211 results on '"Debaille V."'
Search Results
2. Dry Late Accretion inferred from Venus' coupled atmosphere and internal evolution
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Gillmann, C., Golabek, G. J., Raymond, S. N., Schonbachler, M., Tackley, P. J., Dehant, V., and Debaille, V.
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Astrophysics - Earth and Planetary Astrophysics ,Physics - Geophysics - Abstract
The composition of meteoritic material delivered to the terrestrial planets after the end of core formation as late accretion remains contentious. Because the evolution of Venus' atmospheric composition is likely to be less intricate than the Earth's, we test implications of wet and dry late accretion compositions, using present-day Venus atmosphere measurements. Here we investigate the long-term evolution of Venus using self-consistent numerical models of global thermochemical mantle convection coupled with both an atmospheric evolution model and a late accretion N-body delivery model. Atmospheric escape is only able to remove a limited amount of water over the history of the planet. We show that late accretion of wet material exceeds this sink. CO2 and N2 contributions serve as additional constraints. A preferentially dry composition of the late accretion impactors is in agreement with observational data on H2O, CO2 and N2 in Venus' present-day atmosphere. Our study suggests that the late accreted material delivered to Venus was mostly dry enstatite chondrite, conforming to isotopic data available for Earth. Our preferred scenario indicates late accretion on Venus contained less than 2.5% wet carbonaceous chondrites. In this scenario, the majority of Venus' and Earth's water has been delivered during the main accretion phase., Comment: 14 pages, 4 figures, 4 supplementary figures
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- 2020
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3. A new shergottite martian meteorite analog system (SAS) for alteration experiments
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Fortier, V., Debaille, V., Dehant, V., and Bultel, B.
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- 2023
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4. Sample return of primitive matter from the outer Solar System
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Vernazza, P., Beck, P., Ruesch, O., Bischoff, A., Bonal, L., Brennecka, G., Brunetto, R., Busemann, H., Carter, J., Carli, C., Cartier, C., Ciarniello, M., Debaille, V., Delsanti, A., D’Hendecourt, L., Füri, E., Groussin, O., Guilbert-Lepoutre, A., Helbert, J., Hoppe, P., Jehin, E., Jorda, L., King, A., Kleine, T., Lamy, P., Lasue, J., Le Guillou, C., Leroux, H., Leya, I., Magna, T., Marrocchi, Y., Morlok, A., Mousis, O., Palomba, E., Piani, L., Quirico, E., Remusat, L., Roskosz, M., Rubin, M., Russell, S., Schönbächler, M., Thomas, N., Villeneuve, J., Vinogradoff, V., Wurz, P., and Zanda, B.
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- 2022
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5. The meteorite flux of the last 2 Myr recorded in the Atacama desert
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Drouard, A., Gattacceca, J., Hutzler, A., Rochette, P., Braucher, R., Bourlès, D., Team, ASTER, Gounelle, M., Morbidelli, A., Debaille, V., Van Ginneken, M., Valenzuela, M., Quesnel, Y., and Martinez, R.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
The evolution of the meteorite flux to the Earth can be studied by determining the terrestrial ages of meteorite collected in hot deserts. We have measured the terrestrial ages of 54 stony meteorites from the El M\'edano area, in the Atacama Desert, using the cosmogenic nuclide chlorine 36. With an average age of 710 ka, this collection is the oldest collection of non fossil meteorites at the Earth's surface. This allows both determining the average meteorite flux intensity over the last 2 Myr (222 meteorites larger than 10 g per km2 per Myr) and discussing its possible compositional variability over the Quaternary period. A change in the flux composition, with more abundant H chondrites, occurred between 0.5 and 1 Ma, possibly due to the direct delivery to Earth of a meteoroid swarm from the asteroid belt., Comment: accepted in Geology
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- 2019
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6. Pre-eruptive storage conditions and magmatic evolution of the Bora-Baricha-Tullu Moye volcanic system, Main Ethiopian Rift
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Tadesse, A.Z., Fontijn, K., Caricchi, L., Bégué, F., Gudbrandsson, S., Smith, V.C., Gopon, P., Debaille, V., Laha, P., Terryn, H., Yirgu, G., and Ayalew, D.
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- 2023
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7. Multi-method dating constrains the diversification of early eukaryotes in the Proterozoic Mbuji-Mayi Supergroup of the D.R.Congo and the geological evolution of the Congo Basin
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François, C., Baludikay, B.K., Debaille, V., Birck, J.L., Limmois, D., Jourdan, F., Baudet, D., Paquette, J.L., Delvaux, D., and Javaux, E.J.
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- 2023
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8. Detection of incipient aqueous alteration in carbonaceous chondrites
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Krämer Ruggiu, L., Devouard, B., Gattacceca, J., Bonal, L., Leroux, H., Eschrig, J., Borschneck, D., King, A.J., Beck, P., Marrocchi, Y., Debaille, V., Hanna, R.D., and Grauby, O.
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- 2022
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9. Definition and use of functional analogues in planetary exploration
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Foucher, F., Hickman-Lewis, K., Hutzler, A., Joy, K.H., Folco, L., Bridges, J.C., Wozniakiewicz, P., Martínez-Frías, J., Debaille, V., Zolensky, M., Yano, H., Bost, N., Ferrière, L., Lee, M., Michalski, J., Schroeven-Deceuninck, H., Kminek, G., Viso, M., Russell, S., Smith, C., Zipfel, J., and Westall, F.
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- 2021
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10. Samples Collected From the Floor of Jezero Crater With the Mars 2020 Perseverance Rover
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Simon, J. I., primary, Hickman‐Lewis, K., additional, Cohen, B. A., additional, Mayhew, L. E., additional, Shuster, D. L., additional, Debaille, V., additional, Hausrath, E. M., additional, Weiss, B. P., additional, Bosak, T., additional, Zorzano, M.‐P., additional, Amundsen, H. E. F., additional, Beegle, L. W., additional, Bell, J. F., additional, Benison, K. C., additional, Berger, E. L., additional, Beyssac, O., additional, Brown, A. J., additional, Calef, F., additional, Casademont, T. M., additional, Clark, B., additional, Clavé, E., additional, Crumpler, L., additional, Czaja, A. D., additional, Fairén, A. G., additional, Farley, K. A., additional, Flannery, D. T., additional, Fornaro, T., additional, Forni, O., additional, Gómez, F., additional, Goreva, Y., additional, Gorin, A., additional, Hand, K. P., additional, Hamran, S.‐E., additional, Henneke, J., additional, Herd, C. D. K., additional, Horgan, B. H. N., additional, Johnson, J. R., additional, Joseph, J., additional, Kronyak, R. E., additional, Madariaga, J. M., additional, Maki, J. N., additional, Mandon, L., additional, McCubbin, F. M., additional, McLennan, S. M., additional, Moeller, R. C., additional, Newman, C. E., additional, Núñez, J. I., additional, Pascuzzo, A. C., additional, Pedersen, D. A., additional, Poggiali, G., additional, Pinet, P., additional, Quantin‐Nataf, C., additional, Rice, M., additional, Rice, J. W., additional, Royer, C., additional, Schmidt, M., additional, Sephton, M., additional, Sharma, S., additional, Siljeström, S., additional, Stack, K. M., additional, Steele, A., additional, Sun, V. Z., additional, Udry, A., additional, VanBommel, S., additional, Wadhwa, M., additional, Wiens, R. C., additional, Williams, A. J., additional, and Williford, K. H., additional
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- 2023
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11. Investigation of metasomatism using Cu, Zn and Fe stable isotopes: Rodingitization of mafic and ultramafic rocks in ophiolites from northern Greece
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Zaronikola, N., primary, Debaille, V., additional, Rogkala, A., additional, Petrounias, P., additional, Mathur, R., additional, Decrée, S., additional, Pomonis, P., additional, Hatzipanagiotou, K., additional, and Tsikouras, B., additional
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- 2023
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12. Blue ice in Antarctica: The gateway to travel in time and space
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Tollenaar, V., Zekollari, H., Tuia, D., Rußwurm, M., Kellenberger, B., Lhermitte, S., Tax, D., Debaille, V., Goderis, S., Claeys, P., and Pattyn, F.
