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16 results on '"Toppani A"'

1. Combining IR and X‐ray microtomography data sets: Application to Itokawa particles and to Paris meteorite

Author

Akira Tsuchiyama, David Troadec, Tomoki Nakamura, Rosario Brunetto, Zahia Djouadi, Christophe Sandt, Anne Cécile Buellet, Alessandra Rotundi, Donia Baklouti, Ferenc Borondics, Alice Aléon-Toppani, Andrew King, Stefano Rubino, Z. Dionnet, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Physiogénomique / NeuroTranscriptomes et Paléogénétique (LPG), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), Tohoku University [Sendai], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), SMIS Beamline, Synchrotron SOLEIL, Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Centrale de Micro Nano Fabrication - IEMN (CMNF - IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Division of Earth and Planetary Sciences [Kyoto], Kyoto University, Centre National d’Etudes Spatiales, Agence Nationale de la Recherche, This work is supported by the 'IDI 2015' project funded by the IDEX Paris-Saclay (Grant ANR-11-IDEX- 0003-02). The FT-IR microspectroscopy activities are supported by grants from Région Ile-de-France (DIM-ACAV) and SOLEIL. This work has been funded by the Centre National d’Etudes Spatiales (CNES-France, Hayabusa2 mission) and by the ANR project CLASSY (Grant ANR-17-CE31-0004-02) of the French Agence Nationale de la Recherche. This work was partly supported by the French RENATECH network. We wish to thank the Italian Space Agency (ASI, Italy) contract no. I/024/12/2 and MIUR, contracts PNRA16-00029 and PRIN2015-20158W4JZ7. We are grateful to the JAXA Curator for allocating the Hayabusa particles. We thank T. Yada and L. Bonal for useful discussion, B. Zanda for providing the Paris meteorite sample, and the ANATOMIX team (SOLEIL) for their help with Avizo., Renatech Network, ANR-11-IDEX-0003,IPS,Idex Paris-Saclay(2011), ANR-17-CE31-0004,CLASSY,Composition des surfaces du Système Solaire de bas albédo(2017), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Centrale de Micro Nano Fabrication - IEMN (CMNF-IEMN), and Kyoto University [Kyoto]

Subjects
[SPI]Engineering Sciences [physics], Geophysics, X-ray microtomography, Materials science, Meteorite, Space and Planetary Science, 0103 physical sciences, Mineralogy, 010502 geochemistry & geophysics, 010303 astronomy & astrophysics, 01 natural sciences, 0105 earth and related environmental sciences
Abstract

International audience; In the near future, a new generation of sample return missions (Hayabusa2, OSIRIS-REx, MMX, etc.) will collect samples from small solar system bodies. To maximize the scientific outcome of laboratory studies and minimize the loss of precious extraterrestrial samples, an analytical sequence from less destructive to more destructive techniques needs to be established. In this work, we present a combined X-ray and IR microtomography applied to five Itokawa particles and one fragment of the primitive carbonaceous chondrite Paris. We show that this analytical approach is able to provide a 3-D physical and chemical characterization of individual extraterrestrial particles, using the measurement of their 3-D structure and porosity, and the detection of mineral and organic phases, and their spatial co-localization in 3-D. We propose these techniques as an efficient first step in a multitechnique analytical sequence on microscopic samples collected by space missions.

Published
2020
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2. NORTHWEST AFRICA (NWA) 12563 and ungrouped C2 chondrites: Alteration styles and relationships to asteroids

Author

R. Maupin, R. H. Hewins, Zahia Djouadi, J. Gattacceca, Alice Aléon-Toppani, V. Malarewicz, Ashley J. King, Hugues Leroux, Sylvain Courrech du Pont, C. Le Guillou, Pierre-Marie Zanetta, Damien Deldicque, Z. Dionnet, Thomas Rigaudier, Sylvain Bernard, Rosario Brunetto, Laurette Piani, C. Sognzoni, Ferenc Borondics, Brigitte Zanda, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Unité Matériaux et Transformations - UMR 8207 (UMET), Centrale Lille-Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de géologie de l'ENS (LGENS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), ANR-19-CE31-0027,HYDRaTE,Distribution of HYdrogen in the protoplanetary Disk and deliveRy to the Terrestrial planEts(2019), ANR-10-LABX-0038,P2IO,Physics of the 2 infinities and the origins(2010), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Centrale Lille Institut (CLIL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris)

Subjects
Chondrite parent bodies, Olivine, Chemistry, Geochemistry, Chondrule, Hyperspectral cartography, Pyroxene, engineering.material, 010502 geochemistry & geophysics, 01 natural sciences, Parent body, Silicate, Porphyritic, Chondrite-asteroid connection, chemistry.chemical_compound, Geochemistry and Petrology, Chondrite, [SDU]Sciences of the Universe [physics], 0103 physical sciences, engineering, Phenocryst, C2-ungrouped chondrites, Amorphous silicate, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

