LUNAR NEWS

In This Issue:

Editor's Notes 2

Curatorial Phone Numbers 2

New Assignments

Curator's Comments 3

Magma Ocean Workshop 3

Lunar Meteorites

Samples of Lunar Core 6001 416001 3 are Available

Accessing Databases 15

1990- 199 1 was a time of change for the JSC Solar System Exploration Division. In February 199 1, Mike Duke announced he was leaving the division to take on the job of Science Manager in the Lunar and Mars Exploration Program Office which is located at JSC. Mike has long been a leading voice in the quest to return to the Moon and to explore Mars. His new position engages that task head-on and is responsible for maintaining a high science content

Doug Blanchard is now the Division Chief. Doug was the Lunar Sample Curator from 1981 to 1988 and the Chief of the Planetary Science Bmch fiom 1988 to 1990. The division is in excellent condition and Doug expects no change in the intense level of curation and planetary and space science research.

Gordon McKay has taken over the reins of the Planetary Science Branch. Gordon brings a very strong background of research in planetary geochemistry and experience as the manager of the electron microprobe lab and as the technical manager of the Lockheed support contract.

continued on page 3

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2 Lunar News

Curator 3 Comments By Jlm Goodlng NASAIJSC

One Curator Retires While Another Aspires

Dr. John W. Dietrich retired from NASA service on December 31,199 1 after a successful career in lunar and planetary science. John's 25-year career at Johnson Space Center began in 1966 with support for the Apollo program, first as a photogeologist mapping the Moon with Lunar Orbiter data and then as an instructor in the geological training program for astronauts who were to explore the lunar surface. After helping guide the Apollo missions to the Moon, John worked in the Earth Observations Division using data from a variety of space-based sensors, including LANDSAT. In 1981, he moved to the Solar System Exploration Division and joined the lunar sample curation effort. After accepting increasingly substantial responsibilities for lunar sample curation, John was appointed Lunar Sample Curator, and Deputy Chief of the Planetary Science Branch, in 1988. Thus, John's NASA career achieved poetic completion as he supervised distribution of samples from the same rocks that his mapping and coaching had helped to collect. We bid John a fond farewell and confess to being envious of his new freedom to return to the geology and scenery of Texas which he knows and loves so well.

I am honored by my appointment to succeed John Dietrich and I am committed to sustaining the planetary materials curation efforts for which our organization is well known. In my ten years at JSC, I have served separately as Associate Curator of Cosmic Dust and as Associate Curator of Meteorites, while remaining actively involved in planetary materials research. More recently, I have acted as Contamination Control Officer for the Cosmic Dust Laboratory although much of my time has been spent helping NASA plan possible future Mars exploration projects, including Mars sample return. Therefore, I understand and endorse the importance of high-quality curation of planetary samples while also enjoying a forward-looking perspective on new opportunities. Our lunar curatorial team would be delighted to someday receive and curate new samples from the Moon. Until then, we remain devoted to the Apollo lunar samples and to providing the best possible support for the scientists who study them. The Curator may be new, but our quest for excellence has not changed.

Dr. John Dietrich

New Assignments continued from page 2

John Dietrich, who replaced Doug as Lunar Sample Curator in 1988, served through 1991 then passed the baton to Jim Gooding (see "Curator's Comments, this page). The curatorial team has moved Chuck Meyer to lab manager for the Lunar Processing Labs. David Lindstrom has taken on the duties of the Contamination Control Officer. Marilyn Lindstrom and Mike Zolensky continue to curate the Antarctic Meteorite and Cosmic Dust collections, respectively.

Magma Ocean Workshop By John Longhi Larnont-Doherty Geological Observatory

Some 58 planetary scientists from Japan, Canada, Russia, Czechoslovakia, and the U.S. participated in the LPI-LPSAT sponsored workshop on The Physics and Chemistry of Magma Oceans held in Burlingame, CA from December 6 through 8. Keynote speakers began each of the formal sessions and were followed by several contributed talks. Keynote addresses included: Evidence For and Against Magma Oceans (G J. Taylor), Phase Equilibria (C. Agee), Dynamics and Evolution @.J. Stevenson), Mechanisms of Formation (W. Kaula), and Geophysical Conse- quences (G. Shubert).

There were lively discussions in all of the sessions with most of the emphasis on the characteristics of a terrestrial magma ocean, although lunar, martian, and asteroidal magma oceans were not

continued on page 4

Lunar News 3

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in Geochimica, and in the Proceed- ings of the Symposium on Antarctic Meteorites, No. 4 (1991). The first non-Antarctic lunar meteorite was discovered in southwestern Australia, apparently sometime in the 1960's.

