Comparison of elemental abundances in sun, meteorites and earth

provides understanding of the formation and evolution of the solar

system. Yet, the majority of the solar system abundances are based on

meteoritic values [1–6]. Here we report an attempt to estimate a feasibility

of direct measurements of iodine and bromine in the GENESIS solar

wind Aluminum on Sapphire collector (AloS) using neutron induced

conversions: ^(127)I(n,γβ)^(128)Xe, ^(79)Br(n,γβ)^(80)Kr and ^(81)Br(n,γβ)^(82)Kr

Beckett, J. R.

Connolly, H. C., Jr.

Huss, G. R.

Ma, C.

Nagashima, K.

Rossman, George R.

Young, E. D.

Ziegler, K.

Calcium-, aluminum-rich inclusions (CAIs) are the first rocks to form in the solar system. Some inclusions are igneous and a very few of these (called F inclusions) experienced significant mass dependant fractionation in oxygen [1], and in some cases, other isotopic systems

(FUN inclusions). Increasing the number and types of F inclusions will provide additional constraints on CAI formation and their formation environments. We report here on a Compact Type A (CTA) inclusion from Allende with an overall snake-like morphology, is an F inclusion,

and initial ^(26)Al/^(27)Al that was canonical

Caltech Authors - Main

5313
ALLENDE 3509 HC-2: A COMPACT TYPE A—‘F’ INCLUSION
WITH A SNAKE-LIKE MORPHOLOGY
H. C. Connolly Jr.1,2,3, J. R. Beckett4, G. R. Huss5, K. Nagashima5, E.
D. Young6, K. Ziegler6, C. Ma4 and G. R. Rossman4. 1Dept. Physical
Sci., Kingsborough Community College of CUNY, Brooklyn NY 11235
& Dept. Earth & Envir. Sci., The Graduate Center of CUNY, New York,
NY 10016, USA. 2Dept. Earth & Planet. Sci., AMNH, New York, NY
10024, USA. 3LPL, Univ. of Arizona, Tucson, AZ 85721, USA. 4Div. of
Geol. & Planet. Sci., Caltech, Pasadena, CA 91125, USA. 5Hawai’i
Institute of Geophysics & Planetology, Univ. of Hawai’i at Ma˜noa,
Honolulu, HI 96822, USA. 6Dept. of Earth & Space Sci., UCLA, Los
Angeles, CA 90095, USA. E-mail: chondrule@haroldconnolly.com.
Introduction: Calcium-, aluminum-rich inclusions (CAIs) are the ﬁrst
rocks to form in the solar system. Some inclusions are igneous and a very
few of these (called F inclusions) experienced signiﬁcant mass dependant
fractionation in oxygen [1], and in some cases, other isotopic systems
(FUN inclusions). Increasing the number and types of F inclusions will
provide additional constraints on CAI formation and their formation
environments. We report here on a Compact Type A (CTA) inclusion
from Allende with an overall snake-like morphology, is an F inclusion,
and initial 26Al/27Al that was canonical.
Analytical Methods: The entire inclusion, HC-2, was recovered from
a slab of Allende 3509 (USNM). Major and minor element abundances
were determined with the Cameca SX-50 at the LPL UAz. Oxygen
isotopes and Al-Mg isotopic systematics were analyzed for on the Cameca
1280 ion microprobe at the Univ. of Hawai’i, Ma˜noa [2]. Si isotopes were
analyzed by LA-MC-ICPMS at UCLA.
Results: HC-2 has an overall morphology that is snake-like,
wrapping throughout a 1.5 cm thick (total width is approximately
0.75 cm) section of the meteorite, inspiring it to be nicknamed The Snake.
It has a Wark-Lovering rim on both sides, although the rim is thicker on
one side. The inclusion has experienced some brittle deformation. HC-2 is
dominated by spinel (Ti = 0.14–0.37; V = 0.44–0.64; Cr = 0.08–0.14; all
wt%) and melilite (Ak = approximate 4 to approximate 50). Perovskites
are numerous, ranging in size from sub-micron to approximately 0.5 mm.
There appear to be two smaller (approximately 400 lm) CAIs that are
mineralogically layered included.
SIMS analysis on spinel and melilite yield an isochron with an
initial 26Al/27Al of (4.9 ± 0.2) · 10)5. A´Aˆ25Mg (variations from the
standard in stable Mg isotope) range from approximately 5 to 13&.
Oxygen isotopes: Melilites have d18O- d17O- values that span
approximately 10& and plot on the CCAM line near the TF line. Two
perovskite grains are isotopically diﬀerent with d18O, d17O of (in &)
approximately )28, )31 in one and )40, )44 in the other. Overall, the
spinels are 16O-rich and show a clear mass fractionation of 4& amu)1,
(d18O = )34 to )42&; d17O = )41 to –45&) with the overall trend to
the right of the CCAM line.
Conclusion: HC-2 is clearly igneous. The reason for its unusual
shape is not clear, but it must have formed while plastic. Based on the
stable isotope data, HC-2 experienced considerable mass-dependent
isotopic fractionation, most likely while molten and while 26Al was
present. We will compare our data to other ‘F’ inclusions to place new
constraints on CAI formation and the environment in which they formed.
References: [1] Bullock E. S. et al. 2011. Abstract #2312. 42nd
Lunar and Planetary Science Conference. [2] Kentaro et al. 2009.
Geochimica et Cosmochimica Acta. [3] Shahara and Young. 2009. Earth
and Planetary Science Letters.
5054
MAJOR AND TRACE ELEMENTS AND OXYGEN ISOTOPES IN
DIFFERENTIATED COSMIC SPHERULES RELATED TO VESTA-
LIKE ASTEROIDS
C. Cordier1, L. Folco1, C. Suavet1, P. Rochette2 and C.
Sonzogni2. 1MNA, Siena, Italy. E-mail: cordier@unisi.it. 2CEREGE,
Aix-en-Provence, France.
Cosmic spherules (CSs) are extraterrestrial particles <2 mm in size,
captured by the Earth’s gravitational ﬁeld and melted during atmospheric
entry. Generally, CSs have geochemical aﬃnities with chondritic material
[1]. The ongoing investigation of large and unbiased collections of CSs
from the South Pole Water Well and the Transantarctic Mountains
(TAM) have, however, led to the identiﬁcation of new types, including
nine diﬀerentiated CSs [2, 3]. Here, we deﬁne the geochemical
characteristics of this new type of CSs from the TAM collection [4] in
terms of major (n = 11, EPMA), trace element (n = 6, LA-ICP-MS) and
oxygen isotope (n = 15, IRMS) compositions.
The 11 diﬀerentiated CSs have high Fe/Mg ratios (0.6–1.6) and
homogeneous Fe/Mn ratios (31 ± 4). Oxygen isotope compositions
(d18O = 14.37% to 20.12 % and D17O = )0.47% to )0.65%) suggest a
Vesta-like parent body. Systematic variations in refractory major and
trace elements result from diﬀerences of the mineralogy of the spherule
precursors. Type-1 spherules (n = 4) are akin to bulk eucrites, with high
CaO and Al2O3 contents, ﬂat REE patterns and high REE contents (La/
YbN = 0.4 to 1.0, REEN = 8.5 to 14 · CI). They derive from ﬁne-
grained precursors with typical eucritic mineralogy. Type-2 spherules
(n = 4) have lower CaO and Al2O3 contents, higher MgO, FeO, and Sc
contents, and strong LREE depletions (La/YbN < 0.2) relative to
eucrites. These compositions suggest large amounts of pigeonite in their
precursors. Type-3 spherules (n = 2) have ﬂat REE patterns with
chondritic REE abundances (REEN = 1.5 to 2.2 · CI), and are enriched
in Co (>50 lg g)1) and Ni (>17 lg g)1) relative to eucrites. Their
composition suggests they derive from howardite-like precursors rich in
orthopyroxene. The mineralogies proposed for the diﬀerentiated
precursors are consistent with those expected for micrometeoroids
deriving from the regolith of Vesta-like asteroids [5].
The combination of elemental and isotopic data shows that the
elemental ratios and contents (Fe/Mg and Fe/Mn, REEs, Ni and Co, V,
Zn) previously proposed to identify the diﬀerentiated CSs and their
parent body [3] are suitable, provided that the mineralogical control is
understood. Diﬀerentiated CSs deriving from pigeonite-rich precursors
(Type 2) tend to have slightly lower Fe/Mg and Fe/Mn ratios and higher
V contents than basaltic eucrites, whereas large amount of opx in
spherule precursor may result in lower Fe/Mg and higher Ni and Co
contents.
The relative frequency of Vesta-like micrometeorites in the TAM
micrometeorite collection (1.6%) is consistent with the proportion
amongst meteorites of eucrites and howardites (1.8%), which are the
main constituents of the regoliths of Vesta-like asteroids.
Acknowledgments: This work was supported by the PNRA and by
the EU-funded ORIGINS Marie Curie Action.
References: [1] Engrand C. and Maurette M. 1998. Meteoritics &
Planetary Science 33:565–580. [2] Taylor S. et al. 2007. Meteoritics &
Planetary Science 42:155–304. [3] Cordier et al. 2011. Geochimica et
Cosmochimica Acta 75:1199–1215. [4] Rochette P. et al. 2008. Proceedings
of the National Academy of Sciences 105:18206–18211. [5] Burbine T. H.
et al. 2009. Meteoritics & Planetary Science 44:1331–1341.
74th Annual Meeting of the Meteoritical Society: Abstracts A47