International audience; Many asteroids in the main belt have spectra like those of Mighei-type CM chondrites, but some Near Earth Objects (NEO) resemble less well known types of C2 chondrite. Northwest Africa (NWA) 12563, a new find with affinities to C2 chondrites, could help us understand the differences between observations of CM2 chondrites and bodies that are currently being studied by the Hayabusa2 and OSIRIS-REx space missions. NWA 12563 contains 14% chondrules supported by 86% fine grained matrix consistent with CM2 chondrites, but differs from them in other respects. In both matrix and chondrules, olivine is unaltered and pyroxene shows incipient alteration. Metal in chondrules is pseudomorphed by serpentine, and mesostasis is replaced by serpentine-saponite and chlorite. Many Type I chondrules have highly irregular shapes resulting from fracturing and selective metal replacement. Type II porphyritic chondrules are clusters of phenocrysts set in matrix-like material. Type II chondrules may be kinked and partially disbarred. The matrix of NWA 12563 differs from CM2 chondrites in the absence of tochilinite-cronstedtite intergrowths. It contains hydrated and oxidized amorphous silicate (Fe3+/∑Fe ~75%) richer in magnesium than in other chondrites (with embedded sulfides). Serpentine-saponite is also present, as well as abundant framboidal magnetite.NWA 12563 has similarities to a number of ungrouped magnetite-rich and 18O-rich chondrites (Bells, Essebi, Niger I, WIS 91600, Tagish Lake, and MET 00432) that we call C2-ung1, as opposed to C2-ung2 chondrites (poorer in 18O and magnetite). The oxygen isotopic composition coupled with a magnetic susceptibility of log χ = 4.67 places NWA 12563 with these ungrouped chondrites in a cluster distinct from CM2 chondrites. NWA 12563 is closest to WIS 91600 among the C2-ung1 chondrites in alteration style and light element compositions. WIS 91600, however, has suffered light thermal metamorphism, suggesting that NWA 12563 might represent its altered but unheated precursor material within the same parent body if it were zoned. The average Vis-NIR spectrum of NWA 12563 matches the asteroid taxonomic class K and resembles that of CO3 Frontier Mountain (FRO) 95002, but its spectra range from very “red” in dark matrix areas and very “blue” in magnetite-rich areas. The average MIR spectrum shows features indicating phyllosilicates, aliphatic CH compounds, hydrated silicates, and olivine. It is significantly different from those of other chondrites including FRO 95002, and closest to Bells (from which it differs in carbon isotopic composition) and WIS91600. The variety of mineralogical, chemical and isotopic properties among C2-ung1 chondrites requires several different parent bodies. However, the high abundance of magnetite common to this cluster of ungrouped chondrites, and to a lesser extent CI chondrites, indicates that they should be considered as possible material from Bennu, which has an 18 µm magnetite signal in its spectrum not seen in the CM2 chondrites (Hamilton et al., 2019).

Published
2021
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3. A preparation sequence for multi‐analysis of µm‐sized extraterrestrial and geological samples

Author

Alice Aléon-Toppani, François Brisset, Jérôme Aléon, David Troadec, Michael E. Zolensky, Ferenc Borondics, Rosario Brunetto, Daniel Lévy, Andrew King, Stefano Rubino, Z. Dionnet, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Physics of Complex Systems, Weizmann Institute of Science [Rehovot, Israël], Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-JUNIA (JUNIA), Université catholique de Lille (UCL)-Université catholique de Lille (UCL), Centrale de Micro Nano Fabrication - IEMN (CMNF - IEMN), Université catholique de Lille (UCL)-Université catholique de Lille (UCL)-Centrale Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-JUNIA (JUNIA), Institut de Chimie Moléculaire et des Matériaux d'Orsay (ICMMO), Institut de Chimie du CNRS (INC)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), PSICHÉ beamline, Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), his work was partly supported by the French RENATECH network, grants from Ile de France (DIM-ACAV) and SOLEIL (IR microscopic analyses), and grants from LabeX CHARMMMAT, LaSIPS, and Region Ile de France (TEM). It was also supported by the CNRS INSU PNP National Planetary Programme and by the CentreNational d’Etudes Spatiales (CNES-France, Hayabusa2 mission), Renatech Network, ANR-11-LABX-0039,CHARMMMAT,CHimie des ARchitectures MoléculairesMultifonctionnelles et des MATériaux(2011), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and Centrale Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-JUNIA (JUNIA)-Centrale Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-JUNIA (JUNIA)

Subjects
[SPI]Engineering Sciences [physics], Geophysics, Materials science, Space and Planetary Science, Extraterrestrial life, 0103 physical sciences, Mineralogy, 010502 geochemistry & geophysics, 010303 astronomy & astrophysics, 01 natural sciences, 0105 earth and related environmental sciences, Sequence (medicine)
Abstract

International audience; With the recent and ongoing sample return missions and/or the developments of nano-to microscale 3-D and 2-D analytical techniques, it is necessary to develop sample preparation and analysis protocols that allow combination of different nanometer-to micrometer-scale resolution techniques and both maximize scientific outcome and minimize sample loss and contamination. Here, we present novel sample preparation and analytical procedures to extract a maximum of submicrometer structural, mineralogical, chemical, molecular, and isotopic information from micrometric heterogeneous samples. The sample protocol goes from a nondestructive infrared (IR) tomography of~10 to~70 µm-sized single grains, which provides the distribution and qualitative abundances of both mineral and organic phases, followed by its cutting in several slices at selected sites of interest for 2-D mineralogical analysis (e.g., transmission electron microscopy), molecular organic and mineral analysis (e.g., Raman and/or IR microspectroscopy), and isotopic/chemical analysis (e.g., NanoSIMS). We also discuss here the importance of the focused ion beam microscopy in the protocol, the problems of sample loss and contamination, and at last the possibility of combining successive different analyses in various orders on the same micrometric sample. Special care was notably taken to establish a protocol allowing correlated NanoSIMS/TEM/IR analyses with NanoSIMS performed first. Finally, we emphasize the interest of 3-D and 2-D IR analyses in studying the organics-minerals relationship in combination with more classical isotopic and mineralogical grain characterizations.