The great value of the lunar meteorites stems frcrn the possibility th?.t thew represent otherwise unv-%:;led regions of the Moon, but the @~?mber of such regions depends on whether each meteorite represents a separate source crater. Some of the high- lands meteorites are obviously paired with one another, in the traditional sense of having struck the Earth as part of a single shower (Table 1). Thus, the number of distinct lunar meteorites is not twelve but nine or less. To check for less obvious source-crater pairing, isotopic clocks sensitive to cosmic-ray exposure can be used to constrain the ages of the cratering events responsible for blasting the samples to the Earth. Exposure ages have thus far been obtained for five lunar meteorites: all four of the distinct highlands meteorites plus EET8752 1 (these data are

gathered by 0. Eugster at Bern and K. Nishiizumi at San Diego, among others). The results reveal that at least two separate source craters, and more likely 3-5, are repre- sented by this group.

Most (arguably d) of the four highlands meteorites are regolith breccias, which is fortunate in the sense that it implies they formed by thorough mixing of the crust surrounding their locations of origin. In terms of mineralogy, petrography, and major-element geochemistry, the highlands meteorites have basically con- f m e d the 1970s assumption that the anorthositic Apollo 16 site is representative of the highlands surface crust. Volatile and labile trace metal concentrations are also generally similar. For other trace elements, however, the meteorites indicate that the Apollo 16 site is highly unrepresentative. The highlands meteorites tend to have far lower contents of REE and other incompatible elements. The highlands meteorites also tend to have far lower siderophile-element contents, and less fractionated (relatively low, more nearly

chondritic) N i b and Au/lr ratios. Also, among the many clasts found in these breccias are a few that appear "pristine" (i.e., they retain bulk compositions, although not necessarily textures, unaffected by impact-mixing). Several of these pristine clasts are geochemically unique, and thus add important new constraints for models of lunar crustal evolution.

Lunar meteorites composed dominantly of mare material have suddenly become relatively common. In late 1989, data for FelMn, Ga/Al, Co/Cr, etc., revealed the lunar affinity of EET87521, which had been classified as a eucrite. Two other mare meteorites were found by K. Yanai and H. Kojima at Tokyo, and the Y -793274 meteorite once classified as highlands was shown from numerous detailed studies to consist of a mixture of highlands and mare materials, mainly the latter. Compared to mare samples from the nine Apollo/Luna sites, the mare meteorites all have uncommonly low Ti contents. At least two, and arguably all four, are dominantly composed of hitherto-

continued on page 6

Table 1. Summary of Known Lunar Meteorites, as of End of 1991

Mas% Rock Season Year Shown Meteorite grams Type Collected to be Lunar

723.7 Highlands @aired) Highlands

Yamato-82192 total Yamato-82193 712.1 Yamato-86032 @aired)

Highlands Highlands Highlands

Asuka-3 1 442.1 Mare gabbro 88-89 90

Yamato-791197 52.4 Highlands 79-80 83

ALHA8 1005 31.4 Highlands 81-82 82

EET87521 30.7 Mare breccia 87-88 89

Calcalong Creek, Australia 19 KREEP breccia ? 91

Yamato-793274 8.7 Mare-highlands breccia 79-80 ' 87

Yamato-793 169 6.1 Mare basalt 79-80 90

Lunar News 5

Lunar Meteorites continued from page 5

rare "very-low-Ti" (VLT) mare basalt. Also, mare-type clasts found within several highlands meteorites typically have pyroxene composi- tions that imply VLT affmity. These mends suggest that the global average Ti content for mare basalts is considerabl? Swer than previ- ously supposed. Alm, VLT-mare materials are ~ h t i v e l y close in composition to some types of nonmare Mg-gabbronorites. Thus, the abundance of VLT meteorites suggests that the dichotomy of lunar magmatic events into mare and nonmare types was less abrupt than previously envisaged.

These are just a few of the important lunar-science implica- tions of these meteorites. As the total number of collected meteor- ites continues to grow, we can be sure that additional lunar rocks will be among them, at a rate of roughly one per thousand. Although the exact locale of origin of any individual lunar meteorite cannot be determined, collectively these samples afford a vastly improved coverage of the compositional- petrologic characteristics of the total lunar surface. Improved coverage is necessary because, as the lunar meteorites have under- scored, the Moon's upper crust is in some respects remarkably hetero- geneous. Many key models relatable to the Moon's crust (e.g., origin of the Earth-Moon system, the magmasphere hypothesis) are to a high degree testable through further investigations of lunar meteorites.

6 Lunar News

Samples of Lunar Core 6001 416001 3 Are Available By Carol Schwarz Lockheed Engineering & Sciences Company

Dissection of both segments of the Apollo 16 double drive tube 60014160013 has been completed. The core was dissected in 0.5 cm depth increments along three 1 cm thick longitudinal layers (passes), starting at the lunar surface and continuing through the length, 61.9 cm, of the core. (The length of 60014 is 28.2 cm and 60013 is 33.7 cm.) Soil from each incre- ment of the fust and third passes was separated into coarse and fine fractions using a 1 cm sieve. The coarse particles were examined under a binocular microscope, classified (as much as possible), and photodocumented. All samples are now available for study. Thin sections of 60014 are available now and those of 600 13 are being prepared and will be available soon.

