M P R

17 - 18 december 2012
Salle «ESPACE» Head quarters
CNES - paris
Cosmochemistry of primitive bodies:
the need for MarcoPolo a european sample
return space mission
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V. Heber
S. Tachibana
10:30
10:45
J. Trigo
G. Libourel
17:00
17:15
17:30 - 19:00
M. Roskosz
Chondrule formation: quicker and faster?
Icebreaker
Leaming about the degree of aqueous alteration of NEOs from laboratory IR sêctra of primitive Antarctic chondrites
Experimental approach of dust processing in protoplanetary disks and comparison with returned samples
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The importance of sample return for accurate and precise scientific analysis: Examples from the Genesis Mission
Genesis as an Example of a Sample Return Mission
Marco Polo-R: return of NEA primitive sample in Europe
Welcome address
Registration, coffee
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istHayabusa-2: Sample return mission from a near-Earth C-type asteroid, 1999JU3
T. Nakamura
New
ryperspective for early solar system evolution derived from recent sample return missions
a
I. Tsuchiyama
Eu Outline
oof fHayabusa sample initial analysis and recent progress
I. Yurimoto
returnp
mission, isotope microscope, and isotope nanoscope
rSample
o
riSolar
pein primitive
P. Hoppe
Stardust
Current status, recent advances, and future prospects
miSystem materials:
H. Leroux
Comet Wilda
2 particles
n in interaction
tiv with the Stardust aerogel
sa
12:30 - 14:00
Break
eb
minplaboratory
J. Brucato
Stardust grains investigated
odto the primitive asteroid 1999RQ36
le mission
P. Michel
OSIRIS-REx, the NASA sample return
re ies:
R. Wieler
Some highlights from returned lunar samples
tu high precision
New science with samples collected 40 years ago:
F. Moynier
rn theisotopic composition of transition metals in Apollo
samples and the origin of the lunar volatile depletion
ne
B. Marty
The lunar soil record of accretion onto planetary surfacessp
ed
M. Bizzaro
Absolute and relative chronology of the first solar system solidsac
e
fomaterials
F. Robert
The scales of the spatial heterogeneities of the hydrogen isotopic ratio inm
solar system
iss r M
15:45 - 16:00
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io
C.O.M.D. Alexander
The asteroid-comet connection: The water and organic stories
n. rco
M. Chaussidon
Al constraints on the origin and history of refractory components of chondrites
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A. Saladino
Role of non terrestrial minerals in the prebiotic synthesis of genetic and metabolic apparatuses
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Monday, 17th december
L. Bonal
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S. Krot
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H. Busemann
M. Moreira
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C. Smith
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J. Aléon
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Characterization of the post-accretion history of the C-type asteroid sampled by MarcoPolo-R
New Evidence for Compositional Diversity Among Primitive Asteroids
The physical properties of dark meteorites
Organic-mineral interface in the CI type carbonaceous chondrite Orgueil
D/H measurements in the water of comets using Herschel
Sampling the asteroid comet continuum
Chondritic Kr and Xe: result of irradiation processes in the accretion disk?
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Noble Gases in (Cometary) Interplanetary Dust and samples returned from comet Wild 2 and asteroid Itokawa.
Status and Plans
Chemical and isotopic characterization of asteroidal matter in the Goëttingen
the requirements for the successful operation of a European curation facility
Curation of the samples returned by Marco Polo-R : state of the art
is Are meteorites the parent materials of planets ?
ry of ferroan olivine in matrices of "primitive" (petrologic type of 3.0) chondrites
a E tOrigin
of between chondrules and matrix in chondrites
B. Zanda
The relationship
uThe
roso-called"refractory
J.A. Barrat
elements in enstatite chondrites
rimlithophile"
pe ofporganic
L. Remusat
The evolution
matter in chondrites through secondary processes on the parent body
an of primitive
iticarbonaceous meteorites
Z. Martins
The organic content
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M. Lee
Resolving models for aqueousp
alteration ofo
primitive meteorites by sample return
le returneddtoiEarth
A. Davis
New analytical techniques for samples
spacecraft
es byPolo-R
re by Marco
U. Ott
Noble gas studies of asteroidal matter returned
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ur th
J. Gilmour
Measuring Xenon and Krypton in Primitive Material
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Taking apart sample return grains, atom by atom
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Ion microprobe U-Pb dating of a single apatite grain in meteorites
ac eed
P. Rochette
Non destructive characterization of extraterrestrial materials: techniques
applications of magnetism
e and
orprecautions
mi fand
A. Cheng (organizer)
Discussion - Sampling an asteroid : requirements
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N. Starkey
Oxygen Isotopic Measurements of Fine Grained Primitive Material; The Challenge s
of Small Samples
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Implications for curation of the Marco-Polo samples from recent Hayabusa analyses
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H. Palme
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G. Consolmagno
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P. Ehrenfreund
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Tuesday, 18th december
ABSTRACTS
Cosmochemistry of
primitive bodies:
the need for MarcoPolo-R
a European sample return space mission.
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Marco Polo-R: return of NEA primitive sample in Europe
M.A. Barucci1 and MarcoPolo-R ESA Science study team
LESIA-Observatoire de Paris, CNRS, Université Pierre et Marie Curie,
Université Paris Diderot, 92195 Meudon Principal Cedex, France, antonella.barucci@obspm.fr
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MarcoPolo-R is a sample return mission to a primitive Near-Earth
Asteroid (NEA) selected for a second Assessment Study Phase in
the framework of ESA’s Cosmic Vision (CV) programme. The new
assessment study started at ESA on May 2011, will continue until
the end of 2013, when ESA will finally select the M3 class mission
for launch. MarcoPolo-R is a European-led mission with a possible
contribution from other agencies. MarcoPolo-R will rendez-vous with a
primitive NEA, scientifically characterize it at multiple scales, and return
a unique sample to Earth unaltered by the atmospheric entry process
or terrestrial weathering.
The mission will answer to the fundamental CV questions “How
does the Solar System work?” and “What are the conditions for life and
planetary formations?”.
MarcoPolo-R will return bulk samples from an organic-rich asteroid
to Earth for laboratory analyses, allowing us to:
• explore the origin of planetary materials and initial stages of
habitable planet formation,
• identify and characterize the organics and volatiles in a primitive
asteroid.
The new baseline target as well the status of the mission will be
presented and discussed.
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Genesis as an Example of a Sample Return Mission
D. S. Burnett
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Caltech,
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Div. of Geological and Planetary Sciences. MS 100-23
Pasadena CA, 91125. burnett@gps.caltech.edu
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The NASA Genesis Discovery Mission returned samples of the solar
wind for isotopic and elemental analyses in terrestrial laboratories.
Much remains to be done, but we have been very successful to date in
showing that the terrestrial planets are anomalous relative to the Sun
in terms of the isotopic composition of O, N, and the noble gases. In
the case of N, the Sun and Jupiter have the same ratio of 15N /14N, but
the terrestrial atmosphere in a full 40% enriched in this ratio, and many
inner solar system materials are even more enriched.
Reference: D. Burnett et al., Proc. Nat. Acad Sci. USA 108, 19147, 2011
The importance of sample return for accurate and precise
scientific analysis: Examples from the Genesis Mission
V. S. Heber & K. McKeegan
Department of Earth and Space Sciences UCLA
595 Charles Young Drive East, Box 951567; Los Angeles,
CA 90095-1567, USA
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The solar wind composition is analyzed much more precisely in
samples returned by the NASA Genesis mission than by space-borne
instruments. For example, we detected differences in the isotopic
composition of He, Ne and Ar between different solar wind regimes,
which allows us to assess and constrain fractionation processes in
the solar wind. Furthermore, returned samples enable us to repeat
analyses with different methods. The first measurements of the N
isotopic composition of solar wind were contradictory. This discrepancy
was only solved by subsequent analyses involving other groups and
methods. Finally, a wealth of materials and methods available in
laboratories allow an accurate calibration of the compositional data.
