Nous savons que la grande majorité des étoiles WC9 produit de la poussière à base de carbone. Cette dernière doit se former dans des zones de très haute densité afin de survivre à l’environnement hostile qu’est celui du vent d’une étoile WR. Les étoiles WC appartenant à un système binaire WR + O produisent de la poussière quand les vents des deux étoiles entrent en collision et forment une zone de choc pouvant augmenter la densité du gaz d’un facteur 1000. Par contre, plusieurs étoiles WC9 n’ont, à ce jour, montré aucun signe de la présence d’un compagnon. Le but du projet est de tenter d’identifier un mécanisme alternatif responsable de la formation de poussière dans les étoiles WC9 n’appartenant pas à un système binaire. Nous présentons les résultats d’une campagne d’observation visant à caractériser la variabilité spectroscopique d’un échantillon de huit étoiles WC9 et une étoile WC8d. Nos résultats indiquent que la majorité des étoiles montrent des variations à grande échelle dans la raie d’émission C III 5696, soit à un niveau d’au moins 5% du flux de la raie et que les structures dans le vent ont une dispersion de vitesses de l’ordre de 150-300 km/s. De manière générale, les variations de vitesse radiales sont anti-corrélées avec le coefficient d’asymétrie de la raie, ce qui semble infirmer la présence d’un compagnon. Des observations en photométrie de l’étoile WR103 montrent une période de 9.1 ± 0.6 jours qui s’accorde avec les variations spectroscopiques et qui ne semble pas, de manière évidente, d’origine binaire. / We know that the majority of WC9 stars produces carbon-based dust. To survive in the hot and harsh environement that is the wind of a WR star, the dust grains must be formed in regions of very high density. We know that WC stars that are part of a WR + O system can produce dust at periastron passage where the collision of the two stellar winds is strong enough to produce shocks that compress the gas to densities up to a factor 103 higher than that of the WR star. However, so far, many WC9 stars have shown no signs of a companion. The goal of the current project is to identify a mechanism that could be responsible for the formation of dust in single WC9 stars. We present the results of an observing campaign which aimed to characterize the spectroscopic variability of eight WC9 stars and one WC8d star. Our results indicate that most stars show large scale variations of their C III 5696 emission line that reach at least 5% of the total line flux, and that the structures in the wind have a mean velocity dispersion of 150-300 km/s. In general, the radial velocity variations are anti-correlated with the skewness variations. This seems to indicate that the variations are not due to the presence of a companion. Photometric observations of WR 103 show a period of 9.1 ± 0.6 days that agrees with the spectroscopic variations and does not seem from binary origin.

Mémoire numérisé par la Division de la gestion de documents et des archives de l'Université de Montréal

Mémoire numérisé par la Division de la gestion de documents et des archives de l'Université de Montréal

Prostate cancer is the most common malignancy afflicting Canadian men in 2011. Physicians use digital rectal exams (DRE), blood tests for prostate specific antigen (PSA) and transrectal ultrasound (TRUS)-guided biopsies for the initial diagnosis of prostate cancer. None of these tests detail the spatial extent of prostate cancer - information critical for using new therapies that can target cancerous prostate. With an MRI technique called proton magnetic resonance spectroscopic imaging (1H-MRSI), biochemical analysis of the entire prostate can be done without the need for biopsy, providing detailed information beyond the non-specific changes in hardness felt by an experienced urologist in a DRE, the presence of PSA in blood, or the “blind-guidance” of TRUS-guided biopsy. A hindrance to acquiring high quality 1H-MRSI data comes from signal originating from fatty tissue surrounding prostate that tends to mask or distort signal from within the prostate, thus reducing the overall clinical usefulness of 1H-MRSI data. This thesis has three major areas of focus: 1) The development of an optimized 1H-MRSI technique, called conformal voxel magnetic resonance spectroscopy (CV-MRS), to deal the with removal of unwanted lipid contaminating artifacts at short and long echo times. 2) An in vivo human study to test the CV-MRS technique, including healthy volunteers and cancer patients scheduled for radical prostatectomy or radiation therapy. 3) A study to determine the efficacy of using the 1H-MRSI data for optimized radiation treatment planning using modern delivery techniques like intensity modulated radiation treatment. Data collected from the study using the optimized CV-MRS method show significantly reduced lipid contamination resulting in high quality spectra throughout the prostate. Combining the CV-MRS technique with spectral-spatial excitation further reduced lipid contamination and opened up the possibility of detecting metabolites with short T2 relaxation times. Results from the in vivo study were verified with post-histopathological data. Lastly, 1H-MRSI data was incorporated into the radiation treatment planning software and used to asses tumour control by escalating the radiation to prostate lesions that were identified by 1H-MRSI. In summary, this thesis demonstrates the clinical feasibility of using advanced spectroscopic imaging techniques for improved diagnosis and treatment of prostate cancer.

