Recombination line profile shapes are derived for ionized spherical stellar winds at radio wavelengths. It is assumed that the wind is optically thick owing to free-free opacity. Emission lines of arbitrary optical depth are obtained assuming that the free-free photosphere forms in the outer, constant expansion portion of the wind. Previous works have derived analytic results for isothermal winds when the line and continuum source functions are equal. Here, semi-analytic results are derived for unequal source functions to reveal that line shapes can be asymmetric about line center. A parameter study is presented and applications discussed.

L’étude des propriétés du boson de Higgs représente une excellente opportunité pour la recherche de Nouvelle Physique. En particulier, sa masse est mesurée avec une précision impressionnante, de l’ordre de 0.1%, tandis qu’elle est aussi prédite par certains modèles au-delà du Modèle Standard, notamment les modèles supersymétriques. Le but de cette thèse est de faire avancer le calcul des corrections radiatives aux masses des scalaires dans les modèles au-delà du Modèle Standard, ainsi que l’automatisation de ces calculs, afin d’établir ou d’améliorer les limites sur les couplages entre la Nouvelle Physique et le boson de Higgs. Nous calculons d’abord les corrections dominantes à deux boucles, de la forme O(alpha_s alpha_t), aux masses des scalaires neutres dans les modèles supersymétriques à jauginos de Dirac. Ensuite, nous montrons comment surmonter la Catastrophe des Bosons de Goldstone, un cas de divergences infrarouges dues aux bosons de Goldstones de masses nulles qui affecte les calculs de potentiels effectifs, d’équations « tadpoles » et d’énergies propres, en adoptant un schéma de renormalisation « on-shell » pour les masses des bosons de Goldstone. Nous illustrons la mise en œuvre numérique de notre solution dans le programme SARAH, et finalement, nous considérons le comportement aux hautes énergies de modèles non-supersymétriques avec des secteurs scalaires étendus. / The Standard Model-like Higgs boson provides an excellent setting for the indirect search of New Physics, through the study of its properties. In particular its mass is now measured with an astonishing precision, of the order of 0.1%, while being predicted in some models of Beyond the Standard Model (BSM) Physics, such as supersymmetric (SUSY) models. The main purpose of this thesis is to push further the calculation of radiative corrections to Higgs boson masses in BSM models, as well as the automation of these calculations, in order to set or improve constraints on New Physics coupling to the Higgs boson. A first chapter is devoted to the computation of the leading two-loop O (alpha_s alpha_t) corrections to neutral scalar masses in SUSY models with Dirac gauginos. Then, we show to address the Goldstone Boson Catastrophe -- a case of infra-red divergences due to massless Goldstone bosons that plague the calculation of effective potentials, tadpole equations, and self-energies -- in the context of general renormalisable field theories, by adopting an on-shell renormalisation scheme for the Goldstone masses. Afterwards, we illustrate the numerical implementation of our solution to the Goldstone Boson Catastrophe in the public tool SARAH. Finally, in a last chapter, we consider the high-scale behaviour of non-supersymmetric models with extended Higgs sectors.

