49 resultados para MEV-EDX


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The compounds responsible for the colours and decorations in glass and glazed ceramics include: colouring agents (transition metal ions), pigments (micro-and nano-precipitates of compounds that either do not dissolve or recrystallize in the glassy matrix) and opacifiers (microcrystalline compounds with high light scattering capability). Their composition, structure and range of stability are highly dependent not only on the composition but also on the procedures followed to obtain them. Chemical composition of the colorants and crystallites may be obtained by means of SEM-EDX and WDX. Synchrotron Radiation micro-X-ray Diffraction has a small beam size adequate (10 to 50 microns footprint size) to obtain the structural information of crystalline compounds and high brilliance, optimal for determining the crystallites even when present in low amounts. In addition, in glass decorations the crystallites often appear forming thin layers (from 10 to 100 micrometers thick) and they show a depth dependent composition and crystal structure. Their nature and distribution across the glass/glazes decorations gives direct information on the technology of production and stability and may be related to the color and appearance. A selection of glass and glaze coloring agents and decorations are studied by means of SR-micro- XRD and SEM-EDX including: manganese brown, antimony yellow, red copper lusters and cobalt blue. The selection includes Medieval (Islamic, and Hispano Moresque) and renaissance tin glazed ceramics from the 10th to the 17th century AD.

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In 2009, Cygnus X-3 (Cyg X-3) became the first microquasar to be detected in the GeV γ-ray regime, via the satellites Fermi and AGILE. The addition of this new band to the observational toolbox holds promise for building a more detailed understanding of the relativistic jets of this and other systems. We present a rich data set of radio, hard and soft X-ray, and γ-ray observations of Cyg X-3 made during a flaring episode in 2010 May. We detect a ~3 day softening and recovery of the X-ray emission, followed almost immediately by a ~1 Jy radio flare at 15 GHz, followed by a 4.3σ γ-ray flare (E > 100 MeV) ~1.5 days later. The radio sampling is sparse, but we use archival data to argue that it is unlikely the γ-ray flare was followed by any significant unobserved radio flares. In this case, the sequencing of the observed events is difficult to explain in a model in which the γ-ray emission is due to inverse Compton scattering of the companion star's radiation field. Our observations suggest that other mechanisms may also be responsible for γ-ray emission from Cyg X-3.

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High-energy charged particles in the van Allen radiation belts and in solar energetic particle events can damage satellites on orbit leading to malfunctions and loss of satellite service. Here we describe some recent results from the SPACECAST project on modelling and forecasting the radiation belts, and modelling solar energetic particle events. We describe the SPACECAST forecasting system that uses physical models that include wave-particle interactions to forecast the electron radiation belts up to 3 h ahead. We show that the forecasts were able to reproduce the >2 MeV electron flux at GOES 13 during the moderate storm of 7-8 October 2012, and the period following a fast solar wind stream on 25-26 October 2012 to within a factor of 5 or so. At lower energies of 10- a few 100 keV we show that the electron flux at geostationary orbit depends sensitively on the high-energy tail of the source distribution near 10 RE on the nightside of the Earth, and that the source is best represented by a kappa distribution. We present a new model of whistler mode chorus determined from multiple satellite measurements which shows that the effects of wave-particle interactions beyond geostationary orbit are likely to be very significant. We also present radial diffusion coefficients calculated from satellite data at geostationary orbit which vary with Kp by over four orders of magnitude. We describe a new automated method to determine the position at the shock that is magnetically connected to the Earth for modelling solar energetic particle events and which takes into account entropy, and predict the form of the mean free path in the foreshock, and particle injection efficiency at the shock from analytical theory which can be tested in simulations.

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High-energy charged particles in the van Allen radiation belts and in solar energetic particle events can damage satellites on orbit leading to malfunctions and loss of satellite service. Here we describe some recent results from the SPACECAST project on modelling and forecasting the radiation belts, and modelling solar energetic particle events. We describe the SPACECAST forecasting system that uses physical models that include wave-particle interactions to forecast the electron radiation belts up to 3 h ahead. We show that the forecasts were able to reproduce the >2 MeV electron flux at GOES 13 during the moderate storm of 7-8 October 2012, and the period following a fast solar wind stream on 25-26 October 2012 to within a factor of 5 or so. At lower energies of 10- a few 100 keV we show that the electron flux at geostationary orbit depends sensitively on the high-energy tail of the source distribution near 10 RE on the nightside of the Earth, and that the source is best represented by a kappa distribution. We present a new model of whistler mode chorus determined from multiple satellite measurements which shows that the effects of wave-particle interactions beyond geostationary orbit are likely to be very significant. We also present radial diffusion coefficients calculated from satellite data at geostationary orbit which vary with Kp by over four orders of magnitude. We describe a new automated method to determine the position at the shock that is magnetically connected to the Earth for modelling solar energetic particle events and which takes into account entropy, and predict the form of the mean free path in the foreshock, and particle injection efficiency at the shock from analytical theory which can be tested in simulations.