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Antarctica has unique areas that expose blue ice, which contrast to most of the continent (~98%) that is covered by snow. Some of these blue ice areas (BIAs) contain meteorite concentrations and (very) old ice, making them very valuable for understanding our Solar System and the climate of the past, respectively. Meteorites and old ice become accessible through ablative processes that remove upper layers of ice and leave embedded material exposed on the surface. As a result, very old ice has been found in blue ice areas (>2 million years old), and >60% of meteorites retrieved on Earth come from Antarctica.However, not all BIAs act as figurative gateways to travel in time and space. Different processes need to combine favorably to find meteorites and old ice. To understand where to go in Antarctica, we accessed and combined various remote sensing data in a deep-learning framework to identify BIAs. By using a multi-sensor approach, we could also detect blue ice under temporary snow covers. Moreover, we created a map of potential meteorite collection sites using machine learning. The analyses showed that the ice flow velocity, the exposure of ice, the surface slope, and the extreme surface temperature are the most important indicators for the presence of meteorites. The machine-learning framework also allowed us to project how the presence of meteorites is to change in the future. Next, we will use data-driven techniques to direct old ice sampling efforts in BIAs., The 28th IUGG General Assembly (IUGG2023) (Berlin 2023)
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- 2023
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13. Time-Sensitive Aspects of Mars Sample Return (MSR) Science
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Tosca, N. J., Agee, Carl, Cockell, C., Glavin, D P, Hutzler, Aurore, Marty, B., McCubbin, F. M., Regberg, Aaron, Velbel, Michael, Kminek, G., Meyer, M., Beaty, D.W., Carrier, B. L., Haltigin, T., Hays, Lindsay, Busemann, H., Cavalazzi, Barbara, Debaille, V, Grady, M., Hauber, Ernst, Pratt, Lisa, Smith, Alvin, Smith, C., Summons, R E, Swindle, T. D., Tait, Kimberly, Udry, Arya, Usui, Tomohiro, Wadhwa, M., Westall, F., Zorzano, M.-P., Tosca N. J., Beaty D. W., Carrier B. L., Agee C. B., Cockell C. S., Glavin D. P., Hutzler A., Marty B., McCubbin F. M., Regberg A. B., Velbel M. A., Kminek G., Meyer M. A., Haltigin T., Busemann H., Cavalazzi B., Debaille V., Grady M. M., Hauber E., Hays L. E., Pratt L. M., Smith A. L., Smith C. L., Summons R. E., Swindle T. D., Tait K. T., Udry A., Usui T., Wadhwa M., Westall F., Zorzano M. -P., University of Cambridge [UK] (CAM), The University of New Mexico [Albuquerque], University of Edinburgh, NASA Goddard Space Flight Center (GSFC), European Space Agency (ESA), 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), NASA Johnson Space Center (JSC), NASA, Michigan State University [East Lansing], Michigan State University System, Smithsonian Institution, NASA Headquarters, California Institute of Technology (CALTECH), Canadian Space Agency (CSA), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Bologna, Université libre de Bruxelles (ULB), The Open University [Milton Keynes] (OU), German Aerospace Center (DLR), Indiana University [Bloomington], Indiana University System, The Natural History Museum [London] (NHM), University of Glasgow, Massachusetts Institute of Technology (MIT), University of Arizona, Royal Ontario Museum, University of Nevada [Las Vegas] (WGU Nevada), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Arizona State University [Tempe] (ASU), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), University of Aberdeen, Tosca, Nicholas [0000-0003-4415-4231], and Apollo - University of Cambridge Repository
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Minerals ,geology ,Extraterrestrial Environment ,laboratory experiments ,Sulfates ,[SDV]Life Sciences [q-bio] ,astrobiology ,Mars ,Space Flight ,Mars Sample Return (MSR) Science ,sample return ,Agricultural and Biological Sciences (miscellaneous) ,Space and Planetary Science ,Exobiology ,Clay ,Gases - Abstract
Samples returned from Mars would be placed under quarantine at a Sample Receiving Facility (SRF) until they are considered safe to release to other laboratories for further study. The process of determining whether samples are safe for release, which may involve detailed analysis and/or sterilization, is expected to take several months. However, the process of breaking the sample tube seal and extracting the headspace gas will perturb local equilibrium conditions between gas and rock and set in motion irreversible processes that proceed as a function of time. Unless these time-sensitive processes are understood, planned for, and/or monitored during the quarantine period, scientific information expected from further analysis may be lost forever. At least four processes underpin the time-sensitivity of Mars returned sample science: (1) degradation of organic material of potential biological origin, (2) modification of sample headspace gas composition, (3) mineral-volatile exchange, and (4) oxidation/reduction of redox-sensitive materials. Available constraints on the timescales associated with these processes supports the conclusion that an SRF must have the capability to characterize attributes such as sample tube headspace gas composition, organic material of potential biological origin, as well as volatiles and their solid-phase hosts. Because most time-sensitive investigations are also sensitive to sterilization, these must be completed inside the SRF and on timescales of several months or less. To that end, we detail recommendations for how sample preparation and analysis could complete these investigations as efficiently as possible within an SRF. Finally, because constraints on characteristic timescales that define time-sensitivity for some processes are uncertain, future work should focus on: (1) quantifying the timescales of volatile exchange for core material physically and mineralogically similar to samples expected to be returned from Mars, and (2) identifying and developing stabilization or temporary storage strategies that mitigate volatile exchange until analysis can be completed. Executive Summary Any samples returned from Mars would be placed under quarantine at a Sample Receiving Facility (SRF) until it can be determined that they are safe to release to other laboratories for further study. The process of determining whether samples are safe for release, which may involve detailed analysis and/or sterilization, is expected to take several months. However, the process of breaking the sample tube seal and extracting the headspace gas would perturb local equilibrium conditions between gas and rock and set in motion irreversible processes that proceed as a function of time. Unless these processes are understood, planned for, and/or monitored during the quarantine period, scientific information expected from further analysis may be lost forever. Specialist members of the Mars Sample Return Planning Group Phase 2 (MSPG-2), referred to here as the Time-Sensitive Focus Group, have identified four processes that underpin the time-sensitivity of Mars returned sample science: (1) degradation of organic material of potential biological origin, (2) modification of sample headspace gas composition, (3) mineral-volatile exchange, and (4) oxidation/reduction of redox-sensitive materials (Figure 2). Consideration of the timescales and the degree to which these processes jeopardize scientific investigations of returned samples supports the conclusion that an SRF must have the capability to characterize: (1) sample tube headspace gas composition, (2) organic material of potential biological origin, (3) volatiles bound to or within minerals, and (4) minerals or other solids that host volatiles (Table 4). Most of the investigations classified as time-sensitive in this report are also sensitive to sterilization by either heat treatment and/or gamma irradiation (Velbel et al., 2022). Therefore, these investigations must be completed inside biocontainment and on timescales that minimize the irrecoverable loss of scientific information (i.e., several months or less; Section 5). To that end, the Time-Sensitive Focus Group has outlined a number of specific recommendations for sample preparation and instrumentation in order to complete these investigations as efficiently as possible within an SRF (Table 5). Constraints on the characteristic timescales that define time-sensitivity for different processes can range from relatively coarse to uncertain (Section 4). Thus, future work should focus on: (1) quantifying the timescales of volatile exchange for variably lithified core material physically and mineralogically similar to samples expected to be returned from Mars, and (2) identifying and developing stabilization strategies or temporary storage strategies that mitigate volatile exchange until analysis can be completed. List of Findings FINDING T-1: Aqueous phases, and oxidants liberated by exposure of the sample to aqueous phases, mediate and accelerate the degradation of critically important but sensitive organic compounds such as DNA. FINDING T-2: Warming samples increases reaction rates and destroys compounds making biological studies much more time-sensitive. MAJOR FINDING T-3: Given the potential for rapid degradation of biomolecules, (especially in the presence of aqueous phases and/or reactive O-containing compounds) Sample Safety Assessment Protocol (SSAP) and parallel biological analysis are time sensitive and must be carried out as soon as possible. FINDING T-4: If molecules or whole cells from either extant or extinct organisms have persisted under present-day martian conditions in the samples, then it follows that preserving sample aliquots under those same conditions (i.e., 6 mbar total pressure in a dominantly CO2 atmosphere and at an average temperature of -80°C) in a small isolation chamber is likely to allow for their continued persistence. FINDING T-5: Volatile compounds (e.g., HCN and formaldehyde) have been lost from Solar System materials stored under standard curation conditions. FINDING T-6: Reactive O-containing species have been identified in situ at the martian surface and so may be present in rock or regolith samples returned from Mars. These species rapidly degrade organic molecules and react more rapidly as temperature and humidity increase. FINDING T-7: Because the sample tubes would not be closed with perfect seals and because, after arrival on Earth, there will be a large pressure gradient across that seal such that the probability of contamination of the tube interiors by terrestrial gases increases with time, the as-received sample tubes are considered a poor choice for long-term gas sample storage. This is an important element of time sensitivity. MAJOR FINDING T-8: To determine how volatiles may have been exchanged with headspace gas during transit to Earth, the composition of martian atmosphere (in a separately sealed reservoir and/or extracted from the witness tubes), sample headspace gas composition, temperature/time history of the samples, and mineral composition (including mineral-bound volatiles) must all be quantified. When the sample tube seal is breached, mineral-bound volatile loss to the curation atmosphere jeopardizes robust determination of volatile exchange history between mineral and headspace. FINDING T-9: Previous experiments with mineral powders show that sulfate minerals are susceptible to H2O loss over timescales of hours to days. In addition to volatile loss, these processes are accompanied by mineralogical transformation. Thus, investigations targeting these minerals should be considered time-sensitive. FINDING T-10: Sulfate minerals may be stabilized by storage under fixed relative-humidity conditions, but only if the identity of the sulfate phase(s) is known a priori. In addition, other methods such as freezing may also stabilize these minerals against volatile loss. FINDING T-11: Hydrous perchlorate salts are likely to undergo phase transitions and volatile exchange with ambient surroundings in hours to days under temperature and relative humidity ranges typical of laboratory environments. However, the exact timescale over which these processes occur is likely a function of grain size, lithification, and/or cementation. FINDING T-12: Nanocrystalline or X-ray amorphous materials are typically stabilized by high proportions of surface adsorbed H2O. Because this surface adsorbed H2O is weakly bound compared to bulk materials, nanocrystalline materials are likely to undergo irreversible ripening reactions in response to volatile loss, which in turn results in decreases in specific surface area and increases in crystallinity. These reactions are expected to occur over the timescale of weeks to months under curation conditions. Therefore, the crystallinity and specific surface area of nanocrystalline materials should be characterized and monitored within a few months of opening the sample tubes. These are considered time-sensitive measurements that must be made as soon as possible. FINDING T-13: Volcanic and impact glasses, as well as opal-CT, are metastable in air and susceptible to alteration and volatile exchange with other solid phases and ambient headspace. However, available constraints indicate that these reactions are expected to proceed slowly under typical laboratory conditions (i.e., several years) and so analyses targeting these materials are not considered time sensitive. FINDING T-14: Surface adsorbed and interlayer-bound H2O in clay minerals is susceptible to exchange with ambient surroundings at timescales of hours to days, although the timescale may be modified depending on the degree of lithification or cementation. Even though structural properties of clay minerals remain unaffected during this process (with the exception of the interlayer spacing), investigations targeting H2O or other volatiles bound on or within clay minerals should be considered time sensitive upon opening the sample tube. FINDING T-15: Hydrated Mg-carbonates are susceptible to volatile loss and recrystallization and transformation over timespans of months or longer, though this timescale may be modified by the degree of lithification and cementation. Investigations targeting hydrated carbonate minerals (either the volatiles they host or their bulk mineralogical properties) should be considered time sensitive upon opening the sample tube. MAJOR FINDING T-16: Current understanding of mineral-volatile exchange rates and processes is largely derived from monomineralic experiments and systems with high surface area; lithified sedimentary rocks (accounting for some, but not all, of the samples in the cache) will behave differently in this regard and are likely to be associated with longer time constants controlled in part by grain boundary diffusion. Although insufficient information is available to quantify this at the present time, the timescale of mineral-volatile exchange in lithified samples is likely to overlap with the sample processing and curation workflow (i.e., 1-10 months; Table 4). This underscores the need to prioritize measurements targeting mineral-hosted volatiles within biocontainment. FINDING T-17: The liberation of reactive O-species through sample treatment or processing involving H2O (e.g., rinsing, solvent extraction, particle size separation in aqueous solution, or other chemical extraction or preparation protocols) is likely to result in oxidation of some component of redox-sensitive materials in a matter of hours. The presence of reactive O-species should be examined before sample processing steps that seek to preserve or target redox-sensitive minerals. Electron paramagnetic resonance spectroscopy (EPR) is one example of an effective analytical method capable of detecting and characterizing the presence of reactive O-species. FINDING T-18: Environments that maintain anoxia under inert gas containing <
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- 2022
14. The case for metamorphic base metal mineralization: pyrite chemical, Cu and S isotope data from the Cu-Zn deposit at Kupferberg in Bavaria, Germany
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Höhn, S., Frimmel, H.E., Debaille, V., Pašava, J., Kuulmann, L., and Debouge, W.