Les Noyaux actifs de galaxie (AGN) incluent les sources quasi stables les plus énergétiques connues dans l'univers jusqu'à aujourd’hui. Du fait de leur distance, de leur haute luminosité et de leur petite taille, leurs régions intérieures ne sont pas directement résolvables avec les télescopes actuels. C’est pour ces raisons que nous avons besoin de techniques d’observation indirectes et de modèles théoriques pour discerner leur structure. Dans cette optique, le rôle de la polarimétrie est crucial. Elle a été ces dernières années la méthode clé qui a permis de développer le modèle unifié des AGN et pourrait, à l’avenir, nous offrir des nouveaux éléments pour sonder les régions des AGN irrésolues. Dans cette thèse, j’ai conduit des simulations sur les transferts radiatifs relatifs aux rayonnements continus émis des différentes régions intérieures des AGN en utilisant la nouvelle technique de cartographie de réverbération polarimétrique. Ce travail a été inspiré par les recherches de Gaskell et al. (2012). Le but de cette recherche est de fournir des modèles théoriques sur les différents composants des AGN en considérant le rayonnement polarisé en fonction du temps. La polarisation induite par la diffusion a été modélisée et différentes géométries de poussières circumnucléaires ont été testées. Les résultats incluent les effets de l’agrégation des poussières et différentes compositions de poussière. Pour étendre le modèle, les effets complémentaires des vents ionisés s’étirant en direction des pôles ont également été étudiés ainsi que ceux de l’anneau de diffusion équatorial théorique, avec pour postulat qu'il explique l’angle de polarisation observé dans les pôles des AGN. Les simulations ont été exécutées en utilisant une version du code STOKES incluant la dépendance temporelle. Il sera possible d'étendre ce travail à l'avenir. Les prochaines étapes suggérées incluront des raies d'émission aux modélisations ainsi que plus de complexité concernant la géométrie et la distribution de la poussière et/ou des électrons dans les régions de diffusion. Ce travail sera important pour profiter de futures données observationnelles systématiques avec un bon échantillonnage temporel. / Active galactic nuclei (AGN) include the most powerful quasi-steady sources of energy known to date in the universe. Due to their distance, high brightness and small size, their inner regions are not directly resolvable with current telescopes. This is the reason why indirect techniques and theoretical models are needed to discern their structure. In this scenario the role of polarimetry is crucial. In the past it was the key method that led to the development of the Unified Model of AGN and in the future, it may give us new clues to probe unresolved AGN regions. In this thesis, I conducted radiative transfer simulations for continuous radiation of different inner regions of the AGN using the new technique of polarimetric reverberation mapping. This work has been inspired by the work of Gaskell et al. (2012). The goal of this research is to provide theoretical models of the different components of the AGN considering time-dependent polarized radiation. Scattering induced polarization has been modeled and different circumnuclear dust geometries have been explored. The results include the effects of clumpiness and different dust compositions. To further extend the model, the effects of additional extended ionized winds along the polar direction have also been explored as well as the putative equatorial scattering ring postulated to explain the polarization angle observed in pole-on AGN. The simulations were run using a time-dependent version of the STOKES code. It will be possible to extend this work in the future. Suggested future steps are including emission lines in the models, as well as more complexity in the geometry and distribution of dust and/or electrons in the scattering regions. This work will be important for taking advantage of systematic future observational data with good temporal sampling.

Les domaines millimétrique et submillimétrique sont des domaines qui permettent de caractériser la physico-chimie des atmosphères <br />planétaires par l'observation des molécules qui les composent. Le télescope spatial Herschel et l'interféromètre ALMA, qui <br />entreront prochainement en service, permettront d'améliorer considérablement notre connaissance des atmosphères planétaires.<br /><br />L'un des principaux objectifs de cette thèse est de développer un modèle d'analyse des observations millimétriques et submillimètriques qui seront effectuées avec Herschel et ALMA. C'est en ce sens que nous détaillons un modèle qui tient compte de la géométrie sphérique des corps observés et des spécificités instrumentales propres aux télescopes utilisés. <br /><br />Dans un premier temps, ce qui a permis notamment de valider notre modèle de transfert radiatif, nous avons étudié l'origine des <br />composés oxygénés dans les atmosphères des planètes géantes. Nous présentons l'analyse d'observations de Saturne et d'Uranus, effectuées avec les télescopes de l'IRAM et du JCMT, pour contraindre les sources de monoxyde de carbone dans ces atmosphères. Nous améliorons ainsi les limites supérieures précédemment publiées et réalisons la première observation du monoxyde de carbone dans l'atmosphère de Saturne dans <br />le domaine submillimètrique. Cette observation prouve l'existence d'une source externe pour ce composé. Nous analysons également des observations récentes de Jupiter, effectuées par le télescope spatial Odin, pour contraindre l'origine externe de l'eau dans la stratosphère de cette planète. Les observations confirment que la chute de la comète Shoemaker-Levy~9 est vraisemblablement la source principale d'eau. <br /><br />Dans un second temps, nous avons appliqué notre modèle à l'étude de la structure thermique et la dynamique de l'atmosphère de Mars, à partir d'observations du monoxyde de carbone. Ces observations sont comparées aux prédictions d'un modèle de circulation générale, ce qui permet de vérifier la validité de ses prédictions et de fournir de nouvelles contraintes observationnelles pour ce type de modélisations.<br /><br />Enfin, nous avons appliqué notre modèle à l'étude des planètes géantes avec le télescope spatial Herschel, dans le cadre du programme-clé de temps garanti du télescope spatial Herschel "Water and related chemistry in the Solar System''. Nous avons également identifié les améliorations à apporter à notre modèle pour analyser des observations ALMA.

