Дисертації з теми "Simulation of magnetic fields"

Les dispersions col·loïdals, un terme encunyat pel científic escocès Thomas Graham el 1861, han estat objecte d’interès en diferents àrees científiques durant més d'un segle. Una dispersió col·loïdal es caracteritza per l’existència d'una fase dispersa uniformement distribuïda dins un medi dispersiu. Diferents compostos entren dins aquesta categoria, com els aerosols (fum, boira, núvols o pols), les escumes, les emulsions (maionesa o llet) o els gels (mantega o melmelada). Les millores recents en la síntesi de partícules i l'estabilitat col·loïdal han impulsat la millora en el disseny de nous col·loides, conferint-los les propietats requerides en cada aplicació. Entre la gran varietat de dispersions col·loïdals (existents en la naturalesa o dissenyades per l'home), hem estudiat un tipus singular de dispersions on les partícules col·loïdals mostren un comportament superparamagnetic anomenades dispersions col·loïdals superparamagnètiques. En aquestes dispersions, sorgeixen característiques sorprenents quan un camp magnètic extern és aplicat, com a conseqüència del balanç entre les interaccions característiques entre col·loides i la interacció magnètica anisotròpica dipol-dipol entre les partícules col·loïdals constituents. Al llarg d'aquesta tesi s'ha utilitzat diferents models teòrics i de simulació per tractar diferents fenòmens que apareixen en aquestes dispersions col·loïdals superparamagnètiques. Per una banda, hem mostrat com l’aplicació de camps magnètics uniformes a aquestes dispersions indueix l’agregació reversible de les partícules superparamagnètiques. A la vista dels models teòrics i simulacions, hem proposat un nou criteri basat en les propietats físiques de les dispersions col·loïdals per predir la formació d'agregats, i la seva validesa s'ha discutit comparant el comportament predit amb resultats experimentals. Hem aportat evidencies de la existència d'un estat d'equilibri on els agregats assoleixen una distribució de mides estable, un fet ja suggerit amb anterioritat però establert sense prou claredat. També ens hem centrat en la descripció de la cinètica de creixement d'aquests agregats i en la seva implicació en diferents fenòmens observats experimentalment. La necessitat d'assolir escales de temps grans, com en certes situacions experimentals, ha motivat el desenvolupament de nous models i estratègies de simulació per reduir els temps de càlcul requerits en simulacions estàndard. Hem presentat un nou model de simulació que proporciona un mètode fiable i més ràpid per descriure la formació d'estructures en forma de cadena que apareixen en dispersions superparamagnètiques. El model ha estat validat comparant-ne els resultats obtinguts amb altres resultats de simulacions estàndard de Dinàmica de Langevin i s'ha aplicat a situacions experimentals, com ara el temps de relaxació T2 dels protons en solucions aquoses de nanopartícules superparamagnètiques. Mencionar també que aquest model de simulació ha estat implementat i el corresponent programari s’ha posat a disposició de la comunitat científica de forma gratuïta, concebut com una eina de simulació que pot ser ampliada fàcilment per resoldre altres problemes d’interès. Per altra banda, també hem discutit diferents efectes que sorgeixen com a conseqüència de l’aplicació de camps magnètics inhomogenis a aquestes dispersions superparamagnètiques. En concret, hem estudiat el moviment de les partícules magnètiques disperses en fluids a través de camps magnètics inhomogenis, el que es coneix com magnetoforesi. Per a tal efecte, hem centrat els esforços en la descripció de la separació magnètica de col·loides mitjançant l’aplicació de gradients de camp magnètic uniformes, des de dispersions superparamagnètiques a mescles de col·loides amb diferent resposta magnètica. Hem validat aquests models teòrics comparant-los amb simulacions per ordinador i n’hem discutit la seva utilitat comparant-ne les prediccions amb resultats experimentals. L’anàlisi racional d'aquests resultats proporciona un marc idoni per a millorar el disseny i el rendiment de diferents separadors magnètics, així com plantejar noves estratègies de separació, com per exemple la separació cooperativa en dispersions superparamagnètiques. Existeixen, encara, problemes oberts que esperem que aquest treball ajudi a afrontar com, per exemple, entendre la interconnexió entre les estructures induïdes en dispersions superparamagnètiques i la seva dinàmica d’agregació. Aquest és un aspecte important en una gran varietat d'aplicacions industrials i de laboratori com són els processos de separació magnètica, tractament d’aigües residuals i eliminació de contaminants, immunoassaigs en aplicacions clíniques o la creació de nous materials supramoleculars. Tanmateix, esperem que els resultats que es presenten al llarg d'aquest document encoratgin nous estudis dins el camp de col·loides magnètics, ja sigui perfeccionant els resultats i mètodes aquí presentats o contribuint al desenvolupament de noves estratègies per afrontar problemes encara per resoldre.
Colloidal dispersions, a term coined by the Scottish scientist Thomas Graham in 1861, have been the subject of interest in different scientific areas during more than a century. A colloidal dispersion is characterized by the existence of a dispersed phase uniformly distributed throughout a dispersion medium. Many different compounds fall in this category like aerosols (smog, fog, clouds or dust), foams, emulsions (mayonnaise or milk) or gels (butter or jelly). Recent improvements in particle synthesis and colloidal stability have boosted the controlled design of new colloids on demand, targeting the required properties for each application. Among the large variety of different colloidal dispersions (either found in nature or man-made), we have studied a singular type of such dispersions where the colloids have a superparamagnetic behavior called superparamagnetic colloidal dispersions. In these dispersions, surprising features arise under the application of an external magnetic field, as a consequence of the interplay between characteristic colloidal interactions and the anisotropic magnetic dipole-dipole interaction between their constituent colloidal particles. Along this thesis we have used different theoretical and simulation methods to discuss a number of phenomena appearing in superparamagnetic colloidal dispersions. On the one hand, we have shown that the application of a uniform magnetic field to such dispersions may induce the reversible aggregation of superparamagnetic particles. In view of theoretical models and computer simulations, a new criterion based on the physical properties of the colloidal dispersion has been proposed to predict the formation of aggregates, and its validity has been discussed by comparing the predicted behavior with experimental results. We have provided evidences of the existence of an equilibrium state, where aggregate sizes acquire a steady distribution, an issue previously suggested but unclear up to now. We have also focused our attention on the growth kinetics of the aggregates and its implications in different phenomena observed in experiments. The need to reach the large time scales of some experiments has motivated the development of new models and simulation strategies to overcome the large time consuming calculations required in standard simulations. We have presented a new simulation model that provides a faster and reliable approach to address the formation of chain-like structures in superparamagnetic dispersions. The model has been validated by direct comparison with standard Langevin Dynamics simulations and has been applied to experimental situations like the T2 relaxation time of protons in aqueous solutions of superparamagnetic nanoparticles. Let us mention that the simulation model has been implemented and the corresponding computer code is free and available to the scientific community, envisaged as a new modeling tool readily extensible to other problems of interest. On the other hand, we have analyzed different effects arising as a consequence of the application of inhomogeneous magnetic fields to such superparamagnetic dispersions. Specifically, we have studied the controlled motion of magnetic particles dispersed in a liquid medium by using inhomogeneous magnetic fields, what is known as magnetophoresis. To do so, we have focused the efforts on the description of the magnetic separation of colloids by the application of uniform magnetic field gradients, from superparamagnetic dispersions to mixtures of colloids with different magnetic response. We have validated the theoretical models adopted against computer simulations and we have discussed their usefulness by comparing the predictions obtained with experimental results. The rational analysis of these results provides a proper starting framework to enhance the design and performance of different magnetic separators, as well as to shape new separation strategies, like the cooperative magnetophoretic separation in superparamagnetic dispersions. There exists, of course, open problems that we hope this work will help to deal with. For instance, a better understanding of the interplay between the induced structures in superparamagnetic dispersions and their aggregation kinetics. This is an important issue in a vast variety of industrial and lab applications as, for example, in magnetic separation-based processes, waste-water treatment and pollutant removal, immunoassays in clinical applications or in the assisted assembly of new supramolecular materials. Nevertheless, we hope that the results presented along this document could encourage further studies in magnetic colloids science, either refining the results and approaches provided here or developing new strategies to face unsolved problems.

付記する学位プログラム名: 京都大学卓越大学院プログラム「先端光・電子デバイス創成学」
京都大学
新制・課程博士
博士(工学)
甲第23205号
工博第4849号
京都大学大学院工学研究科電気工学専攻
(主査)教授 小林 哲生, 教授 松尾 哲司, 特定教授 中村 武恒
学位規則第4条第1項該当
Doctor of Philosophy (Engineering)
Kyoto University
DFAM

Magnetic fields play a key role in a wide variety of phenomena found on the Sun. One such phenomena is the Coronal Mass Ejection (CME) where a large amount of material is ejected from the Sun. CME’s may directly affect the earth, therefore understanding their origin is of key importance for space weather and the near-Earth environment. In this thesis, the nature and evolution of solar magnetic fields is considered through a combination of Magnetic Flux Transport Simulations and Potential Field Source Surface Models. The Magnetic Flux Transport Simulations produce a realistic description of the evolution and distribution of the radial magnetic field at the level of the solar photosphere. This is then applied as a lower boundary condition for the Potential Field Source Surface Models which prescribe a coronal magnetic field. Using these two techniques, the location and variation of coronal null points, a key element in the Magnetic Breakout Model of CMEs, are determined. Results show that the number of coronal null points follow a cyclic variation in phase with the solar cycle. In addition, they preferentially form at lower latitudes as a result of the complex active latitude field. Although a significant number of coronal nulls may exist at any one time (≈ 17), it is shown that only half may satisfy the necessary condition for breakout. From this it is concluded that while the Magnetic Breakout Model of CMEs is an important model in understanding the origin of the CMEs, other processes must occur in order to explain the observed number of CMEs. Finally, the Magnetic Flux Transport Simulations are applied to stellar magnetic fields and in particular to the fast rotating star HD171488. From this speculative study it is shown that the Magnetic Flux Transport Simulations constructed for the Sun may be applied in very different stellar circumstances and that for HD171488 a significantly higher rate of meridional flow (1200-1400 ms⁻¹) is required to match observed magnetic field distributions.

