SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES • NUMBER 24

Catalog of Meteorites

from Victoria Land,

Antarctica, 1978-1980

Ursula B. Marvin

and Brian Mason

EDITORS

ISSUED

JUL291982

SMITHSONIAN PUBLICATIONS

SMITHSONIAN INSTITUTION PRESS

City of Washington

1982
ABSTRAC T

Marvin, Ursula B., and Brian Mason, editors. Catalog of Meteorites from

Victoria Land, Antarctica, 1978-1980. Smithsonian Contributions to the Earth

Sciences, number 24, 97 pages, frontispiece, 41 figures, 13 tables, 1982.—This

is the second catalog of meteorite specimens collected on expeditions to

Victoria Land led by William A. Cassidy of the University of Pittsburgh. The

first {Catalog of Antarctic Meteorites, 1977-1978, U. B. Marvin and B. Mason,

editors, 1980) presented the results of the 1976-1977 and 1977-1978 field

seasons and described the collection and curation procedures that were

adopted under a three-agency agreement between the National Science

Foundation, the National Aeronautics and Space Administration, and the

Smithsonian Institution for the purpose of protecting the meteorites from

terrestrial contamination and allocating them for research. This catalog

reports the results of the subsequent two seasons: 309 specimens were collected

in 1978-1979, and 73 in 1979-1980. Classifications are given for all specimens

weighing more than about 100 grams and also for some smaller pieces from

each of the four field seasons. The catalog describes the field camps, the

geodetic measurements of ice motion and ablation at the Allan Hills site, and

the search for new concentrations. Current information about the character of

the collections and new types of meteorites represented in them is outlined in

brief articles describing Antarctic achondrites, carbonaceous chondrites and

irons, and meteorite weathering and terrestrial residence times on the polar

icecap. There is a bibliography of major articles on Antarctic meteorites. An

Appendix lists all of the Victoria Land specimens classified as of December

1980, by 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: Aerial view of Ulawan

Volcano, New Britain.

Library of Congress Cataloging in Publication Data

Main entry under title:

Catalog of meteorites from Victoria Land, Antarctica, 1978-1980.

(Smithsonian contributions to the earth sciences ; no. 24)

Bibliography: p.

Includes bibliographies.

Contents: The field season in Victoria Land, 1978-1979 / by Ursula B. Marvin — The traverse

to Reckling Peak, 1979-1980 / by William A. Cassidy and L. A. Rancitelli — The Allan

Hills Icefield and its relationship to meteorite concentration / by John O. Annexstad —

[etc.]

Supt. of Docs, no.: SI 1.26:24

1. Meteorites—Antarctic regions—Catalogs. 2. Meteorites—Antarctic regions—Addresses,

essays, lectures. I. Marvin, Ursula B. II. Mason, Brian Harold, 1917- . III. Series.

QE1.S227 no. 24. [QB755] 550s [523.5'1'09989] 81-607125 AACR2
Contents

Page

Editors' Introduction, by Ursula B. Marvin and Brian Mason 1

The Field Season in Victoria Land, 1978-1979, by Ursula B. Marvin. . 3

The Traverse to Reckling Peak, 1979-1980, by W.A. Cassidy and L.A.

Rancitelli 9

The Allan Hills Icefield and Its Relationship to Meteorite Concentration, by John O. Annexstad 12

Descriptions of Stony Meteorites, by Roberta Score, Trude V.V. King,

Carol M. Schwarz, Arch M. Reid, and Brian Mason 19

Descriptions of Iron Meteorites, by Roy S. Clarke, Jr 49

Overview of Antarctic Irons, by Roy S. Clarke, Jr 57

Overview of Antarctic Achondrites, by Arch M. Reid 59

Overview of Antarctic Carbonaceous Chondrites, by Carleton B.

Moore 65

Weathering Effects in Antarctic Meteorites, by Michael E. Lipschutz. . 67

Aluminum-26: Survey of Victoria Land Meteorites, by J.C. Evans, J.H.

Reeves, and L.A. Rancitelli 70

Bibliography of Antarctic Meteorites, by Karen Motylewski 75

Appendix: Tables of Victoria Land Meteorites 85

Literature Cited 95

in
FRONTISPIECE.—The midnight sun of 6 January 1979 illuminates the Allan Hills campsite, with

snow crystals streaming northward before the polar wind.
Catalog of Meteorites

from Victoria Land,

Antarctica 1978-1980

Editors' Introduction

Ursula B. Marvin and Brian Mason

The United States has sent yearly meteorite

collecting expeditions, under the leadership of

William A. Cassidy of the University of Pittsburgh, to Victoria Land, Antarctica, since the

austral summer of 1976. This catalog describes

those specimens weighing more than 100 grams

that were collected during the expeditions of

1978-1979 and 1979-1980. In addition, it describes some of the cherry-sized meteorites collected in these and other years. Descriptions of

the larger specimens from the 1976-1977 and

1977-1978 expeditions are presented in the Catalog of Antarctic Meteorites, 1977-1978 (Marvin

and Mason, 1980). That earlier catalog also provides descriptions of field areas, collecting procedures, and curation procedures.

Current research results show that the Antarctic specimens include mineralogical and textural

varieties of meteorites that are new to the world

collections. In order to make this catalog more

informative we include brief reviews of the range

of compositions observed among the achondrites,

carbonaceous chondrites, and irons, and progress

Ursula B. Marvin, Smithsonian Astrophysical Observatory, 60 Garden

Street, Cambridge, Massachusetts 02138. Brian Mason, Department

of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, D.C. 20560.

reports on topics such as geodetic measurements

of ice motion and ablation at the Allan Hills site,

meteorite weathering under polar conditions, and

aluminum-26 determinations of terrestrial residence times.

The field parties collected 11 meteorite specimens the first year (1976-1977), 300 specimens in

1977-1978, 309 specimens in 1978-1979, and 73

in 1979-1980 — a season when most of the effort

was devoted to measuring ice motion and searching for new meteorite concentrations. Table 1

shows the distribution of meteorite types found

in the latter two seasons. All of the Victoria Land

specimens that were classified as of December

1980 are listed in the three-part appendix. Appendix Table A lists specimens for each locality

by consecutive numbers; Appendix Table B lists

specimens consecutively by meteorite class; and

Appendix Table C lists the paired meteorites that

have been identified according to our current,

but far from complete, knowledge of them.

The final entry in the catalog is a bibliography

of the literature on Antarctic meteorites. Articles

containing substantive data (analytical information, petrographic descriptions, comparisons with

other meteorites, etc.) for Antarctic meteorites

have been included. In general, brief abstracts of

1
SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

TABLE 1.—Meteorite specimens collected in 1978-1979 and 1979-1980

Type

Irons

Achondrites

Carbonaceous

chondrites

Chondrites

Totals

Irons

Achondrites

Chondrites

Totals

Allan

Hills

2

6

1

253

262

1

52

53

Darwin

Glacier

9

34

43

Elephant

Moraine

1978-1979

1979-1980

6

4

10

Reckling

Peak

4

4

1

9

10

Totals

11

6

1

291

309

1

7

65

73

information published elsewhere in more complete form have been excluded. No attempt has

been made to survey the literature in Japanese,

although some frequently referenced papers are

listed. We hope these additions will increase the

usefulness of the catalog.

During the past three years research on Antarctic specimens has burgeoned in laboratories

around the world. Th e procedures for collecting

the specimens and maintaining them at belowfreezing temperatures until they can be processed

at the curatorial facility at the Johnson Space

Center in Houston are governed by an interagency agreement between the National Science

Foundation, the Smithsonian Institution, and the

National Aeronautics and Space Administration

and are outlined in the previous catalog (Marvin

and Mason, 1980). Newly examined and classified specimens are described in the Antarctic Meteorite Newsletter, published periodically by 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 specimens

or thin sections for research should be addressed

to the Secretary, Antarctic Meteorite Working

Group, Lunar and Planetary Institute, 3303

NASA Road 1, Houston, Texas 77058. Sample

requests should detail sample numbers, desired

weights, and the type of studies planned.

The Antarctic Meteorite Working Group meets

twice yearly, usually in April and September.

Dates of meetings and deadlines for sample requests are published in the newsletter. Sample

requests are welcome from all qualified scientists.

Requests are considered on the basis of their

merit, without regard to whether a scientist is

currently funded for meteorite research. The allocation of Antarctic meteorite samples in no way

commits any funding agency to support the proposed research.

Libraries of polished thin sections have been

established in Washington, Houston, and Tokyo

for the use of visitors who wish to make optical

examinations. (Library thin sections are not available for loan.) To obtain meteorite samples from

the Japanese collections or to use the thin section

library in Tokyo, contact T. Nagata, Director, or

K. Yanai, Curator, at the National Institute of

Polar Research, 9-10, Kaga 1-chome, Itabushiku, Tokyo 173, Japan. Arrangements for using

the thin-section library at the Johnson Space

Center in Houston may be made by contacting

the Secretary of the Antarctic Meteorite Working

Group. To use the library at the National Museum of Natural History, Smithsonian Institution, Washington, DC 20560, contact Brian Mason, Curator.
The Field Season in Victoria Land, 1978-1979

Ursula B. Marvin

The 1978-1979 field season had three main

objectives: to search new areas near the head of

the Darwin Glacier for meteorite concentrations,

to lay out a geodetic network to measure ice

motion and ablation at the Allan Hills, and to

continue systematic collection of specimens in the

Allan Hills icefield.

This was the third and final year of the cooperative agreement by which scientists from the

United States and Japan, working out of McMurdo Station, collected meteorites together and

shared specimens equally. Led by William A.

Cassidy, of the University of Pittsburgh, the participants included John O. Annexstad, NASA

Johnson Space Center, Ursula B. Marvin, Smithsonian Astrophysical Observatory, Dean Clauter,

University of Pittsburgh, and Fumihiko Nishio,

Kazuyuki Shiraishi, and Minoru Funaki of the

National Institute for Polar Research in Tokyo.

Annexstad and Nishio set up camp at Allan

Hills on December 7 and remained there for 26

days (through more than one 4-day storm that

kept them tentbound) installing a 15-km triangulation chain across the meteorite concentration

field (see Annexstad, this issue). Without making

any special effort to search for them, Annexstad

and Nishio picked up nearly 100 meteorites along

the snowmobile paths from their camp to the

network stations.

Cassidy and Shiraishi began a careful search

by helicopter of the region around the head of the

Darwin Glacier (79°50'S, 158°00'E), where the

Ursula B. Marvin, Smithsonian Astrophysical Observatory, 60 Garden

Street, Cambridge, Massachusetts 02138.

National Science Foundation set up a camp to

support a number of field parties during that

season (Figure 1). A short time later Cassidy

transferred to the Allan Hills camp and Marvin

and Clauter joined Shiraishi at the Darwin

Camp. The sites examined in that area included

the Warren and Boomerang Ranges, Butcher,

Finger, and Turnstile Ridges, Haven Mountain,

and Westhaven, Bates, and Lonewolf Nunataks.

Most of these sites proved barren, but six meteorites, all moderately weathered and looking suspiciously like fragments from a single fall, were

collected near Bates Nunatak. The three largest,

BTNA78001, 78002, and 78004, were later classified as L6, L6, and LL6 chondrites, respectively

(see Appendix Table A).

Five specimens were found in the upland between the head of the Darwin Glacier and that of

the Hatherton Glacier. Twenty-three specimens,

most of them small and weathered to a chestnut

brown, were collected from ripple identations on

a rather steeply sloping, bare ice-surface near the

west end of the Darwin Mountains. Their similar

appearance and their distribution over an open

slope suggested that they represented a relatively

recent strewnfield from atmospheric break-up of

a single meteorite.

In mid-December a group of geologists from

the University of Waikato, New Zealand, led by

Michael Selby, discovered six iron meteorites on

the rocky slopes of Derrick Peak, a conical mountain visible on the northern skyline from Darwin

Camp (Figure 2). They radioed the news to Cassidy at Darwin Camp and he and Shiraishi spent

two days searching the slopes with the New Zea-
SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

Syowa Base

Darwin Camp

Purgatory Peak

Mt. Baldr

1 Allan Hills

Reckling Peak

Antarctica

KEY:

— Continental Boundary

""""• Ice Shelf Border

$==* Major Glaciers

• Meteorite Find

180

500 km

FIGURE 1.—Location maps of Antarctic meteorite finds: a, outline map of continent; b, areas

searched and location of finds in Victoria Land.

land team. A short time later, Shiraishi, Marvin,

and Clauter spent another day there. In all, nine

more specimens were collected, and, later, another specimen was donated by Peter King, a

New Zealand climber associated with the Darwin

Base support group.

The Derrick Peak irons range in weight from

about 130 grams to 138 kilograms (see Clarke,

herein: 54-55). The two largest ones were strikingly handsome specimens, very difficult to carry

from the steep mountainside to a waiting helicopter. All of these irons have a distinctive appearance, with large, elongate inclusions standing up

in relief on surfaces hollowed by deep regmaglypts or corrosion pits. This unusual textural

feature indicates that they belong to a single

shower, and the distribution of the specimens

high on an ice-free mountain side suggests they

fell at that site rather than having been transported. Preliminary metallurgical observations
NUMBER 24

Lonewolf Nunatak

Bates Nunatak

Haven Mt.

^Turnstile Ridge

\ ,v-~-Westhaven Nunatak

Hatherton Glacier

Darwin Camp

Tentacle Ridge

Darwin Glacier

Carlyon Glacier

Scot t Bas e

 KJcMurdo StatioVV Victoria Dry Valley

MocKay Glacier

Carapace Camp

Allan Hills

Camp

Mawson Glacier

/ Reckling Peak

Elephant

Nunatak
SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

FIGURE 2.—Meteorite hunter on boulder-strewn slope of Derrick Peak.

have confirmed the common parentage of the

individual specimens. The raised inclusions are

crystals of schreibersite.

The Darwin Camp was located on the upper

glacier amid superb mountain scenery. All facilities—bunkhouse, workroom, gallery, radio shack,

repair shop—were housed in demountable Jamesway huts. A cook served three meals each day

and, whenever the generators worked, there were

a shower, flush toilets, a washer and dryer for

laundry. Field parties came and went all season,

but there were always enough people in camp for

a volley-ball game at 5 o'clock in the afternoon.

The Darwin Camp lay about 320 km from

McMurdo Station. Personnel and equipment

were carried there by ski-equipped Hercules LC130 cargo planes. Three helicopters were kept at

Darwin to ferry parties in and out of the field.

One fully operational helicopter was always on

the ground for possible use in rescue missions.

All field parties gathered at Darwin Camp for

a festive Christmas dinner featuring roast turkey

and cranberry sauce, with a generous array of

other dishes. The celebration helped alleviate the

sense shared by many polar researchers of being

too far from home at holiday time.

Shortly before New Year's Day, Shiriashi, Marvin, and Clauter left Darwin Camp for McMurdo, and on 2 January they joined Cassidy at

Allan Hills. After a long and eventful season,

Annexstad and Nishio left Allan Hills on the

same helicopter that carried in the newcomers. In

contrast to Darwin, the Allan Hills Camp was a

traditional Antarctic do-it-yourself operation in

which the campers pitched their own Scott tents

and were expected to take turns cooking for the

party over a Coleman stove. Happily for everyone, after sampling the efforts of others, Shiraishi,

who was well supplied with frozen Japanese delicacies, voluntarily did more than his share of

the cooking.

Daily trips were made by snowmobile to search

for meteorites on the nearby expanse of blue ice,

in a moraine at the foot of the Allan Hills ice

monocline, or on the polar plateau above it. On

the bare ice a fairly high percentage of the rocks

present were meteorites. On the plateau, few rocks

were sighted but all were meteorites. One iron
NUMBER 24

FIGURE 3.—Communications hut and tent city at Darwin Glacier Camp, with Roadend

Nunatak in background.

meteorite was found part way up the slope to the

plateau. In the moraine, meteorites occurred

among cobbles and boulders of local ("trash")

rocks. The moraines of this area are not similar

to the lobate heaps of rubble and clay associated

with mountain glaciers; they are collections of

rocks, probably derived from a shallow subsurface

ridge, scattered over the ice and snow. Keen

observation is necessary to detect meteorites and

to distinguish some of them from wind-polished

dolerites, especially since our sterile collection

procedures forbid picking up specimens for close

examination. The wind scoops (Figure 4) that

form around the base of large boulders proved to

be good hunting ground for cherry-sized meterorites, which are small enough to skitter along the

ice until they fall into the hollows. Laboratory

studies of cherry-sized stones are revealing a high

proportion of unequilibrated chondrites containing newly discovered assemblages of graphite and

magnetite (Taylor et al., 1981).

Although some meteorites may be covered by

snow, only one has been discovered frozen beneath the surface of the bare ice. That one was

small, nearly flat, and had a bronzy luster suggestive of either an iron meteorite or a weathered

piece of dolerite. Still frozen in a block of ice, the

specimen was shipped to Houston where it proved

to be a hexahedrite, ALHA78100.

The total number of specimens collected at

Allan Hills in 1978-1979 was 262. The average

size was smaller than that of previous seasons. It

appears that, at any one site, the largest and most

conspicuous specimens will be collected the first

year. Thin drifts of snow may alternately conceal

and expose smaller ones. An example of this

occurred during an afternoon's search when one

member of the party discovered a small ureilite

within the moraine and marked the spot by building a cairn topped with a red flag. A short time

later, when the whole party came to view the

meteorite, no meteorite was seen. Presently the

specimen was found under a fresh mound of

wind-blown snow; the presence of the cairn had
SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

FIGURE 4.—Wind scoop around boulder in a moraine, ideal trap for cherry-sized meteorites

that skitter downwind along ice surface.

changed wind patterns enough to cover the meteorite within minutes.

Helicopter reconnaissance yielded five specimens from a patch of ice about 20 km west, and

upstream in the sense of ice motion, from the

Allan Hills concentration (Cassidy, 1979). The

previous year, 25 specimens, all apparently from

a single fall, had been found about midway between the two sites. The ice flowing toward Allan

Hills from the west may be carrying many meteorites, most of them covered with snow.

Early in the season, Cassidy flew to the Ellsworth Mountains to check that area. He concluded that the ice was moving too rapidly to

form any significant meteorite concentrations

there. He also made reconnaissance flights over

the Thiel Mountains, where one meteorite was

discovered in 1969 and patches of blue ice are

visible on satellite photographs. Cassidy feels that

area holds sufficient promise to justify future field

exploration.

During a geological traverse, Philip Kyle of

Ohio State University, found five meteorites on

a patch of ice a short distance west of Reckling

Peak. His discovery led to a snowmobile traverse

there in the 1979-1980 season (Cassidy and Rancitelli, this issue).

The meteorite types collected in the 1978-1979

and 1979-1980 field seasons are listed in Table 1.

Much more laboratory work will be necessary

before it will be possible to estimate the number

of falls that are represented among the Victoria

Land specimens.
The Traverse to Reckling Peak, 1979-1980

W.A. Cassidy and L.A. Rancitelli

Reckling Peak is located at 159°15'E, 76°16'S.

A blue ice patch extends west from Reckling Peak

for about 100 km. The effective limit for routine

travel by helicopter from McMurdo Station is

reached at Allan Hills, therefore to investigate

the Reckling Peak ice patch we travelled north

by snowmobile from our Allan Hills put-in site,

towing our supplies on Nansen sledges (Figure 5).

Other members of the group were J. O. Annexstad, NASA Johnson Space Center, and Lee

Benda, University of Washington.

We left Allan Hills on 5 January and made 24

km before camping about 4 km west of Battlements Nunatak (Figure 6). On this traverse we

skirted families of crevasses resulting from

changes in ice flow velocity about the Battlements

Nunatak barrier. The next two days were spent

at this site due to high winds and consequent low

visibility that made travel inadvisable. On 8 January the wind died, we broke camp, and made

32 km to a point where increasing size and frequency of crevassing made further progress difficult. We were approaching a change in elevation

where the ice surface descends fairly steeply to

become part of a well-defined convergence area

leading to the David Glacier. Crevassing here

results from the fact that at the crest of the slope

each unit of ice volume at the upper surface is

forced to travel a greater distance in the same

time than any similar unit below it, i.e., acceleration by change of direction.

Kyle's party had descended somewhere near

W.A. Cassidy, Department of Geology and Planetary Science, University of Pittsburgh, Pittsburgh, Pennsylvania 15260. L.A. Rancitelli, Battelle Memorial Institute, Columbus, Ohio 43201.

our location, and Annexstad and Benda soon

found several of his trail markers from the previous year. We camped, and the next day descended the slope with some care—we had to

make a detour at one point when the lead sledge

made a hole at the edge of a snow bridge. The

lower part of the slope was bare ice, and we used

snowmobiles in tandem, one in front pulling and

the other behind braking, to transfer each sledge

to the bottom. At the bottom, we were on the ice

patch within the area where Kyle's party had

picked up five meteorites. In a rising wind, we

proceeded to a clear, snow-covered spot in an

adjacent moraine and set up our camp. We were

located about 12 km west of Reckling Peak.

During a day and a half spent searching, we

recovered 13 meteorites (Figure la).

Travelling west along the northern edge of the

ice patch on January 12, we were off the bare ice

surface so we have no knowledge of whether or

not meteorites can be found along its entire

length. At a point about 65 km west of Reckling

Peak we reached a second large moraine which,

by a strange configuration of rock debris and ice

sculpting, appears on the aerial photos to have

the outline of an elephant. We refer to it as

Elephant Moraine. One day's searching around

Elephant Moraine netted 12 meteorite specimens

(Figure 7 b). On 14 January we recrossed the ice

field there, ascended the monocline, and headed

south again for a helicopter pickup near Allan

Hills.

In assessing the results of this part of the 1979—

1980 field effort, several interesting points

emerged. The Reckling Peak ice field, 100 km
10 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

FIGURE 5.—Snowmobiles pulling sledges across Reckling Peak icefield during traverse from

Allan Hills to Reckling Peak.

FIGURE 6.—Route of snowmobile traverse from Allan Hills to Reckling Peak and return via

Elephant Moraine.
NUMBER 24 11

a

1047

1001

1003

1007

1009

1002

apparent direction

of Ice Flow

Moraine Camp

500 m

1048

1180

1185

apparent

direction

I of

vlce Flowy

Elephant Moraine

Camp

FIGURE 7.—Positions of majority of specimens at two sites

relative to apparent direction of ice flow: a, Moraine Camp;

b, Elephant Moraine Camp.

long by several km wide, seems to be associated

with a bedrock barrier parallel to its long dimension over which ice spills in the same manner as

at the Allan Hills and parts of the Yamato Mountains. This produces a step-like ice surface configuration. Aside from Reckling Peak, no rocks crop

out along its entire length although morainal

deposits, suggesting the presence of bedrock near

the surface, are found at two points.

Meteorites have been concentrated in at least

two locations along this linear ice field. They are

associated with moraine deposits on the lower

level of the ice step, but apparently are not found

in such great numbers at Reckling Peak as at the

Allan Hills site. The Allan Hills outcrop penetrates the ice and forms an absolute barrier to

further ice flow downstream from the monocline.

There is no such barrier at the Reckling Peak ice

field. This may help explain the lower abundances of meteorites exposed at the latter site. We

may find also that meteorite concentrations have

a higher surface density when associated with

moraines than they do elsewhere along the length

of an ice field, because the bedrock barrier is

closer to the surface at those locations and the ice

may be flowing more slowly there. Further field

reconnaissance is necessary before commenting

further on this.

Our total recovery on the traverse was 26 specimens. An estimate of possible pairings suggests

that at most we recovered only 15 individual falls

at the two sites we examined. Of these 15, however, at least four (>25%) were relatively rare

types (i.e., one iron and three achondrites; one of

the achondrites is a shergottite). Inasmuch as the

majority of meteorites in any random collection

should be ordinary chondrites, one might project

higher total numbers in this area than we report

here. Alternatively, these two sites could be presenting samples that fell during some time frame

when the meteorite flux at the earth had a different average composition. In either case, the Reckling Peak icefield appears to be a promising site

for further work.

ACKNOWLEDGMENTS.—This field work was supported by grant NSF DPP 78100. Louis Rancitelli's efforts were supported in part under NASA

contract NAS-9-11712. John Amrexstad's expenses were supported in part by his organization,

NASA Johnson Space Center.
The Allan Hills Icefield and Its Relationship

to Meteorite Concentration

John 0. Annexstad

The United States Antarctic Search for Meteorites (ANSMET) has centered on the Allan Hills

icefield (76°45'S, 159°40'E) from 1976 through

1979. This area has yielded nearly 700 specimens

of varying sizes and types. The main advantage

of this icefield for meteorite search is its close

proximity to McMurdo Station (230 kilometers)

which makes it easily accessible by helicopter.