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- 2017
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15. PLANET TOPERS: Planets, Tracing the Transfer, Origin, Preservation, and Evolution of their ReservoirS
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Dehant, V., Asael, D., Baland, R. M., Baludikay, B. K., Beghin, J., Belza, J., Beuthe, M., Breuer, D., Chernonozhkin, S., Claeys, Ph., Cornet, Y., Cornet, L., Coyette, A., Debaille, V., Delvigne, C., Deproost, M. H., De WInter, N., Duchemin, C., El Atrassi, F., François, C., De Keyser, J., Gillmann, C., Gloesener, E., Goderis, S., Hidaka, Y., Höning, D., Huber, M., Hublet, G., Javaux, E. J., Karatekin, Ö., Kodolanyi, J., Revilla, L. Lobo, Maes, L., Maggiolo, R., Mattielli, N., Maurice, M., McKibbin, S., Morschhauser, A., Neumann, W., Noack, L., Pham, L. B. S., Pittarello, L., Plesa, A. C., Rivoldini, A., Robert, S., Rosenblatt, P., Spohn, T., Storme, J. -Y., Tosi, N., Trinh, A., Valdes, M., Vandaele, A. C., Vanhaecke, F., Van Hoolst, T., Van Roosbroek, N., Wilquet, V., and Yseboodt, M.
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- 2016
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16. Nd–Hf Isotope Systematics of Megacrysts from the Mbuji-Mayi Kimberlites, D. R. Congo: Evidence for a Metasomatic Origin Related to Kimberlite Interaction with the Cratonic Lithospheric Mantle
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Pivin, M., Debaille, V., Mattielli, N., Demaiffe, D., Pearson, D Graham, editor, Grütter, Herman S, editor, Harris, Jeff W, editor, Kjarsgaard, Bruce A, editor, O’Brien, Hugh, editor, Rao, N V Chalapathi, editor, and Sparks, Steven, editor
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- 2013
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17. The evolution of Hadean–Eoarchaean geodynamics
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O'Neill, C. and Debaille, V.
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- 2014
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18. Aqueously altered igneous rocks sampled on the floor of Jezero crater, Mars
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Farley, K. A., primary, Stack, K. M., additional, Shuster, D. L., additional, Horgan, B. H. N., additional, Hurowitz, J. A., additional, Tarnas, J. D., additional, Simon, J. I., additional, Sun, V. Z., additional, Scheller, E. L., additional, Moore, K. R., additional, McLennan, S. M., additional, Vasconcelos, P. M., additional, Wiens, R. C., additional, Treiman, A. H., additional, Mayhew, L. E., additional, Beyssac, O., additional, Kizovski, T. V., additional, Tosca, N. J., additional, Williford, K. H., additional, Crumpler, L. S., additional, Beegle, L. W., additional, Bell, J. F., additional, Ehlmann, B. L., additional, Liu, Y., additional, Maki, J. N., additional, Schmidt, M. E., additional, Allwood, A. C., additional, Amundsen, H. E. F., additional, Bhartia, R., additional, Bosak, T., additional, Brown, A. J., additional, Clark, B. C., additional, Cousin, A., additional, Forni, O., additional, Gabriel, T. S. J., additional, Goreva, Y., additional, Gupta, S., additional, Hamran, S.-E., additional, Herd, C. D. K., additional, Hickman-Lewis, K., additional, Johnson, J. R., additional, Kah, L. C., additional, Kelemen, P. B., additional, Kinch, K. B., additional, Mandon, L., additional, Mangold, N., additional, Quantin-Nataf, C., additional, Rice, M. S., additional, Russell, P. S., additional, Sharma, S., additional, Siljeström, S., additional, Steele, A., additional, Sullivan, R., additional, Wadhwa, M., additional, Weiss, B. P., additional, Williams, A. J., additional, Wogsland, B. V., additional, Willis, P. A., additional, Acosta-Maeda, T. A., additional, Beck, P., additional, Benzerara, K., additional, Bernard, S., additional, Burton, A. S., additional, Cardarelli, E. L., additional, Chide, B., additional, Clavé, E., additional, Cloutis, E. A., additional, Cohen, B. A., additional, Czaja, A. D., additional, Debaille, V., additional, Dehouck, E., additional, Fairén, A. G., additional, Flannery, D. T., additional, Fleron, S. Z., additional, Fouchet, T., additional, Frydenvang, J., additional, Garczynski, B. J., additional, Gibbons, E. F., additional, Hausrath, E. M., additional, Hayes, A. G., additional, Henneke, J., additional, Jørgensen, J. L., additional, Kelly, E. M., additional, Lasue, J., additional, Le Mouélic, S., additional, Madariaga, J. M., additional, Maurice, S., additional, Merusi, M., additional, Meslin, P.-Y., additional, Milkovich, S. M., additional, Million, C. C., additional, Moeller, R. C., additional, Núñez, J. I., additional, Ollila, A. M., additional, Paar, G., additional, Paige, D. A., additional, Pedersen, D. A. K., additional, Pilleri, P., additional, Pilorget, C., additional, Pinet, P. C., additional, Rice, J. W., additional, Royer, C., additional, Sautter, V., additional, Schulte, M., additional, Sephton, M. A., additional, Sharma, S. K., additional, Sholes, S. F., additional, Spanovich, N., additional, St. Clair, M., additional, Tate, C. D., additional, Uckert, K., additional, VanBommel, S. J., additional, Yanchilina, A. G., additional, and Zorzano, M.-P., additional
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- 2022
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19. Report of the iMOST Study
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Zorzano, M.P, Zipfel, J, Wheeler, R.M, Westall, F, Werner, S.C, Weiss, B.P, Wadhwa, M, Van Kranendonk, M.J, Usui, T, Tosca, N.J, Kate, I.L, Swindle, T.D, Steele, A, Spry, J.A, Smith, C.L, Siljeström, S, Shuster, D.L, Sharp, Z.D, Shaheen, R, Sephton, M.A, Schwenzer, S.P, Schmitz, N, Rucker, M.A, Rettberg, P, Raulin, F, Ori, G.G, Niles, P.B, Mustard, J.F, Moynier, F, Moser, D.E, McLennan, S.M, McCubbin, F.M, McCoy, J.T, Mayhew, L.E, Mangold, N, Mackelprang, R, Kleinhenz, J, Kleine, T, Humayun, M, Horgan, B, Herd, C.D.K, Hausrath, E.M, Harrington, A.D, Hallis, L.J, Goreva, Y.S, Glavin, D.P, Fogarty, J, Filiberto, J, Fernandez-Remolar, D.C, Farmer, J.D, Ehlmann, B.L, Dixon, M, Des Marais, D.J, Debaille, V, Czaja, A.D, Campbell, K.A, Busemann, H, Brucato, J.R, Boucher, D, Borg, L.E, Bishop, J.L, Benning, L.G, Anand, M, Ammannito, E, Amelin, Y, Altieri, F, Carrier, B. L, Sefton-Nash, E, McSween, H. Y, Grady, M. M, and Beaty, D. W
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UNKNOWN
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- 2018
20. Report of the iMOST Study
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Beaty, D. W, Grady, M. M, McSween, H. Y, Sefton-Nash, E, Carrier, B. L, Altieri, F, Amelin, Y, Ammannito, E, Anand, M, Benning, L.G, Bishop, J.L, Borg, L.E, Boucher, D, Brucato, J.R, Busemann, H, Campbell, K.A, Czaja, A.D, Debaille, V, Des Marais, D.J, Dixon, M, Ehlmann, B.L, Farmer, J.D, Fernandez-Remolar, D.C, Filiberto, J, Fogarty, J, Glavin, D.P, Goreva, Y.S, Hallis, L.J, Harrington, A.D, Hausrath, E.M, Herd, C.D.K, Horgan, B, Humayun, M, Kleine, T, Kleinhenz, J, Mackelprang, R, Mangold, N, Mayhew, L.E, McCoy, J.T, McCubbin, F.M, McLennan, S.M, Moser, D.E, Moynier, F, Mustard, J.F, Niles, P.B, Ori, G.G, Raulin, F, Rettberg, P, Rucker, M.A, Schmitz, N, Schwenzer, S.P, Sephton, M.A, Shaheen, R, Sharp, Z.D, Shuster, D.L, Siljeström, S, Smith, C.L, Spry, J.A, Steele, A, Swindle, T.D, Kate, I.L, Tosca, N.J, Usui, T, Van Kranendonk, M.J, Wadhwa, M, Weiss, B.P, Werner, S.C, Westall, F, Wheeler, R.M, Zipfel, J, and Zorzano, M.P
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- 2018
21. Seeking Signs of Life on Mars: the Importance of Sedimentary Suites as Part of a Mars Sample Return Campaign
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Mangold, N, McLennan, S. M, Czaja, A. D, Ori, G. G, Tosca, N. J, Altieri, F, Amelin, Y, Ammannito, E, Anand, M, Beaty, D. W, Benning, L. G, Bishop, J. L, Borg, L. E, Boucher, D, Brucato, J. R, Busemann, H, Campbell, K. A, Carrier, B. L, Debaille, V, Des Marais, D. J, Dixon, M, Ehlmann, B. L, Farmer, J. D, Fernandez-Remolar, D. C, Fogarty, J, Glavin, D. P, Goreva, Y. S, Grady, M. M, Hallis, L. J, Harrington, A. D, Hausrath, E. M, Herd, C. D. K, Horgan, B, Humayun, M, Kleine, T, Kleinhenz, J, Mackelprang, R, Mayhew, L. E, McCubbin, F. M, McCoy, J. T, McSween, H. Y, Moser, D. E, Moynier, F, Mustard, J. F, Niles, P. B, Raulin, F, Rettberg, P, Rucker, M. A, Schmitz, N, Sefton-Nash, E, Sephton, M. A, Shaheen, R, Shuster, D. L, Siljeström, S, Smith, C. L, Spry, J. A, Steele, A, Swindle, T. D, ten Kate, I. L, Usui, T, Van Kranendonk, M. J, Wadhwa, M, Weiss, B. P, Werner, S. C, Westall, F, Wheeler, R. M, Zipfel, J, and Zorzano, M. P
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Space Sciences (General) - Abstract
Seeking the signs of life on Mars is often considered the "first among equal" objectives for any potential Mars Sample Return (MSR) campaign. Among the geological settings considered to have the greatest potential for recording evidence of ancient life or its pre-biotic chemistry on Mars are lacustrine (and marine, if ever present) sedimentary depositional environments. This potential, and the possibility of returning samples that could meaningfully address this objective, have been greatly enhanced by investigations of an ancient redox stratified lake system in Gale crater by the Curiosity rover.