Design of magnetic component is a key factor in achieving high frequency, high power-density converters. Planar magnetics are widely used in bias power supplies for the benefits of low profile and their compatibility with printed-circuit boards (PCB). The coupled inductors with winding layers sandwiched between two core plates are studied in this dissertation in order to model the self-inductance, winding loss, and core loss. The most challenging task for the plate-core inductor is to model the magnetic field with finite core dimensions, very non-uniform flux pattern, and large fringing flux. The winding is placed near the edge of the core to maximize the energy within the limited footprint and the amount of energy stored outside the core volume is not negligible. The proportional-reluctance, equal-flux (PREF) model is developed to build the contours with equal amount of flux by governing the reluctance of the flux path. The shapes of the flux lines are modeled by different functions that guided by the finite-element simulation (FES). The field from the flux lines enables calculation of inductance, winding loss, and core loss, etc. The inductance matrix including self-inductance and mutual inductance of a coupled inductor is important for circuit simulation and evaluation. The derivation of the inductance matrix of inductors with plate-core structure is described in Chapter 2. Two conditions are defined as common-mode (CM) field and differential-mode (DM) field in order to compute the matrix parameters. The proportional-reluctance, equal-flux (PREF) model introduced is employed to find the CM field distribution, and the DM field distribution is found from functions analogous to that of a solenoid's field. The inductance calculated are verified by flex-circuit prototypes with various dimensions, and the application of the inductance model is presented at the last with normalized parameters to cover structures within a wide-range. In circuit where coupled inductors are used instead of transformers, the phase shift between the primary and secondary side is not always 180 degrees. Therefore, it is important to model the winding loss for a coupled inductor accurately. The winding loss can be calculated from the resistance matrix, which is independent of excitations but only relates to the frequency and geometry. The methodology to derive the resistance matrix from winding losses of coupled inductors is discussed. Winding loss model with 2D magnetic field is improved by including the additional eddy current loss for better accuracy for the plate-core structures. The resistance matrix calculated from the model is verified by both measurement results and finite-element simulation (FES) of coupled-inductor prototypes. Accurate core loss model is required for designing magnetic components in power converters. Most existing core loss models are based on frequency domain calculation and they cannot be implemented in SPICE simulations. The core loss model in the time domain is discussed in Chapter 5 for arbitrary current excitations. An effective ac flux density is derived to simplify the core loss calculation with non-uniform field distribution. A sub-circuit for core loss simulation is established in LTSPICE that is capable of being integrated to the power stage simulation. Transient behavior and accurate simulation results from the LTSPICE matches very well with the FES results. An equivalent circuit for coupled windings is developed for inductors with significant fringing effect. The equivalent circuit is derived from a physical model that captures the flux paths by having a leakage inductor and two mutual inductors on the primary and secondary side. A mutual resistor is added to each side in parallel with one mutual inductor to model the winding loss with open circuit and phase-shift impact. Two time-varying resistors are employed to represent the core loss in the time-domain. The equivalent circuit is verified by both finite-element simulation (FES) and prototypes fabricated with flexible circuit.
Ph. D.

Magnetic flux continually emerges from the Sun, rising through the solar interior, emerging at the photosphere in the form of sunspots and expanding into the atmosphere. Observations of sunspot rotations have been reported for over a century and are often accompanied by solar eruptions and flaring activity. In this thesis, we present 3D numerical simulations of the emergence of twisted flux tubes from the uppermost layers of the solar interior, examining the rotational movements of sunspots in the photospheric plane. The basic experiment introduces the mechanism and characteristics of sunspot rotation by a clear calculation of rotation angle, vorticity, magnetic helicity and energy, whereby we find an untwisting of the interior portion of the field, accompanied by an injection of twist into the atmospheric field. We extend this model by altering the initial field strength and twist of the sub-photospheric tube. This comparison reveals the rotation angle, helicity and current show a direct dependence on field strength. An increase in field strength increases the rotation angle, the length of fieldlines extending into the atmosphere, and the magnetic energy transported to the atmosphere. The fieldline length is crucial as we predict the twist per unit length equilibrates to a lower value on longer fieldlines, and hence possesses a larger rotation angle. No such direct dependence is found when varying the twist but there is a clear ordering in rotation angle, helicity, and energy, with more highly twisted tubes undergoing larger rotation angles. We believe the final angle of rotation is reached when the system achieves a constant degree of twist along the length of fieldlines. By extrapolating the size of the modelled active region, we find rotation angles and rates comparable with those observed. In addition, we explore sunspot rotation caused by sub-photospheric velocities twisting the footpoints of flux tubes.

Le travail réalisé au cours de cette thèse concerne le développement du système de bobines de l'expérience n2EDM à l'Institut Paul Sherrer (PSI). Le but de cette expérience est de mettre en évidence de nouvelles sources de violation CP à travers la mesure du moment dipolaire électrique du neutron. L'actuelle limite supérieure sur la mesure de nEDM, $2.9 \cross 10^{-26}$ e.cm (90\% C.L.) à été obtenue par la collaboration RAL-Sussex-ILL en 2006.L'expérience n2EDM vise à améliorer d'un ordre de grandeur la sensibilité statistique en gardant sous contrôle les effets systématiques. Cela requiert la production d'un champ magnétique très uniforme. Les non-uniformités de ce dernier sont en effet responsable de la dépolarisation des neutrons et impliqués dans plusieurs effets systématiques.Dans le premier chapitre, les motivations physiques sont discutées.Le second chapitre décrit le principe de mesure de l'expérience n2EDM, ainsi que l'importance de l'uniformité du champ magnétique. Le chapitre s'achève par une présentation globale du dispositif expérimental.Le troisième chapitre présente le logiciel COMSOL et discute du design et des performances de la bobine B$_{0}$, en charge de la production du champ magnétique principal.Dans le quatrième chapitre, le système de bobines correctrices chargées de corriger les non-uniformités du champ magnétique et celles devant produire des gradients spécifiques sont présentées.Finalement, le cinquième et dernier chapitre présente l'étude des dipôles magnétiques localisés et de leur influence sur l'expérience
This work presents the design of the coils system developed for the n2EDM experiment at the Paul Sherrer Institute (PSI). The goal of this experiment is to reveal new sources of CP violation through the measurement of the neutron electric dipole moment. The current upper limit of the nEDM measurement, $2.9 \cross 10^{-26}$ e.cm (90\% C.L.) was achieved by the RAL-Sussex-ILL collaboration in 2006.The n2EDM experiment aims at improving by one order of magnitude the statistical sensitivity while keeping under control the systematics effects. It requires to produce a very uniform field, its non-uniformities being responsible of the neutron's depolarization and of severals systematic effects.In the first chapter, the theoretical motivation are discussed.The second chapter describes the measurement principle of the n2EDM experiment, as well as the importance of the magnetic field uniformity. This chapter ends by an overview of the apparatus.The third chapter introduces the COMSOL software and discuss the design and the performances of the B0 coil, in charge of the production of the main magnetic field.In the fourth chapter, the correcting coils used to suppress the non-uniformities of the magnetic field and the ones which produce specific gradients are presented.Finally, the fifth and last chapter talks about the study of localised magnetic dipoles and their influence on the experiment

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

Magnetic field permeates the solar atmosphere and plays a crucial role in the dynamics, energetics and structures observed. In particular, magnetic flux tubes provide the structure for coronal loops that extend from the solar surface into the corona. In this thesis, we present 3D numerical simulations examining the heating produced by reconnection between flux tubes driven by rotational footpoint motions. The basic model consists of two, initially aligned, flux tubes that are forced to interact by rotational driving velocities on the flux concentrations on the boundaries. A single, twisted current layer is created in the centre of the domain and strong, localised heating is produced. We extend this model by altering the number, distribution and strength of the sources, while maintaining the same total magnetic flux on the boundaries. The dynamical evolution and the resultant magnitude, distribution and timing of the heating events are examined for the different flux distributions. In all cases, the magnetic field is stressed by the boundary motions and a current grows within the domain. A comparison of cases with two and four sources shows that there are more locations of current concentrations, but with reduced maximum current density values, for the four source case. This produces weaker reconnection and less efficient heating. In addition, for the case with two sources, we also consider the effect of splitting up one of the sources into many smaller flux fragments. The evolution and heating are shown to be very similar to the two source case. The impact of increasing the strength of the background field between the flux tubes is also examined and we find that it delays and increases the strength of the heating, although by how much depends on the distribution of the flux sources.

Recently, the use of permanent magnets as magnetic field sources in biomedical applications has become widespread. However, usage of permanent magnets in magnetic resonance imaging (MRI) is limited due to their inhomogeneous magnetic field distributions. In this thesis, shape and geometry optimization of a magnet is performed. Moreover, placement of more than one magnet is optimized to obtain desired magnetic field distribution in specific region of space. However, obtained magnetic field distribution can not be used in the conventional MRI image reconstruction techniques. Consequently, an image reconstruction technique for MRI in inhomogeneous magnetic fields is developed. Apart from these, since any reconstruction technique requires signal data, an MRI simulator in inhomogeneous magnetic fields is constructed as a part of this thesis. Obtained results show that the theory developed in this thesis is valid. Consequently, new MRI devices that have permanent magnets as magnetic field sources can be constructed in the future.

The effect of an imposed magnetic field on the thermal convection between rigid plates heated from below under the influence of gravity is numerically simulated in a computational domain with periodic horizontal extent. The numerical technique is based on solenoidal basis functions satisfying the boundary conditions for both velocity and induced magnetic field. The expansion bases for the thermal field are also constructed to satisfy the boundary conditions. The governing partial differential equations are reduced to a system of ordinary differential equations governing the time evolution of the expansion coefficients under Galerkin projection onto the subspace spanned by the dual bases. In the process, the pressure term in the momentum equation is eliminated. The system validated in the linear regime is then used for some numerical experiments in the nonlinear regime.