Published
2021
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4. Vis–NIR Reflectance Microspectroscopy of IDPs

Author

Rosario Brunetto, Alice Aléon-Toppani, Romain Maupin, Pierre Vernazza, Zahia Djouadi, Cateline Lantz, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and ANR-16-CE29-0015,RAHIIA_SSOM,Analyses de résidus provenant d'analogues de glace interstellaire pour la compréhension de la formation de la matière organique du Système Solaire(2016)

Subjects
Astronomy and Astrophysics, 010502 geochemistry & geophysics, 01 natural sciences, Reflectivity, Astrobiology, Geophysics, Interplanetary dust cloud, Meteorite, 13. Climate action, Space and Planetary Science, Asteroid, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Spectroscopy, 010303 astronomy & astrophysics, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

Visible near-infrared (Vis–NIR) reflectance spectroscopy is a powerful nondestructive technique allowing the parent bodies identification of cosmomaterials such as meteorites, micrometeorites, and interplanetary dust particles (IDPs) studied in the laboratory. Previous studies showed that meteorites do not represent the full diversity of the solar system small bodies. We present here an experimental setup we developed for measuring Vis–NIR microspectroscopy of individual IDPs. We acquired diffuse Vis–NIR reflectance spectra of 15 particles ranging 7–31 μm in size. We discuss the requirements, the abilities, as well as the limitations of the technique. For sizes smaller than 17 μm, the slopes increase with decreasing particles sizes, while for sizes larger than 17 μm, the slopes are randomly distributed. The visible reflectance levels do not appear to be affected by the size of the IDPs, and show a bimodal distribution. Among the studied particles, we identified an IDP (L2079C18) exhibiting a feature at 0.66 μm, which is similar to the one observed by remote sensing on the surface of hydrated asteroids. This is the first detection of a hydration band in the reflectance spectrum of an IDP that could indicate a possible link between hydrated IDPs with hydrated asteroid surfaces.

Published
2020
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5. Alkali magmatism on a carbonaceous chondrite planetesimal

Author

Alice Aléon-Toppani, François Brisset, Kevin D. McKeegan, Jacques-Marie Bardintzeff, Jérôme Aléon, Bernard Platevoet, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Géosciences Paris Saclay (GEOPS), Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California-University of California, Institut de Chimie Moléculaire et des Matériaux d'Orsay (ICMMO), Institut de Chimie du CNRS (INC)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), and University of California (UC)-University of California (UC)

Subjects
Planetesimal, Multidisciplinary, 010504 meteorology & atmospheric sciences, Partial melting, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, 010502 geochemistry & geophysics, 01 natural sciences, Mantle (geology), Astrobiology, Meteorite, 13. Climate action, Chondrite, [SDU]Sciences of the Universe [physics], Carbonaceous chondrite, Physical Sciences, Formation and evolution of the Solar System, Planetary differentiation, Geology, 0105 earth and related environmental sciences
Abstract

International audience; Recent isotopic and paleomagnetic data point to a possible connection between carbonaceous chondrites and differentiated planetary materials, suggesting the existence, perhaps ephemeral, of transitional objects with a layered structure whereby a metal-rich core is enclosed by a silicate mantle, which is itself overlain by a crust containing an outermost layer of primitive solar nebula materials. This idea has not received broad support, mostly because of a lack of samples in the meteoritic record that document incipient melting at the onset of planetary differentiation. Here, we report the discovery and the petrologic–isotopic characterization of UH154-11, a ferroan trachybasalt fragment enclosed in a Renazzo-type carbonaceous chondrite (CR). Its chemical and oxygen isotopic compositions are consistent with very-low-degree partial melting of a Vigarano-type carbonaceous chondrite (CV) from the oxidized subgroup at a depth where fluid-assisted metamorphism enhanced the Na content. Its microdoleritic texture indicates crystallization at an increasing cooling rate, such as would occur during magma ascent through a chondritic crust. This represents direct evidence of magmatic activity in a carbonaceous asteroid on the verge of differentiating and demonstrates that some primitive outer Solar System objects related to icy asteroids and comets underwent a phase of magmatic activity early in the Solar System. With its peculiar petrology, UH154-11 can be considered the long-sought first melt produced during partial differentiation of a carbonaceous chondritic planetary body, bridging a previously persistent gap in differentiation processes from icy cometary bodies to fully melted iron meteorites with isotopic affinities to carbonaceous chondrites.

