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148 results on '"Bulk composition"'

51. NEUTRON RESONANCE CAPTURE ANALYSIS OF SOME GENUINE AND FAKE ETRUSCAN COPPER ALLOY STATUETTES.

Author

Postma, H., Schillebeeckx, P., and Halbertsma, R. B.

Subjects
*NEUTRON resonance, *NUCLEAR magnetic resonance, *FIGURINES, *CHEMICAL structure, *ELECTRONS, *ETRUSCAN antiquities
Abstract

The probability of nuclei capturing neutrons reveals sharp peaks, so-called‘resonances’, which occur at neutron energies that are specific for each element. These resonances are very suitable for analysing the elemental composition of objects. They are the basis of a new analytical method,‘neutron resonance capture analysis’ (NRCA). This is a fully non-destructive method, which is applicable to almost all stable isotopes, determines the bulk elemental composition, does not require any sample preparation and results in a negligible residual activity. Recently, NRCA has been applied in a study of a series of bronze statuettes, obtained from the National Museum of Antiquity in Leiden (NL). [ABSTRACT FROM AUTHOR]

Published
2004
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52. A quantitative relationship between the affinity of component to adsorbent in liquid–solid system, βa, and composition of bulk solution

Author

Wang, Yan and Geng, Xindu

Subjects
*STOICHIOMETRY, *ADSORPTION (Chemistry), *SURFACE chemistry, *LIQUID chromatography
Abstract

Based on the stoichiometric displacement theory for adsorption (SDT-A) of solute, an equation expressing the linear relationship between the affinity of component to adsorbent, βa, and the logarithm of the molar concentration of solvent in the bulk solution, log aD, was derived. The derived equation was tested by the derivatives of benzene under different methanol concentrations by frontal analysis (FA) of reversed-phase liquid chromatography (RPLC). A satisfactory result was obtained. Moreover, the n and q terms’ values (moles of the solvent separately released from the adsorbent and solute, respectively, as 1 mol of solute is adsorbed) which are summed in the stoichiometric parameter Z (Z=n+q), are very useful but hard to obtain only by RPLC alone. However, both were obtained from this relationship and tested with the presented method. It was also examined by the combination of the SDT-A with stoichiometric displacement theory for retention (SDT-R). Both n and q were further validated to follow the homologue rule. More solvent was released by adsorbent than by solute (n>q) and the fraction of solvent released by the adsorbent increased when the group attached to benzene was nonpolar. [Copyright &y& Elsevier]

Published
2003
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53. On the principal building blocks of Mars and Earth

Author

Amir Khan and Christian Liebske

Subjects
Solar System, Planetesimal, 010504 meteorology & atmospheric sciences, Astronomy and Astrophysics, Mars Exploration Program, Mars, Earth, Oxygen isotopes, Nucleosynthetic isotopes, Chondrites, Bulk composition, 01 natural sciences, Mantle (geology), Physics::Geophysics, Astrobiology, Space and Planetary Science, Chondrite, Planet, Physics::Space Physics, 0103 physical sciences, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Achondrite, Geology, 0105 earth and related environmental sciences
Abstract

The terrestrial planets are believed to have been formed from primitive material sampling a broad region of the inner solar system. Several meteoritic mixing models attempting to reconcile isotopic characteristics of Mars and Earth have been proposed, but, because of the inherent non-uniqueness of these solutions, additional independent observations are required to resolve the question of the primary building blocks of the terrestrial planets. Here, we consider existing isotopic measurements of Δ ′ 17 O, ϵ48Ca, ϵ50Ti, ϵ54Cr, ϵ62Ni, and ϵ84Sr for primitive chondrites and differentiated achondrites and mix these stochastically to reproduce the isotopic signatures of Mars and Earth. For both planets we observe ∼ 105 unique mixing solutions out of 108 random meteoritic mixtures, which are categorised into distinct clusters of mixtures using principal component analysis. The large number of solutions implies that isotopic data alone are insufficient to resolve the building blocks of the terrestrial planets. To further discriminate between isotopically valid mixtures, each mixture is converted into a core and mantle component via mass balance for which geophysical properties are computed and compared to observations. For Mars, the geophysical parameters include mean density, mean moment of inertia, and tidal response, whereas for Earth upper mantle Mg/(Mg+Fe) ratio and core size are employed. The results show that Mars requires an oxidised, FeO-rich differentiated object next to chondritic material as main building blocks. In contrast, Earth's origin remains enigmatic. From a redox perspective, it appears inescapable that enstatite chondrite-like matter constitutes a dominant proportion of the building blocks from which Earth is made. The apparent need for compositionally distinct building blocks for Mars and Earth suggests that dissimilar planetesimal reservoirs were maintained in the inner Solar System during accretion.