Flux is continually emerging on the Sun, making its way from the solar interior up into the atmosphere. Emergence occurs on small-scales in the quiet Sun where magnetic fragments emerge, interact and cancel and on large-scales in active regions where magnetic fields emerge and concentrate to form sunspots. This thesis has been concerned with the large-scale emergence process and in particular the results from previous solar flux emergence modelling endeavours. Modelling uses numerical methods to evolve a domain representing simplified layers of the Sun’s atmosphere, within which the subsurface layer contains magnetic flux. The flux is initialised such that it will rises towards the surface at the start of the simulation. Once the flux reaches the solar surface, it can only emerge into the atmosphere if a magnetic buoyancy instability occurs, after which it expands rapidly both vertically and horizontally. The aim of this thesis is to test the robustness of these general findings from simulations to date upon the seed magnetic field. More explicitly, we have used three-dimensional numerical simulations to investigate how variations in the subsurface magnetic field modify the emergence process and the resulting atmospheric field. We initially consider a simple constant twist flux tube for the seed field and vary the tube’s magnetic field strength and degree of twist. Additionally, we have examined the effects of using non-constant twist flux tubes as the seed field by choosing two different profiles for the twist that are functions of the tube’s radius. Finally, we have investigated the effects of increasing the complexity of the seed field by positioning two flux tubes below the solar surface and testing two different configurations for the tubes. In both cases, the magnetic fields of the two tubes are such that, once the tubes come into contact with each other, reconnection occurs and a combined flux system is formed. From our investigations, we conclude that the general emergence results given by previous simulations are robust. However, for constant twist tubes with low field strength and twist, the buoyancy instability fails to be launched when the tubes reach the photosphere and they remain trapped in the low atmosphere. Similarly, when the non-constant twist profile results in a low tension force throughout the tube, we find that the buoyancy instability is not initialised.

Thesis (S.M.)--Massachusetts Institute of Technology, Dept. of Electrical Engineering and Computer Science, 2001.
Includes bibliographical references (leaves 120-125).
by Timothy A. Wagner.
S.M.

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Dissertacao (Mestrado)
IPEN/D
Instituto de Pesquisas Energeticas e Nucleares - IPEN/CNEN-SP

Aircraft have been used for the detection of submarines since World War II. The basic concept is to attach a sensor to the back of an aircraft. Since the aircraft is a moving metallic object, it is bound to generate a great deal of interference. Because of this, mathematical models and software have been developed to help filter out this interference and thus make the detection of the submarine easier. Normally, the engines of the aircraft are placed on the wings, quite far away from the sensor. However, for a maritime patrol system in development, the jet engines are placed at the rear of the airframe, generating the necessity to study whether or not they affect the performance of the sensor, which is the purpose of this thesis.   Several models were created, tested and simulated for the airframe and jet engines. One of each of these were then combined to create a simulation model for the complete aircraft. A jet engine model that included rotating machinery -- a possible source of magnetic interference -- was also created, but could not be added to the model for the complete aircraft. The magnetic interference was mathematically compensated for, removing the static interference, but not the interference during manoeuvres. The jet engine part of the complete aircraft model did not seem to generate a significant amount of magnetic interference compared to the airframe. An electric dipole, representing a submarine, was then added to the simulation. The data from that simulation was put through the mathematical model and distortions of a few~nT were noticeable during straight courses. The jet engine model that included rotating machinery yielded different results compared to the jet engine model in the complete aircraft model. They seemed to contain signals of higher frequency, which were however not detected by a frequency domain study or present during straight courses. It was thus concluded that using this particular engine model the submarine could probably still be detected if the course of the aircraft was kept straight, though further research is needed with more advanced models for the engine, in particular with regards to the rotating machinery.

In this thesis we investigated two major issues in astrophysical flows: the transport of magnetic fields in highly conducting fluids in the presence of turbulence, and the turbulence evolution and turbulent dynamo amplification of magnetic fields in collisionless plasmas. The first topic was explored in the context of star-formation, where two intriguing problems are highly debated: the requirement of magnetic flux diffusion during the gravitational collapse of molecular clouds in order to explain the observed magnetic field intensities in protostars (the so called \"magnetic flux problem\") and the formation of rotationally sustained protostellar discs in the presence of the magnetic fields which tend to remove all the angular momentum (the so called \"magnetic braking catastrophe\"). Both problems challenge the ideal MHD description, usually expected to be a good approximation in these environments. The ambipolar diffusion, which is the mechanism commonly invoked to solve these problems, has been lately questioned both by observations and numerical simulation results. We have here investigated a new paradigm, an alternative diffusive mechanism based on fast magnetic reconnection induced by turbulence, termed turbulent reconnection diffusion (TRD). We tested the TRD through fully 3D MHD numerical simulations, injecting turbulence into molecular clouds with initial cylindrical geometry, uniform longitudinal magnetic field and periodic boundary conditions. We have demonstrated the efficiency of the TRD in decorrelating the magnetic flux from the gas, allowing the infall of gas into the gravitational well while the field lines migrate to the outer regions of the cloud. This mechanism works for clouds starting either in magnetohydrostatic equilibrium or initially out-of-equilibrium in free-fall. We estimated the rates at which the TRD operate and found that they are faster when the central gravitational potential is higher. Also we found that the larger the initial value of the thermal to magnetic pressure ratio (beta) the larger the diffusion process. Besides, we have found that these rates are consistent with the predictions of the theory, particularly when turbulence is trans- or super-Alfvénic. We have also explored by means of 3D MHD simulations the role of the TRD in protostellar disks formation. Under ideal MHD conditions, the removal of angular momentum from the disk progenitor by the typically embedded magnetic field may prevent the formation of a rotationally supported disk during the main protostellar accretion phase of low mass stars. Previous studies showed that an enhanced microscopic diffusivity of about three orders of magnitude larger than the Ohmic diffusivity would be necessary to enable the formation of a rotationally supported disk. However, the nature of this enhanced diffusivity was not explained. Our numerical simulations of disk formation in the presence of turbulence demonstrated the efficiency of the TRD in providing the diffusion of the magnetic flux to the envelope of the protostar during the gravitational collapse, thus enabling the formation of rotationally supported disks of radius ~ 100 AU, in agreement with the observations. The second topic of this thesis has been investigated in the framework of the plasmas of the intracluster medium (ICM). The amplification and maintenance of the observed magnetic fields in the ICM are usually attributed to the turbulent dynamo action which is known to amplify the magnetic energy until close equipartition with the kinetic energy. This is generally derived employing a collisional MHD model. However, this is poorly justified a priori since in the ICM the ion mean free path between collisions is of the order of the dynamical scales, thus requiring a collisionless-MHD description. We have studied here the turbulence statistics and the turbulent dynamo amplification of seed magnetic fields in the ICM using a single-fluid collisionless-MHD model. This introduces an anisotropic thermal pressure with respect to the direction of the local magnetic field and this anisotropy modifies the MHD linear waves and creates kinetic instabilities. Our collisionless-MHD model includes a relaxation term of the pressure anisotropy due to the feedback of the mirror and firehose instabilities. We performed 3D numerical simulations of forced transonic turbulence in a periodic box mimicking the turbulent ICM, assuming different initial values of the magnetic field intensity and different relaxation rates of the pressure anisotropy. We showed that in the high beta plasma regime of the ICM where these kinetic instabilities are stronger, a fast anisotropy relaxation rate gives results which are similar to the collisional-MHD model in the description of the statistical properties of the turbulence. Also, the amplification of the magnetic energy due to the turbulent dynamo action when considering an initial seed magnetic field is similar to the collisional-MHD model, particularly when considering an instantaneous anisotropy relaxation. The models without any pressure anisotropy relaxation deviate significantly from the collisional-MHD results, showing more power in small-scale fluctuations of the density and velocity field, in agreement with a significant presence of the kinetic instabilities; however, the fluctuations in the magnetic field are mostly suppressed. In this case, the turbulent dynamo fails in amplifying seed magnetic fields and the magnetic energy saturates at values several orders of magnitude below the kinetic energy. It was suggested by previous studies of the collisionless plasma of the solar wind that the pressure anisotropy relaxation rate is of the order of a few percent of the ion gyrofrequency. The present study has shown that if this is also the case for the ICM, then the models which best represent the ICM are those with instantaneous anisotropy relaxation rate, i.e., the models which revealed a behavior very similar to the collisional-MHD description.
Nesta tese, investigamos dois problemas chave relacionados a fluidos astrofísicos: o transporte de campos magnéticos em plasmas altamente condutores na presença de turbulência, e a evolução da turbulência e amplificação de campos magnéticos pelo dínamo turbulento em plasmas não-colisionais. O primeiro tópico foi explorado no contexto de formação estelar, onde duas questões intrigantes são intensamente debatidas na literatura: a necessidade da difusão de fluxo magnético durante o colapso gravitacional de nuvens moleculares, a fim de explicar as intensidades dos campos magnéticos observadas em proto-estrelas (o denominado \"problema do fluxo magnético\"), e a formação de discos proto-estelares sustentados pela rotação em presença de campos magnéticos, os quais tendem a remover o seu momento angular (a chamada \"catástrofe do freamento magnético\"). Estes dois problemas desafiam a descrição MHD ideal, normalmente empregada para descrever esses sistemas. A difusão ambipolar, o mecanismo normalmente invocado para resolver estes problemas, vem sendo questionada ultimamente tanto por observações quanto por resultados de simulações numéricas. Investigamos aqui um novo paradigma, um mecanismo de difusão alternativo baseado em reconexão magnética rápida induzida pela turbulência, que denominamos reconexão turbulenta (TRD, do inglês turbulent reconnection diffusion). Nós testamos a TRD através de simulações numéricas tridimensionais MHD, injetando turbulência em nuvens moleculares com geometria inicialmente cilíndrica, permeadas por um campo magnético longitudinal e fronteiras periódicas. Demonstramos a eficiência da TRD em desacoplar o fluxo magnético do gás, permitindo a queda do gás no poço de potencial gravitacional, enquanto as linhas de campo migram para as regiões externas da nuvem. Este mecanismo funciona tanto para nuvens inicialmente em equilíbrio magneto-hidrostático, quanto para aquelas inicialmente fora de equilíbrio, em queda livre. Nós estimamos as taxas em que a TRD opera e descobrimos que são mais rápidas quando o potencial gravitacional é maior. Também verificamos que quanto maior o valor inicial da razão entre a pressão térmica e magnética (beta), mais eficiente é o processo de difusão. Além disto, também verificamos que estas taxas são consistentes com as previsões da teoria, particularmente quando a turbulência é trans- ou super-Alfvénica. Também exploramos por meio de simulações MHD 3D a influência da TRD na formação de discos proto-estelares. Sob condições MHD ideais, a remoção do momento angular do disco progenitor pelo campo magnético da nuvem pode evitar a formação de discos sustentados por rotação durante a fase principal de acreção proto-estelar de estrelas de baixa massa. Estudos anteriores mostraram que uma super difusividade microscópica aproximadamente três ordens de magnitude maior do que a difusividade ôhmica seria necessária para levar à formação de um disco sustentado pela rotação. No entanto, a natureza desta super difusividade não foi explicada. Nossas simulações numéricas da formação do disco em presença de turbulência demonstraram a eficiência da TRD em prover a diffusão do fluxo magnético para o envelope da proto-estrela durante o colapso gravitacional, permitindo assim a formação de discos sutentados pela rotação com raios ~ 100 UA, em concordância com as observações. O segundo tópico desta tese foi abordado no contexto dos plasmas do meio intra-aglomerado de galáxias (MIA). A amplificação e manutenção dos campos magnéticos observados no MIA são normalmente atribuidas à ação do dínamo turbulento, que é conhecidamente capaz de amplificar a energia magnética até valores próximos da equipartição com a energia cinética. Este resultado é geralmente derivado empregando-se um modelo MHD colisional. No entanto, isto é pobremente justificado a priori, pois no MIA o caminho livre médio de colisões íon-íon é da ordem das escalas dinâmicas, requerendo então uma descrição MHD não-colisional. Estudamos aqui a estatística da turbulência e a amplificação por dínamo turbulento de campos magnéticos sementes no MIA, usando um modelo MHD não-colisional de um único fluido. Isto indroduz uma pressão térmica anisotrópica com respeito à direção do campo magnético local. Esta anisotropia modifica as ondas MHD lineares e cria instabilidades cinéticas. Nosso modelo MHD não-colisional inclui um termo de relaxação da anisotropia devido aos efeitos das instabilidades mirror e firehose. Realizamos simulações numéricas 3D de turbulência trans-sônica forçada em um domínio periódico, mimetizando o MIA turbulento e considerando diferentes valores iniciais para a intensidade do campo magnético, bem como diferentes taxas de relaxação da anisotropia na pressão. Mostramos que no regime de plasma com altos valores de beta no MIA, onde estas instabilidades cinéticas são mais fortes, uma rápida taxa de relaxação da anisotropia produz resultados similares ao modelo MHD colisional na descrição das propriedades estatísticas da turbulência. Além disso, a amplificação da energia mangética pela ação do dínamo turbulento quando consideramos um campo magnético semente, é similar ao modelo MHD colisional, particularmente quando consideramos uma relaxação instantânea da anisotropia. Os modelos sem qualquer relaxação da anisotropia de pressão mostraram resultados que se desviam significativamente daqueles do MHD colisional, mostrando mais potências nas flutuações de pequena escala da densidade e velocidade, em concordância com a presença significativa das instabilidades cinéticas nessas escalas; no entanto, as flutuações do campo magnético são, em geral, suprimidas. Neste caso, o dínamo turbulento também falha em amplificar campos magnéticos sementes e a energia magnética satura em valores bem abaixo da energia cinética. Estudos anteriores do plasma não-colisional do vento solar sugeriram que a taxa de relaxação da anisotropia na pressão é da ordem de uma pequena porcentagem da giro-frequência dos íons. O presente estudo mostrou que, se este também é o caso para o MIA, então os modelos que melhor representam o MIA são aqueles com taxas de relaxação instantâneas, ou seja, os modelos que revelaram um comportamento muito similar à descrição MHD colisional.