L'hydrodynamique radiative est le domaine dans lequel gaz et rayonnement interagissent dynamiquement. Ses champs d'application sont très vastes, de l'astrophysique à la fusion par confinement inertiel.<br /><br />Lors de cette thèse, un code numérique parallèle tridimensionnel d'hydrodynamique radiative baptisé HERACLES a été développé. Il s'appuie sur le modèle M1 qui permet de traiter un rayonnement à forte anisotropie. De nombreux tests ont validé HERACLES sur une grande variété de conditions physiques, dont le régime semi-transparent et la diffusion des photons, ses résultats étant comparables aux codes Monte-Carlo. Il a ensuite été utilisé dans deux thématiques.<br /> <br />La première concerne les chocs radiatifs, phénomènes astrophysiques reproduits sur Terre grâce aux lasers de puissance. HERACLES a mis en évidence l'influence de différents paramètres sur l'évolution d'un tel choc : le rapport de la largeur du canal de propagation sur le libre parcours moyen de photons, l'albédo des parois... Il a ensuite contribué à l'analyse d'une expérience réalisée avec le laser PALS. Il a permis de reproduire la courbe de décélération du précurseur observée dans l'expérience ainsi que la transmission du diagnostic transverse.<br /><br />La seconde thématique concerne les jets générés par les étoiles en formation et interagissant avec le nuage moléculaire environnant. Les opacités du milieu interstellaire montrant qu'une partie significative du rayonnement est absorbée, nous avons mené les premières simulations d'un jet tenant compte du transfert radiatif. Elles ont montré que le jet pouvait être fortement comprimé et que le transfert radiatif semble donc pouvoir jouer un rôle important dans sa propagation.

<p>Comets are the most primordial and least evolved bodies in the Solar System. As such, they are unique sources of information regarding the early history of the Solar System. However, little is known about cometary nuclei since they are very difficult to observe due to the obscuring coma. Indirect methods are therefore often used to extract knowledge about nucleus parameters such as size, shape, density, material strength, and rotational properties. For example, tidal and non-tidal splitting of cometary nuclei can provide important information about nuclear densities and material strengths, but only if the criteria for mechanical stability are well known. Masses and densities of cometary nuclei can also be obtained by studying orbital modifications due to non-gravitational forces, but only if the thermophysics of comets can be modelled accurately. </p><p>A detailed investigation is made regarding the mechanical stability of small Solar System bodies. New expressions for the Roche distance are derived, as functions of the size, shape, density, material strength, rotational period, and spin axis orientation of a body. The critical rotational period for centrifugal breakup in free space is also considered, and the resulting formulae are applied to comets for which the size, shape and rotational period have been estimated observationally, in order to place constraints on their densities and material strengths. </p><p>A new thermophysical model of cometary nuclei is developed, focusing on two rarely studied features - layer absorption of solar energy, and parallel modelling of the nucleus and innermost coma. Sophisticated modelling of radiative transfer processes and the kinetics of gas in thermodynamic non-equilibrium form the basis for this work. The new model is applied to Comet 19P/Borrelly, and its density is estimated by reproducing the non-gravitational changes of its orbit.</p>