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Esta contribución presenta el Proyecto de investigación que se está llevando a cabo en la Sección de Conservación¿Restauración de la Facultad de Bellas Artes de la Universidad de Barcelona desde el año 2006. El proyecto tiene por objetivo identificar los problemas que generan los tratamientos con PVAc, poliacetato de vinilo, en diversos bienes patrimoniales, así como el establecimiento de protocolos para la reversibilización del adhesivo. El trabajo se centra en los materiales de archivo, los materiales arqueológicos, la pinturasobre tela, sobre madera y la pintura mural por ser casos especialmente representativos de patrimonio en los que se ha utilizado este adhesivo y en los que se pueden detectar problemas derivados de su utilización. El estudio parte de la selección de obras originales procedentes de museos e instituciones colaboradoras que fueron tratadas con poliacetato de vinilo. De éstas obras se extrajeron muestras para caracterizar su composición y estado conservación. Una vez conocida la estructura de las obras se prepararon muestras probeta simulando las obras originales y se sometieron a un proceso de envejecimiento acelerado. A partir de estos simulacros se realizaron análisis para conocer los efectos derivados del uso del PVAc en tratamientos de conservación-restauración. Las técnicas de análisis empleadas fueron: medición de pH, espectroscopía de IR por transformada de Fourier (FTIR), análisis de pirolisis-cromatografía de gases / espectrometría de masas (Py-GC-MS), espectroscopia Raman por transformada de Fourier (FT-Raman), análisis de color, microscopía electrónica de barrido, espectroscopia de dispersión de rayos X (SEM-EDX) y microscopía óptica. Con la divulgación de los resultados acerca de la composición, pH, color, efectos del adhesivo sobre los soportes, propiedades mecánicas y reversibilización del adhesivo, obtenidos de las muestras probeta antes y después de la primera fase de envejecimiento acelerado, así como en unas muestras de adhesivos envejecidas de forma natural durante 10 años, se pretende fomentar la difusión y el intercambio de información entre los centros dedicados a la Conservación-Restauración del patrimonio.

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Esta contribución presenta el Proyecto de investigación que se está llevando a cabo en la Sección de Conservación¿Restauración de la Facultad de Bellas Artes de la Universidad de Barcelona desde el año 2006. El proyecto tiene por objetivo identificar los problemas que generan los tratamientos con PVAc, poliacetato de vinilo, en diversos bienes patrimoniales, así como el establecimiento de protocolos para la reversibilización del adhesivo. El trabajo se centra en los materiales de archivo, los materiales arqueológicos, la pinturasobre tela, sobre madera y la pintura mural por ser casos especialmente representativos de patrimonio en los que se ha utilizado este adhesivo y en los que se pueden detectar problemas derivados de su utilización. El estudio parte de la selección de obras originales procedentes de museos e instituciones colaboradoras que fueron tratadas con poliacetato de vinilo. De éstas obras se extrajeron muestras para caracterizar su composición y estado conservación. Una vez conocida la estructura de las obras se prepararon muestras probeta simulando las obras originales y se sometieron a un proceso de envejecimiento acelerado. A partir de estos simulacros se realizaron análisis para conocer los efectos derivados del uso del PVAc en tratamientos de conservación-restauración. Las técnicas de análisis empleadas fueron: medición de pH, espectroscopía de IR por transformada de Fourier (FTIR), análisis de pirolisis-cromatografía de gases / espectrometría de masas (Py-GC-MS), espectroscopia Raman por transformada de Fourier (FT-Raman), análisis de color, microscopía electrónica de barrido, espectroscopia de dispersión de rayos X (SEM-EDX) y microscopía óptica. Con la divulgación de los resultados acerca de la composición, pH, color, efectos del adhesivo sobre los soportes, propiedades mecánicas y reversibilización del adhesivo, obtenidos de las muestras probeta antes y después de la primera fase de envejecimiento acelerado, así como en unas muestras de adhesivos envejecidas de forma natural durante 10 años, se pretende fomentar la difusión y el intercambio de información entre los centros dedicados a la Conservación-Restauración del patrimonio.