Melt flow plays an important role in directional solidification of multicrystalline silicon influencing the temperature field and the crystallization interface as well as the transport of impurities. This work investigates the potential of a traveling magnetic field (TMF) for an active control of the melt flow. A system of 3D numerical models was developed and adapted based on open-source software for calculations of Lorentz force, melt flow, and related phenomena. Isothermal and non-isothermal model experiments with a square GaInSn melt were used to validate the numerical models by direct velocity measurements. Several new 3D flow structures of turbulent TMF flows were observed for different melt heights. Further numerical parameter studies carried out for silicon melts showed that already a weak TMF-induced Lorentz force can stir impurities near to the complete mixing limit. Simultaneously, the deformed temperature field leads to an increase of the deflection of crystallization interface, which may exhibit a distinct asymmetry. The numerical results of this work were implemented in a research-scale silicon crystallization furnace. Scaling laws for various phenomena were derived allowing a limited transfer of the results to the industrial scale.

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior
O estudo de discos magnéticos com a configuração de vórtices magnéticos tem atraído grande interesse científico recentemente. Nessa estrutura os spins formam circuitos fechados no plano e, próximo ao centro do disco, se alinham perpendicularmente ao plano de forma a reduzir a densidade de energia de troca. O grande potencial de aplicação de vórtices magnéticos como, por exemplo, em memórias magnéticas e nanopartículas para o tratamento de câncer, chama a atenção para a investigação das condições de estabilidade e o controle de suas propriedades. Neste trabalho, estudamos a alteração que dois tipos diferentes de anisotropia provocam nas propriedades de vórtices através de medidas de Microscopia de Força Magnética (MFM) e simulações micromagnéticas utilizando o código OOMMF (NIST) que aplica a equação de Landau-Lifshitz-Gilbert para simular a configuração de spin e calcular a energia e a magnetização de microestruturas. A primeira parte do trabalho envolveu o estudo da influência da anisotropia magnetocristalina planar na estabilidade de vórtices magnéticos em discos de Co60Fe40 em relação a discos de permalloy, que possui anisotropia magnetocristalina nula. Os resultados de simulação micromagnética para discos com diâmetros entre 0,5 e 8 m mostraram que a anisotropia favorece o alinhamento dos spins e a divisão da estrutura em domínios, reduzindo a estabilidade do vórtice. Os resultados foram comprovados experimentalmente em medidas de MFM de discos de Co60Fe40 com diâmetros entre 2 e 8 m. Na segunda parte do trabalho foi estudada a influência do fenômeno de exchange bias na dinâmica de vórtices magnéticos. Para isso foram realizadas simulações de discos de Permalloy/Fe50Mn50 com diâmetro de 0,5 m variando o acoplamento magnético entre as camadas. As simulações de curvas de histerese mostraram que o acoplamento aumenta a estabilidade dos vórtices. Nas simulações de relaxação foi observado que devido ao exchange bias o movimento girotrópico do núcleo apresenta uma frequência variável que aumenta com o tempo, o que não acontece na ausência de exchange bias. Já nas simulações em que os discos estão sujeitos a um campo magnético girante foi observado que a velocidade crítica em que a polaridade do vórtice é invertida aumenta com o aumento do acoplamento e com o aumento da frequência do campo. Essa velocidade pode ser escolhida em uma ampla faixa escolhendo os valores do acoplamento magnético e da frequência de oscilação. Portanto é possível controlar a velocidade crítica de inversão da polaridade de vórtices magnéticos através do fenômeno de exchange bias.
The study of magnetic dots with magnetic vortex spin configuration has recently attracted great scientific interest. In this structure, the spins form closed circuits in the plane of the magnetic dot and, near the center, align perpendicularly to the plane in order to reduce exchange energy density. The great potential of applications of magnetic vortices (as for example magnetic memories and nanoparticles for cancer treatment) draws attention for the investigation of the stability conditions for the vortex configuration. In the case of soft ferromagnetic materials in micron and submicron scales, small changes in shape, size and materials anisotropy can modify the energy equilibrium. In this work, we studied the change of vortex proprieties in microsized dots due to two different types of anisotropy using the code OOMMF (NIST) that applies the Landau-Lifshitz-Gilbert equation to simulate the spin configuration and compute the energy and magnetization of microstructures. These results were compared to Magnetic Force Microscopy (MFM) investigations of the magnetic configuration in microsized dots prepared by lithographic process. In the first part, we studied by numerical simulation the influence of planar magnetocrystaline anisotropy in Co60Fe40 disks and compare to permalloy disks, material that shows zero magnetocrystalline anisotropy. The results for disks with diameters between 0.5 and 8 m showed that the anisotropy favors spins alignment and domains division, reducing vortex stability. The results for Co60Fe40 disks with diameters between 2 and 8 m were verify experimentally by MFM measurements. In the second part, we studied the influence of exchange bias in the magnetic vortex dynamics. A series of micromagnetic simulations for Permalloy/Fe50Mn50 disks with 0.5 m of diameter was done varying the magnetic coupling constant between the layers. The hysteresis simulations showed that the vortex stability increases with the coupling constant. In relaxation simulations we observed that the gyrotropic movement has a variable frequency that increases with time, which is not observed when exchange bias is absent. Under a rotating magnetic field, the critical velocity for vortex polarity reversion increases with the coupling constant and frequency. Our results show that the critical velocity can be adjusted in a wide range by selecting the magnetic coupling constant and the oscillating frequency, i.e., it is possible to control the critical velocity for vortex polarity inversion through the exchange bias coupling.