Allende 3509 HC-2:  A Compact Type A-‘F’ Inclusion with a Snake-Like Morphology

In condensation calculations for a cooling gas of solar

composition, or dust enriched variants, melilite is invariably the earliest

condensing silicate except at very high dust-to-gas ratios [e.g., 1]. The

possibility that silicates of the highly refractory lithophiles, such as Sc and

Zr, actually form first is not tested because of a lack of thermodynamic

data. Meteoritic occurrences may, therefore, provide the best clues to the

earliest evolution of Si in nebular solids. During a nano-mineralogy

investigation of the Murchison CM2 carbonaceous chondrite, we

identified thortveitite (Sc_2Si_2O_7), along with davisite (CaScAlSiO6),

panguite [(Ti,Sc,Al,Mg)_(1.8)O_3], spinel, and Sc-rich diopside, in the

Sc-enriched ultrarefractory inclusion MUR1. This is the first meteoritic

occurrence of thortveitite and the second natural occurrence of panguite,

a Ti-rich oxide recently discovered in Allende [2]. Field-emission SEM

with EDS, electron back-scatter diffraction, and electron microprobe were

used to characterize the compositions and structures of these two minerals

and associated phases

Ma, Chi

Beckett, John R.

Tschauner, Oliver

5169
DISCOVERY OF METEORITIC LAKARGIITE (CaZrO3), A NEW
ULTRAREFRCTORY MINERAL FROM THE ACFER 094
CARBONACEOUS CHONDRITE
Chi Ma. Division of Geological and Planetary Sciences, California
Institute of Technology, Pasadena, CA 91125, USA. E-mail:
chi@gps.caltech.edu
Introduction: During a nano-mineralogy investigation of the Acfer
094 carbonaceous chondrite, lakargiite (CaZrO3) was identiﬁed as
submicrometer inclusions in an isolated hibonite grain in section USNM
7233-1. The hibonite grain is described in Simon and Grossman [1].
Lakargiite is a recently found perovskite-group mineral from high-
temperature skarns in ignimbrites of the Upper-Chegem volcanic
structure, the North Caucasus, Russia [2]. Reported here is the ﬁrst
extraterrestrial occurrence of lakargiite, as a new ultrarefractory mineral
in a primitive meteorite, among the ﬁrst solids formed in the solar system.
Field-emission SEM with EDS and electron back-scatter diﬀraction
(EBSD) was used to characterize its composition and structure and
associated phases.
Occurrence, Chemistry, and Crystallography: Lakargiite [Ca0.95(Zr0.87
Ti0.16)O3] occurs along with tazheranite [(Zr0.52Ti0.18Ca0.16Y0.06Fe0.05
Sc0.03)O1.75], Zr-bearing perovskite [Ca0.94 (Ti0.98Zr0.06)O3] and Os-W-alloy
[Os0.81W0.13Fe0.06] as ﬁne-inclusions scattered in the central area of the
hibonite [Ca (Al11.70Ti0.14Fe0.10Mg0.06)O19] grain (Fig. 1). Lakargiite
appears as irregular or subhedral lath-shaped grains, 300–900 nm in size,
sometimes in contact with Os-W or perovskite. Associated tazheranite is a
Ca-stabilized cubic zirconia (CSZ), likely being the ﬁrst reported
meteoritic CSZ. EBSD analysis revealed that the lakargiite has a
perovskite Pbnm structure, identical to that of synthetic CaZrO3 [3],
showing a = 5.591 A˚, b = 5.762 A˚, c = 8.017 A˚, V = 258.3 A˚3, Z = 4.
Origin and Signiﬁcance: Lakargiite is a new Zr-dominant
ultrarefractory mineral, joining the Zr-rich refractory minerals allendeite
(Sc4Zr3O12) [4], tazheranite (Sc- or Y- stabilized cubic zirconia) [4, 5] and
panguite [6]. Texturally, lakargiite, tazheranite, Zr-bearing perovskite and
Os-W formed before host hibonite. Lakargiite is likely an early
condensate. Further work is under way to determine its place in the
nebula.
References: [1] Simon S. B. and Grossman L. 2011. Meteoritics &
Planetary Science, in press. [2] Galuskin E. V. et al. 2008. American
Mineralogist 93:1903–1910. [3] Koopmanns H. J. A. et al. 1983. Acta
Crystallographica Section C 39:1323–1325. [4] Ma C. et al. 2009. Abstract
#1402. 40th Lunar and Planetary Science Conference. [5] Ma C. and
Rossman G. R. 2008. Geochimica et Cosmochimica Acta 72:12S, A577. [6]
Ma C. et al. 2011. Abstract #1276. 42nd Lunar and Planetary Science
Conference.
Fig 1. BSE image showing lakargiite in Acfer 094.
5171
THORTVEITITE (Sc2Si2O7), THE FIRST SOLAR SILICATE?
Chi Ma1, John R. Beckett1, Oliver Tschauner1,2 and George R.
Rossman1. 1Division of Geological and Planetary Sciences, California
Institute of Technology, Pasadena, CA 91125, USA. 2High Pressure
Science and Engineering Center and Department of Geoscience,
