Hot microelectrodes are very small electrodes (usually 1 100 µm in diameter), which have a surface temperature much higher than the temperature in the bulk solution. In this work, the heating is achieved by applying an alternating potential of very high frequency (100 MHz 2 GHz) and of high amplitude (up to 2.8 Vrms) to the microelectrode. As a result, very fast (on the order of milliseconds) changes in the temperature of the electrolyte solution surrounding the electrode can be achieved. Due to the size of the heated microelectrodes, the hot zone in solution is small. Therefore, the solution can be easily overheated and temperatures above the boiling point can be reached.<p> The purpose of this research was to investigate and understand the phenomena occurring at ac polarized microelectrodes and to propose new applications of these electrodes. Using both steady-state and fast-scan (10 V/s) cyclic voltammetry measurements, mass transport of redox species has been studied at ac heated microelectrodes. It has been established that the convection at hot-disk microelectrodes is driven primarily by the electrothermal flow of an electrolyte solution. In addition, other effects such as ac dielectrophoresis and Soret (nonisothermal) diffusion are also observed. Numerical simulations have been employed to predict the distribution of temperature in the hot zone, the direction and magnitude of the electrothermal force and the solution flow rate, as well as the voltammetric response of hot-disk microelectrodes. The results of the simulations agree well with the experimental observations. Theoretical findings of this PhD work are very important for the understanding of the fundamentals of high temperature electrochemistry, particularly mass transport. The proposed explanation of the convection mechanism is most likely applicable not only to ac polarized microelectrodes, but also to the microwave heated microelectrodes, since the only difference between these two heating methods is in the way of delivering electrical energy (wired vs. wireless). The results of the studies of Soret diffusion indicate that it contributes significantly to mass transfer of redox species at hot microelectrodes. Taking into account that the magnitude of the Soret effect has been considered negligible by other electrochemists, the results obtained in this work prove the opposite and show that Soret diffusion affects both the faradaic current and the half-wave potential of the redox reaction. Therefore, the Soret effect can not be ignored if working with hot microelectrodes.<p> Hot microelectrodes can have a number of interesting applications. The results of the initial investigations indicate that these electrodes can be successfully used in the arrangement for Scanning Electrochemical Microscopy (such a novel technique is termed Hot-Tip SECM). In addition, the observed dielectrophoretic and electrothermal convection effects can enhance the performance of the electrochemical sensors based on hot microelectrodes. This can lead to the improvement of the detection limits of many biologically important analytes, such as proteins, bacteria and viruses.

Numerical simulations of Mach shock reflections have shown that the Mach stem can bifurcate as a result of the slip line jetting forward. Numerical simulations were conducted in this study which determined that these bifurcations occur when the Mach number is high, the ramp angle is high, and specific heat ratio is low. It was clarified that the bifurcation is a result of a sufficiently large velocity difference across the slip line which drives the jet. This bifurcation phenomenon has also been observed after triple point collisions in detonation simulations. A triple point reflection was modelled as an inert shock reflecting off a wedge, and the accuracy of the model at early times after reflection indicates that bifurcations in detonations are a result of the shock reflection process. Further investigations revealed that bifurcations likely contribute to the irregular structure observed in certain detonations.

Hot microelectrodes are very small electrodes (usually 1 100 µm in diameter), which have a surface temperature much higher than the temperature in the bulk solution. In this work, the heating is achieved by applying an alternating potential of very high frequency (100 MHz 2 GHz) and of high amplitude (up to 2.8 Vrms) to the microelectrode. As a result, very fast (on the order of milliseconds) changes in the temperature of the electrolyte solution surrounding the electrode can be achieved. Due to the size of the heated microelectrodes, the hot zone in solution is small. Therefore, the solution can be easily overheated and temperatures above the boiling point can be reached.<p> The purpose of this research was to investigate and understand the phenomena occurring at ac polarized microelectrodes and to propose new applications of these electrodes. Using both steady-state and fast-scan (10 V/s) cyclic voltammetry measurements, mass transport of redox species has been studied at ac heated microelectrodes. It has been established that the convection at hot-disk microelectrodes is driven primarily by the electrothermal flow of an electrolyte solution. In addition, other effects such as ac dielectrophoresis and Soret (nonisothermal) diffusion are also observed. Numerical simulations have been employed to predict the distribution of temperature in the hot zone, the direction and magnitude of the electrothermal force and the solution flow rate, as well as the voltammetric response of hot-disk microelectrodes. The results of the simulations agree well with the experimental observations. Theoretical findings of this PhD work are very important for the understanding of the fundamentals of high temperature electrochemistry, particularly mass transport. The proposed explanation of the convection mechanism is most likely applicable not only to ac polarized microelectrodes, but also to the microwave heated microelectrodes, since the only difference between these two heating methods is in the way of delivering electrical energy (wired vs. wireless). The results of the studies of Soret diffusion indicate that it contributes significantly to mass transfer of redox species at hot microelectrodes. Taking into account that the magnitude of the Soret effect has been considered negligible by other electrochemists, the results obtained in this work prove the opposite and show that Soret diffusion affects both the faradaic current and the half-wave potential of the redox reaction. Therefore, the Soret effect can not be ignored if working with hot microelectrodes.<p> Hot microelectrodes can have a number of interesting applications. The results of the initial investigations indicate that these electrodes can be successfully used in the arrangement for Scanning Electrochemical Microscopy (such a novel technique is termed Hot-Tip SECM). In addition, the observed dielectrophoretic and electrothermal convection effects can enhance the performance of the electrochemical sensors based on hot microelectrodes. This can lead to the improvement of the detection limits of many biologically important analytes, such as proteins, bacteria and viruses.