As a magnetic therapy apparatus with medical benefits, the Unipolar Pulse Electromagnetic Field (UPEMF) apparatus is presented to produce unipolar pulsed magnetic waveforms with an intensity, shape, and frequency that meet medical requirements. The unipolar pulse is the most significant advantage, as the implemented apparatus is considered to be the first improvement in Pulse Electromagnetic Fields (PEMFs). The magnetic field is generated by a specially designed electromagnetic unit. In this unit, an electromagnet is concentrated by a designed concentrator to strengthen the magnetic field at the north pole and weaken the field on the opposite end. An electromagnetic shield is adopted to eliminate the effects of the south pole but allow the output from the north pole. Excited by a designed pulsed waveform generator, the electromagnetic unit generates a strong alternating-current magnetic field. In my work, the detailed design and development of the electromagnetic unit for UPEMF are introduced, therein being modeled and tested using Finite Element Method simulations. The model is characterized mathematically in three parts: the concentrator, the electromagnetic shield, and the overall unit. The testing and performance measurements of the actual Unipolar Pulse Electromagnetic Field apparatus are achieved using a Gauss meter and oscilloscope.

Magneto-sensitive Elastomere sind Verbundwerkstoffe, die hauptsächlich aus einer Elastomermatrix bestehen, in der magnetischen Partikeln dispergiert sind. Ein ins magnetosensitive Elastomer eingreifende Magnetfeld bewirkt Änderungen der Eigenschaften dieses Materials. Diese Qualität macht die MSE zu einer Option mit hohem Potenzial für Soft Robotics- Anwendungen. Für die Realisierung dieser Masterarbeit wurden MSE-Proben aus einer Elastomermatrix, Silikonöl und Carbonyleisenpartikeln hergestellt. Tests wurden durchgeführt, um Verbesserungen zu entwickeln, die sich auf Soft-Robot- Anwendungen konzentrieren, insbesondere bei Endeffektoren. In dieser Arbeit wurden die Eigenschaften von magneto-sensitive Elastomerproben in Abwesenheit und Gegenwart eines Magnetfeldes experimentell untersucht. Die untersuchungen wurden mittels eines Magnetfeldes realisiert, dass durch einen Permanentmagneten induziert wurde. Um die Intensität zu varriieren, wurde der Permanetmagent in unterschiedlichen Abständen zur Probe positioniert. Die experimentell erhaltenen Ergebnisse wurden verwendet, um den Einfluss der MF über der MSE zu verstehen und ein geeignetes Materialmodell unter Verwendung der Finite-Elemente-Methode zu entwickeln.
Magneto-sensitive elastomers are composite materials made mainly of an elastomer matrix, in which magnetic particles are dispersed. A magnetic field applied in the magneto sensitive elastomers achieves changes in the properties of this material. This quality turns the magneto-sensitive elastomers in an option with high potential in soft robotics applications. In the present thesis, samples of magneto-sensitive elastomers containing an elastomeric matrix, silicone oil and carbonyl iron particles were produced. Tests were performed in order to develop improvements focused on soft robotic applications, particularly in end effectors. In this thesis, the properties of magneto-sensitive elastomers samples have been experimentally studied in the absence and presence of a magnetic field. The magnetic field was induced by a permanent magnet that was moved at different distances from the sample to change the intensity of the magnetic field. The results obtained by experiments were used to understand the influence of the magnetic field on the magneto-sensitive elastomer and to obtain a suitable material model using finite element method.
Los elastómeros magneto-sensibles son materiales compuestos hechos principalmente de una matriz de elastómero, en la que se dispersan las partículas magnéticas. Un campo magnético aplicado en los elastómeros magneto-sensibles logra cambios en las propiedades de este material. Esta cualidad convierte los elastómeros magneto-sensibles en una opción con alto potencial en aplicaciones de robótica blanda. En la presente tesis, se fabricaron muestras de elastómeros magneto-sensibles que contenían una matriz elastomérica, aceite de silicona y partículas de hierro carbonilo. Se realizaron pruebas para desarrollar mejoras enfocadas en aplicaciones de robótica blanda, particularmente en efectores finales. En esta tesis, las propiedades de las muestras de elastómeros magneto-sensibles han sido estudiadas experimentalmente en ausencia y presencia de un campo magnético. El campo magnético fue inducido por un imán permanente que se movió a diferentes distancias de la muestra para cambiar la intensidad de este campo magnético. Los resultados obtenidos por experimentos se utilizaron para comprender la influencia del campo magnético en el elastómero magneto sensible y para obtener un modelo de material adecuado utilizando el método de elementos finitos.
Tesis

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Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)
Universidade Estadual Paulista (UNESP)
O estudo do efeito do campo magnético sobre o processo de implantação iônica por imersão em plasma (3IP) é de grande interesse para o tratamento de materiais. Sendo 3IP uma técnica relativamente nova e de grande relevância para diversas aplicações tecnológicas é importante que ela seja pesquisada e analisada detalhadamente. A aplicação de um campo magnético estático, transversal em relação ao campo elétrico formado durante este processo produz um sistema de campos cruzados ExB. Este sistema de campos cruzados gera um aumento significativo da densidade de plasma na vizinhança do alvo, resultando num maior corrente de implantação, e conseqüentemente um tratamento mais rápido e uma dose retida mais alta em relação ao processo 3IP convencional. Neste trabalho, analisamos mediante simulação numérica, o efeito da distribuição do campo magnético axial no processo 3IP. O campo magnético é produzido por um par de bobinas instaladas fora da câmara de vácuo cujos raios e distância de separação são variadas. Encontramos que a densidade de corrente de implantação depende essencialmente da configuração do campo magnético. Assim, com uma adequada configuração das bobinas (10,0 cm de raio e 42,0 cm de separação) obtivemos uma densidade de corrente quase uniforme de aproximadamente 1,5 mA/cm2 que é 1.5 vezes maior em relação ao caso do sistema 3IP sem campo magnético. O efeito da tensão aplicada assim como da pressão do gás sobre o plasma no processo 3IP é também investigado. O sistema 3IP com campos ExB cruzados é estudado utilizando a técnica de simulação numérica em duas dimensões. Esta simulação é realizada com o código computacional KARAT que emprega o algoritmo “particle-in-cell” (PIC) para simular o movimento de partículas carregadas no campo eletromagnético.
Detailed investigation of the effect of magnetic field on the process of plasma immersion ion implantation (PIII) is of great interest for the material treatment. Being a relatively novel and of great relevance for technological applications technique, the PIII demands further research and careful analysis. The application of static magnetic field, transversal in respect to the electric field established during this process, produces a system of crossed fields ExB. This system of crossed fields promotes an increase of the plasma density, resulting in higher implantation current, and consequently in a shorter treatment time and a higher retained dose in comparison to the conventional PIII process. In this work we have analyzed by means of numerical simulation the effect of magnetic field distribution on the PIII processing. The magnetic field is produced by a pair of external coils, whose radii and separation distance were varied. We found that the density of the implantation current essentially depends on the magnetic field configuration. Thus, with an appropriate configuration of the coils (10,0 cm radius and separation of 42,0 cm) we have obtained an almost uniform current density of approximately 1,5 mA/cm2 that is 1,5 times bigger in relation to the case PIII without magnetic field. The effect of the target bias as well as the gas pressure on the ion current incident on the target is also investigated. The PIII system with crossed ExB fields has been studied using two-dimensional numerical simulation. The simulation is accomplished by the computer code KARAT which employs the particle-in-cell (PIC) algorithm for simulating the movement of charged particles in the electromagnetic field.

A magnetic fluid system could potentially replace mechanically moving parts in a satellite as a means of increasing system reliability and mission lifetime, but rather than a standard ferrofluid with magnetic particles, liquid oxygen (LOX) may be a more adequate working fluid. As a pure paramagnetic cryogen, LOX is already heavily used in space, but still requires basic research before being integrated into system development. The objectives of the research conducted were to verify LOX as a magnetic working fluid through experiment and establish a theoretical model to describe its behavior. This dissertation presents the theoretical, experimental, and numerical results of a slug of LOX being pulsed by a 1.1 T solenoid in a quartz tube with an inner diameter of 1.9 mm. The slug oscillated about the solenoid at 6-8 Hz, producing a pressure change of up to 1.2 kPa. System efficiency based on the Mason number was also studied for various geometric setups, and, using a one-dimensional, finite-differenced model in Matlab 2008a, the numerical analyses confirmed the theoretical model. The research provides groundwork for future applied studies with complex designs.

Black hole-neutron star (BH-NS) mergers are promising candidates for the progenitors of short-duration gamma-ray bursts (GRBs). With the right initial conditions, the neutron star becomes tidally disrupted, eventually forming a dense, accreting disk around the black hole. The thermal energy of this black hole-disk system can be extracted via neutrino processes, while the spin energy of the black hole can be extracted via magnetic processes. Either (or even a combination of these) processes could feasibly power a relativistic jet with energy ≥~ 10 49 erg and duration ≤~ 2 s, hence producing a short-duration GRB. In this thesis, we investigate BH-NS mergers with three-dimensional, pseudo-Newtonian simulations. We use the simulation code Charybdis, which uses a dimensionally-split, reconstruct-solve-average scheme (i.e. using Riemann solvers) to solve the Euler equations of hydrodynamics. Although the code is based on a Newtonian framework, it includes pseudo- Newtonian approximations of local gravitational wave effects and the innermost stable circular orbit of the BH, which are both general relativistic phenomena. The code also includes the effects of global neutrino emission, shear viscosity and self-gravity. This thesis comprises two main projects. The first project is a parameter study of the equation of state, which encapsulates the relationship between the pressure of a fluid and its other thermodynamic properties. Although the EOS is well understood at low densities, it is yet to be constrained at supranuclear densities, and so must be treated as a parameter in numerical studies of BH-NS mergers. We present simulations using three existing EOSs, in order to investigate their effect on the merger dynamics. We find that the EOS strongly influences the fate of the NS, the properties of the accretion disk, and the neutrino emission. In the second project, we begin upgrading Charybdis to include magnetic field effects, in order to investigate the magnetic processes described above. We implement existing reconstruction and Riemann solver algorithms for the equations of magnetohydrodynamics, and present 1D tests to compare them. When modelling magnetic fields in more than one dimension, we must also deal with the divergence-free condition, ∇. B = 0. We develop a new constrained transport algorithm to ensure our code maintains this condition, and present 2D tests to confirm its accuracy. This algorithm has many advantages over existing ones, including easier implementation, greater computational efficiency and better parallelisation. Finally, we present preliminary tests that use these algorithms in simulations of BH-NS mergers.