University of Nevada, Las Vegas, NV 89154, USA. E-mail:
chi@gps.caltech.edu.
Introduction: In condensation calculations for a cooling gas of solar
composition, or dust enriched variants, melilite is invariably the earliest
condensing silicate except at very high dust-to-gas ratios [e.g., 1]. The
possibility that silicates of the highly refractory lithophiles, such as Sc and
Zr, actually form ﬁrst is not tested because of a lack of thermodynamic
data. Meteoritic occurrences may, therefore, provide the best clues to the
earliest evolution of Si in nebular solids. During a nano-mineralogy
investigation of the Murchison CM2 carbonaceous chondrite, we
identiﬁed thortveitite (Sc2Si2O7), along with davisite (CaScAlSiO6),
panguite [(Ti,Sc,Al,Mg)1.8O3], spinel, and Sc-rich diopside, in the
Sc-enriched ultrarefractory inclusion MUR1. This is the ﬁrst meteoritic
occurrence of thortveitite and the second natural occurrence of panguite,
a Ti-rich oxide recently discovered in Allende [2]. Field-emission SEM
with EDS, electron back-scatter diﬀraction, and electron microprobe were
used to characterize the compositions and structures of these two minerals
and associated phases.
Occurrence, Chemistry, and Crystallography: Thortveitite [(Sc1.60
Zr0.13Ti0.08Mg0.06Y0.04Fe0.04Ca0.02)(Si1.91Ti0.08Al0.01)O7] occurs with
davisite (15 wt% Sc2O3), panguite [(Ti0.71Sc0.40Al0.24 Mg0.14Si0.08Fe0.06
Zr0.05Cr0.05Ca0.05Y0.03)
P
1.82O3], and MgAl-spinel. These phases form
clots that are in 2-D mostly or entirely enclosed in Sc-bearing diopside
(3–8 wt% Sc2O3). There is a step function in composition between
davisites and the diopside where in contact. Panguite appears as irregular
grains, 0.5–2 lm in size, along with ﬁne-grained spinel within davisite or
serpentinized regions, presumably after davisite. The thortveitite is
subhedral, 1.5 · 3.5 lm to 6.5 · 9.0 lm, and is in contact with davisite/
alteration or diopside. Where in contact with davisite, thortveitite often
appears embayed, suggestive of a reaction relationship. Thortveitite
appears to be inclusion free.
Origin and Signiﬁcance: With the discovery of thortveitite, the Sc-,
Zr-rich menagerie in carbonaceous chondrites now includes thortveitite,
panguite, davisite, allendeite (Sc4Zr3O12) [3], tazheranite (Sc- and/or Y-
stabilized cubic zirconia) [3, 4], and lakargiite (CaZrO3) [5]. MUR1
contains three of these Sc-enriched phases, thortveitite, panguite and
davisite. Texturally, thortveitite formed ﬁrst in MUR1, possibly with later
partial reaction with vapor (?) to form davisite + spinel + panguite.
Molar Sc/Zr of MUR1 thortveitite (approximately 12) is intermediate
between davisite (approximately 15) and panguite (approximately 9),
consistent with conservation of Sc/Zr in a reaction between thortveitite
and vapor (source of Ti, Ca, Mg, and Al) to produce
davisite + panguite + spinel. Since Sc/Zr in all of these Sc-, Zr-bearing
phases are much higher than solar (1.2), prior fractionation of a separate
Zr-rich phase may be indicated. Further work is required to determine
MUR1’s place in the nebular framework but, if the thorveitite is an early
condensate, it may well be the ﬁrst silicate and it certainly is more
refractory than melilite. Indeed, davisite, which appears to be a reaction
product of thortveitite in MUR1, may also predate melilite.
References: [1] Ebel D. S. and Grossman L. 2000. Geochimica et
Cosmochimica Acta 64:339–366. [2] Ma C. et al. 2011. Abstract #1276.
42nd Lunar and Planetary Science Conference. [3] Ma C. et al. 2009.
Abstract #1402. 40th Lunar and Planetary Science Conference. [4] Ma C.
and Rossman G. R. 2008. Geochimica et Cosmochimica Acta 72:12S,
A577. [5] Ma C. 2011. 74th Annual Meeeting of the Meteoritical Society.
Abstract #5169.
A144 74th Annual Meeting of the Meteoritical Society: Abstracts


Thortveitite (Sc_2Si_2O_7), the First Solar Silicate?

Magmatic volatiles influence igneous phase equilibria, eruptive behavior, atmospheric composition, and climate. Several lines of evidence suggest that Mars is rich in halogens and S relative to

Earth. However, magmatic volatile abundances and their effects on magmatic processes on Mars are controversial. Here we examine igneous apatites in SNC meteorites as indicators of magmatic volatile abundances

Channon, M. B.

Boyce, J. W.