Published
2020
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6. Determination of optical constants from Martian analog materials using a spectro-polarimetric technique

Author

Rosario Brunetto, O. Mivumbi, V. Godard, Alice Aléon-Toppani, E. Garcia-Caurel, C. Boukari, R. G. Urso, François Poulet, Ferenc Borondics, John Carter, G. Alemanno, FRA, Institut d'astrophysique spatiale (IAS), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)

Subjects
Complex data type, Materials science, 010504 meteorology & atmospheric sciences, Infrared, business.industry, Optical constants Mars surface Spectroscopy Ellipsometry Laboratory, Polarimetry, Physics::Optics, Astronomy and Astrophysics, 01 natural sciences, Characterization (materials science), Optics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Ellipsometry, 0103 physical sciences, Light beam, Bidirectional reflectance distribution function, business, Spectroscopy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

The technique of spectroscopic ellipsometry is a powerful tool for the characterization of the optical properties of materials. This technique represents a significant refinement over the semi-empirical approach to optical constants determination using BRDF (Bidirectional Reflectance Distribution Function) measurements of a finite set of grain sizes for each mineral. It also allows obtaining, not only the optical constants, but also information about the dependence of optical response on sample orientation respect to the illuminating light beam. In this work, we present our experimental approach to derive optical constants of Martian analogue materials based on an infrared ellipsometry technique. We derived the optical constants of gypsum between 750 and 5000 ​cm−1 (2–13 ​μm) using data obtained with an infrared spectroscopic Mueller ellipsometer. Thanks to the high sensitivity of the ellipsometric measurements, and despite of a rather complex data analysis protocol, the results obtained for the gypsum samples show that it is possible to successfully use this technique for direct determination of optical constants of natural minerals. The method discussed here can provide the planetary science community with laboratory derived optical constants of a large number of minerals and materials (either natural or synthetic).

Published
2020
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7. NanoSIMS imaging of D/H ratios on FIB sections

Author

Hélène Bureau, Hicham Khodja, Alice Aléon-Toppani, Adriana Gonzalez-Cano, Daniel Lévy, Rémi Duhamel, David Troadec, Jérôme Aléon, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Centrale de Micro Nano Fabrication - IEMN (CMNF-IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Laboratoire d'Etudes des Eléments Légers (LEEL - UMR 3685), Nanosciences et Innovation pour les Matériaux, la Biomédecine et l'Energie (ex SIS2M) (NIMBE UMR 3685), Institut Rayonnement Matière de Saclay (IRAMIS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Institut Rayonnement Matière de Saclay (IRAMIS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Museum National d'Histoire Naturelle, CNRS-INSU PNP national planetology program, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centrale de Micro Nano Fabrication - IEMN (CMNF - IEMN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Institut Rayonnement Matière de Saclay (IRAMIS), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Mineral hydration, 010504 meteorology & atmospheric sciences, Chemistry, [SDU]Sciences of the Universe [physics], Analytical chemistry, [CHIM.MATE]Chemical Sciences/Material chemistry, 010502 geochemistry & geophysics, Nanoscale secondary ion mass spectrometry, 01 natural sciences, Focused ion beam, 0105 earth and related environmental sciences, Analytical Chemistry
Abstract

International audience; The D/H ratio imaging of weakly hydrated minerals prepared as Focused Ion Beam (FIB) sections is developed in order to combine isotopic imaging by Nanoscale Secondary Ion Mass Spectrometry (NanoSIMS) of micrometer-sized grains with other nanoscale imaging techniques, such as Transmission Electron Microscopy. In order to maximize the accuracy, sensitivity, precision and reproducibility of D/H ratios at the micrometer-size, while minimizing the surface contamination at the same time, we explored all instrumental parameters known to influence the measurement of D/H ratios in situ. Optimal conditions were found to be obtained with the use of (i) a Cs$^+$ ion source and detection of H$^-$ and D$^-$at low mass resolving power, (ii) a primary beam intensity of 100 pA, and (iii) raster sizes in the range 8-15 $\mu$m. Nominally anhydrous minerals were used to evaluate the detection limits and indicate a surface contamination level of about 200 ppm equivalent H$_2$O in these conditions. With the high primary intensity used here, the dwell time is not a parameter as critical as found in previous studies and a dwell time of 1 ms/px is used to minimize dynamic contamination during analysis. Analysis of FIB sections was found to reduce significantly static contamination due to sample preparation and improved accuracy compared to using polished sections embedded not only in epoxy but in indium as well. On amphiboles, the typical overall uncertainty including reproducibility is about 20 ‰ on bulk FIB sections and about 50 ‰ at the 1.5 $\mu$m scale using image processing (1$\sigma$).

Published
2019
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8. Organic and mineralogic heterogeneity of the Paris meteorite followed by FTIR hyperspectral imaging

Author

Donia Baklouti, Ferenc Borondics, Alice Aléon-Toppani, François Brisset, Zahia Djouadi, Christophe Sandt, Rosario Brunetto, Z. Dionnet, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), Institut de Chimie Moléculaire et des Matériaux d'Orsay (ICMMO), Université Paris-Sud - Paris 11 (UP11)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), and Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)

Subjects
Materials science, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mineralogy, Hyperspectral imaging, 010502 geochemistry & geophysics, 01 natural sciences, Geophysics, Meteorite, Space and Planetary Science, 0103 physical sciences, Fourier transform infrared spectroscopy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

International audience

Published
2018
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9. Hyperspectral FTIR imaging of irradiated carbonaceous meteorites

Author

Rosario Brunetto, Kohei Kitazato, C. Pilorget, A. Aléon-Toppani, M. A. Barucci, Donia Baklouti, Z. Dionnet, C. Lantz, Ferenc Borondics, Zahia Djouadi, Richard P. Binzel, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), Institut astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Murchison meteorite, [PHYS]Physics [physics], medicine.medical_specialty, Materials science, 010504 meteorology & atmospheric sciences, Analytical chemistry, Hyperspectral imaging, Astronomy and Astrophysics, 01 natural sciences, Space weathering, Spectral line, Spectral imaging, Meteorite, 13. Climate action, Space and Planetary Science, Chondrite, 0103 physical sciences, medicine, Irradiation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

