This thesis deals with the instabilities of the incompressible boundary-layer flow thatis induced by a disk rotating in otherwise still fluid. The results presented include bothwork in the linear and nonlinear regime and are derived from direct numerical sim-ulations (DNS). Comparisons are made both to theoretical and experimental resultsproviding new insights into the transition route to turbulence. The simulation codeNek5000 has been chosen for the DNS using a spectral-element method (SEM) witha high-order discretization, and the results were obtained through large-scale paral-lel simulations. The known similarity solution of the Navier–Stokes equations for therotating-disk flow, also called the von K ́arm ́an rotating-disk flow, is reproduced by theDNS. With the addition of modelled small simulated roughnesses on the disk surface,convective instabilities appear and data from the linear region in the DNS are anal-ysed and compared with experimental and theoretical data, all corresponding verywell. A theoretical analysis is also presented using a local linear-stability approach,where two stability solvers have been developed based on earlier work. Furthermore,the impulse response of the rotating-disk boundary layer is investigated using DNS.The local response is known to be absolutely unstable and the global response, onthe contrary, is stable if the edge of the disk is assumed to be at radius infinity. Herecomparisons with a finite domain using various boundary conditions give a globalbehaviour that can be both linearly stable and unstable, however always nonlinearlyunstable. The global frequency of the flow is found to be determined by the Rey-nolds number at the confinement of the domain, either by the edge (linear case) or bythe turbulence appearance (nonlinear case). Moreover, secondary instabilities on topof the convective instabilities induced by roughness elements were investigated andfound to be globally unstable. This behaviour agrees well with the experimental flowand acts at a smaller radial distance than the primary global instability. The sharpline corresponding to transition to turbulence seen in experiments of the rotating diskcan thus be explained by the secondary global instability. Finally, turbulence datawere compared with experiments and investigated thoroughly. / <p>QC 20170203</p>

L'objectif de cette thèse est d'étudier la formation de tourbillons dans la zone morte des disques protoplanétaires. Un code numérique 3D compressible a été mis au point et utilisé pour cette étude. Deux instabilités hydrodynamiques sont envisagées pour former les tourbillons: l'instabilité de Rossby et l'instabilité barocline.La première entraine la fragmentation d'une sur-densité annulaire en une chaîne de tourbillons qui se rattrapent les uns les autres et finissent par fusionner en un seul tourbillon qui reste stable sur de très longues durées lorsque son rapport d’aspect est suffisamment grand, et possède une structure quasi bidimensionnelle. En revanche, les tourbillons tridimensionnels de petits rapport d'aspect sont affectés par l’instabilité elliptique qui les détruits en quelques rotations. Seuls persistent ceux de grand rapport d'aspect.L'instabilité barocline, fondamentalement non linéaire, produit des tourbillons à partir de perturbations d'amplitude finies ; ces tourbillons sont ensuite amplifiés et fusionnent en tourbillons plus gros si le disque est stratifié de façon instable et s’il permet aussi le transfert de chaleur. Deux types de transfert thermique ont été envisagés pour étudier cette instabilité qui conduit alors à des différences significatives dans la structure des tourbillons formés. Le rapport d'aspect étant lié à la vorticité, l'amplification des tourbillons se traduit par une diminution de leur rapport d'aspect, et les rend donc sujet à l'instabilité elliptique. Cependant, ils ne sont pas détruit et gardent une structure tourbillonnaire grâce à l'amplification barocline. / The objective of this thesis is to study the formation of vortices in the dead-zone of protoplanetary disks. A 3D compressible numerical code has been performed and used for this study. Two hydrodynamical instabilities are considered for vortex formation: the Rossby wave instability and the baroclinic instability.The first one leads tp the fragmentation of an annular bump into a chain of vortices that catch one another and merge in a single vortex; this vortex remains stable on very long durations when its aspect ratio is large enough and has a quasi two-dimensional structure. In contrast, tridimensional small aspect ratios vortices are affected by the elliptical instability and are destroyed in a few rotation periods. Only vortices with large aspect ratios can survive.The baroclinic instability, a basically non-linear one, can produce vortices from small amplitude perturbations; these vortices are then amplified and merge in bigger vortices if the disk is unstably stratified and also permits heat transfer. Two types of heat transfer have been considered leading to significant differences in the structures of the resulting vortices. As aspect ratio and vorticity are strongly related, the baroclinic amplification reduces the aspect ratio and, so, make the vortex sensitive to the elliptical instability. However, such vortices are not destroyed and keep a vertical structure thanks to the baroclinic amplification.

No description available.

