This thesis analyses the behavior of an induction motor based on a mathematical model created for its simulation. The model describes the interaction of its several non linear differential equations to present a simulated output of induced torque and mechanical speed. Considering the applications to marine propulsion, it is also the goal of the project to design and test a control system for the speed of the motor by maintaining a specific cruse speed regardless the perturbations. / by Camilo Carlos Roa. / Thesis (M.S.C.S.)--Florida Atlantic University, 2010. / Includes bibliography. / Electronic reproduction. Boca Raton, Fla., 2010. Mode of access: World Wide Web.

To determine the effect of body shape on the response of underwater vehicles to surface waves in shallow water, the wave radiation hydrodynamic forces are evaluated for a family of (i) prolate spheroidal hull forms and (ii) cylindrical bodies with hemispherical nose and conical tail sections by systematically varying the geometric parameters but keeping displacement constant. The added-mass and wave damping coefficients are determined using a frequency-domain, simple-source based boundary integral method. Results are obtained for a range of wave frequencies and depths of vehicle submergence all for a fixed water depth of 10 m. With the wave exciting force and moment determined using the Froude-Krylov theory, the response transfer functions for heave and pitch are then determined. The heave and pitch response spectra in actual littoral seas are then determined with the sea state modeled using TMA spectral relations. Results show that vehicle slenderness is a key factor affecting the hydrodynamic coefficients and response. The results show two characteristics that increase the radiation hydrodynamic forces corresponding to heave and pitch motions: namely, vehicle length and further-away from mid-vehicle location of the body shoulder. The opposite is true for the oscillatory surge motion. By utilizing these observed characteristics, one can design the lines for maximum radiation forces and consequently minimum hull response for the critical modes of rigid-body motion in given waters and vehicle missions. In the studies carried out in the thesis, a hull with a long parallel middle body with hemispherical nose and conical tail sections has better heave and pitch response characteristics compared prolate spheroid geometry of same volume. The methodology developed herein, which is computationally efficient, can be used to determine optimal hull geometry for minimal passive vehicle response in a given sea. / Includes bibliography. / Thesis (M.S.)--Florida Atlantic University, 2014. / FAU Electronic Theses and Dissertations Collection

In recent decades, ecohydrology has received renewed attention because of the impacts of groundwater withdrawal on ecosystems. Growing population and urban expansion in Palm Beach County, FL. place pressure to eradicate natural areas, such as Florida scrub habitats, and increase groundwater withdrawal. This study presents preliminary results of soil and hydrological characterization of an ecological preserve surrounded by changing land use. Soil moisture and water levels were monitored to assess the effects of precipitation as influenced by plants and soil analysis determined the suitability of current soil conditions for hosting native vegetation habitats. Hydrologic and soil conditions on the preserve fall within values expected for native Florida scrub habitats. Hydrologic response to precipitation varied due to factors including antecedent conditions and vegetation types. These results provide a better understanding of the interactions between soil proper ties, hydrologic cycle, and plants, and assist with establishing a baseline to monitor changes over time. / Includes bibliography. / Thesis (M.S.)--Florida Atlantic University, 2015. / FAU Electronic Theses and Dissertations Collection

In near-shore transforming seas, as waves approach the shoreline, wave shoaling and sometimes wave breaking take place due to the decreasing water depth. When a ship advances through the transforming seas, the ship body and waves interact with each other substantially and can lead to unknown motions of the ship hull. The physical process of how the wave transforms in the surf zone and how the vehicle actually behaves when it passes through the transforming seas is a complicated issue that triggers considerable research interest. The goal of my research is to characterize the dynamics of a high-speed surface ship model in transforming seas through a parametric numerical study of the shipwave interactions. In this study, the vehicle of interest is a surface effect ship (SES) and we aim to contribute to developing a methodology for simulating the transforming wave environment, including wave breaking, and its interactions with the SES. The thesis work uses a commercial software package ANSYS Fluent to generate numerical waves and model the interface between water and air using the volume of fluid (VoF) method. A ship motion solver and the dynamic mesh are used to enable the modeled ship to