Space weathering produces variations in the optical properties of small solar system body surfaces. Laboratory studies have been performed by several groups on different meteorite classes, aimed at simulating space weathering by using ion irradiation and laser ablation. Here we present new FTIR spectral imaging data of ion irradiated carbonaceous chondrites (CV Allende and CM Murchison meteorites), simulating solar wind irradiation on primitive asteroids. Irradiation conditions (40 keV He+ and Ar+ up to 3.1016 ion/cm2) were reported in detail in previous studies. The new analyses were performed with a FTIR micro-spectrometer equipped with an FPA (Focal Plane Array) detector. Micro-reflectance spectra were acquired in the 2.5–12 μm range using a spot size of 20 μm and scanning large areas (from mm2 to cm2) of the meteorite pellets, both on virgin areas and on areas irradiated with different doses. Spectral maps allow us characterizing the heterogeneity of the meteorites at the 20 μm spatial scale. In the irradiated areas, we observe spectral modifications of both anhydrous and hydrated silicates. Spectral shifts are observed after irradiation, larger for anhydrous than hydrated silicates. Compositional heterogeneity of the pristine materials and irradiation effects are compared to each other as a function of the irradiation dose, to determine which spectral features are more sensitive to space weathering. Results are then compared with the IR spectral capabilities of instruments onboard the Hayabusa2/JAXA and OSIRIS-REx/NASA spacecrafts, to provide these missions with spectral criteria on how to distinguish space weathering from compositional heterogeneity effects at the asteroid, and in view of surface selection for sample return.

Published
2018
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10. FTIR Micro-tomography of Five Itokawa Particles and one Primitive Carbonaceous Chondrite

Author

Z. Dionnet, Zahia Djouadi, David Troadec, A.C. Buellet, Ashley J. King, Rosario Brunetto, S. Rubino, Ferenc Borondics, and A. Aléon-Toppani

Subjects
Materials science, Carbonaceous chondrite, 0103 physical sciences, Analytical chemistry, Micro tomography, Fourier transform infrared spectroscopy, 010502 geochemistry & geophysics, 010303 astronomy & astrophysics, 01 natural sciences, Instrumentation, 0105 earth and related environmental sciences
Published
2018
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11. Quantitative compositional analysis of martian mafic regions using the MEx/OMEGA reflectance data

Author

Francois Poulet, A. Aleon-Toppani, Jacques-Marie Bardintzeff, Jean-Pierre Bibring, Bernard Platevoet, Nicolas Mangold, J. F. Mustard, Brigitte Gondet, V. Sautter, Yves Langevin, and Patrick Pinet

Subjects
Basalt, Thermal Emission Spectrometer, Olivine, 010504 meteorology & atmospheric sciences, Noachian, Partial melting, Mineralogy, Astronomy and Astrophysics, Pyroxene, engineering.material, 01 natural sciences, Astrobiology, 13. Climate action, Space and Planetary Science, 0103 physical sciences, engineering, Plagioclase, Mafic, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract

The primary objectives of this paper are to determine the modal mineralogy of selected low albedo terrains of different ages ranging from Noachian to Amazonian exposed on the surface of Mars. This analysis is conducted using the spectral modeling of the Observatoire pour la Mineralogie, l'Eau, les Glaces, et l'Activite (OMEGA) reflectance data. Results from this work are consistent with the major results of previous spectroscopic studies: plagioclase (40–60% in volume) and high calcium pyroxene (20–40%, HCP) are the dominant minerals of the most regions. Low calcium pyroxene (10–15%, LCP) and minor amounts of olivine are also present. The oldest terrains are characterized by the largest amount of LCP and the lowest concentration of plagioclase. These overall compositions are consistent with two-pyroxene basalts. The particle sizes are in the range of a few hundreds of micrometers, which is in good agreement with the thermal inertia of the martian low albedo regions. In the region around the Nili Fossae, localized concentrations of olivine up to 40% with millimeter particle size similar to picritic basalts observed in situ by the Spirit rover in the Gusev crater are inferred. Chemical compositions are calculated for the first time from OMEGA spectra. They are quite consistent with Gusev rocks and shergottite compositions but they appear to be significantly SiO2-poorer than Thermal Emission Spectrometer data. A decreasing low calcium pyroxene abundance with the decreasing age of the low albedo regions is reported. This may be indicative of decreasing degree of partial melting as thermal flux decreases with time. We propose that the ancient Noachian-aged, LCP-rich terrains could have been formed from H2O-bearing melts. Then, dry, basaltic volcanism occurred leading to decreasing LCP abundance with time due to decreasing degree of partial melting. The olivine-bearing material modeled in Nili Fossae resembles the composition of ALH77005 and Chassigny meteorites consistent with prior studies. Implications on the formation of the basaltic Shergottites are discussed.

