated into the center of the sample along
kamacite/kamacite grain boundaries and along cleavages. The
external surface of the slice is bordered for the most part by
about a 0.1 mm rim of terrestrial weathering products. Small
areas of remnant fusion crust remain within and under the
weathering products. Interior to this and around most of the
exterior surface is a heat-altered zone, up to 1.5 mm thick at one
point. The two thickest areas of heat-altered zone are at
opposite ends of the section along its long axis, suggesting that
this may have been an oriented individual during atmospheric
passage.
The data given here are insufficient to place this meteorite
into one of the recognized classification catagories. On the
basis of trace element data, Wasson (1990) has found it to be an
ungrouped meteorite with compositional similarities to the
Horse Creek iron meteorite and to metal nodules from the
Mount Egerton stony iron meteorite.
LEW86211 (163.1 g), 86498 (134.2 g).?These two speci-
mens of 4.5 x 4 x 4 cm and 5x3x3 cm respectively are
distinct from all other meteorites in appearance and physical
properties and are obviously paired.
This macroscopic description is based on a 72.6 g piece of
LEW86211, 4.1 x 2.9 x 2.8 cm, broken from the larger mass
during processing. Two-thirds of its surface area is original
exterior and the remainder is interior surface. The exterior is a
weathered fusion crust, predominantly brown with suggestions
of red and yellow, containing occasional patches of retained
black fusion crust. There are areas of iridescent coloring, and
while smooth to the touch, the surface has an unusual
roughness and angularity of appearance when viewed with low
magnification. The areas of interior surface have a hackly
appearance and a predominately yellow color that varies from
pale yellow to bronze yellow. Under magnification (x20) the
yellow material is seen to be present as globules, as fracture
surfaces and crystal faces, and as fine filaments. A few small
areas appear to be vugs coated with a drusy material. Whether
these vug fillings are indigenous or a weathering phenomenon
is not clear, but they may well prove to be indigenous. A few
small areas of silicate are present as is an occasional chromite.
Metallographic examination was performed on a 6 cm2
polished and etched slice removed from the piece described
above. A thin heat altered zone is present and can be recognized
along edges of both the triolite and metal areas, as well as along
edges of the occasional silicate-rich area. The matrix is coarsely
crystalline troilite that contains globular metal, with metal and
troilite present in roughly equal amounts (40% to 60% troilite
depending on the particular subarea selected). This structure
suggests an eutectic intergrowth. Troilite crystals are in the
mm-size range and are cracked on a one-tenth mm scale. A
typical metal globule is 0.3 x 0.6 mm, although particles larger
or much smaller are also present. A martensitic pattern
develops on the metal with etching, with centers of these
regions containing 8-9 wt% Ni and their edges as high as 20
wt% Ni. Schreibersite was not identified, but preliminary
electron microprobe analyses indicated an unusually high
phosphorus content within the martensite (0.5 to 0.6 wt%). This
is suggestive of an unusually high cooling rate.
The occasional silicate-rich areas are fine-grained, some of
these areas are vesicular, and weathering veins have penetrated
into some of them. Prinz et al. (1991) have described these
associations as highly reduced and consisting of olivine,
orthopyroxene, and clinopyroxene with no feldspathic compo-
nents. Oxygen isotope data establishes it as distinct from other
meteorites, and the authors suggest that it is most similar to the
low-Ni extreme of the HE meteorites. Wasson (1990) has
classified LEW86211 as an ungrouped meteorite composition-
ally similar to, but in significant ways different from, low-Ni
HE meteorites.
Discussion
This group of eight meteorites illustrates the unusual
distribution of Antarctic iron meteorite types as compared to
types recovered elsewhere. An unusually high proportion of
ungrouped or anomalous meteorites is observed (Clarke, 1986;
Wasson, 1990). Group IIIAB irons are the most abundant
among non-Antarctic meteorites, but ALH84165 and
GRO85201 are the only two IIIABs so far recovered by
ANSMET expeditions. Both the great distance separating their
recovery sites and observed chemical differences (Wasson et
al., 1989; Wasson, 1990) suggest that they represent separate
falls.
NUMBER 30 43
Literature Cited
Clarke, R.S., Jr.
1986. Antarctic Iron Meteorites: An Unexpectedly High Proportion of
Falls of Unusual Interest. [Abstract] In 5.0. Annexstad, L. Schultz,
and H. Wanke, editors, Workshop on Antarctic Meteorites. LPI
Technical Report, 86-01, pages 28-29. Houston: The Lunar and
Planetary Institute.
1989. Descriptions of Some Antarctic Iron Meteorites. In U.B. Marvin and
G.J. MacPherson, editors, Field and Laboratory Investigations of
Meteorites from Victoria Land and the Thiel Mountain Range,
Antarctica, 1982-1983 and 1983-1984. Smithsonian Contributions
to the Earth Sciences, 28:61-63.
Jarosewich, E.
1990. Chemical Analyses of Meteorites: A Compilation of Stony and Iron
Meteorites. Meteoritics, 25:323-337.
Mason, B., and R. Martinez
1988. LEW86220. Antarctic Meteorite Newsletter, 11 (1 ):20.
Prinz, M., N. Chatterjee, M.K. Weisberg, R.N. Clayton, and T.K. Mayeda
1991. Silicate Inclusions in Antarctic Irons. [Abstract.] In Lunar and
Planetary Science XXII, pages 1101-1102. Houston: The Lunar and
Planetary Science Institute.
Wasson, J.T.
1990. Ungrouped Iron Meteorites in Antarctica: Origin of Anomalously
High Abundances. Science, 249:900-902.
Wasson, J.T, X. Ouyang, J. Wang, and E. Jerde
1989. Chemical Classification of Iron Meteorites: XI. Multi-Element
Studies of 38 New Irons and the High Abundance of Ungrouped
Irons from Antarctica. Geochimica et Cosmochimica Acta, 53:
735-744.
6. Terrestrial Ages of Victoria Land Meteorites
Derived from Cosmic-Ray-Produced Radionuclides
John Evans, John Wacker,
and James Reeves
Since 1979, Battelle, Pacific Northwest Laboratories (Bat-
telle-Northwest) has continued to assay Antarctic meteorites
for the cosmic-ray-produced radionuclide, 26A1 (tl/2 ~ 720,000
years). This nuclide is assayed rapidly and nondestructively by
multiparameter gamma-ray spectroscopy. These measurements
have been intended to provide a basis for estimation of the
terrestrial residence time of meteorites that have been collected
on the Antarctic ice sheet. While the 26A1 method alone cannot
provide a completely reliable terrestrial age for individual
samples, 26A1 data can be used to evaluate trends for large
groups of samples and provide useful guidance for selecting
samples for more detailed study by other methods. Other
investigators have performed analyses for several other
cosmic-ray-produced radionuclides on some of these same
samples.
In addition to 26A1, the isotopes studied and tabulated in this
article include 53Mn (t1/2 = 3.7 million years), 10Be (t1/2 = 1.5
million years), 36C1 (t1/2 = 300,000 years), and 14C (t1/2 = 5730
years). Very sophisticated and labor intensive techniques that
involve complicated physical and chemical separations are
used for those analyses. Manganese-53 is measured by neutron
activation while 14C, 10Be, and 36C1 are measured by accelerator
mass spectrometry.
Previous issues of Smithsonian Contributions to the Earth
Sciences have reviewed the status of cosmogenic radionuclide
research on Antarctic meteorites (Evans and Rancitelli, 1980;
Evans, Reeves, and Rancitelli, 1982; Nishiizumi, 1984). This
article updates that information but expands the data base
considerably with the addition of previously unreported
information on 214 meteorites. The Battelle-Northwest pro-
John C. Evans, John F. Wacker, and James H. Reeves, Battelle,
Pacific Northwest Laboratories, P.O. Box 999, Richland, Washington
99352.
gram has measured 26A1 in 422 Victoria Land meteorites
(Evans, Rancitelli, and Reeves, 1979; Evans and Reeves,
1987), and these data are tabulated in this article, together with
published data on four other radionuclides. The tabulation
includes 22 10Be, 79 53Mn, 54 36C1, and 15 14C measurements.
Only information on samples studied in the Battelle-Northwest
program is considered here; the tabulation is thus not
completely comprehensive. Multiple measurements on the
same meteorite have also been excluded in the interest of
simplicity. Our information is representative, although the total
data base on cosmogenic radionuclides available in the
published literature is somewhat larger than that presented. A
more complete review of all available data for Antarctic as well
as non-Antarctic meteorite finds and falls has recently been
compiled and published by Nishiizumi (1987).
Several factors influence the interpretation of cosmogenic
radionuclide data when calculating a terrestrial age. Ideally we
may assume that cosmic ray interactions in the meteorite
preatmospheric main mass produce long-lived radionuclides at
a known and constant rate. If the cosmic ray exposure time is
long, compared to the half-life of the isotope of interest, the
meteorite will fall to earth with a constant saturated activity that
will then decay exponentially. The amount of decay provides a
measure of the residence time of the meteorite on earth.
Saturation activities for 26A1 were calculated by Evans and
Reeves (1987) to be 59 and 55 dpm/kg for L and H chondrites,
respectively. The expected saturation activity of ureilites is
given by Wilkening et al. (1973) as 58 ? 4 dpm/kg. The
calculations were based on the production rate data of Fuse and
Anders (1969). Similarly, the corresponding saturation activi-
ties for 53Mn, 10Be, 36C1, and 14C are 414, 20, 22.8, and 60
dpm/kg respectively, according to the evaluation of Reedy,
Arnold, and Lai (1983).
45
46 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
Several factors may modify the activity of cosmogenic
radionuclides found at the time of fall. For example, shielding
may reduce the production rate for either abnormally large or
unusually small preatmospheric bodies. That effect is more
significant for low-energy products such as 26A1, 53Mn, or 14C
and less important for high-energy products such as 36C1.
Another factor affecting production is that meteorites may
occasionally experience unusual irradiation histories (e.g., solar
cosmic ray effects that produce elevated activity). Low-energy
products such as 26A1 and 53Mn can be affected by a solar
component particularly in very small objects. Finally, and most
importantly, the cosmic ray exposure period in space following
breakup from the parent body may not be long enough to reach
radioactive saturation for the isotope of interest. That effect is
quite significant for 53Mn or 10Be and is of occasional
significance for 26A1. The half-life of 36C1 is sufficiently short
that the isotope is almost always found at the saturation value.
Chlorine-36 is thus clearly the isotope of choice for the time
scale of interest in Antarctica.
In this work, we consider terrestrial ages derived from 36C1 to
be the most reliable. Other cosmic ray produced radioisotopes
with appropriate half-lives for terrestrial age determination
include 81Kr (t1/2 = 210,000 years), 59Ni (t1/2 = 76,000 years),
and 41Ca (t1/2 = 100,000). A few 81Kr based ages have been
included in this work although the data were not included in the
table in the interest of conserving space. For more details see
Freundel et al. (1986). 81Kr data are relatively scarce at this
time as the nuclide is generally present in low abundances in
meteorites and is difficult to measure. Interpretation of 81Kr
data is complicated since the production rate of the isotope is
sensitive to trace element chemistry. 59Ni and 41Ca data are also
rather scarce. Interpretation of data for those isotopes is
complicated by neutron capture effects which are typically very
size dependent. Terrestrial ages can also be derived with some
degree of assurance by combining 26A1 and 53Mn data. The
longer lived 53Mn is used to estimate exposure age, and the
shorter lived 26A1 is used to estimate terrestrial age. A
convergent solution to a common pair of terrestrial and
exposure ages can be obtained by numerical solution to the pair
of simultaneous radioactive saturation and decay equations
after only a few iterations.
Table 6-1 summarizes a large body of cosmogenic radionu-
clide data measured on Antarctic meteorites allocated from the
U.S. collection. With only five exceptions, all terrestrial ages
given in the last column of Table 6-1 were calculated or
recalculated specifically for this tabulation. The terrestrial age
estimate for the lunar meteorite, ALHA81005, was taken from
the work of Nishiizumi, Reedy, and Arnold (1988). Terrestrial
age estimates for ALHA77005 (shergottite), ALHA78132
(eucrite), ALHA79017 (eucrite), and EETA79005 (eucrite)
were taken from the age calculations of Freundel et al. (1986)
based on their 81Kr measurements. 36C1 data were used
whenever available to produce firm estimates of terrestrial age;
those data are shown as numbers with a one standard deviation
error. The 36C1 method is capable of measuring terrestrial ages
greater than approximately 70,000 to 90,000 years. In a few
cases, 14C data were used for an age calculation, although most
meteorites have been found to be older than the greatest age
measurable with 14C (30,000 to 50,000 years). Ages shown in
the table as approximate are based on a combination of 26A1 and
53Mn data. In most cases where comparison is possible, the two
methods agree reasonably well; however, the 36C1 method is
clearly more accurate and capable of resolving shorter ages.
The remaining terrestrial age estimates in Table 6-1 are based
only on 26A1 and should be used with great caution. Those ages
are intended as conservative limits based on worst-case
arithmetic propagation of 1 sigma errors in both the measured
and the expected value. That procedure will, in most cases,
significantly overestimate the terrestrial age. A minimum upper
limit of 200,000 years was assumed for terrestrial ages based on
26Al alone. That number is somewhat arbitrarily based on the
authors' best judgement as to the minimum amount of decay
resolvable by 26A1 data alone.
The samples in Table 6-1 have a wide range of terrestrial
ages, with a few specimens having sufficiently short terrestrial
ages that they still contain detectable 14C, while a number of
samples measured for 36C1 have ages of nearly 1 million years;
the oldest sample measured to date is ALHA78153 (970,000 ?
100,000 years). The 970,000 year terrestrial age for
ALHA78153 shown in Table 6-1 is derived from 36C1 data;
however, a nearly identical age estimate can be obtained from
the 26A1 data as well. A number of other samples have been
found recently that have similarly low 26A1 contents and may
have terrestrial ages up to 1 million years. Currently available
evidence continues to suggest that approximately 1 million
years is the approximate age cutoff for the residence time in the
Allan Hills region. There are not enough measurements
available now to draw firm conclusions about the other regions
sampled; however, Nishiizumi (1984) has suggested that the
Allan Hills meteorites have a wider range of terrestrial ages and
are generally older than other Victoria Land and Yamato
meteorites. The distribution of ages and the age cutoff represent
important constraints for models of ice movement, meteorite
accumulation, and destruction of meteorites by weathering in
the Victoria Land region.
Figure 6-1 shows the distribution of 26A1 contents for the
Antarctic meteorites collected in the Victoria Land region
compared with the equivalent treatment for a selection of falls
and finds collected worldwide outside Antarctica. For this
purpose we have assumed that the terrestrial ages of chondrites
outside the Antarctic are, in general, short compared with the
half-life of 26A1 (i.e., less than 100,000 years). The worldwide
data include 135 samples taken from a variety of sources
(Evans, Reeves, Rancitelli, and Bogard, 1982; Cressy, 1976;
Cameron and Top, 1974; Hey man and Anders, 1967).
Approximately one-third of the data originated in our labora-
tory. The frequency distribution of worldwide data (solid bars)
has been renormalized on the figure to give the same integrated
NUMBER 30 47
(I)
QJin
01o
L
QJ
u
?
Z
1 1U -
100 -
90 -
80 -
70 -
60 -
50 -
40 -
30 ~
20 -
10 -
0 -
PvH Antarctic Meteorite s
?? Worldwide Meteorites
f-j
^ r p pi [XI
,
X
X
X
X
Y
?1
,?1
X
X
X
X
X
X
X1
X
X
Xx
Xx
x
X
X
X
X
X
X
\/
X
X
X
X
X
X
x
X
X
X
1?1
X
X
X
X
X
X
X
y
X
X
Y
X
X
Y
11
k/il p/ll 1?'?, 1?1
10 15 20 25 30 35 40 45 50 55 60 65 70 75 80 85 90 95 100
Aluminum-26 (dpm/kg)
FIGURE 6-1.?Distribution of 26A1 contents of ordinary chondrite finds from the Victoria Land region of
Antarctica (crosshatched bars) as compared with the distribution worldwide for both falls and finds (solid bars).
The frequency distribution of worldwide data has been adjusted to have the same integrated area as for Antarctic
specimens. All data are normalized to an L chondrite composition using the saturation values computed from the
production rates of Fuse and Anders (1969), and nominal chondritic compositions. No correction was made for
exposure age. Worldwide data were taken from a variety of sources (Evans, Reeves, Rancitelli, and Bogard, 1982;
Cressy, 1976; Cameron and Top, 1974; Heyman and Anders, 1967).
area as the Antarctic data (crosshatched bars). Only ordinary
chondrites (H, L, and LL) are included. The data for H
chondrites were multiplied by a factor of 1.07 to correct for the
expected differences in production rates caused by composi-
tional differences (Fuse and Anders, 1969). The Antarctic data
show a definite shift to lower values. The shift is evident in the
excess of samples with 26A1 contents between 35 and 50
dpm/kg as well as a corresponding depletion above 65 dpm/kg.
Interpretation of the excess of samples with low values is
somewhat complicated by the inclusion of a number of paired
specimens which may be associated with showers; however,
the low values are associated with a wide range of meteorite
types and cannot be attributed strictly to shower effects. It thus
appears from a strictly statistical basis that the average age of
the collection is a significant fraction of the half-life of 26A1.
This observation is consistent with other observations based on
more direct methods of terrestrial age determination (i.e., 36C1
or 81Kr dating) as discussed above.
Funding for this work was provided by the National Science
Foundation, Division of Polar Programs under grant DPP-
8745437 and the National Aeronautics and Space Administra-
tion under contract NASA No. 86-229. The authors are
indebted to Dr. Kunihiko Nishiizumi for his assistance in
providing data and references for the assembly of Table 6-1.
48 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE 6-1.?Activity and terrestrial age estimates for Victoria Land meteorites1.
Specimen
number
Allan Hills
ALHA76004
ALHA76005
ALHA76006
ALHA76007
ALHA76008
ALHA77001
ALHA77002
ALHA77003
ALHA77004
ALHA77005
ALHA77007
ALHA77008
ALHA77009
ALHA77010
ALHA77011
ALHA77012
ALHA77O13
ALHA77014
ALHA77015
ALHA77016
ALHA77017
ALHA77018
ALHA77019
ALHA77021
ALHA77023
ALHA77025
ALHA77026
ALHA77042
ALHA77047
ALHA77050
ALHA77052
ALHA77060
ALHA77062
ALHA77071
ALHA77078
ALHA77081
ALHA77084
ALHA77O85
ALHA77086
ALHA77087
ALHA77088
ALHA77092
ALHA77111
ALHA77112
ALHA77114
ALHA77115
ALHA77117
ALHA77118
ALHA77124
ALHA77126
ALHA77130
ALHA77131
ALHA77132
ALHA77139
Class
LL3
Eu
H6
L6
H6
L6
L5
C3
H4
Sher
H5
L6
H4
H4
L3
H5
L3
H5
L3
H5
H5
H5
L6
?* H5
H5
H5
H5
H5
L3
L3
L3
LL5
H5
H5
H5
H?
H5
H5
H5
H5
H5
H5
H6
H5
H5
L3
L5
H5
H5
H5
H5
H6
H5
H5
26A1
(7.2 X 105 y)
58 ?6
89 ?9
51 ?5
45 ?4
H?l
52 ?5
30 ?3
45 ?5
52 ?5
55?2
36 ?2*
49 ?3*
32 ? 2
49 ?3
39 ?4
78 ?3
44 ?5*
55 ?3
36 ?4
51 ?5*
53 ?5*
58 ?7*
51 ?4*
63 ?7*
78 ?9*
54 ?5
17 ?9*
53 ? 10*
50 + 6*
36 ?4*
42 ?3*
38 ?3*
47 ?5
55?6
67 ?8*
42 ?4
53 + 7*
37 + 4*
58 ?6
41 ?10*
55 ?6*
44 + 7*
20 ?7*
. 29 ?15*
47 ?9*
48 ?3
45 ?17*
53 ?5
70?7
48 ? 14*
51 ?8*
92 ?11*
42 ?2*
53 ? 6*
10Be
(1.5xl06y)
22.8 ? 0.8
3.9 ? 0.5
19 ?2
14 ? 0.7
14.4 ?1.2
Activity2
53Mn
(3.7xlO6y)
402 ?37
456 ? 33
336 ? 26
22 ?3
422 ? 13
255 ?8
317? 13
326 ?13
270 ?15
352 ?19
162 ?9
162 ?8
173 + 9
36C1 14C
(3.0 x 105 y) (5730 y)
< 1.0
<1.7
<1.2
9.4 ?1.0 <1.7
20.1 ?1.2
4.6 ?1.1
18.4 ?1.2 0.62 ?0.06
15.2 ?0.5 0.65 ?0.02
4.6 ? 0.9
10.7 ? 0.2
age
xlOOOy
<280
> 34,< 340
> 32,< 200
> 34,- 250
100 ?70
<140
690 ?170
90 ?80
180 ?70
190 ?70
<640
<410
330 ?60
<340
-330
<200
<580
<200
-430
<33O
<280
<220
<380
<200
<200
<280
< 2,300
<400
<450
<780
<580
<690
<430
<280
<200
<550
<340
<690
<220
<750
<280
<580
<1640
<1640
<530
-130
<840
<320
<200
<400
<400
<200
<500
<300
'Average saturated activity: 26A1 59 ? 9 (L), 55 ? (H); 53Mn: 414 ? 50; 10Be: 20 ? 2; 36C1: 22.8 ? 3.1; 14C: 60.
2Activity: 26A1, 14C: dpm/kg meteorite; 53Mn: dpm/kg (Fe+l/3Ni); 36C1: dpm/kg metal.
NUMBER 30 49
TABLE 6-1.?Continued.
Specimen
number
ALHA77140
ALHA77143
ALHA77144
ALHA77149
ALHA77150
ALHA77157
ALHA77160
ALHA77162
ALHA77163
ALHA77164
ALHA77165
ALHA77166
ALHA77167
ALHA77168
ALHA77171
ALHA77173
ALHA77174
ALHA77175
ALHA77176
ALHA77177
ALHA77180
ALHA77181
ALHA77182
ALHA77183
ALHA77184
ALHA77185
ALHA77186
ALHA77187
ALHA77188
ALHA77190
ALHA77191
ALHA77192
ALHA77197
ALHA77208
ALHA77209
ALHA77211
ALHA77214
ALHA77215
ALHA77216
ALHA77217
ALHA77221
ALHA77223
ALHA77224
ALHA77225
ALHA77230
ALHA77232
ALHA77233
ALHA77240
ALHA77241
ALHA77242
ALHA77244
ALHA77245
ALHA77246
ALHA77247
ALHA77248
ALHA77249
ALHA77251
ALHA77252
Class
L3
H5
H6
H6
L6
H6
L3
L6
L3
L3
L3
L3
L3
H5
H5
H5
H5
L3
L3
H5
L6
H5
H5
H6
H5
L3
H5
H5
H5
H4
H4
H4
L3
H4
H6
L3
L3
L3
L3
L3
H4
H4
H4
H4
L4
H4
H4
H5
L3
H5
L3
H5
H6
H5
H6
L3
L6
L3
26A1
(7.2 x 105 y)
40?4
57 ?9*
56 ?6
52 ?9*
71 ?3*
52 ?3*
50 ?7*
50 ?15*
57 ?9*
44?5
46 ?8*
35 ?2*
37 ?2
52 ?13*
58 ?13*
59 ?15*
25 ?12*
24 ?14*
48 ? 7*
54 ?3
56 ?2*
44 ?9*
41?4
38 ?2*
48 ?2*
45 ?11*
59 ?3*
66 ?7*
61 ?2*
51 ?3
56 ?4
55 ?6
45 ?11*
52?3
52 ?8*
60 ?12*
56 ?6
36 ?4
40?3
38 ?3
57 ?2*
56 ?2*
51 ?3
51 ?3
51 ?3
54 ?3
47 ?3
71 ? 11*
35 ?2*
47 ?6*
40 ?7*
40 ?5*
67 ?4*
59 ?8*
27 ?3*
37 ?2
52 ?7*
42 ?2*
Activity
10Be 53Mn 36C1 14C
(1.5xlO6y) (3.7xl06y) (3.0xl05y) (5730 y)
178 ?10
156 ?8
137 ?7
350 ?18
297 ? 16
15 ?1 151 ?6 17.0 ?8 0.35 ?0.03
21 ? 1 402 ? 17
377 ? 15
362 ?15
181 ?9 14.9 ?0.5
age
xlOOOy
-330
<280
<260
<400
<200
<280
<480
<300
<610
<200
< 1,440
<750
<350
<500
<35O
<370
< 1,640
< 2,000
<530
<260
<240
<610
<550
<605
<360
<360
<200
<200
<200
<320
<240
<300
<360
<300
<370
<480
130 ?80
<780
<630
<690
<200
<200
<320
<320
-130
<260
<410
<200
<750
<450
<750
<610
<200
<220
< 1,000
180 ?70
<430
50 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE 6-1.?Continued.
Specimen
number
ALHA77253
ALHA77254
ALHA77258
ALHA77259
ALHA77260
ALHA77261
ALHA77262
ALHA77266
ALHA77267
ALHA77268
ALHA77269
ALHA77270
ALHA77271
ALHA77272
ALHA77273
ALHA77274
ALHA77275
ALHA77277
ALHA77278
ALHA77279
ALHA77280
ALHA77281
ALHA77282
ALHA77284
ALHA77285
ALHA77286
ALHA77287
ALHA77288
ALHA77293
ALHA77294
ALHA77295
ALHA77296
ALHA77297
ALHA77299
ALHA77300
ALHA77301
ALHA77303
ALHA77304
ALHA78OO1
ALHA78OO3
ALHA78004
ALHA78005
ALHA78012
ALHA78015
ALHA78027
ALHA78038
ALHA78039
ALHA78040
ALHA78041
ALHA78042
ALHA78043
ALHA78044
ALHA78045
ALHA78046
ALHA78047
ALHA78048
ALHA78049
ALHA78050
Class
H5
L5
H6
H5
L3
US
H4
H5
L5
H5
L6
L6
H6
L6
L6
H5
H5
L6
LL3
H5
L6
L6
L6
L6
H6
H4
H5
H6
L6
H5
EH4
L6
L6
H3
H5
L6
L3
L4
H5
L6
H5
H5
H5
LL3
H5
L3
L6
Eu
L3
L6
L6
L4
L6
L3
H5
L6
H5
L6
26A1
(7.2 x 105 y)
5619*
5312*
2912
4912
3712
3614
4715
4212*
6114*
5112*
4913
4013
3912
3514
3112
5312
4318*
5512
2813
3912*
4412
4212*
4913
4515
3814
5414
5712
4513
6615*
6114
5714*
6714
7017
4314
5414
4116*
4515*
5013
5014
5914
4918*
56111*
6819*
4818*
7818*
3613
4213
9315
3813
4512
3813
5114
3413
4615
3311*
5915
5213
4413
Activity
10Be 53Mn
(1.5xlO6y) (3.7xlO6y)
2011 434118
15018
22.711.4 302113
327113
319117
494120
283115
1812 213111
224111
264111
325116
503127
384117
16.810.8 394116
433 117
25.010.9 428117
317 ?19
211 ?9
170 ?9
428 ? 19
19.4 ?0.7 457 ?22
276118
36C1 14C
(3.0xl05y) (5730 y)
12.210.4
11.110.6
21.712.0
18.310.4
6.710.1
19.410.8
6.610.3 <0.5
6.210.3
10.910.7
12.210.3
12.110.4 1.0710.24
13.610.5
20.810.6 1.610.3
19.610.2 < 0.6
18.910.8
7.310.3
4.010.2
lCTTCS uiulage
xlOOOy
<300
<300
270170
<340
-380
310180
<100
<500
<200
100170
<410
530160
<140
540180
560180
<200
<610
<220
320180
<580
270170
-330
270170
<550
220170
<260
<200
<480
<200
<3012
<250
<220
<130
<160
<260
<690
<550
-130
<340
<220
<530
<350
<200
<550
<200
<430
<580
<200
<690
<480
490170
<380
750180
<530
<720
<240
<300
<530
NUMBER 30 51
TABLE 6-1.?Continued.
Specimen
number
ALHA78051
ALHA78052
ALHA78O53
ALHA78063
ALHA78074
ALHA78075
ALHA78076
ALHA78077
ALHA78078
ALHA78080
ALHA78082
ALHA78085
ALHA78101
ALHA781O2
ALHA78103
ALHA78104
ALHA781O5
ALHA78106
ALHA78107
ALHA781O8
ALHA78109
ALHA78110
ALHA78111
ALHA78112
ALHA78114
ALHA78115
ALHA78116
ALHA78119
ALHA78120
ALHA78121
ALHA78124
ALHA78126
ALHA78127
ALHA78128
ALHA78129
ALHA78130
ALHA78131
ALHA78132
ALHA78133
ALHA78134
ALHA78135
ALHA78136
ALHA78137
ALHA78141
ALHA78142
ALHA78145
ALHA78147
ALHA78149
ALHA78153
ALHA78157
ALHA78159
ALHA78162
ALHA78164
ALHA78170
ALHA78173
ALHA78190
ALHA78194
ALHA78235
Class
H4
H5
H4
LL6
L6
H5
H6
H4
L6
H5
LL6
H5
L6
H5
L6
L6
L6
L6
H5
H5
LL5
H5
H5
L6
L6
H6
H5
L3
H4
H5
H6
L6
L6
H5
H5
L6
L6
Eu
L6
H4
H6
H5
H6
H5
L5
H6
H5/6
L3
LL6
H4
H5
L3
H5
H3
H5
H5
H5
L3
26A1
(7.2 x 105 y)
38 ?3
56 ?4
56 ?3
48 ?7*
66 + 3
49 ?3
52 ?4
42 ?3
49 ?3
75 ?7*
49 + 5*
50 ?2*
48 ?3*
35 ?3
58 ?3
53 ?3
61 ?7
44?4
54?3
55 ?3*
46 ?3
58 ?3
53 ?3*
42 ?3
38 + 2
43 ?3
36 + 2*
42 ? 3*
47 ?7*
56 ?6*
54 ?8*
45 ?3
46?3*
34 + 2
59 ?3*
51 ?4
40?3
68 + 4
50 ?6*
61 ?3
52 ?6*
64?8*
58 + 6*
75 ?8*
60? 11*
63?11*
56 ?10*
72 ?7*
22 ?1
43 ? 10*
53 ?6*
36 ?9*
72 ?9*
48 ?4
64 + 5
67 ?6
74 + 5
38 ?5
10Be
(1.5xl06y)
21 ?2
14?2
16?2
18?2
Activity
53Mn
(3.7xl06y)
427 ?18
323 ?17
453 ? 24
366 ? 19
462 ?21
444 ?28
347 ? 16
360 ? 14
334 ? 14
380 ?15
402 ?19
258 ? 14
36Q 14C
(3.0 x 105 y) (5730 y)
16.9 ?0.5
14.0 ?0.6
10.7 ?1.2
20.1 ? 1.7
12.5 ? 0.3
12.4 ?0.5
13.4 ?0.5
7.8 ? 0.3
21.6 ?0.6
15.2 ?0.4
20.7 ? 0.5
9.3 ? 0.4
22.9 ?1.6
2.44 ? 0.25
age
xlOOOy
<530
<630
<220
<530
<200
<360
130 ?70
<53O
<410
<200
<450
<320
<430
210 ?70
330 ?110
<150
260 ?70
<550
<260
<260
260 ?70
<200
<280
230 ? 70
460?70
<90
<660
<58O
<470
<240
<330
<500
<480
180 ?70
<200
< 110
390 ?70
120 ?50
<450
<90
<33O
<200
<200
<200
<340
<200
<330
<200
970 ?100
<670
<300
<960
<200
<410
<200
<200
<200
<750
52 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE 6-1.?Continued.
Specimen
number
ALHA78251
ALHA79002
ALHA79007
ALHA79012
ALHA79013
ALHA79016
ALHA79017
ALHA79018
ALHA79025
ALHA79026
ALHA79027
ALHA79029
ALHA79033
ALHA79039
ALHA79045
ALHA79046
ALHA79053
ALHA80102
ALHA8O1O3
ALHA80105
ALHA80106
ALHA8O1O7
ALHA8O1O8
ALHA80110
ALHA80112
ALHA8O113
ALHA80114
ALHA80115
ALHA80116
ALHA80117
ALHA80125
ALHA80128
ALHA80129
ALHA80132
ALHA81OO5
ALHA81017
ALHA81019
ALHA81020
ALHA81022
ALHA81024
ALHA81025
ALHA81026
ALHA81029
ALHA81O31
ALHA81032
ALHA81038
ALHA81039
ALHA81040
ALHA81041
ALHA81042
ALHA81O43
ALHA81044
ALHA81048
ALHA81064
ALHA81094
ALHA81099
ALHA81100
ALHA81101
Class
L6
H6
L6
H5
H5
H6
Eu
L6
H5
H5
L6
H5
L6
H4
L3
H5
H5
Eu
L6
L6
H4
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
H4
H5
H5
Ano
L5
H5
H5
H4
L3
L3
L6
L6
L3
L3
H6
H5
L4
H4
H5
H4
H4
H4
H5
H6
L6
H5
URE
26 Al
(7.2 x 105 y)
56 ?6
34?2
71 + 4
52 ?3
59 ?3
50 ?3
97 ?3
58 ?3
53 ?3
60?4
42 ?3
49 ?3
72 ?4
42 ?2
44?3
50 ?3*
60 ?3*
83 ?5
57 ?3
58 ?3
52 ?3
59 ?3
62 ?4
65 ?4
59 ?3
57 ?3
62 ?3
56 ?3
60 ?2*
62 ?3*
58 ?4
59 ?4
56 ?3
58 ?3
46 ?3
54 ?2*
41 ?2*
54 + 3
44 ?2*
40 ?2*
45 ?3*
63 ?3*
39 ?2*
30 ?1*
45 ?2*
35 ?2*
56 ?2*
65 ?3*
52 ?2*
50 ?2*
56 ?3*
53 ?2*
58 ?3*
59 ?3*
58 ?3*
80 ?4*
49 ?2*
35 ?2*
Activity
10Be 53Mn 36C1 14C
(1.5xl06y) (3.7xlO6y) (3.0xl05y) (5730 y)
23.8 ? 0.8 530 ? 75
526 ?27
465 ?70
443 ?31
289 ? 20
281 ?21
4.1 ?0.5 173 ?12 8.8 ?0.4
icricbuiuJage
xlOOOy
<320
<720
<200
<300
<200
<340
< 120 ?50
<220
<300
<200
<580
<380
<200
<500
<530
<340
<200
<300
<100
<100
<320
<200
<200
<200
<200
<240
<200
<260
<200
<200
<240
<200
<100
<200
200-400
<280
<530
<230
<450
<610
<500
<200
<630
<89O
<480
<690
<200
<200
<280
<320
<220
<260
<200
<200
<200
<200
<340
<750
NUMBER 30 53
TABLE 6-1.?Continued.
