Étude polarimétrique d’étoiles jeunes

Afin de mieux comprendre l'évolution des étoiles jeunes, nous avons utilisé un code Monte Carlo simulant leur environnement afin d'étudier une nouvelle distribution chez les étoiles Herbig Ae/Be et pour reproduire des cartes d'intensité et de polarisation linéaire obtenues au télescope Canada-France-Hawaii (TCFH) en novembre 2003. Le code datant de la fin des années 80, nous avons dû non seulement le corriger, mais aussi ajouter quelques éléments afin de tenir compte des dernières avancées dans le domaine de la polarisation provenant du milieu circumstellaire. Les étoiles à l'étude étant jeunes (moins de quelques millions d'années), leur voisinage est toujours constitué de grains de poussière mélangés avec du gaz. Selon leur âge, nous retrouvons cette poussière sous différentes structures soit, par exemple, par un disque entouré d'une enveloppe (objets jeunes de classe I) ou par un simple disque (objets de classe II et III). Selon la structure que prend la poussière, les cartes de polarisation et d'intensité qui en résultent vont changer. Nous allons discuter de cette variation des cartes de polarisation selon la distribution de poussière. Suite aux modifications apportées au code, il a fallu s'assurer que celui-ci fonctionne bien. Pour ce faire, nous avons mis au point quelques critères qui nous assurent, s'ils sont satisfaits, que le code Monte Carlo produit de bons résultats. Après avoir validé le code, il est maintenant possible de l'utiliser aux fins d'avancer le domaine de la polarisation. En effet, Dullemond et al.(2001) proposent une nouvelle distribution de grain autour des étoiles Herbig Ae/Be afin de mieux expliquer leur distribution d'énergie spectrale. Par contre, qu'en est-il des cartes de polarisation résultantes? C'est sur cette question que nous nous sommes arrêtés. Par la suite, nous avons essayé de reproduire du mieux possible, tenant compte des limitations du code, les cartes de polarisation obtenues au TCFH. Nous avons étudié en détail les données de R Mon (résultats qui seront présentés sous forme d'article pour fin de publication) et de V376 Cas. De plus, notre étude de V376 Cas nous a permis d'amener des conclusions sur les processus causant les vecteurs parallèles aux disques des étoiles jeunes.

Développement et caractérisation de sources de neutres réactifs pour l’étude des interactions plasmas-surfaces

L’objectif de ce mémoire de maîtrise est de développer et de caractériser diverses sources de neutres réactifs destinées à des études fondamentales des interactions plasmas-surfaces. Ce projet s’inscrit dans le cadre d’une vaste étude de la physique des interactions plasmas-parois mises en jeu dans les procédés de gravure par plasma des matériaux de pointe. Une revue de la littérature scientifique sur les diverses méthodes permettant de générer des faisceaux de neutres réactifs nous a permis de sélectionner deux types de sources. La première, une source pyrolitique, a été caractérisée par spectrométrie de masse en utilisant le C2F6 comme molécule mère. Nous avons montré que le C2F6 était dissocié à plus de 90% à 1000ºC et qu’il formait du CF4, lui-même dissocié en CF2 vers 900ºC. Ces résultats ont été validés à l’aide d’un modèle basé sur des calculs d’équilibres chimiques, qui a aussi prédit la formation de F à 1500ºC. La seconde source, un plasma entretenu par une onde électromagnétique de surfaces, a été caractérisée par spectroscopie optique d’émission et par interférométrie haute fréquence. Dans le cas du plasma d’argon créé par un champ électromagnétique (>GHz), nos travaux ont révélé une distribution en énergie des électrons à trois températures avec Te-low>Te-high

Déterminants des choix alimentaires d'athlètes adolescents en période de compétition