When an electrically conducting fluid moves through a magnetic field, fluid mechanics and electromagnetism are coupled.

This interaction is the object of magnetohydrodynamics, a discipline which covers a wide range of applications, from electromagnetic processing to plasma- and astro-physics.

In this dissertation, the attention is restricted to turbulent liquid metal flows, typically encountered in steel and aluminium industries. Velocity measurements in such flows are extremely challenging because liquid metals are opaque, hot and often corrosive. Therefore, non-intrusive measurement devices are essential. One of them is the Lorentz force flowmeter. Its working principle is based on the generation of a force acting on a charge, which moves in a magnetic field. Recent studies have demonstrated that this technique can measure efficiently the mean velocity of a liquid metal. In the existing devices, however, the measurement depends on the electrical conductivity of the fluid.

In this work, a novel version of this technique is developed in order to obtain measurements that are independent of the electrical conductivity. This is particularly appealing for metallurgical applications, where the conductivity often fluctuates in time and space. The study is entirely numerical and uses a flexible computational method, suitable for industrial flows. In this framework, the cost of numerical simulations increases drastically with the level of turbulence and the geometry complexity. Therefore, the simulations are commonly unresolved. Large eddy simulations are then very promising, since they introduce a subgrid model to mimic the dynamics of the unresolved turbulent eddies.

The first part of this dissertation focuses on the quality and reliability of unresolved numerical simulations. The attention is drawn on the ambiguity that may arise when interpretating the results. Owing to coarse resolutions, numerical errors affect the performances of the discrete model, which in turn looses its physical meaning. In this work, a novel implementation of the turbulent strain rate appearing in the models is proposed. As opposed to its usual discretisation, the present strain rate is in accordance with the discrete equations of motion. Two types of flow are considered: decaying turbulence located far from boundaries, and turbulent flows between two parallel and infinite walls. Particular attention is given to the balance of resolved kinetic energy, in order to assess the role of the model.

The second part of this dissertation deals with a novel version of Lorentz force flowmeters, consisting in one or two coils placed around a circular pipe. The forces acting on each coil are recorded in time as the liquid metal flows through the pipe. It is highlighted that the auto- or cross-correlation of these forces can be used to determine the flowrate. The reliability of the flowmeter is first investigated with a synthetic velocity profile associated to a single vortex ring, which is convected at a constant speed. This configuration is similar to the movement of a solid rod and enables a simple analysis of the flowmeter. Then, the flowmeter is applied to a realistic three-dimensional turbulent flow. In both cases, the influence of the geometrical parameters of the coils is systematically assessed.
Doctorat en Sciences
info:eu-repo/semantics/nonPublished

Turbulent magnetic fields are ubiquitous in space physics and astrophysics. The influence of magnetic turbulence on the motions of charged particles contains the essential physics of the transport and acceleration of energetic charged particles in the heliosphere, which is to be explored in this thesis. After a brief introduction on the energetic charged particles and magnetic fields in the heliosphere, the rest of this dissertation focuses on three specific topics: 1. the transport of energetic charged particles in the inner heliosphere, 2. the acceleration of ions at collisionless shocks, and 3. the acceleration of electrons at collisionless shocks. We utilize various numerical techniques to study these topics. In Chapter 2 we study the propagation of charged particles in turbulent magnetic fields similar to the propagation of solar energetic particles in the inner heliosphere. The trajectories of energetic charged particles in the turbulent magnetic field are numerically integrated. The turbulence model includes a Kolmogorov-like magnetic field power spectrum containing a broad range of scales from those that lead to large-scale field-line random walk to small scales leading to resonant pitch-angle scattering of energetic particles. We show that small-scale variations in particle intensities (the so-called "dropouts") and velocity dispersions observed by spacecraft can be reproduced using this method. Our study gives a new constraint on the error of "onset analysis", which is a technique commonly used to infer information about the initial release of energetic particles. We also find that the dropouts are rarely produced in the simulations using the so-called "two-component" magnetic turbulence model (Matthaeus et al., 1990). The result questions the validity of this model in studying particle transport. In the first part of Chapter 3 we study the acceleration of ions in the existence of turbulent magnetic fields. We use 3-D self-consistent hybrid simulations (kinetic ions and fluid electrons) to investigate the acceleration of low-energy particles (often termed as "injection problem") at parallel shocks. We find that the accelerated particles always gain the first amount of energy by reflection and acceleration at the shock layer. The protons can move off their original field lines in the 3-D electric and magnetic fields. The results are consistent with the acceleration mechanism found in previous 1-D and 2-D simulations. In the second part of Chapter 3, we use a stochastic integration method to study diffusive shock acceleration in the existence of large-scale magnetic variations. We show that the 1-D steady state solution of diffusive shock acceleration can be significantly modified in this situation. The results suggest that the observations of anomalous cosmic rays by Voyager spacecraft can be explained by a 2-D shock that includes the large-scale magnetic field variations. In Chapter 4 we study electron acceleration at a shock passing into a turbulent magnetic field by using a combination of hybrid simulations and test-particle electron simulations. We find that the acceleration of electrons is greatly enhanced by including the effect of large-scale magnetic turbulence. Since the electrons mainly follow along the magnetic lines of force, the large-scale braiding of field lines in space allows the fast-moving electrons interacting with the shock front multiple times. Ripples in the shock front occurring at various scales also contribute to the acceleration by mirroring the electrons. Our calculation shows that this process favors electron acceleration at perpendicular shocks. We discuss the application of this process in interplanetary shocks and flare termination shocks. We also discuss the implication of this study to solar energetic particles (SEPs) by comparing the acceleration of electrons with that of protons. The intensity correlation of electrons and ions in SEP events indicates that perpendicular or quasi-perpendicular shocks play an important role in accelerating charged particles. In Chapter 5 we summarize the results of this thesis and discuss possible future work.

Orientador: Konstantin Georgiev Kostov
Banca: Joaquim José Barroso de Castro
Banca: Mario Ueda
Resumo: O estudo do efeito do campo magnético sobre o processo de implantação iônica por imersão em plasma (3IP) é de grande interesse para o tratamento de materiais. Sendo 3IP uma técnica relativamente nova e de grande relevância para diversas aplicações tecnológicas é importante que ela seja pesquisada e analisada detalhadamente. A aplicação de um campo magnético estático, transversal em relação ao campo elétrico formado durante este processo produz um sistema de campos cruzados ExB. Este sistema de campos cruzados gera um aumento significativo da densidade de plasma na vizinhança do alvo, resultando num maior corrente de implantação, e conseqüentemente um tratamento mais rápido e uma dose retida mais alta em relação ao processo 3IP convencional. Neste trabalho, analisamos mediante simulação numérica, o efeito da distribuição do campo magnético axial no processo 3IP. O campo magnético é produzido por um par de bobinas instaladas fora da câmara de vácuo cujos raios e distância de separação são variadas. Encontramos que a densidade de corrente de implantação depende essencialmente da configuração do campo magnético. Assim, com uma adequada configuração das bobinas (10,0 cm de raio e 42,0 cm de separação) obtivemos uma densidade de corrente quase uniforme de aproximadamente 1,5 mA/cm2 que é 1.5 vezes maior em relação ao caso do sistema 3IP sem campo magnético. O efeito da tensão aplicada assim como da pressão do gás sobre o plasma no processo 3IP é também investigado. O sistema 3IP com campos ExB cruzados é estudado utilizando a técnica de simulação numérica em duas dimensões. Esta simulação é realizada com o código computacional KARAT que emprega o algoritmo "particle-in-cell" (PIC) para simular o movimento de partículas carregadas no campo eletromagnético.
Abstract: Detailed investigation of the effect of magnetic field on the process of plasma immersion ion implantation (PIII) is of great interest for the material treatment. Being a relatively novel and of great relevance for technological applications technique, the PIII demands further research and careful analysis. The application of static magnetic field, transversal in respect to the electric field established during this process, produces a system of crossed fields ExB. This system of crossed fields promotes an increase of the plasma density, resulting in higher implantation current, and consequently in a shorter treatment time and a higher retained dose in comparison to the conventional PIII process. In this work we have analyzed by means of numerical simulation the effect of magnetic field distribution on the PIII processing. The magnetic field is produced by a pair of external coils, whose radii and separation distance were varied. We found that the density of the implantation current essentially depends on the magnetic field configuration. Thus, with an appropriate configuration of the coils (10,0 cm radius and separation of 42,0 cm) we have obtained an almost uniform current density of approximately 1,5 mA/cm2 that is 1,5 times bigger in relation to the case PIII without magnetic field. The effect of the target bias as well as the gas pressure on the ion current incident on the target is also investigated. The PIII system with crossed ExB fields has been studied using two-dimensional numerical simulation. The simulation is accomplished by the computer code KARAT which employs the particle-in-cell (PIC) algorithm for simulating the movement of charged particles in the electromagnetic field.
Mestre