ν Octantis is a spectroscopic binary with a semi-major axis and period of 2.55 AU and 2.9 years, respectively. Ramm et al. (2009) discovered a 52 ms^(-1) radial-velocity (RV) perturbation with a period of 417 days in this system. All evidence, both photometric and spectroscopic, suggests the perturbation is the result of a 2.5 MJ planet orbiting the primary star. However, when assuming a “normal” prograde coplanar orbit, celestial mechanics predicts this orbit is unstable, contradicting the observed stability. Simulations by Eberle and Cuntz (2010) showed a retrograde orbit for the planet to be stable for at least 10^7 years. In this thesis, we performed a 10^8 -yr simulation of the retrograde orbit, and found it remained stable. Simulations over a range of planetary semi-major axes, eccentricities, and primary/secondary masses showed that stable retrograde orbits are not possible past a semi-major axis of 1.315 +/- 0.092 AU . Therefore, planetary retrograde orbits are most likely inherently more stable than prograde orbits owing to the absence of stability at known mean-motion resonances. Eccentricity simulations showed that the period of the planet's dominant eccentricity variation is related to the planet's semi-major axis by a second order exponential. However, retrograde orbits tend to have longer eccentricity periods than prograde orbits at the same semi-major axis. There is also evidence that this eccentricity period is connected to the orbital stability. By fitting a keplerian to both Ramm et al. (2009) and current radial velocities, the period of the ν Octantis binary was determined to be 1050.04 +/- 0.02 days with an eccentricity of 0.2359 +/- 0.001 . The planetary orbital solution for just the data reduced in this thesis gave a period of 416.9 +/- 2.1 days and an eccentricity of 0.099 +/- 0.015 , with an RMS scatter of 9.6 ms^(-1). Therefore, the orbital elements are within 1σ of the Ramm et al. (2009) elements. Assuming a retrograde coplanar orbit about the primary star then the planet has a mass of M_pl = 2.3 M_J and a semi-major axis of a_pl = 1.21 +/- 0.09 AU.