Specimen
number
ALHA81102
ALHA81103
ALHA81104
ALHA81105
ALHA81107
ALHA81111
ALHA81112
ALHA81113
ALHA81115
ALHA81119
ALHA81161
ALHA81183
ALHA81247
ALHA81251
ALHA81260
ALHA81295
ALH82102
ALH82104
ALH82105
ALH82106
ALH82118
ALH82122
ALH82125
ALH82126
ALH82130
ALH83OO1
ALH83002
ALH83O03
ALH83004
ALH83OO5
ALH83OO6
ALH83007
ALH83008
ALH83O1O
ALH83011
ALH83013
ALH83067
ALH83070
ALH84057
ALH84059
ALH84060
ALH84061
ALH84062
ALH84063
ALH84066
ALH84067
ALH84068
ALH84069
ALH84070
ALH84071
ALH84072
ALH84073
ALH84074
ALH84075
ALH84076
ALH84077
ALH84078
ALH84079
Class
H6
H6
H4
H4
L6
H6
H6
H5
H5
L4
H5
H5
L6
LL3
E6
H5
H5
L5
L6
URE
L6
H5
L6
H4
URE
L4
L5
H5
L6
H5
H5
L3
L3
L3
L5
H6
L6
LL6
L6
H4
H5
L6
L6
L5
L6
H5
H5
H5
L6
H6
L6
H5
H5
H5
H5
H5
H5
L6
26A1
(7.2xlO5y)
36 + 2*
49 ?2*
57 ?2*
54 ?3*
70 + 3
38 ?2*
39 ?2*
61 ?3*
40?2*
36 ?2*
54 ?2*
53 ?3*
44 ?2*
45 ?2*
33 ?2*
52 + 2*
39 + 2
62 ?2*
45 ?2*
63 ?6*
59 ?3*
44?2*
36 ?2*
54 + 2*
62 + 5*
40 ?1*
28 ?1*
39 ?2*
53 ?2*
34 ?2*
53 ?2*
58 ?2*
38 ?2*
50 ?2*
44?2*
58 ?3*
42 + 2*
62 ?3*
42 ?2*
43 ?2*
59 ?2*
46 ?2*
46 ?2*
54 ?2*
73 ?3*
54 ?2*
46 ?2*
40?2*
52 ?4*
45 ?1*
41 ?2*
34 ?1*
33 ?1*
49 ?2*
64?3*
45 ?2*
65 ?3*
65 ?3*
Activity
10Be 53Mn 36C1 14C
(1.5xl06y) (3.7xl06y) (3.0xl05y) (5730 y)
21.7 ?0.9
age
xlOOOy
<660
<340
<200
<260
<200
<610
<58O
<200
<550
<660
<240
<280
<500
<480
<720
<280
<100
<200
<480
<200
<200
<450
<720
<240
<200
<560
<960
<580
<300
<720
<260
<200
<660
<360
<500
<200
<550
<200
<500
<480
<200
<450
<450
<260
<200
<240
<450
<550
<360
<410
<580
<690
<720
<340
<200
<430
<200
54 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE 6-1.?Continued.
Specimen
number
ALH84080
ALH84081
ALH84082
ALH84083
ALH84084
ALH84085
ALH84086
ALH84087
ALH84088
ALH84089
ALH84090
ALH84091
ALH84092
ALH84093
ALH84094
ALH84095
ALH84096
ALH84097
ALH84098
Bates Nunatak
BTNA78OO1
BTNA78004
BTNA78OO5
Elephant Moraine
EETA79001
EETA79003
EETA79005
EETA79007
EETA79010
EETA79011
Meteorite Hills
META78001
META78002
META78003
META78004
META78005
META78006
META78009
META78010
META78011
META78013
META78014
META78015
META78018
META78019
META78021
META78023
META78025
META78027
META78028
Mount Baldr
MBRA76001
Outpost Nunatak
OTTA80301
Class
L6
LL6
H6
H6
H4
H5
LL3
L6
H5
H5
L6
H5
L6
H6
H5
L6
C4
L6
H5
L6
LL6
H6
Sher
L6
Eu
H5
L6
Eu
H4
L6
L6
L6
L6
H6
H5
H5
H5
H6
H5
L5
H5
H6
L6
H6
H6
H6
L6
H6
H3
26A1
(7.2xl05y)
26 ?1*
46 ?2*
40 ?2*
38 ?2*
59 ?2*
49 ?2*
56 ?2*
69 ?3*
60 ?3*
49 + 2*
40 ?2*
50 ?2*
63 ?3*
69 + 4*
54 ?3*
33 + 2*
70 ?4*
63 + 4*
65 ?3*
65 ?4
49 ?3
40 + 2
23 ?3
47 ?3
63 ?3
47 + 3
67 ?4
79 ?6
53 ?3
47 ?3
50?3
49 + 4
44?3
60?4
68 + 4
56 + 3
39 ?3
61 ?4
68 ?4
42 ?5
58 ?4
108 ?6
52 ?12
54?5
33 ?2
69 ?6
56?3
73 + 4
82 ?3
Activity
10Be 53Mn
(1.5xl06y) (3.7xl06y)
361 + 22
4.7 + 0.2 65 ?15
333 ?12
11.0 ?0.6
429 ? 17
237 ? 19
302 ? 16
519 ?28
484 ? 25
301 ?19
397 ? 34
36C1 14C
(3.0xl05y) (5730 y)
19.5 ? 0.4
8.1 ?0.6
16.8 ? 2.2
20.5 ? 0.8
21.4 ?0.5
20.4 ? 0.4
20.9 ? 0.5
21.8 ?0.5
10.0 ?2.0
21.3 ?0.6 1.01 ?0.03
1.19 ?0.30
1 lisrrActri oiicrrcauiai
agexlOOOy
<1040
<450
<550
<610
<200
<340
<200
<200
<200
<340
<610
<320
<200
<200
<260
<820
<200
<200
<200
<200
<130
<550
<60
<250
180 ?30
<430
<200
<430
<130
<90
<380
<430
< 110
<100
<200
<80
<600
<200
<200
<630
<200
<100
<55O
<340
<750
<200
32 ?1
31 ?3
<200
NUMBER 30 55
TABLE 6-1.?Continued.
Specimen
number
Reckling Peak
RKPA78OO1
RKPA78O03
RKPA78004
RKPA78005
RKPA79001
RKPA79002
RKPA79003
RKPA79004
RKPA79009
RKPA79013
RKPA80201
RKPA80202
RKPA80209
RKPA80216
RKPA80219
RKPA80222
RKPA80223
RKPA80231
RKPA80232
RKPA80233
RKPA80234
RKPA80235
RKPA80237
RKPA80251
RKPA80254
RKPA80256
RKPA80262
RKPA80264
RKPA80267
Class
L6
L6
H4
H5
L6
L6
H6
H5
H6
L5
H6
L6
L5
L4
L6
LL6
H5
H6
H4
H5
LL5
LL6
H4
H5
H6
L3
H6
L6
H4
26A1
(7.2 x 105 y)
49 ?3
5O?3
39 ?2
65 ?5
58?4
60 ?3
59 ?4
45 ?3
47 ?2
56 ?4
52 ?3
53 ?3
44?2
71 ?5
60?2
61?4
54 ?2
62 ?4
62?4
67 ?4
58 ?3
55 ?3
46?3
49 ?4
60 ?2
62 ?4
40 ?4
48 ?2
44?2
Activity
10Be 53Mn 36C1 14C
(1.5xlO6y) (3.7xlO6y) (3.0xl05y) (5730 y)
363 ?16 19.8 ?0.4
280 ?1 24.0 ?0.6
18.1 ?0.6 292 ?15 21.6 ?0.3
205 ?11 22.7 ?0.5
age
xlOOOy
<400
<130
<580
<200
<70
<200
<200
<480
<38O
<280
<80
<320
<500
<200
<200
<200
<240
<80
<200
<200
<200
<200
<450
<380
<200
<200
<610
<410
<450
References:
Column 1 (26A1):
Column 2 (10Be):
Column 3 (53Mn):
Column 4(36C1):
Column 5 (14C):
Column 6 (age):
Evans et al.,1979, 1980, 1982,1987; Tliniz et al., 1983; Evans, Wacker, and Reeves, herein (data marked with
asterisks is previously unpublished).
Moniot et al.,1982; Nishiizumi, Arnold, Imamura, Inoue, and Honda, 1982; Nishiizumi, Arnold, Klein, and
Middleton, 1982; Nishiizumi, Klein, Middleton, Elmore, Kubiak, and Arnold, 1986; Nishiizumi, Elmore,
Kubik, Bonani, Suter, Wolfli, and Arnold, 1986; Tliniz et al., 1983; Vogt et al., 1986.
Imamura et al., 1979; Nishiizumi et. al., 1979, 1981,1983; Nishiizumi, Klein, Middleton, Elmore, Kubiak, and
Arnold, 1986; Nishiizumi, Elmore, Kubik, Bonani, Suter, Wolfli, and Arnold, 1986; Nishiizumi, 1987;
Nishiizumi, Reedy, and Arnold, 1988; Goswami and Nishiizumi, 1983.
Nishiizumi et al., 1979, 1981, 1983; Nishiizumi, Klein, Middleton, Elmore, Kubiak, and Arnold, 1986;
Nishiizumi, Elmore, Kubik, Bonani, Suter, Wolfli, and Arnold, 1986; Nishiizumi, 1987; Nishiizumi, Reedy,
and Arnold, 1988.
Fireman, 1979, 1980, 1983; Fireman and Norris, 1981; Andrews et al., 1982.
Evans, Wacker, and Reeves, herein; Nishiizumi, Reedy, and Arnold, 1988; Freundel et al., 1986.
56 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
Literature Cited
Andrews, H.R., R.M. Brown, G.C. Ball, N. Burn, Y. Imahori, J.C.D. Milton,
W.J. Workman, and E.L. Fireman
1982. 14C Content of Antarctic Meteorites Measured with the Chalk River
MP Tandem Accelerator. [Abstract.] In Abstracts, Fifth Interna-
tional Conference on Geochronology, Cosmochronology, and
Isotope Geology, Nikko, Japan, pages 8-9.
Cameron, I.R., and Z. Top
1974. Measurement of 26A1 in Stone Meteorites and Its Use in the
Determination of Orbital Elements. Geochimica et Cosmochimica
Ada, 38: 899-909.
Cressy, P.J.
1976. Cosmogenic Radionuclides in Stone Meteorites. NASA TN D-8241.
Evans, J.C., and L.A. Rancitelli
1980. Terrestrial Ages. In U.B. Marvin and B. Mason, editors, Catalog of
Antarctic Meteorites, 1977-1978. Smithsonian Contributions to the
Earth Sciences, 23:45-46.
Evans, J.C., L.A. Rancitelli, and J.H. Reeves
1979. 26A1 Content of Antarctic Meteorites: Implications for Terrestrial
Ages and Bombardment History. In Proceedings of the Tenth Lunar
and Planetary Science Conference, pages 1061-1072. New York:
Pergamon Press.
Evans, J.C., and J.H. Reeves
1987. 26A1 Survey of Antarctic Meteorites. Earth and Planetary Science
Utters, 82:223-230.
Evans, J.C., J.H. Reeves, and L.A. Rancitelli
1982. Aluminum-26: Survey of Victoria Land Meteorites. In U.B. Marvin
and B. Mason, editors, Catalog of Meteorites from Victoria Land,
Antarctica, 1978-1980. Smithsonian Contributions to the Earth
Sciences, 24:70-74.
Evans, J.C., J.H. Reeves, L.A. Rancitelli, and D.D. Bogard
1982. Cosmogenic Nuclides in Recently Fallen Meteorites: Evidence for
Galactic Cosmic-Ray Variations During the Period 1967-1978.
Journal of Geophysical Research, 87:5577-5591.
Fireman, E.L.
1979. 14C and 39Ar Abundances in Allan Hills Meteorites. In Proceedings
of the Tenth Lunar and Planetary Science Conference, pages
1053-1060. New York: Pergamon Press.
1980. Carbon-14 and Argon-39 in ALHA Meteorites. In Proceedings of
the Eleventh Lunar and Planetary Science Conference, pages
1215-1221. New York: Pergamon Press.
1983. Carbon-14 Ages of Antarctic Meteorites. In Lunar and Planetary
Science XIV, pages 195-196. Houston: The Lunar and Planetary
Institute.
Fireman, E.L., and T. Norris
1981. Carbon-14 Ages of Allan Hills Meteorites and Ice. In Proceedings of
the Twelfth Lunar and Planetary Science Conference, pages
1019-1025. New York: Pergamon Press.
Freundel, M., L. Schultz, and R.C. Reedy
1986. Terrestrial 81Kr-Kr Ages of Antarctic Meteorites. Geochimica et
Cosmochimica Ada, 50:2663-2673.
Fuse, K., and E. Anders
1969. Aluminum-26 in Meteorites VI, Achondrites. Geochimica et
Cosmochimica Acta, 33:1783-1980.
Goswami, J.N., and K. Nishiizumi
1983. Cosmogenic Records in Antarctic Meteorites. Earth and Planetary
Science Letters, 64:1-8.
Heyman, D., and E. Anders
1967. Meteorites With Short Cosmic-ray Exposure Ages, As Determined
From Their Al26 Content. Geochimica et Cosmochimica Acta,
31:1973-1981.
Imamura, M., K. Nishiizumi, and M. Honda
1979. Cosmogenic 53Mn in Antarctic Meteorites and their Exposure
History. Memoirs of the National Institute of Polar Research
(Japan), special issue, 15:227-242.
Moniot, R.K., T.H. Kruse, W. Savin, C. Tuniz, T. Milazzo, G.S. Hall, D. Pal,
and G.F. Herzog
1982. Beryllium-10 Contents of Stony Meteorites and Neon-21 Production
Rate. In Lunar and Planetary Science XIII, pages 536-537.
Houston: The Lunar and Planetary Institute.
Nishiizumi, K.
1984. Cosmic-Ray Produced Nuclides in Victoria Land Meteorites. In
U.B. Marvin and B. Mason, editors, Field and Labratory Investiga-
tions of Meteorites from Victoria Land, Antarctica. Smithsonian
Contributions to the Earth Sciences, 26:105-109.
1987. 53Mn, 26A1,10Be, and 36C1 in Meteorites: Data Compilation. Nuclear
Tracks Radiation Measurement 13:209-273.
Nishiizumi, K., J.R. Arnold, D. Elmore, R.D. Ferraro, H.E., Gove, R.C. Finkel,
R.P. Beukens, K.H. Chung, and L.R. Killius
1979. Measurements of 36C1 in Antarctic Meteorites and Antarctic Ice
using a Van de Graaff Accelerator. Earth and Planetary Science
Utters, 45:285-292.
Nishiizumi, K., J.R. Arnold, D. Elmore, X. Ma, D. Newman, and H.E. Gove
1983. 36C1 and 53Mn in Antarctic Meteorites and 10Be-36Cl Dating of
Antarctic Ice. Earth and Planetary Science Utters, 62:407-417.
Nishiizumi, K., J.R. Arnold, M. Imamura, T. Inoue, and M. Honda
1982. Cosmogenic Radionuclides in Antarctic Meteorites. In Seventh
Symposium on Antarctic Meteorites, pages 52-54. Tokyo, Japan:
National Institute of Polar Research.
Nishiizumi, K., J.R. Arnold, J. Klein, and R. Middleton
1982. 10Be and Other Radionuclides in Antarctic Meteorites and Associ-
ated Ice. Meteoritics, 17: 260-261.
Nishiizumi, K., D. Elmore, P.W. Kubik, G. Bonani, M. Suter, W. Wolfli, and
J.R. Arnold
1986. Age of Antarctic Meteorites and Ice II. [Abstract.] In Lunar and
Planetary Science XVII, pages 724-725. Houston: The Lunar and
Planetary Institute.
Nishiizumi, K., J. Klein, R. Middleton, D. Elmore, P.W. Kubik, and J.R.
Arnold
1986. Exposure History of Shergottites. Geochimica et Cosmochimica
Acta, 50:1017-1021.
Nishiizumi, K., M.T. Murell, J.R. Arnold, D. Elmore, R.D. Ferraro, H.E. Gove,
and R.C. Finkel
1981. Cosmic-Ray Produced 36C1 and 53Mn in Allan Hills-77 Meteorites.
Earth and Planetary Science Utters, 52:31-38.
Nishiizumi, K., R.C. Reedy, and J.R. Arnold
1988. Exposure History of Four Lunar Meteorites. [Abstract.] Meteoritics
23:294-295.
Reedy, R.C, J.R. Arnold, and D. Lai
1983. Cosmic Ray Record in Solar System Matter. Science, 219:127-135.
Tuniz, C, D.K. Pal, R.K. Moniot, W. Savin, T.H. Kruse, G.F. Herzog, and J.C.
Evans
1983. Recent Cosmic Ray Exposure History of ALHA 81005. Geophysical
Research Utters, 10:804-806.
Vogt, S., U. Herpers, R. Sarafin, P. Signer, R. Wieler, M. Suter, and W. Wolfli
1986. Cosmic Ray Records in Antarctic Meteorites. [Abstract.] In
Proceedings of the International Workshop on Antarctic Meteorites,
pages 55-57. Houston: The Lunar and Planetary Institute.
Wilkening, L.L., G.F. Herman, and E. Anders
1973. Al-26 in Meteorites VII: Ureilites, Their Unique Radiation History.
Geochimica et Cosmochimica Acta, 37:1803-1810.
7. Natural Thermoluminescence Levels and the
Recovery Location of Antarctic Meteorites
Fouad A. Hasan, Roberta Score, Benjamin M. Myers,
Hazel Sears, William A. Cassidy, and Derek W.G. Sears
In this article, the levels of natural thermoluminescence in
379 Antarctic meteorites are reported; 86 samples were from
the 1985 collection at the Allan Hills site, 88 were collected in
the Lewis Cliff region during the 1985-1986 season and 165
were collected at the Lewis Cliff sites during the 1986-1987
field season. An additional four samples came from the Allan
Hills site in 1986, and 36 came from six other ice fields. The
distributions of natural thermoluminescence data for the 1985
Allan Hills and 1986 Lewis Cliff collections are similar, with
peaks in the histograms at 32-63 krad with values ranging
between <1 krad and 327 ? 3 krad. On the basis of a study of 23
meteorites of known 26A1 content, the natural TL data for these
two collections seem consistent with the majority of the
meteorites having terrestrial ages of 150,000 ? 100,000 years,
while a smaller fraction fall in the 400,000 ? 200,000 year
range. On the other hand, samples from the 1985 Lewis Cliff
collections show a greater proportion of samples with natural
thermoluminescence in the 5-20 krad range, consistent with
the majority having ages in the order of 400,000 ? 200,000
years. The difference within the samples collected at Lewis
Cliff is related to collection site, the meteorites collected at
Meteorite Moraine having a peak at 50-63 krad, with relatively
little spread in natural TL, while the meteorites collected on the
Lewis Cliff Ice Tongue include a larger proportion with natural
TL in the 5-20 krad range. There seems to be a trend in natural
TL with location on the Lewis Cliff Ice Tongue, with natural
TL levels tending to be higher in the northern part of the
Tongue compared with the southern part, but it is not clear if
this is an effect of concentration mechanism or a few major
Fouad A. Hasan, Benjamin M. Myers, Hazel Sears, and Derek W.G.
Sears, Cosmochemistry Group, Department of Chemistry and Bio-
chemistry, University of Arkansas, Fayetteville, Arkansas 72701.
Roberta Score, Planetary Materials Laboratory, Lockheed, NASA
Johnson Space Center, Houston, Texas 77058. William A. Cassidy,
Department of Geology and Planetary Sciences, University of
Pittsburgh, Pittsburgh, Pennsylvania 15260.
pairings. 14% of the 379 samples have low natural TL (<5
krad), which can be attributed to recent heating (close solar
passage, shock, or atmospheric heating). Three meteorites have
extremely high natural TL strongly suggestive of high radiation
doses or low temperatures in space (these are ALH85033,
LEW85448, and LEW86286), while a further 18 have natural
TL values in excess of 100 krad and possibly experienced high
extraterrestrial radiation doses or low temperatures.
Introduction
The mineralogical and petrographic surveys made on
Antarctic meteorites as part of their initial description identify
meteorites which are members of rare or previously unknown
classes. However, they do not generally identify members of
well-populated classes which have experienced unusual histo-
ries, such as particularly long or short terrestrial ages, unusual
orbits, or other events resulting in anomalous thermal or
radiation histories. To some degree, 26A1 measurements
provide such information. Natural thermoluminescence (TL)
measurements provide data which is complementary to the
information available using cosmogenic isotopes and other
techniques, and can help in the identification of meteorites with
interesting and unusual histories. They can also provide an
indication of relative terrestrial ages, and TL measurements can
be useful in identifying fragments of a single meteorite (i.e.,
pairing). The natural thermoluminescence of meteorites was
recently reviewed by Sears and Hasan (1986) and Sears (1988).
Thermoluminescence is a measure of the number of excited
state electrons in a suitable crystalline lattice. In the chondritic
meteorites the lattice is usually feldspar, but it can, on occasion,
be various calcic minerals, forsterite, enstatite, quartz, or other
trace constituents. The means of excitation is the passage of
ionizing radiations, and natural thermoluminescence measure-
ments have successfully been applied to radiation dosimetry
and pottery dating for many years; in both cases the TL level is
57
58 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
used to determine the absorbed dose. In meteorites, because of
the larger dose rates and longer time scales involved, the
number of excited electrons is determined by an equilibrium
between the rate of excitation and de-excitation, the de-
excitation being a thermally controlled process. Simple
theoretical treatments yield the following relationship between
natural TL level (k), dose rate (R) and temperature (T, in ?K):
k= ??
1+aRv
where the other parameters are factors describing the TL
process: s, the Arrhenius factor; k is Boltzmann's constant; E is
the difference in energy of the excited state electrons and the
conduction band; a is the rate constant for excitation of
electrons; 1^ is the maximum TL that can be induced (e.g.,
Sears, 1988). Any event in the history of a meteorite which
involves a change in radiation dose and temperature will affect
natural TL levels to some extent.
The calculated black-body temperature for a meteorite at 1
a.u. is 240 K (assuming plausible values for size and albedo)
and dose rates are in the order of 1 rad/year. On earth,
temperatures and dose rates are probably around 293 and 1
mrad/year, respectively. A relationship between natural TL and
terrestrial age is therefore to be expected as the equilibrium TL
level falls from its extraterrestrial value to its terrestrial value
(Sears and Mills, 1974; Melcher, 1981a; McKeever, 1982).
Thus, taking s = 2 x 1013/sec, E = 1.43 eV (McKeever, 1982),
this simple treatment suggests that at temperatures observed in
the central U.S. (say 15? C) natural TL levels decay by a factor
of 20 in about 5 x 104 years, while at Antarctic temperatures
(say -5? C) the TL fades by a factor of about 20 in 3 x 106 years.
This relationship between natural TL and terrestrial age is
borne out, to some degree quantitatively, by studies in which
natural TL levels are compared with terrestrial ages determined
by cosmogenic isotopes (Sears and Durrani, 1980; Hasan et al.,
1987, see below). It is the case, however, that a small
proportion of meteorites have low levels of natural TL which
cannot be attributed to large terrestrial ages, and these must
have experienced a recent heating event sufficient to lower their
natural TL.
At a perihelion of 0.722 a.u. (the smallest perihelion
observed for bright fireballs falling into the Prairie Network
camera system), the black body temperature is 236? K. The
Lost City meteorite had an orbit with a perihelion of 0.967 a.u.,
at which distance the black body temperature is 275? K.
Substitution of these temperature values into the above
equation shows that a factor of 100 difference in natural TL
level could result from these differences in perihelion (McKee-
ver and Sears, 1980; Melcher, 1981b).
Of course, there are other means by which the meteorite
could have been heated, such as shock-heating. The tempera-
tures involved do not have to be high, but it is necessary for the
heating to have occurred sufficiently recently that the equilib-
rium has not had time to re-establish itself. This time period is
unclear, but theoretical treatments seem to indicate time
periods in the order of 105 years. Another major heating event
is passage through the atmosphere, but the effects are limited to
the outermost centimeter or less (Vaz, 1971; Sears, 1975;
Melcher, 1979). In addition, a factor of two variation in natural
TL levels due to gradients in the cosmogenic dose rate
throughout meteorites has been reported (Vaz, 1971; Sears,
1975; Lalou et al., 1970).
Many of these factors appear to have been involved in
determining the natural thermoluminescence levels in 23
Antarctic meteorites of known 26A1 activity discussed by Hasan
et al. (1987). In Figure 7-1 the earlier data have been replotted
using our current methods of natural TL data reduction (see
below) and normalizing the 26A1 activity to Si, the major target
for 26A1 production. (These changes result in a slightly
improved correlation coefficient, 0.69 compared to 0.62 in the
paper by Hasan et al. (1987). While 17 meteorites lie on or near
a regression line, six plot well below the line and have
presumably suffered recent heating. Two of the six are
shock-blackened L6 chondrites (RKPA79001 and
RKPA80202, which may be paired), and the heat associated
with the shock event may have lowered their natural TL. Two
others, which also are paired, have rather high 26A1 activities;
this situation is analogous to that for Malakal which is known
to have experienced an unusual thermal and radiation history
(Cressy and Rancitelli, 1974; Melcher, 1981a,b). These matters
were discussed by Hasan et al. (1987). Based on our
interpretations of Figure 7-1, we may assume that natural TL
values of significantly less than ~5 krad imply recent heating,
while values greater than this seem to be reflecting differences
in history analogous to those responsible for the 26A1 range,
predominantly differences in terrestrial age (and, on occasion,
low cosmic ray exposure age). We can get some feel, albeit
very approximate, of the terrestrial ages involved from a
compilation of terrestrial ages by Nishiizumi (1984); five of the
meteorites in the natural TL-26A1 "cluster," between 30-80
krad and 250-350 dpm/kg Si, have a mean terrestrial age of
150,000 ? 100,000 years, while six meteorites in the "cluster"
corresponding to 10-30 krad and 150-250 dpm/kg Si have a
mean terrestrial age 400,000 ? 200,000 years. These individu-
als and their terrestrial ages are listed in table 2 of Hasan et al.
(1987). ALHA78008 has an unusual radiation history. Its low
26Al activity (and presumably its low natural thermolumines-
cence relative to other meteorites involved in the regression
line) reflects low cosmic ray exposure, rather than simply a
particularly large terrestrial age (Nishiizumi et al., 1979).
In the present paper, we report natural TL data for 379
Antarctic meteorite fragments, we present histograms for most
of them (separated into various find sites), and we discuss some
possible interpretations of these data.
Experimental Procedures
Our data are listed in Table 7-1. Most of the data were
gathered by Fouad Hasan, while data for 27 samples were
NUMBER 30 59
100 150 200 250 300 350 400
26Al (dpm/kg Si)
FIGURE 7-1.?Plot of natural thermoluminescence against 26A1 activity for 23 Antarctic meteorites. (The samples
are from collections made between 1976 and 1981 at Allan Hills, Meteorite Hills, and Reckling Peak and may be
identified from table 2 in Hasan et al., 1987.) The data are from Hasan et al. (1987), and references therein, but
the TL data have been converted to doses using the method of Hasan et al. (1989) and the Al-26 activities have
been calculated relative to Si assuming 17.2% Si for H chondrites and 18.9% Si for L chondrites. The solid line
is a regression line through 17 meteorites and has the equation Log(Natural TL) = 0.00250 26A1 + 0.8610, and
correlation coefficient 0.69. The broken lines connect samples for which there is evidence for pairing (Scott,
1984).
60 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE 7-1.?Natural thermoluminescence data for Antarctic meteorites. These data supersede previous TL data
(October 1987, April 1988, and February 1989 data sets). The quoted uncertainties are the standard deviations
shown by replicate measurement of a single aliquot.
Specimen
number
ALH85016
ALH85017
ALH85018
ALH85020
ALH85023
ALH85026
ALH85027
ALH85028
ALH85029
ALH85030
ALH85031
ALH85033
ALH85034
ALH85035
ALH85037
ALH85038
ALH85039
ALH85040
ALH85041
ALH85042
ALH85043
ALH85044
ALH85045
ALH85048
ALH85052
ALH85054
ALH85056
ALH85059
ALH85062
ALH85063
ALH85065
ALH85066
ALH85070
ALH85071
ALH85073
ALH85075
ALH85076
ALH85077
ALH85079
ALH85O8O
ALH85082
ALH85083
ALH85084
ALH85086
ALH85087
ALH85090
ALH85091
ALH85094
ALH85097
ALH85098
ALH851OO
ALH85102
ALH85103
ALH85104
ALH85105
ALH85107
ALH85108
ALH85110
Natural TL
(krad at 250? C)
40?3
3.6 + 0.6
33.9 ? 0.6
39 ?2
55 ?1
36 ?2
67 ?4
18?1
28.2 ? 0.9
29 ?1
0.9 ? 0.4
258 ?3
40?3
6.0 ?0.1
6.2 ? 0.4
27.2 ? 0.3
26.6 ? 0.3
40.5 ? 0.2
17.8 ?0.6
48 ?1
107 ?11
20.2 ? 0.3
63 ?2
15.1 ?0.4
2.1 ?0.5
7.7 ? 0.6
2.5 ?0.1
50 ?4
59 ?6
9.0 ?0.2
35.4 ? 0.3
77 ?2
104 ?2
5.3 ?0.1
74.2 ? 0.8
45.9 ? 0.7
16.9 ?0.4
8.3 ?0.2
92 ?1
57 ?5
14.7 ? 0.4
52 ?5
45 + 2
54 + 4
34 ?2
80 ?4
24 ?2
96 ?2
93 ?2
5.6 ? 0.2
57 ?2
1.7 ?0.2
58 ?1
0.56 ? 0.09
60 ?1
19.1 ?0.6
2?1
148 ?2
Specimen
number
ALH85112
ALH85114
ALH85115
ALH85118
ALH85119
ALH85120
ALH85122
ALH85123
ALH85124
ALH85125
ALH85127
ALH85128
ALH85129
ALH85131
ALH85132
ALH85133
ALH85135
ALH85136
ALH85137
ALH85141
ALH85142
ALH85143
ALH85144
ALH85146
ALH85151
ALH85152
ALH85155
ALH85156
ALH86600
ALH86601
ALH86602
ALH86603
BOW85800
DOM85501
DOM85502
DOM85503
LX)M855O4
DOM85505
DOM85506
LX)M85508
DOM85509
DOM85510
EET86800
EET86801
EET86802
GEO85700
GEO85701
GRO85203
GRO85204
GRO85205
GRO85207
GRO85208
GRO85209
GRO85210
Natural TL
(krad at 250? C)
48.0 ? 0.5
8.92 ? 0.07
10?l
38.0 ?0.3
-
10.1 ?0.1
1.9 ?0.4
74 ?2
6.9 ? 0.3
10.1 ?0.1
1.5 ?0.2
4.3 ?0.1
36 ?2
32.2 ? 0.5
13 ?1
57 ?4
43.6 ?0.5
20?l
2.0 ?0.3
21.5 ?0.4
26.2 ? 0.2
5.7 ?0.1
96 ?2
59 ?2
155 ?2
88 ?2
104? 17
8.8 + 0.2
25.4 ?0.5
4 ?0.4
10.0 ?0.2
80 ?2
43 ?3
4.0 ? 0.5
34 ?2
36.3 ? 0.8
52 ?1
14.6 ? 0.3
56+1
20.6 ? 0.7
54.1 ?0.7
63 ?2
2.7 ?0.1
7.7 ?0.1
29 ?1
9.9 ? 0.2
72 ?2
110?4
43 + 2
25.8 + 0.3
77.3 ? 0.4
71.8 ?0.2
18?6
23.2 ? 0.3
Specimen
number
GRO85211
GRO85212
GRO85213
GRO85214
GRO85215
GRO85216
GRO85218
LEW85301
LEW85303
LEW85305
LEW85306
LEW85313
LEW85314
LEW85315
LEW85316
LEW85317
LEW85318
LEW85319
LEW85321
LEW85322
LEW85323
LEW85324
LEW85325
LEW85327
LEW85329
LEW85330
LEW85331
LEW85333
LEW85334
LEW85335
LEW85336
LEW85337
LEW85338
LEW85340
LEW85341
LEW85343
LEW85345
LEW85346
LEW85347
LEW85348
LEW85350
LEW85351
LEW85352
LEW85353
LEW85354
LEW85356
LEW85357
LEW85359
LEW85360
LEW85362
LEW85368
LEW85371
LEW85373
LEW85379
LEW85380
LEW85381
LEW85383
Natural TL
(krad at 250? C)
39 ?1
74 ?1
105 ?1
74 ?2
0.80 ?0.04
12.5 ?0.1
5.6 ? 0.2
0.41 ?0.03
31 ?2
0.036 ? 0.005
_
4.4 ? 0.04
35.8 ?0.5
22.5 ? 0.6
52?2
35.8 ? 0.2
12.2 ?0.1
7.3 ?0.1
41.8 ?0.8
41 ?1
6.6 ?0.1
32 ?3
20?l
0.37 ? 0.05
26?1
12.4 ?0.3
47 ?2
52 ?2
26.2 ? 0.5
6.9 ?0.1
82?4
10.2 ?0.4
25.6 ? 0.6
27.1 ?0.8
14?1
40?l
43 ?3
50?5
52?5
19.5 ?0.6
10.0 ?0.2
6.4 ?0.2
6.6 ? 0.3
0.5 ? 0.2
1.9 ?0.4
14?1
6.4 ? 0.2
24?1
0.16 ?0.01
8.0 ?0.3
0.32 ? 0.02
24 ?3
20 ?3
14.4 ?0.3
6.9 ?0.1
7.8 + 0.3
34 ?2
NUMBER 30 61
TABLE 7-1.?Continued.