The thesis is dealing with spectral analysis of the B[e] star FS CMa, a prototype of FS CMa stars group. These objects are characterized by huge amount of matter in sourrounding shell which origin is not explained for many years. However, solving this issue could enrich stellar astrophysics by enhanced stellar evolution models. The goal of this thesis is to improve our understanding of FS CMa. We described spectral variability on various time scales and simulated spectra for different forms of the system in HDUST code. On the basis of new obtained spectra we confirmed long-term changes in variability of some spectral features and rapid variability of some spectral lines. We gained an estimate of the gas density. The simulations showed that spectral type of FS CMa is not certain and that the star could be surrounded by extended disk, many stellar radii wide. 1

京都大学 / 0048 / 新制・課程博士 / 博士(エネルギー科学) / 甲第20727号 / エネ博第355号 / 新制||エネ||70(附属図書館) / 京都大学大学院エネルギー科学研究科エネルギー基礎科学専攻 / (主査)教授 岸本 泰明, 教授 中村 祐司, 教授 田中 仁 / 学位規則第4条第1項該当 / Doctor of Energy Science / Kyoto University / DFAM

No description available.

Numerical simulations of supercritical coastal flows have been performed. The meso-γ-scale model which has been used in this study is non-linear, hydrostatic and has a higher-order turbulence closure. Previous studies of supercritical coastal flows with this model have given rise to some questions and hypotheses, e. g. is the gradual curvature of the main coastal mountains north of Cape Mendocino sufficient to excite an expansion fan? Is the local terrain of Cape Mendocino responsible for the collapse of the marine atmospheric layer (MABL) in Shelter Cove? This study was designed to answer these questions. The terrain used in the simulations was generated by a simple analytical function and fitted to the real terrain north of Cape Mendocino in a sense that it would reflect it as good as possible, neglecting ”small” changes in the orientation of the coast and height of the terrain. This made it possible to test hypotheses related to the coastline shape one by one. Simulations that were performed are: Piecewise linear coasts with constant terrain height where the change in coastline orientation, the height of the inversion and strength of the background wind speed was varied; Piecewise linear coasts where the height of the terrain was varying along the coast; Curved coastlines with different curvatures; Piecewise linear coasts with simplified capes perpendicular to the coast where the height of the cape was varied. It was found that the angle with which the coast turns away from the flow regulates the amount of acceleration in the following expansion fan. A decreasing height of the terrain along the coast lead to an increased acceleration of the flow, the largest acceleration was found when the slope of the terrain was confined to the change in coastline orientation. It was concluded that this is comparable to an increased change in coastline orientation. The simulations with curved coastlines confirmed the hypothesis that the gradual curvature of the main coastal mountains north of Cape Mendocino is sufficient to excite an expansion fan. In fact, a curved coastline leads to a stronger acceleration of the flow than a piecewise linear coastline. One of the most striking features in this study was that the acceleration of the flow started far upstream of the change in coastline orientation, even though the flows were supercritical. This phenomenon was mainly found in the cases with the highest wind speeds. It is suggested that the upstream acceleration of the flow is due to either high amplitude gravity waves propagating within the MABL or internal gravity waves propagating above the inversion. When a cape was inserted perpendicular to the main coastline, this showed that even with a cape as low as approximately half the depth of the MABL, the flow was significantly blocked. Indications of wave-breaking on the lee side of the cape was also found, which confirmed the hypothesis that the local terrain of Cape Mendocino is responsible for the collapse of the MABL in Shelter Cove.