Stolper, E. M.

Eiler, J. M.

5504
NANOGLOBULE ABUNDANCES IN IOM EXTRACTS:
CORRELATION WITH PARENT BODY PROCESSING
H. G. Changela1,2, R. M Stroud2, B. T. De Gregorio3, L. R. Nittler4,
C. M. O’D. Alexander4 and G. D. Cody4. 1George Washington University,
Department of Physics, Washington, District of Columbia 20052, USA.
2Naval Research Laboratory, 4555 Overlook Ave. SW, Washington,
District of Columbia 20375, USA. E-mail: changela@anvil.nrl.navy.
mil. 3Johnson Space Center, Houston, Texas 77058, USA. 4Carnegie
Institution of Washington, Washington, District of Columbia 20015, USA.
Introduction: Nanoglobules are a form of Insoluble Organic Matter
(IOM) found in chondrites [1], IDPs [2] and Comet 81P/Wild2 [3]. Some
nanoglobules exhibit large 15N and D enrichments relative to solar values,
indicating that they likely originated in the ISM or the outskirts of the
protoplanetary disk [4]. Recent studies of samples from the Tagish Lake
meteorite with varying levels of hydrothermal alteration suggest that
nanoglobule abundance decreases with increasing hydrothermal alteration
[5]. The aim of the present study is to further constrain the morphologies
of IOM from a range of primitive chondrites in order to determine any
correlation between morphology and petrographic grade and chondrite
class.
Methods: We are performing a comprehensive scanning transmission
electron microscopy (STEM) survey of IOM residues prepared by
methods described in [3]. STEM annular dark-ﬁeld (ADF) imaging
surveys were performed with NRL’s JEOL 2200FS on residues from
Murchison (CM2), EET 92042 (CR2) and QUE 97008 (L3). IOM textures
were classiﬁed as either having a ‘globular’ morphology, i.e. spherical,
non-porous regions approximately 50–1000 nm in size; ‘ﬂuﬀy’, i.e. porous
material with ﬁne scale heterogeneity below 50 nm; and ‘dense-irregular’,
i.e. uniformly dense, non-spherical material >50 nm. ADF images were
taken of each chondrite, sampling approximately 100 lm2 of IOM. The
diﬀerent morphologies were manually identiﬁed from the images and
masked using Adobe Photoshop. Area fractions were then obtained using
Image J software. Because some small globules (<100 nm) are diﬃcult to
distinguish from the background of ﬂuﬀy IOM, our results reﬂect a lower
limit on globular abundances.
Results and Discussion: Globular to ﬂuﬀy and dense irregular to
ﬂuﬀy IOM fractions in these chondrites show distinctive variations.
Murchison contains the highest abundance of nanoglobules
(approximately 7%), followed by EET 92042 (approximately 5%) and
then QUE 97008 (approximately 1%). The abundances of dense irregular
IOM fractions are similar for Murchison and EET 92402, but have much
higher abundance (approximately 20% of measured IOM) in QUE 97008.
We will also present new analyses of residues from types 1, 2 and 3 CR
and other chondrites to identify any links between nanoglobule
abundances and petrographic grade. It has been shown that isotopic
enrichment within the IOM is not just localized to globular species, but to
some ‘ﬂuﬀy’ components as well [6]. It is not clear whether some of the
‘dense irregular’ morphologies of IOM contain similar enrichments.
Coordinated analyses of these extracts and in situ IOM studies will enable
us to further constrain the nature of these morphologically distinct
components and how they vary with petrographic grade or chondrite
class.
References: [1] Nakamura-Messenger K. et al. 2006. Science
314:1439–1442. [2] Flynn G. J. et al. 2003. Geochimica et Cosmochimica
Acta 4791–4806. [3] De Gregorio B. T. et al. 2010. Geochimica et
Cosmochimica Acta 74:4454–4470. [4] Alexander C. M. O’D. et al. 2007.
Geochimica et Cosmochimica Acta 71:4380–4403. [5] Herd C. D. K. et al.
2011. Science, in press. [6] De Gregorio et al. 2010. Abstract #2108. 41st
Lunar and Planetary Science Conference.
5401
ABUNDANCES OF Cl, F, H, AND S IN APATITES FROM SNC
METEORITES
M. B. Channon, J. W. Boyce, E. M. Stolper and J. M. Eiler. California
Institute of Technology, Pasadena, CA 91125, USA. E-mail: mchannon@
gps.caltech.edu.
Introduction: Magmatic volatiles inﬂuence igneous phase equi-
libria, eruptive behavior, atmospheric composition, and climate. Several
lines of evidence suggest that Mars is rich in halogens and S relative to
Earth. However, magmatic volatile abundances and their eﬀects on
magmatic processes on Mars are controversial. Here we examine igneous
apatites in SNC meteorites as indicators of magmatic volatile abundances.
Methods: We measured Cl, F, H (reported as wt% H2O), and S in
25 apatites from 3 basaltic shergottites (JaH 479, NWA 856, and NWA
2986), 1 lherzolitic shergottite (NWA 1950), and 1 nakhlite (NWA 998)
using Caltech’s 7f SIMS. We compared our data to literature data for
volatiles in SNC apatites [1–8].
Results: Our measurements of Cl, F, and H in SNC apatites are
similar to previous data, but the increased size of the collective data set
sheds light on systematic variations. Our 3 basaltic shergottites have 0.33–
0.95 wt% H2O (literature data: 0.18–0.64 wt% [1–2]), those from the
lherzolitic shergottite have 0.07–0.27 wt% (the only previously measured
apatite from such a sample has 0.43 wt% [3]); and those from the
nakhlite have 0.07–0.11 wt%. Data are also available for apatites from
Chassigny (0.21 wt% [4]) and ALH 84001 (0.08 wt% [2] and 0.22 wt%
[4]). Apatites from basaltic shergottites appear to be on average H2O-rich
relative to apatites from other lithologies. S contents are variable (<0.01–
0.82 wt%; previous measurements are <0.01–0.08 wt% [5–8]). As with
H2O, S contents are lower in the nakhlite (<0.01 wt%) and lherzolitic
shergottite (0.02–0.04 wt%) than in the basaltic shergottites (0.05–
0.82 wt%).
Discussion: The H in apatites from basaltic shergottites spans a
range similar to apatites from terrestrial maﬁc igneous rocks. The higher
H and S contents of basaltic shergottites relative to other SNC rock types
may indicate higher initial volatile contents or lower extents of degassing
prior to apatite crystallization.
Based on our results, apatites in SNCs, particularly basaltic
shergottites, are signiﬁcantly richer in S (by approximately 2·) than those
in maﬁc terrestrial igneous rocks. S is typically incorporated into apatite
as SO4
2-, and thus is expected to be more strongly partitioned into
igneous apatite at higher fO2 (i.e., where sulfate dominates over sulﬁde in
basaltic melts). As expected, terrestrial S-rich apatites are found in lavas
that are oxidized (DQFM +2 to +6 log units). Estimates of fO2 in
shergottite parent magmas (DQFM )4 to +0.5 log units) would indicate
that S2- was the primary sulfur species. The high S contents of SNC
apatite despite low fO2 could reﬂect (1) high total magmatic S contents;
(2) apatite crystallized late when fO2 levels rose above estimates; or (3)
some S in SNC apatites is present as sulﬁde in the halogen site.
References: [1] Leshin L. A. 2000. Geophysical Research Letters
27:2017–2020. [2] Greenwood J. P. et al. 2008. Geophysical Research
Letters 35:L05203. [3] Guan Y. et al. 2003. Abstract #1830. 34th Lunar
and Planetary Science Conference. [4] Boctor N. Z. et al. 2003.
Geochimica et Cosmochimica Acta 67:3971–3989. [5] Harvey R. P. et al.
1993. Geochimica et Cosmochimica Acta 57:4769–4783. [6] Xirouchakis D.
et al. 2002. Geochimica et Cosmochimica Acta 66:1867–1880. [7]
Greenwood J. P. et al. 2003. Geochimica et Cosmochimica Acta 67:2289–
2298. [8] Treiman A. H. and Irving A. J. 2008. Meteoritics & Planetary
Science 43:829–854.
74th Annual Meeting of the Meteoritical Society: Abstracts A39