We present solar wind data and analytical methods that illustrate the
importance of sample return missions.
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Hayabusa-2: Sample return mission from a near-Earth
C-type asteroid, 1999JU3
S. Tachibana1 & Hayabusa-2 sampler team
Dept. Natural History Sci., Hokkaido Univ., N10 W8, Sapporo 060-0810,
Japan, tachi@ep.sci.hokudai.ac.jp
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A future Japanese asteroidal sample return mission, Hayabusa-2,
plans to return samples from a near-Earth C-type asteroid 1999JU3.
The spececraft will be launched in 2014- 2015, arrive at the target
asteroid in 2018, stay for 1.5 years with remote sensing observations
and three-time sampling at different surface locations. The samples
will be back to the Earth at the end of 2020. In the presentation, we
will illustrate details of the mission focusing on a sampling device with
improvements from the Hayabusa sampler and the science of returned
samples.
New perspective for early solar system evolution derived from
recent sample return missions
Tohoku University, Japan
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T. Nakamura
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Outline of Hayabusa sample initial analysis and recent progress
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Kyoto University, Japan
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A. Tsuchiyama
The outline of the initial analysis of Hayabusa samples (Itokawa
regolith particles) is presented: the surface material on the asteroid
Itokawa corresponds to a mixture of LL4-6 chondrites and has a variety
of features on the asteroid surface processes, such as space weathering,
particle abrasion and solar wind noble gas implantation. Recent progress
on the asteroid surface processes are also presented.
Sample return mission, isotope microscope and isotope
nanoscope
H. Yurimoto
Natural History Sciences, Hokkaido University, Sapporo, Japan, yuri@ep.sci.hokudai.ac.jp
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Primitive materials of our solar system have survived in promitive
bodies as submicrometer-sized matters. Microscopy for isotope
disribution is useful to characterize the primitive matters [e.g. 1]. We
progress instrumental developments of isotope microscope [2] and
isotope nanoscope [3] to apply returned samples from space. In this talk,
we will present examples of isotope microscopy of primitve meteorites
and the future perspective at MarcoPolo-R Reentry.
[1] Kunihiro T. et al., (2005) Geochim. Cosmochim. Acta. 69, 763-773.
[2] Yurimoto H. et al., (2005) Appl. Surf. Sci. 203-204, 793-797.
[3] Ebata S. et al., (2012) Surf. Interface. Anal. 44, 635-640.
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Max Planck Institute for Chemistry, Mainz, Germany,
peter.hoppe@mpic.de
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P. Hoppe1
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Stardust in primitive Solar System materials: Current status,
recent advances, and future prospects
Primitive Solar System materials contain small quantities of socalled presolar grains that formed in the winds of evolved stars or in the
ejecta of stellar explosions [1]. Among the identified presolar minerals
are SiC, graphite, silicon nitride, oxides, and silicates. These grains
represent samples of stardust that can be analyzed in the laboratory
with sophisticated analytical instrumentation in great detail. Of particular
importance are co-ordinated studies involving SIMS, RIMS, and FIB/
TEM. FIB/TEM provides detailed information on the mineralogy
and physical properties of individual stardust grains [2]. The latest
generation SIMS instrument, the NanoSIMS ion probe, permits to do
isotope measurements of the light and intermediate mass elements at
the <100 nm scale, making it a powerful tool to identify stardust grains
in-situ in thin sections of meteorites and IDPs [3]. RIMS has been
used to measure the isotopic compositions of the heavy elements in
stardust grains at the micrometer scale. A new type of RIMS instrument,
“CHILI”, is currently under construction and is aimed to provide <100
nm resolution and better sensitivity [4]. Another promising analysis
technique for future studies is atom probe tomography which might be
useful to create 3D-elemental (and possibly isotopic) maps at the nm
scale [5].
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[1] Zinner E. (2007) In Treatise on Geochemistry, Vol. 1
(eds. A. Davis et al.), 1.
[2] Zega T.J. et al. (2007) MAPS, 42, 1373-1386.
[3] Hoppe P. (2006) Applied Surf. Sci., 252, 7102-7106.
[4] Stephan T. et al. (2012) Lunar Planet. Sci., 43, 2660.
[5] Heck P. et al. (2011) Lunar Planet. Sci., 42, 2070.
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Comet Wild 2 particles in interaction with the Stardust aerogel
H. Leroux1
Unité Matériaux et Transformations, Université Lille 1, Villeneuve
d’Ascq, France, Hugues.Leroux@univ-lille1.fr
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Wild 2 dust particles impacted into low-density silica aerogel at a
speed of 6.1 km.s-1. The deceleration tracks in the Stardust aerogel
display a wide range of morphologies which reveal a large diversity
of incoming particles. The large (> 1µm) and dense mineral grains
survived well the extreme conditions of hypervelocity capture.
Most of them appears to be calcium-aluminum inclusions (CAI) and
chondrules fragments (igneous rounded objects), as seen in primitive
chondrites. On the contrary, the fine-grained aggregate material
(individual component < 1µm) is found strongly damaged within the
aerogel. Due to their low mechanical strength, these assemblages
were disaggregated, dispersed and flash melted in the aerogel in walls
of bulbous deceleration tracks. Their petrologic and mineralogical
properties are found significantly modified by the flash heating of the
capture. Originating from a quenched melt mixture of comet material
and aerogel, the representative microstructure consists of silica-rich
glassy clumps containing Fe-Ni-S inclusions, vesicles and “dust-rich”
patches, the latter being remnants of individual silicate components
of the impacting aggregate. The average composition of these melted
particle fragments is close to the chondritic CI composition. They might
originate from ultrafine-grained primitive components.
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Stardust grains investigated in laboratory
J.R. Brucato1 A. Rotundi2, V. Della Corte2, G.A. Baratta3, J. Borg4, R.
Brunetto4, E. Dartois4, L. d’Hendecourt4, Z. Djouadi4, M. Ferrari2, S.
Merouane4, V. Mennella5, M.E. Palumbo3, P. Palumbo2
INAF-Osservatorio Astrofisico di Arcetri, Firenze, Italy,
jbrucato@arcetri.astro.it
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Dip. Scienze Applicate, Università degli Studi di Napoli “Parthenope”, Napoli, Italy,
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INAF-Osservatorio Astrofisico di Catania, Italy,
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Institut d’Astrophysique Spatiale, Orsay, France,
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INAF-Osservatorio Astronomico di Capodimonte, Napoli, Italy.
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Stardust/NASA space probe captured particles around comet
81P/Wild 2 in 2004, returning them to Earth in 2006. We report on
analyses we performed on 81P/Wild 2 particles prepared in different
configurations: 1) extracted from aerogel as bulk grains and deposited
on KBr and Si substrates; 2) single grains embedded in slices of aerogel
and pressed between to diamond surfaces. We performed on the two
sets of grains Micro IR spectroscopy and micro Raman spectroscopy
with conventional and synchrotron
sources. In addition we performed Field Emission Scanning Electron
Microscopy and EDX analyses. Results are discussed in connection
with sample preparation and aerogel capture.
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P. Michel
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OSIRIS-REx, the NASA sample return mission to the primitive
asteroid 1999RQ36
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UMR 7293 Lagrange/CNRS, Observatoire de la Côte d’Azur
B.P. 4229, 06304 Nice Cedex 4, France
The OSIRIS-REx mission is a 14-year undertaking from selection in
May 2011 through 2025 sample analyses. The spacecraft will be launched
in 2016, travel to a near-Earth carbonaceous asteroid (101955) 1999
RQ36, study it in detail from 2018, and bring back a sample (at least 60
grams or 2.1 ounces) to Earth in 2023. The return to Earth of pristine
samples with known geologic context will enable precise analyses that
cannot be duplicated by spacecraft-based instruments, revolutionizing
our understanding of the early Solar System. It will help us investigate
planet formation and the origin of life, and the data collected at the
asteroid will also aid our understanding of asteroids that can impact
Earth.