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- 2018
22. Seeking Signs of Life on Mars: A Strategy for Selecting and Analyzing Returned Samples from Hydrothermal Deposits
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Campbell, K. A, Farmer, J. D, Van Kranendonk, M. J, Fernandez-Remolar, D. C, Czaja, A. D, Altieri, F, Amelin, Y, Ammannito, E, Anand, M, Beaty, D. W, Benning, L. G, Bishop, J. L, Borg, L. E, Boucher, D, Brucato, J. R, Busemann, J. R, Carrier, B. L, Debaille, V, Des Marais, D. J, Dixon, M, Ehlmann, B. L, Fogarty, James T, Glavin, D. P, Goreva, Y. S, Grady, M. M, Hallis, L. J, Harrington, A. D, Hausrath, E. M, Herd, C. D. K, Horgan, B, Humayun, M, Kleine, T, Kleinhenz, J, Mangold, N, Mackelprang, R, Mayhew, L. E, McCubbin, F. M, Mccoy, Teresa R, McLennan, S. M, McSween, H. Y, Moser, D. E, Moynier, F, Mustard, J. F, Niles, P. B, Ori, G. G, Raulin, F, Rettberg, P, Rucker, Michelle A, Schmitz, N, Sefton-Nash, E, Sephton, M. A, Shaheen, R, Shuster, D. L, Siljestrom, S, Smith, C. L, Spry, J. A, Steele, A, Swindle, T. D, ten Kate, I. L, Tosca, N. J, Usui, T, Wadhwa, M, Weiss, B. P, Werner, S. C, Westall, F, Wheeler, R. M, Zipfel, J, and Zorzano, M. P
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Space Sciences (General) - Abstract
Highly promising locales for biosignature prospecting on Mars are ancient hydrothermal deposits, formed by the interaction of surface water with heat from volcanism or impacts. On Earth, they occur throughout the geological record (to at least approx. 3.5 Ga), preserving robust mineralogical, textural and compositional evidence of thermophilic microbial activity. Hydrothermal systems were likely present early in Mars' history, including at two of the three finalist candidate landing sites for M2020, Columbia Hills and NE Syrtis Major. Hydrothermal environments on Earth's surface are varied, constituting subaerial hot spring aprons, mounds and fumaroles; shallow to deep-sea hydrothermal vents (black and white smokers); and vent mounds and hot-spring discharges in lacustrine and fluvial settings. Biological information can be preserved by rapid, spring-sourced mineral precipitation, but also could be altered or destroyed by postdepositional events. Thus, field observations need to be followed by detailed laboratory analysis to verify potential biosignatures. See Attachment
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- 2018
23. Probing Neodymium Isotopic Variations in the Inner Solar System
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Armytage, R. M. G and Debaille, V
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Space Sciences (General) - Abstract
One of the key problems in planetary science is the identification of the building blocks of Earth, and whether they exist within our current collection of meteorites. Stable mass independent isotopic anomalies, usually nucleosynthetic in origin, are a key tool in fingerprinting material coming from different accretionary regions within the protoplanetary disk. For a number of isotopic systems such as O, Ni, Ti and Cr, enstatite chondrites (EC) appear to be the strongest candidates for Earth's building blocks, despite their low Mg/Si ratios relative to the bulk Earth. It has been proposed that Earth, the Moon-forming impactor and enstatite chondrites all were originally sourced from the same reservoir in the protoplanetary disk, but subsequently experienced divergent chemical evolution pathways. This was recently challenged by who used the correlation between Mo and Nd isotopes in bulk meteorites to argue that such a reservoir does not exist as the isotopic composition of enstatite chondrites is resolvable from Earth. However, in detail the Nd isotopic ratios of EC ((142)Nd/(144)Nd, (148)Nd/(144)Nd, (150)Nd/(144)Nd) show considerable variability, and overlap significantly with the isotopic composition of both the bulk Earth and ordinary chondrites (OC). previously identified Nd isotopic variability in EC, linking it to the degree of equilibration the meteorite had experienced, however they only focused on collecting high precision (142)Nd/(144)Nd, which also has contributions from the decay of the short-lived Sm-146 nuclide (t(sub 1/2) ~103 Myr), making identification of nucleosynthetic anomalies less clear. While the study of reports all the Nd isotopic ratios measured at high precision, only equilibrated EC were analyzed. Therefore, with the currently published data it is unclear to what extent thermal equilibration in the EC is responsible for the variation observed in the stable Nd isotopic ratios, and whether the EC reservoir can be resolved from Earth. In order to better understand the genetic relationship between enstatite chondrites and the Earth we are carrying out a more systematic study including both equilibrated and unequilibrated enstatite chondrites, focusing on high precision analysis of all the stable Nd isotopic ratios.
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- 2018
24. Obsidian and mafic volcanic glasses from the Philippines and Vietnam found in the Paris Museum Australasian tektite collection
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Rochette, P., primary, Bezaeva, N. S., additional, Beck, P., additional, Debaille, V., additional, Folco, L., additional, Gattacceca, J., additional, Gounelle, M., additional, and Masotta, M., additional
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- 2022
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25. CR-TYPE CHONDRITE FOR AIRBURST EVENT OVER EAST ANTARCTICA 430 KA AGO
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Goderis, S., Ginneken, M., Hibiya, Y., Hobin, K., Grigoryan, R., Greenwood, R. C., Maldeghem, F., Chernonozhkin, S. M., Vanhaecke, F., Debaille, V., Philippe Claeys, Chemistry, Analytical, Environmental & Geo-Chemistry, Faculty of Sciences and Bioengineering Sciences, and Earth System Sciences
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Introduction: The geological record contains scarce evidence for airbursts, the most common type of hypervelocity impact events. During airbursts, impactors of 50 to 150 m in size are fragmented and vaporized during atmospheric entry, as exemplified by the Tunguska and Chelyabinsk events [1]. In recent years, meteoritic debris resulting from such low-altitude airbursts has been found on various locations across Antarctica (cf. summary in [2]). Fine-grained (
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- 2022
26. SSP (Synthetic Shergottite Powder), a new martian analogue for destructive analysis and experiments
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Fortier, V., Debaille, V., Dehant, Véronique, Bultel, B., 53rd Lunar and Planetary Science Conference, and UCL - SST/ELI/ELIC - Earth & Climate
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Martian rocky material available on Earth is only composed of meteorites and is quite limited in terms of mass and numbers. So far, less than 200 kg of material distributed unevenly among around 280 martian meteorites is available, and this limited amount directly impairs the possibility to perform destructive analyses and experiments, such as alteration and hydrothermal experiments. One of the main aspects of the current Mars2020 mission and the following ones is to bring back rock samples from Mars in the next 10 years [1]. However, while we will have a geological context for the samples, the total mass that will be collected will also be limited. It is thus crucial to seek for analogs of martian meteorites [2], not suffering this limitation while bearing specific properties of the martian meteorites. It is important to note that an analog must not need to be perfect but fit for the purpose of the considered experiments.
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- 2022
27. Experimental study of serpentinization and abiotic CH$_4$ production in martian conditions
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Fortier, V., Debaille, V., Dehant, Véronique, Bultel, B., Debecker, D., 53rd Lunar and Planetary Science Conference, and UCL - SST/ELI/ELIC - Earth & Climate
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The presence of methane on Mars remains highly debated in particular with contrasted detection results from Curiosity rover [1] and TGO [2]. In addition, the possible methane cycle is also poorly known: source(s) and removal process(es) remain currently undefined; and it is not known yet if this methane emissions might be related to a biological activity. Because of orbital detection of serpentine on Mars [3], and of the mafic-ultramafic nature of Mars ancient crust, a putative abiotic candidate source is serpentinization associated with Sabatier reaction. The aim of this work is to experimentally study the production capacity of H2 and mainly CH4 by those abiotic processes in martian conditions to determine the viability of this origin.