Published
2019

54. Heterogeneous oxidation of multi-component aqueous organic aerosols: The effect of transport phenomena and reaction compartment on reaction kinetics.

Author

Masaya, Tadini wenyika

Subjects
Aqueous organic aerosols, molecular dynamics simulation, reactive uptake coefficient, interfacial reaction, solvation, reaction Kinetics, partitioning, rate coefficients, Bulk Composition, molecule orientation, Analytical Chemistry, Computational Chemistry, Physical Chemistry
Abstract

The surface-bulk partitioning of small organic molecules in aqueous droplets was investigated using molecular dynamics. The air-particle interface was modeled using a 80-Å cubic water box containing series of organic molecules and surrounded by gaseous OH radicals. The properties of the organic solutes within the interface and the water-bulk were examined at a molecular-level using density profiles and radial pair distribution functions. Molecules containing only polar functional groups such as urea and glucose are found predominantly in the water bulk, forming an exclusion layer near the water surface. Substitution of a single polar group by an alkyl group in sugars and amides leads to the migration of the molecule toward the interface. Within the first 2 nm from the water surface, surface-active solutes lose their rotational freedom and adopt a preferred orientation with the alkyl group pointing toward the surface. The different packing within the interface leads to different solvation shell structures and enhanced interaction between the organic molecules and absorbed OH radicals. The simulations provide quantitative information about the dimension, composition, and organization of the air-water interface as well as about the non-reactive interaction of the OH radicals with the organic solutes. It reveals that the enhanced reactivity of surface-active molecules is due to increased concentrations, preferred orientation, and decreased solvation near the air-water surface. The results are important to explain how heterogeneous oxidation mechanisms and kinetics within interfaces may differ from those of the bulk. An atmospheric pressure flow-tube reactor coupled with offline GC-MS analysis techniques was used to determine the kinetics of the OH-initiated oxidation of equimolar aqueous organic aerosol. Saccharides (glucose and MGP) and amides (propionamide, urea, and acetamide), were chosen as model molecules because of their partitioning properties, availability in the atmosphere, and the important role they play in atmospheric chemistry. The decay rates of the solutes (saccharides and amides) were determined by measuring the loss in signal of solutes in the particle phase as a function of OH exposure (time-integrated total concentration of OH radical). The reactivity of MGP towards OH radicals was shown to be higher in the presence of urea (a surface in-active molecule) than when in the presence of propionamide (a surface in-active molecule). The decreases in MGP reactivity was shown by the change in rate coefficients from 1.2(±0.1) x 10-11 cm-3 s-1 in the urea-MGP particles to 4.7(±0.3) x 10-12 cm-3 s-1 in the propionamide-MGP particles. These findings highlight the importance of surface interactions over bulk interactions in determining the reaction rate of reactive species in aqueous aerosols. The change in particle size with change in chemical composition was also demonstrated.