Figure 8 shows the Allan Hills in relation to

McMurdo Station on Ross Island. The icefield

extends from the west side of the Allan Hills on

to the polar plateau.

The Allan Hills icefield has been described by

Nishio and Annexstad (1979) as a limited icefield

that has large concentrations of meteorites. The

meteorites appear to be concentrated on the lower

limb of an ice monocline (Cassidy, 1978) with

other finds scattered throughout the field.

In an attempt to understand the mechanisms

of meteorite concentration, a triangulation chain

was established across the icefield during the

1978-1979 austral summer. This chain is composed of 20 stations, two of which are on bedrock,

and extends westward from the Allan Hills a

distance of 15 kilometers. Figure 9 shows the

triangulation chain and its relationship to the

meteorite concentrations.

Each station is marked by a bamboo or aluminum pole set into a 50-100 centimeter hole

drilled into the ice or firn (Figure 10). Wild T-2

John O. Annexstad, Curator's Office, Johnson Space Center, Houston,

Texas 77058.

theodolites were used to establish the positions of

each station and to measure their evaluations

relative to the datum points (Stations 1 and 2).

The datum points are located on bedrock at an

adopted elevation of 2054 meters (barometricaltimetry) with a base line length of 1546.26

meters.

A small strain net of four stations, about 650

meters per side, was installed 1 kilometer north

of station 11 during late December 1978. Weather

problems precluded an accurate survey of this net

at that time, but basic data were obtained for

ablation measurements.

The triangulation net was resurveyed and the

strain net was precisely located during December

1979. Values were measured for the rates of ablation, horizontal movement, and vertical emergence or submergence of the icefield. It should be

noted that the first resurvey was accomplished

after only one year because of the availability of

personnel. Since the accumulated data are only

one year old, they must of necessity be considered

preliminary. A final resurvey of the triangulation

net is planned for the 1984-1985 austral summer

season.

FIGURE 8.—Allan Hills in relation to McMurdo Station on

Ross Island; icefield with meteorite concentrations extends

from the Allan Hills westward onto polar plateau.

FIGURE 9.—Triangulation chain extending from Allan Hills,

where datum points at Stations 1 and 2 are located on

bedrock, westward across exposures of blue ice (dots =

meteorite finds).

12
NUMBER 24 13

McMurdo Region, Antarctica

Seal* 1:1,000,000

Kilometers

Statute Miles

,~ \ N

x

SNOW COVERED v

\ \ \ EXPOSED ,V$> *?•
14

SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

b

FIGURE 10.—Setting up triangulation network station: a, drilling ice with SIPRE auger; b,

implanting bamboo flagpole to measured depth; c, locating survey point by theodolite.
NUMBER 24 15

TABLE 2.—Allan Hills triangulation network, preliminary survey data

Station

number

1

2

3

4

5

6

7

8

9

10

11

12

13

14

15

16

17

18

19

20

A

B

C

D

Elevation

2054.00

1909.86

1945.69

1955.71

1952.81

1954.14

1951.79

1946.67

1949.42

1945.19

1944.51

2030.50

2008.37

2014.37

2046.54

2022.05

2075.30

2067.58

2075.06

2070.81

NA

NA

NA

NA

Ablation

(cm/yr)

0

0

-2.3

-2.3

-1.1

-1.6

-2.5

-3.7

-4.2

-6.5

-5.6

-4.5

-5.6

-7.0

-5.7

-4.2

-5.1

-4.5

-3.1

-1.8

-6.4

-6.2

-6.0

-5.0

Emergence (+) or

submergence (—)

velocity (cm/yr)

0

0

-0.6

-0.6

-0.8

+ 1.9

-1.2

+ 1.4

+4.6

+6.7

+ 7.1

-1. 7

+6.5

+0.8

-2.7

-1.2

-1.0

-1.0

-3.5

-2.5

NA

NA

NA

NA

Horizontal

velocity (cm/yr)

0

0

7

6

10

20

17

50

30

80

100

123

129

121

140

182

202

237

234

251

NA

NA

NA

NA

Type

surface

Rock

Rock

Firn

Firn

Firn

Firn

Firn

Firn

Ice

Ice

Ice

Ice

Ice

Ice

Ice

Ice

Ice

Ice

Firn

Firn

Ice

Ice

Ice

Ice

Table 2 (Annexstad and Nishio, 1980) shows a

listing of each station along with its elevation,

ablation rate, vertical velocity, horizontal velocity, and type of surface. Because the small 4-

station strain net (Stations A,B,C,D) was not

precisely located until December 1979, only the

rate of ablation for the first year could be included.

The icefield gradually increases in altitude

from those stations located near the Allan Hills

to the westernmost region at Station 20. Stations

I and 2 are located on bedrock with Station 1 on

a promontory overlooking the icefield. The field

exhibits a steplike topography between Stations

I1 and 12 where the altitude increases 85 meters

in less than a kilometer. The main area of meteorite concentration appears to be in the region of

those stations (10 and 11) located on the lower

part of the step.

Using Stations 10 and 11 as a guide in respect

to the meteorite concentration mechanism, it can

be seen that the rate of ablation is fairly constant

at —6.5 and —5.6 cm per year respectively. This

value compares closely with the rate of ablation

measured by Naruse (1978) in the productive

meteorite icefield near the Yamato Mountains. If

all the stations are considered, (see Figure 11), the

rate of ablation ranges from a low of 1.1 cm per

year at Station 5 to a high of 7.0 cm per year at

Station 14. The average rate of ablation on the

ice surface alone is 5.7 cm per year (Figure 12)

while that of the firn surface is less: 2.7 cm per

year. The higher rate of ablation must be due to

the more rapid sublimation of the ice surface once

it is exposed. It is interesting to note, however,

that the ice or firn is wearing away gradually at

all 22 stations.

The velocity of emergence (+) or submergence
16 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

JUUL ICE CLIFF

• STATION

BARE ICE AREA

FIGURE 11.—Rates of ablation measured (cm) after one year at Allan Hills icefield (after Nishio and Annexstad, 1980).

FIGURE 12.—Ablation lowered surface at Station 14 about 7 cm between 1978 and 1979 field

seasons.
NUMBER 24 17

(—) is not so clear as the value of ablation. Nishio

and Annexstad (1980) report that the relative

error in these measurements can be as high as

100% at some stations. The authors note that

these errors are the result of small velocity values

after only one year that cannot be measured

accurately within the tolerances of the instruments. It is instructional, however, to look at the

values in the vicinity of Stations 10 and 11. In

this region of the highest meteorite concentration

it appears that the emergent velocity and the

ablation rates nearly balance. It is possible that

a steady state condition does exist in this part of

the Allan Hills icefield.

The horizontal velocity gradually increases

from a low of 6 cm per year at Station 4 to 251

cm per year at Station 21. Figure 13 shows a

schematic representation of the horizontal ice

flow by both vector direction and magnitude.

The vector direction gradually shifts from NE at

the westernmost station to nearly E as the Allan

Hills are approached. The change in magnitude

as the ice nears the hills indicates that the icefield

is slowing down toward stagnation.

Although the Allan Hills icefield has yielded

over 700 meteorite fragments, it still is a limited

area of concentration. The direction of the horizontal movement vectors at the westernmost staALLAN HILLS TRIANGULATION NETWORK

TRUE NORTH

MAGNETIC NORTH

HORIZONTAL MOVEMENT IN METERS

0 1 2 3 4

FIGURE 13.—Vector directions and magnitudes of ice flow across triangulation chain.

5 KM
18 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

tions indicate that the flow of the icecap is generally NE in that vicinity. This implies that most

of the ice flows into the large David Glacier

(Drewy, 1980) that is north of the Allan Hills.

Therefore, the majority of meteorites collected by

the icecap are probably deposited by the large

outlet glaciers that drain extensive sections of the

eastern Antarctic icesheet. This might help to

explain why the region around the dry valleys,

where the glaciers are small and have correspondly small catchment areas, produce few meteorites. The Allan Hills area appears to be on

the fringe of the major flow into the David Glacier

with its correspondingly large catchment area. It

is predicted that other blue ice fields that intercept large flow areas have the potential for producing many meteorites.
Descriptions of Stony Meteorites

Roberta Score, Trude V. V. King, Carol M. Schwarz,

Arch M. Reid, and Brian Mason

This section provides descriptions of the individual specimens, arranged by class. Within the

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 Newsletter, with additional information as

available. The letter-number designation for each

meteorite concurs with guidelines recommended

by the Committee on Nomenclature of the Meteoritical Society; it carries the following information: ALH (Allan Hills); A78 (Expedition A,

1978); XXX (digits indicating the number of the

specimen). The original weight of the specimen is

given to the nearest gram (nearest 0.1 gram for

specimens weighing less than 100 grams).

This section comprises material on all characterized meteorites collected during the 1978-1979

and 1979-1980 field seasons, together with descriptions of some meteorites collected during the

1977-1978 field season and not included in the

previous catalog (King et al., 1980). Specimens

weighing less than 100 grams are listed without

descriptions, unless they show distinctive features.

Roberta Score, Trude V. V. King, and Carol M. Schwarz, NorthropHouston, Johnson Space Center, Houston, Texas 77058. Arch M.

Reid, Geology Department, University of Cape Town, Rondebosch,

South Africa. Brian Mason, Department of Mineral Sciences, National

Museum of Natural History, Smithsonian Institution, Washington,

DC. 20560.

Chondrites

CLASS C2

FIGURE 14

ALHA78261 (5.1 g).—This triangular stone (2.5

X 1.5 X 1.0 cm) is totally covered with thin, dull

black, polygonally fractured fusion crust, except

along the edges where the fusion crust has

abraded away. The matrix revealed in these areas

is greenish black and has small (<1 mm),

rounded, and irregular white clasts throughout.

Small voids, as much as 1 mm in diameter, are

present on two surfaces. Chipping the specimen

during processing revealed abundant rounded

and irregular inclusions in the meteorite.

The section shows numerous tiny grains (up to

0.1 mm) and irregular aggregates (up to 0.3 mm)

of olivine and polysynthetically twinned clinopyroxene, and a few small chondrules, in a translucent isotropic olive-brown matrix. The section

contains very little troilite as minute scattered

grains, and a little nickel-iron as inclusions in the

chondrules. Porous fusion crust, up to 2.5 mm

thick, rims part of the section. Microprobe analyses show that both olivine and pyroxene have

variable composition. Olivine ranges from Fao to

Faso, with an average of Fa6; it has a notable

chromium content, Cr2O3 ranging from 0.3-0.6

weight percent. Pyroxene is generally close to

clinoenstatite in composition, ranging from Fsi to

Fss, with an average of FS7. This meteorite shows

19
20 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

FIGURE 14.—ALHA78261, C2 chondrite: a, Remnants of fusion crust (lighter gray) present; b,

photomicrograph of thin section (area of field is 3 X 2 mm); irregular grains and rare

chondrules, mainly of olivine (white to light gray) in translucent to opaque matrix (dark gray

to black).

a close similarity to ALHA77306, and is tentatively paired with it.

CLASS H3

FIGURE 15

ALHA78084 (14280 g).—This is a complete

stone, covered with splotchy brown and black

fusion crust. Several large fractures penetrate the

interior. A thin white deposit was evident along

some of these cracks after the meteorite was dried.

Many light-colored, rounded, and irregular inclusions are apparent on the cut faces, some as large

as 4 mm in diameter. Metal is visible, though

most of the metal grains have oxidation halos

around them, giving the cut faces a marbled look

of small fresh areas and large oxidized areas.

The section shows a close-packed aggregate of

chondrules, 0.3-1.2 mm in diameter, and a few

angular enclaves (some are chondrule fragments)

in a minor amount of fine-grained matrix. A wide

variety of chondrules is present, the commonest

being porphyritic olivine and olivine-pyroxene

with interstitial glass; some of the glass is brown

and transparent, but much of it is turbid and

partly devitrified. The pyroxene is polysynthetically twinned clinobronzite. The matrix contains

a considerable amount of fine-grained nickel-iron

and a lesser amount of troilite. Weathering is

extensive, with veins and patches of brown limonite throughout the section. Microprobe analyses

show olivine of rather uniform composition, averaging Fais, and pyroxene of variable composition, Fsg-24, average Fsi3. The mean composition

of the olivine and the amount of nickel-iron indicate H group and the meteorite is tentatively

classified as an H3 chondrite.

CLASS L3

FIGURES 16, 17

ALHA78038 (363 g).—This angular specimen

is approximately 12 X 5 X 5 cm and appears

shiny and reddish brown due to weathering and

staining by iron oxidation. Several fractures penetrate deeply into the sample. One small remnant

patch of shiny black fusion crust remains on the

B surface. During processing the sample fell apart

and revealed no unoxidized material.

The section shows a close-packed aggregate of

chondrules, 0.3-2.7 mm in diameter, and a few

angular enclaves (some are chondrule fragments)

in a minor amount of dark fine-grained matrix.

A wide variety of chondrule types are present, the
NUMBER 24 21

FIGURE 15.—ALHA78084, H3 chondrite: a, fusion crust

coats the stone, which shows several penetrating fractures; b,

photomicrograph of thin section (area of field is 3 X 2 mm);

closely packed aggregate of chondrules and angular enclaves

set in minor amount of dark matrix.

three commonest being granular olivine and olivine-pyroxene, porphyritic olivine, and finegrained pyroxene. Most of the pyroxene is polysynthetically twinned. Many of the chondrules

have dark rims. Troilite is present in minor

amounts in the matrix. Weathering is extensive.

The section is rimmed and veined with brown

limonite, and little nickel-iron remains. Microprobe analyses show olivine ranging from Fa4 to

Faig, with a mean of Fa22; pyroxene ranges from

Fs2 to Fsig, with mean of Fss, and CaO ranging

from 0.1 to 1.3 weight percent. The low content

of nickel-iron and troilite suggests L group, and

the meteorite is tentatively classified as L3 chondrite.

ALHA78188 (0.8 g).—The thin section shows

a close-packed aggregate of chondrules, 0.3-1.2

mm across, with a relatively small amount of

matrix. Porphyritic olivine chondrules contain

intergranular glass, some of which is transparent

brown but much is turbid from partial devitrification. Other chondrules consist of granular olivine and polysynthetically twinned low-Ca clinopyroxene. Many chondrules have dark rims

consisting largely of troilite. A little nickel-iron is

present. Weathering is extensive, with veins and

patches of brown limonite throughout the section.

Microprobe analyses show variable composition

for both olivine and pyroxene: olivine, Fai_34,

average Fais; pyroxene, FS5-29, average Fsn.

ALHA79001 (32.3 g).—The polished thin section shows a closely packed aggregate of chondrules, 0.2-2.0 mm in diameter, and irregular

crystalline aggregates, set in a small amount of

dark, fine-grained matrix that includes minor

subequal amounts of nickel-iron and troilite. A

considerable variety of chondrules is present, the

most common being granular olivine with or

without polysynthetically twinned clinopyroxene,

porphyritic olivine, and fine-grained pyroxene.

Some chondrules have intergranular, transparent, pale brown glass, in others the glass is turbid

and partly devitrified. Some weathering is indicated by the presence of a moderate amount of

brown limonite as veins and patches. Microprobe

analyses show a wide range in the composition of

olivine (Fa6-39) and pyroxene (FS2-31); the pyroxene is a low-calcium clinopyroxene (CaO = 0.2-

1.8%). This range of composition, together with

the presence of glass and twinned clinopyroxene,

indicates type 3, and the small amount of nickeliron suggests L group; the meteorite is therefore

tentatively classed as an L3 chondrite.

ALHA79003 (5.1 g).— The section is texturally

identical and the olivine and pyroxene show a
22 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

FIGURE 16.—ALHA78038, L3 chondrite: a, surface bounded by fractures and little or no fusion

crust remains; b, photomicrograph of thin section (area of field is 3 X 2 mm); round chondrules

and irregular enclaves in dark, fine-grained matrix.

FIGURE 17.—Photomicrographs of thin sections of L3 chondrites (area of fields is 3 X 2 mm):

a, ALHA79001; b, ALHA79003. (Closely packed aggregates of chondrules and angular enclaves

set in minor amount of dark matrix).

similar range of composition to these minerals in

ALHA79001; hence these two specimens are

probably pieces of a single meteorite.

ALHA79022 (31.4 g).—This stone (3.5 X 2.5

X 2 cm) is mostly covered with dull black fusion

crust. The areas devoid of fusion crust appear to

have been spalled off or preferentially plucked off

because they occur along ridges. Chipping the

stone exposed a relatively fresh, light gray interior, with many inclusions of various colors from

black to white. The largest inclusion is white and

7 mm in longest dimension. A narrow (<1 mm)

weathering rind is present.

The thin section shows well-developed chondritic structure, with chondrules ranging up to 1.8

mm in diameter; some have dark rims consisting

largely of troilite. The commonest chondrules are

granular and porphyritic olivine, with intergranular glass; some of the glass is brown and transparent, but most is turbid and partly devitrified.

The groundmass consists largely of fine-grained

olivine and pyroxene, with minor amounts of
NUMBER 24 23

nickel-iron and troilite; limonitic staining is present around the metal grains. Much of the pyroxene is polysynthetically twinned. Microprobe

analyses show olivine and pyroxene of variable

composition: olivine, Fai_28, average Fan; pyroxene, FS9-22, average Fsi6.

ALHA79045 (115 g).—This specimen (5.5 X

4.5 X 3 cm) has a small patch of weathered fusion

crust on one surface; an iridescent, reddish-brown

coating on other areas may be remnant fusion

crust. The rest of the stone is dull red-brown, but

its clastic nature is clearly visible. One clast is 4

mm across and yellow. The thin section shows a

close-packed aggregate of chondrules, 0.3-2.1 mm

across, and irregular clasts (some of them chondrule fragments), with a relatively small amount

of matrix material. Chondrule types include porphyritic and granular olivine and olivine-pyroxene, barred olivine., and fine-grained pyroxene.

Some chondrules have black, troilite-rich rims.

Intergranular glass in chondrules may be transparent and pale brown, but is usually turbid and

partly devitrified. Only a small amount of nickeliron is present. Most of the pyroxene shows

polysynthetic twinning. Brown limonitic staining

pervades the section. Microprobe analysis show

variable composition for both olivine and pyroxene: olivine, Fa2-38, average Fa23; pyroxene FS2-29,

average Fss.

RKPA79008 (72.9 g).—Black fusion crust covers about half of the stone. Areas devoid of fusion

crust are greenish black and show numerous

rounded and irregular clasts, up to 2 mm across,

and cream to black in color; two larger creamcolored clasts, 7 and 15 mm in largest dimension,

are also visible. The stone is extensively fractured.

The thin section shows abundant chondrules,

0.3-1.8 mm in diameter; a wide variety of types

is present, the three commonest being granular

olivine and olivine-pyroxene, barred olivine, and

fine-grained pyroxene. The granular chondrules

have intergranular glass, sometimes pale brown

and transparent, but commonly turbid and partly

devitrified. Irregular clasts, some of them chondrule fragments, are also present. Some of the

pyroxene in the chondrules is polysynthetically

twinned clinoenstatite or clinobronzite. The matrix is fine-grained olivine and pyroxene, with

minor subequal amounts of nickel-iron and troilite. Remnants of fusion crust, up to 0.3 mm thick,

are present along one edge. Minor weathering is

indicated by brown limonitic staining in association with the fusion crust and nickel-iron grains.

Microprobe analysis show that most of the olivine

has composition Fa23, but a range of composition

Fai_29 is present; pyroxene composition is variable, FS2-28, average Fsis.

CLASS H4

FIGURES 18, 19

ALHA77221 (229 g).—All surfaces of the meteorite, except the S surface, have remnant

patches of thin, dull black fusion crust. The exterior surfaces, devoid of fusion crust, are stained

by iron oxidation. Several clasts, approximately

I mm in diameter, are apparent on the S surface.

The specimen is fractured. Chipping revealed no

unweathered material in the interior of the sample.

ALHA77223 (207 g).—The T surface of this

specimen has patches of dull black fusion crust.

The remainder of the sample is stained reddish

brown by iron oxidation. The surfaces devoid of

fusion crust are fracture surfaces. Several cracks

penetrate the sample.

ALHA77225 (5878 g).—This stone (20 X 19 X

I1 cm) has no fusion crust and is uniformly

weathered and stained reddish brown; however,

some surfaces are more shiny than others. It is

extensively fractured. One brassy colored clast,

possibly a troilite nodule, is present on the T

surface. The B surface has what appear to be

slickensides, but because of the severe weathering

of the specimen it is impossible to determine this

unambiguously. No unweathered material is present on the exterior of the sample. When the

specimen was cleaved it fell into many pieces. No

unweathered material was exposed.

ALHA77226 (15323 g).—A small patch of dull

black fusion crust is present on the S surface. The
24 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

FIGURE 18.—H4 chondrites. (Note snow and ice on ALHA78134, present when specimen was

unpacked at Johnson Space Center).

W surface is concave and flow bands are present

in the T-B direction. The specimen is severely

fractured and crumbled into many pieces during

processing. Except for a few, small, light gray

areas, nearly all the material exposed is extensively stained by iron-oxides.

ALHA77232 (6494 g).—The stone (20 X 19 X

14 cm) is rounded, and only small patches of

remnant fusion crust remain on the exterior surface. It is severely weathered, uniformly stained

reddish brown, and fractured. When the sample

was sawed it crumbled into many pieces. No

fresh, unoxidized surfaces were exposed during

processing. White deposits developed on some

surfaces of the meteorite while it dried in the

nitrogen cabinet.

ALHA77286 (245 g).—The B surface and portions of the N surface are devoid of fusion crust.

The remaining surfaces have remnants of a thin

black fusion crust. The surfaces lacking fusion

crust are rough on a small scale. It appears that

many ~l-mm inclusions produce the roughness.

Chondrules and lithic clasts are present. No unweathered material was exposed when the stone

was sawed.

ALHA78053 (179 g).—This 8.0 X 6.0 X 2.5 cm

specimen has a small amount of thin, shiny black

fusion crust on the B face. The remainder of the
NUMBER 24 25

FIGURE 19.—Photomicrographs of thin sections of H4 chondrites (area of fields is 3 X 2 mm):

a, ALHA77221; b, ALHA77223; c, ALHA77232; d, ALHA78134. (Chondritic structure well

developed, but some chondrule margins tend to merge with granular matrix.)

sample is smooth, weathered, and stained reddish

brown by iron oxidation. Fractures are present on

the T and B surfaces. No unweathered material

was exposed during processing.

ALHA78O77 (330 g).—Thin, shiny black fusion

crust covers this 6.5 X 6.0 X 5.0 cm stone. In spots

the fusion crust is weathered away, revealing a

smooth, brownish-red surface. Several deep

cracks penetrate the sample. During processing

the sample cleaved along one of these fractures,

revealing no unoxidized material.

ALHA78134 (458 g).—The stone (7.0 X 5.0 X

7.5 cm) has dull black fusion crust on about 40%

of the surface. The remaining surfaces are weathered and stained by iron oxidation. On the S

surface the inclusions in the meteorite have a

higher relief then the surrounding matrix, probably as a result of preferential weathering. Inclusions (chondrules and lithic fragments) are visible

on the other fracture surfaces but have not experienced any preferential weathering. Several large

fractures penetrate the meteorite. When it was

divided during processing, 60% of the interior was

stained reddish brown. The remaining 40% is

light gray and contains many clasts 1 mm or less

in size.

ALHA79030 (108 g).—This 6 X 5 X 2.5 cm

stone is totally covered with thin, black fusion
26 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

crust that has a blistery texture on the B surface.

The T surface is concave and the B surface is flat.

Most of the interior is somewhat weathered, although areas of light gray material are present.

META78001 (624 g).—This stone (14.5 X 8 X

3 cm) is shaped like a boomerang and is entirely

covered with fusion crust. The fusion crust on the

B surface has an iridescent sheen, is much thinner

than the fusion crust on the remainder of the

sample, and has a well-defined area of weathering

1 cm from the edge of the sample. Remaining

surfaces have dull, brownish-black fusion crust.

Small regmaglypts are apparent on the T and N

surfaces and flow bands are present on the B

surface at the E and W ends. Small fractures exist

on the T and B surfaces, but they do not appear

to penetrate the stone. The interior material

ranges from being completely weathered and

iron-oxide stained to unweathered. The weathered portions are massive and are preferentially

located in the T half of the sample. The unweathered areas are light grayish green and contain

unoxidized metal grains.

RKPA78OO2 (8483 g).—This tabular-shaped

meteorite (17 X 13.5 X 17 cm) has two flat and

two semi-rounded surfaces with sharp ridges.