perform three degree-of-freedom (DoF) motion and the near-region of the ship hull to deform as well as re-mesh. Non-conformal meshes with hybrid compositions of different cell types and various grid sizes are used in the simulations for different purposes. Five user-defined functions (UDFs) are dynamically linked with the flow solver to incorporates ship/grid motions, wave damping and output of the numerical results. A series of steps were taken sequentially: 1) validation for ship motions including simulation of a static Wigley hull under steady flows to compare against previous experimental results by other researchers, and the comparison between the static SES model under steady flows and the moving SES model advancing in the calm water; 2) study of the ship with 3 DoF advancing in calm water of both constant depth and varying depth; 3) validation for numerical waves, including predictions of numerically progressive waves in both a regular tank and a tank with a sloped fringing reef to compare with theoretical and experimental results, respectively; 4) investigation of the transforming characteristics of the wave traveling over the sloped fringing reef, which mimics the near-shore wave environment and a study of the dynamics of the SES through transforming waves. We find that the flow solver used in this study reliably models the wave profiles along the ship hull. The comparison between a static SES in a current and a moving SES in calm water at the same Froude number shows that although the velocity fields around the vehicle are significantly different, the wave profiles inside and outside the rigid cushion of the vehicle are similar and the resistance force experienced by the vehicle in the two scenarios agree well over time. We conducted five numerical simulations of the vehicle traveling from shallow water to deep water across the transition zone for different Froude numbers. From the results, we find that as the Froude number increases, the wave resistance force on the vehicle becomes larger in both shallow water and deep water. In addition, the overall mean resistance force experienced by the vehicle over the whole trip increases with the Froude number. Statistical analysis of the wave motions suggests that the energy flux decreases dramatically in the onshore direction as the waves break. The more severe the wave-breaking process, the greater the decrease in energy flux. Both the increase of Froude number and the wave steepness apparently increase the resistance force on the vehicle in the shallow water. This thesis work captures the impact of the transforming characteristics of the waves and closely replicates the behavior of how waves interact with a ship in transforming seas through numerical modeling and simulation. / Includes bibliography. / Dissertation (Ph.D.)--Florida Atlantic University, 2017. / FAU Electronic Theses and Dissertations Collection

We perform an event-by-event hydrodynamic analysis for Pb-Pb collisions at the incident energy of sqrt(sNN) = 2.76TeV, also studying the effects of two equations of state under the same initial conditions and freeze-out scenario: one characterized by a critical point and the other based on Lattice QCD (Quantum Chromodynamics) calculations. The observables of interest are particle spectra in terms of pseudorapidity and transverse momentum, as well as flow harmonics, which are coefficients that carry information on the initial anisotropies of the system throughout its evolution. Those are computed and compared with experimental Large Hadron Collider (LHC) data. There are slight differences in the results for each equation of state, caused by their distinct features. Lastly, the LHC-based calculations are compared with previous works related to the Relativistic Heavy-Ion Collider (RHIC) experimental data. The main techniques of the latter are performed in this work, which results in differences between some aspects in the outcome for each collision type, from initial energy distributions to freeze-out temperatures. / É feita uma análise de hidrodinâmica evento-por-evento para colisões de Pb-Pb à energia incidente de sqrt(sNN) = 2.76TeV. Estudamos os efeitos de duas equações de estado sob as mesmas condições iniciais e desacoplamento: uma é caracterizada por um ponto crítico e a outra é baseada em cálculos de Lattice QCD (Cromodinâmica Quântica). Os observáveis de interesse são os espectros de partículas em termos da pseudo rapidez e momento transversal, assim como os coeficientes harmônicos de Fourier que, por sua vez, carregam as anisotropias iniciais do sistema durante toda a sua evolução. Tais observáveis são calculados e comparados com dados experimentais do Large Hadron Collider (LHC). Por fim, os cálculos baseados em parâmetros referentes às energias do LHC são comparados com trabalhos anteriores feitos com base em dados experimentais do Relativistic Heavy-Ion Collider (RHIC). Os principais métodos usados no caso anterior são aplicados a este trabalho, o que resulta em algumas diferenças entre os resultados dos dois tipos de colisão, desde a distribuição de energia inicial a temperaturas de freeze-out.