Published
2022

55. SEIS: Insight’s Seismic Experiment for Internal Structure of Mars

Author

L. Perrin, C. Bonjour, N. Toulemont, Jean-Luc Berenguer, G. Perez, James Wookey, A. G. Mukherjee, Hallie Gengl, Edward A. Miller, Delphine Faye, Antoine Mocquet, J. Sicre, B. Vella, D. Dilhan, C. Larigauderie, John C. Bousman, M. Nonon, Y. Bennour, Véronique Dehant, Jeffrey W. Umland, T. Nebut, D. Hernandez, M. Eberhardt, Vincent Conejero, Rudolf Widmer-Schnidrig, Philippe Lognonné, G. de los Santos, S. A. D’Agostino, Savas Ceylan, Justin N. Maki, G. Aveni, P. Revuz, S. de Raucourt, C. Aicardi, Clément Perrin, A. K. Delahunty, Constanza Pardo, Domenico Giardini, L. Pou, Robert J. Calvet, D. Savoie, O. Robert, V. Gharakanian, S. Ben Charef, Constantinos Charalambous, Kerry Klein, S. M. Madzunkov, J. M. Desmarres, Sue Smrekar, S. B. Calcutt, F. Grinblat, Nicholas A Teanby, I. M. Standley, Naomi Murdoch, Brigitte Knapmeyer-Endrun, M. Deleuze, C. Doucet, William T. Pike, Tom L. Hoffman, F. Mialhe, Cecily M. Sunday, J. Paredes-Garcia, Matthew P. Golombek, P. Bhandari, Huafeng Liu, B. Pouilloux, E. Blanco, Gabriel Pont, Simon Stähler, M. E. Johnson, Nicolas Verdier, L. Luno, Ned W. Ferraro, R. Perez, Mélanie Drilleau, F. Ijpelaan, B. Lecomte, M. van Driel, A. Sauron, I. Estève, Mark P. Panning, David Mimoun, P. A. Dandonneau, B. Kenda, T. Gabsi, W. Raff, P. Boutte, T. Warren, Joan Ervin, Fabian Euchner, S. Tillier, K. J. Hurst, Stephen Larson, Davor Mance, Mark A. Wieczorek, J. A. Rodriguez-Manfredi, Justin Lin, Jaime Singer, M. Monecke, Robert W. Denise, E.-P. Miettinen, Maren Böse, E. Locatelli, I. Savin de Larclause, J. Gagnepain-Beyneix, L. Khachikyan, Philippe Laudet, T. Carlier, Alexander E. Stott, Neil Bowles, Brian Bone, C. Imbert, Sharon Kedar, A. Rosak, Fred Calef, O. Pot, O. M. Avalos, P. Labrot, Jeroen Tromp, Lucile Fayon, C. Moreau, J. Baroukh, William B. Banerdt, M. Bierwirth, Ranah Irshad, M. André, Christopher T. Russell, S. L. Marshall, M. Parise, J.-R. Meyer, P. Pasquier, N. Faye-Refalo, Ingrid Daubar, M. A. Balzer, R. Gonzalez, M. Hetzel, K. Brethomé, Y. Pahn, Raphaël F. Garcia, J. tenPierick, U. R. Christensen, Farah Alibay, Renee Weber, Robert G. Deen, Eléonore Stutzmann, J. Temple, Don Banfield, A. Bouisset, D. B. Klein, A. Borrien, Ashitey Trebi-Ollennu, R. Llorca-Cejudo, L. J. Facto, J. M. Mouret, Alexis Paillet, Peter Zweifel, P. Bruneau, Catherine L. Johnson, C. Brysbaert, J. E. Feldman, A. Kramer, Luigi Ferraioli, Jane Hurley, Taichi Kawamura, Nicholas Onufer, W. Kühne, Eric Beucler, Amir Khan, M. Sodki, L. Kerjean, A. Sylvestre-Baron, C. Desfoux, C. Yana, John Clinton, J. R. Willis, Juan Villalvazo, Pierre Delage, Mihail P. Petkov, M. C. Wallace, T. Camus, Ioannis G. Mikellides, Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Institute of Geophysics [ETH Zürich], Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Department of Mechanical Engineering [Imperial College London], Imperial College London, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Centre National d'Études Spatiales [Toulouse] (CNES), Geological Institute (ETHZ), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Oxford, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NASA Marshall Space Flight Center (MSFC), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Mecanique des Fluides et d'Acoustique (LMFA), École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), Advanced Technology and Research, Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Clarendon Laboratory [Oxford], Huazhong University of Science and Technology [Wuhan] (HUST), Kinemetrics, Cornell University [New York], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of California [Los Angeles] (UCLA), University of California (UC), Institut of GeophysicsETHZ, Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Swiss Seismological Service, Royal Observatory of Belgium [Brussels] (ROB), Géotechnique (cermes), Laboratoire Navier (navier umr 8205), Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of British Columbia (UBC), Planetary Science Institute [Tucson] (PSI), Laboratoire national de métrologie et d'essais - Systèmes de Référence Temps-Espace (LNE - SYRTE), Systèmes de Référence Temps Espace (SYRTE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), University of Bristol [Bristol], Department of Geosciences [Princeton], Princeton University, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universität Stuttgart [Stuttgart], School of Earth Sciences [Bristol], Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Max-Planck-Institut für Sonnensystemforschung (MPS), University of Oxford [Oxford], Max Planck Institute for Solar System Research (MPS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California, INSTITUT OF GEOPHYSICS ETHZ, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Karlsruhe Institute of Technology and Stuttgart University, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), California Institute of Technology (CALTECH)-NASA, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Département Electronique, Optronique et Signal (DEOS), Department of Earth Sciences [ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), 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 Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Cornell University, Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), Royal Observatory of Belgium [Brussels], PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), School of Earth Sciences University of Bristol, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Seismometer, DISSIPATIVE FACTOR, 010504 meteorology & atmospheric sciences, FREE OSCILLATIONS, BULK COMPOSITION, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Astronomy & Astrophysics, 01 natural sciences, Transfer function, Article, NETWORK SCIENCE, Autre, 0103 physical sciences, 0201 Astronomical and Space Sciences, INTERIOR STRUCTURE, ddc:530, Ground segment, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, InSight, Data processing, Science & Technology, Physics, Bandwidth (signal processing), Mars seismology, Astronomy and Astrophysics, Moment magnitude scale, SINGLE-STATION, THERMAL EVOLUTION, Mars Exploration Program, Geodesy, Space and Planetary Science, Physical Sciences, WAVE PROPAGATION, ELYSIUM PLANITIA, [SDU.OTHER]Sciences of the Universe [physics]/Other, Robotic arm, SEIS, Geology, METEORITE IMPACTS
Abstract