Black, polygonally fractured fusion crust, 0.5 mm

thick, covers the entire specimen except for areas

along the ridges where it has broken off. The

areas without fusion crust are greenish brown and

contain numerous inclusions. One fraction penetrates the interior of the meteorite. After drying

for several days in the nitrogen cabinet, minute

amounts of white deposit appeared along the

polygonal fractures. The cut face reveals a weathering rind 1-4 mm thick. Abundant metal blebs

are obvious, with most of the metal having oxidation halos around them.

RKPA78004 (166 g).—All but one surface is

covered with thin, dull black fusion crust, although portions of the fusion crust on another

surface appear to have been physically plucked

away. The portions devoid of fusion crust are

shiny reddish brown. Chipping this small stone

was impossible. Sawing revealed an interior with

many clasts discernible in the dark gray matrix.

Metallic grains are present. On the cut face it

appears that the inclusions in the meteorite have

a more dense population around the circumference, from the exterior margin to a depth of

approximately 1 cm.

H4 chondrites weighing less than 100 g are

ALHA78193, 13.3 g; 78196, 11.1 g; 78223, 6.4 g;

79023,68.1 g; 79035, 37.6 g.

The thin sections of the H4 chondrites resemble

each other closely. They all show well-developed

chondritic structure, chondrules 0.2-1.8 mm in

diameter. (ALHA77221 has some unusually large

chondrules, ranging up to 3 mm in diameter.) A

variety of chondrule types is seen, the four commonest being porphyritic to granular olivine,

barred olivine, fine-grained pyroxene, and granular olivine-pyroxene. The chondrules are set in

a fine-grained, granular matrix consisting largely

of olivine and pyroxene, with minor amounts of

nickel-iron and troilite (nickel-iron in greater

amount than troilite). Much of the pyroxene is

polysynthetically twinned clinobronzite. All these

meteorites except META78001 and RKPA78002

are considerably weathered, with brown limonitic

staining throughout the sections, and veins and

patches of limonite often associated with the

nickel-iron grains. The section of META78001

shows areas of blackening that appear to be due

to fine-grained troilite, possibly a shock effect.

Microprobe analyses (Appendix Table A) show

that the olivine in these meteorites has essentially

uniform composition (Fai7_ig); pyroxene may

have uniform composition (Fsis_i6), but in many

of these H4 chondrites shows some variability.

CLASS H5

FIGURES 20, 21

ALHA77259 (294 g).—This appears to be a

nearly complete stone, with only a small area of

the T surface not intact; this area is weathered

yellowish brown and shows traces of inclusions.

The rest of the surface shows remnant patches of

dull black fusion crust over a weathered surface

stained reddish brown with iron oxide. Regmaglypts are present on the E/S surface.
NUMBER 24 27

FIGURE 20.—H5 chondrites: ALHA781O2, rounded weathered stone with small patches of

remnant fusion crust; ALHA78107, angular stone bounded largely by fractures.

FIGURE 21.—Photomicrographs of thin sections of H5 chondrites (area of fields is 3 X 2 mm):

a, ALHA77259; b, ALHA781O7. (Chondritic structure easily discernible, but many chondrules

show partial integration with granular matrix.)

ALHA77268 (272 g).—This appears to be a

complete specimen with dull black fusion crust

on all surfaces. One small area with an iridescent

sheen is present on the T surface. A large fracture

penetrates the entire stone. No unweathered material was exposed during processing.

ALHA77274 (288 g).—A small patch of black

fusion crust remains on the B surface. The other

surfaces are devoid of fusion crust and are stained

reddish brown with iron oxides.

ALHA77287 (230 g).—Small patches of remnant fusion crust are preserved on the T and B

surfaces. The remaining surfaces are smooth and

weathered reddish brown. Small areas of the

surface have an iridescent sheen. No unweathered

material was exposed during processing.

ALHA78075 (280 g).—Thin, shiny fusion crust

covers most of this (7X6X 3 cm) specimen, with

the exception of portions of the T and W faces.

Areas devoid of fusion crust are smooth and
28 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

weathered to a shiny, dark reddish brown. Lightcolored inclusions and metal grains are apparent

in the dark matrix. Several fractures are present.

ALHA78085 (219 g).—Except for very thin,

black fusion crust on the B surface, this specimen

(6.5 X 4.5 X 3.5 cm) is bounded by fracture

surfaces that are weathered to a dark reddish

brown. A small clast (~2 mm), possibly troilite,

is present on the T surface. Processing revealed a

brecciated interior with a light-dark structure.

The light portion consists of numerous clasts in a

wide range of sizes, surrounded by dark material.

ALHA78102 (336 g).—Most of the surface of

this specimen (9X6X 6 cm) is weathered and

stained by iron oxidation and spotted with small

patches of black fusion crust. The specimen is

totally weathered except for the innermost material, which contains many small (up to 3 mm)

dark clasts.

ALHA78107 (198 g).—The B, S, and portions

of the E surfaces are covered with thin, black,

polygonally fractured fusion crust that is slightly

stained by iron oxides. Shallow regmaglypts are

present on the S surface. Other surfaces are fractured and are weathered and stained reddish

brown. No unweathered material was seen during

processing.

ALHA78108 (172 g).—Remnants of fusion

crust are present on the T and N surfaces, the

specimen (6.0 X 5.5 X 4.0 cm) being elsewhere

bounded by weathered, red-brown fracture surfaces. The specimen appears to be severely

shocked and brecciated. Many slickensided surfaces were exposed during processing. Two black

veins (~1 mm wide), with higher relief than the

surrounding material, are present in the interior.

ALHA7811O (160 g).—The stone (7.0 X 5.0 X

2.5 cm) is covered with thin, patchy black fusion

crust except on the B surface, which is stained

reddish brown with iron oxides and shows two

protruding, chondrules. Small, rounded, and irregular inclusions are visible through the fusion

crust. The matrix is reddish brown and shows

many inclusions and chondrules (up to 2 mm in

diameter), as well as metal grains.

ALHA78128 (154 g).—Fusion crust is absent,

this specimen being weathered and stained a dark

reddish brown. The B surface has some small,

nearly black spots, and in other areas, where the

weathering is less severe, chondrules (maximum

diameter 2 mm) can be recognized. The specimen

is extensively fractured.

ALHA79012 (191 g).—Thin patches of fusion

crust are present over all but the B surface of this

stone (9.0 X 5.5 X 3.5 cm). Fractures penetrate

the interior of the meteorite, which is extensively

weathered to a deep reddish brown. Field notes

state that this stone was found near ALHA79029,

another H5 chondrite.

ALHA79025 (1208 g).—Thin, black fusion

crust covers the S and B faces of this specimen

(10 X 13 X 7 cm). Otherwise it is bounded by

fractures that are weathered to a dark reddish

brown; remnants of fusion crust are present on

the E surface.

ALHA79026 (572 g).—This 9 X 6 X 5.5 cm

specimen is angular with flat surfaces covered

with a very thin, black to brown fusion crust. The

fusion crust has been lost from the T and a corner

of the N face, exposing a rough, irregular surface,

weathered reddish brown. A few small white

clasts are visible. The interior is friable and fractured. The matrix is gray with oxidation haloes

around metal grains.

ALHA79029 (505 g).—This 10 X 7 X 4.5 cm

stone has a very thin, patchy fusion crust on the

T, E, N, and S faces. Where the fusion crust has

been worn away, the surfaces are dark reddish

brown. Fusion crust and weathered surfaces are

smooth and shiny with an iridescent appearance.

The stone is extensively fractured.

EETA79OO7 (199 g).—When this meteorite was

received, it was numbered as two different samples; however, they fit together perfectly and are

therefore numbered as a single specimen. The

specimen (8 X 4.5 X 3.5 cm) is covered with black

fusion crust except for a few spalled areas. The

fracture surface between the two pieces has a 5-

mm thick weathering rind of reddish-brown color.

Many chondrules are visible. An area exposed by

chipping is relatively fresh and gray.

META78010 (233 g).—Smooth, black fusion
NUMBER 24 29

crust covers this specimen (8.5 X 5 X 4.5 cm).

Cleaving the stone into two approximately equal

parts revealed a light-dark structure. Dark, veinlike areas, which contain small light-colored clasts

(1-2 mm), surround large lighter-colored clasts

up to 1 cm across. Some areas of the stone are

weathered to a dark reddish brown.

,RKPA79004 (370 g).—When the Reckling

Peak meteorites were initially processed, it was

found that six stones appeared identical. Field

notes state that the six stones were found within

49 meters of each other. Examination of thin

sections confirm their identity, and they have

been combined as RKPA79004. All six stones

have brown-black fusion crust on at least one

surface. No stone was completely covered with

fusion crust, but two stones have fusion crust on

a fracture surface, indicating that the meteorite

broke up during flight in the upper atmosphere.

Fracture surfaces have all weathered to a reddish

brown and have uniformly pitted surfaces where

chondrules and inclusions have been plucked

away. Chondrules, <1 to 3 mm in diameter, are

visible on weathered surfaces.

H5 CHONDRITES WEIGHING LESS THAN 100

g.—ALHA78209, 12.1 g; 78221, 5.4 g; 78225, 4.5

g; 78227, 2.4 g; 78233, 1.2 g; 79004, 34.9 g; 79006,

40.9 g; 79008, 12.0 g; 79009, 75.6 g; 79010, 25.1

g; 79011, 14.0 g; 79013, 28.3 g; 79014, 10.8 g;

79015, 63.9 g; 79021, 29.4 g; 79031, 2.7 g; 79032,

2.6 g; 79036, 20.2 g; 79038, 49.6 g; 79040, 13.2 g;

79041, 20.1 g; 79042, 11.4 g; 79046, 89.7 g; 79047,

19.3 g; 79048, 36.7 g; 79050, 27.0 g; 79051, 24.0

g; 79053, 86.0 g; 79054, 36.0 g; RKPA79014, 77.7

gIn thin sections all the H5 chondrites show a

generally well-developed chondritic structure,

with a variety of chondrule types, the four commonest being barred olivine, granular and porphyritic olivine and olivine-pyroxene, and finegrained pyroxene. The groundmass is fine- to

medium-grained, and consists largely of olivine

and pyroxene, with minor amounts of nickel-iron

and troilite; small grains of sodic plagioclase can

sometimes be seen. The compositions of the olivine (Fai6-i8) and orthopyroxene (FS14-17) are essentially uniform within the individual specimens. ALHA79004 contains an enclave of granular polysynthetically twinned clinopyroxene

that appears to be of a lower petrographic type.

ALHA79008 contains a granular olivine-pyroxene enclave, 3 mm across, with the same olivine

and pyroxene compositions as the main mass of

the meteorite. ALHA79026 contains some unusually large chondrules, up to 3 mm across.

CLASS L5

FIGURE 22

EETA79009 (140 g).—This stone (6X5X 3

cm) was received as two different samples, consisting of three pieces. The three pieces fit perfectly together and are therefore numbered as a

single specimen. Dull black fusion crust covers

most of the surface. A weathering rind up to 4

mm thick is present. The interior is whitish gray

and shows numerous dark gray, fine-grained inclusions up to 14 mm in maximum dimension.

The thin section shows moderately abundant

chondrules, many of which are deformed or fragmented. The matrix consists of fine-grained olivine and pyroxene, with minor amounts of nickeliron and troilite; much of the nickel-iron and

troilite is finely dispersed through the silicates,

possibly a shock effect. Brown limonitic staining

pervades much of the section. Microprobe analyses give the following compositions: olivine, Fa24;

pyroxene, FS20.

RKPA79013 (11.0 g).—This small stone (2.5

X 1 X 1.5 cm) is completely covered with dull

brown to black fusion crust. Chipping revealed a

weathered interior with two gray, rounded inclusions, 2 mm in diameter. The thin section shows

well-developed chondritic structure, with chondrules ranging from 0.3 to 2.2 mm across. Fusion

crust, up to 0.5 mm thick, rims most of the

section. Brown limonitic staining is concentrated

around nickel-iron grains and below the fusion

crust. Microprobe analyses give the following

compositions: olivine, Fa23; pyroxene, FS20; accessory merrillite was identified with the microprobe.
30 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

FIGURE 22.—Photomicrographs of thin sections of L5 chondrite (area of fields is 3 X 2 mm): a,

EETA79009; b, RKPA79O13. (Chondrules discernible, but their margins tend to be poorly

defined and to merge with granular matrix.)

FIGURE 23.—ALHA78109, LL5 chondrite: a, fusion crust

(black) broken away over parts of stone and exposed light

gray interior; b, photomicrograph of thin section (area of

field is 3 X 2 mm); well-defined chondrules, some broken

and deformed, in fine-grained granular matrix.

CLASS LL5

FIGURE 23

ALHA78109 (233 g).—Approximately 75% of

this stone (7.0 X 5.5 X 3.5 cm) is covered with

dull black fusion crust. Areas without fusion crust

are light gray and show abundant dark gray

chondrules up to 2 mm in diameter. Chondrules

are easily removed from the matrix, many falling

out on handling. Troilite nodules, 3-10 mm

across, and gray clasts are also present. The thin

section shows prominent and well-defined chondrules, some broken and deformed. A variety of

types is present, the three commonest being granular olivine, barred olivine, and fine-grained pyroxene. The matrix is dominantly olivine with

lesser amounts of pyroxene, and a little nickeliron and troilite; plagioclase is present as very

small grains difficult to recognize. Some limonitic

staining occurs in association with the nickel-iron

grains. Microprobe analyses gave the following

compositions: olivine, Fa2s; orthopyroxene, FS23;

plagioclase, Ann.

CLASS H6

FIGURES 24, 25

ALHA77183 (288 g).—This is a well-rounded

specimen, except for a flat B surface. Fusion crust
NUMBER 24 31

FIGURE 24.—H6 chondrites: Fusion crusts coats most of surface of ALHA78076, whereas on

ALHA78115 much of fusion crust has been removed by weathering.

*'1-.

FIGURE 25.—Photomicrographs of thin sections of H6 chondrites (area of fields is 3 X 2 mm):

a, META78OO7; chondritic structure barely discernible, chondrules merging with granular

matrix; b, ALHA78O76 (reflected light); rounded intergrowth (possibly chondrule) of chromite

(white) and plagioclase (light gray) occupies center of field.

is absent, and all surfaces are stained a uniform

reddish brown. Small inclusions are visible on the

T surface. No unweathered material was seen

when the stone was cleaved.

ALHA78076 (275 g).—Thin, black fusion crust

covers most of the stone (8.0 X 5.0 X 4.5 cm).

Where the fusion crust is absent, the surface is

stained reddish brown with iron oxides and 1-2

mm clasts are visible. Polygonal fractures are

present on the T and N surfaces. Cleaved surfaces

shows clasts up to 3 mm across, in gray matrix.

Minor amounts of iron oxides are present around

metal grains.

ALHA78115 (847 g).—This is a smooth,

rounded stone with scattered fusion crust on the

B and E surfaces, and a very small amount on
32 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

the W surface. The fusion crust is black, thin, and

pitted. Where fusion crust is absent the surface is

weathered reddish brown. Clasts and chondrules,

as much as 9 mm across, are present. The interior,

exposed during processing, contains metal particles and is moderately weathered.

ALHA79002 (222 g).—A small, thin patch of

black fusion crust and remnant red-brown fusion

crust cover the stone (8 X 5 X 4.5 cm). Several

fractures penetrate the interior. No unweathered

material was exposed by chipping.

ALHA79016 (1146 g).—This stone (13 X 8 X

6.5 cm) is covered with smooth, black fusion crust,

except for small patches on the T and E surfaces;

these patches are weathered to a reddish brown

color. Shallow regmaglypts are present on several

faces. The S and B faces appear to have been

fracture surfaces that have been covered with

fusion crust. The interior has a yellowish color, is

friable, and shows metallic particles; no chondrules are visible.

META78006 (409 g).—This specimen is completely covered with fusion crust. Cleaving revealed that the interior is considerably stained

with iron oxides; unstained areas are light gray;

a few darker-colored inclusions are present.

META 78007 (174 g.)—Fusion crust, ranging

from dull black to iridescent red-brown, totally

covers this irregular-shaped meteorite. The interior of the stone is 75% weathered; the unweathered part appears to have many clasts, up to 5

mm across. This stone was magnetically oriented

in Antarctica and the orientation has been kept

throughout processing.

RKPA79003 (182 g).— This semi-rounded

stone (7 X 4.5 X 3.5 cm) is covered with black

fusion crust. Small areas where the crust has been

plucked off reveal a reddish-brown interior with

many inclusions.

H6 chondrites weighing less than 100 g:

ALHA78211, 11.4 g; 78213, 9.5 g; 78215, 6.3 g;

78229, 1.9 g; 78231, 1.8 g; 79005, 60.0 g; 79019,

12.1 g; 79020, 4.2g; 79024, 21.6 g; 79028, 16.2 g;

79034, 12.6 g; 79037, 14.8 g; 79049, 54.0 g; 79055,

15.2 g; RKPA79009, 54.6 g; 79012, 12.8 g.

In thin sections all the H6 chondrites show very

similar petrographic features. Chondrules are

sparse and poorly defined, tending to merge with

the granular groundmass, which consists mainly

of olivine and pyroxene, with minor amounts of

nickel-iron, troilite, and sodic plagioclase, and

accessory chromite. Compositions of the olivine

(Fan-19) and pyroxene (FS15-17) are uniform

within the individual specimens. The thin section

of ALHA78076 showed a rounded aggregate of

closely-packed chromite grains with interstitial

plagioclase, possibly a chondrule of unusual composition. A vein of nickel-iron up to 0.5 thick is

present in ALHA79016.

CLASS L6

Figures 26, 27

ALHA77180 (190 g).—This stone has remnant

fusion crust on three surfaces; other surfaces are

fractures and stained reddish brown with iron

oxides. Processing revealed a light gray, finegrained interior and one fine-grained inclusion

approximately 10 mm in diameter.

ALHA77292 (199 g).—This is an incomplete

stone. The T surface is less severely weathered

than the other surfaces; the N surface has remnants of dull black fusion crust. Surfaces devoid

of fusion crust are rough and stained reddish

brown with iron oxides. Fractured surfaces show

rounded and irregular inclusions.

ALHA78039 (299 g).—This specimen (8X 4

X 5 cm) is totally covered with black fusion crust

except for a 4.0 X 2.5 cm area that shows a light

gray interior. Cleaving the stone revealed a light

gray matrix with light gray clasts. A well-defined

weathering rind penetrates the stone to a depth

of 1-10 mm. Scattered areas of partly oxidized

metal are present throughout the meteorite.

ALHA78042 (214 g).—The T surface of this

5.5 X 4.0 X 5.0 cm specimen has a 4 X 3 cm area

of reddish-black fusion crust; the remaining surfaces are fractures that are weathered reddish

brown. The sawed specimen revealed a relatively

fresh interior with a light gray matrix and

rounded and irregular inclusions up to 1 mm in

diameter.

ALHA78043 (680 g).—This stone, 10.0 X 8.5

X 6.0 cm, is covered with black fusion crust, ~1
NUMBER 24 33

FIGURE 26.—L6 chondrites.

mm thick, that shows some weathering; the W

surface appears to be less weathered than the

other surfaces. A large chondrule is present on the

B surface. The T surface is a fracture with some

remnant fusion crust. During processing the stone

broke along fractures that were weathered and

stained with iron oxides. The matrix is yellowish

green and contains some small (<3 mm) clasts. A

few metallic flakes are present in the matrix.

ALHA78045 (396 g).—This tabular specimen,

(8.0 X 5.0 X 5.0 cm) is covered with blackish

brown fusion crust except for a 2.5 X 3.5 cm area

on the T/E surfaces that is very smooth and

highly polished. Three large fractures penetrate

the specimen. During processing the specimen

broke into two approximately equal pieces along

one of the fractures. The matrix is weathered to

a reddish yellow.

ALHA78048 (190 g).—This specimen is partly

covered with brown to black fusion crust. Where

fusion crust is absent, a light gray matrix with

some iron-oxide staining is seen. Shallow regmaglypts are present on all surfaces. When the stone

was cleaved a thin (1-2 mm) weathering rind was

exposed. The interior is light gray with darker

gray inclusions and shows some unoxidized metal

grains.

ALHA78050 (1045 g).—This 15 X 8 X 6 cm

specimen is an incomplete stone, being bounded

by fractures on the N, T, and B surfaces; these

surfaces are stained reddish brown with iron oxides. Inclusions are apparent on these surfaces,
34 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

FIGURE 27.—Photomicrographs of thin sections of L6 chondrites (area of fields is 3 X 2 mm in

a, b, c; 0.9 X 0.7 mm in d): a, ALHA78106; b, BTNA78002; c and d, RKPA78003. (Chondritic

structure barely discernible in these sections, chondrules almost completely integrated with

granular matrix; ALHA78106 has thick fusion crust (top of section); d, enlargement of c, with

shock vein containing ringwoodite and majorite (tentative determinations).)

and patches of remnant fusion crust, mottled

brown and black, remain on the B surface. Sawed

surfaces show metallic grains, some with oxidation halos, and small irregular inclusions.

ALHA78074 (200 g).—This is an incomplete

stone, with shiny fusion crust (1-2 mm thick) on

the B, W, and parts of the S, N, and E surfaces;

polygonal fractures are present on the B and N

surfaces. Fracture surfaces are rough, slightly

weathered, and stained with iron oxides. The

matrix is light gray, it includes darker gray clasts

and chondrules.

ALHA78078 (290 g).—This 6.0 X 4.5 X 8.0 cm

stone is covered with thin black fusion crust except at the corners. Processing revealed a light

gray matrix speckled with light and dark clasts

and metallic grains.

ALHA78103 (589 g).—This rounded specimen

(11 X 7X 4 cm) is weathered and stained with

iron oxides, except for a small patch of remnant

fusion crust on the E surface. The B surface,

which is least weathered, displays several chondrules, 3-5 mm in diameter. The stone broke

along fractures during processing, showing a

greenish-gray matrix with some metallic grains

and oxidation halos. A weathering rind, ~3 mm
NUMBER 24 35

thick, is present on the T surface.

ALHA78104 (672 g).—The W surface is partly

covered with black fusion crust, but the remainder of the surface is weathered and stained with

iron oxides. A large clast (~7 mm) is exposed on

the N surface, and a smaller (~3 mm) possibly

metallic clast on the T surface. A number of

smaller clasts that appear to be metallic are scattered over the surface. Processing revealed a light

gray matrix with metallic particles. Weathering

rind, ~5 mm thick, is present on some surfaces.

ALHA78105 (941 g).—The surface of this stone

(11X7X 6 cm) is rough and irregular on a mm

scale, apparently as a result of the weathering of

the fusion crust, of which small patches remain

on the B and N surfaces. The interior shows a

light to medium gray matrix with chondrules,

lithic clasts, and sparse metal grains.

ALHA78106 (464 g).— This semi-pyramidal

specimen appears to be completely unweathered

(a recent fall?). It is covered with a spotted, brown

to black, polygonally fractured fusion crust, ~1

mm thick. Shallow regmaglypts are present on all

surfaces. The interior shows a light gray matrix

with dark and light clasts up to 2 mm across.

ALHA78112 (2485 g).—This stone (14 X 13

X 13 cm) is covered with fusion crust, 0.5-1 mm

thick, on four surfaces; on one surface the fusion

crust has weathered to a brown color, on the

other surfaces it is black. The S surface is a

fracture, and 80% is weathered and stained with

iron oxides. Sawing the specimen revealed light

gray matrix with oxidation halos around most of

the metal grains; clasts up to 3 mm across are

present.

ALHA78114 (808 g).—The B surface of this

meteorite is planar and has small patches of dull

black fusion crust on a shiny reddish-brown background, which may possibly be severely weathered fusion crust. All other surfaces are covered

with dull black fusion crust except for small areas

on the S surface. Small regmaglypts are present

on this surface. Many shallow voids are present

on the exterior. The stone was cleaved along a

large crack, exposing mostly weathered material.

Unweathered material is light gray and flecked

with light and dark clasts (~1 mm).

ALHA78126 (606 g).—Thin black fusion crust,

weathering brown in some areas and polygonally

fractured on the B surface, covers this specimen

(12X8X 5 cm) except on the NE corner. Matrix

material exposed during processing is greenish

gray, with several darker veins penetrating it;

small metallic particles were also apparent in this

friable specimen.

ALHA78127 (194 g).—The stone is covered

with very thin shiny fusion crust on the T, B, N,

and W surfaces; remnants of fusion crust are

present on the S surface, and the E surface is a

fracture surface. Where fusion crust is absent, the

specimen is reddish brown. Processing showed

that nearly all of the specimen is severely weathered.

ALHA78130 (2733 g).—This meteorite (18 X

9 X 9 cm) is covered with a thin, dull black fusion

crust, except along the edges and a 4 X 4 cm area

on the W surface. There is preferential weathering

of the fusion crust around clasts. The stone is

covered with shallow regmaglypts and is extensively fractured. Processing revealed that about

70% of the interior is severely oxidized. The unweathered portion is light gray and speckled with

light and dark clasts, some up to 5 mm across.