Some highlights from returned lunar samples
R. Wieler1
ETH Zürich, Earth Sciences, NW C84, CH-8092 Zürich
wieler@erdw.ethz.ch
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I will present a few science highlights obtained by analyses of lunar
samples returned by the Apollo (and some Luna) missions. This will
include but not be restricted to results from noble gas and nitrogen
studies.
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F. Moynier1, Randal Paniello2, James Day3
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New science with samples collected 40 years ago: high precision
isotopic composition of transition metals in Apollo samples and
the origin of the lunar volatile depletion
Department of Earth and Planetary Sciences and McDonnell Center for
Space Sciences, Washington University, St. Louis, MO 63130, USA. moynier@wustl.edu
2
Geosciences Research Division, Scripps Institution of Oceanography,
La Jolla, CA 92093-0244, USA
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Volatile elements play a fundamental role in the evolution of planets.
However, our understanding of how volatile budgets were set in
planets, and the nature and extent to which planetary bodies became
volatile-depleted during the earliest stages of Solar System formation
remain poorly understood. Since the return of lunar samples by the
Apollo mission ~40 years ago, the Moon has been considered to be
volatile-depleted and consequently it has been predicted that volatile
loss should have fractionated stable isotopes of moderately volatile
elements. Recent analytical developments allow us to now measure
the isotopic composition of moderately volatile metals to very high
precision. One such element, zinc, exhibits strong isotopic fractionation
during volatilisation in planetary rocks but is hardly fractionated during
terrestrial igneous processes, making Zn a powerful tracer of the volatile
histories of planets. Here we present high-precision Zn isotopic and
abundance data that show lunar magmatic rocks are enriched in the
heavy isotopes of Zn and have lower Zn concentrations than terrestrial
or martian igneous rocks. Conversely, Earth and Mars have broadly
chondritic Zn isotopic compositions. We show that these variations
represent large-scale evaporation of Zn, most likely in the aftermath of
the Moon-forming event, rather than small-scale evaporation processes
during volcanic processes. These results therefore represent the first
evidence for volatile depletion of the Moon through evaporation and are
consistent with a giant impact origin for the Earth and Moon.
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The lunar soil record of accretion onto planetary surfaces
B. Marty1, S. Assonov2, M. Chaussidon1, E. Füri1, K. Hasizume3,
F.A. Podosek4, R. Wieler5
CRPG-CNRS, Université de Lorraine, BP 20,
54501 Vandoeuvre-lès- Nancy Cedex, France
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Max Planck Institute for Chemistry, Mainz, Germany
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Osaka University, Japan
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Washington University, St. Louis, MO, USA
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ETH Zürich, Earth Sciences, NW C84, CH-8092 Zürich
wieler@erdw.ethz.ch
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Soil samples returned by the Apollo missions constitute an exceptional
archive of ET contributions to planetary surfaces over eons. The
analysis of single regolith grains by either laser extraction - static mass
spectrometry or ion probe has revealed the complexity of processes
and cosmochemical sources. We propose, from our investigations in
the last decade, that the main contributors are the solar wind and IDPlike dust over at least 2 Ga, with an increase of the flux of the latter in
the last 0.5 Ga. Comets do not appear a major contributor, although this
conclusion awaits further analysis of cometary material, especially for
the D/H and 15N/14N ratios. The analysis of lunar meteorites presumably
sampling randomly the Moon leads us to conclude that the terrestrial
atmosphere was not a major contributor of volatile elements to the
lunar surface.
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Absolute and relative chronology of the first solar system solids
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M. Bizzaro
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StarPlan - Centre for Star and Planet Formation
Natural History Museum of Denmark, University of Copenhagen
Øster Voldgade 5-7, Copenhagen, Denmark, DK-1350
The scales of the spatial heteorgeneities of the hydrogen isotopic
ratio in solar system materials
F. Robert
CNRS/Muséum National d’Histoire Naturelle UMR-7202
LMCM Paris. robert@mnhn.fr
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The most striking characteristic of the hydrogen isotopic ratio in
solar system material is its heterogeneous distribution at all scales: at
the scale of planets (AU), of comets and planetesimals (km to cm), of
minerals (μm to nm). Scientific communities and informations derived
form these variations can be sorted according to this scale range. As
a whole the D/H ratio in the solar system varies by almost 3 orders of
magnitude. Based on the D/H variations at all these scales, two recent
studies [1,2] have provided a coherent model for the origin of water in
the solar system. Similarly, laboratory experiments are in progress to
adress the origin of organic materials. These models could be tested on
samples returned from a chemically well identified asteroïd.
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1: Jaquet E., Robert F. Water transport in protoplanetary disks and the
hydrogen isotopic composition of chondrites. Icarus, submitted.
2 : Yang L., Ciesla F. J. and Alexander C. M. O. (2012). The D/H Ratio of
Water in a Forming and Evolving Protoplanetary Disk. In LPSC Abstracts, Vol.
43. P. 2023.
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The asteroid-comet connection: The water and organic stories
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DTM, Carnegie Institution of Washington, 5241 Broad Branch Road,
Washington DC 20015, USA. alexander@dtm.ciw.edu.
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Recent dynamical models suggest that C-complex and D-type asteroids formed well
beyond (4-13 AU) the formation location of Jupiter, and in some cases as far out as the
source regions of Oort and Jupiter-family comets [1, 2]. The discovery of so-called main
belt comets in the asteroid belt would certainly be consistent with this [3]. On the other
hand, in the models the S-complex and E-type asteroids would have formed at ≤3 AU.
The C- and D- asteroids are thought to be the sources of the carbonaceous chondrites
(CCs), while the S- and E- asteroids the sources of the ordinary (OCs) and enstatite
chondrites (ECs). Objects that formed beyond the formation location of Jupiter are likely
to have been water-ice- and organic-rich. Thus, the organic material and water-OH in
chondrites may be important tests of these models.
The dominant amino acids in the primitive CCs (CI, CM, CR and ungrouped CCs like
Tagish Lake) are probably formed by Strecker synthesis, in which case the accreted ices
were HCN- and NH3-bearing, like comets. The insoluble organic material (IOM) is the
dominant organic component in chondrites, and in the primitive CCs its bulk composition
is like that of Halley CHON particles [4]. The less primitive CCs (e.g., CO, CV), OCs and
ECs have all experienced varying degrees of thermal metamorphism that has modified
their organics. At least for the IOM, the less primitive chondrites seem to have accreted
similar material to the primitive CCs [4].
The D/H ratio of water is expected to have increased with increasing radial distance
from the Sun, and therefore can potentially constrain the relative formation distances
of planetesimals. Most comets have measured water D/H ratios that are roughly twice
the terrestrial ratio. Except for the CRs, CCs have water-OH D/H ratios that are less
than the terrestrial ratio [5]. The CRs have a water-OH ratio that is slightly higher than
terrestrial. The OC and R chondrites, on the other hand, have water-OH D/H ratios that
are, respectively, comparable to and higher than comets.
The D/H results for the chondrites are the reverse of what is expected from the
predictions of formation distances made by the dynamical models. However, it is unlikely
that the OC and R chondrites formed at or beyond the formation location of the measured
comets. Rather, it seems likely that their water-OH has been enriched in D by isotopic
fractionation during oxidation of Fe by water [6]. This process has probably also affected
the CCs to varying degrees, so all their D/H ratios are upper limits. Consequently, it is
unlikely that the CCs formed in the source regions of the comets. In fact, the CCs must
have formed inward of the formation location of Saturn’s moon Enceladus, which has a
comet-like D/H ratio, and may have formed between ~3 AU and ~7AU.
[1] Walsh K. J. et al., (2011) Nature, 475, 206.
[2] Levison H. F. et al., (2009) Nature, 460, 364.
[3] Jewitt D. (2012) Astronom. J., 143, 66.
[4] Alexander C. M. O’D. et al., (2007) GCA, 71, 4380.