High Mach-number compressible flows with heat release are inherently more complicated than incompressible flows due to, among other reasons, the activation of the thermal energy mode. Such flow fields can experience significant fluctuations in density, temperature, viscosity, conductivity and specific heat, which affect velocity and pressure fluctuations. Furthermore, the flow field cannot be assumed to be dilatation-free in high Mach numbers and even in low Mach-number flows involving combustion, or in boundary layers on heated walls. The main issue in these high-speed and highly-compressible flows is the effect of thermal gradients and fluctuations on turbulence. The thermal field has various routes through which it affects flow structures of compressible turbulence. First, it has direct influence through pressure, which affects turbulence via pressure-strain correlation. The indirect effects of thermal fields on compressible turbulence are through the changes in flow properties. The high temperature gradients alter the transport coefficient and compressibility of the flow. The objective of this work is to answer the following questions: How do temperature fluctuations change the compressible flow structure and energetics? How does compressibility in the flow affect the non-linear pressure redistribution process? What is the main effect of spatial transport-coefficient variation? We perform direct numerical simulations (DNS) to answer the above questions. The investigations are categorized into four parts: 1) Turbulent energy cascade and kinetic-internal energy interactions under the influence of temperature fluctuations; 2) Return-to-isotropy of anisotropic turbulence under the influence of large temperature fluctuations; 3) The effect of turbulent Mach number and dilatation level on small-scale (velocity-gradient) dynamics; 4) The effect of variable transport-coefficients (viscosity and diffusivity) on cascade and dissipation processes of turbulence. The findings lead to a better understanding of temperature fluctuation effects on non-linear processes in compressible turbulence. This improved understanding is expected to provide direction for improving second-order closure models of compressible turbulence.

Abstract Reformer, the most important link of fuel cell, is the main set to create the hydrogen. After the fuel passes through the catalytic reaction by reformer, will produce hydrogen and chemical substances, the hydrogen will become the energy to support fuel cell. At the present day, the technology of PEM fuel cell and traditional fuel reformer has already existed, only need to reduce the volume, cost and to promote the efficiency. Catalytic layer, with the construction of microchannel, makes the adequate impact to gas and catalyst to promote the efficiency. This research uses the Lattice Boltzmann method (LBM) to simulate the fluid field and heat-mass transfer of microchannel, to discuss the function influence to the different parameter such as velocity, temperature, channel length, and channel height. The result displays, with the same inlet speed and temperature, by the increasing of the channel length, the amount of hydrogen will raise and residual methanol will reduce. When the channel length is more than 500£gm, the produce rate of hydrogen will not be a big change. If fix the channel length at 500£gm, under the different inlet temperature, while the maximum concentration at inlet, the speed of hydrogen at inlet is not the same. The best inlet speed will increase with the higher temperature. When fix the channel length at 500£gm, raising the altitude to 500£gm, the hydrogen product will not increase, on the contrary, it¡¦ll go down. Keywords¡GFuel cell reformer¡BMicorchannel of hat and mass transfer¡BNumerical simulations

Numerical simulations of Mach shock reflections have shown that the Mach stem can bifurcate as a result of the slip line jetting forward. Numerical simulations were conducted in this study which determined that these bifurcations occur when the Mach number is high, the ramp angle is high, and specific heat ratio is low. It was clarified that the bifurcation is a result of a sufficiently large velocity difference across the slip line which drives the jet. This bifurcation phenomenon has also been observed after triple point collisions in detonation simulations. A triple point reflection was modelled as an inert shock reflecting off a wedge, and the accuracy of the model at early times after reflection indicates that bifurcations in detonations are a result of the shock reflection process. Further investigations revealed that bifurcations likely contribute to the irregular structure observed in certain detonations.