Consideram-se neste trabalho seções bidimensionais oscilando em balanço. Adotam-se modelos representativos do movimento segundo este único grau de liberdade. Estimam-se os parâmetros de inércia e de amortecimento hidrodinâmicos por meio de experimentos de decaimento. Simulações numéricas incorporando os parâmetros estimados experimentalmente, bem como previsões empíricas de resultados da literatura, são confrontadas à registros experimentais para verificação da adequação das previsões, e para avaliação da adequação dos modelos à representação da dinâmica da oscilação. Com a metodologia de análise escolhida, avalia-se a influência de determinados parâmetros sobre as propriedades hidrodinâmicas; consideram-se variações: de proporções da seção, de posição vertical do centro de massa, de inércia própria em balanço, de forma do bojo, e quanto a presença de bolina e suas proporções. Também é considerada a influência do ângulo inicial de banda nas propriedades hidrodinâmicas, bem como a participação da energia irradiada pela onda na energia acumulada pelo sistema anterior ao início do movimento. Os elementos anteriores levam à proposição de orientações para avaliação da influência das propriedades geométricas e inerciais no comportamento do casco em balanço. / The scope of this work is the verification of hydrodynamic properties of two dimensional rolling sections. Analytical models of a single degree-of-freedom movement are adopted. The added inertia and damping are estimated by free decay tests. Numerical simulations with the obtained experimental parameters as well as empirical literature results are compared to the data tests in order to verify the adequacy of the procedures. With the chosen method of analysis, the influence of the hydrodynamic parameters are verified. The following parameters are considered: the beam draft ratio, vertical position of center of gravity, moment inertia, bilge shape and the addition or not of bilge keels. The initial angle of roll is also considered as well as the transport of the energy accumulated before the decay by the wave generated by the movement of the model. These elements lead to the proposition of orientations for the verification of the influence of geometric and inertial properties in the behave of rolling two-dimensional sections.

De acordo com o modelo sequencial de acreção, os planetas gigantes se formam através de um núcleo sólido a partir da captura de planetesimais. Esse núcleo, atingindo uma determinada massa, é capaz de capturar o gás residual do disco protoplanetário que constituirá o seu envelope, formando, então, um planeta gigante (Mizuno, 1980; Pollack et al., 1996). A parte crtica desse cenário está no ajuste dos tempos de formação do núcleo sólido, de captura do gás e dos processos de migração planetária com o tempo de vida do disco (Mordasini et al., 2010). Resultados numéricos mostram que o tempo necessário para a formação de um planeta gigante é muito alto em relação ao tempo de vida do disco, e, que a migração planetária pode ser muito rápida, levando os planetas a carem na estrela antes de sua completa formação. Em geral, os trabalhos sobre formação planetária tratam a migração do planeta utilizando prescrições analíticas (Fortier et al., 2013). No entanto, diversos efeitos associados à termodinâmica do disco de gás fazem com que esses modelos analíticos sejam limitados para lidar com a migração planetária (Paardekooper et al., 2010). De fato, para lidar com a migração planetária de tipo I, esses resultados analíticos se utilizam de discos de gás fisicamente simples e da linearização das equações da hidrodinâmica (Meyer-Vernet e Sicardy, 1987; Tanaka et al., 2002). Para a migração de tipo II, a situação é ainda mais complicada, já que a alta massa do planeta cria um gap em torno da órbita planetária, que impõe uma quebra da linearidade, impossibilitando a obtenção de uma prescrição analtica (Bryden e Lin, 1999). Assim, os resultados numéricos obtidos a partir de simuladores hidrodinâmicos, como o FARGO3D (Masset, 2000; Bentez-Llambay e Masset, 2016), ZEUS (Stone e Norman, 1992), PLUTO (Mignone et al., 2012), entre outros, são essenciais para uma análise mais robusta dos processos de migração planetária dentro de uma gama maior de condições