15
Al constraints on the origin and history of refractory
components of chondrites
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M. Chaussidon
CRPG-CNRS, Université de Lorraine, Vandoeuvre-lès-Nancy, France, chocho@crpg.cnrs-nancy.fr
The recent developments of high precision Mg isotopic analysis by
MC-SIMS and MC-ICPMS has allowed to make significant advances in
the study and understanding of the 26Al-26Mg systematics in CAIs, AOAs,
Al-rich chondrules and ferro-magnesian chondrules from chondrites.
The determination of mineral isochrons and bulk isochrons for the same
objects, and of precise values for the slopes and intercepts, constrain
the distribution of 26Al and 26Mg in the accretion disk and the timing of
the high temperature events which took place in the disk during its first
few million years of history.
A. Saladino
Co
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Role of non terrestrial minerals in the prebiotic synthesis of
genetic and metabolic apparatuses
16
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Experimental approach of dust processing in protoplanetary
disks and comparison with returned samples
M. Roskosz
UMET Bat. C6, Université de Lille 1, France
In the past decade, a large number of experimental studies have been
dedicated to the processing of analogs of extraterrestrial fine-grained
materials. Traditionally, the results were compared to spectroscopic
signatures collected from ground or from orbiters. More recently, the
opportunity was offered to compare directly experimental results to
materials collected during sample-return missions. For these samples,
the source regions are identified and secondary processing are limited
(and better controlled than for stratospheric dust samples). Therefore,
with such samples in hands, it is possible to study in laboratory the
subtle mechanisms at work during low-temperature crystallization and
irradiation of the dust. Our experimental results, focussing on these
two processes, will be discussed and compared to some features of
recently returned samples (Stardust, Hayabusa).
J. M. Trigo-Rodriguez
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Learning about the degree of aqueous alteration of NEOs from
laboratory IR spectra of primitive Antarctic chondrites»
Institute of Space Sciences (CSIC-IEEC)
17
M ARCOP OLO - R
G. Libourel
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Chondrule formation: quicker and faster?
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CRPG-CNRS, Université de Lorraine, Vandoeuvre-lès-Nancy, France. libou@crpg.cnrs-nancy.fr
Owing to a set of isothermal experiments, I will show that chondrule
formation must be more the result of processes generating crystal
growth by chemical disequilibrium at high temperature, i.e., dC/dt than
processes generating crystallization by cooling rates, i.e., dT/dt (as
in dynamical cooling rate experiments). This finding challenges both
the common view that cooling rate is the only driving force during the
chondrule crystallization, and the reliability of cooling rate values inferred
for producing porphyritic textures [1]. Chondrule thermal histories
with shorter durations of heating at high temperature (i.e., few tens
of minutes) followed by faster cooling rates than those deduced from
furnace simulations (i.e., > 103 K/h) are inferred to match both textural
and chemical constraints of chondrules. Implications on chondrule
formation models [1, 2] will be discussed.
[1] Desch et al., (2012) Meteoritics, 47, 1139-1156.
[2] Alexander and Ebel, (2012) Meteoritics, 47, 1-19.
Sampling the asteroid-comet continuum
M. Gounelle
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LMCM, UMR7202, MNHN-CNRS, 57 rue Cuvier, 75005 Paris
gounelle@mnhn.fr
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Bases on laboratory analyses of chondrites and Stardust cometary
samples, as well as on dynamical studies I will show that there exists
an asteroid-comet continuum. Sampling this continuum is essential for
understanding the formation and early evolution of our Solar System.
18
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D/H measurements in the water of comets using Herschel
D. Bockelee-Morvan and the HSSO team
LESIA, Observatoire de Paris, Section de Meudon.
5, place Jules Janssen. 92195 MEUDON Cedex
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Measurements of isotopic ratios in comets provide key information
about the formation of cometary materials and possible links with other
Solar System primitive bodies and the interstellar medium. The D/H
ratio in water was measured in several Oort cloud comets (OCC) using
different techniques, with most measurements agreeing with a value of
~ 3 x 10-4. The Herschel observatory allowed us to measure for the first
time the D/H ratio in comet 103P/Hartley 2, a Jupiter family comet (JFC)
presumably formed in the Kuiper Belt. The D/H ratio was found to be a
factor of 2 lower than the earlier measurements in Oort cloud comets
and the same as the terrestrial value VSMOW. The D/H ratio was also
measured using Herschel in the long-period comet C/2009 P1 (Garradd).
We will present the D/H ratio measured in comet C/2009 P1 (Garradd)
and discuss the results in the context of previous measurements in
OCCs and JFCs.
19
M ARCOP OLO - R
Organic-mineral interface in the
CI type carbonaceous chondrite Orgueil
Space Policy Institute, Washington DC
University of Wisconsin Madison, WI 53706 USA
pehren@gwu.edu
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P. Ehrenfreund1 and H. Xu2
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The amino acid composition of the CI carbonaceous chondrite
Orgueil is strikingly distinct, suggesting that this meteorite came from
a different type of parent body [1]. We recently exposed a sample from
Orgueil to a simulated Mars environment in a diurnal cyclic mode. The
results indicated substantial destruction of the two major amino acids
glycine and b-alanine and provided evidence for UV-assisted reactions
involving the mineral matrix. We also present a recent study of Orgueil’s
mineral composition using Scanning Transmission Electron Microscopy
(TEM/STEM) and Energy-dispersive X-ray spectroscopy.
[1] Ehrenfreund P. et al., (2001) PNAS, 98, 2139-2141.
The physical properties of dark meteorites
G. J. Consolmagno1, D. T. Britt2, R. J. Macke3, C. P. Opeil3
Specola Vaticana, Vatican City State. gjc@specola.va
University of Central Florida, Orlando, FL, USA
3
Boston College, Chestnut Hill, MA USA
1
2
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We review the density, porosity, magnetic susceptibility, and thermal
properties of low-albedo meteorites including those from three major
classes of carbonaceous chondrites (volatile rich, volatile poor, and
metal rich) and shock-blackened ordinary chondrites. These four
types of meteorite all are characterized by having very low albedos,
making them hard to tell apart by the usual Earth-based remote
sensing techniques. But they are very different in composition (as
will be immediately apparent in the returned samples) and they have
very different physical properties, which in turn will have important
implications for the structure and history of the parent body.
20
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New Evidence for Compositional Diversity Among
Primitive Asteroids
H. Campins1, J. De Leon2, J. Emery3
University of Central Florida, Orlando, Florida, USA.
campins@physics.ucf.edu
2
University of La Laguna,Tenerife, Spain
3
University of Tennessee, Knoxvilee, Tenneesee, USA
1
Recent observations have revealed new and diagnostic spectral
differences among primitive asteroids [1,2,3]. For example, the
reflectance spectra of B-type asteroids in the 0.8–2.5 µm range show a
continuous shape variation, ranging from a monotonic negative (blue)
slope to a positive (red) slope. This spectral trend correlates with a
compositional trend with CM2 chondrites (water-rich, aqueously altered)
as analogs for the reddest spectra, to CK4 chondrites (dry, heated/
thermally altered) as analogs for the bluest ones [1]. In addition, a clear
diversity in the 3µm and 10 µm spectral features of primitive asteroids
may be related to the level of hydration and particle sizes on the
surfaces [2,3]. The implications of these new results on the expected
composition of primitive spacecraft-targeted near-Erath asteroids will
be discussed.
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[1] de León J. et al., (2012) Icarus, 218, 196-206.
[2] Takir D. & Emery J.P. (2012) Icarus, 219, 641-654.
[3] Hargrove K.D. et al., (2012) Icarus, 221,453-455.