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- 2022
28. Science and Curation Considerations for the Design of a Mars Sample Return (MSR) Sample Receiving Facility
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Carrier, B. L., Beaty, D., Hutzler, Aurore, Smith, Alvin, Kminek, G., Meyer, M., Haltigin, T., Hays, Lindsay, Agee, Carl, Busemann, H., Cavalazzi, B., Cockell, C., Debaille, V, Glavin, D P, Grady, M., Hauber, Ernst, Marty, B., McCubbin, F. M., Pratt, Lisa, Regberg, Aaron, Smith, C., Summons, R E, Swindle, T. D., Tait, Kimberly, Tosca, N. J., Udry, Arya, Usui, Tomohiro, Velbel, Michael, Wadhwa, M., Westall, F., Zorzano, M.-P., California Institute of Technology (CALTECH), European Space Agency (ESA), NASA Headquarters, Canadian Space Agency (CSA), The University of New Mexico [Albuquerque], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Bologna, University of Edinburgh, Université libre de Bruxelles (ULB), NASA Goddard Space Flight Center (GSFC), The Open University [Milton Keynes] (OU), German Aerospace Center (DLR), 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), NASA Johnson Space Center (JSC), NASA, Indiana University [Bloomington], Indiana University System, The Natural History Museum [London] (NHM), University of Glasgow, Massachusetts Institute of Technology (MIT), University of Arizona, Royal Ontario Museum, University of Cambridge [UK] (CAM), University of Nevada [Las Vegas] (WGU Nevada), Japan Aerospace Exploration Agency [Tokyo] (JAXA), Michigan State University [East Lansing], Michigan State University System, Smithsonian Institution, Arizona State University [Tempe] (ASU), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), University of Aberdeen, Agence Spatiale Européenne = European Space Agency (ESA), University of Bologna/Università di Bologna, Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Frapart, Isabelle, Carrier B. L., Beaty D. W., Hutzler A., Smith A. L., Kminek G., Meyer M. A., Haltigin T., Hays L. E., Agee C. B., Busemann H., Cavalazzi B., Cockell C. S., Debaille V., Glavin D. P., Grady M. M., and Hauber E., Marty B., McCubbin F. M., Pratt L. M., Regberg A. B., Smith C. L., Summons R. E., Swindle T. D., Tait K. T., Tosca N. J., Udry A., Usui T., Velbel M. A., Wadhwa M., Westall F., Zorzano M. -P.
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geology ,Extraterrestrial Environment ,laboratory experiments ,Sample Safety Assessment Protocol (SSAP) ,Plant Extracts ,astrobiology ,Reproducibility of Results ,Mars ,intrumentation ,Space Flight ,sample return ,Agricultural and Biological Sciences (miscellaneous) ,[SDU] Sciences of the Universe [physics] ,containment ,contamination ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Sample Receiving Facility (SRF) ,Mars Sample Return (MSR) Campaign ,Spacecraft - Abstract
The most important single element of the "ground system" portion of a Mars Sample Return (MSR) Campaign is a facility referred to as the Sample Receiving Facility (SRF), which would need to be designed and equipped to receive the returned spacecraft, extract and open the sealed sample container, extract the samples from the sample tubes, and implement a set of evaluations and analyses of the samples. One of the main findings of the first MSR Sample Planning Group (MSPG, 2019a) states that "The scientific community, for reasons of scientific quality, cost, and timeliness, strongly prefers that as many sample-related investigations as possible be performed in PI-led laboratories outside containment." There are many scientific and technical reasons for this preference, including the ability to utilize advanced and customized instrumentation that may be difficult to reproduce inside in a biocontained facility, and the ability to allow multiple science investigators in different labs to perform similar or complementary analyses to confirm the reproducibility and accuracy of results. It is also reasonable to assume that there will be a desire for the SRF to be as efficient and economical as possible, while still enabling the objectives of MSR to be achieved. For these reasons, MSPG concluded, and MSPG2 agrees, that the SRF should be designed to accommodate only those analytical activities that could not reasonably be done in outside laboratories because they are time- or sterilization-sensitive, are necessary for the Sample Safety Assessment Protocol (SSAP), or are necessary parts of the initial sample characterization process that would allow subsamples to be effectively allocated for investigation. All of this must be accommodated in an SRF, while preserving the scientific value of the samples through maintenance of strict environmental and contamination control standards. Executive Summary The most important single element of the "ground system" portion of a Mars Sample Return (MSR) Campaign is a facility referred to as the Sample Receiving Facility (SRF), which would need to be designed and equipped to enable receipt of the returned spacecraft, extraction and opening of the sealed sample container, extraction of the samples from the sample tubes, and a set of evaluations and analyses of the samples-all under strict protocols of biocontainment and contamination control. Some of the important constraints in the areas of cost and required performance have not yet been set by the necessary governmental sponsors, but it is reasonable to assume there will be a desire for the SRF to be as efficient and economical as is possible, while still enabling the objectives of MSR science to be achieved. Additionally, one of the main findings of MSR Sample Planning Group (MSPG, 2019a) states "The scientific community, for reasons of scientific quality, cost, and timeliness, strongly prefers that as many sample-related investigations as possible be performed in PI-led laboratories outside containment." There are many scientific and technical reasons for this preference, including the ability to utilize advanced and customized instrumentation that may be difficult to reproduce inside a biocontained facility. Another benefit is the ability to enable similar or complementary analyses by multiple science investigators in different laboratories, which would confirm the reproducibility and accuracy of results. For these reasons, the MSPG concluded-and the MSR Science Planning Group Phase 2 (MSPG2) agrees-that the SRF should be designed to accommodate only those analytical activities inside biocontainment that could
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- 2021
29. Preliminary Planning for Mars Sample Return (MSR) Curation Activities in a Sample Receiving Facility
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Tait, Kimberly, McCubbin, F. M., Smith, C., Agee, Carl, Busemann, H., Cavalazzi, B., Debaille, V, Hutzler, Aurore, Usui, Tomohiro, Kminek, G., Meyer, M., Beaty, D., Carrier, B. L., Haltigin, T., Hays, Lindsay, Cockell, C., Glavin, D. P., Grady, M., Hauber, Ernst, Marty, B., Pratt, Lisa, Regberg, Aaron, Smith, Alvin, Summons, R E, Swindle, T. D., Tosca, N. J., Udry, Arya, Velbel, Michael, Wadhwa, M., Westall, F., Zorzano, M.-P., Royal Ontario Museum, NASA Johnson Space Center (JSC), NASA, The Natural History Museum [London] (NHM), University of Glasgow, The University of New Mexico [Albuquerque], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Bologna, Université libre de Bruxelles (ULB), European Space Agency (ESA), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), NASA Headquarters, California Institute of Technology (CALTECH), Canadian Space Agency (CSA), University of Edinburgh, NASA Goddard Space Flight Center (GSFC), The Open University [Milton Keynes] (OU), German Aerospace Center (DLR), 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), Indiana University [Bloomington], Indiana University System, Massachusetts Institute of Technology (MIT), University of Arizona, University of Cambridge [UK] (CAM), University of Nevada [Las Vegas] (WGU Nevada), Michigan State University [East Lansing], Michigan State University System, Smithsonian Institution, Arizona State University [Tempe] (ASU), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), University of Aberdeen, Tait K. T., McCubbin F. M., Smith C. L., Agee C. B., Busemann H., Cavalazzi B., Debaille V., Hutzler A., Usui T., Kminek G., Meyer M. A., Beaty D. W., Carrier B. L., Haltigin T., Hays L. E., Cockell C. S., Glavin D. P., Grady M. M., Hauber E., Marty B., Pratt L. M., Regberg A. B., Smith A. L., Summons R. E., Swindle T. D., and Tosca N. J.
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geology ,laboratory experiments ,Extraterrestrial Environment ,Mars Sample Return Planning Group 2 (MSPG2) ,astrobiology ,Mars ,Dust ,curation ,sample return ,Space Flight ,exploration ,Agricultural and Biological Sciences (miscellaneous) ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,sample receiving facility ,Exobiology ,Gases - Abstract
The Mars Sample Return Planning Group 2 (MSPG2) was tasked with identifying the steps that encompass all the curation activities that would happen within the MSR Sample Receiving Facility (SRF) and any anticipated curation-related requirements. An area of specific interest is the necessary analytical instrumentation. The SRF would be a Biosafety Level-4 facility where the returned MSR flight hardware would be opened, the sample tubes accessed, and the martian sample material extracted from the tubes. Characterization of the essential attributes of each sample would be required to provide enough information to prepare a sample catalog used in guiding the preparation of sample-related proposals by the world's research community and informing decisions by the sample allocation committee. The sample catalog would be populated with data and information generated during all phases of activity, including data derived concurrent with Mars 2020 sample-collecting rover activity, sample transport to Earth, and initial sample characterization within the SRF. We conclude that initial sample characterization can best be planned as a set of three sequential phases, which we have called Pre-Basic Characterization (Pre-BC), Basic Characterization (BC), and Preliminary Examination (PE), each of which requires a certain amount of instrumentation. Data on specific samples and subsamples obtained during sample safety assessments and time-sensitive scientific investigations would also be added to the catalog. There are several areas where future work would be beneficial to prepare for the receipt of samples, which would include the design of a sample tube isolation chamber and a strategy for opening the sample tubes and removing dust from the tube exteriors. Executive Summary All material collected from Mars (gases, dust, rock, regolith) would need to be carefully handled, stored, and analyzed following Earth return to minimize the alteration or contamination that could occur on Earth and maximize the scientific information that can be attained from the samples now and into the future. A Sample Receiving Facility (SRF) is where the Earth Entry System (EES) would be opened and the sample tubes opened and processed after they land on Earth. Samples should be accessible for research in biocontainment for time-sensitive studies and eventually, when deemed safe for release after sterilization or biohazard assessment, should be transferred out of biocontainment for allocation to scientific investigators in outside laboratories. There are two main mechanisms for allocation of samples outside the SRF: 1) Wait until the implementation of the Sample Safety Assessment Protocol (Planetary Protection) results concludes that the samples are non-hazardous, 2) Render splits of the samples non-hazardous by means of sterilization. To make these samples accessible, a series of observations and analytical measurements need to be completed to produce a sample catalog for the scientific community. Specialist members of the Mars Sample Return Planning Group Phase 2 (MSPG2), referred to here as the Curation Focus Group, have identified four curation goals that encompass all of the activities within the SRF: 1.Documentation of the state of the sample tubes and their contents prior to opening, 2.Inventory and tracking of the mass of each sample, 3.Preliminary assessment of lithology and any macroscopic forms of heterogeneity (on all the samples, non-invasive, in pristine isolators), 4.Sufficient characterization of the essential attributes of each sample to prepare a sample catalog and respond to requests by the sample allocation committee (partial samples, invasive, outside of pristine isolators). The sample catalog will provide data for the scientific community to make informed requests for samples for scientific investigations and for the approval of allocations of appropriate samples to satisfy these requests. The sample catalog would be populated with data and information generated during all phases of activity, including data derived from the landed Mars 2020 mission, during sample collection and transport to Earth, and reception within the Sample Receiving Facility. Data on specific samples and subsamples would also be generated during curation activities carried out within the Sample Receiving Facility and during sample safety assessments, time-sensitive studies, and a series of initial sample characterization steps we refer to as Pre-Basic Characterization (Pre-BC), Basic Characterization (BC), and Preliminary Examination (PE) phases. A significant portion of the Curation Focus Group's efforts was to determine which instrumentation would be required to produce a sample catalog for the scientific community and how and when certain instrumentation should be used. The goal is to provide enough information for the PIs to request material for their studies but to avoid facilitating studies that target scientific research that is better left to peer-reviewed competitive processes. We reviewed the proposed scientific objectives of the International MSR Objectives and Samples Team (iMOST) (Beaty
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- 2021
30. A Younger Age for ALH84001 and Its Geochemical Link to Shergottite Sources in Mars
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Lapen, T. J., Righter, M., Brandon, A. D., Debaille, V., Beard, B. L., Shafer, J. T., and Peslier, A. H.