Specimen
number
LEW85384
LEW85385
LEW85386
LEW85398
LEW85402
LEW854O3
LEW854O4
LEW854O5
LEW854O6
LEW85413
LEW85418
LEW85420
LEW85423
LEW85426
LEW85427
LEW85428
LEW85429
LEW85433
LEW85441
LEW85443
LEW85445
LEW85446
LEW85448
LEW85449
LEW85450
LEW85451
LEW85454
LEW85455
LEW85456
LEW85457
LEW85458
LEW85459
LEW85460
LEW85461
LEW85463
LEW85464
LEW85465
LEW85472
LEW86001
LEW86002
LEW86011
LEW86012
LEW86013
LEW86014
LEW86015
LEW86016
LEW86017
LEW86018
LEW86019
LEW86020
LEW86021
LEW86022
LEW86023
LEW86O24
LEW86025
LEW86026
LEW86028
LEW86030
LEW86031
LEW86033
Natural TL
(krad at 250? C)
48 ? 0.5
8.2 ?0.1
0.090 ? 0.0O4
14?1
31.0?0.9
18.2 ?0.4
35 ?1
5.9 ? 0.2
22 ? 0.4
7.9 ?0.2
10.1 ?0.2
96 ?4
31.8 ?0.2
6.5 ?0.1
77?4
13.6 ?0.4
54 ?1
93 ?1
0.60 ? 0.01
46 ?1
25.4 ? 0.5
48 ?1
206?5
6.2 ? 0.4
3.2 ? 0.6
0.88 ? 0.02
1.76 ?0.01
3.4 ? 0.3
62.5 ? 0.6
1.63 ?0.03
33 ?0.06
1.7 ?0.1
11.24 ?0.5
77 ?2
1.5 ?0.1
12.5 ?0.3
5.3 ? 0.2
24.2 ? 0.7
28 ?4
13?3
157 ?1
50.8 ?0.9
93 ?2
93 ?2
122 ?6
8.2 ? 0.3
17?1
-
114.8 ?0.7
37.0 ?0.2
36 ?2
_
32 ?3
21.9 ?0.1
0.9 ?0.1
64?2
38 ?2
75. ? 0.6
127 ?2
62 ?2
Specimen
number
LEW86035
LEW86037
LEW86039
LEW86040
LEW86041
LEW86043
LEW86044
LEW86047
LEW86050
LEW86053
LEW86055
LEW86056
LEW86057
LEW86060
LEW86070
LEW86072
LEW86073
LEW86074
LEW86076
LEW86077
LEW86O78
LEW86079
LEW86081
LEW86083
LEW86084
LEW86085
LEW86086
LEW86088
LEW86089
LEW86090
LEW86091
LEW86096
LEW86098
LEW86099
LEW86101
LEW86104
LEW86107
LEW86110
LEW86111
LEW86115
LEW86118
LEW86119
LEW86120
LEW86123
LEW86134
LEW86135
LEW86138
LEW86152
LEW86160
LEW86161
LEW86163
LEW86164
LEW86165
LEW86166
LEW86168
LEW86174
LEW86181
LEW86183
LEW86186
LEW86195
Natural TL
(krad at 250? C)
96.0 ? 0.2
79 ?1
5?2
139 ?5
2.34 ? 0.08
24.8 ?0.3
21.9 ?0.9
32.2 ?0.8
136 ?14
52 ?5
37.1 ?0.5
11 ? 0.6
77 ?6
1.4 ?0.07
58 ?1
60.5 ? 0.6
47 ?4
47 ?1
42.7 ? 0.9
101 ?6
107 ?4
66.7 ? 0.4
93 ?1
36 ?2
29 ?1
19 ?1
93 ?2
54.9 ?0.4
4.7 ?0.3
6.9 ?0.1
12.7 ?0.1
76 ?1
2.9 ?0.1
9.7 ? 0.4
6?1
27.2 ? 0.2
40?2
53.2 ? 0.5
59 ?28
52.5 ? 0.7
3.6 ? 0.65
1.7 ?0.08
22.9 ?0.9
21 ?3
-
88 ?4
196 ? 22
107 ?2
10.2 ?0.2
69?2
10?3
13.1 ?0.5
50.6 ? 0.7
2.3 ?0.2
96?2
93 ?4
16?1
22.3 ? 0.6
17.9 ?0.3
16.0 ?0.5
Specimen
number
LEW86199
LEW86203
LEW86204
LEW86206
LEW86207
LEW86211
LEW86213
LEW86215
LEW86225
LEW86226
LEW86228
LEW86232
LEW86238
LEW86241
LEW86249
LEW86250
LEW86251
LEW86252
LEW86255
LEW86258
LEW86266
LEW86268
LEW86273
LEW86282
LEW86286
LEW86295
LEW86302
LEW86305
LEW86311
LEW86312
LEW86314
LEW86317
LEW86327
LEW86337
LEW86340
LEW86344
LEW86349
LEW86350
LEW86352
LEW86354
LEW86360
LEW86364
LEW86366
LEW86367
LEW86368
LEW86371
LEW86376
LEW86380
LEW86382
LEW86385
LEW86388
LEW86393
LEW86395
LEW86396
LEW86397
LEW86407
LEW86418
LEW86438
LEW86442
LEW86451
Natural TL
(krad at 250? C)
27.6 ?0.2
16?3
9.7 ?0.1
96 ?1
8?1
6?1
13?2
9.0 ?0.9
42.5 ?0.7
64?2
55.8 ?0.9
62 ?4
59 ?9
20 ?1
17?1
45 ?2
55.8 ?0.7
155 ?19
60.7 ?0.6
4?2
24.2 ? 0.6
16?1
31 ?1
89 ? 0.2
327 ?3
5.7 ? 0.3
1.7 ?0.1
33 ?1
53 ?1
19.5 ?0.1
74?2
68 ?2
19.6 ?0.1
53 ?2
96 ?8
19.4 ?0.7
84 ?2
3?1
20.4 ?0.1
25.0 ?0.3
57 ?1
29.7 ?0.3
44?1
8?2
96?4
28.4 ? 0.8
9.9 ? 0.6
45 ?9
3.76 ?0.07
50?l
67?2
21.7 ?0.4
22.5 ?0.1
2.6 ?0.2
25.9 ? 0.3
16.5 ?0.1
0.85 ? 0.07
88 ?2
28.7 ? 0.6
52?2
62 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE 7-1.?Continued.
Specimen
number
LEW86463
LEW86465
LEW86466
LEW86470
LEW86471
LEW86472
LEW86473
LEW86479
LEW86485
LEW86489
Natural TL
(krad at 250? C)
30 ?4
39.6 ? 0.7
47 + 1
21.3 ?0.4
5 ?0.6
42.7 ? 0.3
87.1 ?0.2
80 ?10
28 ? 0.9
30.0 ? 0.9
Specimen
number
LEW86490
LEW86499
LEW86500
LEW86503
LEW86514
LEW86515
LEW86522
LEW86525
LEW86528
LEW86534
Natural TL
(krad at 250? C)
58.5 + 0.2
13.5 ?0.5
38 ?1
28.4 ?0.3
63.0 ? 0.8
54 ?1
0.9 ? 0.2
7.3 ?0.1
27 + 0.3
14.4 + 0.4
Specimen
number
LEW86544
LEW86546
LEW86549
QUE86900
RKP867OO
RKP86701
RKP86702
RKP86703
RKP86704
RKP86705
Natural TL
(krad at 250? C)
18.9 ?0.3
57 ?2
52 ?4
16?7
9?1
37.8 ?0.8
12?1
10.2 ?0.4
38?2
13.7 ?0.4
gathered by Roberta Score. Over the eighteen month period
during which the data were gathered, which is also the first
eighteen months of the project, our techniques and procedures
were constantly improved and, therefore, the data vary in
quality. The procedures are essentially those described by
Hasan et al. (1987), but improvements concerned primarily the
criteria for the selection of samples and subsequent storage
conditions. Initially, samples were taken randomly. Later, an
attempt was made to take samples at least 1 cm from any
obvious fusion crust. Most recently, sampling was restricted to
those meteorites in which it was possible to take samples at
least 1 cm away from all existing surfaces. This restricts the
measurements to samples >20g. Samples in the present data
base were sent from JSC to the TL laboratory at Arkansas
through the United States mail. In the future, samples will be
hand-carried to avoid the danger of accidental heating in transit.
We also have developed a means of standardizing our
reporting procedure, so that a single datum for each meteorite
is reported. The natural TL signal must be normalized to
remove the major effects of meteorite-to-meteorite differences
in TL sensitivity due to sample heterogeneity, shock, and
metamorphism. There are two commonly used means of doing
this, and the relative advantages and disadvantages of each
were discussed by McKeever and Sears (1980). Here we use a
composite method described by Hasan et al. (1989). It is
important to note that (1) these new data replace both measures
of natural TL in earlier versions of our data (Antarctic Meteoric
Newsletter, 11(1), 11(2)); and (2) the uncertainties quoted refer
only to the standard deviation shown by replicate measure-
ments of a single powder and not to total accuracy, which
would require measurements on several separate chips of
meteorite. We quote natural TL values observed at 250? C,
since this appears to be the optimum temperature: low enough
to be sensitive to the events of interest and yet high enough to
avoid the most trivial heating (Melcher, 1981a,b; Hasan et al.,
1987, 1989).
Results and Discussion
Histograms of natural TL values for the present samples
from the Allan Hills and Lewis Cliff regions are shown in
Figure 7-2. The histograms have been labeled to identify
individual meteorites in the belief that in this form the data will
be most helpful, especially with regard to identifying paired
meteorites. Unfortunately, most of the samples are unclassified
at the present time, and there is little other information relevant
to pairing.
The distribution in natural thermoluminescence for the 1986
samples from Lewis Cliff resembles that for the Allan Hills
1985 samples, but the Lewis Cliff 1985 samples seem to show
a distribution that favors lower values (Hasan and Sears, 1988).
The distribution of natural TL data for the Allan Hills 1985
meteorites shows a peak in the 32-63 krad intervals, consistent
with the cluster in Figure 7-1 showing a mean terrestrial age of
150,000 ? 100,000 years. Seventy-five per cent of the samples
fall in the range 5-100 krad, while three show values
exceeding 125 krad, and one (ALH85033) is particularly
noteworthy at 258 ? 3 krad. The other highs are 148 ? 2 krad
(ALH85110) and 155 ? 2 krad (ALH85151). Such values seem
high even for observed falls, and may indicate meteorites which
have experienced high radiation doses or unusually low storage
temperatures in space. The distribution tails more slowly
toward lower values. Thirteen samples (i.e., 15% of all the
ALH85 meteorites) register below the 5 krad level we would
associate with heated samples, affected by small perihelia,
recent shock heating, or atmospheric heating. There are some
minor peaks in the histogram (e.g., those at 5.0-6.3 krad and
1.6-2.5 krad) which might indicate that some of the individuals
in these peaks are paired. Of the five meteorites in the 5.0-6.3
krad range, three (ALH85071, 85098, and 85143) are H5
chondrites and are possibly paired. The other two are an H6
chondrite (ALH85037) and an LL6 chondrite (ALH85035).
The group in the 1.6-2.5 krad range are two H5 chondrites
(ALH85102, 85122), which may be paired, two H6 chondrites
(ALH85052, 85108), which also may be paired, and one LL6
chondrite (ALH85137).
The 1985 collection from the Lewis Cliff site does not seem
to show any tendency to an overall "preferred" value. Instead,
values are fairly uniformly spread between 7.3 and 63 krad,
although there is an indication that the distribution is bimodal
NUMBER 30 63
with a hiatus in the 16 to 20 krad interval. The 20-63 krad
range corresponds to the "cluster" in Figure 7-1 with 150,000
? 100,000 year terrestrial ages, while the 5-16 krad range
corresponds, approximately, to the "cluster" in Figure 7-1 with
400,000 ? 200,000 year terrestrial ages. There is only one
Lewis Cliff sample with natural TL greater than 100 krad,
namely LEW85448 (206 ? 5 krad), whereas six samples in the
Allan Hills 1985 data set had values this high. Eighteen
samples, making up 17% of the Lewis Cliff 1985 collection,
have natural TL less than 5 krad and have presumably suffered
some form of recent heating.
The shape of the histogram for the LEW86 samples
resembles that of the ALH85 samples, but with a more
pronounced peak at 50-63 krad. Seventy per cent of the
samples have values between 13 and 100 krad, which is very
similar to the group in Figure 7-1 that has a mean terrestrial age
of 150,000 ? 100,000 years. There are also minor peaks at
79-100, 25-32, 7.9-10 krad, which may not be significant.
High values are relatively common in the LEW86 data, 12
meteorites (7.2%) having values over 100 krad with
LEW86286 at a remarkable 327 ? 3 krad, suggestive of high
radiation doses or low temperatures in space. Eighteen
meteorites (11% of the LEW86 samples) have values below 5
krad, suggestive of recent heating.
The difference in the distribution of natural TL data between
the 1985 and 1986 collections at Lewis Cliff is related to find
location. Histograms of the natural TL in samples collected on
the Lewis Cliff icefields are shown in Figure 7-3. The
meteorites have been separated into those found at Meteorite
Moraine and those found on the Ice Tongue (Figure 7-4, 7-5),
and the latter have also been subdivided according to latitude
(Figure 7-4). The northernmost tip of the Tongue has not yet
been systematically searched, so the lack of meteorites in the
latitude intervals numbered 8-10 in Figure 7-3 is not
significant. Nevertheless, it is clear that the distribution of
meteorites over the region is not random, but that meteorites
tend to cluster along the western edge of the Tongue. The
latitude intervals are not equal, but were chosen to separate
meteorites found on the Upper Ice Tongue from those found on
the Lower Ice Tongue; these regions are separated by a steep
step in the ice surface.
The peak in the histogram for the Lewis Cliff 1986 samples
(50-63 krad), which is absent in the distribution for the 1985
Lewis Cliff samples, is due, in large part, to the meteorites from
Meteorite Moraine. On the basis of the appearance of
hand-specimens, considerable pairing among the Meteorite
Moraine samples was suspected, and the spread in TL data is
less for this site than the others. However, only 25 of our 67
Meteorite Moraine meteorites have yet been classified (10 are
H5, 9 are L6, 4 are H6, 1 is LL6, and 1 is L4), while 10 of the
13 in the 50-63 krad peak are unclassified; the other three are
L4, L6, and LL6.
Most of the 13% of the samples with natural TL levels below
5 krad were found on the upper part of the tongue (latitude
intervals 1-5). Furthermore, there may be a weak tendency for
the histograms to be skewing to higher TL values as one
proceeds from the upper part of the Tongue to the lower part
(i.e., proceeds north); intervals 3, 4, and 5, for instance, have
about half of the samples with TL >5 krad in the range 5-20
krad, while the intervals 6 and 7 have the bulk of their samples
in the range 16-100 krad. It is possible that a few major
pairings are responsible for this spatial distribution. However,
it is also possible that systematic variations in terrestrial age
(and therefore natural TL) with location on the ice could result
from the mechanisms by which the meteorites were accumu-
lated (e.g., Bull and Lipschutz, 1982; Annexstad, 1986;
Drewry, 1986). It will be necessary to make a careful study of
potential pairing before seriously examining the possibility of
a spatial variation in natural TL levels at this field. It will also
help to have data for samples from the remainder of the ice
field. The northern tip of the Lewis Cliff Ice Tongue is the
prime site for the 1988-1989 field season.
Data for 36 samples collected at other sites, and a further 4
samples collected in the Allan Hills region in 1986, are listed in
Table 7-1 but are too few for meaningful discussion of possible
trends. Four of the samples have natural TL values less than 5
krad, and two have values in excess of 100 krad (these are listed
below). Three of the 5 samples collected at Reckling Peak in
the 1986-1987 season have values in the 7.9-16 krad range,
while the "preferred values" among samples collected at
Grosvenor Mountains and the Dominion Range during the
1985-1986 season, based on these very limited data, are in the
50-125 krad range.
Conclusions
Data for the first eighteen months of systematic measure-
ment of natural thermoluminescence levels in Antarctic
meteorites identify several meteorites with unusual histories,
allow some crude sorting of meteorites by terrestrial age, and
provide data which will be useful in the recognition of paired
meteorites. There is evidence in the data that the patterns of
natural TL levels vary with find site, which could have
implications for concentration mechanisms.
Based on a comparison with Figure 7-1, and the known
terrestrial ages for the samples in the plot determined from
cosmogenic isotopes, the majority of samples in Allan Hills
1985 and Lewis Cliff 1986 collections have terrestrial ages in
range 150,000 ? 100,000 years, with most of the remainder in
the order of 400,000 ? 200,000 years. For the Lewis Cliff 1985
collection, the majority of the meteorites have natural TL
values suggestive of terrestrial ages in the range 400,000 ?
200,000 years, with a smaller fraction in the 150,000 ? 100,000
year range.
Fourteen percent of the 379 Antarctic meteorites in the
present study have natural TL values suggestive of recent
heating (small perihelion orbits, shock heating, or heating
during atmospheric passage). These are as follows:
ALH85; 017, 031, 052, 056, 102, 104, 107, 112, 115, 119,
127, 128, 137,
24
22
20
18
16
14
12
10
6-
4
2-J
0
LEW 86
522
418
D25
302166
119 041
382 258 101 525 399 091 164
207 163
099 039 090 016 056 002 017 024 001
204 160 213 181
544
407 470 485
344 395 463
327 39; 442 500 472 165
312 352 397 465 466115
268 266 371305 380111
534 195
499 186
044 104
249 241364 083 366110
203 W3 354 055 250 088161
120 199 028 107
123 273 047 225 072 096
023 076 05C 057
085 043 064 021 374 033 CMC 014 31S 031
MO 073 012 >26
228 SV 282
388 20$
317 I74
314 168
22(135
086
070 079 037 378 050
013
081152 252
035 077 040
315 011
8
6
4-
2
LEW 85
426
381
380
357
352
351
465 335 413 337 379
418 428
350 398
472 423
406 402 458 384 456
372 340 404 345 42E
449 323 385 330 356 403 325 329 317 322 333 461 42C
313 405 319 362 318 341 348 315 303 314 321 316 427 336
445
371 338 383 343 347
359 334 324 331 346433
12
10-
8-
6-
4-
2-
0
ALH85
119 104
122 108
156
114 125 132 076136 338 026 MO
127 I02 052 056 017 128 D35 054 063 115 048 028 044 029 018 016 323 027 079 043 110
107 141 039 065 J42 ?C 07C 097
142 087 075 )83 123 144
037124 077 120 082 041 091 030 020 034 OSS 045 09C 070 151
131 t35
129 112
118 064 )86 152
062 06C 094 155
S?MMM 130.1 5 4.0 6.3 1Q 16 25 40 63
NATURAL THERMOLUMINESCENCE (krad)
FIGURE 7-2.?Histograms of natural TL values in 86 meteorites from the 1985 collection at the Allan Hills, 86
meteorites collected from the Lewis Cliff region in 1985-1986 and 162 meteorites collected in the Lewis Cliff
region in 1986-1987. Two samples from the LEW85 collection (LEW85305 and 85306), and three from LEW86
(LEW86022, 86018, and 86134) collections, plot off the graph to lower values.
12
10
8
6
4
2
METEORITE MORAINE
576
21S
399 091
344 393 371047 366 370 226 )81
)16 056 019 017 044 104 320 074 312 330 >13 )78 011
442 083 472 372 314 *79
337 470 364 028 225 053 196 03S 077 031
436
588(388 D?
84?14'S-84?13.5'S 10
84?14.5'S-84?14'S
84?15'S-84?14.5'S
4
2
0
6
4-
2
84?15.4'S-84?15'S
84?15.7'S-84?15.4'S
|i19[i66[09aj118| [iOi|o90f2O7[i6O 428 161 I20 107 033 161 314 015
4-
2
84?16'S-84?15.7'S
4-
2
84?16.5'S-84?16'S
84?17'S-84?16.5'S
84?17.5'S-84?17'S
2-
[34J| J315|340|324|446|
4-
2-
84?18'S-84?17.5'S
.IM05.!*0! J13.16'20.25'32.40"5?.63"74 -J'3 1.6 2? 2.5 a2 4.0 5?&3 7.9 ' 13 ^ 20 25 3210
 ia " w w ioo5i582O?251"
NATURAL THERMOLUMINESCENCE (krad)
FIGURE 7-3.?Histograms of natural TL values for meteorites collected in the Lewis Cliff region of the Antarctic
in the 1985-1986 and 1986-1987 field seasons. Samples from Meteorite Moraine and from the Lewis Cliff Ice
Tongue have been plotted separately, the latter being subdivided into 10 regions according to latitude; the sites
are located in Figure 7-4. The five samples plotting off the graphs to the left are distributed over the regions as
follows: region 2, LEW85305; region 3, LEW85306; region 6, LEW86134; region 10, LEW86022; Meteorite
Moraine, LEW86018.
66 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
/ Meteorite
Moraine
FIGURE 7-4.?Sketch map showing the locations of the regions referred to in
Figure 7-3. North is to the top of the figure, the Tongue is approximately 2.3 km
wide. The shading refers to moraine and snow (circles) and regions of the
highest meteorite densities (dots). Regions 8-10 were searched in the
1988-1989 field season and data are not yet available.
LEW85; 301, 305, 306, 313, 327, 353, 354, 360, 368, 386,
441, 450, 451, 454, 455, 457, 459, 463,
LEW86; 018, 022, 025, 041, 060, 089, 098, 118, 119, 134,
166, 258, 302, 350, 382, 396, 418, 522,
DOM85501, EET86800, GRO85215, ALH86601.
Three meteorites have exceptionally high natural thermolu-
minescence values which suggest high radiation doses or low
storage temperatures in space; these are ALH85033,
LEW85448 and LEW86286. Meteorites with natural thermolu-
minescence values greater than 100 krad, and for which the
possibility of exposure to high radiation doses or low
temperatures should be borne in mind, are:
ALH85; 043, 070, 110, 151, 155,
LEW86; 011, 015, 019, 031, 040, 050, 077, 078, 138, 152,
252.
ACKNOWLEDGMENTS.?We are grateful to Rene Martinez,
Cecilia Satterwhite, and Carol Schwarz for their help in various
forms, the MWG for their cooperation, Ralph Harvey for his
discussions, Steve McKeever and an anonymous reviewer for
helpful reviews, Raye Stucker for help in manuscript prepara-
tion, and Ursula Marvin for her gracious editorial assistance.
This work is supported by grants from the National Science
Foundation and the National Aeronautics and Space Admini-
stration (DPP-8613998 and NAG 9-8I/natural TL, respec-
tively, to DWGS, and DPP-8314496, to WAC).
Literature Cited
Annexstad, J.O.
1986. Meteorite Concentration Mechanisms in Antarctica. In J.O. An-
nexstad, L. Schultz, and H. Wanke, editors, Workshop on Antarctic
Meteorites. LPI Technical Report, 86-01, pages 23-25. Houston:
The Lunar and Planetary Institute.
Antarctic Meteorite Newsletter, 11(1), February. 1988.
Antarctic Meteorite Newsletter, 11(2), August. 1988.
Bull, C, and M.E. Lipschutz
1982. Introduction. In C. Bull and M.E. Lipschutz, editors, Workshop on
Antarctic Glaciology and Meteorites. LPI Technical Report, 82-03,
pages 6-26. Houston: The Lunar and Planetary Institute.
Cressy, P.J., and L.A. Rancitelli
1974. The Unique Cosmic-ray History of the Malakal Chondrite. Earth
and Planetary Science Letters, 22:275-283.
Drewry, D.J.
1986. Entrainment, Transport, and Concentration of Meteorites in Polar Ice
Sheets. In J.O. Annexstad, L. Schultz, and H. Wanke, editors,
Workshop on Antarctic Meteorites. LPI Technical Report, 86-01,
pages 37-47. Houston: The Lunar and Planetary Institute.
Hasan, F.A., M. Haq, and D.W.G. Sears
1987. The Natural Thermoluminescence of Meteorites; I: Twenty-three
Antarctic Meteorites of Known 26A1 Content. Proceedings of the
17th Lunar and Planetary Science Conference, Journal of Geophysi-
cal Research, 92:E703-E709.
Hasan, F.A., R. Score, and D.W.G. Sears
1989. The Natural Thermoluminescence Survey of Antarctic Meteorites; A
Discussion of Methods for Reporting Natural TL Data. Lunar and
Planetary Science XX, pages 383-384. Houston: The Lunar and
Planetary Institute.
Hasan, F.A., and D.W.G. Sears
1988. Thermoluminescence Evidence for a Terrestrial Age Difference
between Allan Hills and Lewis Cliff Meteorites. Lunar and
Planetary Science XIX, pages 457-458. Houston: The Lunar and
Planetary Institute.
Lalou, C, D. Nordemann, and J. Labyrie
1970. Etude Preliminaire de la Thermoluminescence de la Meteorite Saint
Severin. Compte Rendu Hebdomadaire des Seances de I'Academie
des Sciences, Serie B (Sciences Physiques), 270:2401-2404.
McKeever, S.W.S.
1982. Dating of Meteorite Falls Using Thermoluminescence: Application
to Antarctic Meteorites. Earth and Planetary Science Letters,
58:419.
McKeever, S.W.S., and D.W.G. Sears
1980. Natural Thermoluminescence of Meteorites: A Pointer to Orbits?
Modern Geology, 7:137-145.
Melcher, C.L.
1979. Kirin Meteorite: Temperature Gradient Produced during Atmos-
pheric Passage. Meteoritics, 14:309-316.
1981a. Thermoluminescence of Meteorites and their Terrestrial Ages.
Geochimica et Cosmochimica Acta, 45:615-626.
1981b. Thermoluminescence of Meteorites and their Orbits. Earth and
Planetary Science Letters, 52:39-54.
Nishiizumi, K.
1984. Cosmic-ray Produced Nuclides in Victoria Land Meteorites. In U.B.
Marvin and B. Mason, editors, Field and Laboratory Investigations
NUMBER 30 67
FIGURE 7-5.?Aerial photograph of the Lewis Cliff Ice Tongue looking northeast with the tongue in the
foreground. Note the step in the tongue, which is highlighted by the snow infilling. Meteorite Moraine is on the
center, extreme right of the photograph. (Photograph TMA999-044 of the United States Geological Survey).
of Meteorites from Victoria Land, Antarctica. Smithsonian Contri-
butions to the Earth Sciences, 26:105-109.
Nishiizumi, K., J.R. Arnold, D. Elmore, R.D. Ferraro, H.E. Gove, R.C. Finkel,
R.P. Beukens, K.H. Chang, and L.R. Kilius
1979. Measurements of 36C1 in Antarctic Meteorites and Antarctic Ice
Using a Van de Graff Accelerator. Earth and Planetary Science
Utters, 45:285-292.
Scott, E.R.D.
1984. Pairing of Meteorites Found in Victoria Land, Antarctica. In
Proceedings of the Ninth Symposium on Antarctic Meteorites.
Memoirs of National Institute of Polar Research (Japan), special
issue, 35:102-125.
Sears, D.W.G.
1975. Thermoluminescence Studies and the Pre-atmospheric Shape and
Mass of the Estacado Meteorite. Earth and Planetary Science
Letters, 26:559-568.
1988. Thermoluminescence of Meteorites: Shedding Light on the Cosmos.
Nuclear Tracks and Radiation Measurement/International Journal
68 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
of Radiation Applied Instrumentation, part D, 14:5-17. The Lunar and Planetary Institute.
Sears, D.W.G., and S.A. Durrani Sears, D.W.G., and A.A. Mills
1980. Thermoluminescence and the Terrestrial Age of Meteorites: Some 1974. Thermoluminescence and the Terrestrial Age of Meteorites. Mete-
Recent Results. Earth and Planetary Science Letters, 46:159-166. oritics, 9:47-67.
Sears, D.W.G., and F.A. Hasan Vaz, J.E.
1986. Thermoluminescence and Antarctic Meteorites. In J.O. Annexstad, 1971. Asymmetric Distribution of Thermoluminescence in the Ucera
L. Schultz, and H. Wanke, editors, Workshop on Antarctic Meteorite. Nature Physical Science, 230:23-24.
Meteorites. LPI Technical Report, 86-01, pages 83-100. Houston:
Appendix
Tables of ANSMET Meteorites
Terminology
Class and type: A = achondrite, unique; An = angrite; Au = aubrite; C = carbonaceous
chondrite; Chon. (unique) = unique or ungrouped chondrite; Di = diogenite; E = enstatite
chondrite; Eu = eucrite; Ho = howardite; H = high-iron chondrite; I = iron (I, IIA, IIB, FVA
= iron groups; silicate incl. = silicate inclusions); L = low-iron chondrite; LL = low-iron
low-metal chondrite; M = mesosiderite; Sh = shergottite; Ur = ureilite. Chondrite
petrologic type is indicated by digit following the abbreviation.
Olivine composition in mole percent fayalite (Fa), Fe2Si04.
Pyroxene (orthopyroxene or low calcium clinopyroxene) composition in mole
percent ferrosilite (Fs), FeSiO3.
Degree of weathering: A = minor; metal flecks have inconspicuous rust haloes, oxide
stain along cracks is minor. B = moderate; metal flecks show large rust haloes, internal
cracks show extensive oxide stain. C = severe; specimen is uniformly stained brown, no
metal survives, e = evaporite deposits visible to naked eye.
Degree of fracturing: A = slight; specimen has few or no cracks and none penetrate
the entire specimen. B = moderate; several cracks extend across the specimen, which can
be readily broken along the fractures. C = severe; specimen has many extensive cracks and
readily crumbles.
Locations: ALH = Allan Hills; BTN = Bates Nunatak; BOW = Bowden Neve; DRP
= Derrick Peak; DOM = Dominion Range; EET = Elephant Moraine; GEO = Geologists
Range; GRO = Grosvenor Mountains; ILD = Inland Forts; LEW = Lewis Cliff; MET =
Meteorite Hills; MIL = Miller Range; MBR = Mount Baldr; OTT = Outpost Nunatak; PCA
= Pecora Escarpment; PGP = Purgatory Peak; QUE = Queen Alexandra Range; RKP =
Reckling Peak; TIL = Thiel Mountains; TYR = Taylor Glacier.
Source of classifications: * = S.G. McKinley and K. Keil; t = S.J.B. Reed and S.O.
Agrell; $ = C.B. Moore; ? = M. Rhodes and S. Haggerty.
~ = Classified using refractive indices.
Abbreviations: n.d. = no data.
69
70 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE A.?Meteorites listed by source area in numerical sequence (fractions of grams in weight dropped unless
total weight is less than 1 gram).
Specimen
number
ALHA
76001
76002
76003
76004
76005
76006
76007
76008
76009
77001
77002
77003
77004
77005
77007*
77008*
77009
77010
77011
77012
77013*
77014
77015
77016*
77017*
77018*
77019*
77021
77022*
77023*
77025
77026*
77027*
77029*
77031*
77033
77034*
77036*
77038*
77039*
77041*
77042*
77043*
77045*
77046*
77047*
77049*
77050*
77051*
77052*
77054*
77056*
77058*
77060*
77061
77062
77063*
Weight
(g)
20151
1510
10495
305
1425
1137
410
1150
407000
252
235
780
2230
483
99
93
236
296
292
180
23
309
411
78
78
52
60
17
16
21
19
20
4
1
0.5
9
2
8
19
8
17
20
11
18
8
20
7
84
15
112
10
12
4
64
13
17
3
Class
and
type
L6
I
L6
LL3
Eu
H6
L6
H6
L6
L6
L5
C3O
H4
Sh
H5
L6
H4
H4
L3
H5
L3
H5
L3
H5
H5
H5
L6
H5
H5
H5
H5
L6
L6
C3O
L3
L3
L3
L3
H5
H5
LL6
H5
L3
H5
H6
L3
L3
L3
H5
L3
H5
H4
H5
LL5
H5
H5
H5
%Fa in
olivine
25
25
0-34
18
24
19
24
25
25
4-48
17-20
28
19.1
24.6
18
18
4-36
18
9-28
18
1-21
18.6
18.8
19.0
24.9
18
19.1
19.1
18
24.3
25.0
23.0
n.d.
8-38
n.d.
n.d.
19.0
18.5
30.7
19.0
1-37
18.7
19.0
n.d.
n.d.
n.d.
18.8
n.d.
18.5
18.8
18.8
28.1
18
18
18.0
%Fsin
pyroxene
21
21
0-53
37-57
16
21
17
21
21
22
2-25
15-27
23
16.7
20.6
16
15-18
1-33
16
1-35
17
4-24
17.1
16.3
17.0
21.4
17
17.0
16.8
17
20.7
21.5
2.6
n.d.
8-9
n.d.
n.d.
17.1
16.3
25.1
16.6
1-28
17.0
16.7
n.d.
n.d.
n.d.
16.5
n.d.
16.9
16.3
16.1
23.2
17
17
16.8
Degree of
weathering
A
A
A
A
Ce
B
B/C
B
B
B
Ae
C
A
B
A
C
C
C
Ce
B
C
Ce
B
B
B/C
B/C
C
A
B
C
B/Ce
B/C
A/B
B/C
C
B/C
B
A/B
A/B
A
A/B
B/C
A
A/B
C
B/C
B/C
A
B/C
B
A/B
B
A
B
B
B
Specimen
number
ALHA
77064
77066*
77069*
77070*
77071
77073*
77074
77076*
77078*
77079*
77081
77082*
77084*
77085*
77086
77087*
77088
77089*
77091*
77092*
77094*
77096*
77098*
77100*
77101*
77102
77104*
77106*
77108*
77111*
77112*
77113*
77114*
77115*
77117*
77118
77119
77120*
77122*
77124
77125*
77126*
77127*
77129*
77130*
77131*
77132*
77133*
77134*
77136*
77138*
77139*
77140
77142*
77143*
77144
Weight
(g)
6
5
0.8
18
11
10
12
2
24
8
9
12
44
46
19
31
51
8
4
45
7
2
8
18
4
12
6
8
0.7
52
22
2
45
154
21
8
6
4
5
4
19
25
4
2
25
26
115
19
19
4
2
66
79
3
39
8
Class
and
type
H5
H5
L6
H5
H5
H5
H5
H5
H5
H5
"H(?)
%Fain
olivine
18
19.0
25.4
18.4
18
18.8
18
19.5
19.5
18.2
"* 11
*(Acapulco-like)
H5
H5
H5
H5
H5
H5
L6
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H6
H5
H5
H5
L3
L5
H5
H5
H5
H5
H5
H5
H5
L5
H5
H5
H6
H5
H6
H6
H5
H5
H5
L3
H5
H5
H6
19.3
18.8
18.8
19
19.0
19
25.5
18.9
18.5
18.5
18.7
18.7
19.2
18.6
19
18.9
18.8
18.5
19.0
18.7
18.7
19.6
n.d.
24.4
19
18
18.5
19.1
19
17.2
18.3
25.0
18.9
18.9
19.2
19.0
19.0
18.9
19.1
19.2
18.6
8-44
18.9
18.7
19
%Fsin
pyroxene
17
17.4
21.4
16.8
17
17.7
17
16.1
16.7
15.8
11
16.5
16.8
17.6
17
16.7
17
21.4
16.1
16.5
16.2
17.1
16.7
16.4
17.0
15
16.9
16.5
15.9
16.6
16.7
17.2
17.2
n.d.
21.0
17
17
16.0
16.8
16
15.5
16.2
21.1
16.6
16.5
16.8
16.9
17.0
16.7
16.4
17.0
16.4
2-17
17.1
16.2
17
Degree of
weathering
B
A
B/C
B
B
A/B
B
B
B
A
B
A/B
A/B
B
C
B
C
B
B/C
A
B
A
B
A/B
B
B
A
A/B
A/B
C
A
B
B
B/C
A/B
C
C
A/B
B
C
A/B
A/B
B
B
A
A/B
A/B
A
A
A/B
A
A/B
Ce
A/B
A/B
B
NUMBER 30 71
TABLE A.?Continued.
Specimen
number
ALHA
77146*
77147*
77148
77149*
77150
77151*
77152*
77153*
77155
77156*
77157*
77158*
77159*
77160
77161*
77162*
77163*
77164
77165
77166*
77167
77168*
77170*
77171*
77173*
77174*
77175*
77176*
77177
77178*
77180
77181*
77182
77183
77184*
77185*
77186*
77187*
77188*
77190
77191
77192
77193*
77195*
77197*
77198*
77200*
77201*
77202*
77205*
77207*
77208
77209*
77211*
77212*
77213*
77214
Weight
(g)
18
19
13
26
58
17
18
12
305
18
88
20
17
70
6
29
24
38
31
139
611
25
12
24
26
32
23
55
368
6
191
33
1135
288
128
28
122
52
109
387
642
845
7
5
20
7
0.9
15
3
3
5
1733
32
27
17
8
2111
Class
and
type
H6
H6
H6
H6
L6
H5
H5
H5
L6
E4
H6
H5
L6
L3
H5
L6
L3
L3
L3
L3
L3
H5
L3
H5
H5
H5
L3
L3
H5
L3
L6
H5
H5
H6
H5
L3
H5
H5
H5
H4
H4
H4
H5
H5
L3
L6
H6
H5
H5
H5
H5
H4
H6
L3
H6
H5
L3
%Fain
olivine
18.9
19.0
18
19.1
25
18.9
18.7
19.2
24
0.8
18.6
18.9
24.4
3-46
19.3
25.3
n.d.
6-39
8-33
n.d.
2-41
19.0
n.d.
18.9
19.1
18.3
n.d.
0.3-34
18
1-36
24
20.0
19
19
17.8
n.d.
18.8
18.1
18.1
17-19
16-18
16-18
19.0
18.9
10-27
24.4
19.7
18.8
18.6
18.8
17.8
17
18.8
n.d.
18.9
18.6
? 1-49
%Fsin
pyroxene
16.9
16.6
16
16.9
22
16.4
16.9
16.7
20
1.5
15.7
16.9
20.8
6-40
17.1
20.9
n.d.
3-41
6-35
n.d.
3-17
16.5
n.d.
17.0
17.0
16.0
n.d.
1-37
16
2-40
20
17.3
17
16
15.9
n.d.
16.0
16.3
16.1
15-22
14-16
15-21
15.7
16.4
4-21
20.6
17.6
15.3
16.6
16.7
16.7
14
16.4
n.d.