fsicas para o disco de gás. No entanto, os simuladores hidrodinâmicos que tratam da interação do planeta com o disco de gás, em geral, não possuem um modelo para formação planetária. Em alguns deles, modelos para acreção de gás são construdos com base no regime de runaway dessa acreção (Kley, 1999). Todavia, a acreção de sólidos e a acreção de gás para planetas de baixa massa, na maior parte dos casos, não são levadas em consideração. Boa parte disso se deve ao fato de os modelos de formação planetária usarem simulações N-corpos, que, aliados ao código hidrodinâmico, seriam altamente custosos computacionalmente. Assim, torna-se necessário o uso de modelos alternativos para a formação planetária, que sejam capazes de reproduzir os resultados de uma simulação N-corpos de forma confiável. Construir um modelo que considera a acreção de sólidos e gás é uma tarefa árdua e ao mesmo tempo desafiadora. Assim, o presente projeto propõe a implementação de um cenário fisicamente plausível para a formação planetária dentro do código magneto hidrodinâmico FARGO3D. Para modelar a acreção de planetesimais, usamos como base os trabalhos de Guilera et al. (2010) e Fortier et al. (2013), que utilizam um modelo estatstico para determinar a taxa de acreção de planetesimais (Inaba et al., 2001). Esse modelo será implementado pela primeira vez no FARGO3D. Atualmente, sabe-se que a acreção de peebles (material sólido entre cm e mm) tem um impacto importante na formação planetária (Lambrechts e Johansen, 2014; Guilera, 2016; Johansen e Lambrechts, 2017). No entanto, núcleos de poucas massas terrestres possuem um envelope planetário que poderia destruir esses pebbles antes dele alcançar o núcleo (Venturini et al., 2015). Nesta tese, iremos nos preocupar apenas com a acreção de planetesimais, deixando o estudo do pebbles para trabalhos futuros. Para a acreção de gás, iremos modificar o modelo de Kley (1999) incorporado no FARGO antecessor. Essas modificações visam incorporar o raio de Bondi (Bondi, 1952) para determinar a zona de acreção, o efeito da altura do disco e a mudança na taxa de acreção de gás de acordo com a massa do planeta. As modificações implementadas no modelo de acreção de gás foram realizadas com base nos trabalhos de Dürmann e Kley (2015), Russell (2011) e Fortier et al. (2013). A adaptação no código de acreção de gás para levar em conta uma faixa maior de massas planetárias foi realizada utilizando a escala de tempo de Kelvin-Helmoltz. Para isso, seguimos o trabalho de Ikoma et al. (2000) e Idae Lin (2004b). Para testar o modelo de formação planetária no FARGO3D, a simulação padrão para o disco de gás utilizada nesta tese adota um disco bidimensional fino com taxa de acreção constante. A razão de aspecto do disco será de h = 0.05 com um fator de curvatura de = 0.0. Esses valores são consistentes com a teoria de discos finos e são usados nas maioria das simulações que envolvem discos de acreção (Bell et al., 1997; Frank et al., 2002). O disco é assumido localmente isotérmico e a viscosidade do disco é dirigida pela prescrição de Shakura e Sunyaev (1973), com = 0.03. O modelo de disco é simplificado e caractersticas importantes podem influenciar no processo de formação e migração planetária, como as trocas de energia. No entanto, ele é um ótimo modelo inicial para um teste consistente do modelo de formação planetária implementado, já que possui um resultado analtico conhecido. Casos mais complexos serão explorados em trabalhos futuros. Com o modelo de formação planetária implementado, foi possível estudar simultânea- mente a formação e a migração do planeta dentro do simulador hidrodinâmico. Isto é, analisamos a escala de tempo envolvida no processo de migração em conjunto com a escala de tempo da formação planetária para vários parâmetros fsicos envolvidos no modelo. A análise revelou, para nosso modelo de disco, que a escala de crescimento do planeta conseguiu se manter mais baixa que a escala de migração, mesmo quando o planeta atravessou a linha de gelo, local onde há menor quantidade de material disponvel para a acreção de sólidos. Assim, para planetesimais pequenos (raio 0.1 km), foi possvel obter planetas com massas próximas de 5 massas de Júpiter em regiões entre 0.5 e 1 ua, num tempo menor que o