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- 2010
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31. Sample return of primitive matter from the outer Solar System
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Vernazza, P., primary, Beck, P., additional, Ruesch, O., additional, Bischoff, A., additional, Bonal, L., additional, Brennecka, G., additional, Brunetto, R., additional, Busemann, H., additional, Carter, J., additional, Carli, C., additional, Cartier, C., additional, Ciarniello, M., additional, Debaille, V., additional, Delsanti, A., additional, D’Hendecourt, L., additional, Füri, E., additional, Groussin, O., additional, Guilbert-Lepoutre, A., additional, Helbert, J., additional, Hoppe, P., additional, Jehin, E., additional, Jorda, L., additional, King, A., additional, Kleine, T., additional, Lamy, P., additional, Lasue, J., additional, Le Guillou, C., additional, Leroux, H., additional, Leya, I., additional, Magna, T., additional, Marrocchi, Y., additional, Morlok, A., additional, Mousis, O., additional, Palomba, E., additional, Piani, L., additional, Quirico, E., additional, Remusat, L., additional, Roskosz, M., additional, Rubin, M., additional, Russell, S., additional, Schönbächler, M., additional, Thomas, N., additional, Villeneuve, J., additional, Vinogradoff, V., additional, Wurz, P., additional, and Zanda, B., additional
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- 2021
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32. A 650 km2 Miocene strewnfield of splash-form impact glasses in the Atacama Desert, Chile
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Gattacceca, J., primary, Devouard, B., additional, Barrat, J.-A., additional, Rochette, P., additional, Balestrieri, M.L., additional, Bigazzi, G., additional, Ménard, G., additional, Moustard, F., additional, Dos Santos, E., additional, Scorzelli, R., additional, Valenzuela, M., additional, Quesnel, Y., additional, Gounelle, M., additional, Debaille, V., additional, Beck, P., additional, Bonal, L., additional, Reynard, B., additional, and Warner, M., additional
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- 2021
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33. The Scientific Importance of Returning Airfall Dust as a Part of Mars Sample Return (MSR)
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Grady, M., Summons, R E, Swindle, T. D., Westall, F., Kminek, G., Meyer, M., Beaty, D., Carrier, B. L., Haltigin, T., Hays, Lindsay, Agee, Carl, Busemann, H., Cavalazzi, B., Cockell, C., Debaille, V, Glavin, D P, Hauber, Ernst, Hutzler, Aurore, Marty, B., McCubbin, F. M., Pratt, Lisa, Regberg, Aaron, Smith, Alvin, Smith, C., Tait, Kimberly, Tosca, N. J., Udry, Arya, Usui, Tomohiro, Velbel, Michael, Wadhwa, M., Zorzano, M.-P., The Open University [Milton Keynes] (OU), Massachusetts Institute of Technology (MIT), University of Arizona, Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), European Space Agency (ESA), NASA Headquarters, California Institute of Technology (CALTECH), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Canadian Space Agency (CSA), The University of New Mexico [Albuquerque], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Bologna, University of Edinburgh, Université libre de Bruxelles (ULB), NASA Goddard Space Flight Center (GSFC), German Aerospace Center (DLR), 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), Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, Indiana University [Bloomington], Indiana University System, NASA, The Natural History Museum [London] (NHM), University of Glasgow, Royal Ontario Museum, University of Cambridge [UK] (CAM), University of Nevada [Las Vegas] (WGU Nevada), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Michigan State University [East Lansing], Michigan State University System, Smithsonian Institution, Arizona State University [Tempe] (ASU), University of Aberdeen, and Grady Monica M., Summons Roger E., Swindle Timothy D., Westall Frances, Kminek Gerhard, Meyer Michael A., Beaty David W., Carrier Brandi L., Haltigin Timothy, Hays Lindsay E., Agee Carl B., Busemann Henner, Cavalazzi Barbara, Cockell Charles S., Vinciane Debaille, Glavin Daniel P., Hauber Ernst, Hutzler Aurore, Marty Bernard, McCubbin Francis M., Pratt Lisa M., Regberg Aaron B., Smith Alvin L., Smith Caroline L., Tait Kimberly T., Tosca Nicholas J., Udry Arya, Usui Tomohiro, Velbel Michael A., Wadhwa Meenakshi, Zorzano Maria-Paz
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geology ,Extraterrestrial Environment ,MSR Sample Receiving Facility, MSR Campaign elements ,surface-atmosphere interaction ,Atmosphere ,Earth, Planet ,Mars ,Dust ,sample return ,Agricultural and Biological Sciences (miscellaneous) ,MSR Campaign ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Humans ,samples ,global circulation ,mineralogy ,surface processes ,laboratory analysis - Abstract
International audience; Dust transported in the martian atmosphere is of intrinsic scientific interest and has relevance for the planning of human missions in the future. The MSR Campaign, as currently designed, presents an important opportunity to return serendipitous, airfall dust. The tubes containing samples collected by the Perseverance rover would be placed in cache depots on the martian surface perhaps as early as 2023-24 for recovery by a subsequent mission no earlier than 2028-29, and possibly as late as 2030-31. Thus, the sample tube surfaces could passively collect dust for multiple years. This dust is deemed to be exceptionally valuable as it would inform our knowledge and understanding of Mars' global mineralogy, surface processes, surface-atmosphere interactions, and atmospheric circulation. Preliminary calculations suggest that the total mass of such dust on a full set of tubes could be as much as 100 mg and, therefore, sufficient for many types of laboratory analyses. Two planning steps would optimize our ability to take advantage of this opportunity: (1) the dust-covered sample tubes should be loaded into the Orbiting Sample container (OS) with minimal cleaning and (2) the capability to recover this dust early in the workflow within an MSR Sample Receiving Facility (SRF) would need to be established. A further opportunity to advance dust/atmospheric science using MSR, depending upon the design of the MSR Campaign elements, may lie with direct sampling and the return of airborne dust.
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- 2021
34. Long-Term Evolution of the Martian Crust-Mantle System
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Grott, M., Baratoux, D., Hauber, E., Sautter, V., Mustard, J., Gasnault, O., Ruff, S. W., Karato, S.-I., Debaille, V., Knapmeyer, M., Sohl, F., Van Hoolst, T., Breuer, D., Morschhauser, A., and Toplis, M. J.
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- 2013
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35. A large meteoritic event over Antarctica ca. 430 ka ago inferred from chondritic spherules from the Sør Rondane Mountains
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Van Ginneken, M., primary, Goderis, S., additional, Artemieva, N., additional, Debaille, V., additional, Decrée, S., additional, Harvey, R. P., additional, Huwig, K. A., additional, Hecht, L., additional, Yang, S., additional, Kaufmann, F. E. D., additional, Soens, B., additional, Humayun, M., additional, Van Maldeghem, F., additional, Genge, M. J., additional, and Claeys, P., additional
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- 2021
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36. Coupled 142Nd-143Nd evidence for a protracted magma ocean in Mars
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Debaille, V., Brandon, A. D., Yin, Q. Z., and Jacobsen, B.
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Environmental issues ,Science and technology ,Zoology and wildlife conservation - Abstract
Author(s): V. Debaille (corresponding author) [1]; A. D. Brandon [2]; Q. Z. Yin [3]; B. Jacobsen [3] Resolving early silicate differentiation timescales is crucial for understanding the chemical evolution and [...]
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- 2007
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37. Coupled [sup.142]Nd-[sup.143]Nd evidence for a protracted magma ocean in Mars
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Debaille, V., Brandon, A.D., Yin, Q.Z., and Jacobsen, B.
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Environmental issues ,Science and technology ,Zoology and wildlife conservation - Abstract
Resolving early silicate differentiation timescales is crucial for understanding the chemical evolution and thermal histories of terrestrial planets (1). Planetary-scale magma oceans are thought to have formed during early stages [...]