By the end of 2018, 42 years after the landing of the two Viking seismometers on Mars, InSight will deploy onto Mars’ surface the SEIS (Seismic Experiment for Internal Structure) instrument; a six-axes seismometer equipped with both a long-period three-axes Very Broad Band (VBB) instrument and a three-axes short-period (SP) instrument. These six sensors will cover a broad range of the seismic bandwidth, from 0.01 Hz to 50 Hz, with possible extension to longer periods. Data will be transmitted in the form of three continuous VBB components at 2 sample per second (sps), an estimation of the short period energy content from the SP at 1 sps and a continuous compound VBB/SP vertical axis at 10 sps. The continuous streams will be augmented by requested event data with sample rates from 20 to 100 sps. SEIS will improve upon the existing resolution of Viking’s Mars seismic monitoring by a factor of ∼2500 at 1 Hz and ∼200000 at 0.1 Hz. An additional major improvement is that, contrary to Viking, the seismometers will be deployed via a robotic arm directly onto Mars’ surface and will be protected against temperature and wind by highly efficient thermal and wind shielding. Based on existing knowledge of Mars, it is reasonable to infer a moment magnitude detection threshold of Mw∼3 at 40∘ epicentral distance and a potential to detect several tens of quakes and about five impacts per year. In this paper, we first describe the science goals of the experiment and the rationale used to define its requirements. We then provide a detailed description of the hardware, from the sensors to the deployment system and associated performance, including transfer functions of the seismic sensors and temperature sensors. We conclude by describing the experiment ground segment, including data processing services, outreach and education networks and provide a description of the format to be used for future data distribution., Space Science Reviews, 215 (1), ISSN:1572-9672, ISSN:0038-6308

Published
2019
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56. Bulk and surface composition, amorphous structure, and thermocrystallization of electrodeposited alloys of tungsten with iron, nickel, and cobalt.

Author

Donten, Mikołaj

Abstract

It has been shown for iron-group alloys of tungsten, using ESCA spectroscopy of samples sputtered with argon ions and SEM/EDS analysis, that no oxygen is present in the alloy bulk. A very weak internal organization in the alloys, which follows from low and wide diffractograms usually obtained for electrodeposited layers, is thought to be a heavily distorted structure of the major metal component of the alloy. Thermal crystallization of thin layers of the amorphous tungsten alloys does not lead to formation of well-known intermetallic crystal structures. [ABSTRACT FROM AUTHOR]

Published
1999
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58. Tidal response of rocky exoplanets

Author

Sohl, F., Csizmadia, S., Dubrovinsky, L., Dubrovinskaia, N., Hellard, H., Padovan, S., and Wagner, F.W.