17.0
16.5
4-23
Degree of
weathering
A/B
A/B
C
A/B
C
A
A
A
A/B
B
A/B
B
A/B
C
B
A
B/C
C
C
C
C
B
B/C
A/B
B
A
B/C
B
C
B/C
C
B
C
C
B
A/B
A/B
A/B
A/B
C
C
C
A
A
A/B
B
C
A
B
B
A/B
C
B
B/C
A/B
A
C
Specimen
number
ALHA
77215
77216
77217
77218*
77219
77220*
77221
77222*
77223
77224
77225
77226
77227*
77228*
77230
77231
77232
77233
77235*
77237*
77239*
77240*
77241*
77242*
77244*
77245*
77246*
77247*
77248*
77249
77250
77251*
77252
77253*
77254
77255
77256
77257
77258
77259
77260
77261
77262
77263
77264
77265*
77266*
77267*
77268
77269
77270
77271
77272
77273
77274
77275*
77277
Weight
(g)
820
1470
413
45
637
69
229
125
208
787
5878
15323
16
19
2473
9270
6494
4087
5
4
19
25
144
56
40
33
42
44
96
504
10555
69
343
24
246
765
676
1996
597
294
744
412
862
1669
11
18
108
104
272
1045
589
610
674
492
288
25
143
Class
and
type
L3
L3
L3
L5
M
H5
H4
H4
H4
H4
H4
H4
H5
H5
L4
L6
H4
H4
H5
H5
H6
H5
L3
H5
L3
H5
H6
H5
H6
L3
I
L6
L3
H5
L5
I
Di
Ur
H6
H5
L3
L6
H4
I
H5
H5
H5
L5
H5
L6
L6
H6
L6
L6
H5
H5
L6
%Fa in
olivine
22-26
15-35
17-25
23.4
26
17.7
15
18.0
17
19
17
18
18.9
18.5
22-25
24
17
14-21
18.9
18.5
18.7
18.8
n.d.
18.8
n.d.
19.2
19.2
18.8
18.7
7-35
25.0
22-28
19.2
23
13
18
18
7-23
24
15-19
19
17.6
19.6
24.7
18
24
24
18
24
24
18
18.3
24
%Fsin
pyroxene
9-21
14-23
9-26
19.1
24-28
16.0
13-15
15.3
15-23
17
16
16
16.6
16.3
18-29
21
15
15-17
16.7
15.8
15.9
16.0
n.d.
16.2
n.d.
17.2
16.5
16.4
16.7
2-25
21.3
2-22
16.9
20
23
12
16
15
1-28
21
13-16
16
15.9
17.7
20.9
16
22
21
16
20
20
16
15.6
20
Degree of
weathering
B
A/B
B
A
B
B
C
A/B
C
C
Ce
Ce
A
B
C
A/Be
C
C
A/B
A
B
A
C
B
B/C
A/B
B
A/B
B/C
C
B
B
A/B
A/B
A/B
Ae
B/Ce
C
C
B
B/Ce
A/B
B
B
A
C
Be
A/B
C
B/C
B
C
A
A/B
72 SMITHSONIAN CONTRIBUTIONS TO TO THE EARTH SCIENCES
TABLE A.?Continued.
Specimen
number
ALHA
77278
77279*
77280
77281
77282
77283
77284
77285
77286
77287
77288
77289
77290
77291*
77292
77293*
77294
77295*
77296
77297
77299
77300
77301*
77302
77303*
77304
77305
77306
77307
78001$
78002$
78003
780041
78005$
78006
78008
78010$
78012
78013
78015
78017$
78018$
78019
78021
78023
78025$
780271
78028
78029$
78031
78033$
78035
78037$
78038
78039
78040
Weight
(g)
313
175
3226
1231
4127
10510
376
271
246
230
1880
2186
3784
6
200
110
1351
141
963
952
261
235
55
236
79
650
6444
20
181
85
11
125
36
28
8
7
1
38
4
35
3
18
30
17
10
8
29
4
4
5
5
2
0.5
363
299
212
Class
and
type
LL3
H5
L6
L6
L6
I
L6
H6
H4
H5
H6
I
I
H5
L6
L6
H5
E4
L6
L6
H3
H5
L6
Eu
L3
L4
L6
C2
C3
H5
H6
L6
H5
H5
Ho
H5
H5
H5
L3
L3
L3
H5
Ur
H5
H5
H5
H5
H5
H4
H5
H4
H6
L3
L3
L6
Eu
%Fa in
olivine
11-29
18.8
24
24
24
25
18
17
18
19
18.9
24
24.7
17
0.8
24
24
11-21
18
24.9
n.d.
18-27
24
1-45
1-30
18.6
19.0
24
19.2
19.3
18
19.4
18
11-45
8-35
3-43
19.2
22
18
18
18.9
19.3
18
19.2
18
19.2
18
7-38
4-42
24
%Fs in
pyroxene
9-21
17.1
21
20
20
21
16
12-16
16
17
15.9
20
20.9
15
1.7
21
20
15-20
16
20.9
37-64
n.d.
13-19
21
1
1-12
20
25-61
16
16
1-31
18
16
16
16
16
16
2-19
21
33-52
Degree of
weathering
A
A
Be
B
B
A/B
C
C
cc
A
B
B
Ae
B
A/Be
A
A
C
A
A
B/C
B
B/C
A
Ae
B
A
C
B
A
B
B
B
B/C
A
B
B
B
C
B
A
Specimen
number
ALHA
78041$
78042
78043
78044
78045
78046
78047t
78048
78049$
78050
78051
780521
78053
78055$
78057
78059$
78062
78063$
78065$
78067
78069$
78070
78074
78075
78076
78077
78078
78079
78080
7808It
78082$
78084
78085
78086f
78088t
78090t
78092f
780941
780961
780981
78100
78101
78102
78103
78104
78105
78106
78107
78108
78109
78110
78111
78112
78113
78114
78115
781161
Weight
(g)
118
214
680
164
397
70
130
191
96
1045
120
97
179
14
9
9
11
77
7
8
4
10
200
281
276
331
290
5
25
18
24
14280
219
9
5
8
16
4
7
2
85
121
337
590
672
942
465
198
173
233
161
127
2485
299
808
848
128
Class
and
type
L3
L6
L6
L4
L6
L3
H5
L6
H5
L6
H4
H5
H4
L6
H4
L6
LL6
LL6
H6
H6
H6
L4
L6
H5
H6
H4
L6
H5
H5
H5
LL6
H4
H5
H6
H5
H5
H5
H5
H5
H5
I
L6
H5
L6
L6
L6
L6
H5
H5
LL5
H5
H5
L6
Au
L6
H6
H5
%Fa in
olivine
0-41
24
25
23-25
25
8-25
18.8
24
19.4
23
18
17.9
17
25.5
18
21.5
29
29.1
18.0
18
19.1
23
24
18
18
19
24
18
18
19.1
27.7
18
18
19.0
18.8
18.7
19.0
19.1
18.9
18.9
24
18
24
24
23
24
18
18
28
18
18
25
25
18
18.7
%Fsin
pyroxene
20
21
19-24
21
8-20
21
20
15-18
16
16
24
16
13-25
21
16
16
15-18
20
16
16
8-24
16
21
17
20
20
20
20
17 '
16
23
16
16
20
20
16
Degree of
weathering
B
B
B
B/C
B/C
B
A/B
B
B
C
C
B
B
A
B
B
B
B/C
B
C
A/B
A
B/Ce
Be
B/C
B
B
B
A/B
C
B/C
A/B
B/C
B/C
B
A/Be
B/C
B
B
NUMBER 30 73
TABLE A.?Continued.
Specimen
number
ALHA
78117$
78119$
78120
78121t
78122
78123$
78124
78125t
78126
78127
78128
78129$
78130
78131
78132
78133
78134
78135f
78136$
78137
78138$
781391
78140$
78141
781421
78145$
78146
781471
78149$
78150
78152
78153
78154$
78156
78157$
78158
78159
781601
78162$
78163$
78164
78165
78168$
78169$
78170
78171$
78172$
78173$
78174$
78176$
78178$
78180$
78182
78184
78186
78188
78189
Weight
(g)
4
103
44
30
5
18
28
19
607
195
155
128
2733
269
656
60
458
131
52
70
11
17
17
24
32
34
17
31
23
16
5
152
12
9
63
15
23
16
33
10
25
21
34
22
21
23
29
20
13
8
7
8
10
8
3
0.9
23
Class
and
type
H5
L3
H4
H5
H6
H5
H6
L6
L6
L6
H5
H5
L6
L6
Eu
L3
H4
H6
H5
H6
LL3
H5
H4
H5
L5
H6
H5
H5
L3
H5
H6
LL6
H5
L6
H4
Eu
H5
H5
L3
H5
H5
Eu
H4
H6
L3
L6
H4
H5
H5
L3
H5
L3
H5
H6
L3
L3
H6
%Fain
olivine
18.5
0-28
18
19.2
19
19.3
17
25.0
25
24
19
19.4
25
25
1-34
18
19.0
19.1
17
0-35
19.3
18.4
18
24.2
19.6
18
6
18-31
18
18
29
19.3
24
19.0
18
19.3
2-30
18.7
18
19.2
19.2
3-36
25.4
19.7
19.7
18.2
8-26
19.0
2-33
18
18
3-36
1-34
18
%Fs in
pyroxene
16
17
15
21
20
17
21
21
40-68
1-16
15-20
15
16
16
19.4
16
16
24
21
40-68
16
16
37-61
16
16
3-24
5-29
16
Degree of
weathering
A
A
B
B
B
B/C
C
B
B/C
B/C
A
B/C
B
A
B
B
A
B
B/C
B
B
A
B
B
A
B
B
B
B
B
B
B
B
B
B
C
Specimen
number
ALHA
78190
78191
78193
78194
78196
78197
78199
78201
78203
78205
78207
78209
78211
78213
78215
78217$
78219$
78221
78223
78225
78227
78229
78231
78233
78235$
78236
78238
78239$
78241
78243
78245
78247
78249
78251
78252
78253$
78255$
78257$
78259$
78261
78262
79001
79002
79003
79004
79005
79006
79007
79008
79009
79010
79011
79012
79013
79014
79015
Weight
(g)
20
20
13
25
11
20
13
10
11
9
8
12
11
10
6
8
8
5
6
5
2
2
2
1
19
14
10
16
7
2
4
3
4
1312
2789
7
3
2
6
5
26
32
223
5
35
60
41
142
12
76
25
14
192
28
11
64
Class
and
type
H5
H6
H4
H5
H4
H5
H5
H5
H5
H5
H6
H5
H6
H6
H6
H5
H5
H5
H4
H5
H5
H6
H6
H5
L3
L3
L3
L3
H5
L3
H5
H5
H6
L6
I
H5
H5
H5
H5
C2
Ur
L3
H6
LL3
H5
H6
H5
L6
H5
H5
H5
H5
H5
H5
H5
H5
%Fa in
olivine
18
18
18
18
18
18
18
18
18
18
19
18
18
18
18
18.8
19.4
18
18
18
18
18
18
18
8-28
2-37
2-34
1-34
18
1-36
18
18
18
23
18.9
19.4
19.2
19.7
0-50
22
6-39
16
10-38
16
18
18
23
17
18
17
18
17
18
18
17
%Fs in
pyroxene
16
16
16
16
16
16
16
16
16
16
17
15
16
15
16
16
16
16
16
15
16
16
3-26
3-21
16
3-30
16
16
16
20
1-8
19
2-31
18
5-26
14
16
15
19
15
15
15
16
15
16
16
15
Degree of
weathering
B/C
B/C
B/C
B
B
B/C
B
B
B
B
B
B/C
B
B/C
B/C
B
B
B
B
A
B
A
A
B/C
C
C
B
B/C
B
B/C
A/B
B
Ce
B/C
B/C
C
cB
B
74 SMITHSONIAN CONTRIBUTIONS TO TO THE EARTH SCIENCES
TABLE A.?Continued.
Specimen
number
ALHA
79016
79017
79018
79019
79020
79021
79022
79023
79024
79025
79026
79027
79028
79029
79031
79032
79033
79034
79035
79036
79037
79038
79039
79040
79041
79042
79043
79045
79046
79047
79048
79049
79050
79051
79052
79053
79054
79055
80101
80102
80103
80104
80105
80106
80107
80108
80110
80111
80112
80113
80114
80115
80116
80117
80118
80119
Weight
(g)
1146
310
121
12
4
29
31
68
22
1208
572
133
16
506
3
3
281
13
38
20
15
50
108
13
20
11
62
115
90
19
37
54
27
24
23
86
36
15
8725
471
536
882
445
432
178
125
168
42
331
313
233
306
191
89
2
34
Class
and
type
H6
Eu
L6
H6
H6
H5
L3,4
H4
H6
H5
H5
L6
H6
H5
H5
H5
L6
H6
H4
H5
H6
H5
H4
H5
H5
H5
L6
L3
H5
H5
H5
H6
H5
H5
L6
H5
H5
H6
L6
Eu
L6
I
L6
H4
L6
L6
L6
H5
L6
L6
L6
L6
L6
L6
H6
L6
%Fa in
olivine
17
23
17
17
18
1-28
17
17
17
18
24
18
18
16
16
24
18
17
18
18
17
16
18
18
18
23
2-38
18
18
18
18
18
18
23
17
18
18
24
24
24
19
24
24
24
18
24
24
24
24
24
24
17
24
%Fs in
pyroxene
15
28-53
20
15
15
17
9-22
14-17
15
15
16
20
16
16
14
14
20
16
14-18
16
16
15
15
15
16
16
20
2-29
15
15
16
16
15
15
20
15
16
16
20
34-52
20
20
16-19
20
20
20
16
20
20
20
20
20
20
15
20
Degree of
weathering
B/C
A
B/C
B
B/C
B
A/B
B/C
C
C
B
B
B
C
C
C
B
B
B
B
B
C
B
B
B
B
C
C
B
B
B
C
C
C
B/C
B/C
B
B/C
Be
A
B
B
C
B
B
B
B
B
B
B
B
B/C
B
B
B
Specimen
number
ALHA
80120
80121
80122
80123
80124
80125
80126
80127
80128
80129
80130
80131
80132
80133
81001
81002
81003
81004
81005
81006
81007
81008
81009
81010
81011
81012
81013
81014
81015
81016
81017
81018
81019
81020
81021
81022
81023
81024
81025
81026
81027
81028
81029
81030
81031
81032
81033
81034
81035
81036
81037
81038
81039
81040
81041
81042
Weight
(g)
60
39
50
28
12
139
35
47
138
93
5
20
153
4
53
14
10
5
31
255
164
44
229
219
406
37
17727
188
5489
3850
1434
2237
1051
1353
695
913
418
798
379
516
3835
80
153
1852
1595
727
252
255
256
252
320
229
206
195
729
534
Class
and
type
L6
H4
H6
H5
H5
L6
H6
H5
H4
H5
H6
H4
H5
L3
Eu
C2
C3V
C2
Lunar
Eu
Eu
Eu
Eu
Eu
Eu
Eu
I
I
H5
L6
L6
L5
H5
H5
E6
H4
L5
L3
L3
L6
L6
L6
L6
L3
L3
L3
H5
H5
H6
H5
H6
H6
H5
L4
H4
H5
%Fain
olivine
24
19
18
18
18
24
19
18
18
18
18
19
18
1-35
0-52
0-60
0-52
11-40
19
25
25
24
19
19
19
25
3-28
1-41
25
25
25
25
1-49
1-43
0-42
18
19
19
19
20
19
19
25
18
19
%Fsin
pyroxene
20
17
16
16
16
20
17
16
15-20
15
16
16-22
16
5-30
59
0-2
1
0-2
7-47
35-60
38-55
32-59
30-63
31-57
33-60
33-62
16
21
21
21
16
16
0-1
17
21
2-24
3-40
21
21
21
21
5-33
3-35
2-14
16
17
17
17
17
17
17
21
15-23
17
Degree of
weathering
B
B/C
B/C
C
B
B/C
A/B
B
B
B
B/C
B
B
B
Ae
Ae
A/B
A/B
A/B
A
A/B
A/B
A
A
A/B
A/B
Be
Be
B
B
B/Ce
Be
A
B/C
B
C
C
B
C
B
C
B/C
C
cc
B
C
C
B
C
A/B
B/C
C
C
NUMBER 30 75
TABLE A.?Continued.
Specimen
number
ALHA
81043
81044
81045
81046
81047
81048
81049
81050
81051
81052
81053
81054
81055
81056
81057
81058
81059
81060
81061
81062
81063
81064
81065
81066
81067
81068
81069
81070
81071
81072
81073
81074
81075
81076
81077
81078
81079
81080
81081
81082
81083
81084
81085
81086
81087
81088
81089
81090
81091 .
81092
81093
81094
81095
81096
81097
81098
81099
Weight
(g)
106
387
90
17
81
191
9
26
43
29
3
2
5
1
8
66
540
28
24
0.5
5
191
13
9
228
24
7
4
2
3
3
8
16
10
4
6
7
17
5
6
7
16
16
6
8
4
11
10
12
16
271
152
59
83
80
71
152
Class
and
type
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
L3
H6
H6
H4
H4
H4
M
L3
L3
H5
H5
H5
L3
L3
H5
H4
L3
H5
H5
H5
H4
H4
H5
H6
H5
H6
H6
H5
H5
H5
H5
H5
L3
H6
L3
H5
H5
H5
H5
H4
H6
H6
H4
H6
H4
M
L6
%Fain
olivine
18
18
18
18
18
18
18
18
18
18
1-29
19
19
19
19
18
28
2-28
3-33
18
18
18
10-41
1-44
19
19
4-38
19
19
19
19
19
19
19
19
19
19
19
19
19
19
19
1-39
19
2-29
19
19
19
19
19
20
19
18
19
18
25
%Fs in
pyroxene
15
16
16
16
16
16
16
16
16
16
1-42
17
16
17
13-21
15
25-32
5-27
5-27
16
16
15
5-24
1-25
17
16
1-31
17
17
17
8-18
16
17
16
17
16
16
17
17
17
16
16
2-25
16
3-31
17
17
16
16
17
17
16
16
17
16
28
21
Degree of
weathering
B/C
C
C
cB/C
B/C
B/C
C
B/C
C
C
B
B
B
B
C
C
C
B/C
C
B/C
C
B/C
C
C
B
B/C
B/C
B
B/C
B/C
B
B
B
B
B/C
C
A/B
B
B
B
B
C
B
B/C
B
B
B
B
B
A/B
C
B/C
B
B
C
A/B
Specimen
number
ALHA
81100
81101
81102
81103
81104
81105
81106
81107
81108
81109
81110
81111
81112
81113
81114
81115
81116
81117
81118
81119
81120
81121
81122
81123
81124
81125
81126
81127
81128
81129
81130
81131
81132
81133
81134
81135
81136
81137
81138
81139
81140
81141
81142
81143
81144
81145
81146
81147
81148
81149
81150
81151
81152
81153
81154
81155
81156
Weight
(g)
155
119
196
136
184
93
48
140
69
1
3
210
150
111
79
155
2
33
85
107
14
88
21
2
9
10
22
15
16
32
30
13
5
21
15
10
1
9
4
7
14
1
1
13
3
21
24
2
13
9
2
5
10
4
1
5
20
Class
and
type
H5
Ur
H6
H6
H4
H4
L6
L6
H5
H4
H5
H6
H6
H5
H4
H5
H5
H4
H5
L4
H5
L3
L6
LL6
H5
H5
H5
H6
H5
H5
H5
L6
H5
H5
H6
H5
H5
H6
H5
H5
H4
H5
H4
H5
H5
L3
H6
H4
H5
H4
L6
LL5
H5
L5
H6
H5
L3
%Fa in
olivine
19
10-22
19
19
19
18
24
24
18
19
19
19
19
18
18
19
19
18
19
24
18
8-40
25
30
19
19
19
19
19
18
18
25
18
18
18
19
20
19
19
19
19
19
18
18
19
5-40
18
19
19
19
25
28
18
24
19
19
4-42
%Fsin
pyroxene
17
17
17
17
16
20
21
16
17
17
17
17
16
16
17
17
14-21
16
21
16
1-24
21
25
17
17
16
17
17
16
16
22
16
16
16
16
17
17
17
17
17
17
16
16
16
3-23
16
16
17
16
22
23
16
21
17
17
1-30
Degree of
weathering
B
A/B
B/C
B/C
C
C
B
B
B
B
B/C
B/C
B/C
B/C
B/C
C
B
B
B/C
B
B/C
B
B
B
B
B
B
B/C
B/C
A/B
B
A/B
B
B
B/C
B
B
B/C
B
B/C
B/C
B/C
B/C
B/C
B
B
C
B
B
B
C
B/C
B
B
B
A/B
B/C
76 SMITHSONIAN CONTRIBUTIONS TO TO THE EARTH SCIENCES
TABLE A.?Continued.
Specimen
number
ALHA
81157
81158
81159
81160
81161
81162
81163
81164
81165
81166
81167
81168
81169
81170
81171
81172
81173
81174
81175
81176
81177
81178
81179
81180
81181
81182
81183
81184
81185
81186
81187
81188
81189
81190
81191
81192
81193
81194
81195
81196
81197
81198
81199
81200
81201
81202
81203
81204
81205
81206
81207
81208
81209
81210
81211
81212
81213
Weight
(g)
12
2
10
12
122
59
82
20
6
26
59
8
6
59
24
33
26
33
13
95
17
30
14
17
15
5
104
17
65
23
40
9
3
48
30
9
13
17
5
9
68
0.5
16
9
7
5
4
7
3
4
14
2
14
0.6
7
11
3
Class
and
type
H4
H5
L6
H6
H5
L3
H5
H5
H5
H5
L6
H5
H5
H5
H5
L6
H5
H5
H5
H5
H4
H5
H5
H6
L6
H5
H5
L4
LL6
H5
A
H5
E4
L3
L3
H5
H6
H5
H5
H6
H5
L5
H4
H4
H5
H5
L6
H6
L6
H4
H5
Di/M
H5
H6
H5
H4
H5
%Fa in
olivine
19
19
25
19
19
1-40
19
18
19
19
25
19
18
19
19
24
19
19
19
19
19
19
19
18
25
18
17
24
30
18
4
19
2
0.3-32
2-29
19
18
19
18
18
17
24
19
19
18
19
25
18
25
18
18
18
19
18
18
19
%Fsin
pyroxene
17
17
21
17
16
4-20
17
16
16
16
22
17
16
17
17
21
16
17
17
17
16
17
17
16
22
16
15
20
25
16
6.5
17
3
4-28
1-30
16
16
16
16
16
15
21
16
17
16
17
21
16
23
15-21
16
25
16
17
16
16
17
Degree of
weathering
B/C
B/C
B/C
C
C
C
C
B
B
B
B/C
C
B
B
B/C
C
A/B
B
A/B
B
B/C
B/C
B
C
B
B
C
A/B
A/B
B
B/C
A/B
C
C
cA/B
B
B
B
B
B/C
B/C
C
B/C
B/C
C
C
B
B
B/C
C
Ce
B/C
B
B
B/C
B/C
Specimen
number
ALHA
81214
81215
81216
81217
81218
81219
81220
81221
81223
81224
81225
81226
81227
81228
81229
81230
81231
81232
81233
81234
81235
81236
81237
81238
81239
81240
81241
81242
81243
81244
81245
81246
81247
81248
81249
81250
81251
81252
81253
81254
81255
81256
81257
81258
81259
81260
81261
81262
81263
81265
81266
81267
81268
81269
81270
81271
Weight
(g)
4
11
2
5
6
24
3
9
10
14
14
3
11
8
40
13
9
5
25
5
7
41
27
24
32
41
34
20
15
5
4
3
104
5
10
17
158
2
10
9
12
28
29
1
10
124
12
55
6
8
12
27
18
5
4
28
Class
and
type
L3
H5
H5
L6
H5
H5
H5
L6
H6
H6
H6
H5
H5
H5
L3
H5
H4
H5
H5
H4
L6
H5
H5
H5
H5
H5
H5
H5
L3
H5
H5
H5
L6
H6
H5
H6
LL3
H5
H6
H6
H5
H5
L6
C3V
L3
E6
"H(?)
%Fain
olivine
0.2-38
18
18
24
19
19
18
25
18
19
19
19
19
18
7-32
18
19
18
19
18
25
18
18
19
19
19
17
18
5-44
19
19
19
25
18
18
18
1-29
18
18
18
18
18
24
0-28
0-22
'* 11
*(Acapulco-like)
L6
H5
H5
L6
H4
H6
H5
H5
H6
25
18
19
24
18
18
18
18
18
%Fsin
pyroxene
0.1-45
16
17
20
16
17
16
21
16
17
17
17
17
16
2-30
16
16
16
17
16
21
16
16
16
17
18
14
17
6-31
17
17
17
21
16
17
16
2-28
16
16
16
16
15
21
0-1
0-29
0.3
11
16
17
21
15-22
16
16
16
16
Degree of
weathering
B/C
A
C
C
cB
B/C
C
A/B
B/C
B
C
B
B/C
C
B
B/C
B
C
C
C
A/B
B
C
B
C
B
B/C
C
B
B/C
C
A/B
C
B/C
B
B/C
B
A/B
C
B
C
B
B
C
A/Be
A/B
B
B/C
A/B
C
C
B/C
C
B
NUMBER 30 77
TABLE A.?Continued.
Specimen
number
ALHA
81272
81273
81274
81275
81276
81277
81278
81279
81280
81281
81282
81283
81284
81285
81286
81287
81288
81289
81290
81291
81292
81293
81294
81295
81296
81297
81298
81299
81300
81301
81302
81303
81304
81305
81306
81307
81308
81309
81310
81311
81312
81313
81314
81315
81316
81317
ALH
82100
82101
82102
82103
82104
82105
82106
82107
Weight
(g)
23
43
19
11
42
7
1
27
55
46
31
0.6
10
20
28
78
20
4
2
4
13
2
9
105
13
20
16
0.5
10
12
4
4
42
1
7
57
19
0.6
0.7
0.9
0.7
0.5
3
2
0.7
0.4
24
29
48
2529
399
363
35
9
Class
and
type
L3
H6
H5
H5
H5
H5
L6
H4
L3
H5
L6
H5
H5
LL6
H5
H5
H6
L6
H4
H6
L3
H5
H5
H5
H5
H5
H6
L3
H5
H5
H5
H6
L6
H5
H5
L6
H5
H4
H6
L6
C2
Eu
H5
"H(?y
%Fa in
olivine
2-36
19
18
18
18
18
24
17
1-32
18
24
18
19
27
19
17
18
24
18
18
11-34
18
18
19
17
18
19
1-37
19
19
18
18
24
18
19
24
18
18
19
24
1-35
18
* 11
*(Acapulco-like)
LL4
H6
C2
C3O
H5
H5
L5
L6
Ur
L5
29
18
1-47
1-50
18
17
25
24
3
22
%Fs in
pyroxene
3-22
17
16
16
16
16
21
16
2-24
16
21
16
17
23
17
15
16
21
17
16
2-31
16
16
16
15
16
17
2-16
16
16
16
16
21
16
17
21
16
16
17
21
1-31
38
16
11
23
16
1-2
1-10
16
16
21
21
4
19
Degree of
weathering
C
C
A/B
B
C
B
B
C
C
B
A/B
B/C
B/C
C
B
C
B
A
B
B
C
B
B
C
B/C
B
B
C
A/B
B/C
B/C
B/C
A/B
B/C
B
B
B/C
C
B
B
A
B
A/B
B
C
A
A
B/C
B
A
A/B
B
B/C
Specimen
number
ALH
82108
82109
82110
82111
82112
82113
82114
82115
82116
82117
82118
82119
82120
82121
82122
82123
82124
82125
82126
82127
82128
82129
82130
82131
82132
82133
82134
82135
82136
82137
82138
82139
82140
82141
82142
82143
82144 .
83001
83002
83003
83004
83005
83006
83007
83008
83009
83010
83011
83012
83013
83014
83015
83016
83017
83018
83019
Weight
(g)
14
47
39
63
28
61
41
48
18
4
111
24
7
2
142
111
26
178
140
5
15
14
45
1.0
6
20
28
12
4
11
5
0.2
0.3
0.6
20
3
7
1569
367
322
814
228
230
285
272
2
395
213
203
246
1
3
4
0.6
4
3
Class
and
type
H5
H5
H3
L6
H5
H6
H5
H5
H6
L5
L6
H5
H5
L6
H5
L6
H6
L6
H4
H6
H4
H5
Ur
C2
E4
H4
H5
C4
H4
L5
H6
L6
L6
H5
L6
H6
H5
L4
L5
H5
L6
H5
H5
LL3
L3
Au
L3
L5
H5
H6
Ur
Au
C2
L3
E6
H4
%Fa in
olivine
18
18
1-24
24
17
18
17
18
18
25
24
18
19
24
18
25
18
24
18
18
18
18
3
0.3
18
16
27
18
23
19
24
25
19
25
18
19
23-28
23
17
23
17
17
0.5-43
10-24
4-31
23
18
18
18
0.3-30
0.8-28
17-21
%Fs in
pyroxene
16
16
4-27
21
16
16
15
16
16
22
20
16
17
20
16
20
16
20
15
16
16
17
4
0.4
16
15
24
5-20
20
17
20
20
17
21
16
17
20-32
19
15
19
15
15
3-37
5-24
2-28
19
16
16
15
0-1
4-20
0
11-22
Degree of
weathering
B/C
B/C
B/C
A/B
C
A/B
A/B
A/B
B
B
A/B
B/C
B
A
B
B
C
C
B/C
A/B
B/C
B/C
B
A
Ce
B/C
B/C
A
B
B
B
B
C
C
C
C
B
B
B
A/B
B
C
B/C
B
B
A/B
B
C
B/C
A/B
B
A/B
A/B
B/C
B/C
78 SMITHSONIAN CONTRIBUTIONS TO TO THE EARTH SCIENCES
TABLE A.?Continued.
Specimen
number
ALH
83020
83021-
83022-
83023
83024
83025
83026
83027-
83028-
83029
83030
83031
83032-
83033
83034
83035
83036
83037
83038
83039
83040
83041-
83042
83043-
83044
83045
83046
83047
83048
83049
83050
83051
83052
83053
83054-
83055
83056
83057
83058-
83059
83060
83061
83062
83063-
83064
83065
83066
83067
83068
83069
83070
83071
83072
83073
83074
83100
83101
Weight
(g)
3
42
5
4
6
78
0.1
3
16
96
49
10
3
21
6
1
24
2
87
6
78
0.3
0.5
3
5
2
33
20
2
6
10
16
53
63
17
18
1
63
29
4
9
34
77
17
12
54
46
96
0.8
78
216
5
2
49
6
3019
639
Class
and
type
H5
L6
LL6
L4
H6
H5
C3O
L6
H6
H5
H5
H5
LL6
L6
H5
H5
H5
H5
L3
H5
H5
L6
H3
L6
H5
L5
H5
H5
L5
H5
H6
H5
L6
H5
LL6
H5
H5
H5
L6
H5
H5
H5
H5
L6
H5
H5
H5
L6
H5
L5
LL6
H6
H5
H5
H5
C2
L6
%Fa in
olivine
18
23
17
17
0.3-18
19
18
19
23
18
18
17
18
7-35
18
18
7-33
19
24
17
19
24
18
17
17
23
17
18
18
18
19
18
17
17
18
17
17
24
17
25
29
18
18
18
17
25
%Fs in
pyroxene
16
20
15
15
0.7-12
16
16
16
20
16
16
15
16
2-22
16
16
2-16
17
20
15
16
20
16
15
15
20
15
16
16
16
17
16
15
15
16
15
15
20
15
21
23
16
16
16
16
23
Degree of
weathering
B
B
B
B
B/C
C
B
B
B
B/C
B/C
B
B
B/C
B
B
A
B/C
C
B
B/C
C
B
B
A
B/C
A/B
B/C
B/C
B
A/B
A/B
C
C
A
B/C
A/B
B
A
B/C
C
B/C
B/C
A/B
C
C
C
A/B
C
A
A
B/C
C
C
C
Be
A
Specimen
number
ALH
83102
83103-
83104
83105-
83106
83107
83108
84001
84002
84003
84004
84005
84006
84007
84008
84009
84010
84011
84012
84013
84014
84015
84016
84017
84018
84019
84020
84021
84022
84023
84024
84025
84027
84028
84029
84030
84031
84032
84033
84034
84035
84036
84037
84038
84039
84040
84041
84042
84043
84044
84045
84046
84047
84048
84049
84050
Weight
(g)
1786
52
2
0.7
22
38
1519
1931
7554
3089
9000
12000
16000
706
302
336
303
138
225
160
49
264
150
80
82
93
191
36
13
262
194
5
8
736
120
6
12
8
60
44
3
3
3
12
33
29
1
51
17
147
11
2
4
13
29
3
Class
and
type
C2
H6
H5
L6
C2
H5
C3O
Di
L6
H5
H4
L5
H4,5
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Brachinite
LL7?
C3V
C2
C2
C2
C2
C2
C2
C2
C2
C3V
C4
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
%Fain
olivine
0-2
18
0.2-5
18
0.9-38
24
16
17-18
21
18
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
32-33
27
0-50
0-2
0-2
0-2
0-2
0-1
0-2
0.5-6
0.7-40
0.8-9
25-30
0.4-31
0-2
0-2
0.3-2.1
%Fsin
pyroxene
16
16
1-17
27
20
15
16-19
18
17-18
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
11
23
2
2
2
0.7-7
2-13
0.5-12
26-28
0.8-1.5
0.7-1.0
Degree of
weathering
B/Ce
B
B
A
A
B/C
A
A/B
Be
A/B
Be
A/B
B/Ce
Ae
A/B
A
A
A
A
A/B
A/B
A
A
A
A
A
A/B
A
A
A
A
A/Be
B
Ae
Ae
A
Ae
A
Ae
A
Ae
A
Be
Ae
A/B
Ae
Ae
A
Ae
Ae
Ae
A
A/Be
Ae
Ae
Ae
NUMBER 30 79
TABLE A.?Continued.
Specimen
number
ALH
84051
84052
84053
84054
84055
84056
84057
84058
84059
84060
84061
84062
84063
84064
84065
84066
84067
84068
84069
84070
84071
84072
84073
84074
84075
84076
84077
84078
84079
84080
84081
84082
84083
84084
84085
84086
84087
84088
84089
84090
84091
84092
84093
84094
84095
84096
84097
84098
84099
84100
84101
84102
84103
84104
84105
84106-
84107
Weight
(g)
34
11
5
19
6901
2140
368
2003
857
339
676
958
760
1889
1642
356
391
1114
1136
3952
798
721
631
758
789
369
276
283
750
287
612
557
420
332
554
234
315
298
304
202
215
214
114
208
277
294
389
261
150
110
221
214
137
201
261
95
134
Class
and
type
C2
LL6
C2
C2
H5
L6
L6
L6
H4
H5
L6
L6
L5
H5
L6
L6
H5
H5
H5
L6
H6
L6
H5
H5
H5
H5
H5
H5
L6
L6
LL6
H6
H6
H4
H5
LL3
L6
H5
H5
L6
H5
L6
H6
H5
L6
LL6
L6
H5
H5
H5
H6
L6
H4
L6
H6
L6
LL6
%Fain
olivine
29
0.5-1.5
0.5-36
16
24
23
23
18
17
24
23
22
17
23
23
17
17
19
23
19
24
17
17
17
18
18
18
23
24
29
19
18
18
17
25-29
24
18
18
25
19
23
17
17
24
31
24
17
17
18
19
24
17
24
15
29
%Fs in
pyroxene
24
5
3
14
21
19
20
16
15
21
19
19
15
20
19
15
15
16
19
16
20
15
15
15
16
16
16
20
20
23
17
16
16
15
17-26
20
16
16
22
17
20
15
15
20
27
21
15
15
16
17
21
15
20
14
23
Degree of
weathering
A/Be
A/B
A
Ae
Be
Be
B/Ce
B
B/C
B
B
A/B
A/B
B
A/B
B
C
B
A
A/B
B
Be
B
A/B
C
B/C
B
B/C
A/B
B
A
C
B/C
B
B/C
A/B
A/B
B
B/C
Ce
B/C
A/B
B
C
A/B
A/B
B
B/C
B/C
B
C
B
B
B
C
B/C
A
Specimen
number
ALH
84108
84109
84110
84111
84112
84113
84114
84115
84116
84117
84118
84119
84120
84121
84122-
84123-
84124
84125-
84126
84127-
84128
84129
84130-
84131
84132
84133
84134
84135
84136
84137
84138
84139
84140
84141
84142-
84143-
84144
84145
84146
84147
84148
84149
84150
84151
84152
84153
84154
84155
84156
84157
84158
84159
84160-
84161
84162
84163
84164
Weight
(g)
215
246
319
132
146
212
120
195
56
72
114
34
129
141
81
97
114
76
41
84
2
38
45
108
158
70
113
31
84
145
20
157
164
130
78
74
54
19
33
54
168
12
20
112
6
243
88
114
28
89
54
101
54
83
42
135
101
Class
and
type
H6
H6
H6
H5
L6
H6
H6
H6
LL6
H5
H6
LL6
L3
H5
LL6
LL6
H5
LL6
LL3
L6
H5
L6
L6
H5
L6
H5
L6
H5
Ur
H5
H5
H5
L6
L6
L6
L6
H5
H5
H5
H6
H5
H5
H6
H6
H5
H6
LL6
H5
H5
H5
H5
H6
L6
H5
H5
H5
L6
%Fa in
olivine
18
19
18
18
24
18
18
18
28
18
18
28
22
17
18
7-31
19
23
18
23
18
23
18
0-5
18
19
19
24
24
17
17
18
17
17
17
19
18
17
17
31
18
18
17
18
19
17
18
17
24
%Fsin
pyroxene
16
16
16
16
21
16
16
16
23
16
16
23
6-21
15
16
3-24
17
20
15
20
16
20
16
4
16
17
17
21
21
15
15
16
15
15
15
17
15
15
15
25
16
16
15
15
17
15
15
15
20
Degree of
weathering
B
B/C
B/C
B
A/B
B/C
B
B/C
B
B
B
A
A/B
C
A/B
B
C
A
B
B
C
A
B/C
C
B
B
B
B/C
B
B/C
B
A
C
B
A/B
B
C
B
B
C
C
C
B/C
B
B/C
B/C
A
B/C
B/C
B/C
B/C
C
B
C
C
C
A/B
80 SMITHSONIAN CONTRIBUTIONS TO TO THE EARTH SCIENCES
TABLE A.?Continued.