Published
2009
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12. Experimental simulation of atmospheric entry of micrometeorites

Author

Guy Libourel, M. Maurette, Alice Toppani, Cécile Engrand, Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM)

Subjects
Murchison meteorite, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010504 meteorology & atmospheric sciences, Partial melting, 010502 geochemistry & geophysics, 01 natural sciences, Astrobiology, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Atmosphere, chemistry.chemical_compound, Geophysics, Meteorite, chemistry, Space and Planetary Science, Mineral redox buffer, Micrometeorite, Atmospheric entry, Geology, 0105 earth and related environmental sciences, Magnetite
Abstract

— Depending on their velocity, entry angle and mass, micrometeorites suffer different degrees of heating during their deceleration in the Earth's atmosphere, leading, in most cases, to significant textural, mineralogical and chemical modifications. One of these modifications is the formation of a magnetite shell around most micrometeorites, which until now could not be reproduced, neither theoretically nor experimentally. The present study was designed to better understand the entry heating effects on micrometeorites and especially the formation of the magnetite shell. Fragments of the Murchison and Orgueil meteorites were used as analogue material in flash-heating experiments performed in a high-temperature furnace; effects of temperature, heating duration, and oxygen fugacity were investigated. These experiments were able to reproduce most of the micrometeorites textures, from the vesicular fine-grained micrometeorites to the totally melted cosmic spherules. For the first time, the formation of a magnetite shell could be observed on micrometeorite analogues. We suggest that the most plausible mechanism for the formation of this shell is a peripheral partial melting with subsequent magnetite crystallization at the surface of the micrometeorite. Furthermore, with this study, it is possible to estimate the atmospheric entry conditions of micrometeorites, such as the peak temperature and the duration of flash-heating.

Published
2001
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13. Effects of atmospheric entry heating on the noble gas and nitrogen content of micrometeorites

Author

Evelyn Füri, Bernard Marty, Guy Libourel, Alice Aléon-Toppani, Laurent Zimmermann, Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11)

Subjects
volatile flux, Orgueil, chemistry.chemical_element, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, 010502 geochemistry & geophysics, 01 natural sciences, nitrogen, Astrobiology, Atmosphere, Neon, Geochemistry and Petrology, Chondrite, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), entry heating, 010303 astronomy & astrophysics, Helium, 0105 earth and related environmental sciences, Cosmic dust, Noble gas, micrometeorites, Isotopes of nitrogen, Geophysics, chemistry, 13. Climate action, Space and Planetary Science, Carbonaceous chondrite, noble gases, Geology
Abstract

International audience; Fragments of the carbonaceous chondrite Orgueil were subjected to pulse-heating sequences in order to simulate the heating conditions experienced by micrometeorites (MMs) upon entry into Earthʼs atmosphere. By increasing the experimental run times from 2 to 120 s at a fixed temperature of 1350 °C, the different textures of natural MMs (from non-vesicular fine-grained particles to melted cosmic spherules) were reproduced, and the noble gas (He, Ne, Ar) and nitrogen abundances and isotope ratios of the MM analogues were subsequently determined by CO2 laser extraction-static mass spectrometry analysis. The starting material shows a heterogeneous He–Ne–Ar–N signature, consistent with the mineralogical heterogeneity of CI chondrites and the inhomogeneous distribution of various noble gas and nitrogen components among meteoritic minerals. Nonetheless, our experiments demonstrate that moderately to strongly heated Orgueil fragments retain only a few percent of their initial noble gas and nitrogen inventories, indicating that atmospheric entry heating results in extensive degassing of meteoritic dust particles. The evolution of the noble gas and nitrogen isotope ratios may, in part, be explained by equilibration with the atmosphere; however, the decreasing δ15N values may also indicate preferential degradation of a 15N-rich component by thermal processing of chondritic matter. Furthermore, the efficient loss of helium and cosmogenic neon during heating will lead to an underestimate of the 3He and 21Ne exposure ages of MMs, as well as to large uncertainties for cosmic dust accretion rates derived from extraterrestrial 3He abundances in deep-sea sediments or polar ice cores. While the relative proportions of infalling cometary and asteroidal dust on Earth are unknown, the contribution of noble gases, nitrogen, and water from cosmic dust to the terrestrial volatile inventory appears negligible.

Published
2013
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14. Mineralogy and Petrology of Comet 81P/Wild 2 Nucleus Samples