This thesis considers various topics and open questions in galaxy formation during the epoch of reionization and presents multiple new computational techniques developed specifically to study this era. This work naturally divides into two main sections: 1) The formation of the first massive black holes and 2) Interpreting ALMA observations of galaxy formation during the epoch of reionization. The first topic addresses the existence of super massive black holes (SMBHs) with $M_{\rm BH} > 10^9$M$_{\odot}$ at $z > 6$. It is well established that stellar mass black holes are very unlikely to be able to accrete matter efficiently enough to grow to this mass at this redshift. For this reason, many alternative channels have been proposed for black hole formation that produce objects with significantly larger initial masses. In this thesis, I consider a mechanism whereby runaway stellar collisions in dense primordial star clusters form a very massive star that is likely to collapse to an intermediate mass black hole (IMBH) with $M_{\rm BH} > 10^3$M$_{\odot}$. In order to test this scenario, I added 12 species non-equilibrium chemistry to the massively parallel adaptive mesh refinement code RAMSES, and simulated, at sub-pc resolution, the collapse of the first metal-enriched halo which is likely to host a Population II star cluster. The properties of the central gas cloud in the collapsing halo were then extracted from the simulation and used to create initial conditions for the direct N-body integrator, NBODY6. These star clusters were simulated for 3.5Myr (until the first supernova is expected to occur) and it was determined that the properties of the gas clouds that form in cosmological simulations were indeed suitable to form a very massive star by collisional runaway. This suggests that this mechanism is a promising channel for forming the seeds of SMBHs at high redshift. The second topic of this thesis aims to help interpret the plethora of recent and upcoming ALMA observations of star forming galaxies during the epoch of reionization. These observations target far-infrared lines such as [CII] and [OIII] which directly probe the interstellar medium (ISM) of these $z > 6$ galaxies. In order to study this epoch, I employ the RAMSES-RT code, which allows for the computation of multifrequency radiative transfer on-the-fly. I modified this code in a number of ways so that it can handle radiation-coupled H$_2$ non-equilibrium chemistry (including Lyman-Werner band radiation) and I developed the variable speed of light approximation which changes the speed of light in the simulation depending on the density of gas so that ionisation fronts propagate at the correct speed in all gas phases. Cosmological boxes were initialised to include galaxies with masses comparable to the observations of Maiolino et al. (2015) and run at various resolutions to test convergence properties. One of the major goals of this study was to identify the physical mechanism responsible for the spatial offset observed between [CII] and UV/Lyα in many high-redshift galaxies.

L'origine de certains champs magnétiques stellaires observés et leur impact sur l'évolution des étoiles sont mal compris. C'est particulièrement vrai dans le cas des étoiles de masse intermédiaire de la séquence principale. Des relevés spectropolarimétriques récents ont en effet révélé l'existence d'une dichotomie magnétique inexpliquée, de 2 ordres de grandeur en terme de champ longitudinal, entre le fort champ des étoiles Ap/Bp et le faible champ des étoiles Vega-like. Le but de cette thèse est de tester la possibilité que cette dichotomie magnétique soit liée, comme proposé par Aurière el al. (2007), au développement d'instabilités magnétohydrodynamiques (MHD) dans la zone radiative des étoiles de masse intermédiaire. Pour cela, j'ai réalisé des simulations numériques MHD 2D et 3D qui permettent de suivre l'évolution d'un champ magnétique axisymétrique soumis initialement à une rotation différentielle dans une zone stratifiée de façon stable puis de considérer le développement d'instabilités MHD non-axisymétriques. L'influence de différents paramètres physiques des simulations, comme l'intensité initiale du champ magnétique poloïdal, le profil de rotation différentielle, la valeur des coefficients de diffusion ou encore l'importance de la stratification stable, a été testée. L'analyse des résultats des simulations montre que des instabilités MHD comme l'instabilité magnétorotationnelle et celle de Tayler peuvent se déclencher dans une zone radiative en rotation différentielle. En accord avec le scénario de Aurière et al. (2007), ces instabilités se développent assez pour modifier la structure spatiale à grande échelle d'un champ magnétique si l'intensité initiale du champ poloïdal est suffisamment faible par rapport à l'intensité initiale de la rotation différentielle. Le champ longitudinal calculé pour nos simulations les plus instables est diminué de 15% par rapport à un cas stable. Ce travail de thèse montre donc que les instabilités MHD sont des possibles candidats pour expliquer le désert magnétique des étoiles de masse intermédiaire de la séquence principale. / The origin of some of the observed stellar magnetic fields and their impact on stellar evolution are not well understood. This is particularly true for the main sequence intermediate-mass stars. Recent spectropolarimetric surveys have indeed exhibited an unexplained magnetic dichotomy, of 2 orders of magnitude in term of the longitudinal field, between the strong field of Ap/Bp stars and the weak field of Vega-like stars. This thesis aims to test the possibility that this magnetic dichotomy is linked to the development of magnetohydrodynamic (MHD) instabilities in the radiative zone of intermediate-mass stars, as proposed by Aurière et al. (2007). To do that, I have performed 2D and 3D MHD numerical simulations that allow to follow the evolution of an axisymetric magnetic field which is initially submitted to a differential rotation in a stably stratified zone and then to consider the development of non-axisymetric MHD instabilities. The influence of different physical parameters of the simulations, as the initial strength of the poloidal magnetic field, the differentially rotating profile, the diffusion coefficient values or the effect of the stable stratification, has been tested. The analysis of the simulation results show that MHD instabilities as the magneto-rotational instability or the Tayler instability can be triggered in a differentially rotating radiative zone. In agreement with the scenario of Aurière et al. (2007), these instabilities are enough developed to modify the large scale spatial structure of a magnetic field if the initial strength of the poloidal field is sufficiently weak with respect to the initial strength of the differentially rotation. The computed longitudinal field in our most unstable simulations is reduced by 15% with respect to a stable case. Therefore, this thesis work shows that the magnetic instabilities are possible candidates to explain the magnetic desert of the main sequence intermediate-mass stars.