Specimen
number
ALH
84165
84166-
84167
84168
84169
84170
84171-
84172
84173
84174-
84175
84176
84177
84178
84179
84180
84181-
84182
84183
84184
84185
84186-
84187
84188
84189-
84190
84191
84192
84193-
84194
84195
84196
84197-
84198
84199
84200
84201
84202
84203-
84204-
84205
84206
84207-
84208
84209
84210-
84211
84212-
84213
84214-
84215
84216
84217
84218-
84219-
84220
84221
Weight
(g)
95
39
151
14
98
39
37
3
2
32
35
5
7
0.4
46
47
33
14
28
42
5
20
26
3
9
8
14
4
9
4
2
10
8
5
27
8
6
88
9
24
25
15
4
21
6
9
49
7
7
5
9
5
3
33
10
8
16
Class
and
type
I
L6
H5
LL6
L6
E3
H6
H5
L6
L6
H5
H6
L5
H5
H5
H6
L6
L6
H5
H5
H5
H6
H6
E4
H6
A
C2
H5
L6
H5
L4
H5
L6
LL6
H5
E4
H5
H5
L6
H6
L3
E4
L6
H6
L5
L6
H6
L6
H5
H6
H6
H5
H5
L6
L6
E4
H5
%Fa in
olivine
17
30
25
0.6-28
16
25
19
18
24
18
18
18
24
17
18
18
18
4
0.4-.8
18
18
22
18
29
17
18
17
12-33
17
23
19
18
18
18
18
18
%Fsin
pyroxene
15
24
22
0.9-17
15
21
16
16
20
16
16
16
21
15
16
16
16
0.7-3
6
0.8-7
16
16
15-20
16
24
15
0.6-4
16
15
4-19
0.7-6
15
20
17
16
16
16
16
1-4
16
Degree of
weathering
B
C
B
B/C
B
C
B/C
C
B
C
C
B
B
B/C
B
A/B
B
B
B
C
B
C
C
C
C
A
C
A/B
C
B
B/C
B
A/B
C
B
B/C
C
A/B
C
B
A/B
B
C
C
C
B/C
B/C
B
B/C
B/C
B/C
C
A/B
C
C
C
Specimen
number
ALH
84222
84223
84224
84225
84226
84227
84228
84229-
84230
84231-
84232
84233
84234-
84235
84236
84237
84238-
84239
84240
84241
84242
84243-
84244-
84245
84246
84247-
84248
84249
84250
84251
84252
84253
84254
84255
84256-
84257-
84258
84259
84260
84261 -
84262
84263
84264
85001
85002
85003
85004
85005
85006
85007
85008
85009
85010
85011
85012
85013
Weight
(g)
10
11
7
9
28
12
10
7
2
43
10
14
4
6
32
8
2
15
26
17
17
49
34
19
2
50
5
23
10
34
3
7
2
11
3
19
3
23
15
5
15
5
138
212
438
50
8
19
49
82
32
47
3
11
4
130
Class
and
type
H5
H5
H6
H5
H5
H5
H5
L6
H4
L6
H4
I (incl.)
L6
E4
H5
H5
L6
H5
H5
H5
H6
H6
L6
H5
H5
L6
H5
H5
E4
H5
H6
H5
E4
LL6
L6
H6
L5
H5
H5
L6
H6
H5
L6
Eu
C4
C3O
C2
C2
C3V
C2
C2
C2
C2
C2
C2
C2
%Fain
olivine
19
18
18
18
17
18
18
18
17
18
17
18
18
17
19
17
18
19
18
18
18
18
28
25
18
19
17
18
24
30
1-56
0.5-39
0.3-43
0.3-30
0.3-45
0.4-59
0.7-28
0.6-39
0.5-18
0.5-36
%Fsin
pyroxene
17
16
16
16
15
16
16
14-19
14-20
0.5-2.3
16
15
16
16
15
17
15
16
16
16
0.5-4
16
16
16
0.3-4
24
21
16
16
15
16
21
32
23-29
0.5-23
0.9-2.2
0.9-4.9
0.9-2.5
0.8-1.6
3-20
0.8-2.5
0.7-46
Degree of
weathering
C
C
B
C
B
C
B/C
B
B
B
C
e
A
C
B
C
B
B
C
C
C
Ce
B
B
A/B
A/B
B
B/C
B
B/C
B/C
B/C
B
A
B
B
B
C
B
A
C
C
A
A/B
A
A/B
B
A
A
B
B
A
A/B
A/B
Be
A
NUMBER 30 81
TABLE A.?Continued.
Specimen
number
ALH
85014
85015
85016
85017
85018
85019
85020
85021
85022
85023
85024
85025
85026
85027
85028
85029
85030
85031
85032
85033
85034
85035
85036
85037
85038
85039
85040-
85041
85042
85043
85044
85045
85046
85047-
85048
85049-
85050-
85051
85052
85053
85054
85055
85056
85057-
85058
85059-
85060-
85061-
85062
85063-
85064-
85065-
85066
85067
85068
85069
85070
Weight
(g)
75
3
1412
2361
812
633
744
647
952
439
388
713
817
370
326
389
620
201
424
250
344
420
231
141
125
140
96
168
128
205
105
145
149
4
17
5
0.9
5
17
0.5
55
6
7
0.8
0.3
9
0.5
2
167
13
4
10
8
1
4
5
13
Class
and
type
L6
Di
L6
L6
H6
LL6
H6
H5
L6
H6
H5
H5
L6
L6
H6
L6
H6
H6
H6
L4
L6
LL6
H6
H6
H5
L6
L6
H6
H5
H5
H6
L3
L6
L6
H5
L6
L6
H5
H6
L4
H5
H5
H5
LL6
L4
LL6
L6
L6
L3
L6
L6
L6
LL6
H5
H5
H6
L3
%Fain
olivine
25
39
23
24
17
28
17
17
24
18
18
18
24
24
19
24
17
17
17
23
' 24
27
19
18
17
23
18
17
18
18
22-26
23
18
18
18
25
18
18
18
25
1-25
28
18
18
19
4-25
%Fs in
pyroxene
21
25
20
20
15
23
15
15
20
16
15
16
21
20
17
21
15
15
15
6-24
21
23
16
16
15
20
16
15
16
16
13-22
20
16
16
16
14-20
16
16
16
17-19
3-19
23
16
16
16
1-29
Degree of
weathering
A
A
A/B
A
B
A
B
Be
B
B/C
B/C
C
A
B
C
A/B
B/C
B/C
C
A
A
C
C
B/Ce
B/C
A
B
C
B/C
B
C
A/B
B
B
C
B/C
A
B/C
A/B
C
C
cc
A
A/B
A
B
A/B
B/Ce
B
C
B
B
B
C
B
A/B
Specimen
number
ALH
85071
85072-
85073-
85074
85075-
85076-
85077
85078
85079-
85080-
85081
85082-
85083-
85084-
85085
85086
85087-
85088
85089
85090-
85091
85092
85093-
85094-
85095-
85096-
85097
85098
85099
85100
85101-
85102
85103-
85104
85105-
85106
85107
85108
85109-
85110
85111
85112-
85113-
85114
85115-
85117-
85118
85119
85120
85121
85122
85123
85124-
85125
85126
85127
Weight
(g)
19
4
16
3
36
78
12
1
83
54
12
19
93
18
12
12
11
0.4
1
11
31
26
11
9
33
3
61
7
7
58
8
13
87
99
12
3
37
15
21
22
13
23
40
11
22
28
48
21
8
55
61
15
63
19
47
10
Class
and
type
H5
H6
LL6
H5
L6
L6
H5
L6
LL6
L6
H6
L6
L6
LL6
Chon.
%Fain
olivine
18
18
18
23
18
1-5
(unique)
H5
L6
H5
H5
L6
H5
L5
US
H6
L6
L6
H5
H5
H5
H5
L6
H5
L6
H5
L6
C2
H5
H6
H6
H5
H5
L6
L6
H5
L6
H6
L5
E4
H5
H3
H5
L5
L6
H5
H5
H6
18
18
18
18
23
18
18
18
18
18
17
0.3-30
18
17
17
18
18
24
18
9-20
19
23
17
17
19
%Fsin
pyroxene
16
16
16
20
16
1-4
16
16
16
16
19
16
16
16
16
16
15
16
15
15
16
16
21
0.3-12
16
3-31
16
20
15
15
17
Degree of
weathering
C
C
A/B
C
B
Be
B/C
C
A/B
B
B
A/B
A/B
B
A/B
B/C
A/B
C
B/C
B/C
B/C
A/B
B
C
B
A
B/C
C
B/C
B
B
B
A
B/C
A/B
B
B/C
C
Ce
B
C
A/B
A/B
C
B
B/C
B/Ce
Be
C
B
B
B
B
B/C
B/C
C
82 SMITHSONIAN CONTRIBUTIONS TO TO THE EARTH SCIENCES
TABLE A.?Continued.
Specimen
number
ALH
85128-
85129-
85130
85131-
85132-
85133
85134
85135-
85136
85137-
85138-
85139
85140
85141
85142
85143
85144
85145
85146
85147-
85148-
85149-
85150
85151
85152-
85153
85154-
85155
85156
85157-
85158-
85159
86600
86601
86602
86603
86604
86605-
86606
86607
86608-
86609-
86610
86611
86612
BOW
85800
BTNA
78001
78002
78004
78005
Weight
(g)
16
127
100
34
49
91
10
12
75
7
18
26
9
11
51
18
18
46
40
3
4
17
13
14
36
0.4
5
18
32
20
3
11
411
309
265
104
13
12
4
3
10
8
0.8
9
2
141
161
4301
1079
82
Class
and
type
H6
LL6
H6
L6
L6
H5
H5
LL6
H6
LL6
LL6
H6
H6
H5
H5
H5
H5
H5
H5
L6
H6
L6
L5
Chon.
%Fa in
olivine
18
17
18
17
17
19
18
17
19
18
18
18
24
0.4-41
(Carlisle Lakes-like)
LL6
H4
LL6
L3
H6
L6
LL6
E4
L6
H5
L6
H5
L6
L6
H5
H6
L6
L6
L5
H5
H5
H6
L6
L6
LL6
H6
18
8-28
19
24
18
24
18
24
17
18
23
18
19
18
24
24
30
18
%Fs in
pyroxene
16
15
16
15
15
16
16
16
16
16
16
16
19
6-30
16-21
4-20
16
0.3-1.8
21
16
20
16
20
15
16
20
16
17
16
21
20
24
16
Degree of
weathering
C
A/B
B
B
A/B
B
C
B/C
B
A/B
B
B
B/C
C
B/C
C
B
C
A/B
B
A
B/C
B
B
A/B
B
A/B
A/B
C
B
B
B/C
B
B
B
A/B
B/C
A/B
B/C
C
B/C
A/B
C
C
C
B
B
B
B
Specimen
number
DOM
85500
85501
85502
85503
85504
85505
85506
85507
85508
85509-
85510-
DRPA
78001
78002
78003
78004
78005
78006
78007
78008
78009
EETA
79001
79002
79003;
79004
79005
79006
79007
79009
79010
79011
EET
82600
82601
82602
82603
82604
82605
82606
82607
82608
82609
82610
82611
82612
82613
82614
82615
82616
83200
83201
83202
Weight
(g)
60
126
302
720
121
31
59
190
14
76
32
15200
7188
144
134
18600
389
11800
59400
138100
7942
2843
436
390
451
716
200
140
287
86
247
150
1824
8210
1571
625
982
165
95
326
42
13
32
4
8
29
2
779
1060
1213
Class
and
type
H5
H5
L6
L6
L4
LL5
LL5
H5
H6
L6
L6
I
I
I
I
I
I
I
I
I
Sh
Di
L6
Eu
Eu
Ho
H5
L5
L6
Eu
Ho
L3
H4
H5
H5
L6
L6
L6
LL6
H4
H6
L4
L6
L4
H5
H6
H4
H5
H6
L6
%Fa in
olivine
18
17
24
25
24
26
19
19
23-27
24-25
24
18
24
24
2-39
19
19
19
25
25
23
28
18
19
24
25
24
18
19
18
17-18
18-20
24-25
%Fsin
pyroxene
16
15
21
21
18-21
22
17
17
16-67
22
20
30-61
30-61
19-57
16
20
20
30-61
22-53
1-35
16
17
16
21
21
20
23
17
17
21
21
20
16
17
16
17-19
18
22-23
Degree of
weathering
B
C
B
A
B/C
B
A/B
C
C
B/C
B/C
e
e
e
Ae
B
B
B
A
B
B
B
B
B
Ae
B/C
B
Be
B/C
B
B
B/C
A/B
B/C
B
B
A
B
A/B
B
B/C
B/C
B/C
A/B
NUMBER 30 83
TABLE A.?Continued.
Specimen
number
EET
83203
83204
83205
83206
83207
83208
83209
83210
83211
83212
83213
83214
83215
83216
83217
83218
83219
83220
83221
83222
83223
83224
83225
83226
83227
83228
83229
83230
83231
83232
83234
83235
83236
83237
83238
83239
83240
83241
83242
83243
83244
83245
83246
83247
83248
83250
83251
83252
83253
83254
83255-
83256
83257-
83258-
83259
83260
83261 -
Weight
(g)
546
377
471
462
1238
263
520
426
543
402
2727
1398
510
790
375
192
243
331
314
317
219
9
44
33
1973
1206
313
530
66
211
181
255
6
883
382
282
248
203
282
288
384
59
48
22
39
11
261
184
44
8
39
5
14
47
4
15
54
Class
and
type
H5
LL6
L6
L6
H4
H5
L6
L6
H4
Eu
LL3
L6
H6
L6
L6
L6
L6
L6
H4,6
L6
H5
C2
Ur
C2
Eu
Eu
Eu
I
Eu
Eu
Eu
Eu
Eu
L6
L6
L6
L5
L6
L5
L6
L6
I
Di
Di
H3
C2
Eu
L6
L6
E4
L6
H5
L6
L6
L6
L3
L6
%Fain
olivine
20
29-31
25
24
18
17-19
25
24-25
18-20
13-30
24-25
18
24
24
23
23
23
17
24
18
0.2-41
18
0.5-69
25-26
25
24
23
23
23
23
24
3-24
0.3-22
24
23
18
24
7-19
%Fsin
pyroxene
18-21
27
22
22
16-18
16-17
22-23
22
16-20
3-26
22-24
19
20
20
20
i 20
20
15
20
16
0-1
15
0.6-10
23-25
21
20
20
19
20
19
20
3-23
2-14
21
20
0-9
16
20
5-25
Degree of
weathering
B/C
A
A/B
B
B
B/C
B/C
A/B
B/Ce
B
Be
B
B/C
B
B
B
B
B
C
B
B
A/B
B/C
A/B
B
B
B
B
B
B
B
B
B
A
C
B
B
B
A
B
A/B
B/C
B
Be
B
B/C
B
Ce
B
B
B
B/C
A
Specimen
number
EET
83262
83263
83264-
83265-
83266-
83267
83268
83269
83270
83271
83272-
83273-
83274
83275-
83276
83277
83278
83279-
83280-
83281
83282
83283
83284-
83285
83286-
83287
83288-
83289
83290
83291
83292
83293
83294-
83295
83296-
83297-
83298
83299
83300
83301-
83302-
83303
83304-
83305
83306
83307
83308
83309
83310
83311
83312
83314-
83315-
83316-
83317
83318
83319-
Weight
(g)
24
10
17
55
56
28
19
8
2
67
35
147
83
86
49
53
72
36
29
51
79
57
53
3
34
46
38
8
1
5
9
19
82
28
63
18
9
6
115
87
130
12
37
167
42
5
137
61
64
15
93
24
113
51
119
55
7
Class
and
type
H5
H6
L6
L6
L6
H3
L6
L5
H6
L6
L6
LL6
L3
H6
L6
L5
H5
L6
L6
H6
H5
Eu
L6
H5
L6
H5
H6
L6
LL6
L5
H5
H5
L6
H6
L6
L6
L6
H6
H5
L6
L6
H5
L6
H5
L6
E4
L5
Ur
H6
C4
L6
L6
L6
L6
L6
L4
L6
%Fa in
olivine
17
19
13-23
24
23
19
24
5-28
24
23
17
18
18
18
17
24
29
24
18
18
18
24
19
18
18
17
23
2-5
22
11-21
18
31
24
23
23
%Fs in
pyroxene
16
17
12-20
20
19
16
21
5-15
20
19
15
16
16
16
15
20
25
21
16
16
16
20
17
16
15
15
20
0.5-5
18
4-14
16
20
20
19
Degree of
weathering
A
C
B
B
B
B
C
A/B
C
A/B
B
A/B
B
B
B
A/B
B
B
B/C
C
B/C
B
B
B
B
B
C
B
B
B/C
B/C
B
B
B
A/B
B/C
C
C
C
B
A/B
B/C
A/B
B
B
C
B
C
C
A/B
B
B
B/C
B/C
B
A/B
C
84 SMITHSONIAN CONTRIBUTIONS TO TO THE EARTH SCIENCES
TABLE A.?Continued.
Specimen
number
EET
83320
83321
83322
83323
83324
83325-
83326
83328-
83329
83330-
83331
83333
83334
83335
83336-
83338
83339-
83340
83341 -
83342
83343
83344-
83345
83346
83347
83348
83349
83350-
83351
83352-
83353-
83354
83355
83356-
83357-
83358-
83359-
83360-
83361
83362-
83363
83364
83365-
83366-
83367
83368
83369
83370-
83371-
83372
83373
83374
83375-
83376
83377
83378-
83379-
Weight
(g)
56
11
14
140
143
93
113
88
68
49
0.3
189
3
227
130
27
73
15
65
149
125
87
12
22
37
299
28
89
81
20
54
8
66
18
35
26
66
40
6
10
185
205
158
189
107
51
39
24
170
169
159
96
267
79
152
212
177
Class
and
type
H6
H6
E4
L6
H5
L6
H5
L6
L4
L6
H5
I
C2
L6
L6
H5
L6
L5
LL6
L6
L6
L6
L6
H5
H5
L6
H5
L6
H5
LL6
L6
L6
C2
L6
LL6
L6
LL6
H6
LL5
H6
L6
L6
L6
L6
H6
L6
H5
L6
L6
H5
H6
H6
L6
Ho
H5
L6
L6
%Fa in
olivine
18
18
0.2-2
23
17
17
22
17
23
18
26
23
23
24
18
17
23
19
18
24
0-28
27
24
24
18
24
16
18
17
18
18
%Fs in
pyroxene
16
16
20
15
15
5-21
15
20
16
22
20
20
20
16
15
20
16
16
20
0-9
23
20
20
16
20
14
16
15
16
21-49
16
Degree of
weathering
C
C
A/B
B
B/C
C
cB/C
B
B
B/C
A
A/B
B/C
C
B
B
B
B
B
C
C
B
C
A/B
C
A/B
B
B/C
A/B
C
A/B
B
B/C
B/C
C
C
A/B
B/C
B
A/B
B
B
C
C
C
C
B
B
C
C
B
A/B
C
B
B
Specimen
number
EET
83380-
83382
83383-
83384-
83385-
83386
83387-
83388
83389
83390
83391 -
83392-
83393-
83394-
83395
83396-
83397
83398
83399
83400
83401-
83402
83403
84300
84301
84302
84303
84304
84305
84306
84307
84308
86800-
86801
86802
GEO
85700
85701
GRO
85200
85201
85202
85203
85204
85205
85206
85207
85208
85209
85210
85211
85212
85213
Weight
(g)
119
12
117
22
4
38
81
35
19
15
91
164
30
54
65
198
32
67
203
113
112
50
12
72
75
60
58
152
10
4
5
9
116
83
30
2409
439
3822
1401
27
1450
1755
1000
2420
2372
1357
1126
247
355
342
4364
Class
and
type
LL6
H6
L6
L6
H6
L5
L6
H5
C2
I
LL6
L6
H6
H6
L3
L6
H6
L5
L3
H5
LL6
H5
H5
I (incl.)
L6
A
H5
L6
LL6
H6
L6
L6
L6
L6
H4
L6
L6
H5
I
C2
H5
L6
L6
H5
L6
L6
L6
H5
H5
L4
L6
%Fain
olivine
18
24
19
0.2-37
6-30
19
25
3-26
17
17
18
24
5
18
24
27
19
23
24
24
18
24
23
18
0.8-1.2
18
24
25
17
24
23
25
18
19
23
23
%Fsin
pyroxene
16
20
16
1-13
2-17
16
21
6-25
15
15
16
20
8
16
20
22
16
20
20
21
13-17
20
20
16
16
21
20
15
20
20
21
16
17
16-20
20
Degree of
weathering
B
B
B
B
B/C
A/B
C
C
A/B
A/B
B
B/C
C
B
A/B
C
B
C
C
A/B
C
C
B
B/C
C
B
A/B
C
C
B
A
B
A
B
A
B/C
A/Be
B
A
A/B
B/Ce
A/B
A
A
B
B
B
B
NUMBER 30 85
TABLE A.?Continued.
Specimen
number
GRO
85214
85215
85216
85217
85218
ILD
83500
LEW
85300
85301-
85302
85303
85305
85306
85307
85309
85311
85312
85313
85314
85315
85316
85317
85318
85319
85320
85321
85322
85323
85324
85325
85326
85327
85328
85329
85330
85331
85332
85333
85334
85335
85336
85337-
85338
85339
85340
85341
85342
85343
85344
85345
85346-
85347
85348
Weight
(g)
260
35
13
34
7
2523
210
13
115
408
41
6
2
54
200
32
191
14
10
34
9
152
11491
110224
527
582
874
514
537
225
439
107
170
67
54
114
48
177
107
60
57
99
29
103
76
7
78
3
32
30
31
31
Class
and
type
L5
L5
L5
L5
H6
I
Eu
H6
Eu
Eu
Eu
C2
C2
C2
C2
C2
Ho
H5
H6
H5
L4
H5
H5
H5
L6
H6
L6
H5
L6
H5
H5
Ur
H6
H6
H6
Chon.
%Fa in
olivine
24
18
0.2-33
0.6-46
0.2-41
0.4-36
0.2-45
18
18
17
25
17
18
19
24
19
23
18
25
19
17
20
19
18
17
0-37
(unique)
L4
H5
H6
H5
H6
H5
L3
L5
H5
H5
L4
H5
H5
L6
H5
H6
25
18
17
18
16
1-30
23
17
18
22
17
17
17
19
%Fs in
pyroxene
21
16
32-63
24-59
30-62
31-57
0.7-5.5
0.9-1.5
0.9-1.1
0.7-1.8
15-64
16
16
15
18-22
15
16
16
20
17
20
16
21
17
15
17
16
16
15
1-30
21
16
15
16
14
3-13
19
15
16
18
15
16
15
16
Degree of
weathering
B
B
B
B/C
C
e
A/B
B/C
A/B
A/B
A
A
A
A/Be
Be
B
B
C
C
C
A/B
C
B/Ce
Be
B/C
C
Be
B
B/C
C
B/C
B/C
A/B
B/C
B/C
B/C
B
B/C
C
B/C
C
B
A/B
B
C
C
A
C
B/C
B
C
C
Specimen
number
LEW
85349
85350
85351
85352
85353
85354-
85355
85356-
85357
85358
85359
85360-
85361
85362
85363
85364
85365
85366
85367
85368
85369
85370
85371
85372
85373-
85374
85375
85377-
85378-
85379
85380-
85381-
85382
85383
85384-
85385
85386-
85387
85388-
85389
85390
85391
85392
85393
85394
85395
85396
85397
85398
85399-
85400
85401
85402-
85403-
85404
85405
85406
Weight
(g)
17
24
12
9
25
12
6
8
61
14
18
13
4
15
44
4
8
3
6
18
6
11
55
9
45
10
37
31
66
26
14
22
10
18
6
13
14
4
4
4
1
9
28
51
15
17
60
57
38
8
6
4
66
12
34
63
7
Class
and
type
L6
L4
H4
H5
Eu
L6
H5
L6
H5
H5
H6
L6
L6
H6
L5
H5
L4
H4
H5
H6
I
H4
H5
H5
H6
H6
H5
H6
H6
H5
L6
H6
H5
H3
H6
L5
LL6
H5
L6
H5
L4
H6
H6
H5
L5
H5
L3
L6
H4
H6
H6
L3
H6
L6
H5
H5
H5
%Fain
olivine
23
24
17
17
17
18
18
17
23
18
23
18
24
17
17
18
17
18
18
18
17
17
18
6-23
23
17
17
24
18
18
18
23
18
2-26
19-22
18
18
1-28
19
19
19
%Fs in
pyroxene
19
20
14-21
15
22-62
15
16
16
15
20
16
20
16
20
12-18
15
16
15
16
16
16
15
15
16
2-18
20
15
15
12-24
16
16
15
19
16
3-25
17-20
14-18
16
1-20
16
16
16
Degree of
weathering
C
B/C
B/C
C
B
B/C
C
B/C
B/C
C
C
B
C
C
B
C
C
C
C
C
B/C
C
C
Ce
B
C
C
C
C
B
C
B/C
C
C
B/C
A/B
C
B/C
C
C
C
cBe
C
B/C
C
cc
cB/C
B/C
C
A/B
B
B/C
C
86 SMITHSONIAN CONTRIBUTIONS TO TO THE EARTH SCIENCES
TABLE A.?Continued.
Specimen
number
LEW
85407
85408-
85409
85410-
85411-
85412
85413-
85414
85415
85416
85417
85418
85419
85420
85422
85423
85424-
85425
85426
85427
85428-
85429
85430
85431-
85432-
85433
85434
85435
85436
85437
85438-
85439-
85440
85441
85442-
85443
85444-
85445
85446-
85447
85448
85449-
85450
85451
85452
85453
85454-
85455
85456
85457-
85458
85459
85460
85461-
85462
85463-
85464
Weight
(g)
19
3
29
2
4
71
14
26
3
6
9
37
39
12
27
11
4
3
16
15
21
7
13
30
2
57
19
21
9
9
3
3
44
11
29
10
2
11
42
16
34
12
27
15
9
5
8
8
19
20
17
32
6
21
23
12
24
Class
and
type
H5
H6
H5
H6
H6
H6
L6
H5
LL6
H5
L5
H6
L6
L6
H5
H5
L6
L6
H5
L5
L6
LL6
L6
L6
L6
H5
L3
H5
L6
L3
LL6
L6
Ur
Ho
L6
L4
L6
H4
H6
H5
H5
L6
H5
L5
L3
H5
L6
H5
H5
L6
H5
H5
H5
L6
H6
L6
H5
%Fa in
olivine
18
17
19
19
30
18
24
18
23
25
17
17
23
18
25
27
23
18
1-23
17
23
1-23
9
25
18
18
18
17
23
5-23
18
17
18
18
17
18
18
19
%Fs in
pyroxene
16
15
16
17
24
16
20
16
20
20
15
15
20
16
21
23
20
17
2-11
15
20
2-11
8
25-48
10-23
13-16
16
16
15
20
2-18
16
15
16
16
15
16
16
16
Degree of
weathering
C
B
B/C
C
C
C
B
C
A
C
B/C
C
C
B/Ce
C
B/C
B/C
C
B/C
B
B/C
C
C
C
B
C
C
C
C
C
A/B
C
B
B
B/C
B
C
B/C
C
cc
cB/C
B/C
C
C
C
cc
B/C
B/C
B/C
C
B/C
C
C
C
Specimen
number
LEW
85465-
85466
85467-
85468
85469-
85470
85471
85472
86001
86002
86003
86004
86005
86006
86007
86008
86009
86010
86011
86012
86013
86014
86015
86016
86017
86018
86019
86020
86021
86022
86023
86024
86025
86026
86028
86029
86030
86031
86032
86033
86034
86035
86036
86037
86038-
86039
86040
86041
86042
86043
86044
86045
86046
86047
86048-
86049
Weight
(g)
57
14
5
15
8
19
239
67
291
33
2
2
5
0.8
2
6
6
7
3398
2157
1812
662
780
525
688
502
432
361
326
352
322
249
190
22
26
17
13
74
1
22
6
78
9
6
19
41
49
23
5
14
19
5
5
69
6
15
Class
and
type
L6
H5
LL6
H4
H6
H6
L6
L6
Eu
Eu
Eu
C2
C2
C3V
C2
C2
C2
An
L6
L6
L6
L4
H6
L6
H6
L3
L6
H5
L3
L3
L6
L4
L6
H5
H6
H5
H6
H5
H5
H4
L4
H5
H5
H5
L6
H5
L4
H5
L6
L6
H5
H5
H5
H5
L6
H5
%Fain
olivine
18
18
18
25
23
0-54
0-38
0-27
0-42
0-25
0-45
63
25
25
25
24
19
25
19
0.7-32
24
18
18-28
6-34
23
22
23
18
18
18
18
19
18
18
25
19
18
19
19
23
17
24
25
18
18
18
18
18
%Fsin
pyroxene
16
16
16
22
20
22-57
31-61
26-64
0-7
0-3
0-5
0-4
0-3
0-2
19
21
21
21
17-22
17
21
16
2-9
20
16
4-17
1-31
20
19
20
16
16
16
16
16
16
15-17
21-23
16
16
16
16
19
15
21
21
16
16
16
16
16
Degree of
weathering
B
C
B/C
B/C
C
C
C
B/C
Be
A/B
B
B
A/Be
B
A/Be
B
A/Be
A/B
A/B
A
B
C
C
A/B
B
Be
B
C
Ce
B/Ce
B
A/B
Ce
B/C
B
C
C
C
B/C
B/C
C
B/C
B/C
B/Ce
C
B/C
C
B/C
B
B/C
C
C
C
C
C
C
NUMBER 30 87
TABLE A.?Continued.
Specimen
number
LEW
86050
86051
86052
86053
86054-
86055
86056-
86057-
86058
86059
86060
86061
86062
86063
86064-
86065
86066-
86067
86068
86069-
86070-
86071
86072
86073-
86074
86075-
86076
86077
86078
86079
86080
86081
86082-
86083
86084-
86085-
86086
86087
86088
86089
86090-
86091
86092
86093
86094
86095
86096
86097-
86098
86099
86100
86101-
86102
86103
86104
86105
86106
Weight
(g)
11
2
2
4
2
41
7
55
22
2
23
9
13
7
24
9
18
9
6
0.6
19
8
12
38
19
4
24
9
37
7
14
28
8
199
53
197
104
11
38
85
23
67
21
15
15
14
71
2
53
28
24
28
22
9
34
6
6
Class
and
type
H5
H5
H6
H5
L6
H5
L6
LL6
H5
H5
H5
L4
H5
H5
L6
L5
H6
H4
H5
LL6*
LL6
H5
H5
L6
H5
L6
H5
H5
H5
H5
H5
H5
LL6
H5
L6
L6
H5
H5
H5
H6
L6
H5
H5
H5
H5
H5
H5
L6
L4
H5
H5
LL6
H3
H5
H5
H3
H5
%Fa in
olivine
18
18
18
19
19
19
19
17
24
19
18
25
19
18
19
18
19
19
19
19
18
18
18
18
18
18
19
18
18
19
19
19
19
19
23
18
18
1-48
19
19
1-50
18
%Fsin
pyroxene
16
16
16
17
17
17
16
15
20
16
16
21
8-20
16
16
16
16
16
17
16
16
16
16
16
16
16
17
16
17
17
17
17
17
16
19
16
16
1-41
16
16
1-32
16
Degree of
weathering
B/C
B/C
B/C
B/C
B/C
B/C
B/C
B/C
B/C
B/C
C
B
C
C
C
C
C
C
C
C
A/B
B/C
C
B/C
B/C
B/C
B/C
B/C
B/C
B/C
C
C
B
Ce
C
C
C
C
C
C
C
C
B
C
C
C
C
C
C
C
C
B
C
C
C
C
C
Specimen
number
LEW
86107
86108
86109
86110-
86111
86112
86113-
86114
86115-
86116
86117-
86118
86119
86120-
86121
86122
86123
86124
86125
86126
86127
86128
86129
86130
86131
86132-
86133-
86134
86135-
86136
86137-
86138
86139-
86140-
86141-
86142
86143
86144
86145
86147
86148
86149
86150
86151
86152
86153
86154
86155
86156
86158
86159
86160-
86161-
86162-
86163-
86164
86165
Weight
(g)
47
4
17
34
33
18
7
9
33
17
13
30
44
33
8
9
12
8
14
7
12
15
7
3
10
12
8
29
10
13
6
47
4
9
5
14
23
11
4
13
2
19
7
13
15
31
9
18
24
9
8
15
29
2
15
26
18
Class
and
type
H5
H5
H5
L6
H5
H5
L6
H4
L6
H5
LL6
H5
H4
H6
H5
H5
H4
L5
H5
H5
L3
H5
H5
H5
H5
L6
L6
L3
L6
H5
H6
L4
H6
L6
L6
H5
H5
L3
LL5
H5
H5
H6
H5
H5
H5
H5
H5
H5
H5
L3
H5
H6
LL6
LL6
H6
H5
H4
%Fa in
olivine
19
18
18
18
19
18
19
18
18
18
19
19
25
17
19
2-26
18
19
19
18
2-24
18
24
18
18
1-25
28
18
17
18
18
18
18
19
19
18
18
5-25
18
19
18
%Fsin
pyroxene
17
16
16
16
17
7-25
17
16
15-20
16
17
10-21
20
15
17
2-17
16
17
16
16
1-20
16
15-24
16
16
2-16
23
16
15
16
16
16
16
16
16
16
16
5-20
16
16
16
Degree of
weathering
C
C
C
C
C
Ce
B/C
B/C
C
C
B
C
C
C
B/C
C
B/C
B/C
C
C
B
C
B/C
C
cc
A
B/C
C
cc
cc
B
C
C
C
B/C
B/C
C
B/C
C
B
C
C
C
B
B/C
B/C
B
C
C
B
A
C
C
c
88 SMITHSONIAN CONTRIBUTIONS TO TO THE EARTH SCIENCES
TABLE A.?Continued.
