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Made available in DSpace on 2014-10-09T12:49:51Z (GMT). No. of bitstreams: 0 / Made available in DSpace on 2014-10-09T14:03:04Z (GMT). No. of bitstreams: 1 09826.pdf: 5905522 bytes, checksum: b0354cc2f21014da9657b88019b2b992 (MD5) / Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) / Tese (Doutoramento) / IPEN/T / Instituto de Pesquisas Energeticas e Nucleares - IPEN/CNEN-SP / FAPESP:99/07068-0

Propõe-se analisar teoricamente a instabilidade disruptora que ocorre em plasmas confinados em Tokamaks, investigando-se a influencia de campos helicoidais ressonantes em seu equilíbrio. Para isso, considerou-se a superposição do campo magnético do plasma em equilíbrio MHD estático com o campo associado às ressonâncias, levando-se em conta a geometria toroidal do Tokamak. Devido a falta de simetria, as linhas do campo magnético total resultante desta superposição devem formar superfícies magnéticas apenas em algumas regiões do plasma. Usando o método da media, foram obtidas (analiticamente) funções de superfícies aproximadas que contem, em torno das regiões de ressonância do plasma, as linhas deste campo magnético total. Verificou-se que estas superfícies aproximadas têm estruturas de ilhas magnéticas. / It is proposed to analyse theoretically the disruptive instability that occurs in confined plasmas in Tokamaks, through investigation of the influence of resonant helical fields on their equilibrium. With this aim, a superposition of the magnetic field of the plasma in static MHD equilibrium with the field associated with the resonances is considered, taking into account the toroidal geometry of the tokamak. Due to the lack of symmetry, the lines of the total magnetic field resulting from this superposition must form magnetic surfaces only around some regions of the plasma. Using the averaging method, functions of approximate magnetic surfaces are obtained (analitically) around the regions of resonances of the plasma (they contain the lines of this total magnetic field). It was verified that these approximate surfaces have structures of magnetic islands.

O presente trabalho realiza a investigação de interações hiperfinas em amostras de silício monocristalino através da técnica de Correlação Angular γ-γ Perturbada (CAP), baseada em interações hiperfinas. Para a realização das medidas, utilizou-se núcleos de prova radioativos de 111In -> 111Cd que decaem através da cascata gama 177-245keV com nível intermediário de 245keV (I = 5+/2 , Q = 0.83b, T1/2 = 84.5ns). As amostras foram confeccionadas utilizando vários métodos de inserção de núcleos de prova, possibilitando maior compreensão acerca dos impactos gerados por cada um destes métodos nas medidas CAP. As técnicas de implantação iônica, difusão e evaporação foram cuidadosamente investigadas ressaltando-se suas particularidades. Realizou-se então, um estudo acerca das concentrações de defeitos intrínsecos em função de vários processos de tratamento térmico. Finalmente, foi feita uma análise comparativa para os vários métodos de inserção dos núcleos de prova. Realizou-se, também, medidas CAP em silício monocristalino dopado com fósforo através do processo NTD. A altíssima uniformidade de dopagem associada a este método aliada à inexistência de medidas para este tipo de material ressaltam a relevância dos resultados obtidos. Estes resultados são então comparados com os resultados da literatura para amostras dopadas através de métodos convencionais apresentando-se as respectivas conclusões. / In the present work, a microscopic investigation of hyperfine interactions in single crystal silicon samples was carried out by means of Perturbed Angular γ-γ Correlation technique (PAC), which is based in hyperfine interactions. In order to achieve these measurements, it was used 111In ->111Cd radioactive probe nuclei, which decay through the well known γ cascade 177-245keV with an intermediate level of 245keV (I = 5+/2 , Q = 0.83b , T1/2 = 84.5ns). The samples were prepared using diferent probe nuclei insertion methods, making possible to increase our understanding on the impact generated by each of these techniques in PAC measurements. Ion implantation, difusion and evaporation were carefully investigated giving emphasis on its characteristics and particularities. Then, it was made a study about the concentration of intrinsic defects as function of several annealing processes. Finally, a comparative analysis was made for all these probe nuclei insertion methods. This work also accomplished PAC measurements in single crystal silicon doped with phosphorus by means of NTD method, carried out in a research nuclear reactor. The extremely high doping uniformity allied to the non-existence of previous measurements in these materials emphasize the importance of the results obtained. These results are then compared with literature results for samples doped by conventional methods presenting the respective conclusions.