Abundances of Cl, F, H, and S in Apatites From SNC Meteorites

5504
NANOGLOBULE ABUNDANCES IN IOM EXTRACTS:
CORRELATION WITH PARENT BODY PROCESSING
H. G. Changela1,2, R. M Stroud2, B. T. De Gregorio3, L. R. Nittler4,
C. M. O’D. Alexander4 and G. D. Cody4. 1George Washington University,
Department of Physics, Washington, District of Columbia 20052, USA.
2Naval Research Laboratory, 4555 Overlook Ave. SW, Washington,
District of Columbia 20375, USA. E-mail: changela@anvil.nrl.navy.
mil. 3Johnson Space Center, Houston, Texas 77058, USA. 4Carnegie
Institution of Washington, Washington, District of Columbia 20015, USA.
Introduction: Nanoglobules are a form of Insoluble Organic Matter
(IOM) found in chondrites [1], IDPs [2] and Comet 81P/Wild2 [3]. Some
nanoglobules exhibit large 15N and D enrichments relative to solar values,
indicating that they likely originated in the ISM or the outskirts of the
protoplanetary disk [4]. Recent studies of samples from the Tagish Lake
meteorite with varying levels of hydrothermal alteration suggest that
nanoglobule abundance decreases with increasing hydrothermal alteration
[5]. The aim of the present study is to further constrain the morphologies
of IOM from a range of primitive chondrites in order to determine any
correlation between morphology and petrographic grade and chondrite
class.
Methods: We are performing a comprehensive scanning transmission
electron microscopy (STEM) survey of IOM residues prepared by
methods described in [3]. STEM annular dark-field (ADF) imaging
surveys were performed with NRL’s JEOL 2200FS on residues from
Murchison (CM2), EET 92042 (CR2) and QUE 97008 (L3). IOM textures
were classified as either having a ‘globular’ morphology, i.e. spherical,
non-porous regions approximately 50–1000 nm in size; ‘fluffy’, i.e. porous
material with fine scale heterogeneity below 50 nm; and ‘dense-irregular’,
i.e. uniformly dense, non-spherical material >50 nm. ADF images were
taken of each chondrite, sampling approximately 100 lm2 of IOM. The
different morphologies were manually identified from the images and
masked using Adobe Photoshop. Area fractions were then obtained using
Image J software. Because some small globules (<100 nm) are difficult to
distinguish from the background of fluffy IOM, our results reflect a lower
limit on globular abundances.
Results and Discussion: Globular to fluffy and dense irregular to
fluffy IOM fractions in these chondrites show distinctive variations.
Murchison contains the highest abundance of nanoglobules
(approximately 7%), followed by EET 92042 (approximately 5%) and
then QUE 97008 (approximately 1%). The abundances of dense irregular
IOM fractions are similar for Murchison and EET 92402, but have much
higher abundance (approximately 20% of measured IOM) in QUE 97008.
We will also present new analyses of residues from types 1, 2 and 3 CR
and other chondrites to identify any links between nanoglobule
abundances and petrographic grade. It has been shown that isotopic
enrichment within the IOM is not just localized to globular species, but to
some ‘fluffy’ components as well [6]. It is not clear whether some of the
‘dense irregular’ morphologies of IOM contain similar enrichments.
Coordinated analyses of these extracts and in situ IOM studies will enable
us to further constrain the nature of these morphologically distinct
components and how they vary with petrographic grade or chondrite
class.
References: [1] Nakamura-Messenger K. et al. 2006. Science
314:1439–1442. [2] Flynn G. J. et al. 2003. Geochimica et Cosmochimica
Acta 4791–4806. [3] De Gregorio B. T. et al. 2010. Geochimica et
Cosmochimica Acta 74:4454–4470. [4] Alexander C. M. O’D. et al. 2007.
Geochimica et Cosmochimica Acta 71:4380–4403. [5] Herd C. D. K. et al.
2011. Science, in press. [6] De Gregorio et al. 2010. Abstract #2108. 41st
Lunar and Planetary Science Conference.
5401
ABUNDANCES OF Cl, F, H, AND S IN APATITES FROM SNC
METEORITES
M. B. Channon, J. W. Boyce, E. M. Stolper and J. M. Eiler. California
Institute of Technology, Pasadena, CA 91125, USA. E-mail: mchannon@
gps.caltech.edu.
Introduction: Magmatic volatiles influence igneous phase equi-
libria, eruptive behavior, atmospheric composition, and climate. Several
lines of evidence suggest that Mars is rich in halogens and S relative to
Earth. However, magmatic volatile abundances and their effects on
magmatic processes on Mars are controversial. Here we examine igneous
apatites in SNC meteorites as indicators of magmatic volatile abundances.
Methods: We measured Cl, F, H (reported as wt% H2O), and S in
25 apatites from 3 basaltic shergottites (JaH 479, NWA 856, and NWA
2986), 1 lherzolitic shergottite (NWA 1950), and 1 nakhlite (NWA 998)
using Caltech’s 7f SIMS. We compared our data to literature data for
volatiles in SNC apatites [1–8].
Results: Our measurements of Cl, F, and H in SNC apatites are
similar to previous data, but the increased size of the collective data set
sheds light on systematic variations. Our 3 basaltic shergottites have 0.33–
0.95 wt% H2O (literature data: 0.18–0.64 wt% [1–2]), those from the
lherzolitic shergottite have 0.07–0.27 wt% (the only previously measured
apatite from such a sample has 0.43 wt% [3]); and those from the
nakhlite have 0.07–0.11 wt%. Data are also available for apatites from
Chassigny (0.21 wt% [4]) and ALH 84001 (0.08 wt% [2] and 0.22 wt%
[4]). Apatites from basaltic shergottites appear to be on average H2O-rich
relative to apatites from other lithologies. S contents are variable (<0.01–
0.82 wt%; previous measurements are <0.01–0.08 wt% [5–8]). As with
H2O, S contents are lower in the nakhlite (<0.01 wt%) and lherzolitic
shergottite (0.02–0.04 wt%) than in the basaltic shergottites (0.05–
0.82 wt%).
Discussion: The H in apatites from basaltic shergottites spans a
range similar to apatites from terrestrial mafic igneous rocks. The higher
H and S contents of basaltic shergottites relative to other SNC rock types
may indicate higher initial volatile contents or lower extents of degassing
prior to apatite crystallization.
Based on our results, apatites in SNCs, particularly basaltic
shergottites, are significantly richer in S (by approximately 2·) than those
in mafic terrestrial igneous rocks. S is typically incorporated into apatite
as SO4
2-, and thus is expected to be more strongly partitioned into
igneous apatite at higher fO2 (i.e., where sulfate dominates over sulfide in
basaltic melts). As expected, terrestrial S-rich apatites are found in lavas
that are oxidized (DQFM +2 to +6 log units). Estimates of fO2 in
shergottite parent magmas (DQFM )4 to +0.5 log units) would indicate
that S2- was the primary sulfur species. The high S contents of SNC
apatite despite low fO2 could reflect (1) high total magmatic S contents;
(2) apatite crystallized late when fO2 levels rose above estimates; or (3)
some S in SNC apatites is present as sulfide in the halogen site.
References: [1] Leshin L. A. 2000. Geophysical Research Letters
27:2017–2020. [2] Greenwood J. P. et al. 2008. Geophysical Research
Letters 35:L05203. [3] Guan Y. et al. 2003. Abstract #1830. 34th Lunar
and Planetary Science Conference. [4] Boctor N. Z. et al. 2003.
Geochimica et Cosmochimica Acta 67:3971–3989. [5] Harvey R. P. et al.
1993. Geochimica et Cosmochimica Acta 57:4769–4783. [6] Xirouchakis D.
et al. 2002. Geochimica et Cosmochimica Acta 66:1867–1880. [7]
Greenwood J. P. et al. 2003. Geochimica et Cosmochimica Acta 67:2289–
2298. [8] Treiman A. H. and Irving A. J. 2008. Meteoritics & Planetary
Science 43:829–854.
74th Annual Meeting of the Meteoritical Society: Abstracts A39