Cette étude s’insère dans une étude s’intitulant « Choix alimentaires d’adolescents canadiens et attitudes de leurs entraîneurs impliqués dans des activités sportives organisées ». Les objectifs étaient d’étudier chez des adolescents impliqués dans une compétition sportive provinciale où l’offre alimentaire est contrôlée 1) leur maîtrise des recommandations nutritionnelles 2) les facteurs individuels, comportementaux, socio-environnementaux influençant leurs choix alimentaires. Deux observateurs ont visité les différents sites alimentaires et de compétition pendant les Jeux du Québec de 2011 à Valleyfield. Les plateaux des athlètes ont été photographiés à table au moment des repas avec une caméra numérique et les commentaires oraux colligés par écrit. Au total, 173 photographies ont été analysées et comparées aux recommandations reconnues en nutrition sportive. Dans notre étude, les préférences alimentaires, l’offre alimentaire et la présence des coéquipiers sont les facteurs qui influencent le plus les choix alimentaires en compétition. Par contre, le sexe de l’athlète n’a pas influencé les choix alimentaires des athlètes observés. En pré-compétition, 85,4% des plateaux présentent une valeur énergétique supérieure aux recommandations et 66,3% d’entre eux ont une répartition en énergie inadéquate, peu importe le sexe. Un excès de lipides et de protéines au sein du repas précédant l’effort caractérise majoritairement les plateaux dont la répartition en énergie est non optimale (69,5%). Les recommandations en post-compétition (100%) et lors des jours de repos (95,8%) ont facilement été rencontrées. Il en est de même pour l’hydratation (99,4%). Le lait au chocolat est la boisson la plus populaire (59,5%). Les produits céréaliers (99,4%), le lait et substituts (87,3%), les légumes (85,7%), les viandes et substituts (83,2%), les aliments riches en sucres (79,8%), les fruits (70,5%) et les mets riches en gras (59,4%) sont particulièrement appréciés par les athlètes. Les commentaires recueillis font ressortir une vision dichotomique des aliments chez certains athlètes qui classifient les aliments en « bons » ou « mauvais ». Notre étude démontre que la présence d’une politique alimentaire permet de promouvoir des habitudes alimentaires saines et favorise la consommation d’aliments nutritifs lors d’une compétition sportive d’envergure. Cependant, de l’éducation en nutrition est toujours requise pour viser l’amélioration du comportement alimentaire avant l’effort.

Étude des propriétés atmosphériques et magnétiques des étoiles naines blanches froides riches en hydrogène.

Ce mémoire présente une analyse photométrique et spectroscopique d'un échantillon de 16 naines blanches magnétiques froides riches en hydrogène. L'objectif principal de cette étude est de caractériser leurs propriétés atmosphériques et magnétiques afin d'obtenir une vision d'ensemble représentative de cette population d'étoiles. Pour ce faire, il a fallu réunir le plus d'information possible sur toutes les candidates sous la forme de spectres visibles à haut signal-sur-bruit et de données photométriques. Il a également été nécessaire de mettre à jour les modèles d'atmosphère de Bergeron et al. (1992) à l'aide des avancées réalisées par Tremblay & Bergeron (2009). Les paramètres atmosphériques de chacune des étoiles ont ensuite été déterminés en modélisant les distributions d'énergie photométriques observées tandis que la topologie et l'intensité du champ magnétique ont été obtenues en comparant des spectres synthétiques magnétiques au profil d'absorption Zeeman autour de H-alpha. Qui plus est, un processus de déconvolution combinant ces deux approches a aussi été créé afin de traiter adéquatement les systèmes binaires présents dans l'échantillon. Les résultats de ces analyses sont ensuite exposés, incluant une discussion sur la possible corrélation entre les paramètres atmosphériques et les propriétés magnétiques de ces naines blanches. Finalement, cette étude démontre que les données spectroscopiques de la majorité de ces étoiles peuvent uniquement être reproduites si ces dernières se trouvent dans un système binaire composé d'une seconde naine blanche. De plus, les résultats suggèrent que le champ magnétique de ces naines blanches froides ne peut pas être d'origine fossile et doit être généré par un mécanisme physique devant encore être identifié.