Orientador: Carola Dobrigkeit Chinellato / Tese (doutorado) - Universidade Estadual de Campinas, Instituto de Física Gleb Wataghin / Made available in DSpace on 2018-08-19T15:55:43Z (GMT). No. of bitstreams: 1 Selmi-Dei_DanielPakk_D.pdf: 9650136 bytes, checksum: a6af22f88f369a8903480bc20071c354 (MD5) Previous issue date: 2012 / Resumo: Esta tese apresenta um estudo das deflexões nas trajetórias de raios cósmicos com energia ultra-alta (> 1018 eV) devido à sua propagação pelo campo magnético da Via Láctea. Partindo de dados coletados no Observatório Pierre Auger, localizado na Argentina, a técnica do backtracking foi aplicada sob diversas hipóteses relativas à carga elétrica do núcleo primário. Uma situação histórica é feita desde a época da descoberta da radiação cósmica até as últimas técnicas de detecção desenvolvidas por Pierre Auger, descobridor dos chuveiros atmosféricos extensos. A natureza das cascatas é descrita para o entendimento de como direções de chegada e energias são inferidas através dos experimentos de hoje. Alguns detalhes do espectro do uxo de raios cósmicos nas energias mais altas são expostos. As metodologias relativas aos telescópios de uorescência e ao arranjo de superfície, empregados no Observatório Auger, são introduzidas. É estabelecida uma relação entre ambas as técnicas de detecção e alguns resultados importantes, obtidos nos últimos anos pela Colaboração Auger, são apresentados. É feita uma descrição da dinâmica de campos magnéticos em plasmas astrofísicos e de dados observacionais da rotação de Faraday para embasar a escolha dos modelos de campo magnético galácticos. A magnetohidrodinâmica também é usada para explicar por que é interessante considerar certos objetos aceleradores candidatos a fontes de raios cósmicos. A distribuição de matéria na Via Láctea é então caracterizada em relação aos dados de evolução estelar e passa a ser assumida a hipótese de que a nucleossíntese elementar ocorre de modo semelhante em outras galáxias. Em seguida, são definidos os modelos utilizados para a descrição dos campos magnéticos nas regiões do bojo, disco e halo da galáxia. A superposição de um modelo da componente irregular também é considerada. A técnica do backtracking de antipartículas (e, equivalentemente, o forwardtracking de partículas) é descrita segundo um novo método numérico de passos adaptativos introduzido neste trabalho. Algumas ferramentas de análise são propostas a partir dos dados de reconstrução das trajetórias. Em última análise, é demonstrado que esse método desenvolvido concorda com o método numérico de Runge e Kutta de quarta ordem. Os resultados apresentados nesta tese levam à conclusão de que se os modelos presentes descrevem aproximadamente o campo magnético de larga escala da Via Láctea, então raios cósmicos com energia ultra-alta são signicantemente de etidos durante a propagação. Para um evento real detectado no Observatório Auger, a escolha da composição química compatível com núcleos produzidos nas reações de nucleossíntese estelar permitiu indicar regiões da Via Láctea que podem abrigar objetos astrofísicos candidatos a fonte. Assumindo que um magnetar galáctico ativo conhecido radie partículas com E > 1019 eV, foi possível prever excessos do uxo bem localizados em certas direções do céu. Já a depleção desse uxo na direção do Aglomerado de Virgem pode ser explicada através da imposição de limites na composição química da radiação cósmica com incidência normal ao plano galáctico. Por último, sob a hipótese de que AGNs sejam as fontes dos núcleos atômicos ultra-energéticos observados, uma relação entre composição química e energia da partícula primária é derivada / Abstract: This thesis presents a study of the deflections of ultra-high energy (> 1018 eV) cosmic rays caused by its propagation through the large scale magnetic field of the Milky Way. From data collected by the Pierre Auger Observatory, in Argentina, the backtracking technique was applied under several hypotheses relative to the electric charge of the primary nucleus. A historical review is given since the discovery of the cosmic radiation until the last detection techniques developed by Pierre Auger, who was the discoverer of extensive air showers. The nature of the cascades is described for an understanding about how the arrival directions and energies are inferred from experiments performed today. Some details regarding the spectrum of the cosmic ray flux at the highest energies are exposed. The methodologies relative to the fluorescence telescopes and the surface array, employed at the Auger Observatory, are introduced. A relation is established between both techniques of detection and some important results obtained in the last years by the Auger Collaboration are presented. A description of the magnetic field dynamics in astrophysical plasmas and the observational data of Faraday rotation serve as a basis for the choice of galactic magnetic field models. Magnetohydrodynamics is also used to explain why it is interesting to consider certain objects as candidates for the source and acceleration of cosmic rays. The Milky Way is then characterized in respect to stellar evolution data and the hypotheses that the nucleosynthesis of the elements occurs in a similar way in other galaxies is assumed. Finally, models to describe the magnetic fields in the bulge, disk and halo regions are defined. The superposition of a model for the irregular component is also considered. The backtracking technique of antiparticles (and equivalently, the forwardtracking of particles) is described according to a new numerical adaptive stepsize method introduced in this work. Some analysis tools are proposed based on data from the reconstructed trajectories. Lastly, it is shown that the method developed here agrees with the fourth-order Runge-Kutta numerical method. The results presented is this thesis lead to the conclusion that if the present models describe approximately the large scale magnetic field of the Milky Way, then ultra-high energy cosmic rays are significantly de ected during propagation. For a real event detected at the Auger Observatory, the choice for a chemical composition compatible with the nuclei produced in stellar nucleosynthesis reactions allowed to pinpoint regions inside the MilkyWay that can house astrophysical objects as candidate sources. Assuming that a known active galactic magnetar radiates particles with E >1019 eV, it was possible to predict well localized ux excesses in certain directions of the sky. The depletion of that flux in the direction of the Virgo Cluster can be explained by the imposition of limits on the chemical composition of cosmic radiation with incidence normal to the galactic plane. In the last place, under the hypothesis that AGN are sources of the observed ultra-high energy atomic nuclei, a relation between chemical composition and particle energy is derived / Doutorado / Física / Doutor em Ciências