21
M ARCOP OLO - R
Characterization of the post-accretion history of the C-type
asteroid sampled by MarcoPolo-R
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L. Bonal, P. Beck, E. Quirico, B. Schmitt, R. Thissen, V. Vuitton
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IPAG, Institut de Planétologie et d’Astrophysique de Grenoble,
UJF-Grenoble 1 / CNRS, France, lydie.bonal@obs.ujf-grenoble.fr
Primitive asteroids (e.g., C-type) are widely considered to contain the least
processed materials. The determination of their physical and compositional
properties may therefore be keys to understand the formation of the Solar
System. However, (i) identifying the post-accretion geological processes and,
(ii) characterizing the modifications induced on the original components are
indispensable prior any interpretations in terms of solar nebula properties.
The activity of the cosmochemistry team at IPAG is focused on the origin and
evolution of carbonaceous matter and water, as constrained through multianalytical characterization (structural, chemical, and isotopic characterization)
of a large panel of primitive cosmomaterials. Sample-return missions to primitive
Near Earth Asteroids, such as MarcoPolo-R, offer a unique opportunity to
strengthen the link between primitive cosmomaterials available in laboratories
(e.g. chondrites) and their asteroidal counterpart and to get an insight on the
early stages of space weathering.
During the workshop a compilation of results, based on the physico-chemical
characterization of chondritic carbonaceous matter and water, will be presented
and interpreted in terms of thermal and shock metamorphism, and aqueous
alteration history.
Are meteorites the parent materials of planets?
H. Palme
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Sektion Meteoritenforschung, Forschungsinstitut und Naturmuseum
Senckenberg, Senckenberganlage 25, D-60325 Frankfurt am Main Germany Palmeherbert@gmail.com
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The bulk Earth composition is roughly chondritic. Enrichment of refractory
and depletion of volatile elements resemble trends in carbonaceous chondrites.
Stable isotopes, however, exclude carbonaceous chondrites as parent material
for the Earth. Meteorite parent bodies formed in separated local reservoirs but
under similar conditions as carbonaceous chondrites.
22
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Mineralogy, O and Mn-Cr isotope systematics of fayalite in type
3 ordinary, CV and CO carbonaceous chondrites: Implications
for dating of aqueous alteration and sources of water ices in
asteroids
A. N. Krot, K. Nagashima, P. Doyle and K. Jogo
HIGP/SOEST, University of Hawai‘i at Manoa, Honolulu, HI 96822,
USA, sasha@higp.hawaii.edu
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Ferroan olivine (Fa50-100) is one of the major minerals in matrices of unequilibrated ordinary
chondrites (UOC) and CV and CO carbonaceous chondrites which experienced a low degree aqueous
alteration and mild thermal metamorphism. It is absent in matrices of extensively aqueously-altered
carbonaceous chondrites (CM, CR2, and CI), chondrites that largerly avoided aqueous alteration
(e.g., Acfer 094 and CR3), and highly-reduced chondrites (EH, EL, and K). The high-temperature,
nebular and low-temperature, asteroidal models have been proposed to explain the origin of ferroan
olivine [1-5]. Here we report on the mineralogy, O and Mn-Cr isotope systematics of the fayalitebearing assemblages in type 3.0-3.1 ordinary (MET 00452, Semarkona, Ngawi), CV (Kaba, Vigarano,
A-8811317), and CO (MAC 88107, EET 90042, Y-81020) chondrites. In these meteorites, nearly
pure fayalite (fa; Fa98-100) associates with magnetite (mgt), hedenbergite, Ni-nearing sulfides, and
phyllosilicates. This mineral paragenesis occurs as (i) coarse-grained intergrowths in interchondrule
matrix, (ii) veins crosscutting fine-grained rims around chondrules; and (iii) overgrowths on olivine
chondrule fragments. On a three-isotope oxygen diagram, fa and mgt in UOCs, CVs and COs
plot along mass-dependent fractionation lines with a slope of ~0.5 and Δ17O values of 4.3±1.1‰, 0.4±0.9‰, and - 1.6±0.9‰, respectively. The inferred initial 53Mn/55Mn ratios in fa from the CVs and
COs are ~3.4×10-6 and ~2.4×10-6, respectively [6]. This corresponds to ~3 and 5 Myr after CV CAIs
having U-corrected Pb-Pb age of 4567.3±0.16 Myr [7].
Based on these observations and thermodynamic analysis [5], we conclude that the fa-bearing
paragenesis in UOCs, CVs, and COs formed during water-rock (water/rock ratio ~0.1-0.2) interaction
at elevated temperatures (~100-200°C) on the chondrite parent asteroids. The observed differences
in Δ17O values of the fa-mgt assemblages in UOCs, CVs and COs suggest that water ices that
accreted into their parent asteroids had different oxygen-isotope compositions. These compositions
are inconsistent with a significant flux of water from the outer Solar System that is expected to be
isotopically heavy (Δ17O > 50‰) as hypothesized in the CO self-shielding models [8-10]. Instead water
in asteroids had a local, inner Solar System origin.
[1] Lauretta et al. 2003. GCA, 65:1337.
[2] Hutcheon et al. 1998. Science, 282:1865.
[3] Krot et al. 2004. Proc. NIPR, 17:154.
[4] Choi et al. 2000. MAPS, 35:1239.
[5] Zolotov et al. 2006. MAPS, 41:1775.
[6] Doyle et al. 2013. LPSC, 44.
[7] Connelly et al. 2012. Science, 338:651.
[8] Yurimoto & Kuramoto. 2004. Science, 305:1763.
[9] Lyons & Young. 2005. Nature, 435:317.
[10] Hashizume et al. 2011. Nature Geoscience, 4:165.
23
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The relationship between chondrules and matrix in chondrites
oP
B. Zanda1,2 and R. Hewins1,2
LMCM-CNRS-UMR7202, MNHN – CP52, 61, rue Buffon, 75005 Paris
France, zanda@mnhn.fr,
2
Earth and Planetary Sciences, Rutgers University, Piscataway,
NJ08855, USA.
hewins@rci.rutgers.edu
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The origin of chondrites and the genetic relationship between different groups remain poorly
understood. The specific mixture of chondrules, refractory inclusions and matrix of chondrites determines
their oxygen isotopic signatures [1] as well as their bulk chemistry, and more specifically their volatile
element budget [2]. Along with redox and metal/silicate fractionation, volatile elementdepletion is a
major process that affected the inner solar nebula and two types of explanation have been competing
over nearly 40 years: (i) in the “two-component” model of Anders [3], the high T components lost
volatiles when they were formed and are now embedded in a volatile-bearing CIcomposition matrix;
whereas (ii) in the “incomplete condensation” model of Wasson & Chou [4], the high T components
formed from incompletely condensed material due to the dissipation of the nebular gas. The latter
hypothesis implies that volatile fractionation predated chondrule formation and seems supported by
variations in matrix
composition and an apparent complementarity with chondrules in carbonaceous chondrites
[e.g. 5]. In-situ analyses of matrices in a suite of CM chondrites with varying degrees of alteration
including different lithologies of the Paris CM breccia, show that matrix compositions vary with the
the local degree of alteration. In Paris, matrix in the less altered zones has a CI composition, while
that of the more altered zones has lost S and chalcophiles and gained Fe and siderophiles [6]. EMP
data for other CM matrices also indicate that their S/Si decreases with the extent of parent-body
alteration [7]. On the other hand, bulk chemical analyses of chondrites (conducted at NHMFL by an
in-situ rastering with LA-ICP-MS) exhibit no difference between more or less altered regions in Paris
[6]. Matrix compositions thus vary with alteration although the bulk rocks remain isochemical. This
suggests local exchange between matrices and high temperature fractions, and a CI composition for
matrices at the time of accretion. These results contradict pre-accretion complementarity between
matrix and the high T fraction as advocated by [5] and support the two-component model of Anders
[3]. They allow these components to be formed independently and accrete in varying proportions to
generate the range of bulk CC compositions. It is thus possible that high T constituants formed near
the Sun were transported over large distances and mixed with matrix in colder regions of the disk,
which would explain their
presence in cometary materials.
Co
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[1] Zanda, B. et al., (2006). EPSL, 248, 650-660.