tempo de vida do disco. Vale ressaltar que esta tese conta com uma descrição detalhada de como implementar o modelo dentro do FARGO3D, incluindo um apêndice com o programa comentado linha a linha. O intuito é que o leitor possa usar esse modelo de formação e migração planetária para obter novos resultados e vnculos sobre a formação de sistemas exoplanetários ou do nosso Sistema Solar, assim como usar em qualquer outra aplicação que julgar necessária. / According to the sequential model of accretion, the giant planets are formed from a solid nucleus by capturing planetesimals. When this nucleus reaches a certain mass, it captures the residual gas of the protoplanetary disc that will constitute its envelope, forming a giant planet (Mizuno, 1980; Pollack et al., 1996). The critical part of this scenario is to adjust the planet formation and migration timescales with the lifetime of the disk (Mordasini et al., 2010). Numerical results show that the time required for the formation of a giant planet is very long compared to the lifetime of the disc, and that planetary migration can be very rapid, causing the planets to fall into the star before their full formation. In general, works on planetary formation use analytical models to deal with the migration of the planets (Fortier et al., 2013). However, these analytical models are limited given that they do not include several effects associated with the thermodynamics of the gas disc (Paardekooper et al., 2010). Indeed, in order to deal with planetary migration of type I, these analytical models use physically simple gas discs and rely on the linearization of the hydrodynamic equations (Meyer-Vernet e Sicardy, 1987; Tanaka et al., 2002). For the type II migration, the situation is even more complicated. This is due to the fact that the large mass of the planet creates a gap around the orbit of the planet, causing nonlinearities (Bryden e Lin, 1999). Thus, the numerical results obtained using hydrodynamic simulators, such as FARGO3D (Masset, 2000; Bentez-Llambay e Masset, 2016), ZEUS (Stone e Norman, 1992), PLUTO (Mignone et al., 2012), among others, are essential for a more robust analysis of the processes of planetary migration considering a wider range of physical conditions for the gas disc. However, in general, hydrodynamic simulators do not have a model for the planetaryformation. In some of them, models for gas accretion are built based of the runaway regime of accretion (Kley, 1999). Furthermore, the accretion of solids and the accretion of gas for low mass planets are not considered in most of the cases. This is mainly due to the fact that the models of planetary formation use N-body simulations that are computationally very expensive. Thus, it is necessary to use alternative models for the planetary formation, that are capable of reproducing the same results of an N-body simulation. Building a complete model that takes into account all these processes is a hard and challenging task. So, this project aims the implementation of a physically plausible scenario for a planetary formation inside the magneto-hydrodynamic code FARGO3D. For the accretion model we use the works by Guilera et al. (2010) and Fortier et al. (2013), which employ an statistical model to determine the accretion rate of planetesimals (Inaba et al., 2001). This model will be implemented for the first time in the FARGO3D code. It is now known that the accretion of peebles (material with size ranging from mm and cm) has a important impact on the planetary formation (Lambrechts e Johansen, 2014; Guilera, 2016; Johansen e Lambrechts, 2017), although cores with a few masses of the Earth have a planetary envelope that could destroy those pebbles, before they reach the nucleus (Venturini et al., 2015). In this thesis, we will only deal with the accretion of planetesimals, leaving the study of pebbles for future work. For the gas accretion, we use a modified model based on Kley (1999). The modifications aim to incorporate the Bondi radius (Bondi, 1952) to determine the accretion zone, the effect of the height of the disc and the frequency of accretion. The implemented modifications are based on the works by Dürmann e Kley (2015), Russell (2011) and Fortier et al. (2013). The adaptation in the