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We show that the quasifission paths predicted by the one-body dissipation dynamics, in the slowest phase of a binary reaction, follow a quasistatic path, which represents a sequence of states of thermal equilibrium at a fixed value of the deformation coordinate. This establishes the use of the statistical particle-evaporation model in the case of dynamical time-evolving systems. Pre- and post-scission multiplicities of neutrons and total multiplicities of protons and α particles in fission reactions of 63Cu+92Mo, 60Ni+100Mo, 63Cu+100Mo at 10 MeV/u and 20Ne+144,148,154Sm at 20 MeV/u are reproduced reasonably well with statistical model calculations performed along dynamic trajectories whose slow stage (from the most compact configuration up to the point where the neck starts to develop) lasts some 35×10−21 s.

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We analyze the neutron skin thickness in finite nuclei with the droplet model and effective nuclear interactions. The ratio of the bulk symmetry energy J to the so-called surface stiffness coefficient Q has in the droplet model a prominent role in driving the size of neutron skins. We present a correlation between the density derivative of the nuclear symmetry energy at saturation and the J/Q ratio. We emphasize the role of the surface widths of the neutron and proton density profiles in the calculation of the neutron skin thickness when one uses realistic mean-field effective interactions. Next, taking as experimental baseline the neutron skin sizes measured in 26 antiprotonic atoms along the mass table, we explore constraints arising from neutron skins on the value of the J/Q ratio. The results favor a relatively soft symmetry energy at subsaturation densities. Our predictions are compared with the recent constraints derived from other experimental observables. Though the various extractions predict different ranges of values, one finds a narrow window L∼45-75 MeV for the coefficient L that characterizes the density derivative of the symmetry energy that is compatible with all the different empirical indications.

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The recently developed semiclassical variational Wigner-Kirkwood (VWK) approach is applied to finite nuclei using external potentials and self-consistent mean fields derived from Skyrme inter-actions and from relativistic mean field theory. VWK consist s of the Thomas-Fermi part plus a pure, perturbative h 2 correction. In external potentials, VWK passes through the average of the quantal values of the accumulated level density and total en energy as a function of the Fermi energy. However, there is a problem of overbinding when the energy per particle is displayed as a function of the particle number. The situation is analyzed comparing spherical and deformed harmonic oscillator potentials. In the self-consistent case, we show for Skyrme forces that VWK binding energies are very close to those obtained from extended Thomas-Fermi functionals of h 4 order, pointing to the rapid convergence of the VWK theory. This satisfying result, however, does not cure the overbinding problem, i.e., the semiclassical energies show more binding than they should. This feature is more pronounced in the case of Skyrme forces than with the relativistic mean field approach. However, even in the latter case the shell correction energy for e.g.208 Pb turns out to be only ∼ −6 MeV what is about a factor two or three off the generally accepted value. As an adhoc remedy, increasing the kinetic energy by 2.5%, leads to shell correction energies well acceptable throughout the periodic table. The general importance of the present studies for other finite Fermi systems, self-bound or in external potentials, is pointed out.

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We explore the possible association between the microquasar LSI +61°303 and the EGRET source 2CG 135+01/3EG J0241+6103 by studying, with a detailed numerical model, whether this system can produce the emission and the variability detected by EGRET (>100 MeV) through inverse Compton (IC) scattering. Our numerical approach considers a population of relativistic electrons entrained in a cylindrical inhomogeneous jet, interacting with both the radiation and the magnetic fields, taking into account the Thomson and Klein-Nishina regimes of interaction. Our results reproduce the observed spectral characteristics and variability at γ-rays, thus strengthening the identification of LSI +61°303 as a high-energy γ-ray source.