Specimen
number
LEW
86166-
86167
86168-
86169-
86170-
86171
86172
86173-
86174
86175-
86176
86177
86178-
86179-
86180
86181
86182-
86183-
86184
86185
86186-
86187
86188
86189
86190-
86191
86192
86193-
86194
86195-
86196-
86197
86198
86199
86200
86201 -
86202
86203-
86204-
86205-
86206
86207
86208
86209
86210
86211
86212-
86213
86215
86216
86217
86218-
86220
86221-
86222
86223
86224
Weight
(g)
21
13
18
26
4
18
7
2
27
2
6
19
13
5
11
31
19
23
16
5
47
11
6
10
28
11
11
8
10
42
19
18
15
32
3
18
12
61
22
17
36
18
7
12
9
163
6
28
123
6
20
6
25
18
9
13
7
Class
and
type
L6
H5
H6
L6
H6
H4
H5
L6
H5
L6
H4
H6
H6
L6
H5
H6
H6
H6
L6
LL6
L6
H5
H5
H5
H6
H5
H5
L6
H5
L6
H6
H5
H5
H5
H5
H6
H6
L6
H6
H6
H5
L3
H5
H5
M
I
H6
L3
H5
Ur
H5
H6
I (incl.
H6
L5
H5
L5
%Fa in
olivine
19
18
18
18
17
18
18
19
24
28
18
18
17
18
19
18
18
18
18
17
18
18
1-25
17
17
45
2-20
18
12-20
19
) 7
23
19
24
%Fsin
pyroxene
17
15-21
16
16
13-15
16
16
16
20
23
16
16
15
16
17
16
16
16
16
15
16
16
2-21
15
15
24-61
1-16
16
12-18
17
9
19
16
20
Degree of
weathering
C
C
c
B/C
B/C
Ce
C
C
C
B
C
C
C
B/C
C
C
C
C
C
C
Ce
C
C
C
C
C
C
C
C
A/B
B/C
C
B/C
C
C
C
C
B/C
C
C
C
C
C
C
C
C
Ce
C
C
C
C
C
B
C
B/C
Specimen
number
LEW
86225
86226
86228
86230
86231 -
86232
86233
86234
86235
86236-
86237
86238-
86239-
86240
86241
86242
86243
86244
86245
86246
86247
86249
86250
86251
86252-
86253-
86254
86255
86256
86257
86258
86259
86260
86261
86262
86263
86264
86265
86266
86267
86268-
86269-
86270
86271
86272
86273
86274-
86275
86281
86282-
86286
86287-
86288-
86289-
86292
86295-
86302
Weight
(g)
103
49
29
2
18
19
10
14
7
1
14
29
25
7
33
13
6
5
3
2
4
45
142
23
33
10
9
25
22
4
24
8
12
14
10
15
5
2
41
18
22
22
4
20
16
30
36
35
56
62
45
42
11
18
33
44
40
Class
and
type
H5
H5
H5
H5
L6
H5
H5
H5
H5
H6
H5
L6
H6
H5
H6
H5
H5
H5
H5
L3
H5
H6
H5
L4
H6
H6
H5
H5
H5
H5
C4
H5
L5
H5
H5
H5
L4
H5
H5
L4
L6
L6
L3
H5
H5
L6
L6
H5
H6
L6
H5
H6
L6
L6
H5
H6
H5
%Fa in
olivine
18
19
18
17
18
17
17
18
17
17
18
18
17
18
17
1-29
18
18
19
23
17
18
18
17
32
18
25
17
17
18
23
19
18
24
0.6-28
18
18
25
19
17
19
19
19
%Fsin
pyroxene
16
16
16
15
16
15
15
16
15
15
16
16
15
16
15
2-18
16
16
17
12-21
15
16
16
15
26
16
20
15
15
16
13-18
17
16
12-19
0.4-19
16
16
20
16
15
16
17
17
Degree of
weathering
C
C
cc
B/C
C
C
C
C
C
C
B
C
C
C
C
C
C
C
C
cc
cc
c
B/C
cc
cc
B
C
C
C
C
C
C
cc
c
B/C
C
B/C
C
C
B
B/C
C
c
B
B/Ce
C
c
B/C
Ce
B
C
NUMBER 30 89
TABLE A.?Continued.
Specimen
number
LEW
86305
86307
86309-
86311-
86312
86314
86317-
86318
86319
86320
86321
86322
86323
86324
86325
86326
86327
86328-
86329
86330-
86332
86333-
86334
86335-
86336
86337
86338
86339
86340-
86341
86342-
86343-
86344
86345
86346
86347
86348
86349
86350-
86351
86352
86353
86354
86355
86356
86357
86358
86359-
86360
86361
86362
86363
86364-
86365
86366
86367
86368
Weight
(g)
40
5
14
67
102
41
62
7
3
3
33
18
5
8
20
7
44
7
5
21
14
9
6
3
8
26
27
21
25
9
2
6
17
4
3
3
20
38
19
10
27
5
23
7
9
3
5
3
181
6
6
3
20
5
26
11
29
Class
and
type
H5
L3
L6
L6
H5
H5
L6
H4
H5
H5
H5
H5
H5
H5
H5
H5
H5
H6
H5
L6
H5
H6
LL6
H6
H5
H5
H5
L4
H6
H5
H6
H6
H5
H5
L5
L3
H6
L6
H6
H6
L5
H5
H5
H6
H5
L5
H4
L6
L4
H5
H5
H5
H6
H5
H5
L3
H5
%Fa in
olivine
19
3-29
16
19
16
17
19
19
18
17
18
18
17
19
19
18
27
17
18
18
23
17
17
19
25
1-21
17
24
16
23
17
16
17
16
24
17
24
17
17
17
18
19
1-22
18
%Fsin
pyroxene
16
2-14
14
16
14
15
16
16
16
15
16
16
15
17
16
15
23
15
16
16
3-23
16
15
16
21
2-17
15
20
15
20
15
15
15
15
20
15-21
16-20
15
15
15
16
16
2-23
16
Degree of
weathering
C
B
B
B
Be
C
B
Ce
C
C
C
C
C
C
C
C
C
C
C
C
C
C
A
C
C
cc
cc
cc
cc
cc
cc
cc
cA/B
cB/C
C
cA/B
B/C
C
B/C
B/C
C
B/C
C
C
C
B
C
Specimen
number
LEW
86369
86370
86371
86372-
86373
86374
86375
86376
86377
86378-
86379
86380
86381-
86382
86383
86384
86385
86386
86387
86388
86389
86390
86391
86392
86393
86394
86395
86396
86397
86398
86399-
86400
86401
86402
86403
86404-
86405
86407
86408
86409-
86410
86411
86412
86413
86414
86415
86416-
86417
86418
86419-
86420
86421-
86422
86423
86424
86425-
86426-
Weight
(g)
7
9
147
12
30
32
11
41
2
4
9
32
7
22
11
6
34
3
26
24
2
30
15
6
70
3
14
13
10
3
7
19
9
14
7
8
1
36
1
24
3
4
1
14
4
3
18
2
43
2
13
3
8
11
7
2
3
Class
and
type
H5
H5
H5
L6
H5
H5
H5
H5
H4
LL6
H4
H4
H6
H6
H5
H5
H5
LL4
H5
H5
H5
H4
H5
L5
H5
H5
H5
H5
H5
H5
L6
H5
H5
LL5
H5
L6
H5
H5
L3
L6
L4
LL4
H6
H5
H5
H5
H6
L3
H5
LL6
H5
L6
H5
H5
H5
L6
L6
%Fain
olivine
18
18
19
19
19
19
19
16
17
16
18
18
17
18
27
18
19
18
16
19
25
18
18
18
18
19
19
19
18
29
17
19
19
11-25
25
27
19
19
19
18
1-22
17
17
19
18
18
%Fsin
pyroxene
16
16
17
16
16
16
17
14
12-21
14-21
16
16
15
16
18-25
16
17
16
11-15
16
21
16
16
16
16
16
16
16
16
24
15
16
17
2-23
8-24
17-25
17
16
16
16
2-24
15
15
16
16
16
Degree of
weathering
C
C
cc
cc
cc
cc
cB/C
cc
cc
cB
C
C
C
cc
B
C
C
C
B/C
C
cB/C
C
cc
cB/C
cc
cc
B/C
B
B/C
C
C
C
C
B
C
B
C
C
C
C
C
C
C
90 SMITHSONIAN CONTRIBUTIONS TO TO THE EARTH SCIENCES
TABLE A.?Continued.
Specimen
number
LEW
86427
86428
86429-
86430
86431
86432
86433-
86434
86435
86436
86437
86438
86439
86440
86441
86442
86443
86444
86445-
86446
86447-
86449
86450
86451
86452
86453
86454
86455
86456
86457
86458
86459
86460
86461
86462
86463
86464
86465
86466-
86467
86468
86469
86470
86471
86472
86473
86474-
86475
86476
86477
86478-
86479
86480
86481
86482
86483-
86484
Weight
(g)
2
6
7
6
10
7
6
22
5
4
17
45
6
7
11
59
11
15
9
10
10
4
5
34
20
49
3
50
22
13
18
8
19
0.6
25
65
19
26
71
0.4
12
11
59
83
30
21
7
15
0.6
12
2
141
12
11
7
10
24
Class
and
type
H6
H6
L6
H5
H5
LL6
H6
H5
H4
L3
H5
H5
H6
H5
H5
H5
H5
H5
H6
H4
L6
LL5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H6
H5
H5
H5
H5
H6
H5
H5
H6
H5
H5
H5
L6
H5
H5
H6
H5
LL6
H5
%Fa in
olivine
19
18
18
17
30
18
18
6-26
18
17
18
17
18
18
18
19
18
30
19
18
18
18
18
18
18
18
18
18
18
19
18
18
19
18
18
18
19
18
17
19
19
17
18
17
17
17
17
18
18
%Fs in
pyroxene
16
16
16
15
24
16
6-18
2-22
16
15
16
15
16
16
16
17
8-19
24
16
16
16
16
16
16
16
16
16
16
16
16
16
16
16
16
16
16
16
16
15
16
17
15
15
15
15
15
15
16
16
Degree of
weathering
C
C
B/C
C
cB
C
C
C
C
C
C
C
C
C
cc
cc
cB/C
A/B
C
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
B/C
cc
cB/C
A/B
cc
cc
B/C
C
Specimen
number
LEW
86485
86486
86487
86488
86489
86490-
86491
86492
86493-
86494
86495
86496
86497
86498
86499
86500
86501
86502
86503
86504-
86505
86506
86507
86508
86509
86510
86513
86514
86515
86516
86517
86518
86519
86520
86521
86522-
86523
86524
86525
86526
86527
86528-
86529
86530
86531
86532
86533
86534
86535
86536
86537-
86538
86539
86540
86541 -
86542
86543-
Weight
(g)
52
10
15
9
30
2209
15
25
5
14
2
5
6
134
25
45
85
25
22
8
44
30
10
10
33
24
6
65
34
4
32
267
8
6
0.3
43
7
23
46
14
22
50
1
2
21
4
16
89
14
8
17
21
13
21
13
25
26
Class
and
type
H5
H5
H5
H5
H5
L6
H5
H5
H6
H6
L3
H5
H5
I
H5
H5
H5
L5
H5
H6
L3
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H6
H5
L5
H5
H3
H5
L6
H5
H5
L6
H5
H5
H5
H6
H5
H6
H5
H6
I
L6
L5
H6
%Fain
olivine
18
19
17
19
18
17
17
18
1-22
18
17
18
19
18
23
17
2-30
19
18
18
18
18
18
18
18
19
17
18
17
17
18
17
23
17
13-22
17
17
18
23
18
17
18
18
18
17
18
23
%Fsin
pyroxene
16
16
15
16
16
15
15
16
3-17
16
15
16
17
16
20
15
1-20
17
16
16
16
16
16
16
16
16
15
16
15
15
16
15
19
15
8-14
15
15
16
20
16
15
16
16
16
15
16
19
Degree of
weathering
C
C
cc
cBe
B/C
C
C
C
B/C
C
C
C
C
cB
B/C
B/C
Ae
B/C
C
B/C
G
C
B/C
C
B/C
B/C
B/C
B/Ce
C
C
B
C
C
B/Ce
C
B/C
C
A/B
C
B/C
C
C
C
B/C
C
C
C
C
c
B
B/C
B/C
NUMBER 30 91
TABLE A.?Continued.
Specimen
number
LEW
86544
86545
86546
86549
MBRA
76001
76002
META
78001
78002
78003
78004?
78005
78006
78007
78008
78009?
78010
78011
78012
78013?
78014?
78015?
78016?
78017
78018?
78019?
78020
78021?
78022?
78023
78024?
78025?
78026
78027
78028
MIL
85600
OTTA
80301
PCA
82500
82501
82502
82503
82504
82505
82506
82507
82508
82509
82510
Weight
(g)
65
16
41
50
4108
13773
624
542
1726
30
172
410
175
125
29
234
116
86
132
101
37
114
47
82
91
64
23
49
56
22
58
75
53
20657
497
36
91
54
890
8308
3094
3086
5316
480
389
286
254
Class
and
type
H6
H5
L6
L3
H6
H6
H4
L6
L6
L6
L6
H6
H6
Ur
H5
H5
H5
H5
H6
H6
L5
H6
H6
H5
H6
H6
L6
H6
H6
H6
H6
H6
H6
L6
H5
H3
C4
Eu
Eu
L6
L5
L5
Ur
LL6
L6
L6
L5
%Fain
olivine
18
18
23
5-20
18
18
17
23
24
24
18
19
22
19
17
17
18
18
18
18
18
25
18
17-19
31
24
23
23
21
30
23
25
24
%Fsin
pyroxene
16
16
19
1-29
16
16
14-21
20
21
20
15
17
13
17
15
16
16
16
16
15
16
21
15
4-19
41-57
36-61
20
20
20
18
25
20
21
20
Degree of
weathering
C
C
C
B
B
B
B/C
B
B
B
B
C
B/C
B
B
Be
C
B
B
C
B
B/C
B/C
B
A/B
C
B/C
B/C
B
B/C
C
C
B
B
C
B/C
Be
A
A
Ae
A/B
B
A/Be
A
A/B
B
A
Specimen
number
PCA
82511
82512
82513
82514
82515
82516
82517
82518
82519
82520
82521
82522
82523
82524
82525
82526
82527
82528
PGPA
77006
QUE
86900
RKPA
78001
78002
78003
78004
78OO5?
79001
79002
79003
79004
79008
79009
79012
79013
79014
79015
80201
80202
80203
80204
80205
80206
80207
80208
80209
80210
80211
80213
80214
80215
Weight
(g)
149
55
239
130
7
16
41
22
125
23
1
46
11
114
40
25
3
51
19068
1532
235
8483
1276
167
29
3006
204
182
371
73
55
13
11
78
10022
813
545
4
15
54
47
18
10
10
11
2
19
5
9
Class
and
type
H4
H6
L5
L4
H4
H6
H5
E4
L5
H3
H5
H5
H6
H4
L6
H6
H6
L6
I
M
L6
H4
L6
H4
H5
L6
L6
H6
H5
L3
H6
H6
L5
H5
M
H6
L6
H6
Eu
H3
H6
L3
H6
L5
H5
H6
H6
H6
L6
%Fain
olivine
17
18
24
23
17
18
19
0.8
24
15-22
18
18
19
18
24
18
18
25
23
18
23
17
23
24
18
18
1-29
18
18
23
18
19
24
19
17-20
19
15-29
19
25
19
19
19
19
24
%Fsin
pyroxene
14
16
20
11-22
14
16
17
21
2-19
16
16
16
16
20
16
16
21
21-64
20
15
20
14-21
20
20
16
16
2-28
16
16
20
16
24
16
20
17
52-57
5-13
17
6-28
17
21
16
17
17
17
20
Degree of
weathering
B
B
A/B
B
B
B/C
B/C
B
B
B/C
C
B/C
A
A/B
B
B
A
B/C
C
C
Be
Ce
A
B
Be
B
B
B/C
B
C
B
B/C
B/C
A/B
Be
Be
C
A
B
C
C
B
C
B/C
C
B/C
C
c
92 SMITHSONIAN CONTRIBUTIONS TO TO THE EARTH SCIENCES
TABLE A.?Continued.
Specimen
number
RKPA
80216
80217
80218
80219
80220
80221
80222
80223
80224
80225
80226
80227
80228
80229
80230
80231
80232
80233
80234
80235
80236
80237
80238
80239
80240
80241
80242
80243
80244
80245
80246
80247
80248
80249
80250
80251
80252
80253
80254
80255
80256
Weight
(g)
44
8
7
21
124
52
7
25
8
8
160
8
11
14
58
238
80
414
136
261
16
22
18
6
61
0.6
7
3
14
37
6
1
11
10
4
29
11
5
68
7
153
Class
and
type
L4
H5
H5
L6
H5
H6
LL6
H5
Eu
L6
I
H5
L5
M
H5
H6
H4
H5
LL5
LL6
H5
H4
LL6
Ur
H5
C3V
L4
H5
H5
H5
M
H5
LL6
H5
H5
H5
L6
LL5
H6
H6
L3
%Fain
olivine
23
18
18
25
18
19
28
18
25
19
23
18
18
18
18
26
30
18
18
28
16
18
1-6
22
18
18
18
18
27
17
17
17
24
27
19
19
20-25
%Fsin
pyroxene
20
15
15
21
16
17
23
16
54
21
16
19
24
16
16
16
16
22
24
16
16
23
15
16
1-8
19
16
16
16
24
16
23
15
15
15
20
22
17
17
10-26
Degree of
weathering
B
C
C
B
B/C
C
B
C
A/B
C
B/C
C
C
B
C
B
B/C
B
A/B
B/C
C
A/B
B
C
B
B/C
C
C
B/C
C
C
A/B
B/C
B/C
B
A/B
A/B
C
C
B
Specimen
number
RKPA
80257
80258
80259
80260
80261
80262
80263
80264
80265
80266
80267
80268
RKP
86700
86701
86702
86703
86704-
86705
TIL
82400
82401
82402
82403
82404
82405
82406
82407
82408
82409
82410
82411
82412
82413
82414
82415
TYR
82700
Weight
(g)
9
4
20
8
62
32
17
24
8
10
24
3
424
177
195
196
138
68
221
282
476
50
322
1116
152
221
80
231
19
180
35
18
15
70
892
Class
and
type
H5
M
E5
H5
L6
H6
M
L6
H6
H6
H4
L5
L3
H6
L6
H6
LL6
H5
L5
L6
LL6
Eu
L4
H6
L4
L4
LL3
H5
Di
L4
H5
H5
H5
H5
L4
%Fain
olivine
17
18
24
19
24
19
19
19
24
17-27
18
24
19
18
25
25
29
23
19
23
23
1-29
18
24
17
17
17
17
24
%Fsin
pyroxene
15
17-21
0-1
16
20
17
24
20
17
17
16
20
14-23
16
20
17
16
21
21
24
43-58
20
17
19
20
2-21
16
24
21
16
16
15
15
15-23
Degree of
weathering
B/C
B/C
B/Ce
C
B
C
C
B
C
B/C
C
B/C
B
B
C
C
B/C
B
A/B
A/B
A/B
A
B
B
B
B/C
B
B
A
A/B
C
C
B
A/B
Be
NUMBER 30 93
TABLE B.?Meteorites listed by class and source area in numerical sequence (fractions of grams in weight
dropped unless total weight is less than 1 gram).
Specimennumber
ALHA77306
ALHA78261
ALHA81002
ALHA81004
ALHA81312
ALH82100
ALH82131
ALH83016
ALH831OO
ALH83102
ALH83106
ALH84029
ALH84030
ALH84031
ALH84032
ALH84033
ALH84034
ALH84035
ALH84036
ALH84039
ALH84040
ALH84041
ALH84042
ALH84043
ALH84044
ALH84045
ALH84046
ALH84047
ALH84048
ALH84049
ALH84050
ALH84051
ALH84053
ALH84054
ALH84191
ALH85004
ALH85005
ALH85007
ALH85008
ALH85009
ALH85O1O
ALH85011
ALH85012
ALH85013
ALH85106
EET83224
EET83226
EET83250
EET83334
EET83355
EET83389
GRO85202
LEW853O6
LEW85307
LEW85309
LEW85311
LEW85312
Weight
(g)
20
5
14
5
0.7
24
1.0
4
3019
1786
22
120
6
12
8
60
44
3
3
33
29
1
51
17
147
11
2
4
13
29
3
34
5
19
14
8
19
82
32
47
3
11
4
130
3
9
33
11
3
66
19
27
6
2
54
200
32
Class
and
type
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
C2
Degree of
weathering
A
A
Ae
A/B
A
A
A
A/B
Be
B/Ce
A
Ae
A
Ae
A
Ae
A
Ae
A
A/B
Ae
Ae
A
Ae
Ae
Ae
A
A/Be
Ae
Ae
Ae
A/Be
A
Ae
A
B
A
B
B
A
A/B
A/B
Be
A
B
A/B
A/B
Be
A
A/B
A/B
A/Be
A
A
A/Be
Be
B
fracturing
Specimen
number
CHONDRITES
A
A
B
A
A
A
B
B/C
B/C
C
A/B
B
B/C
B
A
B
A
A
A
A
B
B
B
B
B
A/B
A
B
B
B
B
B
A
A
B
C
A
B
A/B
B
A
A
B
A/B
A
B
B
C
A
B
A/B
C
A
A
B/C
B/C
B/C
LEW86004
LEW86005
LEW86007
LEW86008
LEW86009
ALHA77307
ALHA77003
ALHA77029*
ALH82101
ALH83026
ALH831O8
ALH85OO3
ALHA81003
ALHA81258
ALH84028
ALH84037
ALH85006
LEW86006
RKPA80241
ALH82135
ALH84038
ALH85002
EET83311
LEW86258
PCA82500
ALH85085
LEW85332
ALH85151
ALH84170
ALHA81189
ALH82132
ALH84188
ALH84200
ALH84206
ALH84220
ALH84235
ALH84250
ALH84254
ALH85119
ALH85159
EET83254
EET83307
EET83322
PCA82518
ALHA77156*
ALHA77295*
RKPA80259
Weight
(g)
2
5
2
6
6
181
780
1
29
0.1
1519
50
10
1
736
3
49
0.8
0.6
12
12
438
15
24
91
12
114
14
39
3
6
3
8
15
8
6
10
2
21
11
8
5
14
22
18
141
20
Class
and
type
C2
C2
C2
C2
C2
C3
C3O
C3O
C3O
C3O
C3O
C3O
C3V
C3V
C3V
C3V
C3V
C3V
C3V
C4
C4
C4
C4
C4
C4
Chon. (unique)
Chon. (unique)
Chon.
Degree of
weathering
B
A/Be
A/Be
B
A/Be
Ae
Ae
A/B
A
B
A
A/B
A/B
B
Ae
Be
A
B
B
A
Ae
A
A/B
B
Be
A/B
B/C
B
(Carlisle Lakes-like)
E3
E4
E4
E4
E4
E4
E4
E4
E4
E4
E4
E4
E4
E4
E4
E4
E4
E4
E5
B
C
Ce
C
B
A/B
C
C
B
B
Be
B/C
Ce
C
A/B
B
B
B
B/Ce
fracturing
A
A
A
A
A/B
A
A
A/B
A
A
A
A/B
A/B
A
A
A
A
B
A
A
A
A/B
A
C
A/B
B
A/B
A
B
B/C
B
B
A
B
B/C
A
A
B/C
B
B/C
B
B
A
B
94 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE B.?Continued.
Specimennumber
ALHA81021
ALHA81260
ALH83018
ALHA77299
ALH82110
ALH83O42
ALH85121
EET83248
EET83267
LEW85383
LEW86102
LEW86105
LEW86526
OTTA80301
PCA82520
RKPA80205
ALHA77004
ALHA77009
ALHA77O1O
ALHA77056*
ALHA77190
ALHA77191
ALHA77192
ALHA77208
ALHA77221
ALHA77222*
ALHA77223
ALHA77224
ALHA77225
ALHA77226
ALHA77232
ALHA77233
ALHA77262
ALHA77286
ALHA78029$
ALHA78033$
ALHA78051
ALHA78053
ALHA78O57
ALHA78077
ALHA78084
ALHA78120
ALHA78134
ALHA78140t
ALHA78157t
ALHA78168J
ALHA78172$
ALHA78193
ALHA78196
ALHA78223
ALHA79023
ALHA79035
ALHA79039
ALHA80106
ALHA80121
ALHA80128
Weight
(g)
695
124
4
261
39
0.5
55
39
28
18
22
6
14
36
23
54
2230
236
296
12
387
642
845
1733
229
125
208
787
5878
15323
6494
4087
862
246
4
5
120
179
9
331
14280
44
458
17
63
34
29
13
11
6
68
38
108
432
39
138
Class
and
type
E6
E6
E6
H3
H3
H3
H3
H3
H3
H3
H3
H3
H3
H3
H3
H3
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
Degree of
weathering
A
A/Be
B/C
A
B/C
B
B
B
B
C
C
C
B/C
B/C
B/C
B
C
C
C
A/B
C
C
C
C
C
A/B
C
C
Ce
Ce
C
C
B/Ce
C
B
B
C
C
B/Ce
B/C
B
B
B
B
B/C
B/C
B
B/C
B
B
C
B/C
B
fracturing
B
A/B
A
A
B
A
B/C
A
C
A
A
A
A
B
A/B
B
C
A
A
C
B/C
C
C
A
C
C
C
C
C
B
B
B
B
B
B
B/C
A
B
B
C
B
B
B
C
B/C
Specimen
number
ALHA80131
ALHA81022
ALHA81041
ALHA81O43
ALHA81044
ALHA81045
ALHA81046
ALHA81047
ALHA81048
ALHA81049
ALHA81O5O
ALHA81051
ALHA81052
ALHA81056
ALHA81057
ALHA81O58
ALHA81068
ALHA81073
ALHA81074
ALHA81092
ALHA81095
ALHA81O97
ALHA81104
ALHA81105
ALHA81109
ALHA81114
ALHA81117
ALHA81140
ALHA81142
ALHA81147
ALHA81149
ALHA81157
ALHA81177
ALHA81199
ALHA81200
ALHA81206
ALHA81212
ALHA81231
ALHA81234
ALHA81267
ALHA81279
ALHA81290
ALHA81309
ALH82126
ALH82128
ALH82133
ALH82136
ALH83O19
ALH84004
ALH84059
ALH84084
ALH84103
ALH84230
ALH84232
ALH85153
EET82602
EET82609
EET82616
Weight
(g)
20
913
729
106
387
90
17
81
191
9
26
43
29
1
8
66
24
3
8
16
59
80
184
93
1
79
33
14
1
2
9
12
17
16
9
4
11
9
5
27
27
2
0.6
140
15
20
4
3
9000
857
332
137
2
10
0.4
1824
326
2
Class
and
type
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
Degree of
weathering
B
B/C
C
B/C
C
C
C
B/C
B/C
B/C
C
B/C
C
B
B
C
B
B/C
B
B
B/C
B
C
C
B
B/C
B
B/C
B/C
B
B
B/C
B/C
C
B/C
B/C
B/C
B/C
C
C
C
B
C
B/C
B/C
B/C
B
B/C
Be
B/C
B
B
B
C
B
B
B/C
B/C
fracturing
B
A
C
C
cB/C
B/C
B/C
B/C
B
C
B
B
A
A
C
A
A
B
A
C
A
C
B/C
A
B/C
B/C
A
B/C
A
B
B
B
B
A
A
B
B
A
B/C
B/C
A
A
A
A
A/B
B
A
B
B
A
A
A
B
A
B
A/B
A
NUMBER 30 95
TABLE B.?Continued.
Specimen
number
EET83207
EET83211
EET86802
LEW85351
LEW85366
LEW85370
LEW85398
LEW85445
LEW85468
LEW86O33
LEW86067
LEW86114
LEW86119
LEW86123
LEW86165
LEW86171
LEW86176
LEW86318
LEWg635g
LEWg6377
LEW86379
LEW86380
LEW86390
LEW86435
LEW86446
META78001
PCA82511
PCA82515
PCA82524
RKPA78002
RKPA78004
RKPA80232
RKPA80237
RKPA80267
ALH84006
EET83221
ALHA77007*
ALHA77012
ALHA77014
ALHA77016*
ALHA77017*
ALHA77018*
ALHA77021
ALHA77022*
ALHA77023*
ALHA77025
ALHA77038*
ALHA77039*
ALHA77042*
ALHA77045*
ALHA77051*
ALHA77054*
ALHA77058*
ALHA77061
ALHA77062
Weight
(g)
1238
543
30
12
3
11
38
11
15
22
9
9
44
12
18
18
6
7
5
2
9
32
30
5
10
624
149
7
114
8483
167
80
22
24
16000
314
99
180
309
78
78
52
17
16
21
19
19
8
20
18
15
10
4
13
17
Class
and
type
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4
H4,5
H4,6
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
B
B/Ce
A
B/C
C
B/C
C
B/C
B/C
B/C
C
B/C
C
B/C
C
Ce
C
Ce
B/C
C
C
B/C
C
C
C
B/C
B
B
A/B
Be
A
B
C
C
B/Ce
C
B
Ce
C
B
B
B/C
C
A
B
C
A/B
A/B
A/B
A
A
B
B
B
B
fracturing
B
B/C
B/C
A
B
A
A
A
A
A
A
A
A
A
A
A
A
A/B
A
A
A
A
A
A
A
B
B
A/B
B
A/B
A
A
B
A
B
C
A
B/C
A
B
A
B
Specimen
number
ALHA77063*
ALHA77064
ALHA77066*
ALHA77070*
ALHA77071
ALHA77073*
ALHA77074
ALHA77076*
ALHA77078*
ALHA77079*
ALHA77082*
ALHA77084*
ALHA77085*
ALHA77086
ALHA77087*
ALHA77088
ALHA77091*
ALHA77092*
ALHA77094*
ALHA77096*
ALHA77098*
ALHA77100*
ALHA77101*
ALHA77102
ALHA77104*
ALHA77106*
ALHA77108*
ALHA77112*
ALHA77113*
ALHA77114*
ALHA77118
ALHA77119
ALHA77120*
ALHA77122*
ALHA77124
ALHA77125
ALHA77126*
ALHA77129*
ALHA77130*
ALHA77132*
ALHA77136*
ALHA77138*
ALHA77139*
ALHA77142*
ALHA77143*
ALHA77151*
ALHA77152*
ALHA77153*
ALHA77158*
ALHA77161*
ALHA77168*
ALHA77171*
ALHA77173*
ALHA77174*
ALHA77177
ALHA77181*
ALHA77182
ALHA77184*
Weight
(g)
3
6
5
18
11
10
12
2
24
8
12
44
46
19
31
51
4
45
7
2
8
18
4
12
6
8
0.7
22
2
45
8
6
4
5
4
19
25
2
25
115
4
2
66
3
39
17
18
12
20
6
25
24
26
32
368
33
1135
128
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
B
B
A
B
B
A/B
B
B
B
A
A/B
A/B
B
C
B
C
B/C
A
B
A
B
A/B
B
B
A
A/B
A/B
A
B
B
C
C
A/B
B
C
A/B
A/B
B
A
A/B
A/B
A
A/B
A/B
A/B
A
A
A
B
B
B
A/B
B
A
C
B
C
B
fracturing
B
B
B
B
B
B
B
B
A
A
B
96 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE B.?Continued.
Specimen
number
ALHA77186*
ALHA77187*
ALHA77188*
ALHA77193*
ALHA77195*
ALHA77201*
ALHA77202*
ALHA77205*
ALHA77207*
ALHA77213*
ALHA77220*
ALHA77227*
ALHA77228*
ALHA77235*
ALHA77237*
ALHA77240*
ALHA77242*
ALHA77245*
ALHA77247*
ALHA77253*
ALHA77259
ALHA77264
ALHA77265*
ALHA77266*
ALHA77268
ALHA77274
ALHA77275*
ALHA77279*
ALHA77287
ALHA77291*
ALHA77294
ALHA7730O
ALHA78001$
ALHA78004t
ALHA78OO5$
ALHA78OO8
ALHA78010t
ALHA78012
ALHA78018t
ALHA78021
ALHA78023
ALHA78025t
ALHA78027I
ALHA78028
ALHA78031
ALHA78047t
ALHA78049*
ALHA78052I
ALHA78075
ALHA78079
ALHA78080
ALHA78081t
ALHA78085
ALHA78O88I
ALHA78090t
ALHA78092t
ALHA78094I
ALHA78096t
Weight
(g)
122
52
109
7
5
15
3
3
5
8
69
16
19
5
4
25
56
33
44
24
294
11
18
108
272
288
25
175
230
6
1351
235
85
36
28
7
1
38
18
17
10
8
29
4
5
130
96
97
281
5
25
18
219
5
8
16
4
7
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
A/B
A/B
A/B
A
A
A
B
B
A/B
A
B
A
B
A/B
A
A
B
A/B
A/B
A/B
C
A/B
B
B
C
C
A
A
C
A
Ae
C
B
B
B
B
A
B
B
C
B/C
Be
fracturing
B
A
C
A
A
A
B
B
B
B
B
Specimen
number
ALHA78098I
ALHA78102
ALHA781O7
ALHA78108
ALHA78110
ALHA78111
ALHA78116I
ALHA78117$
ALHA78121f
ALHA78123$
ALHA78128
ALHA78129*
ALHA78136t
ALHA78139t
ALHA78141
ALHA78146
ALHA78150
ALHA78154J
ALHA78159
ALHA78160f
ALHA78163$
ALHA78164
ALHA78173J
ALHA78174*
ALHA78178t
ALHA78182
ALHA78190
ALHA78194
ALHA78197
ALHA78199
ALHA78201
ALHA78203
ALHA78205
ALHA78209
ALHA78217*
ALHA78219*
ALHA78221
ALHA78225
ALHA78227
ALHA78233
ALHA78241
ALHA78245
ALHA78247
ALHA78253*
ALHA78255$
ALHA78257t
ALHA78259*
ALHA79004
ALHA79006
ALHA79008
ALHA79009
ALHA79010
ALHA79011
ALHA79012
ALHA79013
ALHA79014
ALHA79015
ALHA79021
Weight
(g)
2
337
198
173
161
127
128
4
30
18
155
128
52
17
24
17
16
12
23
16
10
25
20
13
7
10
20
25
20
13
10
11
9
12
8
8
5
5
2
1
7
4
3
7
3
2
6
35
41
12
76
25
14
192
28
11
64
29
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
B/C
C
B/C
B/C
B/C
B
A
B
C
B
A
B
B
B
B
B
B/C
B
B
B
B
B/C
B/C
B
A
B
A
B/C
B/C
B
Ce
B/C
B/C
C
C
B
B
B
fracturing
B
A
B
B
A
B
B/C
B
A
A
B
B
B
B
B
A
B
A
B
B
A
B
A
NUMBER 30 97
TABLE B.?Continued.
Specimennumber
ALHA79025
ALHA79026
ALHA79029
ALHA79031
ALHA79032
ALHA79036
ALHA79O38
ALHA79040
ALHA79041
ALHA79042
ALHA79046
ALHA79047
ALHA79048
ALHA79050
ALHA79051 .