Author

Frank J. Stadermann, Matthew J. Genge, Anders Meibom, David J. Joswiak, D. A. Papanastassiou, Nick Teslich, Lindsay P. Keller, Kyoko Okudaira, Sean Brennan, Thomas H. See, Jean Susini, M. K. Weisberg, Matthieu Gounelle, Frans J. M. Rietmeijer, Keiko Nakamura-Messenger, Zu Rong Dai, J. Warren, Donald E. Brownlee, Loan Le, Kazushige Tomeoka, Pierre Bleuet, Steven B. Simon, Stewart Fallon, Alice Toppani, Damien Jacob, Mitra L. Taheri, John P. Bradley, Denton S. Ebel, Adrian J. Brearley, Laurence Lemelle, Thomas J. Zega, Jeffrey N. Grossman, Philippe Gillet, Falko Langenhorst, Takashi Mikouchi, Akira Tsuchiyama, John Bridges, Michael E. Zolensky, François Robert, Hope A. Ishii, Alexander N. Krot, Anna L. Butterworth, Giles A. Graham, Rhonda M. Stroud, Michael A. Velbel, Christopher J. Snead, Ron K. Bastien, Miaofang Chi, Antonio Lanzirotti, Graciela Matrajt, Benton C. Clark, Murielle C. Perronnet, Thomas Stephan, Kazumasa Ohsumi, Naotaka Tomioka, Patrick Cordier, Iris Weber, Anton T. Kearsley, George J. Flynn, Matthew A. Marcus, Tomoki Nakamura, Smail Mostefaoui, Hugues Leroux, William Rao, Ichiro Ohnishi, Sue Wirick, Ralph P. Harvey, Peter Tsou, T. Ferroir, Hajime Yano, Kenji Hagiya, Phil Bland, Lawrence Grossman, Andrew J. Westphal, Alexandre Simionovici, European Synchrotron Radiation Facility (ESRF), Laboratoire de Sciences de la Terre (LST), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Institut d'Informatique et de Mathématiques Appliquées de Grenoble (IMAG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Environnement et Minéralurgie (LEM), Institut National Polytechnique de Lorraine (INPL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Modélisation des Transferts dans l'Environnement (LMTE), Service Mesures et modélisation des Transferts et des Accidents graves (SMTA), Département Technologie Nucléaire (DTN), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Département Technologie Nucléaire (DTN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Advanced Light Source [LBNL Berkeley] (ALS), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire de structures et propriétés de l'état solide - UMR 8008 (LSPES), Université de Lille, Sciences et Technologies-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Multidisciplinary, Olivine, x-ray fluorescence, Chemistry, Comet, Sulfur XANES, Mineralogy, Pyroxene, engineering.material, 010502 geochemistry & geophysics, Protoplanetary disk, Stardust, 01 natural sciences, Astrobiology, Carbonaceous chondrite, Silicate minerals, 0103 physical sciences, engineering, Formation and evolution of the Solar System, 010303 astronomy & astrophysics, Refractory (planetary science), 0105 earth and related environmental sciences, [SDU.STU.MI]Sciences of the Universe [physics]/Earth Sciences/Mineralogy
Abstract

著者人数: 75名, 資料番号: SA1003700000

Published
2006
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15. Comet 81P/Wild 2 under a microscope

Author

Brownlee, Don, Tsou, Peter, Aleon, Jerome, Alexander, Conel M. O'D., Araki, Tohru, Bajt, Sasa, Baratta, Giuseppe A., Bastien, Ron, Bland, Phil, Bleuet, Pierre, Borg, Janet, Bradley, John P., Brearley, Adrian, Brenker, F., Brennan, Sean, Bridges, John C., Browning, Nigel D., Brucato, John R., Bullock, E., Burchell, Mark J., Busemann, Henner, Butterworth, Anna, Chaussidon, Marc, Cheuvront, Allan, Chi, Miaofang, Cintala, Mark J., Clark, B. C., Clemett, Simon J., Cody, George, Colangeli, Luigi, Cooper, George, Cordier, Patrick, Daghlian, C., Dai, Zurong, D'Hendecourt, Louis, Djouadi, Zahia, Dominguez, Gerardo, Duxbury, Tom, Dworkin, Jason P., Ebel, Denton S., Economou, Thanasis E., Fakra, Sirine, Fairey, Sam A. J., Fallon, Stewart, Ferrini, Gianluca, Ferroir, T., Fleckenstein, Holger, Floss, Christine, Flynn, George, Franchi, Ian A., Fries, Marc, Gainsforth, Z., Gallien, J.-P., Genge, Matt, Gilles, Mary K., Gillet, Philipe, Gilmour, Jamie, Glavin, Daniel P., Gounelle, Matthieu, Grady, Monica M., Graham, Giles A., Grant, P. G., Green, Simon F., Grossemy, Faustine, Grossman, Lawrence, Grossman, Jeffrey N., Guan, Yunbin, Hagiya, Kenji, Harvey, Ralph, Heck, Philipp, Herzog, Gregory F., Hoppe, Peter, Horz, Friedrich, Huth, Joachim, Hutcheon, Ian D., Ignatyev, Konstantin, Ishii, Hope, Ito, Motoo, Jacob, Damien, Jacobsen, Chris, Jacobsen, Stein, Jones, Steven, Joswiak, David, Jurewicz, Amy, Kearsley, Anton T., Keller, Lindsay P., Khodja, H., Kilcoyne, A. L. David, Kissel, Jochen, Krot, Alexander, Langenhorst, Falko, Lanzirotti, Antonio, Le, Loan, Leshin, Laurie A., Leitner, J., Lemelle, L., Leroux, Hugues, Liu, Ming-Chang, Luening, K., Lyon, Ian, MacPherson, Glen, Marcus, Matthew A., Marhas, Kuljeet, Marty, Bernard, Matrajt, Graciela, McKeegan, Kevin, Meibom, Anders, Mennella, Vito, Messenger, Keiko, Messenger, Scott, Mikouchi, Takashi, Mostefaoui, Smail, Nakamura, Tomoki, Nakano, T., Newville, M., ittler, Larry R., Ohnishi, Ichiro, Ohsumi, Kazumasa, Papanastassiou, Dimitri A., Palma, Russ, Palumbo, Maria E., Pepin, Robert O., Perkins, David, Perronnet, Murielle, Pianetta, P., Rao, William, Rietmeijer, Frans J. M., Robert, Francois, Rost, D., Rotundi, Alessandra, Ryan, Robert, Sandford, Scott A., Schwandt, Craig S., See, Thomas H., Schlutter, Dennis, Sheffield-Parker, J., Simionovici, Alexandre, Simon, Steven, Sitnitsky, I., Snead, Christopher J., Spencer, Maegan K., Stadermann, Frank J., Steele, Andrew, Stephan, Thomas, Stroud, Rhonda, Susini, Jean, Sutton, S. R., Suzuki, Y., Taheri, Mitra, Taylor, Susan, Teslich, Nick, Tomeoka, Kazu, Tomioka, Naotaka, Toppani, Alice, Trigo-Rodriguez, Josep M., Troadec, David, Tsuchiyama, Akira, Tuzzolino, Anthony J., Tyliszczak, Tolek, Uesugi, K., Velbel, Michael, Vellenga, Joe, Vicenzi, E., Vincze, L., Warren, Jack, Weber, Iris, Weisberg, Mike, Westphal, Andrew J., Wirick, Sue, Wooden, Diane, Wopenka, Brigitte, Wozniakiewicz, Penelope, Wright, Ian, Yabuta, Hikaru, Young, Edward D., Zare, Richard N., Zega, Thomas, Ziegler, Karen, Zimmerman, Laurent, Zinner, Ernst, Zolensky, Michael, Okudaira, Kyoko, Yano, Hajime, Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de structures et propriétés de l'état solide - UMR 8008 (LSPES), Université de Lille, Sciences et Technologies-Centre National de la Recherche Scientifique (CNRS), Advanced Light Source [LBNL Berkeley] (ALS), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire Pierre Süe (LPS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Sciences de la Terre (LST), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Environnement et Minéralurgie (LEM), Institut National Polytechnique de Lorraine (INPL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Modélisation des Transferts dans l'Environnement (LMTE), Service Mesures et modélisation des Transferts et des Accidents graves (SMTA), Département Technologie Nucléaire (DTN), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Département Technologie Nucléaire (DTN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'Informatique et de Mathématiques Appliquées de Grenoble (IMAG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), European Synchrotron Radiation Facility (ESRF), Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Unité de Microélectronique, Optoélectronique et Polymères (UMOP), Université de Limoges (UNILIM)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Centre National de la Recherche Scientifique (CNRS)-Université de Limoges (UNILIM)