[2] Zanda, B. et al., (2009). MAPS, A#5280.
[3] Anders E. (1964). Space Sci. Rev., 3, 583-714.
[4] Wasson J.T. & Chou C.-L. (1974). Meteoritics, 9, 69-84.
[5] Bland P. et al. (2005). PNAS, 102, 13755–13760.
[6] Zanda, B. et al., (2011). LPS, A#2040.
[7] Zanda B. et al., (2011). MAPS, A#5358.
24
M ARCOP OLO - R
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The so-called «refractory lithophile» elements in enstatite
chondrites.
oP
J. A. Barrat1, B. Zanda2, C. Bollinger1.
Université Européenne de Bretagne, UBO-IUEM, CNRS UMR 6538,
Place Nicolas Copernic, 29280 Plouzané Cedex, France.
barrat@univ-brest.fr.
2
MNHN & CNRS UMR7202, 61, rue Buffon, 75005 Paris, France.
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We report on the trace element abundances of a series of enstatite chondrites. Our
ICP-MS procedure (adapted from [1]) allows the determination of abundances and ratios
of refractory elements (e.g., REEs+Y, Th, U, Nb, Ta, Sr, Ba) in chondrites with a good
reproducibility (<3% for abundances, < 1.5 % for ratios such as La/Sm, Eu/Eu*, Zr/Hf or
Nb/Ta). In agreement with previous studies (e.g., [2-4]), EL3, EH3, EH4, and some of our
EH-IMB (Abee and Saint Sauveur) samples display basically chondritic abundances and
ratios. The situation is clearly different for all the other EC samples. The EL6 samples
are all light REE depleted and display a small negative Eu anomaly ((La/Lu)n=0.64-0.77,
Eu/Eu*=0.75-0.89). Their patterns are alike those of an oxidized dark inclusion from
Sahara 97158, and the LAP 02225 impact melt. Furthermore, Galim-b display a more
pronounced light REE depletion ((La/Lu)n=0.30-0.40), a small negative Yb anomaly
and a deep negative Eu anomaly (Eu/Eu*=0.18-0.29). The light REE depletion shown
by the impact melted ECs is accompanied by Nb, Sr, Eu, and Ba depletions. Striking
correlations between La/Lu, Nb/Ta, and Eu/Eu* are obtained. We performed a series of
leaching experiments on various ECs in order to constrain the concentrations of trace
elements in leachable sulfides and in silicates (residues). The proportions of REEs and
Nb (among others) in the leachable phases (mainly sulfides) are clearly affected by the
metamorphic history of the meteorites. For example, the Nb budget is largely controlled
by the sulfides in EL6 chondrites, not in EL3s.The ranges of abundances and ratios of
the so-called “lithophile refractory” elements in ECs can be explained by impact-induced
mobilization of sulfides and possibly plagioclase [2]. Vaporization and losses of some
of these elements upon impact cannot be directly rejected, and could account for some
non-chondritic values inferred for planetary or asteroidal bodies (e.g., the Earth, Mercury
and the aubrite parent bodies).
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[1] Barrat J.A. et al. 2008. Meteoritics & Planetary Science, 43: 1759-1775.
[2] Rubin et al. 2009. Geochimica Cosmochimica Acta, 73: 1523-1537.
[3] Kallemeyn G.W. and Wasson J.T. 1985. Geochimica Cosmochimica Acta, 49: 261-270.
[4] Kallemeyn G.W. and Wasson J.T. 1985. Geochimica Cosmochimica Acta, 50: 2153-2164.
25
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The evolution of organic matter in chondrites through secondary
processes on the parent body.
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L. Rémusat1, S. Bernard1, J.-N. Rouzaud2 & C. Le Guillou3
LMCM, UMR CNRS 7202, MNHN, CP 52, 57 rue Cuvier, 75231 Paris,
France, remusat@mnhn.fr
2
Laboratoire de Géologie, UMR CNRS 8538, ENS 24 rue Lhomond,
75231 Paris, France
3
Ruhr-Universität Bochum, Inst. Für Geologie, Mineralogie und
Geophysik, Bochum, Germany
1
The organic matter trapped in carbonaceous chondrites have likely
been synthesized by various chemical reactions before the formation of
the parent body (either during the early stage of the solar system or in
the parent molecular cloud). However, the parent body processes, going
from intense hydrothermal alteration to high temperature metamorphism
have likely induced modifications on the chemical structure [1] and
the H isotopic signature [2]. We will discuss these effects based on
observations on natural samples and laboratory experiments. This
should shed light on the significance to target a non metamorphosed
and poorly to midly hydrated asteroid in order to get useful samples to
understand the origin of organics in the solar system.
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[1] Le Guillou C. et al. (2012). Meteorit. Planet. Sci., 47, 345-362.
[2] Alexander, C. M.O’D. et al., (2010). Geochim. Cosmochim. Acta, 74, 4417-4437.
26
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The organic content of primitive carbonaceous meteorites
Z. Martins
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Imperial College London, Department of Earth Science and Engineering,
South Kensington Campus, UK
z.martins@imperial.ac.uk
Carbonaceous chondrites contain many biologically revelant organic compounds that
may have been involved in the origin and evolution of life on Earth. The abundance
and distribution of the soluble organic compounds present in different carbonaceous
meteorites seem to reflect the different degrees of thermal metamorphism and aqueous
alteration processing in their parent body. Aqueous alteration has showed to influence the
amino acid content. The relative abundance of b-amino acids/glycine seem to increase
with increasing aqueous alteration on the meteorite parent body [1-3]. In relation to
a-amino acids, it has been stated by [1,2] that meteorites with a high degree of aqueous
alteration have a lower relative abundance of a-AIB. However, the data from [3,4] did not
show a trend for the relative abundance of a-AIB versus aqueous alteration in the CM1
and CM2 chondrites analysed.
The soluble organic matter may also be influenced by the metamorphic temperature in the
meteorite parent body. The type 3 chondrites have been suggested to contain the most
pristine matter owing to their relatively unaltered metamorphic and petrological histories
[5,6]. While CV3 chondrites were reported to contain only low to trace levels of amino
acids [7,8], the CR3s MET00426 and QUE 99177 possess high amino acid abundances
[9,10]. On the other hand the amino acid contents of the CO3s Colony and Ornans were
found to be generally lower than most carbonaceous chondrites but contained unusually
high relative abundances of b-alanine and g-ABA [11]. It is possible that these amino acids
present in type 3 carbonaceous chondrites may be formed from Fischer-Tropsch ⁄ HaberBosch type gas-grain reactions after the meteorite parent body cooled to much lower
temperatures [12,13] or during the cooling process in the parent body still at elevated
temperatures but lower than 500ºC [14].
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[1] Glavin D.P. et al. (2006) Meteorit. Planet. Sci., 41, 889-902. [2] Glavin D.P. et al.
(2010) Meteorit. Planet. Sci., 45, 1948-1972. [3] Martins Z. et al., Geochim. Cosmochim.
Acta, submitted. [4] Botta O. et al. (2007) Meteorit. Planet. Sci., 42, 81–92. [5] McSween
H.Y. (1979) Rev. Geophysics, 17, 1059–1078. [6] Bonal L. et al. (2007) Geochim.
Cosmochim. Acta, 71, 1605–1623. [7] Cronin J.R. and Moore C.B. (1971) Science, 172,
1327–1329. [8] Cronin J.R. and Moore C.B. (1976) Geochim. Cosmochim. Acta, 40,
853–857. [9] Glavin D.P., et al. (2011) Meteoritics & Planetary Science 45, 1948–1972.
[10] Pizzarello, S. et al. (2012) Proc. Nat. Acad. Sci. USA, 109, 11949–11954. [11] Chan
H.-S. et al. (2012) Meteorit. Planet. Sci., 47, 1502-1516. [12] Glavin D.P. et al. (2010)
Meteorit. Planet. Sci., 45,1695–1709. [13] Burton A.S. et al. (2011) Meteorit. Planet. Sci.