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Durant les excavacions de l"avinguda de Cambó dutes a terme el 1986 es van recuperar, entre d"altres, diversos elements identificats com a alambins, que han estat relacionats amb la tècnica d"aplicació d"or al foc sobre objectes metàl·lics, activitat que podria haver tingut lloc en un dels àmbits identificats en el quarter de Sant Pere en època medieval.Amb l"objectiu de comprovar si els alambins recuperats són, d"una banda, de producció local i, d"una altra, si presenten evidències que puguin corroborar el seu ús en aquesta tècnica, es va procedir a la caracterització arqueomètrica de tres d"aquests objectes (BCN224, BCN225 i BCN226), de manera que la seva composicióquímica s"ha determinat per fluorescència de raigs X (FRX) i la composició mineralògica a través de la difracció de raigs X (DRX). Per a l"estudi de la microestructura i estadi de sinterització de la matriu i del vidriat, s"han dut a terme observacions i microanàlisis per microscòpia electrònica de rastreig (MER) utilitzant un microscopi Jeol JSM-840 equipat amb un detector de dispersió d"energies de raigs X (EDX). A més, amb la finalitat de fixarles característiques macroscòpiques dels individus es van realitzar observacions a partir de fractures fresques emprant una lupa binocular Olympus SZX10, amb una font d"il·luminació de llum freda Olympus KL 1500 LCD equipada amb filtre de llum de dia i una càmera digital de microfotografia Olympus DP25, amb el software Cell"A. La lupa binocular està equipada amb un objectiu de 1X i oculars de 10X, amb un zoom continuat, amb posicions fixes, que permet fer observacions de 6.3X a 63X, però que s"han estandarditzat a 10X i 25X.

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In 2009, Cygnus X-3 (Cyg X-3) became the first microquasar to be detected in the GeV γ-ray regime, via the satellites Fermi and AGILE. The addition of this new band to the observational toolbox holds promise for building a more detailed understanding of the relativistic jets of this and other systems. We present a rich data set of radio, hard and soft X-ray, and γ-ray observations of Cyg X-3 made during a flaring episode in 2010 May. We detect a ~3 day softening and recovery of the X-ray emission, followed almost immediately by a ~1 Jy radio flare at 15 GHz, followed by a 4.3σ γ-ray flare (E > 100 MeV) ~1.5 days later. The radio sampling is sparse, but we use archival data to argue that it is unlikely the γ-ray flare was followed by any significant unobserved radio flares. In this case, the sequencing of the observed events is difficult to explain in a model in which the γ-ray emission is due to inverse Compton scattering of the companion star's radiation field. Our observations suggest that other mechanisms may also be responsible for γ-ray emission from Cyg X-3.

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The expansion of an isolated hot spherical nucleus with excitation energy and its caloric curve are studied in a thermodynamic model with the SkM∗ force as the nuclear effective two-body inter-action. The calculated results are shown to compare well with the recent experimental data from energetic nuclear collisions. The fluctuations in temperature and density are also studied. They are seen to build up very rapidly beyond an excitation energy of ∼9 MeV/u. Volume-conserving quadrupole deformation in addition to expansion indicates , however, nuclear disassembly above an excitation energy of ∼4 MeV/u.

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A study of D +π−, D 0π+ and D ∗+π− final states is performed using pp collision data, corresponding to an integrated luminosity of 1.0 fb−1, collected at a centre-of-mass energy of 7 TeV with the LHCb detector. The D 1(2420)0 resonance is observed in the D ∗+π− final state and the D∗2(2460) resonance is observed in the D +π−, D 0π+ and D ∗+π− final states. For both resonances, their properties and spin-parity assignments are obtained. In addition, two natural parity and two unnatural parity resonances are observed in the mass region between 2500 and 2800 MeV. Further structures in the region around 3000 MeV are observed in all the D ∗+π−, D +π− and D 0π+ final states.

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Massive protostars have associated bipolar outflows with velocities of hundreds of km s-1. Such outflows can produce strong shocks when they interact with the ambient medium leading to regions of nonthermal radio emission. Aims. We aim at exploring under which conditions relativistic particles are accelerated at the terminal shocks of the protostellar jets and whether they can produce significant gamma-ray emission. Methods. We estimate the conditions necessary for particle acceleration up to very high energies and gamma-ray production in the nonthermal hot spots of jets associated with massive protostars embedded in dense molecular clouds. Results. We show that relativistic bremsstrahlung and proton-proton collisions can make molecular clouds with massive young stellar objects detectable by the Fermi satellite at MeV-GeV energies and by Cherenkov telescope arrays in the GeV-TeV range. Conclusions. Gamma-ray astronomy can be used to probe the physical conditions in star-forming regions and particle acceleration processes in the complex environment of massive molecular clouds.