Subjects
Physics, Solar System, Multidisciplinary, Comet dust, Comet, Astronomy, 010502 geochemistry & geophysics, 01 natural sciences, Astrobiology, Interstellar medium, Meteorite, Asteroid, Silicate minerals, Physics::Space Physics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Formation and evolution of the Solar System, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

著者人数: 183名, 資料番号: SA1003701000

Published
2006
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16. Accretion of neon, organics, CO$_2$, nitrogen and water from large interplanetary dust particles on the early Earh

Author

Jean Duprat, Alice Toppani, Matthieu Gounelle, G. Matrajt, Gero Kurat, Cecile Engrand, M. Maurette, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Lorgeril, Jocelyne

Subjects
Chondrule, Astronomy, Astronomy and Astrophysics, 010502 geochemistry & geophysics, Early Earth, 01 natural sciences, Astrobiology, Interplanetary dust cloud, Meteorite, 13. Climate action, Space and Planetary Science, Abiogenesis, Micrometeorite, Chondrite, 0103 physical sciences, 010303 astronomy & astrophysics, Late Heavy Bombardment, Geology, 0105 earth and related environmental sciences
Abstract

Large interplanetary dust particles (micrometeorites) with sizes of 100– 200 μm , recovered from the Greenland and Antarctica ice sheets, represent by far the dominant source of primitive extraterrestrial material accreted by the Earth today. Comparisons of mineralogical, chemical and isotopic analyses of micrometeorites and meteorites indicate that micrometeorites are mostly related to the relatively rare group (2% of the meteorite falls) of the primitive hydrous-carbonaceous meteorites, and not to the most abundant classes of the ordinary chondrites and differentiated meteorites. But there are differences between these two classes of extraterrestrial objects, such as a high pyroxene to olivine ratio, a strong depletion in chondrules, a much smaller size of the most refractory components, and a much higher AIB (α-isobutyric amino acid) to isovaline ratio in micrometeorites as compared to meteorites. They indicate that micrometeorites represent a new population of solar system objects, not represented as yet in the meteorite collections. The major objective of this work is to predict various effects of the accretion of early micrometeorites on the Earth during the period of heavy bombardment suffered by the Earth–Moon system ⩾3.9 Ga ago. The application of a simple arithmetics of accretion to a selection of measurements (average contents of neon, carbon, nitrogen and water in micrometeorites, and isotopic composition of their Ne and H), shows that during the peak of this cataclysmic epoch (sterilization period) which occurred just after the formation of the young Earth (4.45 Ga ago), the accretion of early micrometeorites did play a major role in the formation of the terrestrial atmosphere and oceans. Later on, during the early life period (around 4 Ga ago), when liquid water and organics could condense and/or survive, micrometeorites were possibly functioning as tiny chemical reactors to synthesize the prebiotic molecules required for the origin of life. Efforts were made to start reducing the number of major speculations in this “early-micrometeorite-accretion” scenario (EMMAC), which is finally extended with some confidence to Mars, where the survival of micrometeorites upon atmospheric entry looks even more favorable than on the Earth.

Published
2000

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