46, 1703–1712. [14] Rodante F. et al. (1992) Thermochim. Acta, 194, 197–213.
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Resolving models for aqueous alteration of primitive meteorites
by sample return
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M.R. Lee1, P. Lindgren1 , M.R. Sofe1, I. Franchi2 and N. Starkey2
School of Geographical and Earth Sciences, University of Glasgow, Glasgow G12 8QQ. U.K. Martin.Lee@Glasgow.ac.uk
2
Planetary & Space Sciences Research Institute, Open University, Milton Keynes, MK7 6 AA, UK.
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The carbonaceous chondrite meteorites contain minerals including phyllosilicates
and carbonates that crystallized from aqueous solutions in parent body interiors, yet they
have retained primitive bulk chemical compositions. This apparent contradiction between
meteorite mineralogy and chemistry can be reconciled only if the fluids that mediated
alteration were static so that the reactions took place in a chemically closed system [1].
Numerical simulations of the thermal evolution of carbonaceous chondrite asteroids
however consistently predict that hydrothermal convection would have been operative so
that alteration would have been chemically open [2]. The closed and open system models
have very different implications for the mechanisms and chronologies of parent body
evolution and the present-day internal structure of primitive asteroids.
Our work on the CM carbonaceous chondrites has found clear evidence for multiple
episodes of aqueous alteration. For example in Pollen (CM2) there are two generations
of calcite, the first a cement and the second replacive of olivine. Prior to the second
generation, the calcite cement was partially replaced by phyllosilicates. NanoSIMS
analyses of another two generations of calcite in the LON 94101 (CM2) meteorite
reveal that they have contrasting oxygen isotope compositions that are consistent with
crystallization from aqueous solutions of a very different provenance and/or temperature.
Results of this work are more consistent with a system that was open, albeit non
necessarily continuously, than one that was closed with static fluids.
It may remain difficult to answer these very fundamental questions about the histories
and properties of primitive parent bodies using the fragmentary meteorite record. The
different models of aqueous alteration can be tested much more effectively by sample
return. For example small bodies altered by static fluids should have a uniform degree
of alteration whereas larger bodies should have a compositional zoning or layering
reflecting paths of fluid flow. In addition, samples can be collected that are too fragile to
survive ejection from the parent body and Earth entry but may provide critical information
on paths of fluid flow.
[1] Bland P.A. et al., (2009) Earth Planet. Sci. Lett., 287, 559–568.
[2] Palguta J. et al., (2010) Earth Planet. Sci. Lett., 296, 235–243.
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A. Davis
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New analytical techniques for samples returned to Earth by
spacecraft
Noble gas studies of asteroidal matter returned by Marco Polo-R
U. Ott1,2
1
2
Max-Planck-Institut für Chemie, Mainz, Germany
University of West Hungary, Szombathely, uli.ott@mpic.de
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Noble gases are trace elements par excellence and often clearly bear a record
of processes barely visible in other elements. Primary among these is the cosmic ray
exposure history and the exposure to the solar wind in the asteroidal regolith. Compared
to meteorites, more complete and unadulterated information can be extracted from
material obtained by a sample return mission. Besides the case of the Moon; valuable
insight has been obtained from the analysis of a few grains from asteroid Itokawa returned
by Haybusa [1]. Compared to the latter, material returned by Marco Polo-R will provide
results for an asteroid from a different region in the Solar System and the much larger
amount to be returned will allow more prepresentative analyses.
Complementing a general comparison with Moon and Itokawa, in particular with
regard to regolith dynamics, a study of chondrules, if present, will be of high interest.
At least in some cases (e.g. CM2 Murchison [2] and CR2 El Djouf [3]) pre-irradiation
appears to have occurred in the parent body regolith, although on a very different scale.
Results may bear on the question on whether pre-irradiation (also) occurred in the solar
nebula.
Another constructive comparison will be with micrometeorites, which currently
dominate the extraterrestrial flux on Earth. Commonly, they are considered to be similar
to CM carbonaceous chondrites [4], but recent work is indicative of a larger variety of
sources [5, 6, 7]. Finally, xenon as the ultimate trace element may serve as a sensitive
tracer for the presence in bulk of unusual materials, such as grains of stardust (see review
[8]).
[1] Nagao K. et al., (2011). Science, 333, 1128-1131.
[2] Roth A.S.G. et al., (2011). MAPS, 46, 989–1006.
[3] Beyersdorf-Kuis U. et al., (2012). 75th Annual Meteor. Soc. Meeting, #5036
[4] Engrand C. and Maurette M., (1998). MAPS, 33, 565–580.
[5] Genge M.J. et al., (2008). MAPS, 43, 497–515.
[6] van Ginneken M. et al., (2012). MAPS, 47, 228–247.
[7] Baecker B. et. al., (2012). 75th Annual Meteoritical Society Meeting.
[8] Ott U. (2003). Space Sci. Rev., 106, 33-48.
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Measuring Xenon and Krypton in Primitive Material
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University of Manchester, United Kingdom,
jamie.gilmour@manchester.ac.uk
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J. D. Gilmour
The heavy noble gases krypton and xenon provide many different avenues
to understand the history of primitive material. Characteristic isotopic signatures
are left by the decay of short-lived radioisotopes (129I and 244Pu) and the
presence of presolar material. The source of trapped gases can be investigated
through the elemental ratio, and the duration of exposure to cosmic rays can
be determined by 81Kr-Kr analyses. Neutron irradiation of samples allows other
elements, especially halogens, to be determined by noble gas analysis. I will
describe current instrumentation based on resonance ionization for xenon and
krypton analysis, outline plans for future developments, and discuss applications
and sample requirements.
Taking apart sample return grains, atom by atom.
I. Lyon1, T. Henkel1, A. King1,2, A. Sattaur1,3
School of Earth, Atmospheric and Environmental Sciences,
The University of Manchester, Manchester M13 9PL, UK.
2
Natural History Museum, Cromwell Road, London SW7 5BD.
3
Dept of Physics, University of York. Ian.Lyon@manchester.ac.uk
1
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The return of micrometre-scale asteroid grains by the Hayabusa mission [1] showed that
techniques to analyse such samples must be as close to 100% efficient as possible in order
to maximise the elemental, isotopic and structural information extracted from the grains
which tell their formation and history. Secondary ion analytical techniques are widely
used for analysis and we show how Time of Flight Secondary Ion Mass Spectrometric
analyses of presolar grains may be used as analogues for asteroid grains to obtain an
understanding of how the sputtering of micrometre-sized grains during analysis proceeds
[2,3] and the advantages and drawbacks of such an approach.
[1] Nakamura et al., (2011). Science, 333, 1113-1116.
[2] King et al., (2012). Meteor. & Planet. Sci., 47, 1624-1643.
[3] Henkel et al., (2012). LPSC, 43, #2135
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Ion microprobe U-Pb dating of a single apatite grain in meteorites
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Y. Sano1, N. Takahata1, M. Koike1 and K. Terada2
Atmosphere and Ocean Research Institute, University of Tokyo,
Kashiwa, Chiba 277-8564, Japan. ysano@aori.u-tokyo.ac.jp
2
Department of Earth and Space Science, Osaka University, Toyonaka
560-0043, Japan
1
We develope an in-situ U-Pb dating method of a single apatite
grain using a NanoSIMS instrument installed at Atmopshere and
Ocean Research Institute, University of Tokyo. Apatite is a common
accessory U-bearing mineral and has higher closure temperature of
500-600˚C [1]. Since the mineral shows wider occurrence than zircon
in meteorites, the method may provide key information on the early
solar system. We have already reported the analytical procedure of
the U-Pb system using a SHRIMP installed at Hiroshima University [2]
and its successful applications to thermal metamorphism of ordinary
chondrites [3], volcanic ages of some Martian meteorites [4], and Lunar
meteorites [5]. Since the NanoSIMS has a higher primary beam intensity
at smaller spot size, it is suitable for tiny apatite grains even though its
lower precision than SHRIMP. The combination of both NanoSIMS and
SHRIMP dating methods may provide significant information on the
choronology of the asteroidal matter returned by Marco Polo-R as well
as Hayabusa and Hayabusa II.