English

During a nano-mineralogy investigation of the Acfer

094 carbonaceous chondrite, lakargiite (CaZrO_3) was identified as

submicrometer inclusions in an isolated hibonite grain in section USNM

7233-1. The hibonite grain is described in Simon and Grossman [1].

Lakargiite is a recently found perovskite-group mineral from hightemperature

skarns in ignimbrites of the Upper-Chegem volcanic

structure, the North Caucasus, Russia [2]. Reported here is the first

extraterrestrial occurrence of lakargiite, as a new ultrarefractory mineral

in a primitive meteorite, among the first solids formed in the solar system.

Field-emission SEM with EDS and electron back-scatter diffraction

(EBSD) was used to characterize its composition and structure and

associated phases

Discovery of Meteoritic Lakargiite (CaZrO_3), a New Ultra-Refractory Mineral from the Acfer 094 Carbonaceous Chondrite

The partitioning of elements between olivine and liquid

is key to understanding igneous processes in mafic and ultramafic systems

[1]. The landmark study of Roeder and Emslie [2] concluded that the

olivine (ol)-liquid (liq) exchange coefficient, K_(D,Fe2+-Mg) = (FeO/MgO)^(ol) /

(FeO/MgO)^(liq) (by weight), is 0.30 ± 0.03, independent of temperature (T)

and liquid composition. Subsequent work [3] has shown a dependence on

liquid composition, but the canonical value of 0.30 is still widely used in

both terrestrial and Martian applications [e.g., 4, 5]. Here, we use

previously published experiments on bulk compositions relevant to

Martian magmas to determine the appropriate K_(D,Fe2+-Mg)(s) for Martian

systems; we then use this value to test whether any of the ol-phyric

shergottites represent liquids

Matzen, A. K.

Baker, M. B.