Prostate cancer is the most common malignancy afflicting Canadian men in 2011. Physicians use digital rectal exams (DRE), blood tests for prostate specific antigen (PSA) and transrectal ultrasound (TRUS)-guided biopsies for the initial diagnosis of prostate cancer. None of these tests detail the spatial extent of prostate cancer - information critical for using new therapies that can target cancerous prostate. With an MRI technique called proton magnetic resonance spectroscopic imaging (1H-MRSI), biochemical analysis of the entire prostate can be done without the need for biopsy, providing detailed information beyond the non-specific changes in hardness felt by an experienced urologist in a DRE, the presence of PSA in blood, or the “blind-guidance” of TRUS-guided biopsy. A hindrance to acquiring high quality 1H-MRSI data comes from signal originating from fatty tissue surrounding prostate that tends to mask or distort signal from within the prostate, thus reducing the overall clinical usefulness of 1H-MRSI data. This thesis has three major areas of focus: 1) The development of an optimized 1H-MRSI technique, called conformal voxel magnetic resonance spectroscopy (CV-MRS), to deal the with removal of unwanted lipid contaminating artifacts at short and long echo times. 2) An in vivo human study to test the CV-MRS technique, including healthy volunteers and cancer patients scheduled for radical prostatectomy or radiation therapy. 3) A study to determine the efficacy of using the 1H-MRSI data for optimized radiation treatment planning using modern delivery techniques like intensity modulated radiation treatment. Data collected from the study using the optimized CV-MRS method show significantly reduced lipid contamination resulting in high quality spectra throughout the prostate. Combining the CV-MRS technique with spectral-spatial excitation further reduced lipid contamination and opened up the possibility of detecting metabolites with short T2 relaxation times. Results from the in vivo study were verified with post-histopathological data. Lastly, 1H-MRSI data was incorporated into the radiation treatment planning software and used to asses tumour control by escalating the radiation to prostate lesions that were identified by 1H-MRSI. In summary, this thesis demonstrates the clinical feasibility of using advanced spectroscopic imaging techniques for improved diagnosis and treatment of prostate cancer.

[Special characters cannot be displayed. Please see the pdf version of the Abstract for an accurate reproduction.] We studied the circumstellar discs, the initial mass function (IMF), mass distribution, binarity and the fundamental properties of the [special character] 9 Myr-old pre-main sequence (PMS) [special character] Chamaeleontis cluster. Using JHKL colour-colour and colour-excess diagrams, we found the circumstellar disc fraction to be [special character] 0.60 among the late-type members. Four stars with [special character] (K - L) > 0.4 were identified as experiencing ongoing accretion which was later confirmed by high-resolution spectroscopic study. Quantitative analysis of the H[special character] profiles found accretion in these four stars at rates comparable to that of two members of the similarly-aged TW Hydrae Association (TWA); rates 1 - 3 orders of magnitude lower than in younger classical T Tauri stars. Together these results suggest that, while the mass accretion rate decreases with age, PMS stars can retain their inner discs for [special character] 10 Myr. An optical photometric survey spanning 1.3 ?? 1.3 pc added two low-mass stars to the cluster inventory. Together with other recent surveys the population is likely to be significantly complete for primaries with masses M > 0.15M[special character]. The cluster now consists of 18 primaries and 9 confirmed and candidate secondaries, with [special character] 2-4 times higher multiplicity than seen in field dwarfs. The cluster IMF is consistent with that of rich young clusters and field stars. By extending the IMF to lower masses, we predict 20-29 low-mass stars and brown dwarfs may remain undiscovered. From study of the cluster???s spatial and mass distribution, we find the [special character] Cha cluster has significant mass segregation, with > 50 per cent of the stellar mass residing within the central 0.17 pc. Lastly we classified members of the cluster with low-resolution spectra, providing information about the fundamental properties of the PMS stars by comparison to standard dwarfs. Broadband VRI colours and pseudocontinuum indices derived for the cluster stars are indistinguishable from dwarfs at visual and red wavelengths. This suggests the temperature sequence for the PMS [special character] Cha cluster is similar to that of the dwarf sequence. Narrow-band spectral indices for the [special character] Cha cluster possibly indicate higher metallicity and strongly indicate lower surface gravity than the dwarf indices.

An Ultraviolet to Visible (UV-Vis) spectroscopic analysis based on fuzzy logic approach has been developed for furan content measurement in transformer oil. Following the successful identification and quantification of furan derivatives in transformer oil by ASTM D5837 standard, the new approach is able to approximate the furan content more conveniently and economically. As furan concentration level would determine the absorption intensity in UV-Vis spectral range, the fuzzy logic software model developed would exploit this characteristic to aggregate the furans content level in transformer oil. The UV-Vis spectral response at other ambient temperature is also studied. The proposed technique provides a convenient alternative to conventional method of furan measurement by High Performance Liquid Chromatography (HPLC) or Gas Chromatography Mass Spectrometry (GC/MS) in ASTM D5837 Standard.