gas accretion code to take into account a wider range of planetary masses was achieved using the Kelvin-Helmoltz timescale, according to the works by Ikoma et al. (2000) and Ida e Lin (2004b). To test the planetary formation model in FARGO3D, the standard simulation for the gas disc uses a bi-dimensional thin disc. The discs aspect ratio is h = 0.05 with a curvature factor of = 0.0. These values are consistent with the theory of thin dics and are used in most of the simulations for accretion discs (Bell et al., 1997; Frank et al., 2002). The disc is assumed to be locally isothermal and the viscosity of the disc is driven by the prescription from Shakura e Sunyaev (1973), with = 0.03. The disc model is simplified and important features, such as energy exchanges, may influence the process of planetary formation andmigration. However, it is a good initial model for a consistent test of the implemented model of planetary formation, which has an known analysical result. More complex cases will be explored in future work. With the newly implemented model for planetary formation, it was possible to simul- taneously study the planet formation and the planet migration using the hydrodynamic simulator. That is, we analyzed both the timescale for planetary formation and the timescale for the migration of the planet, and compared them for the parameters of the model. The analysis revealed that, for our disc model, the timescale of the growth rate of the planet remained lower than the migration timescale, even when the planet crossed the ice line, where there is less material available for solid accretion. Thus, for small planetesimals (1km radius) it was possible to obtain planets with masses of approximately 5 Jupiter masses in regions between 0.5 and 1 au, in nearly the same time as the lifetime of the disc. It is worth noting that this thesis presents a detailed description of how to implement the model for planetary formation in the FARGO3D, including an appendix with the commented code. The goal is to allow the reader to use this planet formation model to obtain new results both about the formation of exoplanetary systems and our Solar System, as well as use it in any relevant application.

L'imagerie par résonance magnétique (IRM) permet maintenant d'observer différents types de tissus avec des résolutions de plus en plus fines. L'arbre vasculaire artériel et veineux est explorable et les flux peuvent y être caractérisés de façon non invasive. Le versant artériel de l'arbre vasculaire peut être obtenu par une imagerie dite par « temps de vol » et le versant veineux par une imagerie en contraste de phase. Le développement de reconstructions de cartographies de susceptibilité magnétique (QSM) permet d'améliorer le niveau de détails atteignable sur les veines en fournissant en plus la possibilité de quantifier des paramètres physiologiques comme la saturation veineuse en oxygène. La mise en place d'algorithmes et outils dédiés permet la reconstruction in-silico d'une architecture cohérente sujet-spécifique. Par ailleurs grâce à l'emploi de séquences de la dynamique telles que le contraste de phase dynamique et l'imagerie par marquage des protons artériels du sang, les débits artériels, veineux, et perfusionnels sont mesurables. L'intégralité de ces acquisitions est non invasive, donc applicable à l'intégralité des sujets passant des IRM. Sur la base de ces données anatomiques et dynamiques, un modèle complet et sujet-spécifique de l'hydrodynamique intracrânienne est proposé. Le flux sanguin et cérébro-spinal est décrit dans ce modèle par les équations bilans fondamentales de l'hydrodynamique : conservation de la masse, conservation de la quantité de mouvement. Pour tenir compte de l'adaptation du diamètre des vaisseaux aux pressions on introduit pour chaque compartiment un paramètre d'élasticité de la paroi et une équation correspondante. Grâce aux données d'imagerie IRM, les compartiments sanguins des artères aux veines, le parenchyme cérébral et le système ventriculaire sont inclus. Le modèle permet de simuler la répartition des flux et des pressions dans les différents compartiments de la vascularisation du patient ainsi que d'évaluer les effets d'occlusions localisées sur l'ensemble de l'architecture. / The