Small veins of darker material, 20-30 mm long

and 3 mm wide, are present in the matrix.

ALHA78131 (268 g).—Thin, shiny black fusion crust covers the specimen except for most of

the T surface and portions of the B and N surfaces. Shallow regmaglypts are present on the S,

W, and T surfaces. Surfaces devoid of fusion crust

are weathered and stained with iron oxides; several light-colored clasts were noted on these surfaces. Processing exposed only a small amount of

unweathered material.

ALHA78251 (1312 g).—This specimen (12 X

7.5 X 10 cm) is completely devoid of fusion crust

and the surface is rough and irregular. The interior is fine-grained and greenish gray, and shows

metal grains surrounded by oxidation halos. Fractures are present with iron oxides along their

margins.

ALHA79007 (142 g).—Dull black fusion crust

covers 50% of this stone (6X4X 4 cm). Areas

devoid of fusion crust range from light gray to
36 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

yellowish brown in color; many clasts are visible,

one of which is 6 X 10 mm, greenish yellow, and

very fine-grained. The interior is relatively fresh;

with a thin weathering rind in some areas and a

small amount of oxidation around metal grains

in the light gray matrix.

ALHA79018 (120 g).—This stone (4.5 X 5 X

3.5 cm) is covered with thin, brown to black,

patchy, fusion crust on all but one surface; this

surface has a yellow to deep reddish-brown color

and shows several inclusions. The interior is

mainly weathered but has small areas of fresh

material. Several black veins are present (infilled

cracks ?), as are rounded inclusions up to 3 mm

in diameter.

ALHA79027 (133 g).—Dull black fusion crust

coats most of this stone (5.5 X 4.5 X 3 cm). A

fracture surface has patches of fusion crust, which

suggests that the stone broke during passage

through the atmosphere. Many inclusions are

visible, with the largest being 4 mm in greatest

dimension.

ALHA79033 (208 g).—All but the T surface of

this stone (7.5 X 6.5 X 3.5 cm) is covered with

dull brown to black fusion crust. The T surface is

a fracture that has weathered reddish brown; a

number of mm-sized inclusions were noted. Fresh

interior material is light gray with darker gray

inclusions; metal grains surrounded by oxidation

halos are present. A weathering rind 1-5 mm

thick is visible.

BTNA78001 (160 g).—The specimen is shaped

like a flat plate, 10 X 6 X 1 cm, and is covered

with black fusion crust except on the B and

portions of the W surface; the B surface is polished

and has a mottled, yellowish-red-brown appearance. Processing revealed a medium gray matrix

with inclusions (~1 mm). The specimen has a

prominent (1 mm) weathering rind.

BTNA78002 (4301 g).—This specimen consists

of two separately collected pieces that fit together.

The complete stone (20 X 12 X 14 cm) is almost

entirely covered with thin, dull brown fusion crust

(apparently weathered) that is dotted with black

fusion crust. An approximately 7 X 10 cm area

on the S surface appears to have been broken

away (this may be BTNA78001, which is petrologically identical to BTNA78002). Areas devoid

of fusion crust are light grayish green except

where flecked with iron oxides around metal

grains. The T surface shows flow bands in the EW direction, and regmaglypts are present on the

B surfaces.

EETA79003 (435 g).—This 7.5 X 6 X 5 cm

stone is covered with thin, shiny black fusion

crust that is pitted and weathered, leaving a

brown surface in some areas. The interior is gray

and very friable, with numerous oxidation halos

around metal grains.

EETA79010 (287 g).—The exterior of this

stone (8.5 X 6 X 4 cm) has weathered yellowbrown to red-brown. One small patch of black

fusion crust remains. The interior is whitish gray

with brown limonitic staining around nickel-iron

grains. A thin weathering rind was noted.

META78002 (542 g).—Thin, dull black fusion

crust is present on three surfaces of this pyramidal

specimen; the fusion crust is pitted, apparently

the result of preferential weathering of small inclusions. The T, W, and B surfaces are fractures

that are stained reddish brown. Many clasts, up

to 3 mm across, can be seen on the T and W

surfaces. Processing revealed a greenish-gray matrix containing metal grains, some of which have

oxidation halos.

META78003 (1726 g).—The E, T, and W

surfaces of this meteorite (15.0 X 7.5 X 8.0 cm)

are covered with thin, dull black fusion crust. The

other surfaces are fractures that are weathered to

a reddish color; light-colored inclusions are visible

on these surfaces. Processing revealed a greenishgray matrix with oxidation halos around metal

grains.

META78005 (172 g).—Three surfaces of this

stone (6.5 X 5.5 X 4.0 cm) are covered with dull

black polygonally fractured fusion crust. Surfaces

devoid of fusion crust are fractures, are weathered

to a reddish yellow, and contain many inclusions

with greater relief than the surrounding matrix.

Processing revealed a light gray matrix with small

clasts and non-oxidized metallic particles.

RKPA78001 (234 g).—Thin dull black fusion

crust covers two surfaces of this angular stone (9

X 5 X 4.5 cm). The other surfaces are fractures
NUMBER 24 37

that are stained reddish brown by iron oxidation.

Processing revealed only a small amount of grayish unweathered material. No inclusions were

seen.

RKPA78003 (1276 g).—This specimen was

found as two pieces, which fit together perfectly.

Most of it is covered with thin, dull black fusion

crust. Surfaces devoid of fusion crust have weathered to a deep reddish brown, as have the two

surfaces that fit together. The W butt end has a

clast, 10 mm across, that appears to be troilite.

Chipping revealed surfaces composed of very dark

gray and very light gray matrix material, possibly

the result of weathering processes.

RKPA79001 (3006 g).—Small patches of shiny

black fusion are present; the remaining surfaces

are fractured, rough, and yellowish brown. Chondrules can be distinguished; most are small, but

the largest one is 6 mm in diameter. Indentations

in the surface indicate chondrules may have been

plucked out. There is a vein of dark material, 1-

3 mm thick, on one surface, probably indicating

weathering along a fracture. A small amount of

white powdery deposit is present on the fusion

crust. The interior matrix is light gray to yellow,

with oxidation halos around metal grains; gray

and cream-colored chondrules, ~2 mm in diameter, are visible.

RKPA79002 (203 g).—Dull black fusion crust

partly covers three surfaces of this stone (8.5 X

5.5 X 3.5 cm). The B surface is highly polished in

areas of fusion crust. Clasts up to 3 mm are visible

on the surface and are identical to those seen in

RKPA79001. Surfaces devoid of fusion crust are

weathered from brownish yellow to reddish

brown. The interior is whitish gray with oxidation

halos around metal grains. A small weathering

rind was noted.

All the RKPA L6 meteorites are petrologically

identical, with maskelynite and shock veins containing majorite and ringwoodite; it is reasonable

to conclude that they are all pieces of a single

meteorite.

L6 chondrites weighing less than 100 g:

ALHA79043, 62.2 g; 79052, 22.6 g.

The L6 chondrites are all very similar in their

petrographic characters. Polished thin sections

show sparse, poorly defined chondrules that tend

to merge with the granular groundmass. Principal

minerals are olivine and orthopyroxene in subequal amounts, together with minor quantities of

plagioclase (or maskelynite), nickel-iron, troilite,

diopside, and accessory chromite and merrillite.

Microprobe analyses (Appendix Table 1) show

essentially uniform compositions for the principal

minerals: olivine, Fa23-25; orthopyroxene, Fsi9_2i;

plagioclase, Anio-12. The following meteorites

contain maskelynite: ALHA78039 (in part),

78048 (in part); 79018; 79043; 79052;

BTNA78001, 78002; RKPA78001, 78003, 79001,

79002. Ringwoodite and majorite were tentatively identified in shock veins in ALHA79018,

BTNA78OO1 and 78002, and RKPA78001,

78003, and 79002.

CLASS LL6

FIGURE 28

ALHA78153 (151 g).—Thick (1-2 mm), dull,

brownish-black fusion crust, with a blistery texture, covers the N, B, and parts of the E surface.

A weathering rind, up to 5 mm thick, is present

in some areas. Fracture surfaces are dark brown

in isolated areas, but the overall color is greenish

yellow. It appears that some large clasts have

been plucked from the surface. This stone shows

an unusual weathering pattern. Dark reddishbrown veins adjoin areas of yellowish material;

areas of less severely weathered gray matrix were

exposed during processing. In thin section chondritic structure is barely discernible, the meteorite

showing a rather uniform granular aggregate of

olivine and pyroxene, with minor amounts of

troilite and plagioclase, a little nickel-iron, and

accessory chromite. Limonitic staining is present

in association with the metal grains. Microprobe

analyses gave the following compositions: olivine,

Fa29; orthopyroxene, FS24; plagioclase, Ann.

BTNA78004 (1079 g).—This stone (12 X 7 X

7 cm) is covered with thin, dull black fusion crust

except on one fracture surface. Regmaglypts are

present on the N and S surfaces. The meteorite

appears to be composed of angular, light-colored

clasts surrounded by greenish-brown to gray in-
38 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

FIGURE 28.—BTNA78004, LL6 chondrite: a, fusion crust (black) coats part of surface; b,

fracture surface showing brecciated structure; c, sawn surface showing brecciated structure with

light and dark clasts; d, photomicrograph of thin section (area of field is 3 X 2 mm), showing

granular clasts bounded and penetrated by black glassy veinlets.

terstitial material. The clasts comprise approximately 70% of the surface area and have a wide

range in size; some are as much as 2.0 cm across.

A thin section shows a granular aggregate consisting mainly of olivine and pyroxene (average

grain size 0.1-0.2 mm), with minor amounts of

plagioclase, nickel-iron, troilite, and accessory

chromite. Chondritic structure is barely visible in

a few places, and the chondrules are somewhat

fragmented. Many of the silicate grains show

undulose extinction. The meteorite has a brecciated structure, and the breccia fragments are

outlined by an anastomosing network of black,

glassy veinlets that contain numerous minute

troilite globules. A small amount of limonite

staining is present around some of the nickel-iron

grains. Microprobe analyses show olivine (Fa3o)

and orthopyroxene (FS24) of essentially uniform

composition; plagioclase is somewhat variable in

composition, Ani3-An22, average Ani9. The black

glass is quite variable in composition, as follows

(range and average, in weight percent): SiO2

31.5-49.9, 40.4; A12O3 0-6.3, 2.8; FeO 17.5-40.9,

23.9; MgO 16.7-31.3, 27.3; CaO 0-3.3, 1.6; Na2O

0-2.4, 1.1; TiO2 0-0.15, 0.09; MnO 0.3-0.5, 0.4.

The meteorite shows to a high degree the brecciation characteristic of many LL chondrites.

Achondrites

EUCRITES

FIGURES 29, 30

Eucrites and howardites are pyroxene-plagioclase achondrites, but different authorities have
NUMBER 24 39

ALHA78040

FIGURE 29.—Eucrites; black glassy fusion crust coats most of specimens, except EETA79011;

note snow and ice still present on ALHA78132 when unpacked at Johnson Space Center.
40 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

FIGURE 30.—Photomicrographs of thin sections of eucrites (area of fields is 3 X 2 mm): a,

ALHA78132; b, ALHA78158; c, ALHA78165; d, ALHA79O17; e, EETA79005;/, EETA79011.

(Photomicrographs show typical brecciated structure of eucrites, with clasts of plagioclase

(white), pyroxene (light gray), and chromite (black) in fine-grained comminuted matrix of these

minerals; (c) has area showing ophitic intergrowth of plagioclase (white laths) and pyroxene.)
NUMBER 24 41

proposed different criteria for distinguishing between the two classes. Duke and Silver (1967)

discussed previous classifications, and adopted

the definition of eucrites as monomict breccias

and howardites as polymict breccias. Takeda,

Miyamoto, Duke, and Ishii (1978:1159), however,

described the Yamato-74159 meteorite as a eucrite that "clearly is polymict in terms of lithic

variability but carries no magnesian orthopyroxene of the type found in howardites," and the

term polymict eucrite has been applied quite

widely since. We accept this term and the

definition thereof. Howardites are then polymict pyroxene-plagioclase achondrites containing

magnesian orthopyroxene. Our experience is that

these orthopyroxenes have compositions En>70,

and some have compositions indicating admixture of a diogenitic component, although the

range of compositions may be considerably

greater than in analysed diogenites.

ALHA78040 (211 g).—This is a complete unweathered specimen (~9.0 X 5.0 X 3.0 cm). Black,

shiny fusion crust 0.5 mm thick covers all the

surfaces of the stone. The crust has been removed

from the edges by spallation and has been preferentially weathered away on the surfaces in small

circular areas. The B and T surfaces have had the

most fusion crust removed, thus revealing light to

medium gray matrix material that contains small

(<1 mm), elongated, white grains, probably feldspar. The T and S surfaces each have a 1.0 cm

clast present. These clasts have a slightly lighter

color than the surrounding fusion crust. On the

N surface an oval vug is present. Inside this vug

is a weathered yellowish-brown inclusion ~0.5

cm diameter that has a coarser texture than the

surrounding matrix material.

ALHA78132 (656 g).—This appears to be a

complete specimen (11 X 10X8 cm) with vitreous

black fusion crust on all sides. The overall shape

is pyramidal with the B surface being flat. The

fusion crust on the T surface has flow bands, most

prominent in the N-S direction and less prominent in the W-E direction. The B surface has

radial flow lines in a concave area. The fusion

crust on the S surface is much duller than on the

rest of the stone. The crust has been spalled or

chipped in some areas, revealing a medium gray

interior material. Small (<1 mm) inclusions, both

lighter and darker than the matrix, are apparent.

Several holes (voids) that penetrate the fusion

crust by as much as ~1 cm were noted over the

entire stone. One in particular is ~9 mm in

diameter and ~ 1 cm deep and contains a yellowish grain (?) ~2 mm long. The cut face shows a

light gray matrix dotted with rounded and irregularly shaped grains (?) that are both lighter and

darker than the matrix. The largest grain is ~0.5

cm in diameter. The voids on the exterior of this

specimen did not appear in the interior. A vein(?)

of white grains extends for 6 cm across the cut

face in the W-E direction.

ALHA78158 (15.1 g).—This is not a complete

specimen. Shiny black fusion crust is present on

one surface. All other surfaces are fractures that

show a medium gray matrix with white flecks.

Some clasts (<1 mm) are oxidized to a yellow

color. An area ~0.5 cm diameter on the B surface

is a darker gray and appears very homogeneous—

this appears to be a rounded clast. One fracture

goes completely across the sample. Overall dimensions are 3.0 X 2.5 X 2.0 cm.

ALHA78165 (20.9 g).—This is not a complete

specimen (~3.5 X 3.0 X 1.5 cm). Shiny black

fusion crust covers only one surface. The other

surfaces are fracture surfaces that have a medium

gray matrix with <1 mm white clasts. A few of

these clasts are weathered and yellow. When this

stone was cleaved in half, a dark gray clast (~0.5

cm) was exposed.

ALHA79017 (310 g).—This meteorite is mostly

covered with a shiny black fusion crust with flow

bands on all surfaces. The areas devoid of fusion

crust are medium gray and speckled with light

and dark clasts that are <1 mm in diameter.

Some clasts are up to 0.5 cm long. The interior

exposed through chipping is lighter gray than the

exterior. Several large clasts of up to 1.2 cm are

visible on the fresh fractures.

Reid and Schwarz (1980:353) have studied the

Allan Hills eucrites and give the following description:

The basaltic achondrite meteorites collected in the Allan

Hills region of Antarctica (76005, 77302, 78040, 78132,
42 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

78158 and 78165) are all petrographically similar and could

even be pieces from a single fall. They are breccias with

abundant but small (from fine dust to a maximum diameter

of approximately 1 cm) angular clasts of rock and mineral

fragments. The lithic clasts are basaltic, consisting of subequal amounts of pyroxene and feldspar with a range of

igneous textures. The diverse clast types correspond to a

range of thermal histories and to a limited range of basaltic

compositions. Rock and mineral fragments studied to date

correspond in texture and in mineral composition to the

known range of eucrites, including both unequilibrated and

equilibrated types. The range in pyroxene compositions is

wide (\V04En69 to \V013En33) but pyroxenes with the compositions of those in diogenites are absent or rare.

The Allan Hills basaltic achondrites are unlike previously

described eucrites and howardites (with the possible exception of Macibini) in that they contain a series of fragments

covering a range of eucrite types and are thus polymict but

they do not appear to contain a diogenite component as in

typical howardites. The name polymict eucrite seems appropriate. Very similar polymict eucrites are common in the

suite of achondrites collected in the Yamato region of Antarctica, almost 3000 km from Allan Hills.

Petrographic examination of ALHA79O17 has

shown that it is a polymict eucrite similar to the

previously collected Allan Hills eucrites, and thus

possibly another piece of a single fall.

Takeda et al. (1980b) have published chemical

analyses of ALHA76005 and ALHA78132 that

show their near-identity in composition. Delaney

et al. (1980) have provided detailed descriptions

of eucritic clasts in ALHA78040 and ALHA

77302.

EETA79004 (390 g).—This oblong achondrite

(11 X 6.5 X 4 cm) is covered with a thin, dull

fusion crust on all but two surfaces. The exterior

matrix appears medium to dark gray and contains numerous clasts as large as 2 cm in diameter.

Most of the larger clasts are dark, though light

clasts do exist. Vugs occur in this meteorite. Most

are concentrated on a surface in an area devoid

of fusion crust. These vugs are as deep as 1 cm, as

wide as 0.5 cm. The interior matrix is light gray

with many inclusions. Many of the clasts in this

achondrite will be easily plucked out. Several

spots of severe oxidation are visible.

The thin section shows a breccia dominantly

made up of monomineralic pyroxene and feldspar

fragments in a fine-grained matrix. Much of the

matrix is dark and may be recrystallized. The

clasts are generally angular but some have poorly

defined outlines and may have been reheated.

Mineral fragments range up to 1.3 mm. They are

pyroxene (some showing exsolution), feldspar,

and minor opaques. Pyroxene compositions show

a range in Ca contents with little variation in

Mg/Fe, (\V02En45Fs53 to Wo4oEn36Fs24 with low

Ca compositions most abundant, in the few grains

analyzed). Feldspars range from OriAbeAn93 to

OriAbi4An85.

Two major types of lithic clasts are present: (1)

angular fragments up to 2.5 mm in size of fine

grained eucrites with igneous textures; (2) fragments up to 1.6 mm across of dark aphanitic

material that appears to consist of extremely fine

pyroxene and feldspar in a subparallel growth.

The overall texture and nature of the clasts resemble those of the Allan Hills polymict eucrites. The

small number of pyroxenes analyzed shows essentially no variation in Mg/Fe. On this evidence

EETA79004 is classified as a monomict equilibrated eucrite rather than a polymict eucrite.

EETA79005 (450 g).—One surface of this

achondrite (10.5 X 8 X 7 cm) is concave; the rest

of the meteorite is convex. Fusion crust is visible

only on one surface and it is very shiny and

polygonally fractured. The matrix is medium

gray in color and is speckled with light and dark

clasts up to 3 mm in diameter. Vugs are apparent

all over the sample. Chipping a corner off the

meteorite revealed one fine-grained, black clast

0.5 cm in diameter. The color of the interior

matrix is considerably lighter gray than the exterior.

EETA79011 (86.4 g).—A patch of dull black

fusion crust appears only on one surface. The rest

of this achondrite is medium gray. Several types

of clasts are visible on the exterior with the largest

one being ~0.7 cm in its longest dimension. The

interior revealed through chipping is lighter gray

in color than the exterior and contains many

clasts.

Petrographically these two meteorites are so

similar that the following descriptions of thin

section EETA79011 can serve for both. It shows

a fine breccia with highly angular, small, monomineralic pyroxene and feldspar clasts predom-
NUMBER 24 43

FIGURE 31.—Howardites: a, ALHA78006; black fusion crust coats most of surface; b,

EETA79006; fusion crust coats part of surface, but mostly fracture exposing vuggy interior; c,

photomicrograph of thin section of ALHA78006 (area of field is 3 X 2 mm) showing brecciated

structure and variety of clasts; d, photomicrograph of EETA79006 showing brecciated structure

and variety of clasts.

inating. Pyroxene grains range up to 2.5 mm,

with the large fragments showing evidence of

deformation. Some single pyroxene fragments

show exsolution textures. Among the small lithic

clasts are: (1) fragments of brown, devitrified

glass, up to 1.6 mm; (2) fine-grained eucrite clasts

with granoblastic texture, up to 0.6 mm; (3) finegrained eucrite fragments, up to 0.7 mm; and (4)

medium-grained eucrite up to 1.6 mm. Pyroxenes

have a range of compositions from \V04En66Fs30

to \V02En37Fs6i. The more magnesian pyroxenes

all have low Ca contents but the more Fe-rich

varieties range from \V02En37Fs6i to \V035En27

Feldspar ranges in composition from

to Ori.5Abi9An8o.

These two meteorites from Elephant Moraine

are classified as polymict eucrites. Their petrological similarity and the fact that they were

found within 400 m of each other, as shown on

the sketch map of Figure 7B (Cassidy and Rancitelli, this volume), strongly suggest that they are

individual pieces of a single fall.

HOWARDITES

FIGURE 31

ALHA78006 (8.0 g).—This is a nearly complete specimen (3.0 X 1.5 X 2.0 cm). Shiny black

fusion crust covers all of the stone except portions

of the E, W, and S surfaces. Where the sample is
44 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

devoid of fusion crust, light to dark gray interior

material is exposed. Cleaving this stone in half

revealed an unweathered, brecciated surface.

The thin section shows a complex breccia of

angular fragments, up to 1 mm long, of pyroxene

(orthopyroxene and pigeonite) and plagioclase,

with numerous polymineralic enclaves, set in a

matrix of comminuted pyroxene and plagioclase.

Accessory chromite and ilmenite and trace

amounts of troilite and nickel-iron are present.

The enclaves are holocrystalline pyroxene-plagioclase aggregates, and range considerably in texture from coarse-grained gabbroic to fine-grained

basaltic types. A slight amount of weathering is

indicated by small areas of rusty staining, usually

in association with metal grains. Microprobe

analyses show a wide range in pyroxene composition: Wo2-i2En3i_72Fs25-6i; a number of grains

with uniform composition \V03EnnFs26 suggests

the presence of a diogenitic component. Plagioclase averages Angi. A single grain of iron-rich

olivine (Fagi) was analyzed.

Takeda, Yanai, and Shiraishi (1980) have published analyses of orthopyroxene and inverted

pigeonite from ALHA78006.

EETA79006 (7167 g).—This meteorite (14 X

8.5 X 4.5 cm) is partly covered with dull to shiny

black fusion crust. Many vugs are present, some

with interior clasts. The medium gray matrix

contains a variety of clasts (dark gray, yellow,

white), the largest being 1 cm in its longest dimension. Several rounded spots of oxidation are

obvious and several cracks appear to penetrate

the sample. The interior of the meteorite is lighter

gray than the exterior. Several clasts (~3 mm

diameter) were revealed by chipping the specimen.

The thin section shows a fine-grained breccia

with angular pyroxene and feldspar fragments

and minor opaques. The larger pyroxene fragments, up to 1 mm, are commonly deformed and

some show exsolution. A variety of clast types

include the following: (1) fine grained eucritic

fragments, up to 2 mm; (2) polymineralic pyroxene-feldspar intergrowths; (3) fragments of brown

devitrified glass, up to 1 mm; (4) one fragment,

2 mm, with feldspar :» pyroxene; (5) one fragment, 2 mm, with pyroxene >> feldspar; and (6)

one 4.5 mm recrystallized eucrite clast with mosaic texture. Analysis of pyroxenes yields a wide

range of compositions from WoiEngoFsig to

\V015En28Fs57.

SHERGOTTITE

FIGURE 32

EETA79001 (7942 g).—All but one surface of

this achondrite (22 X 17 X 14 cm) is covered with

black fusion crust, but there are areas on all

surfaces where the fusion crust has been plucked

away. One surface has a deep regmaglypt that is

covered with fusion crust. The areas void of fusion

crust are white-gray and the matrix appears porous. Veins (~0.5 mm wide) of dark material

criss-cross each other. Whitish-yellow clasts (~3

mm diameter) are scattered all over this achondrite. Most of the specimen appears very finegrained but a small part near the E surface has a

different lithology. Sawing exposed a light interior with rounded white clasts, as large as 0.5 cm

in diameter. Several large, black, fine-grained

clasts, as large as 2.5 cm, are scattered over the

cut face. Some of these black clasts contain vugs

with glass in their interior. Upon chipping one of

these clasts containing a vug, the entire clast

popped out easily without adhering matrix. Numerous veins of black material criss-cross each

other. Most of these veins run through a black

clast. The longest vein is ~14 cm long. Near the

W end of the cut face are brownish clasts that

may be pyroxene. Ninety percent of the cut face

is fine-grained. Ten percent (near the E end) of

the cut face consists of intergrown pyroxene and

feldspar in a basaltic texture.