Les carbures et oxydes des métaux de transition sont d'une importance capitale dans le domaine industriel voir catalytique. Le carbure de tungstène WC a été identifié comme un bon substituant des métaux nobles tel que le platine dans le domaine catalytique. Le but de ce travail de thèse est d'appliquer des méthodes de chimie quantique les plus poussées pour déterminer la structure électronique, la stabilité et la nature de liaison chimique des diatomiques WC et WC2+. Notre recherche préliminaire est motivée par les données spectroscopiques disponibles sur W, W+, W2+, WC et WC2+. La méthodologie adoptée, CASSCF/MRCI/MRCI+Q/aug-cc-pV5Z(-PP) implémentée dans le code MOLPRO, consiste à réaliser des calculs quantique tenant en compte des effets de corrélation et relativistes avec un traitement spécifique du couplage spin−orbite pour la recherche des courbes d'énergie potentielle de l'état fondamental et des états excités de plus basses énergies de WCn+ (n=0-2) tout en utilisant une base suffisamment étendue. Les résultats de ce travail sont en bon accord avec ceux disponibles dans la littérature. En outre, dans ce travail nous avons confirmé pour la première fois que le carbure diatomique dicationique WC2+ est thermodynamiquement stable / Metal carbides and oxides are more interesting in catalytic and industrial domains. Tungsten carbide WC has been detected as serious substituent of platinum Pt catalytic. The ultimate goal of this thesis is theoretical studies of electronic structure, stability and the bound nature on WC, WO and its cations. Our preliminary research were motiving by the available spectroscopic data on W, W+, W2+, WC et WC2+. We used the methodology (CASSCF/MRCI/MRCI+Q/aug-cc-pV5Z(-PP)) implemented on MOLPRO package to perform quantum calculations with high accuracy taking into account the correlation and relativistic effects with a specific treatment of spin orbit coupling for some low lying excited electronic states of WCn+, (n=0, 1 et 2). Our results are shown in good agreement with those available in the literature. Furthermore, in this work for the first time we demonstrated that a carbide dication (WC2+) is thermodynamically stable