magnetic resonance imaging (MRI) allows the observation of various kind of tissues with always increasing resolution. The arterial and venous vascular trees can be explored, and the flows can be characterized in a noninvasive way. As an example, the arterial part of the tree can be obtained using so-called “Time Of Flight” MRI, and the venous part with phase contrast techniques. The development of quantitative susceptibility maps (QSM) improves the level of details achievable regarding veins; furthermore, it provides a new way to estimate physiological parameters such as venous saturation in oxygen. Eventually the implementation of dedicated algorithms and tools allows the in-silico reconstruction of a subject-specific coherent architecture. Moreover, due to the use of dynamic imaging sequences such as the dynamic phase contrast imaging and the arterial spin labeling, the arterial, venous and cerebral blood flow are measurable. All of these sequences are noninvasive and so usable on every subjects. Based on these anatomical and dynamics data, a full subject-specific model of the brain hydrodynamics is proposed here. The blood and cerebrospinal flow are described using basic balance equations of the hydrodynamics: continuity and momentum. To take into account of the adaptation of vessel diameter to the pressure, a wall elasticity parameter is added for each compartment together with the corresponding equation. Thanks to the MRI data, all the blood compartments, from arteries to vein, the cerebral parenchyma and the ventricular system are included. The model is able to simulate the flow and pressure repartition in all compartments of the subjects as well as show the impact of a located occlusion on the whole architecture.

Les instabilités de digitation sont des instabilités hydrodynamiques qui déforment l’interface entre deux fluides sous forme de doigts. Elles apparaissent lorsqu'un fluide plus mobile déplace un fluide moins mobile, ce qui peut être engendré par des gradients de densité (auquel cas on parlera de digitation de densité), de viscosité (digitation visqueuse) ou encore de tension de surface. Dans ce cadre, l’objectif de ce travail est d'étudier par une approche principalement expérimentale dans quelle mesure des réactions chimiques et des propriétés de mélange non idéal peuvent modifier voire induire de telles instabilités. Le but est de comprendre les dynamiques spatio-temporelles résultant de l’interaction entre réactions chimiques, diffusion, propriétés de mélange et instabilités de digitation. Pour ce faire, nous explorons expérimentalement et analysons à l’aide de modèles théoriques simples différentes dynamiques hydrodynamiquement instables dans des mélanges réactifs ou non idéaux. <p>Nous étudions tout d’abord l’évolution de la zone de mélange non idéal entre deux fluides purs lorsque le fluide le moins dense est placé au dessus du fluide le plus dense dans le champ de gravité. Nous montrons que le fait que la densité du mélange évolue de manière non monotone en fonction de sa composition peut être la source de digitation de densité. Nous étudions ensuite l'influence de réactions chimiques simples sur la digitation de densité à l'interface entre fluides miscibles et partiellement miscibles, en clarifiant l’impact de la diffusion différentielle entre divers solutés de solutions réactives et du taux de miscibilité sur le phénomène de digitation. Dans le cas de la digitation de viscosité, nous analysons tout d'abord dans quelle mesure une réaction chimique, en induisant des profils de viscosité non monotones, peut accroître ou limiter le développement de la digitation visqueuse. Nous démontrons de plus que, dans le déplacement stable d'un fluide moins visqueux par un fluide plus visqueux, une réaction chimique peut générer de la digitation visqueuse en induisant des profils de viscosité non monotones. Enfin, nous explorons expérimentalement l’étalement de films minces réactifs sur des substrats solides. Nous démontrons que, dans certaines conditions, des réactions chimiques peuvent induire des flux convectifs de Marangoni liés à des gradients de tension superficielle qui déstabilisent le bord du film par digitation, produisant un motif fractal. <p> / Doctorat en Sciences / info:eu-repo/semantics/nonPublished