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[1] Krogstad E.J. and Walker R.J. (1994). GCA, 58, 3845–3853.
[2] Sano Y. et al. (1999). Chem. Geol., 153, 249-258.
[3] Terada K. and Sano, Y. (2002). GRL, 29 doi:10.1029/2001 GL013945.
[4] Sano Y. et al. (2000). MAPS, 35, 341-346.
[5] Terada K. et al. (2007). Nature, 450, 849-852.
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Non destructive characterization of extraterrestrial materials:
techniques and applications of magnetism.
P. Rochette
CEREGE UMR6635, Aix-Marseille Université CNRS
Europole de l’Arbois BP80,13545 Aix en Provence Cedex 4, France
rochette@cerege.fr
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Non destructive and invasive techniques are fundamental for a sample
return mission. Regolith sampling may provide very heterogenous
material and indentification of different lithologies is an important
aspect. We will review the applications of magnetic measurement
to the characterization of extraterrestrial material, in particular on
carbonaceous chondrites (CC). The majority of CC have their magnetic
properties carried by 1 to 10% of magnetite [1]. Magnetite content may
be highly homogeneous, or heterogeneous in case of complex breccias
like Sutter Mill. The recent finding of significant large magnetic field
recorded in some CC pose the question of the possibility of dynamo
action in a CC parent body [2], implying some sort of differenciation.
Sample return from a CC like asteroid will allow to further constrain this
field intensity.
[1] Rochette P. et al., 2008. Meteorit. Planet. Sci., 43: 959-980.
[2] Carporzen L. et al., 2011. Proc. Nat. Acad. Sci. U.S.A. 108, 6386.
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N. A. Starkey & I. A. Franchi
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Oxygen Isotopic Measurements of Fine Grained Primitive
Material; The Challenge of Small Samples.
Planetary and Space Sciences, The Open University, Walton Hall,
Milton Keynes, MK7 6AA.
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Cometary interplanetary dust particles (IDPs), collected in the
Earth’s stratosphere, currently represent the best way to sample outer
Solar System primordial dust. The fine-grained (sub-µm) minerals
of IDPs show strong similarities to the textures expected for primary
condensates from the solar nebula. We have analysed IDPs for bulk
carbon, nitrogen and hydrogen isotopes, and high precision oxygen
isotopes by NanoSIMS 50L which allows us to combine all of these
techniques on an individual <20µm IDP fragment. This analytical
approach allows for a comparison of the organic, silicate and presolar
grain reservoirs in primitive materials, probing the earliest processes
occurring in the protoplanetary disk. Oxygen isotope analyses reveal
that some IDPs are more 16O-rich than any bulk meteorite compositions,
extending to O-isotope compositions in between chondritic- and solarlike values (d17O = -20‰, d18O = -20‰). The 16O-rich IDPs display more
primitive organic signatures than the chondritic-like 16O-poor IDPs but,
rather interestingly, they also have lower presolar grain abundances.
The 16O-poor signatures probably indicate an abundant component
of chondritic-like material, processed in the inner protoplanetary disk.
These analyses can be used to better understand the accretion,
mixing and distribution of primitive reservoirs in the Solar System, and
ultimately, how these came together in the cometary and asteroidal
parent bodies. Such studies are a useful preparation for future sample
return missions of primitive Solar System materials.
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Implications for curation of the Marco-Polo samples from recent
Hayabusa analyses
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M. Zolensky
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KT NASA Johnson Space Center, Houston, TX 77058, USA
Recent TEM investigations of the returned Itokawa samples reveal
that despite the fact that they have never been exposed to 1 atm of
terrestrial air, they are beginning to alter. The bulk of the alteration is
changing the space exposure record, which significantly reduces the
value iof these samples. The implication of this observation is that
samples returned from an asteroid should best be recovered from a
sealed capsule, and stored in a vacuum or very inert gas (curation
grade nitrogen has proved to be insufficient to the task).
Curation of the samples returned by Marco Polo-R:
state of the art
J. Aléon1, and the curation facility working group
1
CSNSM, CNRS/IN2P3-Univ. Paris Sud, 91405 Orsay, France,
jerome.aleon@csnsm.in2p3.fr
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The Marco Polo-R space mission is planned to return to the Earth
samples of a C-type asteroid for studies by state-of-the-art laboratory
analytical facilities in order to better understand the very first million
years of our solar system. The definition of a curation protocol is a critical
issue for all sample return space missions, to make samples available
for the scientific community with minimal terrestrial contamination,
maximal safety and as rapidly and conveniently as possible to maximize
the scientific outreach. This presentation will report the current state of
the discussion regarding key aspects of this protocol. Such key aspects
include notably location, contamination control, safety, sample handling
(and eventually preparation) for laboratory analysis, sample storage
and allocation procedures.
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Curatorial facilities for sample return missions – requirements
and considerations
C. L. Smith1 and M.M. Grady
Department of Earth Sciences, The Natural History Museum, Cromwell
Road, London, SW7 5BD, UK.
1
The curation of samples is a critical element of any sample return
space mission. Top level mission requirements state that the ‘scientific
integrity’ of the samples is retained from sample collection through to
curation post-return. The design and operation of a curatorial facility
must ensure that the samples are not damaged or compromised, e.g.
through contamination or physical operations such as handling and
even poor documentation.
Chemical and isotopic characterization of asteroidal matter in the
Goëttingen
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A. Pack
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University of Göttingen, Geoscience Center, Goldschmidtstraße 1
37077 Göttingen.
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Noble Gases in (Cometary) Interplanetary Dust and samples
returned from comet Wild 2 and asteroid Itokawa Status and Plans.
H. Busemann1, N. Spring1, J.D. Gilmour1, S.A. Crowther1,
L.R. Nittler2
SEAES, University of Manchester
DTM, Carnegie Institution of Washington
henner.busemann@manchester.ac.uk
1
2
Noble gases are important to understand the origin, transport,
evolution (which includes, e.g., incorporation, loss, radioactive growth,
spallogenic production, or mixing) of the volatile elements in the solar
system. For example, comets could have played a role for the delivery
of volatiles to the inner solar system. Also, relative elemental noble gas
abundances in cometary ices may indicate the formation temperatures
and location. However, except for a few studies [e.g., 1], the noble
gases in comets remain relatively unconstrained.
Here we summarize our current programme to identify cometary
interplanetary dust particles (IDPs, [2-5]), characterize their heavy
noble gas contents by resonance ionization mass spectrometry [6], and
present plans for the detection of Kr and Xe in samples returned by
the Stardust mission. Furthermore, we will discuss our collaboration
to study noble gases in “Hayabusa” samples returned from asteroid
Itokawa.
[1] Marty B., et al., (2008). Science, 319, 75-78.
[2] Busemann H. et al. (2009). EPSL, 288, 44-57.
[3] Busemann H. et al. (2010). LPSC, 41, #1947.
[4] Spring N.H. & Busemann H. (2011). M&PS Suppl., 46, #5519.
[5] Spring N.H., et al. (2012). M&PS Suppl., 47, #5394.
[6] Gilmour J.D. (2012). this meeting.
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Chondritic Kr and Xe: result of irradiation processes in the
accretion disk ?
M. Moreira
IPGP
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We propose a scenario for the origin of the chondritic Kr and Xe
(Phase Q) based on irradiation processes in the solar system. The
model of irradiation is able to explain the isotopic compositions observed
in the so-called Phase Q, which is the carrier of heavy noble gases. We
will also discuss the origin the observed Kr and Xe in CO2-well gases,
which are the most precise noble gas data obtained on Earth, in the
light of the calculations obtained with the proposed model.
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