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- 2007
38. Long-Term Evolution of the Martian Crust-Mantle System
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Grott, M., primary, Baratoux, D., additional, Hauber, E., additional, Sautter, V., additional, Mustard, J., additional, Gasnault, O., additional, Ruff, S. W., additional, Karato, S.-I., additional, Debaille, V., additional, Knapmeyer, M., additional, Sohl, F., additional, Van Hoolst, T., additional, Breuer, D., additional, Morschhauser, A., additional, and Toplis, M. J., additional
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- 2012
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39. Caleta el Cobre 022 Martian meteorite: Increasing nakhlite diversity
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Krämer Ruggiu, L., primary, Gattacceca, J., additional, Devouard, B., additional, Udry, A., additional, Debaille, V., additional, Rochette, P., additional, Lorand, J.‐P., additional, Bonal, L., additional, Beck, P., additional, Sautter, V., additional, Busemann, H., additional, Meier, M. M. M., additional, Maden, C., additional, Hublet, G., additional, and Martinez, R., additional
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- 2020
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40. Dry late accretion inferred from Venus’s coupled atmosphere and internal evolution
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Gillmann, C., primary, Golabek, G. J., additional, Raymond, S. N., additional, Schönbächler, M., additional, Tackley, P. J., additional, Dehant, V., additional, and Debaille, V., additional
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- 2020
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41. Structural and Geochemical Interactions Between Magma and Sedimentary Host Rock: The Hovedøya Case, Oslo Rift, Norway
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Poppe, S., primary, Galland, O., additional, Winter, N. J., additional, Goderis, S., additional, Claeys, P., additional, Debaille, V., additional, Boulvais, P., additional, and Kervyn, M., additional
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- 2020
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42. The effects of terrestrial weathering on samarium-neodymium isotopic composition of chondrites
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Pourkhorsamdi, H., Debaille, V., Armytage, R. M. G., Ginneken, M., Rochette, P., Jerome Gattacceca, Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Collège de France (CdF (institution))-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA), Université libre de Bruxelles (ULB), National Aeronautics and Space Administration, Partenaires INRAE, Royal Belgian Institute of Natural Sciences (RBINS), ProdInra, Migration, Institut de Recherche pour le Développement (IRD)-Institut National de la Recherche Agronomique (INRA)-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), and National Aeronautics and Space Administration (NASA)
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[SDV] Life Sciences [q-bio] ,[SDV]Life Sciences [q-bio] ,hot deserts ,ComputingMilieux_MISCELLANEOUS - Abstract
International audience
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- 2019
43. Caleta el cobre 022: An unusual nakhlite with abundant aqueous alteration
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Ruggiu, Lk, Gattacceca, J, Devouard, B, Udry, A, Debaille, V, Rochette, P., Lorand, Jp, Bonal, L, Beck, P, Sautter, V, Meier, Mmm, Gounelle, M, Marrocchi, Y, Maden, C, Busemann, H, Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Meteoritical Society, and Lucas, Nelly
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[SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry ,[SDU.STU.GC] Sciences of the Universe [physics]/Earth Sciences/Geochemistry ,ComputingMilieux_MISCELLANEOUS - Abstract
International audience
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- 2019
44. Onset of plate tectonics on Earth and implications for habitability
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François, C., Debaille, V., Paquette, Jean-Louis, Baudet, D., Javaux, E.J., Université libre de Bruxelles (ULB), Laboratoire Magmas et Volcans (LMV), Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement et la société-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut national des sciences de l'Univers (INSU - CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Université Jean Monnet [Saint-Étienne] (UJM), Département de Géologie, Université de Liège, Université Clermont Auvergne [2017-2020] (UCA [2017-2020]), Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Institut de Recherche pour le Développement et la société-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), Institut national des sciences de l'Univers (INSU - CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), and Jouhannel, Sylvaine
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[SDU]Sciences of the Universe [physics] ,[SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry ,[SDU.STU.GC] Sciences of the Universe [physics]/Earth Sciences/Geochemistry ,ComputingMilieux_MISCELLANEOUS - Abstract
International audience; Understanding the geodynamic processes of the Early Earth is crucial because they have strong implications for the habitability of the Earth but also for other planets. The Earth is the only proven planet in the solar system displaying lithospheric plate tectonics. However, plate tectonics on Earth did not always function as today, and the Archean was likely characterized by a stagnant-lid regime. Characterizing the transition from ancient to modern-style geodynamic regimes, including subduction process, is therefore important to understand the evolution of our own planet but also to compare our model to other rocky planets in our solar system. Here, we have characterized the oldest high pressure and low temperature eclogite worldwide (2089 ± 13 Ma) discovered in the Democratic Republic of the Congo (Kasai Block). Eclogites are generally only produced in subduction geodynamic setting. Moreover, we have identified the protolith of this eclogite, a gabbro, which formed 2216 ± 26 Ma ago in a narrow basin opening in a continental environment, and was then buried at 55 km in the mantle by subduction, before being exhumed to the surface during a complete Wilson cycle lasting about 130 Ma. This discovery evidences a modern-style plate tectonics operating since at least 2.2-2.1 Ga. This highlights the fundamental differences between the ancient Earth, without plate tectonics, and the modern Earth, as we know it today. The appearance of plate tectonics had important impacts on Life evolution on our planet, with an increasing supply of nutrients by erosion, increasing diversity of ecological niches and geographic isolation leading to increasing biodiversity, variable climatic conditions and oceanic circulation, as well as volcanic gases of different composition that may have influenced the composition of our atmosphere.
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- 2019
45. The potential science and engineering value of samples delivered to Earth by Mars sample return
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Beaty, D. W., Grady, Monica, McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., M. Hausrath, E., Herd, C. D. K., Horgan, B., Humanyun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Rucker, M. A., Schmitz, N., Schwenzer, S. P., Sephton, M. A., Shaheen, R., Sharp, Z. D., Schuster, D. L., Siljestrom, S., Smith, C. L., Spry, J. A., Steele, A., Swindle, T. D., ten Kate, I. L., Tosca, N. J., Usui, T., Van Kranendonk, M. J., Wadhwa, M., Weiss, B. P., Werner, S. C., Westall, F., Wheeler, R. M., Zipfel, J., Zorzano, M. P., Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), The Open University [Milton Keynes] (OU), School of Earth Sciences [Bristol], University of Bristol [Bristol], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Australian National University (ANU), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Planetary and Space Sciences [Milton Keynes] (PSS), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU)-Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Génotoxicologie et cycle cellulaire (GCC), Institut Curie [Paris]-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Planetary and Space Sciences Research Institute [Milton Keynes] (PSSRI), Centre for Earth, Planetary, Space and Astronomical Research [Milton Keynes] (CEPSAR), Université libre de Bruxelles (ULB), NASA Ames Research Center (ARC), Laboratoire d'étude de la pollution atmospherique, Institut National de la Recherche Agronomique (INRA), California Institute of Technology (CALTECH), ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), NASA Goddard Space Flight Center (GSFC), University of Glasgow, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), McDonnell Center for Space Sciences, Washington University in St Louis, Department of Geological Sciences [Providence], Brown University, Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, International Research School of Planetary Sciences [Pescara] (IRSPS), Università degli studi 'G. d'Annunzio' Chieti-Pescara [Chieti-Pescara] (Ud'A), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), DLR Institute of Aerospace Medicine, Deutsches Zentrum für Luft- und Raumfahrt [Köln] (DLR), Max Planck Institute for Nuclear Physics (MPIK), Max-Planck-Gesellschaft, SP Technical Research Institute of Sweden, Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science [Washington], Geological Survey of Western Australia, 100 Plain Street, East Perth, WA 6004, Australia, Department of Geology, The Field Museum, Massachusetts Institute of Technology (MIT), Centre de géochimie de la surface (CGS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Conception, Ingénierie et Développement de l'Aliment et du Médicament (CIDAM), Université d'Auvergne - Clermont-Ferrand I (UdA), Université Libre de Bruxelles [Bruxelles] (ULB), Division of Geological and Planetary Sciences [Pasadena], Department of Earth, Ocean and Atmospheric Science [Tallahassee] (EOAS), Florida State University [Tallahassee] (FSU), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), RISE Research Institutes of Sweden, Centre National de la Recherche Scientifique (CNRS)-Université Louis Pasteur - Strasbourg I-Institut national des sciences de l'Univers (INSU - CNRS), Department of Earth, Ocean and Atmospheric Science [Tallahassee] (FSU | EOAS), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Washington University in Saint Louis (WUSTL), Carnegie Institution for Science, Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), International Mars Exploration Working Group, Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), California Institute of Technology (CALTECH)-NASA, Agence Spatiale Européenne = European Space Agency (ESA), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Laboratoire de Physico-Chimie de l'Atmosphère (LPCA), and Université du Littoral Côte d'Opale (ULCO)-Centre National de la Recherche Scientifique (CNRS)
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Value (ethics) ,Engineering ,GeneralLiterature_INTRODUCTORYANDSURVEY ,Science and engineering ,Mars ,sample return ,010502 geochemistry & geophysics ,Exploration of Mars ,01 natural sciences ,Strahlenbiologie ,[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology ,0103 physical sciences ,Géographie physique ,GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries) ,010303 astronomy & astrophysics ,ComputingMilieux_MISCELLANEOUS ,0105 earth and related environmental sciences ,Martian ,Mars sample return ,business.industry ,Environmental resource management ,Mars Exploration Program ,Sciences de l'espace ,Geophysics ,IMOST ,[SDU]Sciences of the Universe [physics] ,Space and Planetary Science ,[SDU.OTHER]Sciences of the Universe [physics]/Other ,business - Abstract
Executive summary provided in lieu of abstract., SCOPUS: no.j, info:eu-repo/semantics/published
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- 2019
46. The potential science and engineering value of samples delivered to Earth by Mars sample return: International MSR Objectives and Samples Team (iMOST)
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Beaty, D. W., Grady, M. M., McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., Hausrath, E. M., Herd, C. D.K., Horgan, B., Humayun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Schmitz, N., ten Kate, I. L., and Petrology
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Geophysics ,Space and Planetary Science - Abstract