Thin sections were cut from the three different

lithologies: (1) the main mass of the meteorite;

(2) the material with basaltic texture at one end

of the sample; and (3) the dark clasts included in

the main mass. The main mass is a shocked but

unbrecciated pyroxenite with pyroxene as the

major phase but also containing maskelynite, MgAl chromite, iron sulfide, and ilmenite(P). The

major pyroxene is polysynthetically twinned pigeonite^) resembling twinned clinobronzite,
NUMBER 24 45

FIGURE 32.—EETA79001, shergottite: a, black fusion crust spalled off in some areas, exposing

light gray interior; b, sawn surface showing black glassy clasts; c, photomicrograph (area of field

is 3 X 2 mm) showing typical shergottite structure with maskelynite (white), pyroxene (gray),

and accessory chromite (black); d, photomicrograph (area of field is 3 X 2 mm) showing

twinned clinopyroxene (crossed polars).

ranging in composition from \Y05En70Fs25 to

\V012En50Fs38. Orthopyroxene forms the cores of

larger pyroxene grains and ranges in composition

from \V01.5En83Fsi6 to Wo3En7sFsi9. The larger

pyroxene grains, up to 3.5 mm, comprise untwinned cores zoned outward to polysynthetically

twinned rims. The smaller pyroxenes, 0.3 to 1

mm, are twinned clinopyroxenes and are intergrown with maskelynite laths. The maskelynite

ranges in composition from OriAb3gAn6o to

Ori.5Ab44An55. A few large olivines, F077 to F073,

range to 2.5 mm. The less abundant lithology

closely resembles Shergotty in texture but is finer

grained. The major minerals are clinopyroxene

and maskelynite; calcium phosphate, S1O2, ilmenite(?), and magnetite(?), are also present.

Elongate clinopyroxene and laths of maskelynite

are about one mm long and generally subparallel;

many of the maskelynite grains contain pyroxene

inclusions. Analysed pigeonites range from

\V010En52Fs38 to Woi8Eni5Fs67- The maskelynite

also shows a range in composition from

Oro.5Ab38An62 to Or4AbsoAn46. The dark clasts

are apparently loci of melting; in many cases they

connect with the thin, black, glassy(?) veinlets

that traverse much of the meteorite. Thin sections

from these dark areas show glass (with relict

olivine, pyroxene, and maskelynite inclusions),

devitrified glass, areas with mosaic texture, and

vesicular areas with quench textures. The dark
46 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

ALHA78OI9 1 cm cube

ALHA78262

FIGURE 33.—Ureilites: a, ALHA78019; patchy fusion crust is present; b, ALHA78262; fusion

crust coats most of the surface; c, d, photomicrographs (area of fields is 3 X 2 mm) of

ALHA78019 (c) and ALHA78262 (d); olivine (white, without cleavage cracks) and pyroxene

(light gray, with cleavage cracks), bordered by black material consisting largely of carbon.

areas appear to be more common in olivine-bearing portions of the main mass.

The meteorite is classed as a shergottite because

of the close similarities to the shergottites in texture and mineralogy. Both lithologies, however,

are distinct from Shergotty and Zagami.

UREILITES

FIGURE 33

ALHA78019 (30.3 g).—Fusion crust is present

on all surfaces but is patchy and does not cover

the entire stone. The fusion crust is smooth, dull

brownish black, and has polygonal fracture.

Where the fusion crust is missing the surface is

reddish brown and crystalline. The stone (3.0 X

2.5 X 3.0 cm) was cleaved in half and no unweathered material was exposed. The sample is

reddish brown throughout.

The thin section shows an aggregate of rounded

to subhedral grains (0.5-3 mm across) of olivine,

with minor pyroxene. The grains are rimmed

with black carbonaceous material. Trace

amounts of troilite and nickel-iron are present,

the latter largely altered to translucent brown

limonite concentrated along grain boundaries.

Microprobe analyses show olivine of uniform

composition (Fa22) with notably high CaO (0.4%)

and O2O3 (0.7%) contents; the pyroxene is a

pigeonite of composition WoioFsi8En72. This meteorite is a ureilite, with mineral compositions

essentially identical to those in the Kenna ureilite
NUMBER 24 47

*.**

FIGURE 34.—ALHA78113, aubrite: a, dark fusion crust

spalled off most of surface, exposing interior consisting

largely of white enstatite; b, sawn surface showing brecciated

structure of interior; c, photomicrograph of thin section (area

of field is 3 X 2 mm) showing brecciated enstatite (white)

veined by fine-grained, dark gray material.

(Berkley et al., 1976); it appears to be relatively

unshocked compared to most ureilites. ALHA

78019 has been described by Takeda and

Yanai (1979).

ALHA78262 (26.1 g).—This specimen (4.0 X

2.5 X 2.0 cm) is triangular and has thin, dull

black fusion crust on three surfaces. The remaining surfaces are fracture surfaces that are rough

on a small scale, resulting from exposed crystal

faces. The overall color is very dark greenish

black. The thin section is identical with that of

ALHA78019 in all respects, and these two stones

are apparently pieces of a single fall.

AUBRITE

FIGURE 34

ALHA78113 (298 g).—This specimen (8.5 X

6.5 X 3 cm) has a brecciated structure, with

abundant large enstatite grains (~2.5 X 2.0 cm)

and less numerous dark clasts exposed on the

surface; patches of very thin, black fusion crust

are present. Half of the B surface has thin, yellowish-brown weathering discoloration. Very small

spots (< 1 mm) of iron oxidation are present on

some surfaces. A cut face shows many large, white

enstatite clasts, a few containing isolated rounded

blebs of metal, some with oxidation halos. The

clasts are surrounded and veined by fine-grained,

dark gray material.

The thin section consists almost entirely of

clasts of orthopyroxene, up to 2 mm long, in a

groundmass of comminuted pyroxene. Accessory

amounts of sulfides and nickel-iron are present as

small grains in the groundmass. The section

shows a moderate amount of brown limonitic

staining concentrated around the metal grains.

Microprobe analyses show that the pyroxene is

an iron-free enstatite (FeO 0.1%) with minor and

variable amounts of CaO (0.2-0.6, average 0.5%).
48 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

FIGURE 35.—EETA79002, diogenite: a, dull black fusion crust coats stone, except in small areas

where spalled off to reveal light gray interior; b, photomicrographs of thin section (area of field

3 X 2 mm); orthopyroxene clasts (white) in matrix of comminuted orthopyroxene (gray) and

a little chromite (black).

Watters et al. (1980) have provided a detailed

mineralogical and petrographic description of

ALHA78113 and compared it with other aubrites. In addition to the minerals mentioned

above, they record the presence of accessory

amounts of forsterite (Fo 99.99) albite (An 3.39)

diopside (Wo 43.89, En 56.09, Fs 0.02), oldhamite, ferromagnesian alabandite, daubreelite, and

schreibersite.

DIOGENITE

FIGURE 35

EETA79002 (2843 g).—This rounded meteorite (15 X 13.5 X 10 cm) is covered with dull fusion

crust except on one fracture surface. Fusion crust

has been plucked away in places, revealing a

medium gray matrix with many light to creamcolored clasts (~0.5 cm diameter). Several areas

have been heavily oxidized giving these parts a

red-brown color. Many fractures penetrate this

meteorite. Chipping revealed an extensive orange-brown weathering rind as wide as 1 cm. The

interior matrix is blue-gray with many small (< 1

mm) clasts. Two white clasts ~0.5 cm diameter

were exposed. No metal was obvious.

The thin section shows a breccia with a very

cohesive, fine-grained matrix. Clasts are monomineralic, angular, and range up to 2 mm. One

angular lithic clast is polymineralic but extremely

fine-grained. The vast majority of the mineral

fragments are low-calcium pyroxenes of near-constant composition, Wo2En76Fs22- The only other

silicate phase identified is olivine, F075-76. Small

areas within the breccia are rich in very fine

opaque minerals. The meteorite is a diogenite but

is texturally distinct from the common diogenites.
Descriptions of Iron Meteorites

Roy S. Clarke, Jr.

This section provides descriptions of the 19 iron

meteorite specimens that have been collected in

Victoria Land since 1976. Their textural and

chemical properties indicate that five irons from

the Allan Hills derive from a single shower as do

nine from Derrick Peak (plus six more that were

collected from the same site by a New Zealand

party). Therefore, the total number of iron meteorite falls from Victoria Land is now seven.

Descriptions of specimens are given below and in

Table 3 in the order of their chemical classification groups. Specimens grouped as members of a

single fall are listed by the lowest-numbered specimen retained in United States collections.

Coarse Octahedrites

GROUP IA

ALHA76002 Group

ALHA76002 (1.51 kg).—This coarse octahedrite was the first iron meteorite to be recovered

from the Allan Hills. It was listed by King et al.

(1980:42) in the previous Catalog of Antarctic

Meteorites (Marvin and Mason, editors, 1980). It

was described and given an ambiguous classification by Olsen et al. (1978). Clarke et al. (1980)

have re-examined ALHA76002 and found it to

be indistinguishable from four other Allan Hills

specimens that were collected a year later. All

five are typical coarse octahedrites of chemical

group IA.

Roy S. Clarke, Jr., Department of Mineral Sciences, National Museum

of Natural History, Smithsonian Institution, Washington D.C.

20560.

(2.19 kg).—This specimen was

a photograph by King et al.

ALHA77250 (10.5 kg; 26 X 15 X 8 cm).

ALHA77263 (1.68 kg).—This specimen was

described with a photograph by King et al.

(1980:42).

ALHA77289

described with

(1980:42).

ALHA77290 (3.78 kg; 16X13X 6 cm).

All five specimens have generally similar reddish-brown iron oxide coatings. Surfaces that

were probably initially at least partially regmaglypt-covered have undergone severe weathering.

No fusion crust remains. Surfaces of the under

side of specimens are more severely weathered

than those that were exposed to the atmosphere.

An occasional troilite inclusion is visible at the

surface.

Macroetched surfaces reveal the same basic

metallography for all five specimens. They all

have surficial patches of an ablation-produced

zone of ot2 iron. Kamacite grains are 2-3 mm

wide, and their length is generally only a few

times their width. Areas of recrystallized kamacite

are unevenly distributed. Taenite-plessite areas

with comb texture, and grain-boundary taenite

are present. Schreibersite occurs at grain boundaries and as occasional large crystals. There are a

few large troilite-carbon inclusions surrounded by

schreibersite, and, in some instances, also cohenite.

The appearance, structure, and chemical data

given in Table 3 establish these five specimens as

typical coarse octahedrites of Group 1 A. The close

similarity in the chemical values makes it highly

likely that they are all pieces of the same shower.

49
50 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

TABLE 3.—Summary of data on iron meteorites (NMNH = National Museum of Natural

History, Smithsonian Institution, Washington, D.C.; NIPR = National Institute of Polar

Research, Tokyo; data in 4th to 9th columns from Clarke, Jarosewich, Goldstein, and Baedecker

(1980))

Specimen

number

ALHA76002*

77250

77263*

77289*

77290

PGPA77OO6*

ALHA77283

ALHA781OO

DRPA78OO1

78002

78003

78004

78005

78006

78007

78008

78009

ALHA78252

ALHA77255*

Original

wt. (kg)

1.51

10.5

1.68

2.19

3.78

18.9

10.5

0.085

15.2

7.21

0.144

0.134

18.4

0.389

11.9

59.4

138

2.79

0.767

NMNH

wt. (kg)

0.307

4.69

0.839

1.08

1.93

7.75

5.68

0.040

7.21

0.134

18.4

0.389

30.1

65.8

1.41

0.387

NIPR

wt. (kg)

? * *

5.42

0.779

1.01

1.73

8.16

4.34

0.040

15.2

0.144

11.9

26.1

67.6

1.32

0.367

Chemical

group

IA

IA

IA

IA

IA

IA

IA

IIA

IIB

IIB

IVA

Anom

Structural

classification

Og

Og

Og

Og

Og

Og

Og

H

Ogg

Ogg

Of

D

%Ni

6.84

6.84

6.84

6.84

6.84

7.27

7.33

9.33

12.23

ppm Ga

92.1

91.5

92.8

92.6

93.7

78.2

69.0

2.5

0.6

ppm Ge

404

455

414

386

407

245

230

<100

<200

ppm Ir

2.9

3.1

3.0

3.0

3.0

2.5

2.2

0.45

12.0

* Specimens listed in Marvin and Mason, editors (1980).

** Specimen material at both the National Institute of Polar Research, Tokyo and the Field Museum of Natural History,

Chicago.

PGPA77006 (18.9 kg).—This specimen from

Purgatory Peak in the Victoria dry valley was

described with a photograph by King et al.

(1980:42).

A macroetched surface revealed kamacite

band-width in the 1.5 to 2 mm range, with lengthto-width ratios ranging from 4 to 10. Neumann

bands are abundant, and along the rim of the

specimen kamacite has been converted to «2 by

atmospheric ablation. Taenite and taenite-plessite areas occupy at least half of the length of

kamacite grain boundaries, and a number of

areas of comb plessite are present. Schreibersite

occurs along grain boundaries, and occasional

schreibersites surrounded by cohenite are present.

No large inclusions were observed on the small

surface available. The structural and chemical

data from Table 3 establish that this is a typical

coarse octahedrite, a chemical group IA meteorite. It is chemically and structurally distinct from

both the ALHA76002 group and from

ALHA77283.

ALHA77283 (10.5 kg; 16.5 X 16 X 12.5 cm).—

The specimen has a generally rounded anterior

surface that is suggestive of aerodynamic shaping

during oriented atmospheric flight and a slightly

concave posterior surface. The specimen has been

severely weathered, particularly on the posterior

surface. Wind erosion while on the ice also appears to have been important. Taenite bands

stand out in relief over much of the surface,

revealing the internal octahedrite structure of the

meteorite.

Clarke et al. (1981) have studied this specimen

and shown it to contain preterrestrial, impactproduced diamond and lonsdaleite. The meteorite is a carbon-rich, coarse octahedrite of chemical

group IA (Table 3). It is similar in composition

and structure to carbon-rich Canyon Diablo specimens and its metallography indicates shock load-
NUMBER 24

51

FIGURE 36.—Polished and etched slice of ALHA77283: large inclusion at lower right is troilitecarbon-schreibersite-cohenite; carbonado-like material containing diamond and lonsdaleite

found in number of such inclusions, generally at borders between troilite and schreibersite;

dark mineral distributed throughout surface and generally at centers of kamacite lamellae is

cohenite; kamacite lamellae are arranged in coarse Widmanstatten pattern, with their lengths

short compared to their widths; taenite lamellae and taenite-plessite fields present at borders of

kamacite lamellae (length of bottom edge of specimen = 9.5 cm).

ing to moderate intensity. It contains a number

of troilite-carbon-schreibersite-cohenite inclusions

that are rich in carbonado-like material containing diamond and lonsdaleite (Figure 36). The

presence of an ablation-produced, heat-altered

zone indicates an uninterrupted passage through

the atmosphere and a non-explosive impact on

the earth. This establishes that the diamond and

lonsdaleite were produced preterrestrially.

Hexahedrite

GROUP IIA

ALHA78100 (85.0 g; 5 X 4.5 X 0.9 cm).—This

specimen, unlike others, was found frozen within

the ice. It is a thin, flat, slightly irregular plate

that appears to have been oriented during atmospheric flight. The anterior surface is rounded at

the edges and the posterior surface has been

affected more severely. It is covered with an

essentially featureless, reddish-brown oxide. The

anterior surface contains numerous 1 to 2 mm

pockmarks.

A microetched median section of the specimen

reveals single-crystal kamacite containing Neumann bands and inclusions. Schreibersite is abundant as rhabdites, and is also present as lamellar

schreibersite and as hieroglyphic schreibersite surrounding troilite-daubreelite inclusions. Troilitedaubreelite inclusions are present with only small

bordering schreibersites. The edge of the anterior

surface has an ablation rim averaging about 0.7

mm wide. No OL<L was observed on the posterior

surface. Fusion crust was not present, and surfaces

are covered with terrestrial oxide up to 0.25 mm

thick. The specimen is a Group IIA hexahedrite.
52 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES
NUMBER 24 53

FIGURE 37.—Derrick Peak irons: left, DRPA78009, largest of irons found on mountainside;

unusual appearance due to both lustrous, deep, reddish brown color and protruding schreibersite crystals; combination of corrosion and erosion appears to have affected an originally

regmaglypt-covered surface. Above, Photograph of polished and etched surface of DRPA78008;

dominant metallographic structures are areas of swathing kamacite surrounding large schreibersite or schreibersite-troilite inclusions; areas of coarsest Widmanstatten pattern are interspersed.
54 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

Coarsest Octahedrite

GROUP IIB

DRPA 78002 Group

Nine iron meteorites were recovered from

among the boulders covering the slopes of Derrick

Peak, in the Darwin Mountains. They are assumed to be from the same fall because of their

distribution over the mountainside (Marvin, this

issue) and their similar and strikingly unusual

appearances. No other iron meteorites are known

that have the same atypical, rich, reddish brown

color and large protruding blades of schreibersite.

This distinctive appearance is probably due to a

combination of corrosion and erosion of surfaces

of schreibersite-rich specimens in the polar environment (Figure 37).

It was decided by the Meteorite Working

Group that for this group of specimens it would

be better to distribute the smaller specimens between the United States and Japanese collections

rather than to cut each specimen in half.

DRPA78001, 78003, and 78007 were selected for

the National Institute of Polar Research, Tokyo,

in consultation with Professor T. Nagata. Specimens DPRA78002, 78004, 78005, 78006 were

selected for the United States Collection. The two

largest specimens, DRPA78008 and 78009, have

been sawed in half and distributed to the two

collections (Table 3). The United States specimens are listed below. Up to this time, only

DRPA78008 and 78009 have been prepared for

metallographic examination.

DRPA78002 (7.21 kg; 24 X 21 X 9 cm).—This

is a roughly fan-shaped specimen with a smooth

bottom surface that had been in contact with the

ground and a highly irregular and sculptured

upper surface. Depressions in the upper surface

resemble regmaglypts but may be corrosion pits.

Large schreibersites protrude from both surfaces.

Part of the bottom is covered with light-colored

and fresh-appearing corrosion products.

DRPA78004 (134 g; 4.5 X 4 X 2.5 cm).—All

surfaces of this specimen are highly corroded. The

top has a lustrous, reddish-brown oxide coating;

the bottom is lighter and has soil particles attached.

DRPA78005 (18.4 kg; 26 X 21 X 13 cm).—

The bottom surface of this specimen has been

rounded by deep weathering. Most of the specimen appears to have been above ground level but

is also deeply corroded and eroded. The specimen

is comparatively featureless with only a few protruding schreibersites.

DRPA78006 (389 g; 8 X 6 X 3 cm).—This is

a roughly rectangular specimen, the bulk of

which appears to have been exposed for a prolonged period to atmospheric corrosion and erosion. About one-quarter of the specimen appears

to have been below ground. It is deeply corroded

with soil attached. Large schreibersites protrude

from the top.

DRPA78008 (59.4 kg; 34 X 24 X 20 cm).—

This is a large, blocky specimen that has been

severely corroded and eroded. Its upper surfaces

are generally smooth with some areas of deep

pitting. The under surface is more deeply corroded, with some soil attached.

This is the first of the Derrick Peak specimens

to be examined structurally. A large area of

macroetched surface was prepared. The dominant structural units distributed over more than

half of the surface are broad and irregular areas

of swathing kamacite enclosing large hieroglyphic

schreibersites; some of these schreibersites border

centimeter-size troilites. Between these swathing

kamacite areas are areas of coarsest octahedrite

structure. Grain boundary schreibersite is common throughout the surface, and lamellar schreibersites are present in many areas of kamacite.

Neumann bands are abundant in the kamacite,

and deformation zones are a common feature.

Taenite and plessite are present in areas of

coarsest octahedrite structure. Weathering has

penetrated the section, particularly along grain

boundaries bordering swathing kamacite areas.
NUMBER 24 55

What appears to be cleavage cracks are present

in some areas of kamacite. This specimen is a

coarsest octahedrite, a Group IIB meteorite similar to Santa Luzia.

DRPA78009 (138 kg; 42 X 23 X 34 cm).—This

specimen is generally egg-shaped and sculptured

over much of its surface by regmaglypts that have

been deepened by terrestrial corrosion and erosion. Many schreibersites stand out in relief, particularly within depressions in the surface. A large

cut surface reveals that this specimen has the

same structure and composition as DRPA78008.

Although the other Derrick Peak irons have not

yet been analyzed, they clearly derive from the

same fall.

FIGURE 38.—Iron meteorite ALHA78252: left, as found on

slope leading up to the polar plateau; below, polished and

etched slice of meteorite showing fine octahedrite structure

(top curved surface was anterior surface during atmospheric

flight; thick rim of fusion crust accumulated on posterior

surface and is separated from body of specimen by thin layer

of corrosion; width = 10 cm).
56 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

FIGURE 39.—Sawed surface of ALHA77255 revealing large spherical silicate inclusion at

anterior edge of aerodynamically shaped meteorite (inclusion approximately 5 mm in diameter).

Fine Octahedrite

GROUP IVA

ALHA78252 (2.79 kg; 17 X 9.5 X 5 cm).—The

specimen has an elongated dome shape, a smooth

convex surface, and a slightly more irregular

concave surface. The shape is highly suggestive

of oriented atmospheric flight.

Examination of a macroetched surface revealed

kamacite band widths in the less than 0.5 mm

range, with a high length-to-width ratio. A continuous rim of out iron produced by atmospheric

ablation is present on the convex surface. Neumann bands are present, the kamacite has a

matte appearance, and some kamacite bands are

mildly deformed. Taenite bands continuously

border kamacite bands, and taenite-plessite areas

cover much of their surface. Several small troilites

are present. The specimen is a fine octahedrite, a

group IVA meteorite (Figure 38).

Ataxite

ANOMALOUS

ALHA77255 (767 g; 15 X 8 X 2 cm). This

specimen was described with a photograph in

Marvin and Mason (1980:42). It is boomerangshaped with slightly convex anterior and concave

posterior surfaces suggestive of oriented atmospheric flight. A saw cut to remove a slice for study

passed through the edge of a spherical silicate

inclusion approximately 5 mm in diameter (Figure 39).

Metallographic examination revealed an ataxitic structure. Occasional oriented kamacite spindles are present in a dense plessite matrix. Several

small troilites are visible. It is an anomalous

ataxite, similar in composition and structure to

the Nordheim meteorite.
Overview of Antarctic Irons

Roy S. Clarke, Jr.

Antarctica has enriched meteorite collections

in recent years by providing specimens from 10

different iron meteorite falls representing six

structural classes. A total of 22 individual specimens has been reported. The meteorites are listed

with their structural and chemical classifications

in Table 4 in the order of their date of recovery.

This note briefly summarizes the information

available in the literature on these meteorites.

Lazarev, Humboldt Mountains (found

1961).—This specimen was originally described

as a coarse octahedrite containing approximately

10% Ni. Buchwald (1975) has reviewed the available data and finds it to be more appropriate for

a pallasite than for an iron meteorite. He suggested that the meteorite should be re-examined

with this in mind. It is listed herein for completeness but is not counted as one of the 10 separate

iron meteorite falls.

Neptune Mountains, Pensacola Mountains

(found 1964).—This coarse octahedrite was discovered by a U.S. Geological Survey field party

and was first reported by Schmidt (1964). Buchwald (1975) described it in detail, and Scott and

Wasson (1976) established it as belonging to

chemical group IA.

Yamato 75031, Yamato Mountains, Eastern

Queen Maud Land.—The plessitic octahedrite

has been described by Fisher, Spangler, and NaRoy S. Clarke, Jr., Department of Mineral Sciences, National Museum

of Natural History, Smithsonian Institution, Washington, D.C.

20560.

gata (1978); Fisher, Goldstein, and Nagata

(1978); Nagata (1978); and Kracher, Willis, and

Wasson (1980), who list it as anomalous, ungrouped chemically.

Yamato 75105, Yamato Mountains, Eastern

Queen Maud Land.—This reheated hexahedrite

has been described by Nagata, Fisher, and Suguira (1976); Fisher, Goldstein, and Nagata

(1978); and Kracher, Willis, and Wasson (1980)

who grouped it as IIA.

Eighteen iron meteorite specimens were collected by the first three expeditions to Victoria

Land in 1976-1977, 1977-1978, and 1978-1979.