Subjects
transiting exoplanets, planets, bulk composition, mineral phase transitions, interior structure, static tides, photometric light curves
Published
2018

59. Crystallization of the lunar magma ocean and the primordial mantle-crust differentiation of the Moon

Author

Timothy L. Grove, Francois Holtz, Bernard Charlier, and Olivier Namur

Subjects
Geochemistry & Geophysics, Experimental petrology, 010504 meteorology & atmospheric sciences, GIANT IMPACT, BULK COMPOSITION, INTERNAL STRUCTURE, 010502 geochemistry & geophysics, Anorthosite, 01 natural sciences, Mantle (geology), law.invention, chemistry.chemical_compound, PLAGIOCLASE-FLOTATION, CUMULATE OVERTURN, Geochemistry and Petrology, law, Graphite, Crystallization, Petrology, 0105 earth and related environmental sciences, LAPAZ ICEFIELD 02205, FRACTIONAL CRYSTALLIZATION, Science & Technology, Piston cylinder, Crust, Liquid line of descent, Silicate, FERROAN ANORTHOSITES, TERRESTRIAL PLANETS, chemistry, Lunar magma ocean, Physical Sciences, CHEMICAL-MODEL, Lunar crust, Mantle, Phase equilibria, Geology
Abstract

© 2018 Elsevier Ltd We present crystallization experiments on silicate melt compositions related to the lunar magma ocean (LMO) and its evolution with cooling. Our approach aims at constraining the primordial internal differentiation of the Moon into mantle and crust. We used graphite capsules in piston cylinder (1.35–0.80 GPa) and internally-heated pressure vessels (

Published
2018

60. Magnitude Scales for Marsquakes

Author

Domenico Giardini, Maren Böse, Fabian Euchner, John Clinton, Amir Khan, Philippe Lognonné, Martin van Driel, Simon Stähler, Savas Ceylan, William B. Banerdt, Swiss Fed Inst Technol, Swiss Seismol Serv, Sonneggstr 5, CH-8092 Zurich, Switzerland, Swiss Fed Inst Technol, Inst Geophys, Sonneggstr 5, CH-8092 Zurich, Switzerland, Swiss Fed Inst Technol, Swiss Seismol Serv SED, Sonneggstr 5, CH-8092 Zurich, Switzerland, Institut de Physique du Globe de Paris (IPGP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), CALTECH, Jet Prop Lab, M-S 321-B60,4800 Oak Grove Dr, Pasadena, CA 91109 USA, and Swiss National Science Foundation-Agence Nationale Recherche (SNF-ANR) 157133 Swiss National Supercomputing Center (CSCS) sm682

Subjects
010504 meteorology & atmospheric sciences, MODELS, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Magnitude (mathematics), BULK COMPOSITION, MARS SEISMICITY, 010502 geochemistry & geophysics, 01 natural sciences, NOISE, Background noise, Geochemistry and Petrology, EARTH, LOCATION, ENERGY-RELEASE, Seismogram, 0105 earth and related environmental sciences, SEISMOGRAMS, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Attenuation, SINGLE-STATION, Mars Exploration Program, INSIGHT MISSION, Geodesy, Geophysics, Amplitude, 13. Climate action, [SDU]Sciences of the Universe [physics], Seismic moment, Noise (radio), Geology
Abstract