Recent observations have shown that coronal shocks driven by coronal mass ejections can develop and accelerate particles within several solar radii in large solar energetic particle (SEP) events. Motivated by this, we present an SEP acceleration study that including the process in which a fast shock propagates through a streamer-like magnetic field with both closed and open field lines in the low corona region. The acceleration of protons is modeled by numerically solving the Parker transport equation with spatial diffusion both along and across the magnetic field. We show that particles can be sufficiently accelerated to up to several hundred MeV within 2-3 solar radii. When the shock propagates through a streamer-like magnetic field, particles are more efficiently accelerated compared to the case with a simple radial magnetic field, mainly due to perpendicular shock geometry and the natural trapping effect of closed magnetic fields. Our results suggest that the coronal magnetic field configuration is an important factor for producing large SEP events. We further show that the coronal magnetic field configuration strongly influences the distribution of energetic particles, leading to different locations of source regions along the shock front where most high-energy particles are concentrated. This work may have strong implications for SEP observations. The upcoming Parker Solar Probe will provide in situ observations for the distribution of energetic particles in the coronal shock region, and test the results of the study.

Solar transient eruptions are the main cause of interplanetary-magnetospheric disturbances leading to the phenomena known as geomagnetic storms. Eruptive solar events such as coronal mass ejections (CMEs) are currently considered the main cause of geomagnetic storms (GMS). GMS are strong perturbations of the Earth’s magnetic field that can affect space-borne and ground-based technological systems. The solar-terrestrial impact on modern technological systems is commonly known as Space Weather. Part of the research study described in this thesis was to investigate and establish a relationship between GMS (periods with Dst ≤ −50 nT) and their associated solar and interplanetary (IP) properties during solar cycle (SC) 23. Solar and IP geoeffective properties associated with or without CMEs were investigated and used to qualitatively characterise both intense and moderate storms. The results of this analysis specifically provide an estimate of the main sources of GMS during an average 11-year solar activity period. This study indicates that during SC 23, the majority of intense GMS (83%) were associated with CMEs, while the non-associated CME storms were dominant among moderate storms. GMS phenomena are the result of a complex and non-linear chaotic system involving the Sun, the IP medium, the magnetosphere and ionosphere, which make the prediction of these phenomena challenging. This thesis also explored the predictability of both the occurrence and strength of GMS. Due to their nonlinear driving mechanisms, the prediction of GMS was attempted by the use of neural network (NN) techniques, known for their non-linear modelling capabilities. To predict the occurrence of storms, a combination of solar and IP parameters were used as inputs in the NN model that proved to predict the occurrence of GMS with a probability of 87%. Using the solar wind (SW) and IP magnetic field (IMF) parameters, a separate NN-based model was developed to predict the storm-time strength as measured by the global Dst and ap geomagnetic indices, as well as by the locally measured K-index. The performance of the models was tested on data sets which were not part of the NN training process. The results obtained indicate that NN models provide a reliable alternative method for empirically predicting the occurrence and strength of GMS on the basis of solar and IP parameters. The demonstrated ability to predict the geoeffectiveness of solar and IP transient events is a key step in the goal towards improving space weather modelling and prediction.