This core sample was taken in April 1972 at Station lo', about 75 m west-southwest of the LM (Lunar Module) at the Descartes landing site in the Central High- lands. Three cores were taken near the LM in a triangular pattern; 60010/60009 and 60014160013, both double drive tubes; and 60007-60001, a deep drill string. The material sampled by the 60014/60013 core is believed to be South Ray Crater Ejecta.

Core 60014 was extruded from the drive tube on October 26,1990. The color was determined to be approximately lOYR 511 on the Munsell color scale and no distinct color boundaries were observed

during dissection. After the dissections and peel were com- pleted, no boundaries were evident except for a very subtle darkening in a wedge-shaped area extending across the width of the core approximately 3 to 7 cm from the top. Noticeable textural variations were observed while dissecting. The upper 5 cm was loose and followed by a more coherent zone from 6 to 13 cm. From 13 to 19 cm the core became loose once again, grading into a coarse-grained layer at 21 cm and continuing to about 22.5 cm. In this interval were a large number of 4-10 mm particles, mostly soil breccias. The remain- der of the core-- from 23 cm on- was similar to the coherent 6 to 13 cm zone.

A close examination of the >1 mm fraction showed that about 80% (by number) of the particles were in the 1-2 mm size range, 19% were 2-4 mm, 1 % were 4-10 mm, and less than 1% were >10 mm.

The lithology of the >1 mm fraction was determined by binocular examination of the particles and is summarized as follows: 17% of the particles were white or light gray, 15% were dark and coherent, 13% were glasses, and 55% were breccias. The white or light gray particles included plagioclase, anorthositic breccias, crystalling anorthosite, and light gray basalts, and were distributed evenly throughout the core. The dark particles were fine-grained,

Carol Schwarz, scraping a layer off of the lunar core sample 60014. NASA Photo # S91-26935

coherent, and often dusty. The glasses consisted of 68% aggluti- nates, 3% shards, 2% spheres (usually not much larger than 1 mm), and 27% miscellaneous glass fragments. Finally, the breccias included soil breccias, soil breccias with glass, dark matrix breccias, light matrix breccias, and those breccias too dusty to identify. The eleven particles at least 1 cm in diameter which were given

individual split numbers included 5 breccias, 2 anorthosites, 2 basalts, 1 agglutinate and 1 of unknown classification.

Core 600 13 was extruded on June 19, 1991. A distinct color boundary was observed in the core approximately 18 cm from the top. The upper 18 cm was dark, lOYR 5/1 on the Munsell color scale. Below about 18 cm the color was lighter, lOYR 611. Approximately

3 cm above the 18 cm boundary (at 15 cm from the top of 60013) marked the beginning of a zone characterized by numerous large friable soil breccias. Below about 18 cm the number and size of soil breccias decreased abruptly. Near the bottom, at a depth of about 3 1.5 cm, a less obvious darkening was observed. It was irregular and varied with each successive pass. The peel exposed a light-colored zone between 16 and 17 cm with numerous 1-2 mm particles across about half the diameter of the coie.

A close examination of the >1 mm particles showed that about 75% are in the 1-2 mm size range, 23% are 2-4 mm, 1% are4-10 mm, and ~ 1 % are >10 mm.

The lithology of the >1 mm fraction was determined by binocular examination of the particles and is summarized as follows: 55% were breccias, either soil breccias or miscellaneous breccias. About 13% are white and light gray fragments (plagioclase crystals or anorthositic breccias). About 18% of the >1 mm particles are black, fine-grained, coherent, dust-covered particles. Basalts comprise 2% of the >1 mm particles, and about 12% of the particles are glasses, including agglutinates, shards, spheres, and breccias with glass splashes. Among the 21 particles > 10 mm in diameter which were given individual split numbers, include 1 anorthosite, 6 breccias, 11 soil breccias, 1 agglutinate, and 1 possible oblong glass object.

The diagrams which follow illustrate the three dissection passes for each core segment and identify sample splits which are available for allocation. Is/FeO data was provided by Dick Monis.

Lunar News 7

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Lunar News 9

2- d.5

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10 Lunar News

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Soil Breccia Soil Clod Lunar News 13

20 40 Depth in Core 6001 311 4 (cm)

- Figure 1 %f 60014 60013 - =PI

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Special Section of JGR-Planets: Magma Oceans

Many participants at the recent, highly successful LPI- LAPST sponsored workshop on The Physics and Chemis- try of Magma Oceans (see page 3 of this newsletter) expressed interest in contrib- uting to a special issue of a journal. JGR-Planets editor Clark Chapman is enthusias- tic about devoting a portion

of a Fall issue of JGR-Planets to this interesting topic. Papers need to be submitted to him by mid-May, 1992. Jeff Taylor, Associate Editor, will coordinate the review process. Address questions to Jeff: (808) 956-3899; gjtayloI@esther.pgdhawaii.edu; NASAmail: jefftaylor.

Lunar News 14