International audience; In anticipation of the upcoming 2018 InSight (Interior exploration using Seismic Investigations, Geodesy and Heat Transport) Discovery mission to Mars, we calibrate magnitude scales for marsquakes that incorporate state-of-the-art knowledge on Mars interior structure and the expected ambient and instrumental noise. We regress magnitude determinations of 2600 randomly distributed marsquakes, simulated with a spectral element method for 13 published 1D structural models of Mars' interior. The continuous seismic data from InSight will be returned at 2 samples per second. To account for this limited bandwidth as well as for the expected noise conditions on Mars, we define and calibrate six magnitude scales: (1) local Mars magnitude M-L(Ma) at a period of 3 s for marsquakes at distances of up to 10 degrees; (2) P-wave magnitude m(b)(Ma); (3) S-wave magnitude m(bS)(Ma) each defined at a period of 3 s and calibrated for distances from 5 degrees to 100 degrees; (4) surface-wave magnitude M-s(Ma) defined at a period of 20 s, as well as (5) moment magnitudes M-FB(Ma); and (6) M-F(Ma) computed from the low-frequency (10-100 s) plateau of the displacement spectrum for either body waves or body and surface waves, respectively; we calibrate scales (4)-(6) for distances from 5 degrees to 180 degrees. We regress stable calibrations of the six scales with respect to the seismic moment magnitude at M-w 5.5 by correcting filtered phase amplitudes for attenuation with distance and source depth. Expected errors in epicentral distance and in source depth (25% and 20 km, respectively) translate into magnitude errors of 0.1-0.3 units. We validate our magnitude relations with an independent test dataset of 2600 synthetic marsquakes (1.0 15 degrees are expected to be hidden in the Mars background noise and will likely not be detectable.

Published
2018
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61. On the Detectability and Use of Normal Modes for Determining Interior Structure of Mars

Author

Philippe Lognonné, Domenico Giardini, Simon Stähler, Mélanie Drilleau, Tamara Gudkova, Felix Bissig, V. N. Zharkov, Amir Khan, Ana-Catalina Plesa, Martin van Driel, William B. Banerdt, Mark P. Panning, Swiss Fed Inst Technol, Inst Geophys, Sonneggstr 5, CH-8092 Zurich, Switzerland, Institute of Geophysics [ETH Zürich], Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Schmidt Institute of Physics of the Earth of the Russian Academy of Sciences (IPE RAS), Bolshaya Gruzinskaya Str. 10-1, 123242 Moscow, Russia, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA, and Swiss National Science Foundation (SNSF) 200021_172508 Swiss National Supercomputing Centre (CSCS) s830

Subjects
Mars, Seismology, Normal modes, Interior structure, Inverse problems, 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], BULK COMPOSITION, Geometry, WAVE-FORMS, 010502 geochemistry & geophysics, 01 natural sciences, Spectral line, Inverse problems KeyWords Plus:FREE OSCILLATIONS, Normal mode, Interior Structure, LUNAR INTERIOR, Range (statistics), EARTH, MARTIAN SEISMICITY, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, TORSIONAL OSCILLATIONS, Series (mathematics), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Autocorrelation, Astronomy and Astrophysics, SINGLE-STATION, Mars Exploration Program, INSIGHT MISSION, MANTLE MINERALS, Data set, Normal Modes, Space and Planetary Science, Surface wave, [SDU]Sciences of the Universe [physics], Author Keywords:Mars
Abstract

The InSight mission to Mars is well underway and will be the first mission to acquire seismic data from a planet other than Earth. In order to maximise the science return of the InSight data, a multifaceted approach will be needed that seeks to investigate the seismic data from a series of different frequency windows, including body waves, surface waves, and normal modes. Here, we present a methodology based on globally-averaged models that employs the long-period information encoded in the seismic data by looking for fundamental-mode spheroidal oscillations. From a preliminary analysis of the expected signal-to-noise ratio, we find that normal modes should be detectable during nighttime in the frequency range 5–15 mHz. For improved picking of (fundamental) normal modes, we show first that those are equally spaced between 5–15 mHz and then show how this spectral spacing, obtained through autocorrelation of the Fourier-transformed time series can be further employed to select normal mode peaks more consistently. Based on this set of normal-mode spectral frequencies, we proceed to show how this data set can be inverted for globally-averaged models of interior structure (to a depth of $\sim 250~\mbox{km}$ ), while simultaneously using the resultant synthetically-approximated normal mode peaks to verify the initial peak selection. This procedure can be applied iteratively to produce a “cleaned-up” set of spectral peaks that are ultimately inverted for a “final” interior-structure model. To investigate the effect of three-dimensional (3D) structure on normal mode spectra, we constructed a 3D model of Mars that includes variations in surface and Moho topography and lateral variations in mantle structure and employed this model to compute full 3D waveforms. The resultant time series are converted to spectra and the inter-station variation hereof is compared to the variation in spectra computed using different 1D models. The comparison shows that 3D effects are less significant than the variation incurred by the difference in radial models, which suggests that our 1D approach represents an adequate approximation of the global average structure of Mars.