ALHA79053
ALHA79054
ALHA80111
ALHA80123
ALHA80124
ALHA80127
ALHA80129
ALHA80132
ALHA81O15
ALHA81019
ALHA81020
ALHA81033
ALHA81034
ALHA81036
ALHA81039
ALHA81042
ALHA81062
ALHA81063
ALHA81064
ALHA81067
ALHA81070
ALHA81071
ALHA81072
ALHA81075
ALHA81077
ALHA81080
ALHA81081
ALHA81082
ALHA81O83
ALHA81084
ALHA81O88
ALHA81089
ALHA81090
ALHA81091
ALHA81100
ALHA81108
ALHA81110
ALHA81113
ALHA81115
ALHA81116
ALHA81118
ALHA81120
ALHA81124
Weight
(g)
1208
572
506
3
3
20
50
13
20
11
90
19
37
27
24
86
36
42
28
12
47
93
153
5489
1051
1353
252
255
252
206
534
0.5
5
191
228
4
2
3
16
4
17
5
6
7
16
4
11
10
12
155
69
3
111
155
2
85
14
9
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
C
B
C
C
C
B
C
B
B
B
B
B
B
C
C
B/C
B
B
C
B
B
B
B
Be
B/Ce
Be
C
B
C
A/B
C
C
B/C
C
C
B/C
B
B/C
B
B
A/B
B
B
B
B
B
B
B
B
B
B
B/C
B/C
C
B
B/C
B/C
B
fracturing
A
B
B/C
B
B
B
B
A
B
A
B
B
B
B
A
B
A
A
A
B
A
A
B
B
B
A
C
B
A
B
C
A
B
A/B
B
A
A
A
A
A
A
A
A
A
A
A
A
A
B
A
B
A
C
A/B
A
A
B
A
Specimen
number
ALHA81125
ALHA81126
ALHA81128
ALHA81129
ALHA81130
ALHA81132
ALHA81133
ALHA81135
ALHA81136
ALHA81138
ALHA81139
ALHA81141
ALHA81143
ALHA81144
ALHA81148
ALHA81152
ALHA81155
ALHA81158
ALHA81161
ALHA81163
ALHA81164
ALHA81165
ALHA81166
ALHA81168
ALHA81169
ALHA81170
ALHA81171
ALHA81173
ALHA81174
ALHA81175
ALHA81176
ALHA81178
ALHA81179
ALHA81182
ALHA81183
ALHA81186
ALHA81188
ALHA81192
ALHA81194
ALHA81195
ALHA81197
ALHA81201
ALHA81202
ALHA81207
ALHA81209
ALHA81211
ALHA81213
ALHA81215
ALHA81216
ALHA81218
ALHA81219
ALHA81220
ALHA81226
ALHA81227
ALHA81228
ALHA81230
ALHA81232
ALHA81233
Weight
(g)
10
22
16
32
30
5
21
10
1
4
7
1
13
3
13
10
5
2
122
82
20
6
26
8
6
59
24
26
33
13
95
30
14
5
104
23
9
9
17
5
68
7
5
14
14
7
3
11
2
6
24
3
3
11
8
13
5
25
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
B
B
B/C
A/B
B
B
B
B
B
B
B/C
B/C
B/C
B
B
B
A/B
B/C
C
C
B
B
B
C
B
B
B/C
A/B
B
A/B
B
B/C
B
B
C
B
A/B
A/B
B
B
B/C
B/C
C
C
B/C
B
B/C
A
C
C
B
B/C
C
B
B/C
B
B
C
fracturing
A
A
A
A
B
A
A
A
A/B
A
B
B
A
A
A
A
A
A
C
B/C
A
A
A
B
B
A/B
B
A
B/C
B
A
B/C
A
A/B
B/C
A/B
A
A
B
A/B
B/C
A
A
B
A
A
A
A
A
B
A
A/B
A
B
A
B
A/B
B/C
98 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE B.?Continued.
Specimen
number
ALHA81236
ALHA81237
ALHA81238
ALHA81239
ALHA81240
ALHA81241
ALHA81242
ALHA81244
ALHA81245
ALHA81246
ALHA81249
ALHA81252
ALHA81255
ALHA81256
ALHA81263
ALHA81265
ALHA81269
ALHA81270
ALHA81274
ALHA81275
ALHA81276
ALHA81277
ALHA81281
ALHA81283
ALHA81284
ALHA81286
ALHA81287
ALHA81293
ALHA81294
ALHA81295
ALHA81296
ALHA81297
ALHA813OO
ALHA81301
ALHA81302
ALHA81305
ALHA81306
ALHA813O8
ALHA81314
ALH82103
ALH82108
ALH82109
ALH82112
ALH82114
ALH82115
ALH82119
ALH82120
ALH82122
ALH82129
ALH82134
ALH82141
ALH82144
ALH830O3
ALH83OO5
ALH83OO6
ALH83012
ALH83O2O
ALH83025
Weight
(g)
41
27
24
32
41
34
20
5
4
3
10
2
12
28
6
8
5
4
19
11
42
7
46
0.6
10
28
78
2
9
105
13
20
10
12
4
1
7
19
3
2529
14
47
28
41
48
24
7
142
14
28
0.6
7
322
228
230
203
3
78
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
A/B
B
C
B
C
B
B/C
B
B/C
C
B/C
B
B
C
B
B/C
B/C
C
A/B
B
C
B
B
B/C
B/C
B
C
B
B
C
B/C
B
A/B
B/C
B/C
B/C
B
B/C
B
B
B/C
B/C
C
A/B
A/B
B/C
B
B
B/C
B/C
C
B
A/B
C
B/C
B/C
B
C
fracturing
A/B
B
B
B
C
A/B
A
A
A/B
A
A
A
B
A
B
A
A
A/B
A
A
B
A
B
A
A
B
B/C
A/B
A
B/C
B
A
A
A
A
A
A
B
A
B
A
A/B
A
A
A
B
A
A
A
A
A
A
A
B
C
B
B
B
Specimen
number
ALH83029
ALH83O3O
ALH83O31
ALH83034
ALH83O35
ALH83036
ALH83037
ALH83039
ALH83040
ALH83044
ALH83046
ALH83047
ALH83049
ALH83O51
ALH83O53
ALH83O55
ALH83056
ALH83057
ALH83059
ALH83060
ALH83061
ALH83O62
ALH83064
ALH83065
ALH83066
ALH83068
ALH83072
ALH83O73
ALH83074
ALH83104
ALH83107
ALH84003
ALH84055
ALH84060
ALH84064
ALH84067
ALH84068
ALH84069
ALH84073
ALH84074
ALH84075
ALH84076
ALH84077
ALH84078
ALH84085
ALH84088
ALH84089
ALH84091
ALH84094
ALH84098
ALH84099
ALH84100
ALH84111
ALH84117
ALH84121
ALH84124
ALH84128
ALH84131
Weight
(g)
96
49
10
6
1
24
2
6
78
5
33
20
6
16
63
18
1
63
4
9
34
77
12
54
46
0.8
2
49
6
2
38
3089
6901
339
1889
391
1114
1136
631
758
789
369
276
283
554
298
304
215
208
261
150
110
132
72
141
114
2
108
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
B/C
B/C
B
B
B
A
B/C
B
B/C
A
A/B
B/C
B
A/B
C
B/C
A/B
B
B/C
C
B/C
B/C
C
C
C
C
C
C
cB
B/C
A/B
Be
B
B
C
B
A
B
A/B
C
B/C
B
B/C
B/C
B
B/C
B/C
C
B/C
B/C
B
B
B
C
C
C
C
fracturing
A
B/C
A
B
A
A/B
A/B
A/B
A
A
A
A
B
A
C
A
A
B
A
B
A/B
B
A/B
A
B
A
A
B
A
A
A
A
B
A
A
B/C
A
A
A
B
B/C
A
A
A
B/C
A
A
A
B
A
B
A
A/B
A
B/C
B/C
B
B/C
NUMBER 30 99
TABLE B.?Continued.
Specimen
number
ALH84133
ALH84135
ALH84137
ALH84138
ALH84139
ALH84144
ALH84145
ALH84146
ALH84148
ALH84149
ALH84152
ALH84155
ALH84156
ALH84157
ALH84158
ALH84161
ALH84162
ALH84163
ALH84167
ALH84172
ALH84175
ALH84178
ALH84179
ALH84183
ALH84184
ALH84185
ALH84192
ALH84194
ALH84196
ALH84199
ALH84201
ALH84202
ALH84213
ALH84216
ALH84217
ALH84221
ALH84222
ALH84223
ALH84225
ALH84226
ALH84227
ALH84228
ALH84236
ALH84237
ALH84239
ALH84240
ALH84241
ALH84245
ALH84246
ALH84248
ALH84249
ALH84251
ALH84253
ALH84259
ALH84260
ALH84263
ALH85021
ALH85024
Weight
(g)
70
31
145
20
157
54
19
33
168
12
6
114
28
89
54
83
42
135
151
3
35
0.4
46
28
42
5
4
4
10
27
6
88
7
5
3
16
10
11
9
28
12
10
32
8
15
26
17
19
2
5
23
34
7
23
15
5
647
388
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
B
B/C
B/C
B
A
C
B
B
C
C
B/C
B/C
B/C
B/C
B/C
C
C
C
C
B/C
C
B
B/C
B
B
C
C
C
B/C
C
B/C
C
B
B/C
C
C
C
C
C
B
C
B/C
B
C
B
C
C
B
A/B
B
B/C
B/C
B/C
C
B
C
Be
B/C
fracturing
A
A
C
A
A
A/B
B
B/C
C
C
A
A
A
A
A
B/C
B/C
A
B
B
B
A
B/C
B
B
A
A
A/B
A
A
A
B
A
A/B
A
A
A
A
B
A
B/C
B
B
B
A
A
B
A
B
B
A/B
B
A
B/C
A
A
B
A/B
Specimen
number
ALH85025
ALH85038
ALH85042
ALH85043
ALH85048
ALH85051
ALH85054
ALH85055
ALH85056
ALH85067
ALH85068
ALH85071
ALH85074
ALH85077
ALH85086
ALH85O88
ALH85089
ALH85091
ALH85097
ALH85098
ALH85099
ALH851OO
ALH85102
ALH85104
ALH85107
ALH85110
ALH85111
ALH85114
ALH85120
ALH85122
ALH85125
ALH85126
ALH85133
ALH85134
ALH85141
ALH85142
ALH85143
ALH85144
ALH85145
ALH85146
ALH86601
ALH86603
ALH86606
ALH86611
ALH86612
DOM85500
DOM85501
DOM85507
EETA79007
EET82603
EET82604
EET82614
EET83200
EET83203
EET83208
EET83223
EET83256
EET83262
Weight
(g)
713
125
128
205
17
5
55
6
7
1
4
19
3
12
12
0.4
1
31
61
7
7
58
13
99
37
22
13
11
8
61
19
47
91
10
11
51
18
18
46
40
309
104
4
9
2
60
126
190
200
8210
1571
8
779
546
263
219
5
24
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
C
B/C
B/C
B
C
B/C
C
C
C
B
C
C
C
B/C
B/C
C
B/C
B/C
B/C
C
B/C
B
B
B/C
B/C
B
C
C
C
B
B/C
B/C
B
C
C
B/C
C
B
C
A/B
B
A/B
B/C
C
C
B
C
C
B
Be
B/C
A/B
B/C
B/C
B/C
B
B
A
fracturing
A/B
A
A
A
A/B
A
A/B
A
A
A
B
B
A
A
A
A
B
A
B
A
A
A
A
B
A
B/C
B
A
B
B
A/B
B
A/B
A
A
B
A
A
A/B
A
B/C
A
A
A
A
A/B
A
B
B
A
B
A
B
B/C
B
B
A
A
100 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE B.?Continued.
Specimennumber
EET83278
EET83282
EET83285
EET83287
EET83292
EET83293
EET833OO
EET83303
EET83305
EET83324
EET83326
EET83331
EET83338
EET83346
EET83347
EET83349
EET83351
EET83369
EET83372
EET83377
EET83388
EET834OO
EET83402
EET83403
EET84303
GRO85200
GRO85203
GRO85206
GRO85210
GRO85211
LEW85314
LEW85316
LEW85318
LEW85319
LEW85320
LEW85324
LEW85326
LEW85327
LEW85334
LEW85336
LEW85338
LEW85341
LEW85342
LEW85344
LEW85345
LEW85347
LEW85352
LEW85355
LEW85357
LEW85358
LEW85364
LEW85367
LEW85371
LEW85372
LEW85375
LEW85379
LEW85382
LEW85387
Weight
(g)
72
79
3
46
9
19
115
12
167
143
113
0.3
27
22
37
28
81
39
169
152
35
113
50
12
58
3822
1450
2420
247
355
14
34
152
11491
110224
514
225
439
177
60
99
76
7
3
32
31
9
6
61
14
4
6
55
9
37
26
10
4
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
B
B/C
B
B
B/C
B
C
B/C
B
B/C
C
B/C
C
B
C
C
B
C
B
C
C
C
C
C
C
B/C
B
B/Ce
B
B
C
C
C
B/Ce
Be
B
C
B/C
B/C
B/C
B
C
C
C
B/C
C
C
C
B/C
C
C
C
C
C
C
C
B/C
C
fracturing
A
B
B
B
B
A/B
B
A
B/C
B
B
A
B
B
A
B
B
A
C
B/C
A
A
B
A
A
A
B
B
A
A
A/B
B/C
B
B
B
B
A
B
A
A
B/C
A
A
A
A
A
A
A/B
B
B
A
A
A
A
A
A
A/B
A
Specimen
number
LEW85389
LEW85393
LEW85395
LEW85404
LEW85405
LEW85406
LEW85407
LEW85409
LEW85414
LEW85416
LEW85422
LEW85423
LEW85426
LEW85433
LEW85435
LEW85447
LEW85448
LEW85450
LEW85453
LEW85455
LEW85456
LEW85458
LEW85459
LEW85460
LEW85464
LEW85466
LEW86020
LEW86026
LEW86029
LEW86031
LEW86032
LEW86035
LEW86036
LEW86037
LEW86039
LEW86041
LEW86044
LEW86045
LEW86046
LEW86047
LEW86049
LEW86050
LEW86051
LEW86053
LEW86055
LEW86058
LEW86059
LEW86060
LEW86062
LEW86063
LEW86068
LEW86071
LEW86072
LEW86074
LEW86076
LEW86077
LEW86078
LEW86079
Weight
(g)
4
51
17
34
63
7
19
29
26
6
27
11
16
57
21
16
34
27
5
8
19
17
32
6
24
14
361
22
17
74
1
78
9
6
41
23
19
5
5
69
15
11
2
4
41
22
2
23
13
7
6
8
12
19
24
9
37
7
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
C
Be
B/C
B
B/C
C
c
B/C
C
C
cB/C
B/C
C
cc
c
B/C
C
C
C
B/C
B/C
C
C
cc
B/C
C
c
B/C
B/C
B/C
B/Ce
B/C
B/C
C
C
C
C
C
B/C
B/C
B/C
B/C
B/C
B/C
C
cc
c
B/C
C
B/C
B/C
B/C
B/C
B/C
fracturing
A/B
B
A
B
A/B
A/B
A
A
A
A
A
A
A
A/B
A/B
A
A
A
A
A
A
A
A/B
A
A
A
B
A
A
A/B
A
B
A
A
A
A
A
B
B
B
B
A
A
A
A
A
A
A
A
A
A
A
A
A/B
A
A
A
A
NUMBER 30 101
TABLE B.?Continued.
Specimen
number
LEW86080
LEW86081
LEW86083
LEW86086
LEW86087
LEW86088
LEW86091
LEW86092
LEW86093
LEW86094
LEW86095
LEW86096
LEW86099
LEW86100
LEW86103
LEW86104
LEW86106
LEW86107
LEW86108
LEW86109
LEW86111
LEW86112
LEW86116
LEW86118
LEW86121
LEW86122
LEW86125
LEW86126
LEW86128
LEW86129
LEW86130
LEW86131
LEW86136
LEW86142
LEW86143
LEW86147
LEW86148
LEW86150
LEW86151
LEW86152
LEW86153
LEW86154
LEW86155
LEW86156
LEW86159
LEW86164
LEW86167
LEW86172
LEW86174
LEW8618O
LEW86187
LEW86188
LEW86189
LEW86191
LEW86192
LEW86194
LEW86197
LEW86198
Weight
(g)
14
28
199
104
11
38
67
21
15
15
14
71
28
24
9
34
6
47
4
17
33
18
17
30
8
9
14
7
15
7
3
10
13
14
23
13
2
7
13
15
31
9
18
24
8
26
13
7
27
11
11
6
10
11
11
10
18
15
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
C
C
Ce
C
C
C
C
B
C
C
C
C
C
C
C
C
C
C
C
C
C
Ce
C
C
B/C
C
cc
c
B/C
C
C
C
C
C
c
B/C
B
C
C
C
B
B/C
B/C
C
C
C
C
C
C
C
C
C
cc
cc
B/C
fracturing
A
A
A
B
A
A
A
A
A
A
A/B
A
A
A
A
A
A
A
A
A
A
A
A
A
A
A
A
A
A
B
A
A
B
A
A
B
A
A
A
A/B
A
A
A
A
A
A
A
A
A/B
A
A
B/C
A
A
A
A/B
B
A
Specimen
number
LEW86199
LEW86200
LEW86206
LEW86208
LEW86209
LEW86215
LEW86217
LEW86223
LEW86225
LEW86226
LEW86228
LEW86230
LEW86232
LEW86233
LEW86234
LEW86235
LEW86237
LEW86240
LEW86242
LEW86243
LEW86244
LEW86245
LEW86247
LEW86250
LEW86254
LEW86255
LEW86256
LEW86257
LEW86259
LEW86261
LEW86262
LEW86263
LEW86265
LEW86266
LEW86271
LEW86272
LEW86275
LEW86286
LEW86292
LEW86302
LEW86305
LEW86312
LEW86314
LEW86319
LEW86320
LEW86321
LEW86322
LEW86323
LEW86324
LEW86325
LEW86326
LEW86327
LEW86329
LEW86332
LEW86336
LEW86337
LEW86338
LEW86341
Weight
(g)
32
3
36
7
12
123
20
13
103
49
29
2
19
10
14
7
14
7
13
6
5
3
4
142
9
25
22
4
8
14
10
15
2
41
20
16
35
45
33
40
40
102
41
3
3
33
18
5
8
20
7
44
5
14
8
26
27
9
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
C
C
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
c
B/Ce
Ce
C
C
Be
C
C
C
C
C
C
C
C
C
C
C
cc
cc
c
fracturing
A
A
A
A
A
A
A/B
A
B
A
A
A/B
A
A
A/B
A
A/B
A
A
A/B
A
A
B
A
A
A
A
B
A
A
A
A
A
A
A
A
B/C
B
B
A
B
A
A
A
A
B
A
A
A
A
A
A
A
A
A
B
A/B
A
102 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE B.?Continued.
Specimen
number
LEW86344
LEWg6345
LEW86353
LEW86354
LEW86356
LEWg6361
LEW86362
LEW86363
LEW86365
LEW86366
LEW86368
LEW86369
LEW86370
LEW86371
LEW86373
LEWg6374
LEWg6375
LEWg6376
LEWg6383
LEWg6384
LEW86385
LEWg6387
LEW86388
LEW86389
LEW86391
LEWg6393
LEWg6394
LEWg6395
LEWg6396
LEW86397
LEW86398
LEW86400
LEW86401
LEW86403
LEW86405
LEWg6407
LEW86413
LEWg6414
LEW86415
LEW8641g
LEWg6420
LEWg6422
LEWg6423
LEW86424
LEW86430
LEW86431
LEWg6434
LEWg6437
LEW8643g
LEW86440
LEW86441
LEWg6442
LEWg6443
LEWg6444
LEWg6450
LEWg6451
LEWg6452
LEWg6453
Weight
(g)
17
4
5
23
9
6
6
3
5
26
29
7
9
147
30
32
11
41
11
6
34
26
24
2
15
70
3
14
13
10
3
19
9
7
1
36
14
4
3
43
13
g
11
7
6
10
22
17
45
7
11
59
11
15
5
34
20
49
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
C
C
c
B/C
C
B/C
C
B/C
C
C
C
C
C
C
C
C
C
cc
cc
cc
cc
cc
c
B/C
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
cc
c
fracturing
A
A
A
A
A
A
B
A
A
A
A
A
A
B
A/B
A
B
A/B
A
A
A
A
A
A
A
B
A
A
A
A
A
A
A
A
A
A/B
A
B
B
C
A
A
A
A
A/B
A
A/B
A
A
A
A
A
A
A
A
A
A
A/B
Specimen
number
LEWg6454
LEW86455
LEWg6456
LEW86457
LEWg6458
LEW86459
LEWg6460
LEWg6461
LEW86462
LEW86463
LEW86464
LEW86465
LEW86467
LEW86468
LEW86469
LEW86470
LEW86472
LEW86473
LEW86475
LEW86476
LEW86477
LEW86479
LEW86480
LEW86482
LEWg6484
LEWg6485
LEWg6486
LEW86487
LEW86488
LEW86489
LEW86491
LEWg6492
LEWg6496
LEW86497
LEW86499
LEW86500
LEWg6501
LEW86503
LEW86506
LEW86507
LEW86508
LEW86509
LEW86510
LEW86513
LEW86514
LEWg6515
LEW86516
LEW86517
LEW86518
LEW86519
LEW86520
LEW86521
LEWg6523
LEWg6525
LEWg6527
LEWg6529
LEW86530
LEW86532
Weight
(g)
3
50
22
13
18
8
19
0.6
25
65
19
26
0.4
12
11
59
30
21
15
0.6
12
141
12
7
24
52
10
15
9
30
15
25
5
6
25
45
85
22
30
10
10
33
24
6
65
34
4
32
267
8
6
0.3
7
46
22
1
2
4
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
Degree of
weathering
C
C
cc
cc
cc
cc
cc
cc
cc
c
B/C
cc
B/C
cc
cc
cc
cc
c
B/C
cc
cc
cc
B/C
B/C
c
B/C
C
C
B/C
c
B/C
B/C
B/C
B/Ce
C
C
B
C
C
C
C
B/C
C
fracturing
A
A
A
A
A
A
A/B
A
A
A
A
A
A
A
A
A
A
A
A
A
A
A
A
A
A
A
A
A
A
B
A
A
B/C
A
A
A
B
A
A/B
A
A/B
A
B
B
A
A
A
A
B
A
B
A
A
A
A
A
A
A
NUMBER 30 103
TABLE B.?Continued.
Specimen
number
LEW86533
LEW86534
LEW86536
LEW86538
LEW86545
META78009?
META78010
META78011
META78012
META78018?
MIL85600
PCA82517
PCA82521
PCA82522
RKPA78005?
RKPA79004
RKPA79014
RKPA80210
RKPA80217
RKPA80218
RKPA80220
RKPA80223
RKPA80227
RKPA80230
RKPA80233
RKPA80236
RKPA80240
RKPA80243
RKPA80244
RKPA80245
RKPA80247
RKPA80249
RKPA80250
RKPA80251
RKPA80257
RKPA80260
RKP86705
TIL82409
TIL82412
TIL82413
TIL82414
TIL82415
ALH82102
ALHA78147I
ALHA76006
ALHA76008
ALHA77046*
ALHA77111*
ALHA77131*
ALHA77133*
ALHA77134*
ALHA77144
ALHA77146*
ALHA77147*
ALHA77148
ALHA77149*
Weight
(g)
16
89
8
21
16
29
234
116
86
82
497
41
1
46
29
371
78
11
8
7
124
25
8
58
414
16
61
3
14
37
1
10
4
29
9
8
68
231
35
18
15
70
48
31
1137
1150
8
52
26
19
19
8
18
19
13
26
Class
and
type
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5
H5,6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
Degree of
weathering
C
B/C
C
cc
B
Be
C
B
B
C
B/C
C
B/C
B
B/C
B/C
B/C
C
C
B/C
C
B/C
B
B/C
B/C
C
C
C
B/C
C
B/C
B/C
B
B/C
C
B
B
C
C
B
A/B
B/C
Ce
B/C
A/B
C
A/B
A
A
B
A/B
A/B
C
A/B
fracturing
A
A/B
A
A
A
A
A
A
B
A
A
B
A
B
B
B
B
B
A
A
B/C
B
A
B
B
B
A
A
B
B
B
A
A
B
B
B
C
A
B
B
A
A
A
B
B
A
B
Specimen
number
ALHA77157*
ALHA77183
ALHA77200*
ALHA77209*
ALHA77212*
ALHA77239*
ALHA77246*
ALHA77248*
ALHA77258
ALHA77271
ALHA77285
ALHA77288
ALHA78002$
ALHA78035
ALHA78065t
ALHA78067
ALHA780691:
ALHA78076
ALHA78086I
ALHA78115
ALHA78122
ALHA78124
ALHA78135I
ALHA78137
ALHA78145$
ALHA78152
ALHA78169$
ALHA78184
ALHA78189
ALHA78191
ALHA78207
ALHA78211
ALHA78213
ALHA78215
ALHA78229
ALHA78231
ALHA78249
ALHA79002
ALHA79005
ALHA79016
ALHA79019
ALHA79020
ALHA79024
ALHA79028
ALHA79034
ALHA79037
ALHA79049
ALHA79055
ALHA80118
ALHA80122
ALHA80126
ALHA8O13O
ALHA81O35
ALHA81037
ALHA81O38
ALHA81054
ALHA81055
ALHA81076
Weight
(g)
88
288
0.9
32
17
19
42
96
597
610
271
1880
11
2
7
8
4
276
9
848
5
28
131
70
34
5
22
8
23
20
8
11
10
6
2
2
4
223
60
1146
12
4
22
16
13
15
54
15
2
50
35
5
256
320
229
2
5
10
Class
and
type
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
Degree of
weathering
A/B
C
C
B
A/B
B
B
B/C
B/Ce
C
C
C
A
B
B
B
B
B
A
B
B
B
B/C
B
B/C
C
B
B/C
B
B/C
C
B
B
B
C
B/C
B
B/C
A/B
B/C
C
B
C
B
B
B
fracturing
A
A/B
A
B
B
B
A
B
B
B
B
B
B
B
B
B
A
B
B
B
A
B
B
B
A
B
A
A
A/B
A
B
B
A
A
104 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE B.?Continued.
Specimen
number
ALHA81078
ALHA81079
ALHA81086
ALHA81093
ALHA81094
ALHA81096
ALHA81102
ALHA81103
ALHA81111
ALHA81112
ALHA81127
ALHA81134
ALHA81137
ALHA81146
ALHA81154
ALHA81160
ALHA81180
ALHA81193
ALHA81196
ALHA81204
ALHA81210
ALHA81223
ALHA81224
ALHA81225
ALHA81248
ALHA81250
ALHA81253
ALHA81254
ALHA81268
ALHA81271
ALHA81273
ALHA81288
ALHA81291
ALHA81298
ALHA81303
ALHA81310
ALHA81317
ALH82113
ALH82116
ALH82124
ALH82127
ALH82138
ALH82143
ALH83013
ALH83024
ALH83028-
ALH83O5O
ALH83071
ALH83103-
ALH84071
ALH84082
ALH84083
ALH84093
ALH84101
ALH84105
ALH84108
ALH84109
ALH84110
Weight
(g)
6
7
6
271
152
83
196
136
210
150
15
15
9
24
1
12
17
13
9
7
0.6
10
14
14
5
17
10
9
18
28
43
20
4
16
4
0.7
0.4
61
18
26
5
5
3
246
6
16
10
5
52
798
557
420
114
221
261
215
246
319
Class
and
type
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
Degree of
weathering
B/C
C
B
A/B
C
B
B/C
B/C
B/C
B/C
B/C
B/C
B/C
C
B
C
C
B
B
B
B
A/B
B/C
B
C
B
A/B
C
C
B
C
B
B
B
B/C
B
C
A/B
B
C
A/B
B
C
A/B
B/C
B
A/B
B/C
B
B
C
B/C
B
C
C
B
B/C
B/C
fracturing
B
A
B
A/B
B
B
A/B
B/C
B
A
B
B
A/B
B
B
B
B
A
A
A
A
A
A
A
A/B
B
B
A
B/C
B
B/C
A
A
B
A
A
A
A
B
A/B
A
A/B
A/B
A
A
A
B
A
A
B
A
B/C
B
B
C
B
A/B
A
Specimen
number
ALH84113
ALH84114
ALH84115
ALH84118
ALH84147
ALH84150
ALH84151
ALH84153
ALH84159
ALH84171 -
ALH84176
ALH84180
ALH84186-
ALH84187
ALH84189-
ALH84204-
ALH84208
ALH84211
ALH84214-
ALH84215
ALH84224
ALH84242
ALH84243-
ALH84252
ALH84257-
ALH84262
ALH85018
ALH85020
ALH85023
ALH85028
ALH85030
ALH85O31
ALH85032
ALH85036
ALH85037
ALH85041
ALH85044
ALH85052
ALH85069
ALH85072-
ALH85O81
ALH85094-
ALH85108
ALH85109-
ALH85117-
ALH85127
ALH85128-
ALH8513O
ALH85136
ALH85139
ALH85140
ALH85148-
ALH85156
ALH86607
BOW85800
BTNA78005
DOM85508
EET82610
Weight
(g)
212
120
195
114
54
20
112
243
101
37
5
. 47
20
26
9
24
21
49
5
9
7
17
49
3
19
15
812
744
439
326
620
201
424
231
141
168
105
17
5
4
12
9
15
21
28
10
16
100
75
26
9
4
32
3
141
82
14
42
Class
and
type
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
Degree of
weathering
B/C
B
B/C
B
C
B/C
B
B/C
C
C
cB
B
C
C
C
C
B/C
B/C
B/C
B
C
Ce
B/C
B
C
B
B
B/C
C
B/C
B/C
C
C
B/Ce
C
C
A/B
B
C
B
C
C
Ce
B/C
C
C
B
B
B
B/C
A
C
C
C
B
C
B
fracturing
B
B
B
B
A
A
A
A
A/B
A
B/C
A
B/C
B/C
B
B
B
A
A
A
A/B
B
A
A
B
B
A
B
A
B
A
A
A
A
B
B/C
B
A
B
B
B/C
A
A
A
A/B
A/B
A
A/B
B
B
A
A
A
A
A
B
A
A
NUMBER 30 105
TABLE B.?Continued.
Specimennumber
EET82615
EET83201
EET83215
EET83263
EET83270
EET83275-
EET83281
EET83288-
EET83295
EET83299
EET8331O
EET83320
EET83321
EET83360-
EET83362-
EET83367
EET83373
EET83374
EET83382
EET83385-
EET83393-
EET83394-
EET83397
EET84306
GRO85218
LEW85301 -
LEW85315
LEW85322
LEW85329
LEW8.5330
LEW85331
LEW85335
LEW85337-
LEW85348
LEW85359
LEW85362
LEW85368
LEW85373-
LEW85374
LEW85377-
LEW85378-
LEW85381-
LEW85384-
LEW85391
LEW85392
LEW85399-
LEW85400
LEW85402-
LEW85408-
LEW85410-
LEW85411-
LEW85412
LEW85418
LEW85446-
LEW85462
LEW85469-
LEW85470
LEW86015
Weight
(g)
29
1060
510
10
2
86
51
38
28
6
64
56
11
40
10
107
159
96
12
4
30
54
32
4
7
13
10
582
170
67
54
107
57
31
18
15
18
45
10
31
66
22
6
9
28
8
6
66
3
2
4
71
37
42
23
8
19
780
Class
and
type
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
Degree of
weathering
B
B/C
B/C
C
C
B
C
C
B
C
C
C
C
C
B/C
C
C
C
B
B/C
B/C
C
C
C
C
B/C
C
C
A/B
B/C
C
cc
cc
cc
Ce
B
C
C
C
C
C
C
C
B/C
C
B
C
C
C
C
C
C
C
C
C
fracturing
A
A
C
B/C
B
A
B
B
A/B
B/C
A
B
A
A
A
B
A
A
B
A
B
A
B/C
A/B
A
A
A
A
A
A
A
A/B
A
B
B
A
A
B
A
A/B
A/B
A
B
A
A
A
A
B
A
A
A
A
A
A
A
A
B
B/C
Specimen
number
LEW86017
LEW86028
LEW86030
LEW86052
LEW86066-
LEW86089
LEW86120-
LEW86137-
LEW86139-
LEW86149
LEW86160-
LEW86163-
LEW86168-
LEW86170-
LEW86177
LEW86178-
LEW86181
LEW86182-
LEW86183-
LEW86190-
LEW86196-
LEW86201-
LEW86202
LEW86204-
LEW86205-
LEW86212-
LEW86218-
LEW86221-
LEW86236-
LEW86239-
LEW86241
LEW86249
LEW86252-
LEW86253-
LEW86281
LEW86287-
LEW86295-
LEW86328-
LEW86333-
LEW86335-
LEW86340-
LEW86342-
LEW86343-
LEW86348
LEW86350-
LEW86351
LEW86355
LEW86364-
LEW86381-
LEW86382
LEW86412
LEW86416-
LEW86427
LEW86428
LEW86433-
LEW86439
LEW86445-
LEW86466-
Weight
(g)
688
26
13
2
18
85
33
6
4
19
15
15
18
4
19
13
31
19
23
28
19
18
12
22
17
6
6
18
1
25
33
45
33
10
56
42
44
7
9
3
25
2
6
20
19
10
7
20
7
22
1
18
2
6
6
6
9
71
Class
and
type
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
Degree of
weathering
B
B
C
B/C
C
cc
cc
cc
cc
B/C
cc
cc
cc
B/C
cc
cc
cc
cc
cc
cc
B/C
cc
B
C
C
C
cc
cc
cc
cc
cc
B/C
cc
cc
cc
c
fracturing
A/B
A
A
A
B
A
A
A
A
A
A
A
A
A/B
A
A
B
A
A
B
A
A
A
A
A/B
A
A
A
A
B
A
A
A
A
A/B
A/B
A
A
A
A
A
A
A
A
B
A
A
A
B
A
B
A/B
A
A
A
A
A
A/B
106 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE B.?Continued.
Specimen
number
LEW86471
LEW86474-
LEW86481
LEW86493-
LEW86494
LEW86504-
LEW86522-
LEW86535
LEW86537-
LEW86539
LEW86543-
LEW86544
MBRA76001
MBRA76OO2
META78006
META78007
META78013?
META78014?
META78016?
META78017
META78019?
META78O2O
META78022?
META78023
META78024?
META78025?
META78026
META78027
PCA82512
PCA82516
PCA82523
PCA82526
PCA82527
RKPA79003
RKPA79009
RKPA79012
RKPA80201
RKPA80203
RKPA80206
RKPA80208
RKPA80211
RKPA80213
RKPA80214
RKPA80221
RKPA80231
RKPA80254
RKPA80255
RKPA80262
RKPA80265
RKPA80266
RKP86701
RKP86703
TIL82405
ALHA77081
ALHA81261
ALHA81315
Weight
(g)
83
7
11
5
14
8
43
14
17
13
26
65
4108
13773
410
175
132
101
114
47
91
64
49
56
22
58
75
53
55
16
11
25
3
182
55
13
813
4
47
10
2
19
5
52
238
68
7
32
8
10
177
196
1116
1}
Class
and
type
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
H6
-H(?r
(Acapulco-
like)
Degree of
weathering
C
c
cc
cB/C
C
cc
cB/C
C
B
B
C
B/C
B
C
B/C
B/C
A/B
C
B/C
B
B/C
C
C
B
B
B/C
A
B
A
B
C
B
Be
C
C
B
C
B/C
C
C
C
C
C
C
C
B/C
B
C
B
B
A/B
A/B
fracturing
A
A
A
A/B
A
A
A
A
A
A
A
A
B
B
B
B
B
A
B
A
B
A
A
A
B
B/C
A
B
A
B
B
A
A
A
B
B
A
A
B
A
B
B
B
B/C
B/C
B/C
B
B
B
B
A
B/C
A
A
A
A
Specimen
number
ALHA77011
ALHA77013*
ALHA77015
ALHA77031*
ALHA77033
ALHA77034*
ALHA77036*
ALHA77043*
ALHA77047*
ALHA77049*
ALHA77050*
ALHA77052*
ALHA77115*
ALHA77140
ALHA77160
ALHA77163*
ALHA77164
ALHA77165
ALHA77166*
ALHA77167
ALHA77170*
ALHA77175*
ALHA77176*
ALHA77178*
ALHA77185*
ALHA77197*
ALHA77211*
ALHA77214
ALHA77215
ALHA77216
ALHA77217
ALHA77241*
ALHA77244*
ALHA77249
ALHA77252
ALHA77260
ALHA77303*
ALHA78013
ALHA78015
ALHA780171:
ALHA78037*
ALHA78038
ALHA78041$
ALHA78046
ALHA78119$
ALHA78133
ALHA78149t
ALHA78162t
ALHA78170
ALHA78176J
ALHA78180t
ALHA78186
ALHA78188
ALHA78235$
ALHA78236
ALHA78238
ALHA78239J
ALHA78243
Weight
(g)
292
23
411
0.5
9
2
8
11
20
7
84
112
154
79
70
24
38
31
139
611
12
23
55
6
28
20
27
2111
820
1470
413
144
40
504
343
744
79
4
35
3
0.5
363
118
70
103
60
23
33
21
8
8
3
0.9
19
14
10
16
2
Class
and
type
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
Degree of
weathering
C
B
Ce
B/C
C
B/C
B
B/C
C
B/C
B/C
B/C
B/C
Ce
C
B/C
C
C
C
C
B/C
B/C
B
B/C
A/B
A/B
B/C
C
B
A/B
B
C
B/C
C
B
C
B/C
B
B
C
B
A
B
B
B
B
B
C
B
B
fracturing
A
B
B
B
B
C
C
B/C
C
B/C
B/C
B/C
C
C
C
C
B
NUMBER 30 107
TABLE B.?Continued.