Return of samples from the surface of Mars has been a goal of the international Mars science community for many years. Affirmation by NASA and ESA of the importance of Mars exploration led the agencies to establish the international MSR Objectives and Samples Team (iMOST). The purpose of the team is to re-evaluate and update the sample-related science and engineering objectives of a Mars Sample Return (MSR) campaign. The iMOST team has also undertaken to define the measurements and the types of samples that can best address the objectives. Seven objectives have been defined for MSR, traceable through two decades of previously published international priorities. The first two objectives are further divided into sub-objectives. Within the main part of the report, the importance to science and/or engineering of each objective is described, critical measurements that would address the objectives are specified, and the kinds of samples that would be most likely to carry key information are identified. These seven objectives provide a framework for demonstrating how the first set of returned Martian samples would impact future Martian science and exploration. They also have implications for how analogous investigations might be conducted for samples returned by future missions from other solar system bodies, especially those that may harbor biologically relevant or sensitive material, such as Ocean Worlds (Europa, Enceladus, Titan) and others. Summary of Objectives and Sub-Objectives for MSR Identified by iMOST: Objective 1 Interpret the primary geologic processes and history that formed the Martian geologic record, with an emphasis on the role of water. Intent To investigate the geologic environment(s) represented at the Mars 2020 landing site, provide definitive geologic context for collected samples, and detail any characteristics that might relate to past biologic processesThis objective is divided into five sub-objectives that would apply at different landing sites. 1.1 Characterize the essential stratigraphic, sedimentologic, and facies variations of a sequence of Martian sedimentary rocks. Intent To understand the preserved Martian sedimentary record. Samples A suite of sedimentary rocks that span the range of variation. Importance Basic inputs into the history of water, climate change, and the possibility of life 1.2 Understand an ancient Martian hydrothermal system through study of its mineralization products and morphological expression. Intent To evaluate at least one potentially life-bearing “habitable” environment Samples A suite of rocks formed and/or altered by hydrothermal fluids. Importance Identification of a potentially habitable geochemical environment with high preservation potential. 1.3 Understand the rocks and minerals representative of a deep subsurface groundwater environment. Intent To evaluate definitively the role of water in the subsurface. Samples Suites of rocks/veins representing water/rock interaction in the subsurface. Importance May constitute the longest-lived habitable environments and a key to the hydrologic cycle. 1.4 Understand water/rock/atmosphere interactions at the Martian surface and how they have changed with time. Intent To constrain time-variable factors necessary to preserve records of microbial life. Samples Regolith, paleosols, and evaporites. Importance Subaerial near-surface processes could support and preserve microbial life. 1.5 Determine the petrogenesis of Martian igneous rocks in time and space. Intent To provide definitive characterization of igneous rocks on Mars. Samples Diverse suites of ancient igneous rocks. Importance Thermochemical record of the planet and nature of the interior. Objective 2 Assess and interpret the potential biological history of Mars, including assaying returned samples for the evidence of life. Intent To investigate the nature and extent of Martian habitability, the conditions and processes that supported or challenged life, how different environments might have influenced the preservation of biosignatures and created nonbiological “mimics,” and to look for biosignatures of past or present life.This objective has three sub-objectives: 2.1 Assess and characterize carbon, including possible organic and pre-biotic chemistry. Samples All samples collected as part of Objective 1. Importance Any biologic molecular scaffolding on Mars would likely be carbon-based. 2.2 Assay for the presence of biosignatures of past life at sites that hosted habitable environments and could have preserved any biosignatures. Samples All samples collected as part of Objective 1. Importance Provides the means of discovering ancient life. 2.3 Assess the possibility that any life forms detected are alive, or were recently alive. Samples All samples collected as part of Objective 1. Importance Planetary protection, and arguably the most important scientific discovery possible. Objective 3 Quantitatively determine the evolutionary timeline of Mars. Intent To provide a radioisotope-based time scale for major events, including magmatic, tectonic, fluvial, and impact events, and the formation of major sedimentary deposits and geomorphological features. Samples Ancient igneous rocks that bound critical stratigraphic intervals or correlate with crater-dated surfaces. Importance Quantification of Martian geologic history. Objective 4 Constrain the inventory of Martian volatiles as a function of geologic time and determine the ways in which these volatiles have interacted with Mars as a geologic system. Intent To recognize and quantify the major roles that volatiles (in the atmosphere and in the hydrosphere) play in Martian geologic and possibly biologic evolution. Samples Current atmospheric gas, ancient atmospheric gas trapped in older rocks, and minerals that equilibrated with the ancient atmosphere. Importance Key to understanding climate and environmental evolution. Objective 5 Reconstruct the processes that have affected the origin and modification of the interior, including the crust, mantle, core and the evolution of the Martian dynamo. Intent To quantify processes that have shaped the planet's crust and underlying structure, including planetary differentiation, core segregation and state of the magnetic dynamo, and cratering. Samples Igneous, potentially magnetized rocks (both igneous and sedimentary) and impact-generated samples. Importance Elucidate fundamental processes for comparative planetology. Objective 6 Understand and quantify the potential Martian environmental hazards to future human exploration and the terrestrial biosphere. Intent To define and mitigate an array of health risks related to the Martian environment associated with the potential future human exploration of Mars. Samples Fine-grained dust and regolith samples. Importance Key input to planetary protection planning and astronaut health. Objective 7 Evaluate the type and distribution of in-situ resources to support potential future Mars exploration. Intent To quantify the potential for obtaining Martian resources, including use of Martian materials as a source of water for human consumption, fuel production, building fabrication, and agriculture. Samples Regolith. Importance Production of simulants that will facilitate long-term human presence on Mars. Summary of iMOST Findings: Several specific findings were identified during the iMOST study. While they are not explicit recommendations, we suggest that they should serve as guidelines for future decision making regarding planning of potential future MSR missions. The samples to be collected by the Mars 2020 (M-2020) rover will be of sufficient size and quality to address and solve a wide variety of scientific questions. Samples, by definition, are a statistical representation of a larger entity. Our ability to interpret the source geologic units and processes by studying sample sub sets is highly dependent on the quality of the sample context. In the case of the M-2020 samples, the context is expected to be excellent, and at multiple scales. (A) Regional and planetary context will be established by the on-going work of the multi-agency fleet of Mars orbiters. (B) Local context will be established at field area- to outcrop- to hand sample- to hand lens scale using the instruments carried by M-2020. A significant fraction of the value of the MSR sample collection would come from its organization into sample suites, which are small groupings of samples designed to represent key aspects of geologic or geochemical variation. If the Mars 2020 rover acquires a scientifically well-chosen set of samples, with sufficient geological diversity, and if those samples were returned to Earth, then major progress can be expected on all seven of the objectives proposed in this study, regardless of the final choice of landing site. The specifics of which parts of Objective 1 could be achieved would be different at each of the final three candidate landing sites, but some combination of critically important progress could be made at any of them. An aspect of the search for evidence of life is that we do not know in advance how evidence for Martian life would be preserved in the geologic record. In order for the returned samples to be most useful for both understanding geologic processes (Objective 1) and the search for life (Objective 2), the sample collection should contain BOTH typical and unusual samples from the rock units explored. This consideration should be incorporated into sample selection and the design of the suites. The retrieval missions of a MSR campaign should (1) minimize stray magnetic fields to which the samples would be exposed and carry a magnetic witness plate to record exposure, (2) collect and return atmospheric gas sample(s), and (3) collect additional dust and/or regolith sample mass if possible.
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- 2019
47. The potential science and engineering value of samples delivered to Earth by Mars sample return
- Author
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International MSR Objectives and Samples Team (iMOST), Beaty, DW, Grady, MM, McSween, HY, Sefton-Nash, E, Carrier, BL, Altieri, F, Amelin, Y, Ammannito, E, Anand, M, Benning, LG, Bishop, JL, Borg, LE, Boucher, D, Brucato, JR, Busemann, H, Campbell, KA, Czaja, AD, Debaille, V, Des Marais, DJ, Dixon, M, Ehlmann, BL, Farmer, JD, Fernandez-Remolar, DC, Filiberto, J, Fogarty, J, Glavin, DP, Goreva, YS, Hallis, LJ, Harrington, AD, Hausrath, EM, Herd, CDK, Horgan, B, Humanyun, M, Kleine, T, Kleinhenz, J, Mackelprang, R, Mangold, N, Mayhew, LE, McCoy, JT, McCubbin, FM, McLennan, SM, Moser, DE, Moynier, F, Mustard, JF, Niles, PB, Ori, GG, Raulin, F, Rettberg, P, Rucker, MA, Schmitz, N, Schwenzer, SP, Sephton, MA, Shaheen, R, Sharp, ZD, Schuster, DL, Siljestrom, S, Smith, CL, Spry, JA, Steele, A, Swindle, TD, ten Kate, IL, Tosca, NJ, Usui, T, Van Kranendonk, MJ, Wadhwa, M, Weiss, BP, Werner, SC, Westall, F, Wheeler, RM, Zipfel, J, and Zorzano, MP
- Published
- 2019
48. Achondritic cosmic spherules from the Sor Rondane Mountains , East Antarctica: Probing the asteroid belt beyond the meteorite inventory
- Author
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Soens, B., Villeneuve, J., Ginneken, M., Debaille, V., Frank Vanhaecke, Claeys, Ph, Goderis, S., Faculty of Sciences and Bioengineering Sciences, Chemistry, Analytical, Environmental & Geo-Chemistry, and Earth System Sciences
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- 2019
49. Microtektites from the Sor Rondane Mountains, East Antarctica: Towards an extension of the Australasian strewn field?
- Author
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Soens, B., Ginneken, M., Debaille, V., Frank Vanhaecke, Claeys, Ph, Goderis, S., Faculteit van de Wetenschappen, Scheikunde, Analytisch- Milieu- & Geo-Chemie, and Wetenschappen van het Systeem Aarde
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- 2019
50. Duration of a Magma Ocean and Subsequent Mantle Overturn in Mars: Evidence from Nakhlites
- Author
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Debaille, V, Brandon, A. D, Yin, Q.-Z, and Jacobsen, B
- Subjects
Lunar And Planetary Science And Exploration - Abstract
It is now generally accepted that the heat produced by accretion, short-lived radioactive elements such as Al-26, and gravitational energy from core formation was sufficient to at least partially melt the silicate portions of terrestrial planets resulting in a global-scale magma ocean. More particularly, in Mars, the geochemical signatures displayed by shergottites, are likely inherited from the crystallization of this magma ocean. Using the short-lived chronometer Sm-146 - Nd-142 (t(sup 1/2) = 103 Myr), the duration of the Martian magma ocean (MMO) has been evaluated to being less than 40 Myr, while recent and more precise ND-142/ND-144 data were used to evaluate the longevity of the MMO to approximately 100 Myr after the solar system formation. In addition, it has been proposed that the end of the crystallization of the MMO may have triggered a mantle overturn, as a result of a density gradient in the cumulate layers crystallized at different levels. Dating the mantle overturn could hence provide additional constraint on the duration of the MMO. Among SNC meteorites, nakhlites are characterized by high epsilon W-182 of approximately +3 and an epsilon Nd-142 similar to depleted shergottites of +0.6-0.9. It has hence been proposed that the source of nakhlites was established very early in Mars history (approximately 8-10 Myr). However, the times recorded in HF-182-W-182 isotope system, i.e. when 182Hf became effectively extinct (approximately 50 Myr after solar system formation) are less than closure times recorded in the Sm-146-Nd-142 isotope system (with a full coverage of approximately 500 Myr after solar system formation). This could result in decoupling between the present-day measured epsilon W-182 and epsilon Nd-142 as the SM-146 may have recorded later differentiation events in epsilon ND-142 not observed in epsilon W-182 values. With these potential complexities in short-lived chronological data for SNC's in mind, new Hf-176/Hf-177, Nd-143/Nd-144 and Nd-142/Nd-144 were obtained for three nakhlites (Nakhla, MIL03346 and Yamato000593). These new data are combined with previous epsilon W-182 data, to investigate potential discrepancies between the Hf-182-W-182 and Sm-146-Nd-142 systematics, and the relationship between the source of nakhlites and a crystallizing magma ocean
- Published
- 2008
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