Dynamique de croissance par plasma RF magnétron des couches minces à base d’oxyde de zinc

Le but de cette thèse était d’étudier la dynamique de croissance par pulvérisation par plasma RF magnétron des couches minces à base d’oxyde de zinc destinées à des applications électroniques, optoélectroniques et photoniques de pointe. Dans ce contexte, nous avons mis au point plusieurs diagnostics permettant de caractériser les espèces neutres et chargées dans ce type de plasmas, notamment la sonde électrostatique, la spectroscopie optique d’émission et d’absorption, ainsi que la spectrométrie de masse. Par la suite, nous avons tenté de corréler certaines caractéristiques physiques de croissance des couches de ZnO, en particulier la vitesse de dépôt, aux propriétés fondamentales du plasma. Nos résultats ont montré que l’éjection d’atomes de Zn, In et O au cours de la pulvérisation RF magnétron de cibles de Zn, ZnO et In2O3 n’influence que très peu la densité d’ions positifs (et donc la densité d’électrons en supposant la quasi-neutralité) ainsi que la fonction de distribution en énergie des électrons (populations de basse et haute énergie). Cependant, le rapport entre la densité d’atomes d’argon métastables (3P2) sur la densité électronique décroît lorsque la densité d’atomes de Zn augmente, un effet pouvant être attribué à l’ionisation des atomes de Zn par effet Penning. De plus, dans les conditions opératoires étudiées (plasmas de basse pression, < 100 mTorr), la thermalisation des atomes pulvérisés par collisions avec les atomes en phase gazeuse demeure incomplète. Nous avons montré que l’une des conséquences de ce résultat est la présence d’ions Zn+ suprathermiques près du substrat. Finalement, nous avons corrélé la quantité d’atomes de Zn pulvérisés déterminée par spectroscopie d’émission avec la vitesse de dépôt d’une couche mince de ZnO mesurée par ellipsométrie spectroscopique. Ces travaux ont permis de mettre en évidence que ce sont majoritairement les atomes de Zn (et non les espèces excitées et/ou ioniques) qui gouvernent la dynamique de croissance par pulvérisation RF magnétron des couches minces de ZnO.

Investigation of Multiphase Power Converter using Integrated Coupled Inductor Regarding Electric Vehicle Application

The challenge of reducing carbon emission and achieving emission target until 2050, has become a key development strategy of energy distribution for each country. The automotive industries, as the important portion of implementing energy requirements, are making some related researches to meet energy requirements and customer requirements. For modern energy requirements, it should be clean, green and renewable. For customer requirements, it should be economic, reliable and long life time. Regarding increasing requirements on the market and enlarged customer quantity, EVs and PHEV are more and more important for automotive manufactures. Normally for EVs and PHEV there are two important key parts, which are battery package and power electronics composing of critical components. A rechargeable battery is a quite important element for achieving cost competitiveness, which is mainly used to story energy and provide continue energy to drive an electric motor. In order to recharge battery and drive the electric motor, power electronics group is an essential bridge to convert different energy types for both of them. In modern power electronics there are many different topologies such as non-isolated and isolated power converters which can be used to implement for charging battery. One of most used converter topology is multiphase interleaved power converter, pri- marily due to its prominent advantages, which is frequently employed to obtain optimal dynamic response, high effciency and compact converter size. Concerning its usage, many detailed investigations regarding topology, control strategy and devices have been done. In this thesis, the core research is to investigate some branched contents in term of issues analysis and optimization approaches of building magnetic component. This work starts with an introduction of reasons of developing EVs and PEHV and an overview of different possible topologies regarding specific application requirements. Because of less components, high reliability, high effciency and also no special safety requirement, non-isolated multiphase interleaved converter is selected as the basic research topology of founded W-charge project for investigating its advantages and potential branches on using optimized magnetic components. Following, all those proposed aspects and approaches are investigated and analyzed in details in order to verify constrains and advantages through using integrated coupled inductors. Furthermore, digital controller concept and a novel tapped-inductor topology is proposed for multiphase power converter and electric vehicle application.