Le dimensionnement des digues paravalanches s’appuie sur la connaissance des processus physiques liés au ressaut, qui se forme lorsqu’un écoulement fin et rapide rencontre un obstacle suffisamment haut pour ralentir et épaissir l’écoulement incident. La hauteur du ressaut est aujourd’hui calculée à partir d’équations strictement valides pour des écoulements de matériaux non frictionnels et non compressibles tels que l’eau, sur fond plat et lisse. Or, les avalanches de neige dense sont des écoulements compressibles qui ne peuvent avoir lieu qu’en pente, et au sein desquels se produit de la dissipation d’énergie par friction et collisions entre les grains. Il est donc essentiel de mieux connaître le comportement des ressauts dans les écoulements granulaires en pente. Pour cela, la thèse s’appuie sur plusieurs approches. Les ressauts granulaires stationnaires sont d’abord étudiés de manière purement théorique, à l’aide des équations de conservation de la masse et de la quantité de mouvement moyennées dans l’épaisseur, afin de trouver une relation générale pour prédire la hauteur des ressauts quelques soient les conditions d’entrée. Nous simulons ensuite numériquement un grand nombre de ressauts granulaires en faisant varier plusieurs paramètres (la pente du plan incliné, le débit, le diamètre des grains, la friction entre les grains) à l’aide de la méthode aux éléments discrets. Cette méthode permet d’accéder à la structure interne des ressauts, et notamment à la mesure des champs de vitesse, de fraction volumique, ou encore de la dissipation d’énergie. Les simulations sont réalisées en deux dimensions. Enfin, un dispositif de mesure innovant, qui utilise la radiographie à rayons X dynamique, a été adapté à une expérience de laboratoire existante pour créer des ressauts granulaires stationnaires. Cette technique de mesure permet, en particulier, de mesurer la distribution spatiale moyennée dans la largeur de l’écoulement de la fraction volumique avant, à l’intérieur et après le ressaut granulaire. La comparaison du nouveau cadre théorique proposé avec les résultats expérimentaux et numériques nous permet de mettre en évidence une grande diversité des types de ressauts granulaires en fonction des conditions initiales. Pour chaque type de ressaut, les lacunes du cadre théorique classique, qui ne tient pas compte des forces mises en jeu dans le ressaut ni de la compressibilité, sont clairement établies. / The design of avalanche protection dams relies on the understanding and modelling of physical processes related to the formation of jumps that form when a thin and fast flow meets an obstacle high enough to slow down and thicken the incoming flow. The jump height is nowadays calculated through equations that are strictly valid for non-frictional incompressible flows on a horizontal and smooth bottom. However, dense-snow avalanches are compressible granular flows taking place on a slope, and inside which energy is dissipated through enduring frictional contacts and collisions between grains. It is then essential to decipher the behaviour of jumps formed during granular flows down inclines. To this extent, the thesis relies on several approaches. Standing granular jumps are first studied in a purely theoretical way, with the help of depth-averaged mass and momentum conservation equations, in order to find a relation to predict the height of the jumps regardless of the input conditions. A great number of granular jumps are then simulated by varying several parameters (the slope angle of the incline, the discharge, the grain diameter, the grain-grain friction) thanks to the discrete element method. This method allows us to access to the internal structure of the jumps, and in particular to the spatial distributions of velocity, volume fraction and energy dissipation. Those simulations are done in two dimensions. Finally, an innovative measurement technique using dynamic X-ray radiography was adapted to an existing small-scale laboratory device to produce standing granular jumps. This technique allows in particular the measurement of the width-averaged spatial distribution of volume fraction before, inside and after the granular jumps. The comparison between the new theoretical framework proposed and both the experimental and numerical data, allows us to evidence a rich variety of granular jump patterns as a function of the input conditions. For each type of jump pattern, the shortcomings of the classical theoretical framework, which does not account for the forces at stake within the jump volume nor the compressibility, are well established.

Neste trabalho, analisamos três modelos definidos sobre redes e governados por dinÂmicas estocásticas. Nosso principal interesse repousa no estudo das transições de fase e no comportamento crítico desses modelos. O primeiro deles é o autômato celular pobabilístico da Domany-Kinzel, ao qual aplicamos o método de expansões em série. Em seguida, estudamos o comportamento para tempos longos de alguns processos de reação-difusão por meio de simulação numérica. Tais processos podem ser relevantes para o entendimento da compactação em sistemas granulares. Finalmente, também através de dimulações numéricas, analisamos o processo de contato conservativo, que é uma versão do modelo original definida em um ensemble onde o número de partículas é conservado. / In this work, we analyzed three lattice models governed by stochastic dynamics. Our main interest lies on the study of the phase transitions and critical behavior of these models. The first of them is the Domany-Kinzel probabilistic cellular automaton, to which we applied the method of series expansions. Next, we studied the long time behavior of some reaction-diffusion processes by means of numerical simulations. Such processes may be relevant to the understanding of granular compaction. Finally, also by means of numerical simulations, we have analyzed the conserved contact process, which is a version of the original model defined on an ensemble where the number of particles is conserved.

Neste trabalho, analisamos três modelos definidos sobre redes e governados por dinÂmicas estocásticas. Nosso principal interesse repousa no estudo das transições de fase e no comportamento crítico desses modelos. O primeiro deles é o autômato celular pobabilístico da Domany-Kinzel, ao qual aplicamos o método de expansões em série. Em seguida, estudamos o comportamento para tempos longos de alguns processos de reação-difusão por meio de simulação numérica. Tais processos podem ser relevantes para o entendimento da compactação em sistemas granulares. Finalmente, também através de dimulações numéricas, analisamos o processo de contato conservativo, que é uma versão do modelo original definida em um ensemble onde o número de partículas é conservado. / In this work, we analyzed three lattice models governed by stochastic dynamics. Our main interest lies on the study of the phase transitions and critical behavior of these models. The first of them is the Domany-Kinzel probabilistic cellular automaton, to which we applied the method of series expansions. Next, we studied the long time behavior of some reaction-diffusion processes by means of numerical simulations. Such processes may be relevant to the understanding of granular compaction. Finally, also by means of numerical simulations, we have analyzed the conserved contact process, which is a version of the original model defined on an ensemble where the number of particles is conserved.