La majorité des patients atteints d'un cancer sont soignés par la technique de la radiothérapie, l'une des trois principales modalités de traitement avec la chirurgie et la chimiothérapie. Elle consiste en la délivrance d'une radiation de haute énergie sur un volume cible. Son but est de détruire les cellules cancéreuses sans endommager les tissus sains. En pratique, on utilise divers outils numériques afin de prévoir de quelle manière sera déposée l'énergie dans le corps du patient. Ces méthodes peuvent néanmoins présenter des imprécisions ou un temps de calcul trop long pour leur utilisation en milieu clinique. Par conséquent, nous avons développé un nouveau modèle permettant de simuler le transport et le dépôt d'énergie de particules dans des tissus humains, de manière rapide et précise. De nouvelles installations permettant de traiter les patients de cette manière tout en effectuant une imagerie par résonance magnétique entrent actuellement sur le marché. Les champs magnétiques induits par cette technique ont pour effet secondaire et délétère de dévier les particules chargées, injectées ou créées dans le milieu, pouvant modifier fortement le dépôt d'énergie. Malgré cela, il n'existe actuellement pas de modèle permettant de rendre compte de ces effets de manière précise et rapide. Nous nous proposons d'introduire les effets magnétiques dans notre modèle afin de répondre à cette problématique. Nous appuyons la validation de notre modèle par des comparaisons numériques avec un code Monte-Carlo de référence, FLUKA, ainsi que par des comparaisons expérimentales effectuées à l'Institut Bergonié. / The majority of patients diagnosed with cancer are treated by radiotherapy, one of the principal treatment modality with surgery and chemotherapy. It consists in the delivery of high energy radiation on a target volume. It aims to destroy the cancerous cells without damaging sane tissues. In clinical practice, numerical tools are used in order to predict how the energy will be deposited in the patient's body. However, these methods can lack of accuracy or cost too much in terms of calculation time to be suitable for clinical use. As a consequence, we developed a new model able to calculate the transport and energy deposition of ionizing particles in human tissues, efficiently and accurately. New installations allowing the treatment of patients by radiotherapy while imaging them by Magnetic Resonance Imagery are currently marketed. The magnetic fields induced by this technology have as secondary and noxious effect to deflect the charged particles injected or created in the target medium, which might modify highly the deposited energy. Despite that, there aren't yet commercially available numerical solution allowing to reproduce these effects accurately and quickly. We implemented the magnetic effects in our model to. We validate our model by numerical comparisons with a reference Monte-Carlo code, FLUKA, and with experimental comparisons led in the Bergonié Institute (Bordeaux).

In low-mass (≲1.2 M⊙) main-sequence stars, the combination of differential rotation and turbulent flows in the outer convective region generates strong magnetic fields. It has been observed that in these stars, the rotation rate and the strength of the magnetic field decrease over time. This is thought to result from a feedback loop in which magnetized winds carry angular momentum away from the star, braking its rotation and weakening the magnetic dynamo. A well-calibrated age-rotation-activity relation (ARAR) would be particularly valuable for low-mass stars. If we knew the dependence of rotation or magnetic activity on age, a measurement of one of these quantities could be used to determine an accurate age for any isolated field star. Empirical calibrations of the ARAR rely on observations of the co-eval populations of stars in open clusters. In this work, I characterize rotation and magnetic activity, using light curves for the former and X-ray and Hα emission for the latter, in two open clusters of different ages (Alpha Persei, ≈60 Myr, and Messier 37, ≈500 Myr) to analyze the relation between rotation and activity across the low-mass stellar range. I also compare coronal (X-rays) and chromospheric (Hα) activity to understand how magnetic heating varies across stellar atmospheric layers. My results inform models of angular momentum evolution in low-mass stars.

In the second part, after performing in-vitro experiments to measure the resistant force of the small intestine, we propose a magnetic actuation method. The magnetic marker for localization acts as a seed to be actuated by multiple coils placed outside of the human body. The basic idea is that the magnetic seed is subject to a force and a torque in a magnetic field. An efficient computation scheme is designed and implemented to calculate the coil currents for real-time actuation. Simulations are performed on a six-coil actuation system to evaluate the method. As an alternative method, an internal actuator, which consists of a magnetic spring and can propel itself forward under an alternating current, is introduced to increase the mobility of the capsule and decrease the demand for a strong external field. The external magnetic field is also simulated to orient the internal actuator. / The development of wireless capsule endoscope realizes the examination of the whole gastrointestinal tract. The technology reduces patients' pain and benefits the doctors as well. However, it loses some functions that conventional endoscope owns because of the passive locomotion mode. To improve the situation, an active capsule endoscope is preferred by the community. / We put emphasis on two important problems in design of an active capsule endoscope: localization and actuation. The first part of our work focuses on the study of localization of the capsule taking advantage of the magnetic field. A small permanent magnet is enclosed in the capsule as a marker, and a tracking method is proposed based on the modelling of the marker as an ideal dipole. The five localization parameters are computed by minimizing the differences between the theoretical field values and sensing signals using Levenberg-Marquardt algorithm. One-axis Hall sensors and three-axis magnetoresistive sensors are employed respectively to implement the localization method. The system performance is evaluated by a series of tracking experiments. / Wang Xiaona. / "September 2006." / Adviser: Max Meng. / Source: Dissertation Abstracts International, Volume: 68-03, Section: B, page: 1771. / Thesis (Ph.D.)--Chinese University of Hong Kong, 2006. / Includes bibliographical references (p. 155-171). / Electronic reproduction. Hong Kong : Chinese University of Hong Kong, [2012] System requirements: Adobe Acrobat Reader. Available via World Wide Web. / Electronic reproduction. [Ann Arbor, MI] : ProQuest Information and Learning, [200-] System requirements: Adobe Acrobat Reader. Available via World Wide Web. / Abstracts in English and Chinese. / School code: 1307.