Further evidence for variable synchrotron emission in XTE J1118+480 in outburst

We present simultaneous multicolor infrared and optical photometry of the black hole X-ray transient XTE J1118+480 during its short 2005 January outburst, supported by simultaneous X-ray observations. The variability is dominated by short timescales, ~10 s, although a weak superhump also appears to be present in the optical. The optical rapid variations, at least, are well correlated with those in X-rays. Infrared JHKs photometry, as in the previous outburst, exhibits especially large-amplitude variability. The spectral energy distribution (SED) of the variable infrared component can be fitted with a power law of slope α=-0.78+/-0.07, where F_ν~ν^α. There is no compelling evidence for evolution in the slope over five nights, during which time the source brightness decayed along almost the same track as seen in variations within the nights. We conclude that both short-term variability and longer timescale fading are dominated by a single component of constant spectral shape. We cannot fit the SED of the IR variability with a credible thermal component, either optically thick or thin. This IR SED is, however, approximately consistent with optically thin synchrotron emission from a jet. These observations therefore provide indirect evidence to support jet-dominated models for XTE J1118+480 and also provide a direct measurement of the slope of the optically thin emission, which is impossible, based on the average spectral energy distribution alone.

Superthermal ion signatures of auroral acceleration processes

The retarding ion mass spectrometer on the Dynamics Explorer 1 spacecraft has generated a unique data set which documents, among other things, the occurrence of non-Maxwellian superthermal features in the auroral topside ionosphere distribution functions. In this paper, we provide a representative sampling of the observed features and their spatial morphology as observed at altitudes in the range from a few thousand kilometers to a few earth radii. At lower altitudes, these features appear at auroral latitudes separating regions of polar cap and subauroral light ion polar wind. The most common signature is the appearance of an upgoing energetic tail having conical lobes representing significant ion heat and number flux in all species, including O+. Transverse ion heating below the observation point at several thousand kilometers is clearly associated with O+ outflows. In some events observed, transverse acceleration apparently involves nearly the entire thermal plasma, the distribution function becomes highly anisotropic with T⊥ > T∥, and may actually develop a minimum at zero velocity, i.e., become a torus having as its axis the local magnetic field direction. At higher altitudes, the localized dayside source region appears as a field aligned flow which is dispersed tailward across the polar cap according to parallel velocity by antisunward convective flow, so that upflowing low energy O+ ions appear well within the polar cap region. While this flow can appear beamlike in a given location, the energy dispersion observed implies a very broad energy distribution at the source, extending from a few tenths of an eV to in excess of 50 eV. On the nightside, upgoing ion beams are found to be latitudinally bounded by regions of ion conics whose half angles increase with increasing separation from the beam region, indicating low altitude transverse acceleration in immediate proximity to, and below, the parallel acceleration region. These observations reveal a clear distinction between classical polar wind ion outflow and O+ enhanced superthermal flows, and confirm the importance of low altitude transverse acceleration in ionospheric plasma transport, as suggested by previous observations.

Towards the main sequence: detailed analysis of weak line and post-T Tauri stars

A detailed study was performed for a sample of low-mass pre-main-sequence (PMS) stars, previously identified as weak-line T Tauri stars, which are compared to members of the Tucanae and Horologium Associations. Aiming to verify if there is any pattern of abundances when comparing the young stars at different phases, we selected objects in the range from 1 to 100 Myr, which covers most of PMS evolution. High-resolution optical spectra were acquired at European Southern Observatory and Observatorio do Pico dos Dias. The stellar fundamental parameters effective temperature and gravity were calculated by excitation and ionization equilibria of iron absorption lines. Chemical abundances were obtained via equivalent width calculations and spectral synthesis for 44 per cent of the sample, which shows metallicities within 0.5 dex solar. A classification was developed based on equivalent width of Li I 6708 angstrom and Ha lines and spectral types of the studied stars. This classification allowed a separation of the sample into categories that correspond to different evolutive stages in the PMS. The position of these stars in the Hertzsprung-Russell diagram was also inspected in order to estimate their ages and masses. Among the studied objects, it was verified that our sample actually contains seven weak-line T Tauri stars, three are Classical T Tauri, 12 are Fe/Ge PMS stars and 21 are post-T Tauri or young main-sequence stars. An estimation of circumstellar luminosity was obtained using a disc model to reproduce the observed spectral energy distribution. Most of the stars show low levels of circumstellar emission, corresponding to less than 30 per cent of the total emission.