Published
2018
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78. Leucite-Albite Incompatibility

Author

Gupta, Alok K., Yagi, Kenzo, Wyllie, P. J., editor, El Goresy, A., editor, von Engelhardt, W., editor, Hahn, T., editor, Gupta, Alok K., and Yagi, Kenzo

Published
1980
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91. Bulk Composition

Author

Wasson, John T., Wyllie, P. J., editor, von Engelhardt, W., editor, Hahn, T., editor, and Wasson, John T.

Published
1974
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98. Influence of rock-forming and catalytic additives on transformation of highly viscous heavy oil

Author

Petrov S., Ibragimova D., Abdelsalam Y., and Kayukova G.

Subjects
molecular weight distribution of n-alkanes, bulk composition, carbonate additive, heavy oil, kaolin, aquathermolysis
Abstract

© 2016 Pleiades Publishing, Ltd. The influence of the rock-forming additives kaolin and alumina in the presence of nickel compounds on the thermal catalytic conversion of heavy oil at a temperature of 360°C in a reducing atmosphere at different pressures in the system has been revealed. The effect of poly-α-olefins as a hydrogen donor has been examined. It has been found that there are predominant degradation reactions of the resinous components, aliphatic substituents in asphaltenes, and branched aliphatic structures accompanied by redistribution of n-alkanes toward homologues with a lower molecular weight, resulting in reduction in the viscosity of heavy oil. Conducting the process in the presence of Al2O3, Ni, and poly-α-olefins at a pressure of 8 MPa increases the quantity of light fractions of the oil and facilitates the degradation of asphaltenes. A decrease of pressure in the experiment on the oil with kaolin in a reducing atmosphere leads to a decrease in aromaticity of the final product and an increase in the yield of lube oil hydrocarbon and low-boiling fractions.

Published
2016

99. Analytical characterisation of nanoscale zero-valent iron: A methodological review

Author

Ryo Sekine, Enzo Lombi, Ho Kyong Shon, AM Shen, Erica Donner, William Skinner, Laura Chekli, B Bayatsarmadi, Binoy Sarkar, Ravi Naidu, Kirk G. Scheckel, Chekli, L, Bayatsarmadi, B, Sekine, Ryo, Sarkar, Binoy, Shen, A Maoz, Scheckel, K, Skinner, William, Naidu, Ravi, Shon, H, Lombi, Enzo, and Donner, Erica

Subjects
groundwater remediation, Environmental remediation, Groundwater remediation, Nanoparticle, Nanotechnology, surface chemistry, 02 engineering and technology, 010501 environmental sciences, 01 natural sciences, Biochemistry, Analytical Chemistry, characterization techniques, zero-valent iron nanoparticles, Environmental Chemistry, bulk composition, Nanoscopic scale, Spectroscopy, 0105 earth and related environmental sciences, Zerovalent iron, Aggregate (composite), Chemistry, particle size, 021001 nanoscience & nanotechnology, Characterization (materials science), Particle size, 0210 nano-technology
Abstract

Zero-valent iron nanoparticles (nZVI) have been widely tested as they are showing significant promise for environmental remediation. However, many recent studies have demonstrated that their mobility and reactivity in subsurface environments are significantly affected by their tendency to aggregate. Both the mobility and reactivity of nZVI mainly depends on properties such as particle size, surface chemistry and bulk composition. In order to ensure efficient remediation, it is crucial to accurately assess and understand the implications of these properties before deploying these materials into contaminated environments. Many analytical techniques are now available to determine these parameters and this paper provides a critical review of their usefulness and limitations for nZVI characterisation. These analytical techniques include microscopy and light scattering techniques for the determination of particle size, size distribution and aggregation state, and X-ray techniques for the characterisation of surface chemistry and bulk composition. Example characterisation data derived from commercial nZVI materials is used to further illustrate method strengths and limitations. Finally, some important challenges with respect to the characterisation of nZVI in groundwater samples are discussed. Refereed/Peer-reviewed

Published
2015

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