5528
Fe2+-Mg PARTITIONING BETWEEN OLIVINE AND MARTIAN
BASALTIC MELTS
A. K. Matzen, J. R. Beckett, M. B. Baker and E. M. Stolper. California
Institute of Technology, MC 170-25, Pasadena, CA 91125, USA. E-mail:
amatzen@caltech.edu.
Introduction: The partitioning of elements between olivine and liquid
is key to understanding igneous processes in maﬁc and ultramaﬁc systems
[1]. The landmark study of Roeder and Emslie [2] concluded that the
olivine (ol)-liquid (liq) exchange coeﬃcient, KD;Fe2þMg = (FeO/MgO)
ol /
(FeO/MgO)liq (by weight), is 0.30 ± 0.03, independent of temperature (T)
and liquid composition. Subsequent work [3] has shown a dependence on
liquid composition, but the canonical value of 0.30 is still widely used in
both terrestrial and Martian applications [e.g., 4, 5]. Here, we use
previously published experiments on bulk compositions relevant to
Martian magmas to determine the appropriate KD;Fe2þMg(s) for Martian
systems; we then use this value to test whether any of the ol-phyric
shergottites represent liquids.
Experiments on Martian Compositions: One-atm experiments
on model Martian compositions provide the tightest constraint on
KD;Fe2þMg because T and oxygen fugacity (fO2) are well known, allowing
us to use [6] to predict the amount of ferrous iron present in each liquid.
The median of 17 published 1-atm experiments yields KD;Fe2þMg =
0.354 ± 0.008 (error is one mean absolute deviation, MAD). There are
higher pressure (P) experiments on model Martian compositions, but their
fO2s are less well constrained. High-P experiments in graphite capsules
are reducing [7], but Fe3+ still materially aﬀects estimates of KD;Fe2þMg;
correcting for the Fe3+ using [6, 7] increases KD;Fe2þMg, on average, by
0.016. We see no strong correlations of KD;Fe2þMg with liquid or ol
composition for the high or low-P experiments and a weak increase in
KD;Fe2þMg with increasing P. A marked increase in KD;Fe2þMg for high-P
experiments at T<1150 C is likely due to lack of equilibrium.
Accepting high-P experiments with T >1150 C leads to a median
KD;Fe2þMg of 0.369 ± 0.024 (MAD), higher than the 1-atm experiments
but notably higher than the canonical value of 0.30 [2]. Combining 1-atm.
and high-P, high-T experiments yields a median KD;Fe2þMg of
0.360 ± 0.013 (MAD), close to the recently reported value of
0.35 ± 0.01 [8], which was obtained without correcting for Fe3+ in the
liquid.
Olivine-Phyric Shergottites: Using KD;Fe2þMg = 0.30 leads to the
result that none of the ol cores in ol-phyric shergottites is in equilibrium
with liquids equivalent to their bulk. Applying our KD;Fe2þMg to these
shergottites leads to the possibility that Y980459, NWA 5789 and 2990
are liquid compositions (others are not), identical to the results of
Filiberto and Dasgupta [8]. Accounting for Fe3+ in the liquid also allows
us to constrain plausible fO2s during cooling when independent measures
are unavailable or not yet determined; e.g., if the olivines in NWA 2990
are in equilibrium with a liquid whose composition is that of the bulk
meteorite, crystallization must have occurred under reducing conditions
where the Fe3+/
P
Fe is small, IW+0.5 at 1 atm or IW+1 at 1 GPa.
References: [1] Basaltic Volcanism Study Project. 1981. [2] Roeder
P. L. and Emslie R. F. 1970. Contributions to Mineralogy and Petrology
29:275–289. [3] Sack R. O. et al. 1987. Contributions to Mineralogy and
Petrology 96:1–23. [4] Falloon T. J. et al. 2007. Chemical Geology
241:207–233. [5] Peslier A. H. et al. 2010. Geochemistry Geophysics
Geosystems 74:4543–4576. [6] O’Neill et al. 2006. American Mineralogist
91:404–412. [7] Me´dard E. et al. 2008. American Mineralogist 93:1838–
1844. [8] Filiberto J. and Dasgupta R. 2011. Earth and Planetary Science
Letters 304:527–537.
5173
EXPLORING XRF AS A NEW TECHNIQUE FOR BASIC
METEORITE CLASSIFICATIONS
R. G. Mayne1, A. J. Ehlmann1 and K. C. Daviau2. 1Monnig Meteorite
Collection, School of Geology, Energy, and the Environment, Texas
Christian University, TCU Box 298830, Fort Worth, TX 76129, USA.
E-mail: r.g.mayne@tcu.edu. 2Physics Department, Bard College, PO Box
5000, Annandale-on-Hudson, NY 12504, USA.
Current Classiﬁcation Methods: In the 2010/2011 season, the
Antarctic Search for Meteorites (ANSMET) collected around 1200
meteorites. These will all be classiﬁed over the next 2 years, according to
the U.S. Federal Regulation on Antarctic Meteorites [1], by the curatorial
staﬀ at the Smithsonian Institution’s National Museum of Natural
History. The vast majority of the meteorites collected in Antarctica are
equilibrated ordinary chondrites and the current method employed for
their identiﬁcation is that of visual examination combined with oil
immersion of olivine grains. This technique requires that a small amount
of each meteorite be powdered, sieved, and then examined in refractive
index oils under a petrographic microscope. This is a timely process and
the Smithsonian’s main goal is to be able to ‘‘separate the approximately
10% of meteorites that deserve further scientiﬁc study’’ [1].
XRF: The Monnig Meteorite Collection deals with many requests
from the general public for meteorite identiﬁcation. The vast majority of
these samples are industrial slag. The newly purchased Bruker handheld
XRF will be used to analyze these samples to conﬁrm that their
composition is not meteoritic.
The goal of this study is to explore XRF as a new technique for
meteorite identiﬁcation. In this preliminary study we will present data on
the ﬁrst two parts of this study (1) estimating the Ni-content of iron
meteorites (2) examining previously classiﬁed ordinary chondrites to
establish a calibration technique for unknowns. The eventual aim is to see
if the XRF technique outlined here can be used to distinguish LL, L, and
H chondrites from one another, to provide an alternative streamlined
process to oil immersion.
Methodology: All meteorites will be analyzed on the Bruker Tracer
III-SD handheld XRF system at Texas Christian University. For part (1)
only meteorites from the Monnig Meteorite Collection with a published
Ni content were selected for analysis. All Ni contents were taken from [2].
A minimum of three analyses were taken for each sample. The number of
counts for Ni Ka were tabulated each time and a calibration curve was
constructed. Previously classiﬁed ordinary chondrites were selected from
the Monnig Collection for part (2) of the study. Twenty meteorites of
each ordinary chondrite group (H, L, LL) will be measured.
Preliminary Results: Initial results relating Ni Ka counts to Ni
content of iron meteorites show that these two components do appear to
be directly related and no further reduction of the data (into percentage
Ni) is required. The calibration curve constructed from the preliminary
data has an R2 value of 0.94.
At the time of writing, only ﬁve H, L, and LL meteorites have been
analyzed on the XRF. While there appear to be some diﬀerences between
the ordinary chondrite groups, there is currently not enough data for
statistical analysis to see if these diﬀerences are signiﬁcant enough to
allow their identiﬁcation.
References: [1] Corrigan C. M. et al. 2008. Meteoritics & Planetary
Science 43:A180. [2] Wasson J. T. 2010. Geochimica et Cosmochimica Acta
75:1757–1772.
A150 74th Annual Meeting of the Meteoritical Society: Abstracts


Fe^(2+)-Mg Partitioning Between Olivine and Martian Basaltic Melts

Pravdivtseva, O.

Meshik, A.

Hohenberg, C. M.