The oldest open clusters within 250 pc of the Sun, the Hyades and Praesepe, are important benchmarks for calibrating stellar properties such as rotation and magnetic activity. As they have the same age and roughly solar metallicity, these clusters serve as an ideal laboratory for testing the agreement between theoretical and empirical rotation-activity relations at ~650 Myr. The re-purposed Kepler mission, K2, has allowed me to measure rotation periods for dozens of Hyads and hundreds of Praesepe members, including the first periods measured for fully convective Hyads. These data have enabled new tests of models describing the evolution of stellar rotation; discrepancies with these models imply that we still do not fully understand how magnetic fields affect stellar spin-down. I show how we can compare the dependence of H-alpha and X-ray emission on rotation in order to test theories of magnetic field topology and stellar dynamos. These tests inform models of stellar wind-driven angular momentum loss and the age-rotation-activity relation. I also present rotation periods measured for 48 Hyads and 677 Praesepe members with K2, and discuss the impact of unresolved binaries on the study of rotational evolution.

The interstellar medium – the space between the stars in our Galaxy – is multiphase, turbulent, and magnetic. Magnetism in the interstellar medium is difficult to observe and to simulate, and the study of interstellar magnetic fields is riddled with open questions. In this Thesis we make progress in several important areas. We use analytic theory, simulations, and observations to advance our understanding of an important plasma instability, of the diffuse neutral medium, and of prospects for uncovering cosmic inflation. We take an unusual approach to the study of the magnetorotational instability, the mechanism thought to be the primary driver of turbulence and angular momentum transport in astrophysical accretion disks. We conduct a weakly nonlinear analysis of the instability in several important geometries, and derive an envelope equation that governs the evolution of the system on long length- and timescales. We show that the saturated state of the magnetorotational instability may itself be unstable on these large spatial and temporal scales, and we demonstrate that the character of these instabilities will depend on the geometry of the background magnetic field. We posit a possible new saturation mechanism for the magnetorotational instability in a local geometry, when a particular nonideal effect is considered. We derive new insights into the diffuse interstellar medium, where we present the discovery that thin, linear neutral hydrogen structures are ubiquitous in the cold neutral medium. We demonstrate that these linear features are extremely well aligned with the interstellar magnetic field, as traced by both starlight polarization and polarized dust emission. We discuss the implications of this discovery for cosmological studies. A major goal of modern cosmology is the detection of a particular signature in the polarized cosmic microwave background that would be direct evidence for inflation. This goal has thus far been thwarted by the polarized foreground emission from magnetically aligned interstellar dust grains. We demonstrate that the alignment of neutral hydrogen with the interstellar magnetic field can be used to produce higher-fidelity maps of the foreground polarization field, and we present and test a new Bayesian method for constructing improved foreground maps.

Thesis. 1976. Ph.D.--Massachusetts Institute of Technology. Dept of Physics. / Microfiche copy available in Archives and Science. / Vita. / Includes bibliographies. / Ph.D.