TOWARD UNDERSTANDING THE B[e] PHENOMENON. IV. MODELING OF IRAS 00470+6429

FS CMa type stars are a recently described group of objects with the B[e] phenomenon which exhibits strong emission-line spectra and strong IR excesses. In this paper, we report the first attempt for a detailed modeling of IRAS 00470+6429, for which we have the best set of observations. Our modeling is based on two key assumptions: the star has a main-sequence luminosity for its spectral type (B2) and the circumstellar (CS) envelope is bimodal, composed of a slowly outflowing disklike wind and a fast polar wind. Both outflows are assumed to be purely radial. We adopt a novel approach to describe the dust formation site in the wind that employs timescale arguments for grain condensation and a self-consistent solution for the dust destruction surface. With the above assumptions we were able to satisfactorily reproduce many observational properties of IRAS 00470+6429, including the Hi line profiles and the overall shape of the spectral energy distribution. Our adopted recipe for dust formation proved successful in reproducing the correct amount of dust formed in the CS envelope. Possible shortcomings of our model, as well as suggestions for future improvements, are discussed.

Nuclear and extended spectra of NGC 1068-II. Near-infrared stellar population synthesis

We performed stellar population synthesis on the nuclear and extended regions of NGC 1068 by means of near-infrared spectroscopy to disentangle their spectral energy distribution components. This is the first time that such a technique is applied to the whole 0.8-2.4 mu m wavelength interval in this galaxy. NGC 1068 is one of the nearest and probably the most studied Seyfert 2 galaxy, becoming an excellent laboratory to study the interaction between black holes, the jets that they can produce and the medium in which they propagate. Our main result is that traces of young stellar population are found at similar to 100 pc south of the nucleus. The contribution of a power-law continuum in the centre is about 25 per cent, which is expected if the light is scattered from a Seyfert 1 nucleus. We find peaks in the contribution of the featureless continuum about 100-150 pc from the nucleus on both sides. They might be associated with regions where the jet encounters dense clouds. Further support to this scenario is given by the peaks of hot dust distribution found around these same regions and the H(2) emission-line profile, leading us to propose that the peaks might be associated to regions where stars are being formed. Hot dust also has an important contribution to the nuclear region, reinforcing the idea of the presence of a dense, circumnuclear torus in this galaxy. Cold dust appears mostly in the south direction, which supports the view that the south-west emission is behind the plane of the galaxy and is extinguished very likely by dust in the plane. Intermediate-age stellar population contributes significantly to the continuum, especially in the inner 200 pc.

Cosmic shear requirements on the wavelength dependence of telescope point spread functions

Cosmic shear requires high precision measurement of galaxy shapes in the presence of the observational point spread function (PSF) that smears out the image. The PSF must therefore be known for each galaxy to a high accuracy. However, for several reasons, the PSF is usually wavelength dependent; therefore, the differences between the spectral energy distribution of the observed objects introduce further complexity. In this paper, we investigate the effect of the wavelength dependence of the PSF, focusing on instruments in which the PSF size is dominated by the diffraction limit of the telescope and which use broad-band filters for shape measurement. We first calculate biases on cosmological parameter estimation from cosmic shear when the stellar PSF is used uncorrected. Using realistic galaxy and star spectral energy distributions and populations and a simple three-component circular PSF, we find that the colour dependence must be taken into account for the next generation of telescopes. We then consider two different methods for removing the effect: (i) the use of stars of the same colour as the galaxies and (ii) estimation of the galaxy spectral energy distribution using multiple colours and using a telescope model for the PSF. We find that both of these methods correct the effect to levels below the tolerances required for per cent level measurements of dark energy parameters. Comparison of the two methods favours the template-fitting method because its efficiency is less dependent on galaxy redshift than the broad-band colour method and takes full advantage of deeper photometry.

Challenges in Radiative Transfer Modeling - W3 IRS5

By modeling the spectral energy distribution (SED) of the W3 IRS5 high-mass star formation region and matching this model to observed data, we can constrain the physical parameters of the basic system geometry and cloud mass distribution. From these parameters, we hope to add to the understanding of high-mass star formation processes. In particular, we hope to determine if the geometries associated with lowmass star formation carry over into the high-mass regime.