In addition, the Purgatory Peak iron (PGA77006)

came into the collection after being recovered

from the Victoria Valley by a University of

Maine field party.

The current location of all Antarctic irons and

a summary of information available on them is

given in Table 4. Specimens grouped together in

the table are thought to be individual pieces from

the same fall. The Allan Hills grouping is based

on appearance, metallography, and chemical

composition (Clarke et al., 1980). The Derrick

Peak grouping is based on their apparent distribution in a strewn field on a mountainside and

striking similarlity of highly unusual external appearances. In all, seven separate falls are indicated representing five meteorite classes.

Descriptions of the individual iron meteorite

specimens collected in Victoria Land are given

elsewhere in this volume (p. 49). For tabulations

of data see tables 3 and 4.

57
58 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

TABLE 4.—Data on Antarctic iron meteorites (collection numbers: 1 = Mining Institute,

Leningrad and Committee of Meteorites, Moscow; 2 = Division of Meteorites, National

Museum of Natural History, Smithsonian Institution; 3 = National Institute of Polar Research,

Tokyo; 4 = Meteorite Working Group, National Museum of Natural History, Smithsonian

Institution; 5 = specimen of ALHA76OO2 in the Field Museum of Natural History, Chicago)

Name/Specimen number

Lazarev (1961)

Neptune Mountains (1964)

Yamato 75031

Yamato 75105

ALHA76002 Group*

ALHA77255

ALHA77283

PGPA770O6

ALHA78100

ALHA78252

DRPA78002 Group**

Structural

class

Pallasite ?

Og

Opl

H

Og

D

Og

Og

H

Of

Ogg

Chemical

group

IA

Anom

IIA

IA

Anom

IA

IA

IIA

IVA

Number of

specimens

2

1

1

1

5

1

1

1

1

1

9

Collection(s)

1

2

3

3

3, 4, 5

3,4

3,4

3,4

3,4

3 , 4

3,4

* ALHA76002, 77250, 77263, 77289, 77290.

** DRPA78OO1 to 78009.
Overview of Antarctic Achondrites

Arch M. Reid

Introduction

The channeling of research energies into the

study of extraterrestrial materials brought about

by the lunar exploration program has led to a

renewed interest in the achondritic meteorites.

Recent studies of achondrites have helped elucidate the nature of igneous processes active very

early in solar system history and also have revealed the existence of a number of meteorites

that have relatively young crystallization ages.

Despite substantial improvement in analytical

techniques, which have allowed extensive studies

to be made on very small amounts of meteorite

material, the restricted availability of achondrites

has constrained investigations of these irreplacable samples. It is thus a great pleasure to record

that Japanese and United States expeditions to

the Antarctic over the 10-year period, 1969-1979,

added 62 specimens of achondrites to the available collections, and the 1979-1980 Japanese and

United States teams collected over 100 additional

achondritic fragments (see Tables 5 and 6).

The museums of the world contain probably

less than a hundred achondrites collected outside

Antarctica. Table 7 compares the distribution of

achondrite classes in the Antarctic and non-Antarctic collections. The numbers in the non-Antarctic column are an unreliable guide to the real

distribution of achondrite types in the total terrestrial infall because of the vagaries of observation, recognition, and recovery. The Antarctic

meteorites may provide a better guide since they

Arch M. Reid, Geology Department, University of Cape Town,

Rondebosch, South Africa.

are more easily recognized and are all carefully

studied and catalogued. A problem with the Antarctic collection, however, is that it is highly

probable that several individual samples are fragments from a single event, i.e., pieces of the same

meteorite or fragments from a shower.

Table 7 shows that there are marked differences

between the Antarctic and non-Antarctic achondrite collections. Diogenites are more abundant

in the Antarctic collection, comprising over half

the classified samples. The preponderance of diogenites may well be misleading, as the majority

of the samples are very similar to each other, all

having an uncommon granoblastic texture. These

recrystallised diogenites could all be fragments

from a single fall (Takeda, Miyamoto, Yanai, and

Haramura, 1978). The second most abundant

group of Antarctic achondrites are the eucrites.

TABLE 5.—Number of achondrite specimens in Antarctic

meteorite collections

Expeditions

pre-1969

Yamato Mountains

1969 Japanese

1973 Japanese

1974 Japanese

1975 Japanese

1979 Japanese

Victoria Land

1976 United States-Japanese

1977 United States-Japanese

1978 United States-Japanese

1979 United States

Number of

specimens

4

9

12

663

307

>3000

11

300

309

73

Number of

achondrites

0

1

1

28

12

>100

1

4

6

7

59
60 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

TABLE 6.—Types of achondrites in the Antarctic meteorite collections

Year / Location

1969 Yamato Mts.

1973 Yamato Mts.

1974 Yamato Mts.

1975 Yamato Mts.

1976 Allan Hills

1977 Allan Hills

1978 Allan Hills

1979* Allan Hills,

Reckling Peak,

Elephant Moraine

Totals

Diogenite

1

22

7

1

1

32

Howardite

1

1

1

3

Eucrite

polymict

2

5

1

1

4

2

16

monomict

1

1

2

Shergottite

1

1

2

Ureilite Aubrite

3

1

2 1

6 1

* The 1979 Japanese expedition to the Yamato Mountains returned with over 100

achondrites that have not all been classified (Yanai, 1980).

Eucrites and howardites are the most common

achondrites in the non-Antarctic compilation.

The Antarctic samples are distinctive in that

howardites and monomict eucrites are not common and that a particular type of eucrite makes

up the bulk of the collection. This type is the

polymict eucrite, described below, which is rare

in non-Antarctic collections. As with the diogenites, several of the polymict eucrites are very

similar and may be from a single fall. It should

be noted, however, that this unusual type of

eucrite is common at both the Yamato and Allan

Hills sites which are almost 3000 km apart.

Aubrites are rather rare in the Antarctic collection and so far none of the very unusual achondrites such as Nakhla, Chassigny, or Angra dos

Reis have been found. It is of great interest to

note that two shergottite meteorites, related to,

but not identical with, the two previously known

members of the shergottite class, have been recovered.

The differences between the Antarctic and

non-Antarctic collections are intriguing and while

any attempt to understand these differences may

be yet premature, we can speculate that: (a) the

differences are an artifact produced by inadequate sampling; (b) there is some factor that

results in the achondrite flux in the Antarctic

region of the earth being different from elsewhere;

or, (c) the distribution of achondrite meteorites

reaching the earth has changed with time and

the Antarctic collection represents an average

over a much longer time increment.

Descriptions of the individual meteorites are

presented by Score et al., in this volume, and in

a variety of other publications. Some of the more

interesting characteristics of the collection are

briefly summarised below, with particular emphasis on the aspects of the collection that appear

to be unique.

ACKNOWLEDGMENTS.—I thank Roberta Score

for substantial help. The research reported in this

paper was done while the author was a National

TABLE 7.—Comparison between Antarctic (excluding those

from the 1979-1980 Japanese expedition) and non-Antarctic

(Wasson, 1974:292) achondrites

Class

Diogenites

Howardites

Eucrites

Shergottites

Ureilites

Aubrites

Others

Totals

Antarctic

32

3

18

2

6

1

0

62

Non-Antarctic

8

19

24

2

6

9

13

81
NUMBER 24

61

Research Council Associate at the Johnson Space

Center in Houston, Texas and a Visiting Scientist

at the Lunar and Planetary Institute, which is

operated by the Universities Space Research Association under Contract No. NASW-3389 with

the National Aeronautics and Space Administration. This paper is LPI Contribution number 435.

Diogenites

TABLE 8

The initial 1969 Japanese collection of 9 meteorites in the Yamato Mountain regions contained one achondrite, originally named Yamato

(b), but now renamed Yamato 692. This 138 g

TABLE 8.—Data on diogenites in the Antarctic meteorite

collections

Locality

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Allan Hills

Elephant Moraine

Specimen number

692

74005

74010

74011

74013

74031

74037

74096

74097

74109

74125

74126

74136

74150

74151

74162

74344

74347

74368

74448

74546

74606

74648

75001

75004

75007

75014

75285

75299

ALHA77256

EETA79OO2

Weight (g)

138.0

3.8

298.5

206.0

2059.5

6.1

591.9

16.1

2193.9

43.5

107.0

14.5

725.0

33.4

49.1

3.9

1.4

7.8

4.1

17.7

7.3

2.9

185.5

4.1

37.0

2.6

3.0

3.1

9.1

676.2

2843.0

diogenite was described by Okada (1975), Okada

et al. (1975), and by Takeda et al. (1975). While

mineralogically and compositionally similar to

the known diogenites, it is texturally unique,

having a granoblastic texture rather than the

brecciated texture of most diogenites. The recovery of 22 diogenites in the 1974 Yamato expedition demonstrated that this texture, indicative of

severe recrystallisation, is characteristic of the

diogenites from this region of the Antarctic. As

noted above many, if not all, of these diogenites

may represent a single fall as they are petrographically alike and occur in the same geographic

region. The six diogenites in the 1975 Yamato

collection also include samples with granoblastic

textures.

The Yamato diogenites are orthopyroxenites

with pyroxenes around En74_72. One sample in the

1975 collection, 75032, is more iron-rich than

other diogenites and approaches the more magnesian eucrites in composition. Yamato 75032 is an

unrecrystallised monomict diogenite that has as

its dominant phase orthopyroxene (approximately Enes) with exsolved lamellae and blebs of

augite. Takeda et al. (1979) conclude that the

major primary phase in Yamato 75032 was a lowCa pigeonite now inverted to orthopyroxene, but

that primary orthopyroxene may also be present.

The meteorite is transitional between the diogenites and the more magnesian eucrites and fills in

the "apparent" gap in pyroxene crystallisation

trends between diogenites and eucrites.

The one diogenite from the Allan Hills region

(ALHA77256) weighs 676 g and is described as a

normal diogenite. The 2.8 kg diogenite from Elephant Moraine (EETA79002) has the minerals

of a normal diogenite but is a very fine breccia

with a few dark, fine-grained, lithic clasts. The

Antarctic diogenites thus extend the boundaries

of the diogenite class in composition, mineral

assemblage, and texture.

Eucrites and Howardites

TABLE 9

Both eucrites and howardites have been found

in the Antarctic but the most abundant samples

of this type are the "polymict eucrites." Their
62 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

TABLE 9.—Data on eucrites and howardites in the Antarctic

meteorite collections

Locality

Yamato Mountains

Elephant Moraine

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Allan Hills

Allan Hills

Allan Hills

Allan Hills

Allan Hills

Allan Hills

Allan Hills

Yamato Mountains

Allan Hills

Elephant Moraine

Type/Specimen number

EUCRITES

74365

EETA79004

POLYMICT EUCRITES

74159

74450

75011

75015

75295

75296

75305

ALHA76005

ALHA773O2

ALHA 78040

ALHA78132

ALHA78158

ALHA78165

ALHA 79017

HOWARDITES

7308

ALHA78006

EETA 79006

Weight (g)

10.0

390.3

98.2

235.6

121.5

166.6

8.8

8.6

7.9

1425.0

235.5

211.7

656.0

15.1

20.9

310.0

480.0

8.0

716.0

discovery has led to a welcome revision in the

nomenclature of basaltic achondrites (see Score

et al., this volume). Howardites are polymict

pyroxene-plagioclase achondrites containing

magnesian pyroxene that probably indicates admixture of a diogenitic component. Polymict eucrites are polymict pyroxene-plagioclase achondrites in which magnesian pyroxene, like that in

diogenites, is absent or rare. Eucrites can be

monomict or polymict and polymict eucrites can

contain cumulate and/or non-cumulate eucritic

clasts, and fragments of equilibrated or unequilibrated eucrite.

The Antarctic collection of eucrites and howardites is dominated by the polymict eucrites,

which are rare or absent in other collections. The

meteorite Macibini may be the only other known

example. The Antarctic polymict eucrites are all

fine breccias with no large clasts and with mineral

clasts (mostly pyroxene and plagioclase) predominating over lithic fragments. The lithic clasts are

mostly eucritic, and fragments with fine-grained

basaltic textures predominate. In a single sample

there is generally a wide range of clast types,

including clasts with extremely fine quench textures, clasts with more slowly cooled ophitic textures, clasts with cumulate textures, and eucrites

with partly recrystallized and granoblastic textures. Equilibrated and unequilibrated eucrite

fragments may be present in the same sample:

pyroxene compositions cover a wide range and

individual grains may be homogeneous, zoned, or

rimmed, and may or may not be exsolved. Textures indicative of rapid, near-surface cooling are

most common; more plutonic fragments are rarer,

especially in the Allan Hills and Elephant Moraine samples. Glass and devitrified glass fragments occur in some samples. The meteorites are

truly polymict but many of the fragments appear

to be derived from a closely related sequence of

rocks. The oxygen isotope data, however, suggest

that clasts from different oxygen isotope reservoirs

may be present in the same sample (Clayton et

al., 1979). In addition, preliminary chemical and

isotopic studies (Wooden et al., 1981) indicate

significant differences between the larger clasts

and the bulk meteorites.

To date only one of the Antarctic polymict

eucrites, ALHA76005, has been described in detail (Olsen et al., 1978; Miyamoto et al., 1979;

Grossman et al., 1981). The similarities among

the 16 known samples are great, however, and it

seems certain that they do not all represent individual falls. Consortia studies of several of the

Allan Hills samples, and particularly of separated

clasts, are currently underway.

Two eucrites in the collections, Yamato 74365

and Elephant Moraine 79004, appear to be normal monomict eucrites. There also are two howardites, Yamato 7308 and Elephant Moraine

79006, that contain a variety of mineral and rock

fragments. The presence of magnesian pyroxenes

indicates a diogenetic component in these breccias. These are howardites but they are very

similar in most respects to the polymict eucrites

and may only represent a slightly different sampling of a diverse source region that runs the
NUMBER 24 63

gamut from magnesian diogenite to iron-rich eucrite.

Eucrites and howardites from the Antarctic are

breccias of igneous and metamorphic fragments

in which eucritic material predominates. Most

breccias are polymict but the fragments comprise

a series of materials that may be closely related,

i.e., that reflect the effects of a range of different

thermal histories on compositionally similar materials or that comprise a limited range of rock

types related by simple igneous processes. Truly

exotic particles appear to be rare but we must

await more detailed studies, including isotopic

analyses, to test the preliminary petrographic observations.

The samples may be representative of regolith

material on the basaltic achondrite parent body.

The distribution of clast sizes and the relative

absence of severe shock effects and melting is

consistent with a regolith generated by a very

large number of low momentum impacts. Most

igneous fragments appear to derive from rapidly

cooled surface or near-surface environments. Textures indicative of slow cooling are not common

(though they may be more abundant in the Yamato polymict eucrites; Takeda, pers. comm.).

The apparent scarcity of plutonic materials will

also need to be tested in future work as the degree

of comminution in these breccias is not conducive

to the preservation of coarse-grained polymineralic fragments.

The regolith sampled by these achondrites is

dominantly composed of fragments of eucritic

lavas or hypabyssal intrusives and their derivatives. Coarser-grained diogenites may have existed at greater depth, as suggested in the layered

crust model of Takeda (1979). The differences

among the various achondrites may reflect different sampling of a partly stratified surface region.

The nature of the regolith sampled by the Antarctic eucrites and howardites is different from

the type of material sampled by most non-Antarctic basaltic achondrites. If all the eucrites derive from a single parent body then the surface of

that parent varied with respect to place and/or

time.

Shergottites

The Antarctic program has doubled the number of available samples of the rare meteorite

group, the shergottites. This group has been the

focus of much recent attention since it represents

the third example of extraterrestrial basaltic volcanism (in addition to the moon and the eucrites).

This interest was augmented by the discovery

that the shergottites have relatively young crystallisation ages (<1.3 b.y., Nyquist et al., 1979),

raising the problem of the location of heat sources

for basaltic volcanism late in solar system history.

Difficulties in interpreting the evolutionary history of the shergottites and in speculating on their

possible parent bodies will be eased by the results

of studies of two new shergottites, ALHA77OO5

and EETA79001, which are apparently related

to, but certainly not identical with, Shergotty and

Zagami.

Allan Hills 77005 is a 482.5 g achondrite that

is heterogeneous, with regions containing cumulate olivine and chromite poikilitically enclosed

by low-Ca and high-Ca magnesian pyroxenes

(McSween et al., 1979). Other regions consist of

olivine with interstitial maskelynite, chromite, ilmenite, troilite, whitlockite, and pyroxene. The

meteorite is apparently a heterogeneous cumulate

that may have formed from a magma similar to

that which gave rise to the shergottites or alternately may be representative of the type of source

material from which the shergottite parent

magma was derived.

While credible petrogenetic models can be

made linking ALHA77OO5 to the other shergottites, the isotopic data (Nyquist et al., 1979)

indicate that they cannot be comagmatic. Like

the shergottites, ALHA77OO5 appears to have a

young crystallisation age and also has undergone

shock metamorphism that converted the plagioclase to maskelynite. The fourth meteorite in this

group is a recent discovery from the 1979 U.S.

Antarctic collection, EETA79001. The feldspar

in this meteorite also has converted to maskelynite, indicative of a shock history. The mineral

assemblage is similar to, but not identical with,
64 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

the shergottites, and as yet no information on its

age is available.

EETA79001 contains two distinct lithologies.

The main mass is a pyroxenite with large, complexly zoned pyroxenes set in a mostly pigeonitemaskelynite groundmass. In comparison with the

other shergottites, the pyroxenes in EETA79001

are more magnesian and less Ca-rich. The other

lithology in EETA79001 is texturally and mineralogically similar to Shergotty but finer-grained

and seems on first inspection to lack high-Ca

pyroxenes. These two lithologies are in conjunction along what appears to be an undisturbed

igneous contact. Obviously the detailed study of

EETA79001 will add considerably to our knowledge of the shergottites. If the young ages of

Shergotty and Zagami and ALHA77OO5 are crystallisation ages and indicate melting late in solar

system history, then melting could be the result

of magmatic or impact events. An increase in the

number of related but distinct igneous rocks with

young ages argues for magmatic processes rather

than impact melting.

Ureilites

TABLE 10

There are six ureilites recovered from Antarctica but only one, ALHA77257, is sizeable, weighing almost 2 kg. These samples extend the range

of known variability within the group, as could

be expected since there were only eight known

ureilites prior to the Antarctic discoveries. Of

particular interest is Yamato 74659, which is a

low-Fe ureilite carrying the most magnesian pigeonite recorded from the group. The meteorite

also has a higher pyroxene to olivine ratio than

the other ureilites. At the other end of the spectrum Yamato 74130 carries augite rather than

TABLE 10.—Data on ureilites in the Antarctic meteorite

collections

Locality

Yamato Mountains

Yamato Mountains

Yamato Mountains

Allan Hills

Allan Hills

Allan_ Hills

Specimen number

74123

74130

74695

ALHA77257

ALHA78019

ALHA78262

Weight (g)

69.9

17.9

18.9

1995.7

30.3

26.2

pigeonite and has an unusually Fe-rich olivine

(Fo76).

Aubrites

The 1978 collection from the Allan Hills area

contains a single sample of an aubrite,

ALHA78113 (298.6 g). The sample is a breccia

with enstatite grains, described as being up to 2.5

X 2.0 cm, which are essentially iron-free, along

with minor nickel-iron and troilite.

Conclusions

The Antarctic meteorite collections have already yielded a substantial number of unique

achondrites. Future collections will undoubtedly

add to their number and there may be many

surprises still to come. With further extension of

the search areas we may be able to obtain reasonable statistics on the relative abundances of the

various achondrite types. The overall differences

between Antarctic and non-Antarctic achondrite

abundances may simply be an indication that

both data sets are still too small to be representative. The reason for the abundance of polymict

eucrites in the Antarctic is not, however, readily

apparent.
Overview of Antarctic Carbonaceous Chondrites

Carleton B. Moore

Seven carbonaceous chondrite specimens have

been collected from the Yamato Mountains and

three from the Allan Hills region of Antarctica.

At the Sixth Symposium on Antarctic Meteorites

held on 19 February 1981, at the National Institute of Polar Research, Tokyo, it was reported

that, of the approximately 3000 meteorites collected during the 1979-1980 field season, an additional 20 uncharacterized, small, carbonaceous,

chondrite pieces were recovered. This relatively

low yield compared to the large number of ordinary chondrites recovered leads to speculation

that in Antarctica there are processes that act

against the recovery of this interesting meteorite

type. The possibility that the recovered carbonaceous chondrites fell near their recovery sites and

have not been transported long distances by moving ice may ultimately be tested by measurements

of their terrestrial residence times.

The Antarctic carbonaceous chondrites are

mostly C2 chondrites. In addition there are three

C3 and one C4 chondrite. The precise classification of several small specimens from the Yamato

area has not been reported. The carbonaceous

chondrite yield from the Antarctic meteorite expeditions is shown in Table 11.

The Antarctic carbonaceous chondrites appear

to be relatively fresh, unweathered, and uncontaminated with terrestrial organic molecules. The

white precipitates of carbonates and sulfates (reported by Marvin and Motylewski, 1980) on one

C3 (ALHA773O7) are only minor surface features.

Carleton B. Moore, Center for Meteorite Studies, Arizona State

University, Tempe, Arizona 85281.

Interior and exterior samples of ALHA77306 do

not show significant differences in bulk chemical

composition (Table 12).

The concentrations of amino acids in two large

C2 Antarctic meteorites, Yamato 74662 and

ALHA77306, have been well established. Analyses of interior and exterior splits support the

assertion that these meteorite finds are clean,

pristine specimens (see also Lipschutz, this issue).

Analyses done in different laboratories using different techniques give results that do not differ

significantly in the abundances of individual

amino acids. The C2 chondrite, Yamato 74662,

is similar to the Murchison C2 chondrite, while

ALHA77306 shows greater similarities to the Nogoya C2 chondrite. Petrographic study of

ALHA77306 by McSween (1979) establishes its

similarity with Nogoya and other matrix-rich C2

chondrites. ALHA773O6 and Nogoya have significantly lower total amino acid concentrations

than Yamato 74662 and Murchison (Cronin et

al., 1979; Shimoyama, Ponnamperuma, and

Yanai, 1979a,b; Kotra et al., 1979). Holzer and

Oro (1979) reported that pyrolysis products detected in ALHA773O6 are also lower than those

in Murchison. Unpublished work by Cronin (Arizona State University laboratory) on ALHA

77307, a C3 chondrite, showed no significant

indigeneous or terrestrial amino acids.

Magnetic studies of Yamato 74662 and Yamato 693 by Nagata (1980) confirm their classification as C2 and C3 chondrites, respectively.

Brecher (1980) has studied Yamato 74662 and

confirms Nagata's magnetic results.

Hyman and Rowe (1979) suggest that the mag65
66 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

TABLE 11.—Data on carbonaceous chondrites in the Antarctic meteorite collections

Locality

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Yamato Mountains

Allan Hills

Allan Hills

Allan Hills

Allan Hills

Specimen number

693

74641

74642

74662

75003

75260

75293

ALHA77003

ALHA773O6

ALHA773O7

ALHA78261

Type

C3

C?

C2

C2

C?

C2

C?

C3

C2

C3V

G2

Weight (g)

150

4.5

10.6

151

1.5

4.0

8.1

779

19.9

181

5.1

TABLE 12.—Partial chemical analyses of Antarctic carbonaceous chondrites (Allan Hills

analyses by M.-S. Ma and R.H. Schmitt, in litt., June 1980; Yamato analyses by Jochum et al.,

1980; carbon and sulfur analyses by Gibson and Andrawes, 1980)

Constituent

A12O3

FeO

MgO

C a O

Na2O

K2O

Co

Ni

C

s

ALHA77036

Exterior

2.1%

25.4

18.3

1.9

0.52

0.045

0.052

1.1

—

—

Interior

2.1%

25.6

18.5

1.8

0.56

0.038

0.052

1.1

1.32

3.86

ALHA77307

2.7%

30.7

21.0

2.2

0.15

0.029

0.051

1.0

0.83

1.52

Yamato 74662

2.1%

30.1

19.8

1.7

0.22

0.037

0.061

1.4

1.5

3.49

Yamato 693

2.5%

33.2

24.8

2.4

0.43

0.039

0.062

1.3

0.06

1.60

netic properties of ALHA77306 indicate that it

contains less than 0.8% magnetite.

Clayton, Mayeda, and Onuma (1979) state

that Yamato 693 has oxygen isotopic compositions virtually identical with Karoonda, classified

as a C4 or C5.

Matrix phyllosilicates of ALHA77306 have

been studied by McKee and Moore (1980) using

high-resolution, transmission electron microscopy. They have been identified as various components of the serpentine group. ALHA77306

appears to have the most complete assemblage of

the various phyllosilicate groups thus far identified in a single meteorite.