Inserido no paradigma da transdisciplinaridade, o presente trabalho foi desenvolvido em etapas, com os seguintes objetivos: a) Construir um dispositivo com base de metal não magnético para ímãs permanentes, visando à geração de um Campo Magnético Estático (CME) ou de um Campo Magnético Compensado (CMC); b) Expor culturas de células mesenquimais a um CME e a um CMC, ou a nenhum campo (controle); c) Analisar a influência destes campos na viabilidade e proliferação celular e nos casos em que houve alteração em pelo menos um destes parâmetros, utilizar a análise proteômica como ferramenta para a compreensão dos mecanismos envolvidos. O dispositivo foi construído utilizando aço inoxidável, capaz de gerar dois tipos de Campos Magnéticos: Compensado (CMC) com intensidade de aproximadamente 0 mT e Estático (CME) com intensidade média de 165 mT. Estes campos foram aplicados a culturas de células mesenquimais de medula óssea de camundongos AJ (MSC/AJ), nos períodos de 0, 24, 48, 72 e 96 h (CMC) e 24 h (CME). Os efeitos sobre a proliferação e a viabilidade foram avaliados por método de contagem manual de células com marcação por azul de tripan. A análise proteômica foi realizada para os experimentos com CMC, com o objetivo de descrever as proteínas envolvidas nas alterações encontradas. A exposição ao CMC tendeu a reduzir a proliferação das células de medula óssea MSC/AJ em relação ao controle em 96 h, porém sem diferença significativa, o que poderia estar relacionado a proteínas que inibem a transcrição, como a Forkhead box protein P2 Foxp2. Este mesmo campo aumentou a viabilidade celular em relação ao baseline para todos os tempos experimentais, o que poderia estar relacionado a proteínas relacionadas à ligação ao Ca+2. Esses mecanismos, entretanto, precisam ser estudados mais profundamente para que possam ser comprovados ou não. Já a exposição ao CME levou a uma tendência à diminuição da proliferação e viabilidade celular em relação ao grupo controle, embora sem diferenças significativas, provavelmente por conta do tamanho amostral e tempo de avaliação (24 h). / Inserted in the transdisciplinarity paradigm, the present work was developed by steps with the following aims: a) To build a device of non-magnetic metal to hold permanent magnets for the generation of a Static Magnetic Field (SMF) or a Compensated Magnetic Field (CMF); b) To expose mesenchimal cells to the SMF and to CMF or to none of the fields (control); c) To analyze the influence of these fields on cell viability and cell proliferation and in the case where it occurred alteration in at least one of these parameters, to use proteomics as a tool for the comprehension of the involved mechanisms. The device was built in stainless steel, able to generate two kinds of Magnetic Fields: Compesated (CMF) with an intensity of nearly zero mT and Static (SMF) with a mean intensity of 165 mT. These fields were applied to bone marrow mesenchimal cell cultures from AJ mice (MSC/AJ), for 0, 24, 48, 72 and 96 h (CMF) and 24 h (SMF) periods. The effects on the proliferation and viability were assessed by tripan blue dying and manual counting of the cells. Proteomics was done for the experiments with CMF, aiming to describe the involved proteins on found alterations. The exposition to CMF tends to reduce the bone marrow cell proliferation of MSC/AJ in relation to control in 96 h, but with no significant difference, which may be related to proteins that inhibit the transcription, like Forkhead box protein P2 Foxp2. This very field raised the cell viability in relation to the baseline for all the experimental times that could be related to proteins connected to Ca2+ binding. However, these mechanisms need more experiments, so they can be confirmed or not. The exposition to the SMF tends to decrease both cell proliferation and viability in relation to the control group, although with no significant difference, probably because of the sample number and the exposition time (24h).

No description available.

In this thesis we study GaAs one dimensional hole systems with strong spin-orbit interaction effects. The primary focus is the Zeeman splitting of 1D subbands in the two orthogonal in-plane magnetic field directions. We study two types of 1D hole systems based on different (311)A grown heterostructures: a modulation doped GaAs/AlGaAs square quantum well and an undoped induced GaAs/AlGaAs triangular quantum well. The results from the modulation doped 1D wire show enhanced anisotropy of the effective Lande g-factor for the two in-plane field directions (parallel and perpendicular to the wire), compared to that in 2D hole systems. This enhancement is explained by the confinement induced reorientation of the total angular momentum ^ J from perpendicular to the 2D plane to in-plane and parallel to the wire. We use the intrinsic anisotropy of the in-plane g-factors to probe the 0:7 structure and the zero bias anomaly in 1D hole wires. We find that the behaviour of the 0:7 structure and the ZBA are correlated and depend strongly on the orientation of the in-plane field. This result proves the connection between the 0:7 and the ZBA and their relation to spin. We fabricate the first induced hole 1D wire with extremely stable gate characteristics and characterize this device. We also fabricate devices with two orthogonal induced hole wires on one chip, to study the interplay between the confinement, crystallographic anisotropy and spin-orbit coupling and their effect on the Zeeman splitting. We find that the ratios of the g-factors in the two orthogonal field directions for the two wires show opposite behaviour. We compare absolute values of the g-factors relative to the magnetic field direction. For B || [011] the g-factor is large for the wire along [011] and small for the wire along [233]. Whereas for B || [233], the g-factors are large irrespective of the wire direction. The former result can be explained by reorientation of ^ J along the wire, and the latter by an additional off-diagonal Zeeman term, which leads to the out-of-plane component of ^ J when B || [233], and as a result, to enhanced g-factors via increased exchange interactions.

"July 2003." / Bibliography: p. 203-211. / xxii, 211 p. : ill. (some col.) ; 30 cm. / Title page, contents and abstract only. The complete thesis in print form is available from the University Library. / Investigates properties of magnetic fields in galaxy clusters via both statistical Faraday rotation measures and diffuse source polarimetry, and investigates the nature and generation mechanisms for diffuse radio emission in the ACO cluster A3667. / Thesis (Ph.D.)--University of Adelaide, Dept. of Physics and Mathematical Physics, 2003