This dissertation addresses the problem of elevation of the T wave of an electrocardiogram (ECG) signal in the magnetic resonance imaging (MRI). In the MRI, due to the strong static magnetic field the interaction of the blood flow with this strong magnetic field induces a voltage in the body. This voltage appears as a superimposition at the locus of the T wave of the ECG signal. This looses important information required by the doctors to interpret the ST segment of the ECG and detect diseases such as myocardial infarction. This dissertation aims at finding a solution to the problem of elevation of the T wave of an ECG signal in the MRI. The first step is to simulate the entire situation and obtain the magnetic field dependent T wave elevation. This is achieved by building a model of the aorta and simulating the blood flow in it. This model is then subjected to a static magnetic field and the surface potential on the thorax is measured to observe the T wave elevation. The various parameters on which the T wave elevation is dependent are then analyzed. Different approaches are used to reduce this T wave elevation problem. The direct approach aims at computing the magnitude of T wave elevation using magneto-hydro-dynamic equations. The indirect approach uses digital signal processing tools like the least mean square adaptive filter to remove the T wave elevation and obtain artifact free ECG signal in the MRI. Excellent results are obtained from the simulation model. The model perfectly simulates the ECG signal in the MRI at all the 12 leads of the ECG. These results are compared with ECG signals measured in the MRI. A simulation package is developed in MATLAB based on the simulation model. This package is a graphical user interface allowing the user to change the strength of magnetic field, the radius of the aorta and the orientation of the aorta with respect to the heart and observe the ECG signals with the elevation at the 12 leads of the ECG. Also the artifacts introduced due to the magnetic field can be removed by the least mean square adaptive filter. The filter adapts the ECG signal in the MRI to the ECG signal of the patient outside the MRI. Before the adaptation, the heart rate of the ECG outside the MRI is matched to the ECG in the MRI by interpolation or decimation. The adaptive filter works excellently to remove the T wave artifacts. When the cardiac output of the patient changes, the simulation model is used along with the adaptive filter to obtain the artifact free ECG signal.
Ph.D.
School of Electrical Engineering and Computer Science
Engineering and Computer Science
Electrical Engineering PhD

Presented diploma thesis deals with development of the autonomous electric energy source for Health and Usage Monitoring Systems placed at the rear part of a helicopter. Firstly, the HUMS systems were described briefly and the research of available energy sources was made after that. After that, the magnetic properties of the materials were described with the special focus on the permanent magnets. The draft also includes the creation of model of the magnetic field using the final element method. Prototype was assembled and the other design solutions were evaluated. The evaluation of various designs passed in the use of SOMA optimization algorithms. The generator is followed by the draft of the electronics, which streamlines and regulates a voltage supplied by the generator. At the end of the thesis, the complete source prototype was assembled and tested with two different regulators

Abstract The Cassini/Huygens mission is a collaborative mission of NASA and ESA to study the Saturnian system. Cassini Plasma Spectrometer (CAPS)is one of the scientific investigations onboard the Cassini orbiter. It consists of three separate spectrometers: Electron Spectrometer (ELS), Ion Mass Spectrometer (IMS) and Ion Beam Spectrometer (IBS). The University of Oulu has a co-investigator status in the CAPS project, and been mainly involved in simulating the structure and scientific performance of the IBS instrument. IBS is a high resolution hemispherical electrostatic analyser aimed to study the solar wind ions. This thesis contains an Introduction and five original papers. Papers I–III contain a detailed description of the simulation process of the IBS instrument and related results. In Paper I the manufacturing tolerances were calculated in order to verify that the high resolution requirements can be achieved using available manufacturing processes. In Paper II the simulations have been further developed and the instrument properties have been studied in more detail. In Paper III the simulation model is used to help the analysis and interpretation of the laboratory calibrations of the IBS flight model. Papers IV and V study the long-term fluctuations in solar wind and interplanetary magnetic field in the period range of 1–2 years (so called mid-term quasi periodicities, MTQP), using the wavelet transformation method to produce dynamic power spectra. In paper IV the MTQP structure in solar wind speed at 1 AU was studied using the longest available series of geomagnetic activity. It was shown that the long-term occurrence MTQP fluctuations roughly follows the long-term solar activity, suggesting that MTQP fluctuations are closely connected with the solar dynamo activity. Moreover, it was also noted that MTQP activity may offer a possibility for a precursory signal which could be used to predict significant changes in long-term solar activity. While Paper IV presents the temporally longest study of MTQP fluctuations, Paper V gives the spatially widest treatment of the same phenomenon. Paper V studies MTQP fluctuations in solar wind and interplanetary magnetic field measured by four probes in the outer heliosphere. It is shown that two MTQP fluctuations of different periods (1.3 and 1.7 years)co existed during solar cycle 22, while during solar cycle 21 only the 1.7-year band existed. This suggests that the solar dynamo acts differently during even and odd cycles. It is also shown that the two MTQP fluctuations during solar cycle 22 are organized latitudinally. While the 1.3-year periodicity originates from equatorial regions, the 1.7-year fluctuations arise at mid-latitudes
Original papers Original papers are not included in the electronic version of the dissertation. Vilppola, J. H., Keisala, J. T., Tanskanen, P. J., & Huomo, H. (1993). Optimization of hemispherical electrostatic analyzer manufacturing with respect to resolution requirements. Review of Scientific Instruments, 64(8), 2190–2194. https://doi.org/10.1063/1.1143958 Vilppola, J. H., Tanskanen, P. J., Huomo, H., & Barraclough, B. L. (1996). Simulations of the response function of a plasma ion beam spectrometer for the Cassini mission to Saturn. Review of Scientific Instruments, 67(4), 1494–1501. https://doi.org/10.1063/1.1146881 Vilppola, J. H., Tanskanen, P. J., Barraclough, B. L., & McComas, D. J. (2001). Comparison between simulations and calibrations of a high resolution electrostatic analyzer. Review of Scientific Instruments, 72(9), 3662–3669. https://doi.org/10.1063/1.1392337 Mursula, K., Zieger, B., & Vilppola, J. H. (2003). Mid-term quasi-periodicities in geomagnetic activity during last 15 solar cycles: Connection to solar dynamo strength. Solar Physics, 212(1), 201–207. https://doi.org/10.1023/a:1022980029618 Mursula, K., & Vilppola, J. H. (2004). Fluctuations of the Solar Dynamo Observed in the Solar Wind and Interplanetary Magnetic Field at 1 AU and in the Outer Heliosphere. Solar Physics, 221(2), 337–349. https://doi.org/10.1023/b:sola.0000035053.17913.26

Дисертація на здобуття наукового ступеня кандидата технічних наук за спеціальністю 05.09.13 – техніка сильних електричних та магнітних полів. Національний технічний університет "Харківський політехнічний інститут", Харків 2019. Дисертація присвячена вирішенню завдання поліпшення технічних показників обладнання магнітно-імпульсної обробки металів (міоми) для використання в технологіях металообробки і технологіях ремонту транспортних засобів. У роботі представлена розробка альтернативної конструкції вузла заряду ємнісних накопичувачів енергії та розробка системи індукційного нагріву. Дано числові показники нагріву при варіації часових параметрів збуджуючого струму і конструктивних параметрів інструменту індуктора. Розглянута модель системи збудження струму індуктора доповнена експериментальними дослідженнями системи в режимі резонансу напруги. Запропоновано використання модифікованої часової форми біполярного меандру сигналу збудження для зменшення кількості спектральних складових. Сконструйована система індукційного нагріву, що працює в режимі резонансу напруги, показала свою працездатність і ефективність. Було запропоновано виконувати збудження коливань струму імпульсами напруги модифікованої форми з частотою нижче на 20% від резонансної частоти, що забезпечує прийнятний ККД в режимі роботи системи без навантаження. Розробка система індукційного нагріву пройшла апробацію і випробування на підприємствах "Веда Авто Сервіс" (м. Київ) і АТ "Елеватормлинмаш" (м. Харків). Результати дисертаційної роботи використовують при підготовці бакалаврів та магістрів на кафедрі автомобільної електроніки Харківського національного автомобільно-дорожнього університету.
Thesis for the degree of Candidate of Technical Sciences for specialty 05.09.13 "Equipment of strong electric and magnetic fields" – National Technical University "Kharkiv Polytechnic Institute". Kharkiv, 2019. The thesis is dedicated to the solution of the problem of the technical performance of magnetic-impulse metal processing equipment improving for use in metal-working technologies and vehicle repair technologies. The paper presents the development of an alternative design for the capacitive energy storage charge system and the development of an induction heating system. The numerical heating indicators was given with a variation of the time parameters of the exciting current and the design parameters of the inductor tool. The system model of inductor current excitation in the mode of current resonance was considered and supplemented by experimental studies of the system in voltage resonance mode. The use of a modified time form of the bipolar meander of the excitation signal to reduce the number of spectral components was proposed. The induction heating system designed that operates in the voltage resonance mode has shown its efficiency. It was proposed to perform the excitation of current oscillations by voltage pulses of the modified form with a frequency lower than 20% of the resonant frequency, which ensures acceptable efficiency in the system operation without load. The development of the induction heating system has been tested and implicated at the enterprises of "Veda Auto Service" (Kyiv) and "Elevatormlinmash" (Kharkiv). The results of the thesis are used in the preparation of bachelors and masters degree at the department of automobile electronics of the Kharkiv National Automobile and Highway University.