Available data on the Antarctic carbonaceous

chondrites through 1980 are still rather sparse;

however, numerous current investigations will

make more complete characterization possible in

the near future.
Weathering Effects in Antarctic Meteorites

Michael E. Lipschutz

The large number of Antarctic meteorites already recovered includes samples of previously

rare and unknown types, and future recoveries

will enlarge the sample base even further. Potentially, this should permit more complete characterization of extraterrestrial parent objects and

the genetic and evolutionary processes that

formed them; compositional data are essential in

this regard. Chemical studies are useful, however,

only to the extent that the preterrestrial composition is unaltered by weathering during the meteorites' terrestrial residence (see accompanying

summary by Evans, Reeves, and Rancitelli). I

review herein those chemical data bearing upon

effects of chemical alteration by weathering of

Antarctic stony and stony-iron meteorites.

In more temperate regions, weathering effects

in meteoritic finds generally involve contamination—usually to such an extent that trace element

data of finds are viewed very suspiciously. Conditions in Antarctica are sufficiently different that

the principal weathering effect in meteoritic finds

there is element-loss by leaching; contamination,

however, is observed for some elements. Different

elements in the same meteorite can respond differently to weathering; thus, absence of a weathering effect for one element need not mean that

another will be unaffected. Conceivably, element

lability could be affected by host-siting; thus, an

element could be unaffected in one type of meteorite while being very labile in another weathered under the same conditions for an identical

period.

Michael E. Lipschutz, Department of Chemistry, Purdue University,

West Lafayette, Indiana 47907.

Even in meteoritic falls, indigenous compositions vary widely, particularly for elements present at the ppb-ppt levels. Thus, weathering effects in Antarctic meteorites, all of which are

finds, must be established by comparing their

compositions with those of similar falls and/or by

uncovering systematic compositional variations

in exterior versus interior portions.

Macroscopically, stony meteorites are classified

by degree of weathering and fracturing, increasing in severity from class A to C. Minor weathering (A) is characterized by traces of rust halos

around metal grains and oxide staining along

cracks. Moderate weathering (B) produces large

rust halos around metal grains and extensive

oxide staining along internal cracks. Severely

weathered (C) specimens are uniformly stained

brown and retain little or no metal. Slightly

fractured (A) specimens exhibit few or no cracks

and none penetrate the entire specimen. In moderate fracturing (B) several cracks may extend

across the specimen, which can be readily broken

along the fractures. Severely fractured (C) specimens exhibit many extensive cracks and readily

crumble.

Some samples (e.g., seven of ~ 300 collected in

1977-1978) exhibit white surficial deposits that,

Marvin and Motylewski (1980) identify as hydrated magnesium carbonates and sulfates. These

authors attribute these deposits to early stages of

weathering after the samples' exposure on the ice

surface. (The seven specimens include five of

weathering type A and one each of types B and

C.) Marvin and Motylewski (1980) suggest that

the deposits were formed from salts leached from

the meteorites by liquid water produced from

67
68 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

snow on sun-warmed meteoritic surfaces.

Inorganic carbon-containing compounds (and

some organic ones) should be especially sensitive

to weathering. Cronin et al. (1979) report that

amino acid composition and contents in interior

and exterior samples of the weathering type A C2

chondrite ALHA773O6 are similar to those of C2

chondrite falls. Total C contents in this chondrite

(and Yamato 74662) are lower than those in other

C2 chondrite falls; S contents are not atypical,

however (Gibson and Yanai, 1979a,b). Total C

and S contents of a ureilite and C4 and E4

chondrites recovered from the Yamato Mountains region resemble those of similar meteorites

(Gibson and Yanai, 1979a,b) from other regions.

Gibson and Andrawes (1980) report that most of

the 25 ALH meteorites they studied have C and

S contents within ranges reported for similar falls.

(This sampling includes ordinary chondrites of

petrologic types 3-6, C2 and C3 chondrites, and

a ureilite.) Evidence for weathering effects sometimes appears. The weathering type B L6 chondrite ALHA77281 contains 250jiig C/g compared

with 160-200jLtg C/g in the possibly related chondrites 77280 and 77282. Surface samples of

the type B chondrites ALHA7 7002(L5) and

77269(L6) contain nearly twice as much C as

interior samples of the same stones. Exterior samples are depleted in S by about 10% compared

with interior ones. Stepwise pyrolysis of exterior

and interior samples of 77002 and an interior

sample of another weathering type B L6 chondrite, ALHA77273, demonstrates CO2 evolution,

presumably from secondary cabonates. The C

contents of several weathering type C meteorites

seem high but S contents seem normal.

Trace elements should, in principle, be most

informative about weathering processes because

even a small absolute change in concentration

should be reflected in a large relative change. For

example, Patchett and Tatsumoto (1980) studied

Lu/Hf isotopic systematics in eucrites and report

that data for ALHA773O2 (a weathering type A

meteorite) lie slightly off the

 176Hf/177Hf vs.

176Lu/177Hf isochron defined by 9 other eucrites.

They attribute this to loss of Lu by leaching

during weathering, although it is not clear why

Lu should be leached preferentially. Unfortunately, meteoritic contents of trace elements (particularly the more volatile/mobile ones) are intrinsically variable since they can be affected by

primary nebular condensation, secondary thermal processes in parent bodies, or tertiary shockheating. While weathering effects can be established at times by comparing data for interior

and exterior portions of a sample and by examining data for meteorites of a similar type, it is

not always possible to eliminate the possibility

that trace element variations pre-date terrestrial

residence.

Thus far, trace elements studies of Antarctic

meteorites have involved mainly those of weathering type A. Biswas, Ngo, and Lipschutz (1980)

determined Ag, As, Au, Bi, Cd, Co, Cs, Cu, Ga,

In, Rb, Sb, Se, Te, Tl, and Zn in exterior and

interior portions of ALHA77257 ureilite and

77278 L3 chondrite. They found significant Cs

and Rb enrichments in the exterior samples of

both meteorites and attributed this to deposition

of wind-borne oceanic aerosol. Six elements (As,

Au, Co, Cu, Ga, and Zn) seem unaffected by

weathering even in surface samples. The eight

other elements exhibit contrasting trends in exterior/interior parts of the two meteorites.

Trace element data for the 16 elements in

interior samples of Antarctic meteorites (i.e., those

obtained at depths > 1 cm below exterior surfaces) generally accord well with results for similar meteoritic falls. Thus far, comparisons are

available involving the following ALH meteorites: 77005 with shergottites (McSween et al.,

1979; Biswas, Ngo, and Lipschutz 1980); 77081

with Acapulco and 77307 with C3V chondrites

(Biswas et al., unpublished data); 77257 with

ureilites, 77278 with L3 chondrites and 77299

with H3 chondrites (Biswas, Ngo, and Lipschutz

1980); 78113 with enstatite achondrites (Biswas,

Walsh et al. 1980). The comparison for 77005

also includes K, Th, and U. In each case, concordance between data for Antarctic and non-Antarctic meteorites is typically as good as that between samples of any two similar meteorite falls.
NUMBER 24 69

In summary, Antarctic meteorite compositions reflect contamination. With proper precautions,

can be affected by weathering but are unaltered data obtained from Antarctic meteorites are as

for interior portions of type A meteorites, at least. reliable as those determined for meteoritic falls.

Where weathering effects can be detected, they ACKNOWLEDGMENT.—This research was supgenerally involve elemental loss by leaching. Con- ported in part by NASA grant NGL 15-005-140.

tents of a few elements—C and alkali metals—
Aluminum-26: Survey of Victoria Land Meteorites

J.C. Evans, J.H. Reeves, and L.A. Rancitelli

Over the past two years an extensive survey of

the

 26A1 (ti/2 = 720,000 y) content of Victoria

Land meteorites has been carried out by nondestructive gamma-ray analysis. To date a total of

104 samples from the Victoria Land region has

been studied. Most of the samples have been

ordinary chondrites from the Allan Hills region.

Future studies will, however, increasingly emphasize specimens from other regions, as well as

including larger numbers of achondrites. The

ultimate goal of this work is to establish terrestrial

ages for meteorites recovered from the Antarctic

ice sheet. This information can then be used to

infer information on long-term movement of the

ice sheet, as well as helping to provide an understanding of the accumulation mechanism for meteorites at specific sites. Terrestrial residence times

can, in principle, be derived from a measurement

of the decay of a cosmic ray-produced isotope

from its saturation level in space. Shielding and

complex exposure history can influence the production rate in space, making calculation of a

terrestrial residence time from a single Al measurement rather uncertain for individual meteorites. The

 26A1 measurements are thus most useful as a survey to identify interesting cases requiring more detailed analysis by other more timeconsuming techniques. Such additional measurements may include

 10Be, 14C, 36C1, 53Mn, noble

rare gases, cosmic ray tracks, and thermoluminescence.

J.C. Evans, J.H. Reeves, and L.A. Rancitelli, Battelle Pacific

Northwest Laboratories, P. 0. Box 999, Richland, Washington,

99352.

Measurements of

 14C are useful for estimating

terrestrial ages of less than ~35 X 103 years for

setting lower bounds on terrestrial ages. Exposure

history is less significant for

 14C age estimates

than

 26A1 age estimates. Ten Allan Hills meteorites have been investigated for

 14C (Fireman 1979,

1980; Fireman et al., 1981). These are listed in

Table 13. One L chondrite, ALHA77OO3, has

a positive

 14C content, 3.6±1.0 dpm/kg, giving a 14C terrestrial age of (21 ± 4) X 103

years. Cosmogenic

 x C was observed in the achondrite ALHA77256 and in the H chondrite

ALHA77294, giving them

 14C terrestrial ages of

(11±1) X 103 years and (30±2) X 103 years,

respectively. Only limit values for

 14C were obtained for the other seven meteorites; their lower

limit ages range from 25 X 103 years for

ALHA77214 to 32 X 103 years for the others.

When combined with

 26A1 measurements, the

most useful isotopes for determining terrestrial

ages in the 0.1 to 1 m.y. range have been

 36C1

(ti/2 = 300,000 y) and

 53Mn (ti/2 = 3.7 m.y.).

Chlorine-36 has been measured in several Antarctic meteorites by a La Jolla-Rochester collaboration using the newly developed Van de Graaff

accelerator technique. Manganese-53 was measured on the same samples in La Jolla (Nishiizumi

et al., 1978; Nishiizumi et al., 1980) by the nowroutine neutron activation procedure. These published data have been included in Table 13, along

with the much larger volume of

 26A1 data. For the

meteorite studies, by all three methods, it is possible to derive terrestrial ages with some degree of

confidence.

70
NUMBER 24 71

TABLE 13.—Cosmogenic isotope content of Victoria Land meteorites (expected saturation

values:

 26A1 L = 59 ± 9 dpm/kg, H = 55 ± 8 dpm/kg; 36C1 = 25 ± 4 dpm/kg (Fe + Co + Ni

+ 6 Ca);

 53Mn = 450 ± 90 dpm/kg (Fe + 1/3 Ni); 14C = 60 ± 6 dpm/kg

Specimen

number

ALHA76004

ALHA76005

ALHA76006

ALHA76OO7

ALHA76O08

ALHA77OO1

ALHA77OO2

ALHA77OO3

ALHA77OO4

ALHA77OO9

ALHA77O1O

ALHA77O11

ALHA77025

ALHA77062

ALHA77O71

ALHA77O81

ALHA77O86

ALHA77118

ALHA77124

ALHA77144

ALHA7715O

ALHA77164

ALHA77177

ALHA77182

ALHA77190

ALHA77191

ALHA77192

ALHA77208

ALHA77214

ALHA77215

ALHA77216

ALHA77217

ALHA77224

ALHA77225

ALHA7723O

ALHA77232

ALHA77233

ALHA77249

ALHA77256

ALHA77258

ALHA77260

ALHA77261

ALHA77262

ALHA7727O

ALHA77272

ALHA77278

Class

LL3

Eucrite

H6

L6

H6

L6

L5

C3

H4

H4

H4

L3

H5

H5

H5

H

H5

H5

H5

H6

L6

L3

H5

H5

H4

H4

H4

H4

L3

L3

L3

L3

H4

H4

L4

H4

H4

L3

Diog.

H6

L3

L6

H4

L6

L6

LL3

Weathering

category

A

B

C

C

A

B

A

C

C

C

C

C

B

B

B

C

C

C

B

C

C

C

B

C

C

C

C

C

B

B

B

C

C

B

C

C

C

A

B

B

B

B

B

B

A

dpm/kg

58 ± 6

89 ± 9

51 ± 5

45 ± 4

11 ± 1

52 ± 5

30 ± 3

45 ± 5

52 ± 5

32 ± 2

49 ± 3

39 ± 4

54 ± 5

47 ± 5

55 ± 6

42 ± 4

58 ± 6

53 ± 5

70 ± 7

56 ± 6

43 ± 4

44 ± 5

54 ± 3

41 ± 4

51 ± 3

56 ± 4

55 ± 6

52 ± 3

56 ± 6

36 ± 4

40 ± 3

38 ± 3

51 ± 3

51 ± 3

51 ± 3

54 ± 3

47 ± 3

37 ± 2

29 ± 2

37 ± 2

36 ± 4

47 ± 5

40 ± 3

35 ± 4

28 ± 3

26Al

Terrestrial

age (10s y)

< 3 a

< 3 a

< 5 a

<r

<1.2d

7 ± 2e

<1.8e

< 3 a

<7a

< 3 a

< 4 a

< 3 a

< 5 a

<2a

< 3 a

<r

<2a

< 6 a

< 6 a

< 6 a

< 3 a

< 3 a

< 3 a

< 3 a

< 3 a

1.3 ±0.8f

< 8 a

< 6 a

< 7 a

< 3 a

< 4 a

<2a

<2a

<4a

< 7 a

0.11 ± .01f

< 9

5.4 ± 8e

3.2 ± 9e

"C

dpm/kg Terrestrial

age (105 y)

<1.0b >0.3b

<1.7b >0.3b

<1.2b >0.3b

<1.7b >0.3b

4.6 ± 1.0f

<1.4g >0.3g

<3.0f

16.0 ± 1.5f

<0.5f

36Cl

(dpm/kg Fe +

Co + M+6Ca)

9.4 ± 1.0d

20.1 ± 1.2d

4.6 ± l.l e

18.4 ± 1.2e

17.0±0.8e

6.6 ± 3.3e

10.9±0.7e

S3Mn

(dpm/kg

Fe+1/3 Ni)

22 ± 2d

422 ± 13d

255 ± 8e

317 ± 13e

151 ±6 e

213 ± ll e

2 6 4 ± ll e
72 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

TABLE 13.—Continued

Specimen

number

ALHA77282

ALHA77284

ALHA77285

ALHA77294

ALHA77297

ALHA77299

ALHA 7 7300

ALHA77304

ALHA 78001

ALHA78OO3

ALHA 78038

ALHA78039

ALHA 78041

ALHA78043

ALHA78044

ALHA78045

ALHA78046

ALHA78048

ALHA78049

ALHA78050

ALHA 78051

ALHA78O52

ALHA78O76

ALHA78O77

ALHA78102

ALHA 78103

ALHA78104

ALHA78105

ALHA78106

ALHA78109

ALHA78112

ALHA78114

ALHA 78115

ALHA78126

ALHA 78128

ALHA78130

ALHA 78131

ALHA78132

ALHA 78134

ALHA78251

RKPA 78001

RKPA78OO3

RKPA78004

META 78001

META78002

META78003

META78004

META 78005

META78006

Class

L6

L6

H6

H5

L6

H3

H5

LL3

L3

L6

L6

L4

L6

L6

L6

H6

H4

H5

L6

L6

L6

L6

LL5

L6

L6

H6

L6

H5

L6

L6

Eucrite

H4

L6

L6

L6

H4

H4

L6

L6

L6

H6

Weathering

category

B

B

C

A

B

A

C

B

C

B

B

B

B/C

B

B

B

C

C

B

B

B

B

B

B

C

B

B

C

C

C

A

C

B

C

C

A

C

B

B

B

C

dpm/kg

49 ± 3

45 ± 5

38 ± 4

70 ± 7

43 ± 4

54 ± 4

50 ± 3

50 ± 4

59 ± 4

36 ± 3

42 ± 3

38 ± 3

38 ± 3

51 ± 4

34 ± 3

46 ± 5

59 ± 5

52 ± 3

44 ± 3

38 ± 3

56 ± 4

52 ± 4

42 ± 3

35 ± 3

58 ± 3

53 ± 3

61 ± 7

44 ± 4

46 ± 3

42 ± 3

38 ± 2

43 ± 3

45 ± 3

34 ± 2

51 ± 4

40 ± 3

68 ± 4

61 ± 3

56 ± 6

49 ± 3

50 ± 3

39 ± 2

53 ± 3

47 ± 3

50 ± 3

49 ± 4

44 ± 3

60 ± 4

26Al 14C

36r/ 53 yf

ut jvin

Terrestrial dpm/kg Terrestrial (dpm/kg Fe + (dpm/kg

age (l(f y) age (l(f y) Co + M + 6 Ca) Fe + 1/3 Ni)

0.30 ± .02g 1.6±0.3g

< l a

<1.6e 18.9 ±8 e 317 ± 19e

< 5 a

<2a

< 8 a

< 6 a

< 7 a

< 8 a

<2a

< 5 a

< 3 a

< 5 a

<7a

<2a

< 3 a

<2a

< 6 a

<5a

< 6 a

<7a

< 5 a

< 5 a

<7a

< 4 a

< 6 a

< l a

< 3 a

< 4 a

< 4 a

< 6 a

<2a

< 5 a

< 4 a

< 5 a

< l a
NUMBER 24 73

Specimen

number

META78OO9

META78O1O

META78018

META78019

META 78021

META78023

META78025

META78028

BTNA78OO1

BTNA78004

BTNA78005

Class

H5

L6

L6

LL6

Weathering

category

B

B

B

B

dpm/kg

68 ± 4

56 ± 3

58 ± 4

108 ± 6

52 ± 12

54 ± 12

33 ± 2

56 ± 3

65 ± 4

49 ± 3

40 ± 2

TABLE 13.—Continued

26Al 14C

Terrestrial dpm/kg Terrestrial

age (l(fy) age (l(f y)

<2a

<3a

< l a

<4a

S6Cl

(dpm/kg Fe+

Co + Ni + 6Ca)

53Mn

(dpm/kg

Fe+l/3Ni)

a

 This work. Ages given are one sigma upper limits based on the uncertainties in both the expected and measured

 26A1.

Ages have not been calculated for samples lacking type classification.

b

 Fireman, 1979.

c

 Evans et al., 1979.

d

 Nishiizumi et al., 1979.

6

 Nishiizumi et al., 1980.

f

 Fireman, 1980.

g

 Fireman and Norris, 1981.

Of particular interest are ALHA77OO2 and

ALHA77272, for which Nishiizumi et al. (1980)

have derived terrestrial ages of 0.69±0.17 and

0.54±0.08 X 106 years, respectively. Terrestrial

ages in excess of 500,000 years may thus be fairly

common. ALHA76008 has been discussed in detail elsewhere (Evans et al., 1979; Nishiizumi et

al., 1979). The low

 26A1 found in this meteorite

led Fireman et al. (1979) to conclude that it had

a lone; terrestrial asre — 1.54 ±nr>r, \ Chlo-

° ° 0.28 m.y.

rine-36 and Mn measurements made subsequently by Nishiizumi et al. (1979) convincingly

demonstrated that this meteorite had experienced

a complete bombardment history followed by a

relatively short terrestrial residence. A similar

situation was also in evidence for one of the

Yamato meteorites, Yamato 7301. This clearly

demonstrates the hazards of using a single isotopic

measurement for an age determination.

An alternative approach involves a statistical

analysis of the whole body of data. Figure 40 is a

histogram of the frequency distribution of

 26A1

contents of 87 Antarctic meteorites for which type

information was available. A target element correction factor has been included to normalize the

data to an L chondrite composition. The dashed

line on the figure is the shape of the distribution

for contemporary falls and finds obtained by

making similar corrections on falls and finds. It is

quite clear that the Antarctic meteorites are distributed toward lower

 26A1 contents.

Figure 41 shows the same type of distribution

for H and L chondrites. It appears that most of

the low

 26A1 values are found amongst the L

chondrite population, suggesting a possible

shower contribution. There is, nevertheless, a

strong suggestion that terrestrial ages somewhat

in excess of 500,000 years may be fairly common,

while at the same time there is no evidence as yet

of any samples having ages in excess of one

million years. At present only a fraction of the

collection has been surveyed. Future work may

yet turn up older cases as the data base continues

to expand.
74 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

36

32

28

tSE

S

u

u.

O

a.

LLJ

00

3

Z

24

20

16

12

ALL ANTARCTIC CHONDRITES (87 CASES)

WORLD WIDE CHONDRITES (135 CASES)

10 20 40 50

26AI (dpm/kg)

60 70 80

16

12

. ANTARCTIC H CHONDRITES (36 CASES)

NORMALIZED TO

L COMPOSITION

ANTARCTIC L CHONDRITES (51 CASES)

10 20 40 50

6AI (dpm/kg)

70 80

FIGURE 40.—26Al content of Antarctic chondrites normalized

to L-type composition. Dashed line shows expected distribution taken from literature survey of

 26Al measurements

made on meteorites recovered from other parts of earth.

FIGURE 41.—2bAl content of Antarctic chondrites by class

normalized to L-type composition.
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1978. Crystallization of Pyroxenes in Lunar KREEP

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of the Ninth Lunar and Planetary Science Conference,

pages 1157-1171. New York: Pergamon Press.

Takeda, H., M. Miyamoto, M.B. Duke, and K. Yanai

1978. The Yamato-74659 Ureilite and Some New Findings on the Yamato Achondritic Pyroxenes. Meteontics, 13:641-645.

Takeda, H., M. Miyamoto, and T. Ishii

1978. Comparison of the Chemical Trends and Crystallography of Pyroxenes for KREEP Basalts with

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1979. Pyroxenes in Early Crustal Cumulates Found in

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Press.

1980. Comparisons of KREEPy Clasts in Lunar Basalts

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In Lunar and Planetary Science XI, pages 1116-1118.
NUMBER 24 83

Houston: Lunar and Planetary Institute.

1980. Comparison of Basaltic Clasts in Lunar and Eucritic Polymict Breccias. In Proceedings of the Eleventh Lunar and Planetary Science Conference, pages

135-147. New York: Pergamon Press.

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1976. Characterization of Crust Formation on a Parent

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the Seventh Lunar and Planetary Science Conference,

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1979. Mineralogical Examination of the Yamato-75

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Memoirs of the National Institute of Polar Research

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Takeda, H., M. Miyamoto, K. Yanai, and H. Haramura

1978. A Preliminary Mineralogical Examination of the

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Memoirs of the National Institute of Polar Research

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Takeda, H., and K. Yanai

1979. A New Olivine-Augite Achondrite Found in Antarctica. Meteoritics, 14:542-543.

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1980. Experimental Reproduction of Textures of Chondrules. Earth and Planetary Science Letters, 48:

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1980. ALHA78113, Mt. Egerton and the Aubrite Parent

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1978. Noble Gases in 10 Stony Meteorites from Antarctica and Their Exposure Ages. Meteoritics,

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84 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

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1978. Some Information on Topographic Features and

the Characteristics of the Sheet Ice around the

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Appendix

Tables of Victoria Land Meteorites

Terminology

Class and type: Au = aubrite; C = carbonaceous chondrite; Di = diogenite; Eu = eucrite;

Ho = howardite; H = high-iron chondrite; L = low-iron chondrite; LL = low-iron low-metal

chondrite; M — mesosiderite; Sh = shergottite; Ur = ureilite. Chondrite type is indicated by

the digit following the letter.

Olivine composition in mole percent Fe2SiC>4 (Fa).

Pyroxene (orthopyroxene or low-Ca clinopyroxene) composition in mole percent FeSiC>3

(Fs).

Degree of weathering: A = minor; metal flecks have inconspicuous rust halos, oxide stain

along cracks is minor. B = moderate; metal flecks show large rust halos, internal cracks show

extensive oxide stain. C = severe; specimen is uniformly stained brown, no metal survives.

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; DRP = Derrick Peak; EET =

Elephant Moraine; MET = Meteorite Hills; MBR = Mount Baldr; PGP = Purgatory Peak;

RKP = Reckling Peak.