La transfection est le processus de transfert de gènes (ADN) dans des cellules. L'utilisation des plasmas froids à la pression atmosphérique est un excellent vecteur pour la transfection de gènes. Cela peut conduire à une perméabilisation temporaire de la membrane cellulaire permettant ainsi le processus de transfection de gènes, dans lequel l'ADN et les cellules sont exposées aux flux des espèces actives du plasma (électrons, ions et radicaux neutres). Cependant beaucoup de questions restent sans réponse notamment sur les mécanismes de transfection par plasma, en particulier de formation de pores et de perméabilisation de la membrane par interactions avec les espèces actives du plasma. Ainsi, nous avons développé un modèle Monte Carlo simulant la formation de pores de quelques nm de largeur sous l'effet d'un microplasma d'air. Ce model nécessite a priori des données d'entrées sur la densité des espèces chargées et la température du gaz et des électrons. C'est pourquoi nous avons aussi effectué une caractérisation expérimentale par spectroscopie d'émission optique OES de la micro décharge couronne. On a estimé les températures rotationnelles de plusieurs espèces variant entre (700K-2350K) même si dans nos conditions de plasma hors équilibre la température du gaz demeure ~300K. Les variations spatiales de la température vibrationnelle Tvib et des électrons Te le long de l'espace inter-électrode (de la pointe vers l'électrode de masse) ont aussi été estimées (Tvib:3000K-6500K et Te:6.75 eV-3.4eV). Les densités des ions et des électrons ont été déterminées et valent environ 1015 cm-3. Par ailleurs, sachant qu'il n'existe dans la littérature aucune modélisation consacrée à la perméabilisation de la membrane et la formation de pore par interactions avec les espèces actives du plasma, nous avons développé pour la première fois dans la littérature un modèle spécifique de simulation Monte Carlo pour la poration. Chaque espèce du plasma (électrons, ions, neutres radicaux) est considérée comme une macro-espèce (ou super-particule) représentant un grand nombre de particules. La proportion des espèces du plasma arrivant sur la membrane est estimée à partir de leurs flux, calculés à l'aide d'un modèle de cinétique réactionnelle et par mesures spectroscopiques. La membrane est supposée comme une simple structure multicouche de phospholipides et protéines. Les interactions avec les couches membranaires sont considérées comme étant des super-processus (recombinaison, réflexion, activation, ouverture). Une probabilité d'occurrence de chacun de ces super-processus est assignée à chaque super-particule sur la base d'une étude paramétrique. Le but est d'évaluer les effets des paramètres de simulation initiaux ainsi que l'effet des probabilités d'occurrence de chaque processus sur la formation de pores. Plusieurs résultats importants ont été obtenus. Les électrons jouent un rôle principal sur l'activation et l'ouverture des sites dus à leur forte anisotropie dans la direction avant. Malgré les faibles énergies, proche de celle du gaz, des ions et des radicaux, leur processus de réflexion est déterminant pour élargir et approfondir les dimensions des pores. Il a été montré que le nombre initial de particules NP est le paramètre qui contrôle le plus efficacement la formation de pores. De plus, nous avons observé une corrélation directe entre NP et la durée d'exposition de la membrane cellulaire au plasma. Dans les conditions actuelles de simulation, on a obtenu une dynamique de formation de pores avec des dimensions (diamètres~10nm) compatibles pour la transfection de gènes. Les résultats de simulation Monte Carlo ont été qualitativement validés par une comparaison préliminaire avec les mesures des taux de transfection d'ADN et de survie de cellules fibroblaste de souries. La méthode de Monte Carlo développée dans ce travail représente un outil très prometteur pour une meilleure compréhension des mécanismes de transfection de gènes par plasma. / Gene transfection is a technique of deliberately introducing DNA into cells through the membrane. The cold atmospheric plasma CAP is potentially a new alternative, safe and damage-free technique. It can lead to a transient permeabilization of the cell membrane allowing processes of gene transfection in which DNA and cells are both exposed to fluxes of active plasma species (electrons, ions, and neutral radicals). The mechanisms of more particularly membrane poration are far to be clear and controlled. Therefore, the aim of this thesis is to numerically study the mechanisms of plasma-induced membrane permeabilization using a specific micro-air plasma. More precisely, is to develop and exploit a specific Monte Carlo poration model. This model is aimed to simulate the pore formation of few nm of width through cell membranes when irradiated by micro-air plasma. This developed model requires a prior input data on the density of charged particles and the temperature of gas and electrons. Thus, an experimental characterisation by OES of the micro-air corona discharge is performed. Rotation temperature was determined (between 700K to 2350K) even though under our non-equilibrium conditions Tg remains ~300K. OES also has given the space variation from the high voltage tip to the grounded plate of vibration temperatures (between 3000K up to about 6500K) and Te (about 6.75 eV down to 3.4 eV near the plate). A magnitude around 1015cm-3 for the electron and ion densities have been also determined. Moreover, knowing that there are no literature simulations devoted to membrane permeabilization and pore formation when impacted by plasma actives species, we developed for the first time in literature a specific Monte Carlo poration model. In this framework, we assumed each plasma species (electrons, ions, and neutral radicals) as a super-particle grouping a large number of particles. The species fluxes were estimated from a plasma reaction kinetic model and OES study. The membrane layers were assumed as a simple membrane model superposing four layers of phospholipids and proteins. Each layer was constituted by a succession of super-sites subjected to specific super-processes (recombination, reflection, activation of a site, opening, etc). For an accurate exploitation of our model, the estimation of the probability of occurrence of the whole considered super-processes is absolutely necessary. Thus, a large parametric study is conducted. The aim is to evaluate the effects of the initial simulation parameters as well as the magnitude of the occurrence probabilities of each reaction process on pore formation.