Дисертація на здобуття наукового ступеня кандидата технічних наук за спеціальністю 05.09.13 – техніка сильних електричних та магнітних полів. Національний технічний університет "Харківський політехнічний інститут", Харків 2019. Дисертація присвячена вирішенню завдання поліпшення технічних показників обладнання магнітно-імпульсної обробки металів (міоми) для використання в технологіях металообробки і технологіях ремонту транспортних засобів. У роботі представлена розробка альтернативної конструкції вузла заряду ємнісних накопичувачів енергії та розробка системи індукційного нагріву. Дано числові показники нагріву при варіації часових параметрів збуджуючого струму і конструктивних параметрів інструменту індуктора. Розглянута модель системи збудження струму індуктора доповнена експериментальними дослідженнями системи в режимі резонансу напруги. Запропоновано використання модифікованої часової форми біполярного меандру сигналу збудження для зменшення кількості спектральних складових. Сконструйована система індукційного нагріву, що працює в режимі резонансу напруги, показала свою працездатність і ефективність. Було запропоновано виконувати збудження коливань струму імпульсами напруги модифікованої форми з частотою нижче на 20% від резонансної частоти, що забезпечує прийнятний ККД в режимі роботи системи без навантаження. Розробка система індукційного нагріву пройшла апробацію і випробування на підприємствах "Веда Авто Сервіс" (м. Київ) і АТ "Елеватормлинмаш" (м. Харків). Результати дисертаційної роботи використовують при підготовці бакалаврів та магістрів на кафедрі автомобільної електроніки Харківського національного автомобільно-дорожнього університету.
Thesis for the degree of Candidate of Technical Sciences for specialty 05.09.13 "Equipment of strong electric and magnetic fields" – National Technical University "Kharkiv Polytechnic Institute". Kharkiv, 2019. The thesis is dedicated to the solution of the problem of the technical performance of magnetic-impulse metal processing equipment improving for use in metal-working technologies and vehicle repair technologies. The paper presents the development of an alternative design for the capacitive energy storage charge system and the development of an induction heating system. The numerical heating indicators was given with a variation of the time parameters of the exciting current and the design parameters of the inductor tool. The system model of inductor current excitation in the mode of current resonance was considered and supplemented by experimental studies of the system in voltage resonance mode. The use of a modified time form of the bipolar meander of the excitation signal to reduce the number of spectral components was proposed. The induction heating system designed that operates in the voltage resonance mode has shown its efficiency. It was proposed to perform the excitation of current oscillations by voltage pulses of the modified form with a frequency lower than 20% of the resonant frequency, which ensures acceptable efficiency in the system operation without load. The development of the induction heating system has been tested and implicated at the enterprises of "Veda Auto Service" (Kyiv) and "Elevatormlinmash" (Kharkiv). The results of the thesis are used in the preparation of bachelors and masters degree at the department of automobile electronics of the Kharkiv National Automobile and Highway University.

La transition a la turbulence d'ecoulements en geometrie complexe est etudiee par simulation numerique compressible bidimensionnelle et tridimensionnelle. On presente une simulation des grandes echelles d'un jet rond d'air, comparee a une experience en laboratoire et a une autre simulation numerique incompressible. Cette comparaison nous a permis de valider notre outil numerique. Nous montrons un bon accord entre les resultats experimentaux et notre simulation numerique en zone transitionnelle. On applique notre outil numerique a une geometrie complexe et industrielle: l'entree d'air en incidence. Cette etude est effectuee avec un code a gestion multi-domaine des transferts d'informations par methode aux caracteristiques. Les resultats sont compares a ceux d'une experience faite au ceat de poitiers. Nous avons mis en evidence les tourbillons de kelvin-helmholtz, ainsi que les tourbillons longitudinaux, responsables des fluctuations de pression au niveau du premier etage du compresseur. Enfin, on a reproduit une experience magnetohydrodynamique faite au laboratoire madylam, en geometrie bidimensionnelle ronde. L'influence du champ magnetique sur un ecoulement de mercure soumis aux forces de laplace cree un cisaillement au niveau de l'electrode. On presente une evolution temporelle de la vorticite et de la pression, ainsi que les statistiques obtenues en regime permanent. Nous montrons des resultats qualitatifs satisfaisants, mais par contre sur les statistiques, nous surestimons les valeurs moyennes et fluctuantes. Nous montrons que les caracteristiques de l'ecoulement ne sont pas bidimensionnelles, mais doivent etre tridimensionnelles

En Imagerie par Résonance Magnétique (IRM), l’augmentation du champ magnétique statique permet en théorie de fournir un rapport signal sur bruit accru, améliorant la qualité des images. L’objectif de l’IRM à ultra haut champ est d’atteindre une résolution spatiale suffisamment haute pour pouvoir distinguer des structures si fines qu’elles sont actuellement impossibles à visualiser de façon non-invasive. Cependant, à de telles valeurs de champs magnétiques, la longueur d’onde du rayonnement électromagnétique envoyé pour basculer les spins des protons de l’eau est du même ordre de grandeur que l’objet dont on souhaite faire l’image. Des phénomènes d’interférences sont observés, ce qui se traduit par l’inhomogénéité de ce champ radiofréquence (RF) au sein de l’objet. Ces interférences engendrent des artefacts de signal et/ou de contraste dans les images IRM, et rendent ainsi leur exploitation délicate. Il est donc crucial de fournir des solutions pour atténuer la non-uniformité de l’excitation des spins, à défaut de quoi de tels systèmes ne pourront atteindre leurs pleins potentiels. Pour obtenir des diagnostics pertinents à très haut champ, il est donc nécessaire de créer des impulsions RF homogénéisant l'excitation de l'ensemble des spins (ici du cerveau humain), optimisées pour chaque individu. Pour cela, un système de transmission parallèle (pTX) à 8 canaux a été installé au sein de notre imageur à 7 Tesla. Alors que la plupart des systèmes IRM cliniques n’utilisent qu’un seul canal d’émission, l’extension pTX permet de jouer différentes formes d’impulsions RF de concert. La somme résultante de ces interférences doit alors être optimisée pour atténuer la non-uniformité observée classiquement. L’objectif de cette thèse est donc de synthétiser ce type d’impulsions, en utilisant la pTX. Ces impulsions auront pour contrainte supplémentaire le respect des limitations internationales concernant l'exposition à des champs radiofréquence, qui induit une hausse de température dans les tissus. En ce sens, de nombreuses simulations électromagnétiques et de températures ont été réalisées en introduction de cette thèse, afin d’évaluer la relation entre les seuils recommandés d’exposition RF et l’élévation de température prédite dans les tissus. Cette thèse porte plus spécifiquement sur la conception de l’ensemble des impulsions RF refocalisantes utilisées dans des séquences IRM non-sélectives, basées sur l’écho de spin. Dans un premier temps, seule une impulsion RF a été générée, pour une application simple : l’inversion du déphasage des spins dans le plan transverse. Dans un deuxième temps, sont considérées les séquences à long train d’échos de refocalisation appliquées à l’in vivo. Ici, l’opérateur mathématique agissant sur la magnétisation, et non pas son état final comme il est fait classiquement, est optimisé. Le gain en imagerie à très haut champ est clairement visible puisque les opérations mathématiques (la rotation des spins) voulues sont réalisées avec plus de fidélité que dans le cadre des méthodes de l’état de l’art. Pour cela, la génération de ces impulsions RF combine une méthode d’excitation des spins avec navigation dans l’espace de Fourier, les kT-points, et un algorithme d’optimisation, appelé Gradient Ascent Pulse Engineering (GRAPE), utilisant le contrôle optimal. Cette conception est rapide grâce à des calculs analytiques plus directs que des méthodes de différences finies. La prise en compte d’un grand nombre de paramètres nécessite l’usage de GPUs (Graphics Processing Units) pour atteindre des temps de calcul compatibles avec un examen clinique. Cette méthode de conception d’impulsions RF a été validée expérimentalement sur l’imageur 7 Tesla de NeuroSpin, sur une cohorte de volontaires sains
In Magnetic Resonance Imaging (MRI), the increase of the static magnetic field strength is used to provide in theory a higher signal-to-noise ratio, thereby improving the overall image quality. The purpose of ultra-high-field MRI is to achieve a spatial image resolution sufficiently high to be able to distinguish structures so fine that they are currently impossible to view in a non-invasive manner. However, at such static magnetic fields strengths, the wavelength of the electromagnetic waves sent to flip the water proton spins is of the same order of magnitude than the scanned object. Interference wave phenomena are then observed, which are caused by the radiofrequency (RF) field inhomogeneity within the object. These generate signal and/or contrast artifacts in MR images, making their exploitation difficult, if not impossible, in certain areas of the body. It is therefore crucial to provide solutions to mitigate the non-uniformity of the spins excitation. Failing this, these imaging systems with very high fields will not reach their full potential.For relevant high field clinical diagnosis, it is therefore necessary to create RF pulses homogenizing the excitation of all spins (here of the human brain), and optimized for each individual to be imaged. For this, an 8-channel parallel transmission system (pTX) was installed in our 7 Tesla scanner. While most clinical MRI systems only use a single transmission channel, the pTX extension allows to simultaneously playing various forms of RF pulses on all channels. The resulting sum of the interference must be optimized in order to reduce the non-uniformity typically seen.The objective of this thesis is to synthesize this type of tailored RF pulses, using parallel transmission. These pulses will have as an additional constraint the compliance with the international exposure limits for radiofrequency exposure, which induces a temperature rise in the tissue. In this sense, many electromagnetic and temperature simulations were carried out as an introduction of this thesis, in order to assess the relationship between the recommended RF exposure limits and the temperature rise actually predicted in tissues.This thesis focuses specifically on the design of all RF refocusing pulses used in non-selective MRI sequences based on the spin-echo. Initially, only one RF pulse was generated for a simple application: the reversal of spin dephasing in the transverse plane, as part of a classic spin echo sequence. In a second time, sequences with very long refocusing echo train applied to in vivo imaging are considered. In all cases, the mathematical operator acting on the magnetization, and not its final state as is done conventionally, is optimized. The gain in high field imaging is clearly visible, as the necessary mathematical operations (that is to say, the rotation of the spins) are performed with a much greater fidelity than with the methods of the state of the art. For this, the generation of RF pulses is combining a k-space-based spin excitation method, the kT-points, and an optimization algorithm, called Gradient Ascent Pulse Engineering (GRAPE), using optimal control.This design is relatively fast thanks to analytical calculations rather than finite difference methods. The inclusion of a large number of parameters requires the use of GPUs (Graphics Processing Units) to achieve computation times compatible with clinical examinations. This method of designing RF pulses has been experimentally validated successfully on the NeuroSpin 7 Tesla scanner, with a cohort of healthy volunteers. An imaging protocol was developed to assess the image quality improvement using these RF pulses compared to typically used non-optimized RF pulses. All methodological developments made during this thesis have contributed to improve the performance of ultra-high-field MRI in NeuroSpin, while increasing the number of MRI sequences compatible with parallel transmission