Numerical simulations of Mach shock reflections have shown that the Mach stem can bifurcate as a result of the slip line jetting forward. Numerical simulations were conducted in this study which determined that these bifurcations occur when the Mach number is high, the ramp angle is high, and specific heat ratio is low. It was clarified that the bifurcation is a result of a sufficiently large velocity difference across the slip line which drives the jet. This bifurcation phenomenon has also been observed after triple point collisions in detonation simulations. A triple point reflection was modelled as an inert shock reflecting off a wedge, and the accuracy of the model at early times after reflection indicates that bifurcations in detonations are a result of the shock reflection process. Further investigations revealed that bifurcations likely contribute to the irregular structure observed in certain detonations.

Les vagues de tsunami sont des ondes longues générées par des événements géophysiques impulsifs de la croûte terrestre, de volcans, d’impacts d’astéroïdes et de glissements de terrain. Si la majorité des tsunamis sont d'origine tectonique, l'effondrement en masse d'un relief côtier peut constituer une source importante de l’aléa tsunami. Après une brève introduction sur les différentes générations de tsunamis dans l'histoire et les enjeux de cette thèse, le chapitre 1 présente les principaux résultats bibliographiques sur la génération et la propagation de tsunamis, ainsi qu’un rappel sur l’établissement des équations s’appliquant à l’étude des vagues extrêmes. Le second chapitre est dédié à la présentation des différents codes numériques utilisés dans ce manuscrit, à savoir, Gerris et SPHysics. Le chapitre 3 s'intéresse à la génération de tsunami par l’impact d’un bloc solide. Les résultats expérimentaux sont comparés aux résultats numériques des deux codes. A partir de là, une étude systématique a été faite, menant à des lois d’échelles sur le temps d’arrivée et l’amplitude de la première vague générée. Dans le chapitre 4, les interactions entre le glissement de terrain et la vague générée sont étudiées expérimentalement à l'aide d'impact granulaire initialement sec dans l'eau. Une étude systématiques des différents paramètres met en lumière l'importance des propriétés du glissement sur la vague générée. Enfin, Le chapitre 5 est dédié à l’étude de l’effondrement du Cap Canaille à Cassis. Cette étude numérique utilise un modèle de génération et de propagation simplifié afin d'estimer le potentiel destructeur d'un éventuel effondrement majeur. / Tsunami waves are long waves generated by impulsive geophysical events of earth's crust, volcanoes, asteroids impacts or landslides. Even if most of the tsunamis are generated by submarine earthquakes, the massive collapse of coastal landscape may constitute an important source of tsunami hazard. After introducing historical tsunami events, chapter 1 presents a state-of-the-art on the generation and propagation of tsunami waves and the main equations dealing with extreme water waves. Chapter 2 presents the numerical codes used in this thesis: Gerris and SPHysics. Chapter 3 focuses on the generation of tsunami by a solid landslide. Experimental results are compared to numerical simulations obtained using both codes. From this results, we derive scaling laws on the arrival time and amplitude of the first generated wave. The chapter 4 deals with the interactions between the slide and the generated wave by taking into account the impact of an initially dry granular media into water. Systematic studies varying the different parameters exhibit the significance of the internal properties of the slide on the generated wave. Finally, chapter 5 is dedicated to the collapse of the Cap Canaille near Cassis. A idealized model for the generation and the propagation are used to estimate the hazard associated to such a massive collapse.