Specimen
number
ALHA79001
ALHA79045
ALHA80133
ALHA81024
ALHA81025
ALHA81030
ALHA81031
ALHA81032
ALHA81053
ALHA81060
ALHA81061
ALHA81065
ALHA81066
ALHA81069
ALHA81085
ALHA81087
ALHA81121
ALHA81145
ALHA81156
ALHA81162
ALHA81190
ALHA81191
ALHA81214
ALHA81229
ALHA81243
ALHA81259
ALHA81272
ALHA81280
ALHA81292
ALHA81299
ALH83008
ALH83010
ALH83017
ALH83O38
ALH84120
ALH84205
ALH85045
ALH85062
ALH85O7O
ALH85155
EET826O1
EET83260
EET83274
EET83395
EET83399
LEW85339
LEW85396
LEW85401
LEW85434
LEW85437
LEW85452
LEW86018
LEW86021
LEW86022
LEW86127
LEW86134
LEW86144
LEW86158
Weight
(g)
32
115
4
798
379
1852
1595
727
3
28
24
13
9
7
16
8
88
21
20
59
48
30
4
40
15
10
23
55
13
0.5
272
395
0.6
87
129
25
145
167
13
18
150
15
83
65
203
29
60
4
19
9
9
502
326
352
12
29
11
9
Class
and
type
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
Degree of
weathering
C
C
B
C
C
B/C
C
C
C
C
B/C
B/C
C
B/C
C
B/C
B
B
B/C
C
C
C
B/C
C
C
cc
cc
c
B
B
C
A/B
B
A/B
B/Ce
A/B
A/B
B/C
B/C
B
B
C
A/B
C
B/C
C
C
C
Be
Ce
B/Ce
B
B/C
B/C
B
fracturing
A
B
B
B
B
B/C
B/C
A
B
B
A
B
B
A
B
B
B
B
B/C
C
A/B
B/C
A
B/C
B
B
B
B
A/B
A/B
A
A
A
A/B
A
B
A
A/B
A
A
A
A
A
A
A
A
A
A
A
A
A
B
A
B
A
A/B
A/B
A
Specimen
number
LEW86207
LEW86213
LEW86246
LEW86270
LEW86307
LEW86347
LEW86367
LEW86408
LEW86417
LEW86436
LEW86495
LEW86505
LEW86549
RKPA79008
RKPA80207
RKPA80256
RKP86700
ALHA79022
ALHA77230
ALHA77304
ALHA78044
ALHA78070
ALHA81040
ALHA81119
ALHA81184
ALH83OO1
ALH83023
ALH84195
ALH85033
ALH85053
ALH85058
DOM85504
EET82611
EET82613
EET83318
EET83329
GRO85212
LEW85317
LEW85333
LEW85343
LEW8535O
LEW85365
LEW85390
LEW85443
LEW86014
LEW86024
LEW86034
LEW86040
LEW86061
LEW86098
LEW86138
LEW86251
LEW86264
LEW86267
LEW86339
LEW86360
Weight
(g)
18
28
2
4
5
3
11
1
2
4
2
44
50
73
18
153
424
31
2473
650
164
10
195
107
17
1569
4
2
250
0.5
0.3
121
13
4
55
68
342
9
48
78
24
8
1
10
662
249
6
49
9
53
47
23
5
18
21
181
Class
and
type
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3
L3,4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
L4
Degree of
weathering
C
Ce
C
B/C
B
C
B
C
B
C
B/C
Ae
B
B
C
B
B
A/B
C
B
B/C
B/C
B
A/B
B
B
B
A
C
A/B
B/C
B
B
A/B
B
B
A/B
B
A
B/C
C
C
B
C
A/B
C
C
B
C
C
C
C
C
C
B/C
fracturing
A/B
A
A
B
A
A
A
A
A
A
A
A/B
A/B
B
B
A
B
B
B
B
B
A
B
A
A
A
A
A
A
A
A
B
A
A
A
A/B
A
A
A
A
A
A/B
A/B
A
A
A
A
A
A
A
A
A
A
A
A
108 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE B.?Continued.
Specimen
number
LEW86410
PCA82514
RKPA80216
RKPA80242
TIL82404
TIL82406
TIL82407
TIL82411
TYR82700
ALHA77002
ALHA77117*
ALHA77127*
ALHA77218*
ALHA77254
ALHA77267*
ALHA78142I
ALHA81018
ALHA81023
ALHA81153
ALHA81198
ALH82104
ALH82107
ALH82117
ALH82137
ALH83002
ALH83O11
ALH83045
ALH83O48
ALH83069
ALH84005
ALH84063
ALH84177
ALH84209
ALH84258
ALH85092
ALH85118
ALH85123
ALH85150
ALH86610
EETA79009
EET83240
EET83242
EET83269
EET83277
EET83291
EET83308
EET83340
EET83386
EET83398
GRO85214
GRO85215
GRO85216
GRO85217
LEW85340
LEW85363
LEW85385
LEW85394
Weight
(g)
3
130
44
7
322
152
221
180
892
235
21
4
45
246
104
32
2237
418
4
0.5
399
9
4
11
367
213
2
2
78
12000
760
7
6
3
26
48
15
13
0.8
140
248
282
8
53
5
137
15
38
67
260
35
13
34
103
44
13
15
Class
and
type
L4
L4
L4
L4
L4
L4
L4
L4
L4
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
Degree of
weathering
B/C
B
B
B/C
B
B
B/C
A/B
Be
B
A/B
B
A
A/B
A
B
B
B
B/C
A
B/C
B
B
B
C
B/C
B/C
A
A/B
A/B
B
C
B
A/B
B/Ce
B
B
B
B
B
A/B
A/B
B/C
B
B
A/B
B
B
B
B
B/C
B
B
B/C
C
fracturing
A
A
B
B
B
A
A
A
A
A/B
A
B
A/B
A
A
A/B
A
B
A
A
B
A
A
A
A
A
B
A/B
A
A/B
A
B
B
A
B
A/B
B
A/B
A
B
A
B
A
B/C
B
A
A
A
A
A
A
A
Specimen
number
LEW85417
LEW85427
LEW85451
LEW86065
LEW86124
LEW86222
LEW86224
LEW86260
LEW86346
LEW86352
LEW86357
LEW86392
LEW86502
LEW86524
LEW86542
META78015?
PCA82504
PCA82505
PCA82510
PCA82513
PCA82519
RKPA79013
RKPA80209
RKPA80228
RKPA80268
TIL82400
ALHA76001
ALHA76003
ALHA76007
ALHA76009
ALHA77OO1
ALHA77008*
ALHA77019*
ALHA77026*
ALHA77027*
ALHA77069*
ALHA77089*
ALHA77150
ALHA77155
ALHA77159*
ALHA77162*
ALHA77180
ALHA77198*
ALHA77231
ALHA77251*
ALHA77261
ALHA77269
ALHA77270
ALHA77272
ALHA77273
ALHA77277
ALHA77280
ALHA77281
ALHA77282
ALHA77284
ALHA77292
ALHA77293*
Weight
(g)
9
15
15
9
8
9
7
12
3
27
3
. 6
25
23
25
37
3094
3086
254
239
125
11
10
11
3
221
20151
10495
410
407000
252
93
60
20
4
0.8
8
58
305
17
29
191
7
9270
69
412
1045
589
674
492
143
3226
1231
4127
376
200
110
Class
and
type
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L5
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
Degree of
weathering
B/C
B
B/C
C
B/C
B
B/C
C
C
A/B
A/B
B
B
B/Ce
B/C
B
A/B
B
A
A/B
B
B/C
C
C
B/C
A/B
A
A
B
B
B
A
B/C
B/Ce
B/C
B/C
B
C
A/B
A/B
A
C
B
A/Be
B
B
Be
A/B
B/C
B
A/B
Be
B
B
A/B
B
B
fracturing
A
A
A
A
A
A
A
A/B
A
A
A
A
A
A
A
A
B
B
A
A
A
B
B
B
B
B
A
A
A
B
B
B
A
A
A/B
B
A
B
B
B
A
B/C
B
B
B
A
NUMBER 30 109
TABLE B.?Continued.
Specimen
number
ALHA77296
ALHA77297
ALHA77301*
ALHA77305
ALHA78003
ALHA78O39
ALHA78042
ALHA78043
ALHA78045
ALHA78048
ALHA78050
ALHA78055$
ALHA78O59*
ALHA78074
ALHA78078
ALHA78101
ALHA78103
ALHA78104
ALHA78105
ALHA78106
ALHA78112
ALHA78114
ALHA78125I
ALHA78126
ALHA78127
ALHA78130
ALHA78131
ALHA78156
ALHA78171*
ALHA78251
ALHA79007
ALHA79018
ALHA79027
ALHA79033
ALHA79043
ALHA79052
ALHA80101
ALHA8O1O3
ALHA80105
ALHA80107
ALHA8O1O8
ALHA80110
ALHA80112
ALHA80113
ALHA80114
ALHA8O115
ALHA80116
ALHA80117
ALHA80119
ALHA80120
ALHA80125
ALHA81016
ALHA81017
ALHA81026
ALHA81027
ALHA81028
ALHA81029
ALHA81099
Weight
(g)
963
952
55
6444
125
299
214
680
397
191
1045
14
9
200
290
121
590
672
942
465
2485
808
19
607
195
2733
269
9
23
1312
142
121
133
281
62
23
8725
536
445
178
125
168
331
313
233
306
191
89
34
60
139
3850
1434
516
3835
80
153
152
Class
and
type
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
Degree of
weathering
A/Be
A
A
B/C
C
B
B
B
B/C
A/B
B
B
B
B
A/B
B
B
B
A/B
B
B/C
B
B
B/C
B/C
B/C
B
B
A/B
B/C
B
B
C
B/C
Be
B
B
B
B
B
B
B
B
B
B/C
B
B
B
B/C
Be
B
B
C
B
C
A/B
fracturing
A
B
B
B
B
A
B
B
B
B
B
A
B
A
A
A
B
B
B
B
B
B
A
A
B
A/B
A
A
B
B
B
A
B
B
B
B
B
B/C
B
A
B
A
B
B
B
A
A
A
A/B
B
A
A
Specimen
number
ALHA81106
ALHA81107
ALHA81122
ALHA81131
ALHA81150
ALHA81159
ALHA81167
ALHA81172
ALHA81181
ALHA81203
ALHA81205
ALHA81217
ALHA81221
ALHA81235
ALHA81247
ALHA81257
ALHA81262
ALHA81266
ALHA81278
ALHA81282
ALHA81289
ALHA81304
ALHA81307
ALHA81311
ALH82105
ALH82111
ALH82118
ALH82121
ALH82123
ALH82125
ALH82139
ALH82140
ALH82142
ALH83OO4
ALH83021 -
ALH83027-
ALH83033
ALH83041 ~
ALH83043-
ALH83052
ALH83058-
ALH83063-
ALH83067
ALH831O1
ALH831O5-
ALH84002
ALH84056
ALH84057
ALH84058
ALH84061
ALH84062
ALH84065
ALH84066
ALH84070
ALH84072
ALH84079
ALH84080
ALH84087
Weight
(g)
48
140
21
13
2
10
59
33
15
4
3
5
9
7
104
29
55
12
1
31
4
42
57
0.9
363
63
111
2
111
178
0.2
0.3
20
814
42
3
21
0.3
3
53
29
17
96
639
0.7
7554
2140
368
2003
676
958
1642
356
3952
721
750
287
315
Class
and
type
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
Degree of
weathering
B
B
B
A/B
C
B/C
B/C
C
B
C
B
C
C
C
A/B
B
A/B
A/B
B
A/B
A
A/B
B
B
A/B
A/B
A/B
A
B
C
B
C
C
B
B
B
B/C
C
B
C
A
A/B
A/B
A
A
Be
Be
B/Ce
B
B
A/B
A/B
B
A/B
Be
A/B
B
A/B
fracturing
B
A
B
B
A
A
B
B
A
A
A
B/C
A/B
B
B
A
B
B
A
A
A
B
B/C
A
A
A
B
B
A
B
A
A
B/C
A
A
A
B
A
A/B
B
A
A
A
A
A
A/B
A/B
A
A
A
A
A
A
A
A
A
A
A
110 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE B.?Continued.
Specimennumber
ALH84090
ALH84092
ALH84095
ALH84097
ALH84102
ALH84104
ALH84106-
ALH84112
ALH84127-
ALH84129
ALH84130-
ALH84132
ALH84134
ALH84140
ALH84141
ALH84142-
ALH84143-
ALH84160-
ALH84164
ALH84166-
ALH84169
ALH84173
ALH84174-
ALH84181-
ALH84182
ALH84193-
ALH84197-
ALH84203-
ALH84207-
ALH84210-
ALH84212-
ALH84218-
ALH84219-
ALH84229-
ALH84231-
ALH84234-
ALH84238-
ALH84244-
ALH84247-
ALH84256-
ALH84261 ~
ALH84264
ALH85014
ALH85016
ALH85017
ALH85022
ALH85026
ALH85027
ALH85029
ALH85034
ALH85039
ALH85040-
ALH85046
ALH85047-
ALH85049-
ALH85050-
ALH85060-
ALH85061 -
Weight
(g)
202
214
277
389
214
201
95
146
84
38
45
158
113
164
130
78
74
54
101
39
98
2
32
33
14
9
8
9
4
9
7
33
10
7
43
4
2
34
50
3
5
138
75
1412
2361
952
817
370
389
344
140
96
149
4
5
0.9
0.5
2
Class
and
type
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
Degree of
weathering
Ce
A/B
A/B
B
B
B
B/C
A/B
B
A
B/C
B
B
C
B
A/B
B
B
A/B
B
B/C
C
B
A/B
B
A/B
B
A/B
B
C
B/C
A/B
C
B
B
A
B
B
A/B
B
A
A
A
A/B
A
B
A
B
A/B
A
A
B
B
B
B/C
A
B
A/B
fracturing
A
B
A
A
B
B
A
B
B
A
B
A
A
B
B
B
B
A
A
B/C
C
B
B
B
B
C
A
B
A
B/C
A/B
A/B
A
A
B
B
B
A
B
B
A
A
A
A
A
A
A
A
A
A/B
A
A/B
A/B
A
A
A/B
A
B
Specimen
number
ALH85063-
ALH85064-
ALH85065-
ALH85075-
ALH85076-
ALH85078
ALH85O8O-
ALH85082-
ALH85083-
ALH85087-
ALH85090-
ALH85093-
ALH85095-
ALH85096-
ALH85101-
ALH85103-
ALH85105-
ALH85112-
ALH85113-
ALH85115-
ALH85124-
ALH85131-
ALH85132-
ALH85147-
ALH85149-
ALH85157-
ALH86600
ALH86602
ALH86604
ALH86605-
ALH86608-
ALH86609-
BTNA78001
BTNA78002
DOM85502
DOM85503
DOM85509-
DOM85510-
EETA79003
EETA79010
EET82605
EET82606
EET82607
EET82612
EET83202
EET83205
EET83206
EET83209
EET83210
EET83214
EET83216
EET83217
EET83218
EET83219
EET83220
EET83222
EET83237
EET83238
Weight
(g)
13
4
10
36
78
1
54
19
93
11
11
11
33
3
8
87
12
23
40
22
63
34
49
3
17
20
411
265
13
12
10
8
161
4301
302
720
76
32
436
287
625
982
165
32
1213
471
462
520
426
1398
790
375
192
243
331
317
883
382
Class
and
type
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
Degree of
weathering
B
C
B
B
Be
C
B
A/B
A/B
A/B
B/C
B
B
A
B
A
A/B
A/B
A/B
B
B
B
A/B
B
B/C
B
B
B
B/C
A/B
B/C
A/B
B
B
B
A
B/C
B/C
B
B
B
B
B/C
A
A/B
A/B
B
B/C
A/B
B
B
B
B
B
B
B
B
A
fracturing
B
B
A
A/B
B
B/C
B
B
B
B
A
A/B
A
A
B
B
B
B/C
B
C
B
B
A/B
A
A/B
A
B
A
A
A
A
A
B
A
B
B
B
A
B
C
A
B
A
A
B
B
A
A
B
A
A
B
A
A
A
B
A/B
A/B
NUMBER 30 111
TABLE B.?Continued.
Specimen
number
EET83239
EET83241
EET83243
EET83244
EET83252
EET83253
EET83255-
EET83257-
EET83258-
EET83259
EET83261-
EET83264-
EET83265-
EET83266-
EET83268
EET83271
EET83272-
EET83276
EET83279-
EET83280-
EET83284-
EET83286-
EET83289
EET83294-
EET83296-
EET83297-
EET83298
EET83301~
EET83302-
EET.83304-
EET83306
EET83312
EET83314-
EET83315-
EET83316-
EET83317
EET83319-
EET83323
EET83325-
EET83328-
EET83330-
EET83335
EET83336-
EET83339-
EET83342
EET83343
EET83344-
EET83345
EET83348
EET8335O-
EET83353-
EET83354
EET83356-
EET83358-
EET83363
EET83364
EET83365-
EET83366-
Weight
(g)
282
203
288
384
184
44
39
14
47
4
54
17
55
56
19
67
35
49
36
29
53
34
8
82
63
18
9
87
130
37
42
93
24
113
51
119
7
140
93
88
49
227
130
73
149
125
87
12
299
89
54
8
18
26
185
205
158
189
Class
and
type
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
Degree of
weathering
C
B
A
B
B/C
B
B
B
A/B
A
B
B
B
C
A/B
B
B
B
B/C
B
B
B
B
A/B
B/C
C
B
A/B
A/B
B
B
B
B/C
B/C
B
C
B
C
B/C
B
A/B
B/C
B
B
B
C
C
A/B
A/B
A/B
C
B
B/C
B
A/B
B
B
fracturing
A/B
A/B
A
A
A
A
A
A
A
A
A
A
A
A
A
A
B
A
A
A
B
B
B
A
A
A
A
A
B
A
B
A
B
A
A
B
B
B
A
A
A
B
B
B
A
A
A
A
A
B
B
B
A
A/B
A
B/C
A
Specimen
number
EET83368
EET83370-
EET83371-
EET83375-
EET83378-
EET83379-
EET83383-
EET83384-
EET83387-
EET83392-
EET83396-
EET84301
EET84304
EET84307
EET84308
EET86800-
EET86801
GEO85700
GEO85701
GRO85204
GRO85205
GRO85207
GRO85208
GRO85209
GRO85213
LEW85321
LEW85323
LEW85325
LEW85346-
LEW85349
LEW85354-
LEW85356-
LEW85360-
LEW85361
LEW8538O-
LEW85388-
LEW85397
LEW85403-
LEW85413-
LEW85419
LEW85420
LEW85424-
LEW85425
LEW85428-
LEW85430
LEW85431-
LEW85432-
LEW85436
LEW85439-
LEW85442-
LEW85444-
LEW85449-
LEW85454-
LEW85457-
LEW85461-
LEW85463-
LEW85465-
LEW85471
Weight
(g)
51
24
170
267
212
177
117
22
81
164
198
75
152
5
9
116
83
2409
439
1755
1000
2372
1357
1126
4364
527
874
537
30
17
12
8
13
4
14
4
57
12
14
39
12
4
3
21
13
30
2
9
3
29
2
12
8
20
21
12
57
239
Class
and
type
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
Degree of
weathering
C
C
B
B
B
B
B
B
C
B
A/B
B
B
C
B
A
B
B
A
A
A/B
A/B
A
A
B
B/C
Be
B/C
B
C
B/C
B/C
B
C
B
B/C
C
A/B
B
C
B/Ce
B/C
C
B/C
C
C
B
C
C
B/C
C
C
C
B/C
B/C
C
B
C
fracturing
A
B
A
B
A
A
A
A
B
B
A
B
A
A
A
B/C
A
A
A
A/B
A
A
A
A
A
A
A
A
B
A
A
A
B
B
A
A
A
B
A
A
A
A
A/B
A
A
A
A
A
A
A/B
A
A
A
A
A
A
A
A
112 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE B.?Continued.
Specimen
number
LEW85472
LEW86011
LEW86012
LEW86013
LEW86016
LEW86019
LEW86023
LEW86025
LEW86038-
LEW86042
LEW86043
LEW86048-
LEW86054-
LEW86056-
LEW86064-
LEW86073-
LEW86075-
LEW86084-
LEW86085-
LEW86090-
LEW86097-
LEW86110-
LEW86113-
LEW86115-
LEW86132-
LEW86133-
LEW86135-
LEW86140-
LEW86141-
LEW86166-
LEW86169-
LEW86173-
LEW86175-
LEW86179-
LEW86184
LEW86186-
LEW86193-
LEW86195-
LEW86203-
LEW86231-
LEW86238-
LEW86268-
LEW86269-
LEW86273
LEW86274-
LEW86282-
LEW86288-
LEW86289-
LEW86309-
LEW86311-
LEW86317-
LEW86330-
LEW86349
LEW86359-
LEW86372-
LEW86399-
LEW86404-
LEW86409-
Weight
(g)
67
3398
2157
1812
525
432
322
190
19
5
14
6
2
7
24
38
4
53
197
23
2
34
7
33
12
8
10
9
5
21
26
2
2
5
16
47
8
42
61
18
29
22.
22
30
36
62
11
18
14
67
62
21
38
3
12
7
8
24
Class
and
type
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
Degree of
weathering
B/C
A/B
A
B
A/B
B
B
Ce
C
B
B/C
C
B/C
B/C
C
B/C
B/C
C
C
C
C
C
B/C
C
C
A
C
B
C
C
B/C
C
B
B/C
C
Ce
C
A/B
B/C
B/C
B
B/C
C
B
B/C
B
C
B/C
B
B
B
C
C
C
C
B/C
B/C
C
fracturing
A
A
B/C
B
A/B
A/B
A
B
A/B
B
A
B
A
A
A
A
A
A
A
A
B
A
A
A
A/B
A
A
A
A
A
A
A
A/B
A
A
B
A
A
A
A
A/B
A
A
A
A
A
A
B
B
A
A
A
A
A
A
A
A
A
Specimen
number
LEW86421-
LEW86425-
LEW86426-
LEW86429-
LEW86447-
LEW86478-
LEW86490-
LEW86528-
LEW86531
LEW86541-
LEW86546
META78OO2
META78003
META78004?
META78005
META78021?
META78028
PCA82503
PCA82508
PCA82509
PCA82525
PCA82528
RKPA78OO1
RKPA78003
RKPA79001
RKPA79002
RKPA80202
RKPA80215
RKPA80219
RKPA80225
RKPA80252
RKPA80261
RKPA80264
RKP86702
TIL82401
ALHA76004
ALHA77278
ALHA78138J
ALHA79003
ALHA81251
ALH83007
ALH84086
ALH84126
EET83213
TIL82408
ALHA81316
LEW86386
LEW86411
ALHA77060*
ALHA78109
ALHA81151
DOM85505
DOM85506
EET83361
LEW86145
Weight
(g)
3
2
3
7
10
2
2209
50
21
13
41
542
1726
30
172
23
20657
8308
389
286
40
51
235
1276
3006
204
545
9
21
8
11
62
24
195
282
305
313
11
5
158
285
234
41
2727
80
0.7
3
4
64
233
5
31
59
6
4
Class
and
type
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
L6
LL3
LL3
LL3
LL3
LL3
LL3
LL3
LL3
LL3
LL3
LL4
LL4
LL4
LL5
LL5
LL5
LL5
LL5
LL5
LL5
Degree of
weathering
C
C
cB/C
B/C
A/B
Be
A/B
C
B
C
B
B
B
B
B/C
B
Ae
A/B
B
B
B/C
C
Ce
Be
B
Be
C
B
C
A/B
B
B
C
A/B
A
A
B
B
B/C
B
A/B
B
Be
B
B
B
B
A
A/B
B/C
B
A/B
A/B
B/C
fracturing
A
A
A
A/B
A
A
B/C
A/B
A
A
A
A
B
A
B
B
B
B
B
A
B
B
B
B
C
B.
A
B
A
A
A
A
B
A/B
A
A
A
B
B
A
A
B
A
A/B
B
A
A
A
A
B
B
A
B
NUMBER 30 113
TABLE B.?Continued.
Specimen
number
LEW86402
LEW86449
RKPA80234
RKPA80253
BTNA78004
ALHA77041*
ALHA78062
ALHA78063*
ALHA78082J
ALHA78153
ALHA81123
ALHA81185
ALHA81285
ALH83022-
ALH83032-
ALH83054-
ALH83070
ALH84052
ALH84081
ALH84096
ALH84107
ALH84116
ALH84119
ALH84122-
ALH84123-
ALH84125-
ALH84154
ALH84168
ALH8.4198
ALH84255
ALH85019
ALH85035
ALH85O57-
ALH85059-
ALH85066
ALH85073-
ALH85079-
ALH85084-
ALH85129-
ALH85135-
ALH85137-
ALH85138-
Weight
(g)
14
4
136
5
1079
17
11
77
24
152
2
65
20
5
3
17
216
11
612
294
134
56
34
81
97
76
88
14
5
11
633
420
0.8
9
8
16
83
18
127
12
7
18
Class
and
type
LL5
LL5
LL5
LL5
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
Degree of
weathering
C
A/B
B
A/B
B
A
A
A
B/C
B
A/B
C
B
B
A
A
A/B
A
A/B
A
B
A
A/B
B
A
A
B
A/B
A
A
C
A
A
B
A/B
A/B
B
A/B
B/C
A/B
B
fracturing
A/B
A
B
A
A
B
A
A/B
A
A
A
A
A
A
B
A
B
A
A
A
B
A/B
A
A
A
A
A
B
A
A
A/B
A
B
A/B
A
A
B/C
A/B
Specimen
number
ALH85152-
ALH85154-
ALH85158-
EET82608
EET83204
EET83273-
EET83290
EET83341~
EET83352-
EET83357-
EET83359-
EET83380-
EET83391-
EET83401-
EET84305
LEW85386-
LEW85415
LEW85429
LEW85438-
LEW85467-
LEW86057-
LEW86069-
LEW86070-
LEW86082-
LEW86101-
LEW86117-
LEW86161-
LEW86162-
LEW86185
LEW86334
LEW86378-
LEW86419-
LEW86432
LEW86483-
PCA82507
RKPA80222
RKPA80235
RKPA80238
RKPA80248
RKP86704-
TIL82402
ALH84027
Weight
(g)
36
5
3
95
377
147
1
65
20
35
66
119
91
112
10
14
3
7
3
5
55
0.6
19
8
28
13
29
2
5
6
4
2
7
10
480
7
261
18
11
138
476
8
Class
and
type
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL6
LL7?
Degree of
weathering
A/B
A/B
B
A/B
A
A/B
B
B
B/C
B/C
C
B
A/B
A/B
A/B
A/B
A
C
A/B
B/C
B/C
C
A/B
B
B
B
B
A
C
A
C
B
B
B/C
A
B
A/B
A/B
A/B
B/C
A/B
B
fracturing
B
A
B
A
A
A
A
B
B
A
A
A
A
A
B
B/C
A
A
A
A
A
A
A/B
A
A
A
A
A
A
A
A
A
A
A
A/B
B
B
A
A
A
A
B
114 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE B.?Continued.
Specimen
number
ALHA81187
ALH84190
EET84302
ALH84025
LEW86010
ALHA78113
ALH83009
ALH83015
ALH84007
ALH84008
ALH84009
ALH84010
ALH84011
ALH84012
ALH84013
ALH84014
ALH84015
ALH84016
ALH84017
ALH84018
ALH84019
ALH84020
ALH84021
ALH84022
ALH84023
ALH84024
ALHA77256
ALH84001
ALH85O15
EETA79002
EET83246
EET83247
TIL82410
ALHA81208
ALHA76005
ALHA77302
ALHA78O4O
ALHA78132
ALHA78158
ALHA78165
ALHA79017
ALHA80102
ALHA81006
ALHA81007
ALHA81OO8
ALHA81010
ALHA81011
ALHA81012
EETA79004
EETA79005
EETA79011
Weight
(g)
40
8
60
5
7
299
2
3
706
302
336
303
138
225
160
49
264
150
80
82
93
191
36
13
262
194
676
1931
3
2843
48
22
19
2
1425
236
212
656
15
21
310
471
255
164
44
219
406
37
390
451
86
Class
and
type
A
A
A
Brachinite
An
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Au
Di
Di
Di
Di
Di
Di
Di
Di/M
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Degree of
weathering
B/C
C
B/C
A/Be
A/B
A/Be
A/B
A/B
Ae
A/B
A
A
A
A
A/B
A/B
A
A
A
A
A
A/B
A
A
A
A
A/B
A/B
A
B
A/B
B/C
A
Ce
A
A
A
A
A
A
A
A
A
A/B
A/B
A
A/B
A/B
B
A
B
fracturing
Specimen
number
ACHONDRITES
B
B
B
A
A/B
A
A
A
A/B
A
A
B
A/B
A
A/B
A/B
B
A
B/C
B
A/B
A
C
A
A
A
A
B
A
B
A/B
B
B
B
A
A
A
A
A
A
A
B
A/B
A
A/B
A
A
A
B
B
B
EET83212
EET83227
EET83228
EET83229
EET83231
EET83232
EET83234
EET83235
EET83251
EET83283
ALHA81313
ALH85001
EET83236
LEW853OO
LEW85302
LEW85303
LEW85305
LEW85353
LEW86001
RKPA80204
ALHA81001
ALHA81OO9
LEW86O03
TIL82403
LEW86002
PCA82501
PCA82502
RKPA80224
ALHA78006
EETA79006
EET82600
EET83376
LEW85313
LEW85441
ALHA81OO5
ALHA77OO5
EETA79001
ALHA77257
ALHA78019
ALHA78262
ALHA81101
ALH82106
ALH82130
ALH83014
ALH84136
EET83225
EET83309
LEW85328
LEW85440
LEW86216
META78OO8
PCA82506
RKPA80239
Weight
(g)
402
1973
1206
313
66
211
181
255
261
57
0.5
212
6
210
115
408
41
25
291
15
53
229
2
50
33
54
890
8
8
716
247
79
191
11
31
483
7942
1996
30
26
119
35
45
1
84
44
61
107
44
6
125
5316
6
Class
and
type
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu (polymict)
Eu
Eu
Eu
Eu
Eu
Eu
Eu
Eu
Eu
Eu
Eu (polymict?)
Eu (polymict?)
Eu (brecciated)
Eu (brecciated)
Eu (unbrecciated)
Eu (unbrecciated)
Eu (unbrecciated)
Eu (unbrecciated)
Ho
Ho
Ho
Ho
Ho
Ho
Lunar
Sh
Sh
Ur
Ur
Ur
Ur
Ur
Ur
Ur
Ur
Ur
Ur
Ur
Ur
Ur
Ur
Ur
Ur
Degree of
weathering
B
B
B
B
B
B
B
B
B
B
A/B
B
A/B
A/B
A/B
A
B
Be
A
Ae
A
B
A
A/B
A
A
A/B
A
B
Ae
A/B
B
B
A/B
A
Ae
Ae
B/C
B/C
A/B
B
B
B
B
B/C
C
B/C
B
C
B
A/Be
B
fracturing
B
B
B
B
A/C
A/B
B
B
A/B
B
A/B
A
A
A/B
A
A
A/B
A
A
B
A
A
A
A
A
A
A
A
B
B
A/B
B
A/B
A
A
A
B
C
A
B
A
A
A
A/B
B
B
A
A/B
A
B
A
B
NUMBER 30 115
TABLE B.?Continued.
Specimennumber
LEW86211
LEW86498
EET83245
EET83390
DRPA78OO1
DRPA78002
DRPA78003
DRPA78004
DRPA78005
DRPA78006
DRPA78007
DRPA78OO8
DRPA78009
ALHA78100
ALHA81O13
EET83333
LEW86540
ALHA77255
ALHA80104
Weight
(g)
163
134
59
15
15200
7188
144
134
18600
389
11800
59400
138100
85
Mill
189
21
765
882
Class
and
type
Anomalous
(Ungrouped)
Anomalous
(Ungrouped)
IIAB (anom)
I IE (anom)
IIB
IIB
IIB
IIB
IIB
IIB
IIB
IIB
IIB
IIA
IIA
IAB
IIICD
Ataxite
(Ungrouped)
Ataxite
(Ungrouped)
Degree of
weathering fracturing
Specimen
number
IRONS
e
e
e
EET83230
ILD83500
ALHA81014
LEW85369
ALHA78252
ALHA76002
ALHA77250
ALHA77263
ALHA77283
ALHA77289
ALHA77290
PGPA77006
RKPA80226
ALH84165
GRO85201
EET84300
ALH84233
LEW86220
Weight
(g)
530
2523
188
6
2789
1510
10555
1669
10510
2186
3784
19068
160
95
1401
72
14
25
Class Degree of
j
type weathering fracturing
Ataxite
(Ungrouped)
Ataxite e
(Ungrouped)
Ungrouped
Ungrouped
IVA
IA
IA
IA
IA
IA
IA
IA
IA
IIIAB
IIIAB
IAB
(silicate incl.)
Ungrouped e
(silicate incl.)
IAB
(silicate incl.)
TABLE B.?Continued.
Specimen
number
ALHA77219
ALHA81059
ALHA81098
LEW86210
QUE86900
Weight
(g)
637
540
71
9
1532
Class
and
type
M
M
M
M
M
Degree of
weathering fracturing
B
C
C
C
C
Specimen
number
STONY-IRONS
B
B/C
B/C
A
A
RKPA79015
RKPA80229
RKPA80246
RKPA80258
RKPA80263
Weight
(g)
10022
14
6
4
17
Class
and
type
M
M
M
M
M
Degree of
weathering fracturing
A/B
C
C
B/C
C
A
B/C
C
B
B
116 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
TABLE C?ANSMET meteorite subtotals through 1986.
Class
and
type
CHONDRITE subtotals:
C2
C3
C3O
C3V
C4
Chon. (unique)
E3
E4
E5
E6
H3
H4
H4,5
H4,6
H5
H5,6
H6
H? Acapulco-like
L3
L3,4
L4
L5
L6
LL3
LL4
LL5
LL6
LL7?
TOTAL
ACHONDRITE subtotals:
A
An
Au
Di
Di/M
Eu
Ho
Lunar
Sh
Ur
TOTAL
IRON subtotals:
Irons
STONY-IRON subtotals:
Mesosiderites
Number
62
1
6
7
6
3
1
17
1
3
13
132
1
1
932
1
355
3
133
1
47
74
472
10
3
11
79
1
2376
4
1
21
7
1
45
6
1
2
16
104
37
10
Class
weight
(g)
6391
181
2379
801
592
140
39
301
20
823
595
84989
16000
314
213553
31
51543
23
19896
31
9497
26108
635221
4159
8
561
7347
8
1081551
113
7
3888
5542
2
12965
1252
31
8425
8045
40270
328080
12852
TOTALS 2527 1462753