Cette thèse consiste en l'étude expérimentale et numérique des processus de formation des particules de suie au sein des flammes laminaires non-pré-mélangées et partiellement prémélangées sous l'influence d'un champ magnétique ou d'une stimulation acoustique. Dans une premiére étape, la capacité du code CIAO à prédire la fraction volumique de suie dans une flamme axisymétrique est étudiée. Par la suite, deux flammes subissant une stimulation acoustique ont été étudiées. Les résultats peuvent être utilisés pour améliorer les modèles de suie futurs, en particulier concernant les différentes échelles temporelles de la chimie en phase gazeuse, et la formation d'hydrocarbures polyaromatiques (PAH) et de suie couplée avec des flux transitoires. Pour étudier la formation des particules de suie sous l'influence de gradients de champ magnétique, un brûleur de type Santoro est utilisé. Les techniques de mesure utilisées dans le cadre de cette thèse sont l'imagerie directe à haute cadence, la technique Background Oriented Schlieren (BOS) et la méthode d'Absorption/Emission Modulée (MAE). Une augmentation de la fraction volumique de suie intégrée a été mise en évidence lorsque le gradient de champ magnétique est ascendant. Une analyse de stabilité linéaire locale appliquée à l'écoulement non-visqueux est présentée pour une flamme sous l'influence de la perturbation magnétique envisagée. Le gradient de champ magnétique provoque alors une réduction du taux d'amplification. De fait, l'étude est complété par l'identification d'un domaine où les flammes qui oscillent naturellement peuvent être stabilisées et contrôlées par des gradients de champ magnétique. / In this thesis light is shed on the soot formation processes in laminar coflow flames influenced by magnetic field gradients and acoustic forcing. Both influences have been assessed experimentally and numerically. First, the CIAO in-house code's ability to predict soot volume fraction fields in a steady coflow flame is studied. Then, two acoustically forced cases were studied. These findings are used to improve future soot models, especially, concerning the different time scales of gas phase chemistry and the formation of polycyclic aromatic hydrocarbons (PAH) and soot coupled with unsteady flows. To investigate soot formation under magnetic field gradients, a Santoro type burner is used. The measurement techniques applied in the course of this thesis are high-speed luminosity measurements, Background Oriented Schlieren (BOS) and one- and two-color Modulated Absorption/Emission (MAE) techniques. The magnetic field impact on soot formation was first studied experimentally in steady laminar flames. A scaling of soot production similar to the increased integrated soot volume fraction with increased oxygen content in the coflow was documented. A local inviscid stability analysis is presented for an ethylene coflow flame to investigate the flame's response to small perturbations of the mean velocity, temperature, fuel, and oxygen massfraction under magnetic field exposure. The magnetic field is found to reduce the perturbations' growth rate. The magnetic field study is completed by identifying a domain where naturally oscillating flames can be stabilized and controlled by magnetic field gradients.

Zeeman deceleration is an experimental technique which allows for the manipulation of open-shell atoms and molecules in a supersonic beam thus producing mK-cold, velocity-tunable beams of particles in selected quantum states. The method relies on the Zeeman interaction between paramagnetic particles and time-varying, inhomogeneous magnetic fields generated by pulsing high currents through an array of solenoid coils. This thesis describes the construction and implementation of a supersonic beam setup including a 12-stage Zeeman decelerator. The Zeeman decelerator follows an original design that makes it possible to replace individual deceleration coils. Using ground-state hydrogen atoms as a test system, it is shown that the transverse acceptance in a Zeeman decelerator can be significantly increased by generating a rather low, temporally varying quadrupole field in one of the solenoid coils. An electron-impact source was constructed and optimised enabling, for the first time, the Zeeman deceleration of metastable helium atoms in the 23S1 state, with an up to 40 % decrease in the kinetic energy of the beam. It is shown that the pulse duration for electron-impact excitation needs to be matched to the acceptance of the decelerator in order to attain a good contrast between the decelerated and undecelerated parts of the beam. Experimental results are rigorously analysed and interpreted using three-dimensional numerical particle trajectory simulations. A phase-space model provides, for the first time, a means to estimate the six-dimensional phase-space acceptance in a Zeeman decelerator and to find optimum parameter sets for improved Zeeman deceleration schemes. The approach also reveals a hitherto unconsidered velocity dependence of the phase stability which is ascribed mainly to the rise and fall times of the current pulses that generate the magnetic fields inside the deceleration coils. In the future, it is planned to combine the Zeeman decelerator with a source of cold atomic and molecular ions to study chemical collisions at low temperatures. A hybrid magnetic guide consisting of permanent magnet assemblies (Halbach arrays) in hexapole configuration and a set of current-carrying wires is proposed and simulated as an interface between these setups. The design promises very efficient velocity selection, a high degree of quantum-state selection and a nearly complete removal of residual carrier gas. Prospects for using magnetic hexapole focusing in front of the Zeeman decelerator are discussed. The work represents a major step towards the study and control of chemical reactivity of paramagnetic species in the low-temperature regime and it will help in the testing of fundamental chemical reaction theories.