TABLE A.—Characteristics of meteorites listed by source area, in numerical sequence

Specimen

number

ALHA

76001

76002

76003

76004

76005

76006

76007

76008

76009

77001

77002

77003

77004

77005

77009

77010

77011

Weight (g)

20151

1510

10495

305

1425

1137

410

1150

407000

252

235

779

2230

483

235

295

291

Class

and

type

L6

Iron

L6

LL3

Eu

H6

L6

H6

L6

L6

L5

C3

H4

Sh

H4

H4

L3

%Fa

in

olivine

25

25

0-34

18

24

19

24

25

25

4-48

17-20

28

18

18

4-36

%Fs

in

pyroxene

21

21

0-53

37-57

16

21

17

21

21

22

2-25

15-27

23

16

15-18

1-33

Degree

of

weathering

A

A

A

A

B

A

B

B

B

B

A

C

A

C

C

C

Specimen

number

77012

77014

77015

77021

77025

77033

77061

77062

77064

77071

77074

77081

77086

77088

77102

77118

77119

77124

Weight (g)

180

309

411

16.7

19.4

9.3

12.6

16.7

6.5

10.9

12.1

8.6

19.4

51.2

12.3

7.8

6.4

4.4

Class

and

type

H5

H5

L3

H5

H5

L3

H5

H5

H5

H5

H5

H?

H5

H5

H5

H5

H5

H5

%Fa

in

olivine

18

18

1-21

18

18

8-38

18

18

18

18

18

11

19

19

19

19

18

19

%Fs

in

pyroxene

16

17

4-24

17

17

8-9

17

17

17

17

17

11

17

17

15

17

17

16

Degree

of

weathering

C

c

c

c

c

c

B

B

B

B

B

B

C

C

B

C

C

C

85
86 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

TABLE A.—Continued

Specimen

number

77140

77144

77148

77150

77155

77160

77164

77165

77167

77177

77180

77182

77183

77190

77191

77192

77208

77214

77215

77216

77217

77219

77221

77223

77224

77225

77226

77230

77231

77232

77233

77249

77250

77252

77254

77255

77256

77257

77258

77259

77260

77261

77262

77263

77264

77268

77269

77270

77271

Weight (g)

78.6

7.9

13.1

58.3

305

70.4

38.1

30.5

611

368

190

1134

288

387

642

845

1733

2111

820

1470

413

637

229

207

787

5878

15323

2473

9270

6494

4087

504

10555

343

246

765

676

1996

597

294

744

412

862

1669

11.0

272

1045

589

610

Class

and

type

L3

H6

H6

L6

L6

L3

L3

L3

L3

H5

L6

H5

H6

H4

H4

H4

H4

L3

L3

L3

L3

M

H4

H4

H4

H4

H4

L4

L6

H4

H4

L3

Iron

L3

L5

Iron

Di

Ur

H6

H5

L3

L6

H4

Iron

H5

H5

L6

L6

H6

%Fa

in

olivine

8-44

19

18

25

24

3-46

6-39

8-33

2-41

18

24

19

19

17-19

16-18

16-18

17

1-49

22-26

15-35

17-25

26

15

17

19

17

18

22-25

24

17

14-21

7-35

22-28

23

13

18

18

7-23

24

15-19

19

18

24

24

18

%Fs

in

pyroxene

2-17

17

16

22

20

6-40

3-41

6-35

3-17

16

20

17

16

15-22

14-16

15-21

14

4-23

9-21.

14-23

9-26

24-28

13-15

15-23

17

16

16

18-29

21

15

15-17

2-25

2-22

20

23

12

16

15

1-28

21

13-16

16

16

22

21

16

Degree

of

weathering

C

B

C

C

A /B

C

C

C

C

C

C

B

C

C

C

C

C

C

B

A/B

B

B

C

C

C

C

C

B

A/B

C

C

C

B

A/B

A/B

A

B/C

C

C

B

B

A /B

C

B

A/B

C

Specimen

number

77272

77273

77274

77277

77278

77280

77281

77282

77283

77284

77285

77286

77287

77288

77289

77290

77292

77294

77296

77297

77299

77300

77302

77304

77305

77306

77307

78006

78019

78038

78039

78040

78042

78043

78044

78045

78048

78050

78053

78074

78075

78076

78077

78078

78084

78085

78100

78102

Weight (g)

674

492

288

143

313

3226

1231

4127

10510

376

271

245

230

1880

2186

3784

199

1351

963

952

261

235

236

650

6444

19.9

181

8.0

30.3

363

299

211

214

680

164

396

190

1045

179

200

280

275

330

290

14280

219

84.9

336

Class

and

type

L6

L6

H5

L6

LL3

L6

L6

L6

Iron

L6

H6

H4

H5

H6

Iron

Iron

L6

H5

L6

L6

H3

H5

Eu

LL3

L6

C2

C3

Ho

Ur

L3

L6

Eu

L6

L6

L4

L6

L6

L6

H4

L6

H5

H6

H4

L6

H3

H5

Iron

H5

%Fa

in

olivine

24

24

18

24

11-29

24

24

24

25

18

17

18

19

24

17

24

24

11-21

18

18-27

24

1-30

22

4-42

24

24

25

23-25

25

24

23

17

24

18

18

19

24

18

18

18

%Fs

in

pyroxene

20

20

16

20

9-21

21

20

20

21

16

12-16

16

17

20

15

21

20

15-20

16

37-64

13-19

21

1-12

25-61

18

2-19

21

33-52

20

21

19-24

21

21

20

16

21

16

16

15-18

20

8-24

16

17

Degree

of

weathering

B/C

B

C

A/B

A

B

B

B

A/B

C

C

C

B

B

A

A/B

A

A

C

A

B

B/C

A

A

A

B/C

C

B

A

B

B

B/C

B/C

A/B

B

C

B

B/C

B

C

A/B

B/C

B

B/C
NUMBER 24 87

TABLE A.—Continued

Specimen

number

78103

78104

78105

78106

78107

78108

78109

78110

78111

78112

78113

78114

78115

78126

78127

78128

78130

78131

78132

78134

78153

78158

78165

78188

78193

78196

78209

78211

78213

78215

78221

78223

78225

78227

78229

78231

78233

78251

78252

78261

78262

79001

79002

79003

79004

79005

79006

79007

79008

Weight (g)

589

672

941

464

198

172

233

160

126

2485

298

808

847

606

194

154

2733

268

656

458

151

15.1

20.9

0.8

13.3

11.1

12.1

11.4

9.5

6.3

5.4

6.4

4.5

2.4

1.9

1.8

1.3

1312

2789

5.1

26.1

32.3

222

5.1

34.9

60.0

40.9

142

12.0

Class

and

type

L6

L6

L6

L6

H5

H5

LL5

H5

H5

L6

Au

L6

H6

L6

L6

H5

L6

L6

Eu

H4

LL6

Eu

Eu

L3

H4

H4

H5

H6

H6

H6

H5

H4

H5

H5

H6

H6

H5

L6

Iron

C2

Ur

L3

H6

L3

H5

H6

H5

L6

H5

%Fa

in

olivine

24

24

23

24

18

18

28

18

18

25

0

25

18

25

24

19

25

25

18

29

1-34

18

18

18

18

18

18

18

18

18

18

18

18

18

23

0-50

22

6-39

16

10-38

16

18

18

23

17

%Fs

in

pyroxene

20

20

20

20

17

16

23

16

16

20

0

20

16

21

20

17

21

21

40-68

15-20

24

40-68

37-61

5-29

16

16

15

16

15

16

16

16

16

16

15

16

16

20

1-8

19

2-31

18

5-26

14

16

15

19

15

of

weathering

B

B

B

A/B

C

B

A/B

B/C

A

B

A/B

B/C

B

B

B/C

C

B/C

B/C

A

B/C

B /C

A

A

C

B/C

B/C

B/C

B/C

B/C

B/C

B

B

B

B/C

B

B/C

B/C

B

A

A

C

C

B

B/C

B

B/C

A/B

B

Specimen

number

79009

79010

79011

79012

79013

79014

79015

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

BTNA

78001

78002

Weight (g)

75.7

25.1

14.0

192

28.3

10.8

64.0

1146

310

120

12.1

4.2

29.4

31.4

68.1

21.6

1208

572

133

16.2

505

2.7

2.6

208

12.6

37.6

20.2

14.8

49.6

108

13.2

20.1

11.4

62.2

115

89.7

19.3

36.7

54.0

27.0

24.0

22.6

86.0

36.0

15.2

160

4301

Class

and

type

H5

H5

H5

H5

H5

H5

H5

H6

Eu

L6

H6

H6

H5

L3

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

L6

%Fa

in

olivine

18

17

18

17

18

18

17

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

%Fs

in

pyroxene

15

15

16

15

16

16

15

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

21

20

Degree

of

weathering

C

B/C

B/C

C

C

B

B

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

B

B
88 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

TABLE A.—Continued

Specimen

number

78004

DRPA

78001

78002

78003

78004

78005

78006

78007

78008

78009

EETA

79001

79002

79003

79004

79005

79006

79007

79009

79010

79011

META

78001

78002

78003

Weight (g)

1079

15200

7188

144

133

18600

389

11800

59400

138100

7942

2843

435

390

450

716

199

140

287

86.4

624

542

1726

Class

and

type

LL6

Iron

Iron

Iron

Iron

Iron

Iron

Iron

Iron

Iron

Sh

Di

L6

Eu

Eu

Ho

H5

L5

L6

Eu

H4

L6

L6

%Fa

in

olivine

30

23-27

24-25

24

18

24

24

17

23

24

%Fs

in

pyroxene

24

16-67

22

20

30-61

30-61

19-57

16

20

20

30-61

14-21

20

21

Degree

of

weathering

B

A

B

B

B

A

B

B

B

B

B

B/C

B

B

Specimen

number

78005

78006

78007

78010

78028

MBRA

76001

76002

PGPA

77006

RKPA

78001

78002

78003

78004

79001

79002

79003

79004

79008

79009

79012

79013

79014

79015

Weight (g)

172

409

174

233

20657

4108

13773

19068

234

8483

1276

166

3006

203

182

370

73.0

55.0

12.8

11.0

77.7

10022

Class

and

type

L6

H6

H6

H5

L6

H6

H6

Iron

L6

H4

L6

H4

L6

L6

H6

H5

L3

H6

H6

L5

H5

M

%Fa

in

olivine

24

18

19

19

25

18

18

23

18

23

17

24

24

18

18

1-29

18

18

23

18

%Fs

in

pyroxene

20

15

17

17

21

16

16

20

15

20

14-21

20

20

16

16

2-28

16

16

20

16

24

Degree

of

weathering

B

C

B/C

B

B

A

A

C

B

C

A

B

B

B

B/C

B

C

B

B/C

B/C

TABLE B.—Meteorites listed by class and source area in numerical sequence

Specimen

number

ALHA77299

ALHA78084

ALHA77004

ALHA77OO9

ALHA77O1O

ALHA77190

ALHA77191

ALHA77192

ALHA77208

ALHA77221

ALHA77223

ALHA77224

ALHA77225

ALHA77226

ALHA77232

ALHA77233

ALHA77262

ALHA78286

Weight (g)

260

14280

2230

235

295

387

642

845

1733

229

207

786

5878

15323

6494

4087

861

245

Class

and type

ORDINARY

H3

H3

H4

H4

H4

H4

H4

H4

H4

H4

H4

H4

H4

H4

H4

H4

H4

H4

Degree of

weathering

CHONDRITES

A

B/C

C

C

C

C

C

C

C

C

C

C

C

c

c

c

B

C

Degree of

fracturing

A

B

C

A

A

C

B

C

C

A

C

C

C

c

c

B

B

B
NUMBE

R 24

89

TABLE B.—Continued

Specimen

number

ALHA78053

ALHA78O77

ALHA78134

META 78001

RKPA78OO2

RKPA78004

ALHA79O23

ALHA79039

ALHA79O35

ALHA78193

ALHA78196

ALHA78223

ALHA77O12

ALHA77014

ALHA77O21

ALHA77O25

ALHA77061

ALHA77062

ALHA77064

ALHA77O71

ALHA77O74

ALHA77086

ALHA77O88

ALHA771O2

ALHA77118

ALHA77119

ALHA77124

ALHA77177

ALHA77182

ALHA77259

ALHA77264

ALHA77268

ALHA77274

ALHA77287

ALHA77294

ALHA773OO

ALHA78O75

ALHA78085

ALHA78102

ALHA78107

ALHA78108

ALHA78110

ALHA78128

META 78010

ALHA79004

ALHA79006

ALHA79008

ALHA79009

ALHA79010

ALHA79011

ALHA79O12

ALHA79O13

ALHA79014

ALHA79015

ALHA79O21

ALHA79025

ALHA79026

ALHA79029

ALHA79031

ALHA79036

ALHA79038

Weight (g)

179

330

458

624

8483

166

68.1

108

37.6

13.3

11.1

6.4

180

308

16.6

19.4

12.4

16.7

6.4

10.8

12.0

19.4

51.1

12.2

7.8

6.3

4.4

368

1134

294

10.9

272

288

230

1351

234

280

219

336

198

172

160

154

233

34.9

40.9

12.0

75.7

25.1

14.0

191

28.3

10.8

64.0

29.4

1208

572

505

2.7

20.2

49.6

Class

and type H4 H4 H4 H4 H4 H4 H4 H4 H4 H4 H4 H4 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 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 CC

B/C

B/CBA

B/CBB

B/C

B/CBCCCCBBBBBCCBCCCCBC

A/BCCCAC

B/CB

B/CCB

B/CCB

B/C

B/CBC

B/C

B/CCCBBBCBCCBC

Degree of

fracturing BBBBAACBBABBABABABBBBBBBBBAABBACAAABBBBABBBABBBABABBABAABBBBB
90 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

TABLE B.—Continued

Specimen

number

ALHA79040

ALHA79041

ALHA79042

ALHA79046

ALHA79047

ALHA79048

ALHA79050

ALHA79051

ALHA79053

ALHA79054

EETA79007

RKPA79004

RKPA79014

ALHA79O32

ALHA78209

ALHA78221

ALHA78225

ALHA78227

ALHA78233

ALHA76006

ALHA76008

MBRA76001

ALHA77144

ALHA77148

ALHA77183

ALHA77258

ALHA77271

ALHA77285

ALHA77288

ALHA78076

ALHA78115

META78006

META78OO7

ALHA79002

ALHA79005

ALHA79016

ALHA79019

ALHA79020

ALHA79024

ALHA79028

ALHA79O37

ALHA79049

ALHA79055

RKPA79003

RKPA79009

RKPA79012

ALHA79034

ALHA78211

ALHA78213

ALHA78215

ALHA78229

ALHA78231

ALHA77081

ALHA77O11

ALHA77O15

ALHA77033

ALHA77140

ALHA7716O

ALHA77164

ALHA77165

Weight (g)

13.2

20.1

11.4

89.7

19.3

36.7

27.0

24.0

86.0

36.0

199

370

77.7

2.6

12.1

5.3

4.5

2.4

1.3

271

281

1096

7.8

13.1

288

597

609

271

1880

275

847

409

174

222

60.0

1146

12.1

4.2

21.6

16.2

14.8

54.0

15.2

182

55.0

12.8

12.6

11.4

9.5

6.3

1.9

1.8

8.5

291

411

9.3

78.6

70.4

38.1

30.5

Class

and type

H5

H5

H5

H5

H5

H5

H5

H5

H5

H5

H5

H5

H5

H5

H5

H5

H5

H5

H5

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?

L3

L3

L3

L3

L3

L3

L3

Degree of

weathering

B

B

B

B

B

B

C

C

B/C

B

B

B/C

B/C

C

B/C

B

B

B/C

B/C

C

B/C

B/C

B

C

C

B/C

C

c

B

B

B

C

B/C

C

B

B/C

B

B/C

C

B

B

C

B/C

B

C

B

B

B

B

B/C

B

B/C

B

C

C

C

C

C

C

C

Degree of

fracturing

A

B

A

B

B

B

B

A

B

A

B

B

B

B

B

A

A

B

B

B

B

B

A

B

A

A

A

B

B

B

A

B

B

B

B

B

A

B

B

B

B

B

B

A

B

B

A

B

B

B

B

B

A

A

B

B

B

B

C

C
NUMBER 24

91

TABLE B.—Continued

Specimen

number

ALHA77167

ALHA77214

ALHA77215

ALHA77216

ALHA77217

ALHA77249

ALHA77252

ALHA7726O

ALHA78038

ALHA79001

ALHA79003

ALHA 79022

ALHA79045

RKPA79008

ALHA 78188

ALHA77230

ALHA77OO2

ALHA77254

EETA79009

RKPA79013

ALHA76OO7

ALHA76009

ALHA77OO1

ALHA7715O

ALHA77155

ALHA7718O

ALHA77231

ALHA77261

ALHA77269

ALHA7727O

ALHA77272

ALHA77273

ALHA77277

ALHA7728O

ALHA77281

ALHA77282

ALHA77284

ALHA77292

ALHA77296

ALHA77297

ALHA77305

ALHA 78039

ALHA78042

ALHA78043

ALHA78045

ALHA78048

ALHA 78050

ALHA78O74

ALHA78078

ALHA78103

ALHA78104

ALHA78105

ALHA78106

ALHA78112

ALHA78114

ALHA78126

ALHA78127

ALHA78130

ALHA78131

ALHA78251

Weight (g)

611

2111

819

1470

413

503

343

744

363

32.3

5.1

31.4

115

73.0

0.8

2473

235

245

140

11.0

78.5

3950

252

58.3

305

190

9270

411

1045

588

674

492

142

3226

1231

4127

376

199

963

951

6444

299

214

680

396

190

1045

200

290

589

672

941

464

2485

808

606

194

2733

268

1312

Class

and type L3L3L3L3L3L3L3L3L3L3L3 L3L3L3L3 L4L5L5L5L5L6L6L6L6L6L6L6L6L6L6L6 L6L6L6L6L6L6L6L6L6L6L6L6L6L6L6L6L6L6L6L6L6 L6L6L6L6L6L6L6L6

Degree of

weathering CcB

A/BBCBCCCB

A/BCBCBB

A/BB

B/CBBBC

A/BC

A/BBB

A/B

B/CB

A/BBBB

A/BB

A/BA

B/CBBB

B/C

A/BBB

A/BBBB

A/BB

B/CB

B/C

B/C

B/CB

Degree of

fracturing BCBBBCCCCABBBBBBAABBABBBAAABABBBABBBBAABBBABBBBBABAAABBBBBAA
92 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

TABLE B.—Continued

Specimen

number

BTNA 78001

BTNA78002

META78OO2

META78003

META78005

META78028

RKPA 78001

RKPA78003

ALHA79OO7

ALHA79018

ALHA79027

ALHA 79033

ALHA79043

ALHA79052

EETA79003

EETA79010

RKPA 79001

RKPA79OO2

ALHA76004

ALHA77278

ALHA77304

ALHA78109

ALHA78153

BTNA78004

Subtotals

H3

H4

H5

H6

H?

L3

L4

L5

L6

LL3

LL5

LL6

Total

ALHA77OO3

ALHA77306

ALHA773O7

ALHA 78261

Total

ALHA78113

ALHA77256

EETA 79002

ALHA78006

EETA79006

Weight (g)

160

4301

542

1726

172

20657

234

1276

142

120

133

208

62.2

22.6

435

287

3006

203

52.5

312

650

233

151

1079

14,571

50,969

10,550

8,883

8.5

8,536

2,473

632

83,062

1,014

233

1,230

182,161

779

19.9

181.3

5.1

985.3

298

676

2843

8.0

716

Class

and type

L6

L6

L6

L6

L6

L6

L6

L6

L6

L6

L6

L6

L6

L6

L6

L6

L6

L6

LL3

LL3

LL3

LL5

LL6

LL6

Degree of

weathering

B

B

B

B

B

B

C

C

A/B

B/C

B

B

C

B/C

B

B

B

B

A

A

B

A/B

B/C

B

CARBONACEOUS CHONDRITES

Carbonaceous C3

Carbonaceous C2

Carbonaceous C3

Carbonaceous C2

ACHONDRITES

Aubrite

Diogenite

Diogenite

Howardite

Howardite

A

A

A

A

A/B

A/B

B

A

B

Degree of

fracturing

B

A

A

B

B

B

B

B

B

A

A

A

B

B

B

C

C

B

A

A

B

A

B

A

A

A

A

A

A

A

B

A

B
NUMBER 24 93

TABLE B.—Continued

Specimen

number

EETA79004

ALHA76005

ALHA773O2

ALHA78040

ALHA78132

ALHA 78158

ALHA 78165

ALHA79017

EETA79005

EETA79011

ALHA77OO5

EETA79OO1

ALHA77257

ALHA78019

ALHA78262

Subtotals

Aubrites

Diogenites

Howardites

Monomict Eucrites

Polymict Eucrites

Shergottites

Ureilites

Total

ALHA 76002

ALHA7725O

ALHA77255

ALHA77263

ALHA77283

ALHA77289

ALHA7729O

PGPA77OO6

ALHA78252

DRPA 78001

DRPA78002

DRPA78003

DRPA78004

DRPA 78005

DRPA78006

DRPA78OO7

DRPA78008

DRPA78009

ALHA 78100

Total

Weight (g)

390

317

235

211

656

15.1

20.9

310

450

86.4

482

7942

1995

30.3

26.1

298

3,519

724

390

2,303

8,424

2,052

17,710

307

10555

765

1669

10510

2186

3784

19068

2789

15200

7188

144

133

18600

389

11800

59400

138100

85.0

302,672

Class

and type

Monomict Eucrite

Polymict Eucrite

Polymict Eucrite

Polymict Eucrite

Polymict Eucrite

Polymict Eucrite

Polymict Eucrite

Polymict Eucrite

Polymict Eucrite

Polymict Eucrite

Shergottite

Shergottite

Ureilite

Ureilite

Ureilite

IRONS

Iron-Group IA or Og

Iron-Group I or Og

Degree of

weathering

B

A

A

A

A

A

A

A

A

B

A

A

A

B/C

A

Iron-Group Anom (D)

Iron-Group I or Og

Iron-Group I or Og

Iron-Group I or Og

Iron-Group I or Og

Iron-Group I or Og

Iron-Group IVA

Iron-Group IIB

Iron-Group IIB

Iron-Group IIB

Iron-Group IIB

Iron-Group IIB

Iron-Group IIB

Iron-Group IIB

Iron-Group IIB

Iron-Group IIB

Iron-Group IIA

Degree of

fracturing

B

A

A

A

A

A

A

A

B

B

A

A

B

C

A
94 SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES

TABLE B.—Continued

Specimen

number

ALHA77219

RKPA79015

Total

ALHA78044

ALHA78111

Total

Weight (g)

637

10022

10659

164

126

290

Class

and type

Degree of

weathering

STONY-IRON

Mesosiderite

Mesosiderite

B

UNCLASSIFIED

B/C

B/C

Degree of

fracturing

B

B

A

TABLE C.—Meteorites tentatively identified as paired specimens

Class

Eucrite

L3

L4

L6

H4

H5

H6

Diogenite

Iron, IA/Og

Paired specimens

ALHA 76005, 77302, 78040, 78132, 78158, 78165,

79017

ALHA 77015, 77033, 77034, 77036, 77043, 77047,

77049, 77050, 77052, 77140, 77162, 77167,

77170, 77178, 77214

ALHA 77160, 77164, 77165, 77249, 77260

ALHA 77033, 77214

ALHA 79001, 79003

ALHA 77215, 77216, 77217

ALHA 77270, 77277, 77284

ALHA 77001, 77296, 77297

ALHA 77001, 77296, 77297

ALHA 77150, 77305

ALHA 77231, 77272, 77273, 77280

BTNA 78002 (2 stones)

RKPA 78001, 78003, 79001, 79002

ALHA 77004, 77191, 77192, 77208, 77224, 77233

ALHA 77014, 77264

ALHA 77021, 77061, 77062, 77064, 77071, 77086,

77088, 77102

ALHA 77118, 77119, 77124

RKPA 79004 (6 stones)

ALHA 77144, 77148

ALHA 77271, 77288

Yamato 6902 (b), Yamato 74010, 74011, 74037,

74097, 74136, 74648

ALHA 76002, 77250, 77263, 77289, 77290

DRPA 78001, 78002, 78003, 78004, 78005, 78006,

78007, 78008, 78009

Reference

Score et al. (this volume)

McKinley et al. (1981)

Paired with ALHA 77015 group on evidence in King et al. (1980:18, 42)

Separately paired by King et al.

(1980:42)

Score et al. (this volume)

King et al. (1980)

King et al. (1980)

Kinget al. (1980)

King et al. (1980)

King et al. (1980)

King et al. (1980)

Score et al. (this volume)

Score et al. (this volume)

King et al. (1980)

King et al. (1980)

Kinget al. (1980)

Kinget al. (1980)

Score et al. (this volume)

Kinget al. (1980)

King et al. (1980)

Takeda, Miyamoto, Yanai, Haramura

(1978)

Clarke (this volume)

Clarke (this volume)
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