Devido ao processo de urbanização sem planejamento adequado, as cidades costeiras sofrem com as inundações e erosão das praias com a elevação do nível do mar e ação de ondas. Entre as estruturas mais utilizadas para proteção de praias destacam-se os quebra-mares segmentados. Para estudar e prever as respostas praiais à presença destas estruturas, podem ser empregados modelos numéricos, capazes de calcular os processos complexos deste ambiente. Este trabalho teve como objetivo o estudo da resposta hidrodinâmica e sedimentar de uma praia com a implantação de quebra-mares segmentados. O modelo hidrodinâmico utilizado é o MIKE21FM acoplado ao modelo de ondas SW e sedimentos ST e SM. Primeiramente, foram impostas condições hidrodinâmicas simplificadas e diferentes arranjos de quebra-mares segmentados. As áreas erodidas e acrescidas após a implantação da obra foram comparadas e priorizou-se minimizar a área erodida. Em seguida, foram considerados os cenários de condições hidrodinâmicas variadas com uma das estruturas. Os resultados são apresentados em termos de altura significativa e potência de onda para 18 casos de condições hidrodinâmicas constantes, as quais foram feitas variar em nível e características da onda. Para a condição hidrodinâmica mais crítica, obteve-se uma redução de 0,4m da altura significativa média e 2kW/m da potência média da onda. Através desses resultados é possível aquilatar a proteção da região da praia da ação das ondas após a implantação da estrutura. Além disso, foram feitas duas simulações com 3 a 4 meses de evolução do fundo em condições hidrodinâmicas reais, com o intuito de apresentar qualitativamente as áreas de erosão e acreção do fundo da praia. Resultados mostraram que a deriva litorânea local tem direção sudeste, para a Ponta da Praia. Foi observada sedimentação no tardoz dos segmentos e na região de sombra e erosão nas áreas entre segmentos e a frente destes. Com isso, este trabalho colabora com o gerenciamento costeiro na região de Santos, apresentando o início de uma pesquisa para uma possível solução para os problemas de inundação e erosão da região da Ponta da Praia. / Erosion and flooding are common problems faced by coastal cities as a consequence of urbanization process without previous planning, with the sea level rise and the wave action. In order to mitigate these problems, shoreline protection structures are constructed along the coastlines, such as segmented breakwaters. Numerical models are tools frequently used in these studies because of its capacity of calculating the complex processes on a coastal environment. This study aim is to present a study based on the hydrodynamic and sediment transport response of a curved beach to the presence of segmented emerged breakwaters. The numerical model used is the MIKE21FM coupled with wave spectral and sediment transport modules. Firstly, constant boundary conditions were applied for the period of one year in order to understand the response of the beach to five different designs of coastal breakwaters. One of these structures were chosen to continue the study based on the area and length of the beach eroded and accreted. Secondly, eighteen different scenarios of wave and water level were applied to the selected structure and the protection of wave action were compared and analyzed. To the most critical hydrodynamic condition, the structure reduced 0,4 m of the mean significant wave height and 2 kW/m of the mean wave power. Finally, two real hydrodynamic conditions were applied and the sediment transport was qualitatively analyzed. Results show that the littoral drift in the studied area is directed to the southeast end of the beach, straight to the Ponta da Praia, without the spur breakwater, the sediment would end inside the navigation channel. Besides that, it shows the sedimentation and erosion patterns at the beach generated by the presence of the breakwater. The sediment is accumulated at the shadow area and at the lee, whereas the erosion is located at the front of the breakwaters and between the segments, as expected. Therefore, this study collaborates with the management of Santos, by presenting herewith a possible solution for the inundation and erosion problems of this area.