Burnett, D. S.

5116
THE FIRST DOCUMENTED GEORGIA-AREA TEKTITE FOUND IN
BIBB COUNTY, GEORGIA
H. Povenmire. Florida Institute of Technology, 215 Osage Drive, Indian
Harbour Beach, FL 32937, USA. E-mail: katiehal1@yahoo.com.
About 1999, a black glassy rock was found approximately in the
middle of Bibb County just south of Macon, GA. This was identiﬁed as a
Georgia tektite on May 19, 2011. This 18.42 g tektite is a ﬂattened tear
drop shape and is 47 · 22 · 15 mm in size. It had been in running water
for a long time and the surface was smoothed. There are no bubbles or
inclusions. The ﬁnd location was on the Fall Line and the Piedmont
Plateau. The two western adjoining counties, Crawford and Peach have
similar geology and will probably be conﬁrmed with further ﬁeld work.
The approximate ﬁnd location was lat. 32d 42¢N and long. 83d 44¢W.
In 2010, a spectacular Georgia-area tektite was found in Aiken
County, South Carolina. In 2011, a second tektite was found in Allendale
County, South Carolina. This is a small disk- shaped tektite and was
found in an Indian midden overlooking the Savannah River. It was not
found in situ and further ﬁeld work is in progress for more specimens.
About ten percent of Georgia tektites have shown indications of
being ﬂaked by early Indians. However, complete artifacts are extremely
rare. In early 2011, a second Georgia tektite which had been ﬂaked into a
projectile point was reported. This specimen was found in Dodge county
and artifact specialists have suggested that it was of archaic age and the
aborigines ﬂaking it were likely of the Pickwick or Wacissa Cultures. This
7.1 g tektite was ﬂaked, then damanged and then reworked several times.
In 2010, the third largest Georgia splash form tektite was re-ported
from Bleckley County. It has a weight of approximately 65 g. Precise data
on it is not available but it is of signiﬁcant importance because it ﬁlls a
statistical gap in the size distribution of the large Georgia tektites.
In the last year, several museum quality tektites have been found.
These have come from Bleckley, Wilcox and Houston counties. Since
these specimens have come from previously con-ﬁrmed counties, they are
good scientiﬁc specimens but do not add to our knowledge of
distribution.
There have now been approximately 2700 Georgia-area tektites
found in 26 counties. The total area of the Georgia-area strewn ﬁeld is
now approximately 10,000 square miles and this is larger than the Texas
bediasite strewn ﬁeld.
Acknowledgments: I want to thank the help of Mike Stokes,
Thomas Thurman, Sharon Veal and Kalen Icard.
References: [1] Povenmire H. 2003. Tektites: A Cosmic Enigma Blue
Note Publishing, Cocoa Beach, FL. [2] Povenmire H. and Lambert J.
2010. The First Georgia-Area Tektite found in Aiken County, South
Carolina, Meteoritics & Planetary Science, 73rd Annual Meeting Abstract,
New York.
5509
FEASIBILITY OF IODINE AND BROMINE ANALYSIS IN GENESIS
SOLAR WIND COLLECTORS
O. Pravdivtseva1, A. Meshik1, C. M. Hohenberg1 and D. S.
Burnett2. 1McDonnell Center for the Space Sciences and Physics
Department, Washington University, St. Louis, MO 63130, USA. E-mail:
olga@physics.wustl.edu. 2Geology 100-23, CalTech, Pasadena, CA, USA.
Comparison of elemental abundances in sun, meteorites and earth
provides understanding of the formation and evolution of the solar
system. Yet, the majority of the solar system abundances are based on
meteoritic values [1–6]. Here we report an attempt to estimate a feasibility
of direct measurements of iodine and bromine in the GENESIS solar
wind Aluminum on Sapphire collector (AloS) using neutron induced
conversions: 127I(n,cb)128Xe, 79Br(n,cb)80Kr and 81Br(n,cb)82Kr.
To estimate the extent of terrestrial halogen contamination in
GENESIS collectors, several ﬂown fragments of AloS were submerged in
methanol (for 1 h and for 48 h), rinsed in methanol, dried, sealed under
vacuum in fused quartz ampoules and irradiated at the Missouri
University Research Reactor receiving ﬂuence 2 · 1019 thermal neutrons
cm)2.
We analyzed two areas (0.07 and 0.7 cm2) of AloS the solar wind
collector washed for 48 h, and one area (0.13 cm2) of the collector washed
for 1 h. Xenon extracted from the largest area had a clear signature of
solar wind as indicated by 129Xe/132Xe = 1.045 ± 0.005 and other major
isotopes, while 128Xe/132Xe = 1.01 ± 0.03 had a 12-fold excess compared
to the solar value. Longer washing apparently reduces iodine
contamination 4 times, implying that it is surface correlated. Evidently, to
separate 128Xe, derived from solar iodine, and the solar wind 128Xe, the
iodine contamination should be reduced further, at least 10 times. It may
be achieved by combination of a longer and more aggressive cleaning
procedure (i.e., ozone cleaning followed by washing in non-polar solvents
at elevated temperatures) and depth-proﬁling laser extraction.
Krypton analyses of the irradiated AloS collectors demonstrates
solar wind signature with 17% excess in 82Kr and 3-fold excess in 80Kr.
Apparently, cleaning in methanol is much more eﬃcient for Br that for I,
since a longer 48-hour washing reduced bromine contamination 50 times.
Our ﬁrst ‘‘quick and dirty’’ experiment suggests that determination
of solar iodine and bromine is potentially feasible, especially considering
availability of cleaner Si-based Genesis collectors and the possibility of
analyzing larger collector areas irradiated with tripled neutron ﬂuence.
Acknowledgment: This work is supported by NASA grant
NNX07AM76G.
References: [1] Anders E. and Ebihara M. 1982. Geochimica et
Cosmochimica Acta 46:2363–2380. [2] Anders E. and Grevesse N. 1989.
Geochimica et Cosmochimica Acta 53:197–214. [3] Cameron A. G. W.
1968. In Origin and distribution of the elements, Ahrens L. H., ed.
Pergamon, Oxford. pp. 125–143. [4] Cameron A. G. W. 1973. Space
Science Reviews 15:121–146. [5] Suess H. E. and Urey H. C. 1956.
Reviews of Modern Physics 28:53–74. [6] Lodders K. 2010. Principles and
Perspectives in Cosmochemistry 379–417.
A192 74th Annual Meeting of the Meteoritical Society: Abstracts