Desenvolvimento de método de planejamento e programação de operações de prestação de serviços

Este trabalho pretende contribuir com questões relacionadas ao planejamento e programação de operações de prestação de serviços. Seu enfoque é nos bastidores das operações de serviços, onde ocorre o fluxo de materiais e são observadas características similares às da manufatura. Ainda assim, algumas características específicas das operações de serviços influenciam o processo a ser planejado. O tema desta dissertação consiste na definição de um método de planejamento e programação das operações dos bastidores de empresas prestadoras de serviço. Este método engloba conceitos utilizados tanto na manufatura quanto nos serviços. Na etapa inicial do trabalho, é apresentada uma revisão bibliográfica sobre planejamento da produção na manufatura, planejamento da prestação de serviços e gerenciamento de projetos. Na etapa seguinte, apresenta-se um método de planejamento e programação para operações dos bastidores de empresas prestadoras de serviço. A etapa final apresenta a validação prática do método proposto em uma empresa do setor elétrico que atua no segmento de distribuição de energia.

Uso de técnicas de otimização baseadas em derivadas como suporte do planejamento operacional de redes de distribuição de energia elétrica

The usual programs for load flow calculation were in general developped aiming the simulation of electric energy transmission, subtransmission and distribution systems. However, the mathematical methods and algorithms used by the formulations were based, in majority, just on the characteristics of the transmittion systems, which were the main concern focus of engineers and researchers. Though, the physical characteristics of these systems are quite different from the distribution ones. In the transmission systems, the voltage levels are high and the lines are generally very long. These aspects contribute the capacitive and inductive effects that appear in the system to have a considerable influence in the values of the interest quantities, reason why they should be taken into consideration. Still in the transmission systems, the loads have a macro nature, as for example, cities, neiborhoods, or big industries. These loads are, generally, practically balanced, what reduces the necessity of utilization of three-phase methodology for the load flow calculation. Distribution systems, on the other hand, present different characteristics: the voltage levels are small in comparison to the transmission ones. This almost annul the capacitive effects of the lines. The loads are, in this case, transformers, in whose secondaries are connected small consumers, in a sort of times, mono-phase ones, so that the probability of finding an unbalanced circuit is high. This way, the utilization of three-phase methodologies assumes an important dimension. Besides, equipments like voltage regulators, that use simultaneously the concepts of phase and line voltage in their functioning, need a three-phase methodology, in order to allow the simulation of their real behavior. For the exposed reasons, initially was developped, in the scope of this work, a method for three-phase load flow calculation in order to simulate the steady-state behaviour of distribution systems. Aiming to achieve this goal, the Power Summation Algorithm was used, as a base for developing the three phase method. This algorithm was already widely tested and approved by researchers and engineers in the simulation of radial electric energy distribution systems, mainly for single-phase representation. By our formulation, lines are modeled in three-phase circuits, considering the magnetic coupling between the phases; but the earth effect is considered through the Carson reduction. It s important to point out that, in spite of the loads being normally connected to the transformer s secondaries, was considered the hypothesis of existence of star or delta loads connected to the primary circuit. To perform the simulation of voltage regulators, a new model was utilized, allowing the simulation of various types of configurations, according to their real functioning. Finally, was considered the possibility of representation of switches with current measuring in various points of the feeder. The loads are adjusted during the iteractive process, in order to match the current in each switch, converging to the measured value specified by the input data. In a second stage of the work, sensibility parameters were derived taking as base the described load flow, with the objective of suporting further optimization processes. This parameters are found by calculating of the partial derivatives of a variable in respect to another, in general, voltages, losses and reactive powers. After describing the calculation of the sensibility parameters, the Gradient Method was presented, using these parameters to optimize an objective function, that will be defined for each type of study. The first one refers to the reduction of technical losses in a medium voltage feeder, through the installation of capacitor banks; the second one refers to the problem of correction of voltage profile, through the instalation of capacitor banks or voltage regulators. In case of the losses reduction will be considered, as objective function, the sum of the losses in all the parts of the system. To the correction of the voltage profile, the objective function will be the sum of the square voltage deviations in each node, in respect to the rated voltage. In the end of the work, results of application of the described methods in some feeders are presented, aiming to give insight about their performance and acuity