<p>This thesis is a detailed observational study of the accretion processes in T Tauri stars (TTS). The interaction between the central star, the circumstellar disk and the magnetic field gives rise to a wide range of features in the spectra of TTS. The current picture of TTS is based on rather simple models assuming that accretion is a homogeneous and axisymmetric process. Although these models have been successful in explaining some observational signatures of TTS such as the shape of emission lines, the static nature of these models makes them unsuitable for describing the strong variability of the veiling spectrum and emission lines of TTS. An improved understanding of this variability is of key importance to study the dynamic processes related to the accretion flow and the winds.</p><p>This study is based on a set of high-quality spectroscopic observations with the UVES spectrograph at the 8-m VLT in 2000 and 2002. These spectra, with exposure times as short as 10-15 minutes, have high spectral resolution and high signal-to-noise ratios and cover a large part of the optical wavelength range. From this dataset we determine the basic physical parameters of several TTS and model their photospheres. These models then serve as a basis for a detailed investigation of variations of the veiling continuum and line emission. We confirm that the level of veiling correlates with some of the strongest emission lines and that coherent changes in accretion occur on a timescale of a few hours, comparable to the free-fall time from the disk to the star. From the properties of the emission lines formed close to the central star and in the stellar wind we derive restrictions on the geometry of the observed systems.</p><p>Because the intrinsic axial symmetry of a single star makes it almost impossible to disentangle rotational modulation from inhomogeneity and axial asymmetry of the accretion flow, we study a series of spectra of a close spectroscopic binary at different orbital phases and derive the 3D structure of flows between the disk and the star. Finally, we calculate the profiles of hydrogen emission lines by iteratively solving 3D NLTE radiative transfer in a state-of-the-art magnetospheric model.</p>

<p>This thesis treats the mass range of charmonium states and excited gluonic fields in two experiments, BESII and PANDA, and outlines a phenomenological model that connects them.</p><p>In BESII, <i>e</i>⁺<i>e</i>^– form a charmonium initial state, which is utilised as a source for secondary particles. The analysed channels, <i>ψ</i>´→ <i>γK</i>⁺<i>K</i>^– and <i>ψ</i>´→ <i>γπ</i>⁺<i>π</i>^–, give access to intermediate scalar states such as the two glueball candidates: f₀(1500) and f₀(1710). The f₀(1710) is indeed observed in decay into both <i>π</i>⁺<i>π</i>^– and <i>K</i>⁺<i>K</i>^– and the f₀(1500) is accepted as a necessary part of the <i>π</i>⁺<i>π</i>^– signal at the moderate 5% level. In addition, we observe the two tensor states f₂(1270) (in both channels) and f₂´(1525) (in <i>K</i>⁺<i>K</i>^–), but the need for the f₂´(1525) is not firmly established. The region around 2 GeV/<i>c</i>² is fitted with an f₄(2050) and an f₀(2200) in <i>π</i>⁺<i>π</i>^–. This region is fairly flat in <i>K</i>⁺<i>K</i>^– with a slight peak at the f₀(2200). Branching ratios for all eight channels are given. A fit to the angular distribution of ψ´→ γ f₂(1270) → <i>γ π</i>⁺<i>π</i>^–gave two possible solutions for the relative importance of helicity projections zero, one and two.</p><p>The future <i>pp</i>bar experiment PANDA is still in the development phase; important physics goals have been defined and we are now taking on the laborious task of constructing a detector that is able to fulfil them. A simulation investigation of a theoretically preferred <i>J</i><i>PC</i>=1^–+ charmonium hybrid (<i>H</i><i>c</i>) is presented: <i>ppbar</i> → <i>H</i><i>c</i><i>π</i>⁰/<i>η</i>, <i>H</i><i>c</i> → <i>χ</i><i>c</i>₁ (<i>π</i>⁰<i>π</i>⁰)<i>S–wave</i>, <i>χ</i><i>c</i>₁ → <i>J</i>/<i>ψπ</i>⁰, with a final state of seven photons and a lepton pair. To detect this channel next to full coverage of CM phase space is needed and as little material as possible before the electromagnetic calorimeter. </p><p>A second simulation study of <i>pp</i>bar → <i>η</i><i>c</i> → <i>γγ</i> at PANDA, suggests that the channel should be possible to detect with a signal-to-background ratio of 5±1 and a detection efficiency of at least 10%. </p><p>By assuming a constant matrix element we obtain a relation between the decay width for <i>ψ</i> → <i>pp</i>bar+<i>m</i>, which has been measured at BES for several cases, and the cross section for <i>pp</i>bar charmonium production in association with the same light meson, <i>m</i> (at for example PANDA). Cross sections of ~300–3000 pb were predicted for J/ψ production and ~30 pb for <i>ψ</i>' production. Isoscalars seem to be preferred to isovectors in <i>J</i>/<i>ψ</i> production, this might however be an artefact of simplifications within the model. A comparison with the only measured cross section, <i>pp</i>bar → <i>J</i>/<i>ψπ</i>⁰, suggests that the model is useful as a first estimate.</p>

<p>Part I of this thesis is a theoretical background to parts II and III.</p><p>Part II treats the phenomenon of decreased visibility through a glazing due to external water condensation, dew, on the external surface. Some simulations are presented where it is shown that under certain circumstances condensation can be expected. A combination of coatings on the external surface is suggested to overcome the problem of external condesation. It consists of both a coating which decreases the emissivity of the surface and a hydrophilic coating which reduces the detrimental effects to the view through the window.</p><p>Fresnel calculations of the optical properties are used to discuss the feasibility of using different coatings. A new test box was used to verify that the proposed window coatings perform as expected.</p><p>Part III is a study on the angular dependence of solar absorptance in windows. Optical properties vary with the angle of incidence of the incoming light. The variation is different from one window pane to another. </p><p>A model is proposed to approximate the angular variation of the solar absorptance in window panes. The model is semi-empirical and involves dividing the wide range of windows into nine groups. To which group a window belongs, depends on how many panes it has and on the features of the outer pane. The strength of the model is that it can be used without knowing the exact optical properties of each pane of the window. This makes it useful in the many cases when these data are not given by the manufacturer and Fresnel calculations to get the optical properties of the window are not feasible. The model is simple and can be added as an appendix to existing standards for measuring optical properties of windows.</p>

Radiative feedbacks associated with changes in water vapor, temperature, surface albedo and clouds remain a major source of uncertainty in our understanding of climate's response to anthropogenic forcing. In this dissertation climate model data is used to investigate variations in feedbacks that result from changing CO��� forcing and the time scales on which feedbacks operate, focusing on the applicability of one method in particular, the radiative kernel technique, to these problems. This computationally efficient technique uses a uniform, incremental change in feedback variables to infer top-of-atmosphere (TOA) radiative flux changes. The first chapters explore the suitability of the linear radiative kernel technique for large forcing scenarios. We show that kernels based on the present-day climate misestimate TOA flux changes for large perturbations, translating into biased feedback estimates. We address this issue by calculating additional kernels based on a large forcing climate state with eight times present day CO��� concentrations. Differences between these and the present-day kernels result from added absorption of radiation by CO��� and water vapor, and increased longwave emission due to higher temperatures. Combining present-day and 8xCO��� kernels leads to significant improvement in the approximation of TOA flux changes and accuracy of feedback estimates. While climate sensitivity remains constant with increasing CO��� forcing when the inaccurate present-day kernels are used, sensitivity increases significantly when new kernels are used. Comparison of feedbacks in climate models with observations is one way towards understanding the disagreement among models. However, climate change feedbacks operate on time scales that are too long to be evaluated from the observational record. Rather, short-term proxies for greenhouse-gas-driven warming are often used to compute feedbacks from observations. The third chapter of this dissertation examines links between the seasonal cycle and global warming using pattern correlations of spatial distribution of feedback variables and radiative flux changes. We find strong correlations between time scales for changes in surface temperature and climate variables, but not for TOA flux anomalies, reaffirming conclusions drawn in previous work. Finally, we investigate the fitness of the radiative kernel technique for evaluation of short-term feedbacks in a comparison with the more accurate, but more computationally expensive, partial radiative perturbations. / Graduation date: 2013